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I woke up today super depressed. It snowed, and we have our heat on in our apartment so it just has that winter vibe. I'm just really triggered and I feel immobilized. I know logically it's probably the anniversary effect but it still feels like swimming through honey. | eng | 4a077f6f-540b-42a3-a7e0-0d5777a01f47 | https://www.alike.health/posts/d4ed6080-71c6-4e56-a8f6-6908535101a1 |
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What Causes An Eye Stye And How Can You Prevent One
A stye is a red, painful lump near the edge of the eyelid that may look like a boil or a pimple. It usually forms on the outside of the eyelid. Sometimes it can form on the inner side. In most cases, eye styes don't last long and will begin to appear on its own within a couple of days.
Most styes are harmless and won't affect your ability to see clearly. Try self-care measures first, such as applying a warm washcloth to your closed eyelids several times a day. The information following will help you identify the cause of eye stye so as to help you to figure out how to avoid it effectively.
Cause #1: Touching Mucus
Styes occur when the eyelid become blocked and infected. This infection is usually caused by common bacteria that reside on the lids. One of the easiest ways to spread bacteria are to touch the mucus from your nose. Make sure to wash your hands after touching any mucus before touching your eyelids. | eng | eeb7e669-e1d8-48b6-a4f0-772d4e6bb853 | https://www.livefit101.com/posts/what-causes-an-eye-stye-and-how-can-you-prevent-one/?itm_source=livefit101&itm_medium=under&itm_campaign=internal |
Chiapas: Corporate Polluters Lust for Trees
REDD (Reducing Emissions from Deforestation and Forest Degradation) purports to combat global warming by saving rainforests, but without reducing greenhouse gas emissions, nor putting the capitalist system and its excesses—the real causes of environmental disaster—on the table.
With REDD, the companies contaminating the planet the most will be able to continue their activity if, in return, they financially support communities in the Global South to conserve the forests they live in. Photo Orin Langelle.
REDD in the Lacandon Jungle: The Political Use of a Program Against Climate Change
Carbon Offsets: A Solution to Deforestation? REDD (Reducing Emissions from Deforestation and Forest Degradation) is a United Nations program meant to fight climate change. It will be put into effect after the Kyoto Protocol expires in 2012, and it includes forests on the Carbon Credit market.
With REDD, the companies contaminating the planet the most will be able to continue their activity if, in return, they financially support communities in the Global South to conserve the forests they live in. According to the program's promoters, it will absorb these companies' CO2 emissions, thereby saving our planet, while at the same time these communities grow economically. "These mechanisms fulfill the objectives of sustainable development: they fight poverty and climate change at the same time", Mexican president Felipe Calderón declared at the COP16 in Cancún.
As such, it purports to combat global warming without reducing greenhouse gas emissions, and without putting the capitalist system and its excesses—the real causes of environmental disaster—on the table. Some consider the program a danger to biodiversity, indigenous communities and carbon markets
REDD in Mexico. A view from Mexico shows that REDD is not a panacea to solve deforestation and yet, it may contribute to existing programmes that strengthen sustainable (community) forest management.
Deforestation is often driven by economic needs of local communities, but economic greed is the determinant: illegal logging, tourism developments, public and private infrastructure creation (from highways to oil drilling), forest fires, activities of drug cartels, local power conflicts and unsustainable ideas of economic modernization.
Consider an approximated 70 – 80% of Mexican forests are ejidos, i.e. under communal management. The economic reforms under President Salinas two decades ago strengthened property rights of ejidos, yet, given strict land use regulations, communities have little possibility to gain incomes from forestry related activities, not to mention conservation. Thus, the opportunity cost to leave forests standing is too high for many of the impoverished forest communities and (illegal) land conversion for agricultural purposes is one of the main causes of deforestation according to one of the latest reports of the National Forest Commission (CONAFOR).
In this scenario, REDD earnings could support existing programmes to a) decrease the opportunity costs of conserving forests; b) do justice to communities who protect their forests and pay for their conservation of environmental services; and c) support government and communities in fighting against illegal land conversion and deforestation.
"REDD: The Lust for Trees and the Case of Chiapas: the Lacandon Rainforest to the Highest Bidder" Produced by Otros Mundos AC/Amigos de la Tierra México with the help of Amigos de la Tierra Internacional, Fundación Siemenpuu and Global Justice Ecology Project.
REDD in the Lacandon Rainforest
Analyzing the application of REDD to the Lacandon Jungle in the Mexican state of Chiapas, all of the problems brought by the program begin to surface. California and the state of Acre (Brazil) have for some time now had their eyes on the Chiapan jungle, Latin America's second lung. In November 2010, the two governments signed an agreement with governor Juan Sabines Guerrero laying the foundations for REDD's introduction in Chiapas.
ECOSUR (El Colegio de la Fontera Sur) collaborates in the implementation of REDD+ projects to open the path in the Lacandon Jungle called—not accidentally—"Early Actions." In particular, ECOSUR promotes productive reconversion projects under the framework of the Mesoamerican Biological Corridor Initiative. The objective of the Corridor, according to its supporters, is to connect protected nature areas in the Mesoamerican region, conserving biodiversity and promoting eco-tourist projects or the cultivation of monocrops like fruits or palm oil. According to others, the true objective of productive reconversion is to prepare communities for the introduction of REDD.
In the Montes Azules Biosphere Reserve, which is part of the Lacandon Jungle, institutions like CONAFOR [Comisión Nacional Forestal, or National Forestry Commission] and Proárbol are working on the introduction of REDD through Payments for Environmental Services (PSA), whose stated goal is the same as REDD: reducing deforestation and poverty.
What's more, governor Juan Sabines Guerrero is already paying 2,000 pesos monthly to certain indigenous Lacandon families to preserve the area. "We can't allow human settlements within the Reserve's interior", Sabines declared. It is true that the colonization of the Lacandon Jungle has precipitated an environmental disaster: to make room for houses, crops, and husbandry, settlers have cut down a large number of trees. But isn't it the logging firms that are primarily responsible for deforestation in the jungle?
To understand what is happening in the Lacandon and the political use to which REDD is being put by the governor of Chiapas, it is necessary first to open up a small historical parenthesis. In 1972, the federal government handed 614,321 hectares of jungle over to 66 indigenous Lacandonans (though this is not their true name, and they are not original settlers of this region), threatening thirty-seven communities from other indigenous nations (Chol and Tztetzal) though they had settled, sometimes legally, on this land. The Lacandonans, in turn, signed an agreement in which they promised the company Cofolasa 35,000 cubic meters of mahogany and cedar a year at below market value for 10 years.
Lacandon child photographed by Gertrude Duby Blom in 1959.
The titling law, known as the Decree of the Lacandon Community, was the first step (and REDD is the last) in the opening of the "Lacandon gap"—that is to say, the bid to physically delimit the territory belonging to the Lacandonans, who continue cooperating with the government's policies (thereby leaving those who do choose not to do so by the wayside). One of the next steps in the opening up of the gap was the creation, in 1978, of the Montes Azules Biosphere Reserve: these 'protected natural areas' are policies meant to strip indigenous communities of their rights to their land. Inside the Reserve there is a "restricted-use zone", where human settlement has been banned and the families that lived in the area have been evicted and forcefully relocated. At times this was carried out with the cooperation of paramilitary operatives, as occurred in 2006 in the Viejo Velasco community. The next year, the communities of El Buen Samaritano and San Samuel were occupied by the army and disbanded.
A documentary about the Zapatista's struggle in the Chiapas region of southern Mexico – a reminder that large-scale multi-national development schemes can have significant impacts on indigenous subsistence and abuses can lead to insurrection.
In the documentary "REDD: Lust for Trees", Francisco Alfonso de Amador Hernández claims that, out of fear, many communities have begun to negotiate transfers with the government to a Sustainable Rural City. The Sustainable Rural Cities (link) are impersonal and miserable housing areas where people relocated from different communities—belonging to different indigenous nations, not speaking the same language—live together. In this way, the government can exercise greater control over them and employ them as cheap manual labor in the cultivation of agrocombustibles.
In the pamphlet "Mexico's Vision of REDD+", the federal government stresses the importance of "respecting the rights to social property and promoting communal management of forests, both in regard to ownership and possession of a community's lands and in the benefits derived from said management. We recognise the importance of community participation in the design and implementation of the project". In reality, indigenous people have not participated in the design of REDD, and its supposed benefits are not distributed equally among communities. Often, they are not distributed equally even within the same community: for example, in Frontera Corozal, which has 1,100 residents, the agreement was signed with the consent of only 60 community members. Thus, REDD, and the projects that are setting the ground for its introduction, do nothing more than sharpen the tensions already present in the Lacandon | eng | ce135ed7-1c21-4b09-9715-cc5acb01d099 | https://wilderutopia.com/international/earth/chiapas-corporate-polluters-lust-for-trees/ |
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Special Activities
Free Monthly STEAM Club for kids in Golden!
Department / Organization: Fairmount steamHouse
Check out the URL to join! June's Event: "Seesaw with a heehaw," "Gallop with a goat," and "Snuggle with a snake!"
Fairmount steamHouse is a monthly STEAM club for kids. They hold a different event each month, and the June event looks especially exciting for kids. Given the interest Mines faculty have in STEM, this Golden-based group might be of interest!
Here's their June event:
Aurelia our amelanistic Burmese Python turns 10! We'll check to see if she's really 13' and 90 lbs! Help us celebrate by earning a shirt to say you've see sawed with the hee haw, galloped with a goat and snuggled with a snake!
Brenton will give five minute framing on relationship of snakes, reptiles, mammals, amphibians and fish. Clem will help welcome Aurelia's fellow chronospatial navigators and steamHouse-new axlotls, fish, and aquatic plants living in a scale model of the ancient Shark Park of Fairmount! | eng | 38ffeda6-7416-4f6b-b279-f2fa53781618 | https://webapps.mines.edu/DailyBlast/Home/ShowDigestItem?ID=39135 |
Following the launch of the iPad in 2010, children's digital habits changed radically. Today, chil-dren and youngsters can touch the screen and swipe away the less interesting before they can walk. Alongside the spreading of the iPad, digital online educational platforms were developed from where teaching courses easily can be accessed. With the increasing use of technologies and digital tools and the fact that children born around 2010 and onwards have a far greater digital use than ever, there has been a widespread belief that Danish youngsters are in the digital elite. Despite that many youngsters spend a lot of time on their computers or mobile phones, reality is that their digital competencies and understanding of the most basic digital skills are far from good enough to navigate critically and safely in a digitalized society according to this investiga-tion. Around 20% of young people have no knowledge of tools such as spell check and Appwriter when solving tasks in school. This prompts frustrations, a lot of time waste and the experience of a 'gap' between those who can and those who cannot among the students in this investigation. This is partly confirmed by the ICILS report. It paints a picture that Danish youngsters are among the best in relation to those countries we compare ourselves with. However, their investigation shows that about 20% of these youngsters have so bad digital competencies that they need help with a variety of basic software functions and that they need guidance in opening files and "fin-ishing routinely text – and layout editing (translated from Danish)." Furthermore, there is a risk that students in this group get tricked online, because they do not know how to navigate safely on the internet (ICILS - Bundsgaard, Bindslev, Caeli, Pettersson, & Rusmann, 2019).
In this investigation, the digital competencies of a seventh-grade class have been examined through a structured diary method and digital test. It is found that around 20% of the students in the examined class scores at the low digital competencies level. This means that from 2018, where the ICILS report was published, until today, 2022, there has not been a significant change in the digital insight of the students in this seventh-grade class. The diary investigation shows that there are challenges in the students' digital competencies but there are also other interesting findings from the students' diaries. It is interesting that the investigation points to a desire among the students to change their own digital skills. In the diaries, over half of the class students write that they want to learn how to use spell check or Txt-Analyser. Also, several of the students reflect upon how the different tools function when they are used in other programmes. For example, that Appwriter does not function properly in online documents which indicates that the students have great insight into their own digital competencies. In everyday life the experi-ence of the teachers are filled with contrasts. There is an experience that to a varied degree the majority of the students are on their way to develop great and reflexive digital competencies. However, a small portion of the students in a class are challenged in using basic tools that are intended as a help, but in practice becomes a barrier to their development. In an organizational perspective, there is a need for change in how we think of education. Not only among the teach-ers, but the investigation also calls for further change in practice. From the discussion, it is clear that there is a myth that youngsters of generation alfa have greater digital competencies than they have in practice where around 20% as mentioned have relatively great challenges. | eng | b00eca2e-9a10-405a-b982-1968f7cf2c12 | https://projekter.aau.dk/projekter/da/studentthesis/hvor-digitale-er-generation-alfa-udskolingselevers-digitale-kompetencer(f301b129-fa26-4dc6-8621-757a8becc9af).html |
"I'm not going to live in a town where a group of masked thugs gets to just wander the town, terrorizing people. I'm not going to allow that to happen. As a journalist, I'm going to tell that story," Overman told KOMO-TV News. | eng | 9cba3708-0d0d-4666-855b-7cff5b5d2ecc | https://visualjournalism.info/2011/06/13/journalism-isnt-snithcing/ |
Mendocino County has a rich history of agriculture and Ukiah High is keeping that alive by helping FFA students raise their animals on campus. Sophomore student, Autumn Walker is one of these choice students looking ahead into a future of agriculture and working with animals. Raising an animal for FFA is no easy task and Walker has many jobs with her animals that she has to do during the day. Walker is one of the few students raising goats for FFA which makes her jobs different from other students who raise pigs.
"I sweep the pens and give them (the goats) a few scoops of food" Walker described her day-to-day chores that she does to take care of her animals and it is no easy task. "Then I renew their water every day. Every Saturday I give them a bath but I groom them every morning and every night." Even with all the care that Walker gives her animals on a day-to-day basis, it can take the goats some time to get used to the daily interactions with humans which can make raising the animals even harder if they try to avoid human contact that they need. "I spend at least one to two hours a day with them and try to get them used to me," Walker says. "My male goat is still getting used to me but the female goat is very friendly."
Autumn Walker with her goat [Picture taken by Bennett Gaylord]
As Walker tries to get the goats used to her presence, she is also preparing them for auction in the summertime where they will be sold off as Market goats. "I plan on giving the goats the best time I can for as long as I have them. I will be selling them as market goats and taking the money from them to buy another goat." After auctioning the goats off and buying another, Walker will have some money left over to buy supplies to help take care of her new goat. The process repeats itself for as long as she continues to raise goats for FFA.
Even though raising the goats is a difficult task, to students like Walker, it is worth all of the work that she puts into it. With all of the ways that raising animals can help students look ahead to a bright future in agriculture, learning all of the ways to take care of the animals is extremely beneficial to students for their future careers. Getting to be around animals all the time is not only good for the future but is also good for the present moment. Even auctioning the animals off gives students a taste into business in the future and the give and take of earning your own money. "I love [raising goats] because I get to watch them grow up and become a big part of today's food production! The bond I make with the animals is so fun having." After watching Walker interact with the animals, the love that she claims for the animals was apparent in the gentle way that she cared for them and her loving tone when speaking with them.
A goat and a pig meet
For students interested in a career pathway involving agriculture, raising animals through FFA is a great way to get involved in Ukiah's agriculture community and start looking ahead into a successful future no matter what students want to do. Overall, creating the connection between humans and animals at such a young age is an amazing thing that can lead to a bright future and help give students a boost into whatever career they may want to pursue in the | eng | c21afd93-ff63-48ef-aca0-0f94b2bbefd9 | https://ukiahhighnews.com/2021/05/17/ukiah-highs-agriculture-program-animal-husbandry-and-caring-for-goats/ |
Tuesday, April 28, 2009
The Farthest Explosion
From the European Southern Observatory: Astronomers have detected the farthest object ever seen, a gamma ray explosion at a redshift of 8.2. The object exploded when the Universe was barely 600 million years old. GRB 090423 was first detected by the SWIFT spacecraft, which was designed to catch these gamma ray bursts "on the fly." Follow-on observations were made by the ESO Very Large Telescope in Paranal, Chile. ESO Press ReleaseThis GRB may be the sign of a massive Black Hole.
Separately, the Subaru telescope atop Mauna Kea has found a "blob" formed only 800 million years after the Big Bang. The object iss comparab;le in size to our Milky Way galaxy. Press Release Astronomers are baffled as to how such a large object could have formed so early. Possibly the best way to form a galaxy-size object is around a supermassive Black Hole. Giant Black Holes formed soon after the Big Bang are indicators that the speed of light has changed.
2 Comments:
Wow! 8.2 ly. I have been to a number of excellent talks about GRBs and black holes, and it is difficult to see how one could interpret these objects as something other than large black holes in the early universe | eng | dd799633-1581-4cb2-b51a-1082b86e1b26 | https://riofriospacetime.blogspot.com/2009/04/farthest-explosion.html |
Wall Builder NYT Crossword Clue
We have all of the known answers for the Wall builderWall Builder Crossword Answer
The answer to the Wall builder crossword clue is:
MASON | eng | a15a0367-fe78-4f45-80a7-21a44fd6e4a0 | https://gamerjournalist.com/wall-builder-crossword-clue/ |
We Buy All Cars, Running or Not!
Does the Condition of the Car Affect the Price I Will Receive?
As car owners, we often wonder whether the condition of our car affects the price we will receive when we sell it. The truth is, the condition of the car plays a significant role in determining its value. In this article, we will dive deep into the different factors that affect the price of a car and how its condition impacts its value.
Auto Repairs Are EXPENSIVE
When it comes to selling a car, its condition is a critical factor that determines its worth. Cars that are well-maintained and in excellent condition are likely to fetch a higher price compared to cars that are in poor condition. In fact, the condition of a car is one of the primary factors that dealers and buyers consider when determining its value.
Age of the Car:
The age of the car is a critical factor that affects its value. Generally, the older the car, the lower its value. This is because older cars tend to have more wear and tear and may require expensive repairs.
Mileage:
The mileage of the car is another important factor that affects its value. The higher the mileage, the lower the value of the car. This is because high mileage cars are more prone to mechanical issues and may require costly repairs.
Exterior Condition:
The exterior condition of the car plays a significant role in determining its value. Cars that are in excellent condition, with no dents or scratches, are likely to fetch a higher price compared to cars that have visible signs of damage.
Interior Condition:
The interior condition of the car is another factor that impacts its value. Cars that have clean and well-maintained interiors, with no tears or stains, are likely to sell for a higher price compared to cars that have a worn-out or dirty interior.
Mechanical Condition:
The mechanical condition of the car is perhaps the most critical factor that affects its value. Cars that have been well-maintained and are in excellent mechanical condition are likely to fetch a higher price compared to cars that have significant mechanical issues.
Service History:
The service history of the car is also an important factor that impacts its value. Cars that have a complete and detailed service history, showing that they have been regularly maintained, are likely to sell for a higher price compared to cars with incomplete or no service history.
Market Demand:
The market demand for a particular type of car is also an essential factor that determines its value. Cars that are in high demand are likely to sell for a higher price compared to cars that are not in demand.
Brand and Model:
The brand and model of the car also play a crucial role in determining its value. Some car brands and models have a better resale value compared to others.
Location:
The location where the car is being sold can also impact its value. In some areas, certain types of cars are in high demand and may sell for a higher price compared to other regions.
Negotiation:
Finally, the negotiation skills of the buyer and seller can also impact the final price of the car. A skilled negotiator can influence the final price of the car.
FAQs:
Q1. How can I increase the value of my car?
A: To increase the value of your car, you should maintain it well and keep it in excellent condition. Regular servicing, fixing minor issues, and keeping it clean can help improve its value.
Q2. Should I repair my car before selling it?
A: Yes, repairing your car before selling it can help increase its value. Minor repairs such as fixing dents, scratches, and replacing worn-out parts can help improve its resale value.
Q3. Can I sell my car without a service history?
A: Yes, you can sell your car without a service history, but it may significantly affect its value. Cars that have a detailed and complete service history are more likely to sell for a higher price compared to cars without a service history.
Q4. Is the color of the car important in determining its value?
A: The color of the car can play a small role in determining its value, but it is not a significant factor. Generally, popular car colors such as black, white, and silver have a better resale value compared to less popular colors.
Q5. How can I find the true value of my car?
A: There are many online tools and resources available that can help you find the true value of your car. Websites such as Kelley Blue Book and Edmunds can provide an estimate of your car's value based on its make, model, year, and condition.
Conclusion:
your particular type of car. This will help you set a fair price that is in line with the current market value. When negotiating the sale of your car, it is essential to be prepared and know the value of your car. This will help you make informed decisions and get the best possible price for your car.
Finally, if you are in the market to purchase a car, understanding the factors that impact the value of a car can help you make an informed decision. By considering the age, mileage, exterior and interior condition, mechanical condition, service history, market demand, brand and model, location, and negotiation skills, you can make a wise investment and purchase a car that will retain its value over time.
In conclusion, the condition of a car plays a critical role in determining its value. Whether you are selling or buying a car, understanding the different factors that impact its value can help you make informed decisions and get the best possible price. By maintaining your car well, providing a detailed service history, and being aware of the market demand, you can ensure that your car retains its value and is a wise investment. | eng | fb451fed-606e-46af-bbf2-fee93edf8771 | https://www.cashcarsbuyer.com/does-the-condition-of-the-car-affect-the-price-i-will-receive/ |
Dirty Dozen List | eng | f9216a4f-eddf-4ce2-94ec-b5500b87d3c8 | https://taxmethodexperts.com/tag/dirty-dozen-list/ |
Map of Regional Languages in Indonesia, Which Province Has the Most?
goodmorningpapua.com – Indonesia has 718 regional languages spread throughout Indonesia. The data is based on a study from the Ministry of Education and Culture which has been validated in 2,560 observation areas from 1991 to 2019. Based on its area, Papua is the province with the most regional languages in Indonesia.
There are 326 regional languages spoken on Earth of Cenderawasih. One of the regional languages in Papua is the Aabinomin language. The Aabinomin language is the language spoken by the Aabinomin tribe in Baso Village, Mamberamo Hulu District, Mamberamo Raya Regency, Papua. West Papua follows in second place with 102 regional languages. Several regional languages exist in West Papua, including Bantanta, Esaro, and Kalabra. After that there is East Nusa Tenggara which has 72 regional languages.
Then, there are 23 regional languages used in Maluku. Meanwhile, the Riau Islands and Yogyakarta are the provinces with the fewest regional languages in Indonesia. Only one regional language is spoken in the two provinces. Javanese is the only regional language spoken in Yogyakarta. Meanwhile, Malay is the only regional language used in the Riau Archipelago. West Java, Central Java, and the Bangka Belitung Islands are also among the provinces with the fewest regional languages in Indonesia. The three provinces only use two regional languages in each region.
Meanwhile, there are several regional languages that are used across provinces. One of them is the Bajo language which is used in East Nusa Tenggara and West Nusa Tenggara. Banjar language is also used in Riau, Jambi, Central Kalimantan, and South Kalimantan. | eng | 78988464-b80c-42ab-a89c-ff8d5c1398aa | https://www.goodmorningpapua.com/map-of-regional-languages-in-indonesia-which-province-has-the-most/ |
You are not forgotten bear shirt is made of cool, soft, non-fading fabric, less dust, less wrinkles. The shirt has a beautiful shape, delicate colors, eye-catching prints, promising to be very hot this year. You can find You are not forgotten bear shirt at lelemoon.com at affordable price. | eng | b47a71ec-ba34-4ebf-8aa0-7ac50f4832d6 | https://www.lelemoon.com/product/you-are-not-forgotten-bear-shirt/ |
people's garden initiative
Over the past three years, USDA has welcomed seventh-graders from Alice Deal Middle School in Washington, D.C. to participate in "Deal Gives Back," a day of service that empowers students to serve their community. This year was no exception. Alongside local volunteers, 118 students and faculty spent a day at USDA's People's Garden planting, weeding, and tilling soil to better understand how community gardens can increase access to fresh, healthy food choices in communities where nutritious options aren't easily accessible.
All work and no play? Not a chance. After a warm welcome from USDA Assistant Secretary for Administration Dr. Gregory Parham, the students checked out demonstrations from the Agricultural Research Services' (ARS) Bee Research and Systematic Etymology Labs to learn about insect classification, research, and the vital role pollinators play in growing healthy fruits and vegetables. And to wrap up the day, National Institute of Food and Agriculture (NIFA) Director Dr. Sonny Ramaswamy stopped by with a surprise treat – an invitation to try toasted mealworms. Yum!
Torey Powell, USDA Center for Faith Based and Neighborhood Partnerships
Posted in
Initiatives
It's "Back-to-School Night" at the USDA Farmers Market on Friday, September 18, from 5 p.m. to 8 p.m., in Washington, D.C., near the National Mall. This month's educational exhibitors and vendors will appeal to students of any age. Market visitors can learn more about healthy eating, reducing food waste or take a trip down memory lane and eat a snack or meal off a planet-friendly disposable lunch tray!
Members of USDA's Team Nutrition will be at the market to explain how to eat healthy in and out of school. Executive Chef Adam Tanner, from the Mandarin Oriental Washington, DC, will show you how to cook delicious and nutritious snacks.
Nothing says springtime more than the sprouts and shoots of a garden. Secretary Vilsack has declared April, 2015 as National Garden Month. The official proclamation celebrates the great American tradition of gardening at home, at school and in the community.
USDA's commitment to gardening has deep roots. The USDA People's Garden Initiative, was launched in 2009 and since 2,116 gardens have registered as People's Gardens in communities across the United States and its territories and in 12 foreign countries. The First Lady's Let's Move! Initiative has great information about starting a kitchen, school or community garden and the Plant Hardiness Zone Map, developed by USDA's Agricultural Research Service, is a go-to guide for gardeners across the nation. Have a gardening question? Visit eXtension for in-depth and research-based gardening and landscape advice from your local land grant university.
This article was originally posted on ServiceNation.org. Read the original here.
As Secretary of Agriculture, I take USDA's nickname of the "People's Department"—first coined by President Abraham Lincoln—to heart. Over the past five years, we have worked hard to build upon our tradition of service to the American people, supporting both the farmers and ranchers who grow our food and giving American families confidence that the food they buy at the grocery store is safe, healthy and affordable.
We could not accomplish our mission without the contributions of partner organizations and individual volunteers across the country. While our work with volunteers is by no means exclusive to nutrition and nutrition education, volunteers act as our boots on the ground in classrooms and communities to teach kids about where food comes from and why the diet and lifestyle choices they make today matter for their future. Volunteers, along with parents, teachers, school administrators, and school food service professionals, are absolutely critical to our efforts to improve childhood nutrition and help this generation of youngsters grow up healthy and strong.
It's National Volunteer Week and an ideal time to share how USDA employees and partners are volunteering their time to green communities and provide fresh food to those in need.
It all started in 2009 when Agriculture Secretary Vilsack established a Department-wide volunteer program for the People's Garden Initiative. He encouraged every USDA employee to get involved by volunteering time and expertise to create a People's Garden - a challenge he then extended to all Americans.
Employees of USDA's Natural Resources Conservation Service (NRCS) work every day to help private landowners improve environmental quality on their properties. So when staff at the NRCS East Remote Sensing Lab (ERSL) in Greensboro, N.C. noticed a stream near their building had become a dumping ground, they took it upon themselves to address the problem.
Let's get together to enjoy the fruits of our labor! USDA's People's Garden is sponsoring a Harvest Festival on Friday, October 28 from 10 am to 2 pm at USDA Farmers Market, on the northeast lawn of Jamie L. Whitten Building and along 12th Street in-between Jefferson Drive and Independence Avenue, SW. The festival marks the culmination of a very productive growing season for the People's Garden at USDA Headquarters. | eng | 0f6d87b1-50cd-4658-9dc0-6f5f63268a53 | https://www.usda.gov/media/blog/archive/tag/people%27s-garden-initiative |
sweets nakaya – Enjoy Their Flavorful Apple Pie
Shop famous for its apple pies, located in Sunagawa City. The crust is made with cultured butter, with a crisp, flaky texture, and a delicious buttery aroma. The inside is filled with apples, with all of their texture and flavor. They also sell a variety of other snacks/confections, all made with thoughtfully considered ingredients. | eng | e900c6b8-a595-47c2-a44d-f3a7ba73f9fe | https://en.visit-hokkaido.jp/destinations/sweets-nakaya-enjoy-their-flavorful-apple-pie |
Warm Up to Throw, Don't Throw to Warm Up
You show me a fielder who has never had a sore arm or shoulder from throwing and I will assume they "choose" to field at slip, irrespective of the state of the game!
For the rest of us, one thing that helps is learning how to warm up, condition and strengthen your shoulder and arm ahead of pinging the ball in matches or practice.
A few token arm swings just doesn't cut it!
Before we get into that, remember there are many causes of throwing related shoulder and arm pain. It's always worth a technical check. See here and the PitchVision fielding courses such as "First Class Fielding". This will help iron our any technical glitches.
Warming up to throw
Most people think that a few low intensity throws to a mit is the way to prepare the arm for 100% efforts just a few minutes later. This doesn't do the job.
You don't need a heap of kit to warm up and strengthen the vulnerable shoulder and arm either.
My throwing kit bag is this,
A piece of theraband tubing. The baseball versions are called J-Bands.
1KG med ball.
Variety of sand filled balls.
The great thing about the J-bands is that you can have them posted just outside the boundary line in a few key positions around the field. Your deep fielders can keep their arms loose and moving at breaks in game time. We attach them to the 3rd man and fine leg boundary fences on Millfield's main ground.
Here is Millfield and Somerset Cricketer, Tom Diamond doing some of the exercises from the J-band manual.
These are great exercises to do the following things:
Oxygenates and warms the shoulder.
Provides a deeper, more isolated workout for the rotator cuff muscles. The rotator cuff is a group of muscles and their tendons that act to stabilize the shoulder. This is also the part of the shoulder that is most likely to break down.
Strengthens the shoulder from "inside out".
Optimises elasticity, flexibility and range of motion.
Provides rotator cuff muscle balance, strength and endurance.
Fast tracks the recovery period in between performances.
Keep the movements controlled and smooth ensuring that the larger muscles groups including the trapezius are neutral and switched off.
It is easy for the larger muscle groups to take over. If you feel this happening then reduce the tension in the band by moving slightly towards the pivot point.
If time is an issue and you need a speedier warm up then run through this shortened version:
Reverse flys
Flys
Internal rotation
External rotation
Elevated internal rotation
Elevated external rotation
Within a few sessions, you will feel that the shoulder feels more stable, that your internal and external range of movement has increased (which facilitates increased ball velocity) and that you reduce the stress on your shoulder when you move from warm up to throwing in anger | eng | fe847f97-1766-4f36-b625-25e8c9ec461e | https://www.pitchvision.com/throwing-warmup |
Finding a Korean language Dating Place
If you're foreign people, and youre thinking about online dating a Korean language woman, you should know a few stuff. It's not easy, but it can be a lot of entertaining.
The most important matter to remember is usually you must make sure you are compatible. Whether you are looking for a romance korean girl personality or simply a date, you should attempt to find somebody who is a good fit for your character.
In terms of online dating, there are countless options. Many are more targeted and cater to specific ethnic demographics, although some are more general.
Another great destination to meet true romance in Korea is through friends. This can be a relatively secure way to meet up with people, in fact it is often easier than accidental encounters in the street.
Blind goes are also common in Korea, especially if you're buying a serious romantic relationship. This is usually performed through a friend, therefore it's not as well risky, but you should still be aware of their very own background the moment conference someone new.
You can also continue sogaeting, which is a group window blind date, often used by students. It's a smart way to meet other Koreans and it can be extremely fun!
Another popular location to meet Koreans is at a fitness center. Many Koreans prefer to workout in communities, so becoming a member of a fitness school could be the simplest way for you to meet up with potential complements. | eng | c2db1c4f-bb67-4451-aeed-c424525f56a6 | https://www.immocasapiu.com/finding-a-korean-language-dating-place/ |
A Healthier You
Updated: May 27, 2022
Everyone loses weight in different ways but there are basic sciences that help us become closer to our goals. For example there are studies done on blood types that tell you what foods to eat more of and what foods to stay away from. Think of yourself as part of the earth and listen to you body and what it needs. I remember gaining weight, it was so fast I didn't even realize it was happening. I had just started a new career that was looking upward and the extra money I was using it to eat. I love trying new things and eating and sitting definitely packed on the pounds. So I had to do what had to be done.
PORTION CONTROLI'm telling you portion control works. Diets are already difficult because you are having to stop eating what you like. The idea is just eat what you want just smaller portions. Say you have a burger, just eat half of it and save the rest for later. What it does is shrinks your stomach, eventually you will not even be able to stomach as much food as before. When this happens this ignites endorphins that make you more aware of the foods that you are putting in your body. It becomes exciting to see your efforts actually make a change.
Plus I started only ordering meals that would be good heating up later being that I was only eating small portions. Which inadvertently caused me to immediately eliminate fast foods. Because who wants cold McDonalds fries, because I don't. Instead I would order the 3 for $10 at chilies or authentic style grilled chicken tacos from one of my favorite Mexicans restaurants if I wanted to eat out.
WATER
I know I know. This is the obvious but hear me out. Water works wonders on you skin, it also helps with flexibility & it helps eliminate the consumption of empty calories. If you want to see a new you, Water has to be your best friend.
EXERCISE
Working out is different for everyone. I personally love to dance and lift weights, so that's what I do. Dancing is something you can do at home, you can learn dance videos on youtube and just learning the video itself is a workout. Stay tunned to our News page for updates on upcoming TWERK fitness classes in a city near you. Click here to see the Goodies Music Video filmed at the Twerkalations Twerk Class! | eng | d4eb2db9-252d-40ea-ae04-d53c69508415 | https://www.kenisetaylor.com/post/new-indie-bands-climbing-the-chart |
Abstract
Alternative splicing of messenger RNA can generate an array of mature transcripts, but it is not clear how many go on to produce functionally relevant protein isoforms. There is only limited evidence for alternative proteins in proteomics analyses and data from population genetic variation studies indicate that most alternative exons are evolving neutrally. Determining which transcripts produce biologically important isoforms is key to understanding isoform function and to interpreting the real impact of somatic mutations and germline variations. Here we have developed a method, TRIFID, to classify the functional importance of splice isoforms. TRIFID was trained on isoforms detected in large-scale proteomics analyses and distinguishes these biologically important splice isoforms with high confidence. Isoforms predicted as functionally important by the algorithm had measurable cross species conservation and significantly fewer broken functional domains. Additionally, exons that code for these functionally important protein isoforms are under purifying selection, while exons from low scoring transcripts largely appear to be evolving neutrally. TRIFID has been developed for the human genome, but it could in principle be applied to other well-annotated species. We believe that this method will generate valuable insights into the cellular importance of alternative splicing. | eng | c660a1e4-fad5-4b0a-a8d8-c64285fbd7be | https://pubmed.ncbi.nlm.nih.gov/34046593/ |
How To Pronounce "U" In French
Pronouncing sounds that are uncommon in your background language is a unique struggle in the general challenge of learning French pronunciation. If you've ever had trouble with the French "u", be sure to try these four practical tips to help you master it for good.
Let's be honest, French can be a very difficult language to master. To be fluent in French, you need to: memorize countless verb conjugations, remember thousands of vocabulary words, and understand complex grammar rules… the list goes on. To further complicate things, French has about 10 different vowel sounds, along with an additional four nasal vowels (depending on the dialect and/or idiolect). Many people learning French find it hard to pronounce all of these vowels correctly, seeing as some of these vowels do not exist in other languages.
One vowel sound that is often difficult for non-native speakers to pronounce is the French u. This sound can be found in a wide variety of words such as tu, cru, du, and many more. In this short article, I am going to outline four simple steps to pronounce the u sound like a native speaker. The four steps are:
Dis-associate u From ou
Say "Cheese!"
Round Your Lips
Practice u In Different Words
Step 1: Disassociate u From ou
Many people who are studying French believe that the u found in words like tu or du, is similar to the ou sound found in words such as tous or doux. This could not be further from the truth, and it's the most common mistake made by beginners. It's crucial that you disassociate these two sounds before you even start trying to pronounce the French u. Otherwise, you will end up pronouncing words incorrectly. This, in turn, will cause you to have an accent and even potentially be misunderstood when speaking French.
Step 2: Say "Cheese!"
With my students who struggle to pronounce the u sound, I'll often have them pronounce the word "cheese" as a starting point. This is because the first step to being able to pronounce u is to be able to say the ee sound in the word "cheese". Notice how when you say ee, the tip of your tongue is touching the inside of your bottom two teeth in your mouth. This is going to be an important part for step three, so keep that in mind. If you do not maintain that tongue position, you'll find that it is virtually impossible to pronounce a French u.
Step 3: Round Your Lips
This is where things get a little bit trickier, so kindly pay attention. As you are saying the ee sound in "cheese"? Now round your lips. It's almost as if you are saying "cheese" while trying to give someone a kiss. Focus on keeping your tongue in the exact same position as when you pronounced ee in the word "cheese". If you don't, you will end up pronouncing the ou sound in French instead of u.
This can take a lot of practice to perfect, so don't get discouraged if you're not able to pronounce it perfectly the first time. Just keep working at it. For some people, it can sometimes take hours of practice before being able to say the sound properly.
Step 4: Practice u In Different French Words
Once you're able to comfortably say u, it's time to practice this in different words. Usually, it is best to start by practicing with the word tu. Initially, start by saying tee, then slowly round your lips as you did in step three so that you're saying tu. Once you've done that a few times, shorten the length of time that you are saying tee, and increase the speed at which the tee turns into tu.
Repeat this process for any word with the u sound that you are struggling with. For instance, if you're struggling with the word du, start off by saying dee and then round your lips to say du.
Once you've gotten the hang of pronouncing the French u, here is a progression of words to master the u sound in different words. The list starts with some simple words or phrases and finishes with some difficult ones:
Tu
Du
Lu
Fallu
Attendu
Cru
J'ai vu un ours
Je veux que tu fasses tes devoirs
As-tu vu le tutu de tulle de Lili d'Honolulu?
We've now gone through the four steps to pronounce the u sound in French. To summarize, in order to successfully pronounce u, you need to say ee (like in the English word "cheese") and round your lips. Once you're able to do this comfortably, test yourself by saying simple French words that have the u sound such as tu or du.
Be mindful to keep your tongue pressed against your bottom two front teeth as you are practicing. Otherwise, you will end up saying ou (as in the words tous or doux). Although it may seem hard at first, don't give up! With time and practice, being able to pronounce this vowel sound will become second nature to you. | eng | 64677a38-0d11-457d-9583-11dd013c0341 | https://www.italki.com/en/article/887/how-to-pronounce-%E2%80%9Cu%E2%80%9D-in-french |
Every restaurant owner fears the odious Yelp reviewer. Heck, there's even an entire South Park episode making fun of amateur food critic culture. As annoying as the wannabe Trip Advisor and Yelpers can be, they play an important role is your restaurant's online presence. Answering reviews actually helps improve your Google Business Profilerankings. Responding to a bad review can quell a negative situation. Conversely, answering a great review can mean more return business. SpotOn POS can help you manage and answer reviews to leave no customer unanswered. Today, let's break down why answering customer reviews is vital for your restaurant's business.
Answering Reviews Improves SERP
The first major area that answering reviews helps is on Google. Google users can leave reviews on your Google Business Profile, or GBP. Your GBP is one of the most important parts of your restaurant's online presence. Everybody, including yourself, has likely judged a restaurant based on a GBP.
What you may not know is that the GBP isn't just a place to load pictures, check opening times, and leave a review. Believe it or not, a GBP's review section is very important when it comes to SERP. SERP, or search engine ranking position, is where your website ranks in Google searches. Having a higher SERP means more customers will find your business compared to competition.
Answering reviews on your GBP rewards your SERP. Why? Google rewards uses who actively use their GBP. When you answer every single customer review, you are actively using the profile. It also shows that you are having real interaction with customers. Over time, GBP users' profiles will go up as a result of answering Google reviews. That means, for example, a pizza restaurant with an equal number of reviews as another pizza restaurant will rank higher if they answer each review on their GBP.
Better Reviews Means Better Local SEO
Reviews are also important for your local SEO. Local SEO, or search engine optimization, is how your business' presence is formatted online to attract local business. This feature is a keystone for local businesses, especially restaurants, in order to rank above their competition.
Let's use an example as to why answering reviews is important for local SEO. As we've discussed, simply answering reviews helps improve your GBP rankings. Prompting more customers to leave more reviews will slowly help your local SEO over time. Why? If you are a pizzeria with 1,000+ positive reviews, a customer is more likely to choose you over a restaurant with 100 positive reviews. This can result in more business, bringing in more customers, and, thus, leaving more reviews.
Customers that review restaurants on Yelp and Trip Advisor can play a critical role in local SEO. Both platforms allow restaurants to be flagged as 'Best Pizzeria Philadelphia' or a different combination of terms. These longer forms of terms can create what we callongtail keywords Try typing 'pizza' into your search engine. You may get a bunch of results. Now type in 'Best Pizza in Doylestown PA' and the search will drastically narrow to local business in that direct area. This longer form of a keyword is better and more niche than a short keyword. More longtail keyterms like this are better for local SEO. Answering these reviews can help your profile, regardless of if they are positive or not.
Leaving Bad Reviews Unanswered is a Bad Idea
What if a customer does leave a bad review? "The food was horrible". "The service SUCKED." "My dog could cook something better with both of its eyes closed." Surely, your restaurant has had to handle bad customer reviews online. A bad review on Yelp, Facebook or other platforms can deter customers. Occasionally, you may have the gall to answer one of these reviews in a snarky manner. Yes, that may feel great, but it's a bad idea.
Customers are actually turned off when a restaurant owner answers a bad review with an equally sarcastic and bad review. It's usually seen as pompous and doesn't resolve the situation. What if a future customer has legitimate feedback? Are they going to be expecting to be bullied or listened to? The answer should be the latter. Restaurant owners should refrain from answering negatively. Respond in a positive manner that shows professionalism and that you are above the fray.
Furthermore, bad reviews need to be answered! Why? First, let's recap. Every review needs to be answered, especially on your GBP, in order to improve SERP and local SEO. Second, when bad reviews aren't answered, they stay there and can leave a lasting impression. Responding to a negative review in a professional way shows that you are focused on understanding the customer. The conversation thread in the review can lead to a positive outcome if it is navigated correctly.
Responding to Great Reviews Improves Customer Service
To build off of why to never leave a bad review unanswered, let's consider why it's important to respond to great reviews. Customers that take time to leave a positive review on your GBP, Yelp or any other platform because of a phenomenal experience. A restaurant can simply look at these reviews and say, "we did our job, time to move on." That mentality is wrong!
Again, restaurants need to answer every review. Responding to great reviews makes the customer feel even better and heard following their experience. When responding to a great review, prompt the customer with responses like, "Thank you for your review! We can't wait to serve you again." Small responses like these can leave a big impression on a customer and convert them into return business.
SpotOn Reviews Makes Managing Review Platforms Easier
Managing all of these reviews can be difficult. A great way to respond to all of them is in SpotOn's back officereview management software. Sync your profiles like Google, Facebook, and Trip Advisor into SpotOn software. Track review averages, total reviews written, and answer reviews in real time. It's all included with SpotOn's monthly subscription software. This can improve your SERP, local SEO, resolve bad review scenarios, and reward great reviewers with positive responses. Want to improve your online ratings with SpotOn? Contactus for a free consultation to get started today! | eng | cd4a4c7d-3124-4d51-b5e7-6fb2b3fde1dd | https://posphilly.com/4-reasons-answering-online-reviews-is-vital-for-restaurants/ |
How Sioux Falls launched South Dakota into the Space Age: Looking Back
Eric Renshaw
For the Argus Leader
In the mid 1960s, Sioux Falls entered the Atomic Age when NSP built its Pathfinder Nuclear Generating Station northeast of town.
For a short time, the area had the atomic feather in its cap, and the chamber of commerce wasn't shy about sharing that fact. A short time later, when South Dakota Sen. Karl Mundt, and local leaders like Al Schock, saw an opportunity for the state to enter the Space Age, they did not hesitate to make it so. The EROS Data Center was the fruit of this effort.
On Sept. 20, 1966, Secretary of the Interior Stewart L. Udall announced Project EROS. EROS is an acronym for Earth Resources Observation Satellites. Using dedicated satellites, EROS would be able to collect data about this big blue marble we call home. This research would revolutionize our understanding of our planet, natural resources, and weather.
Once launched, EROS satellites would need a staff to collect, store, and analyze the data received. It was determined that a location in the central United States would enable the data collected by the satellites to be more easily received. This data center would need to have a modern airport nearby and have an unobstructed view of the sky. Mundt, at the time a member of the Senate Appropriations Committee, saw an opportunity for his state, and didn't hesitate to tout the Sioux Falls area as a perfect location. The city had Joe Foss Field, a well-established airport, capable of receiving jet aircraft. The area also had a pretty clear view of the sky.
By 1967, design had begun on ERTS-A, the first Earth Resources Technology Satellite. In 1970, General Electric's space division in Valley Forge, Pennsylvania began construction. This satellite would later be renamed Landsat-1, or LS1.
In March of 1970, the Sioux Falls area was chosen as the general location for the EROS Data Center. Six sites in the area were under consideration. Two were near Parker, one was near Dell Rapids, and the remainder were situated near Garretson. After careful analysis and surveying of the sites, a spot six miles west of Garretson and 12 miles north of Sioux Falls was chosen. Up to that point, the Rudy Froseth farm had occupied a quarter of the location, while Alfred Hegge owned the other quarter.
On Jan. 2, 1972, EROS personnel moved into temporary offices at 132 S. Dakota Avenue. Offices were needed in the area to oversee the development of the data center. The groundbreaking ceremony for the building was on April 14, 1972. The ground was broken in an unconventional, but apropos way – with a walking plow pulled by mules named Jenny and Maude. Officials took turns guiding the plow. These included Gov. Richard Kneip, North Dakota Sen. Milton Young, Undersecretary of the Interior William Pecora, and others.
ERTS-A was put into orbit on July 23, 1972. Upon achieving orbit, it circled the globe once every 103 minutes, 14 orbits per day. It was equipped with two camera systems, the Return Beam Vidicon, and a Multispectral Scanner. The latter ended up providing superior imaging – and though it had been added as an experiment, it went on to become the primary camera. The data from ERTS-A was analyzed at the interim facility on Dakota Avenue until the EROS Data Center was completed in 1973.
On Nov. 10, 1972, following congressional approval, President Richard Nixon declared the building to house EROS the Karl E. Mundt Federal Building. The building was dedicated the following August, and staff from the interim office began moving in. On hand for the dedication were EROS officials and Secretary of the Interior Rogers Morton. The space age had finally fully arrived in the Sioux Falls area.
This era —the late 1960s and early 1970s — was a time of great optimism for young people with their eyes focused on the skies. The first episode of Star Trek aired in the United States just 12 days before Secretary Udall's announcement of the EROS program. It began to seem as though casual space flight for most citizens might actually be on the horizon. It may yet happen. EROS was a big step into a wider world in which we could gather images of our planet and discover how to better care for it.
Over the years, EROS has continued to grow and analyze more information from more and more improved satellites. In September, EROS will celebrate 50 years. Here's hoping that, over the next 50 years, EROS will continue its mission to contribute to the understanding of a changing Earth.
Correction: A previous version of this story incorrectly stated who owned land chosen for the EROS site. The story has been updated to reflect this change. | eng | 5623132b-c727-46f5-afd0-780ad1e81863 | https://www.argusleader.com/story/opinion/voices/2023/04/23/how-sioux-falls-launched-south-dakota-into-the-space-age-looking-back/70130103007/ |
Professional Watermelon Farmer
I wanna start a church sometime so I can pass that collection plate around, and then, spend it on booze, comic books and butt-plugs, and whatever else I want. I tried other way of makin' a living, maybe I need to give this one a go.
New Member
Nemnth Ferheart Dragon
I was raised going to church as a kid. It was fun, kinda, until I slowly started realizing how what they taught, which is in my opinion, was a bunch of shit. This was through personal experimentation, all the chaos in the world, nothing being answered, etc. Anything that happens in world that is good, to call it a miracle belittles the actual process of what happened.
I was told when I was younger that god had something for me in my destiny, given I only had a 5% chance to live from a C-section. To say that means the Doctor has nothing to do with saving my life at all. It wasn't god that saved me, it was the professionals that saved me. | eng | 5a174b11-9cc6-42e1-b12f-f6907783ef8f | https://forums.furaffinity.net/threads/your-opinion-on-churches.1528724/page-4#post-5510591 |
How Singapore Approaches Their Food Waste Recycling
Food waste is one of the key areas of focus for Singapore's waste reduction efforts. According to the National Environment Agency (NEA), food waste accounts for about 10% of the total waste generated in the country. Singapore has implemented several initiatives to promote food waste recycling to address this issue.
1. Food Waste Segregation At Source
One of the most notable initiatives is the implementation of mandatory food waste segregation at source. This means that households, commercial and industrial premises, and institutions must separate their food waste from other types of waste before disposal. The separated food waste is then collected and sent to a dedicated treatment facility.
2. Food Waste Recycling Programme (FWRP)
Singapore has also launched several food waste recycling programs to encourage individuals and organizations to recycle their waste. One such program is the Food Waste Recycling Programme (FWRP), which provides households and commercial premises with food waste recycling bins and composting machines.
The FWRP aims to reduce the amount of food waste sent to landfills by diverting it to composting facilities, where it can be turned into nutrient-rich compost for landscaping and agricultural purposes.
3. Food Waste Reduction And Recycling Fund (FWR2)
Another program is the Food Waste Reduction and Recycling Fund (FWR2), which supports companies and organizations implementing food waste reduction and recycling projects. The fund encourages innovation and collaboration in food waste recycling and has supported several successful projects.
In addition to these initiatives, Singapore has also launched public awareness campaigns to educate individuals and organizations on the importance of food waste reduction and recycling. These campaigns include workshops, exhibitions, and other events to raise awareness and encourage action. As a result of these efforts, Singapore has made significant progress toward achieving zero waste.
According to the NEA, the overall recycling rate in Singapore reached 63% in 2019, up from just 42% in 2000. In addition, the amount of food waste generated per capita has decreased from 140 kg in 2011 to 101 kg in 2020. However, there is still much work to be done. Despite the progress made, food waste remains a significant challenge in Singapore. According to the NEA, only about 17% of food waste was recycled in 2019. To address this issue, the government has set a target of recycling 30% of all food waste by 2030.
However, continued efforts and innovation will be necessary to achieve the country's ambitious waste reduction targets and ensure a sustainable future for future generations. Check out how significant food waste recycling Singapore has achieved through the help of banking institutions like DBS. DBS kickstarted its bank-wide Zero Food Waste (ZFW) initiative in 2020. | eng | f99c62d3-e68f-4219-bfed-9eae475464ba | https://zumboly.com/lifestyle/food-waste-recycling/ |
What impressed you negatively?
What did you wish you had known ahead of time?
What are your general comments?
"It was a great dat overall. One of my interviewers was "non-traditional" but one of the woman in admissions warned me beforehand. That helped de-stress me a bit when I actually met him0-1 hour
What was your primary mode of travel?
Train or subway01/05/12
How do you rank this school among other schools to which you've applied?
9 out of 10
What is your ranking of this school's location?
2 out of 10
What is your ranking of this area's cultural life?
9 out of 10
How is the responsiveness of the admissions office?
6 out of 10
How is the friendliness of the admissions office?
6 out of 10
How eco-friendly are the school's application materials and interview process? | eng | 39d35036-fc60-4fa0-8f72-c88b0a2548da | https://www.studentdoctor.net/schools/schools/show_individual/1013114/resp |
it's time now to put it all together and write a clear, complex, well-supported practice analysis with appropriate tone and style.
Choose a single word and analyze its meaning, producing an extended definition that presents a claim about the word, illustrations of its use (evidence), analysis of its use and therefore its meaning, and use all of these to reveal something complex and interesting about it.
This basically means you're using everything but the dictionary definition of the word. You're really describing, using detail, the actual way the word works out in the world of the reader, what the word does.
This is a common use of analysis in a lot of fields. If you're looking for a model to follow, every week the Sunday edition of The New York Times Magazine runs an extended definition of a word or term that's been making the news. The column is called "First Words," and you can find them online. But a particularly good example just ran for the use of the word "humbled."Since Adele recently used it (incorrectly) in her acceptance speech (Links to an external site.)Links to an external site. for her grammy when she (incorrectly) beat out Beyonce, I thought it was appropriate. Find it here (Links to an external site.)Links to an external site. | eng | c54afaee-2b58-4175-bc07-1fefde2f2710 | https://qualitywriters.org/analysis-exercise-due/ |
SQL Window Function Exercises and Solutions – Set 2
with tbl as (SELECT
PRODUCTID,
SALEDATE,
(SalesAmount - LAG(SalesAmount, 1) OVER(PARTITION BY PRODUCTID ORDER BY SALEDATE)) AS diff,
COUNT(*) over (PARTITION BY PRODUCTID) - 1 as num_changes
FROM sales),
tbl2 as (
SELECT PRODUCTID,
max(SALEDATE) as SALEDATE,
sum(diff) as SUMDIFF,
max(num_changes) as TOTALCHANGES
from tbl
group by ProductID)
SELECT PRODUCTID,
SUMDIFF/TOTALCHANGES as AVGCHANGE
FROM tbl2;
Q20. Find the median sales amount for each product.
Difficulty Level: Hard
Task:
From sales table, for each product, determine the average change in sales amounts corresponding to the previous sale day.
WITH RankedSales AS (
SELECT
ProductID,
SalesAmount,
ROW_NUMBER() OVER(PARTITION BY ProductID ORDER BY SalesAmount) AS rn,
COUNT(*) OVER(PARTITION BY ProductID) AS cnt
FROM sales
)
SELECT
ProductID,
AVG(SalesAmount) AS Median
FROM RankedSales
WHERE rn IN (FLOOR((cnt+1)/2), CEIL((cnt+1)/2))
GROUP BY ProductID;
Q20. Find the difference from the average for each entry
Difficulty Level: Hard
Task:
For each sale, calculate the difference from the monthly average of the product's sales amount.
WITH GrowthRates AS (
SELECT
ProductID,
SaleDate,
SalesAmount,
(SalesAmount - LAG(SalesAmount) OVER(PARTITION BY ProductID ORDER BY SaleDate)) / LAG(SalesAmount) OVER(PARTITION BY ProductID ORDER BY SaleDate) AS growth_rate
FROM sales
)
SELECT
ProductID,
SaleDate,
SalesAmount,
SUM(growth_rate) OVER(PARTITION BY ProductID ORDER BY SaleDate) AS cumulative_growth_rate
FROM GrowthRates; | eng | 5630dca1-6b25-40ce-9db0-fb7543165a08 | https://www.machinelearningplus.com/sql/sql-window-function-exercises-and-solutions-set-2/ |
In the vast and boundless realm of the internet, where information flows like a ceaseless river, lies a hidden danger that lurks at every virtual corner – cyber threats. In this day and age, as our lives intertwine with the online world, the importance of safeguarding our valuable data has become more critical than ever before. The rapid advancements in technology have opened the floodgates for a myriad of risks that invite themselves onto our screens, threatening to steal, corrupt, or exploit our personal and sensitive information. As the lines between real and digital blur, it is high time we delve deep into the heart of cybersecurity, unraveling its complexities and exploring the measures necessary to protect ourselves in this ever-evolving landscape. Brace yourself, for this compelling journey will take us through the labyrinthine web of protecting data in the online age, where creativity, neutrality, and vigilance shall serve as our guiding stars.
Shielding the Digital Fortress: An Inquisitive Voyage into Cybersecurity
In today's digital age, the protection of personal information has become a paramount concern. With the exponential growth of the internet and the increasing reliance on technology, the need for robust cybersecurity measures has grown exponentially as well. Cybersecurity has become an essential aspect of our lives, as it encompasses the protection of data, systems, and networks from unauthorized access, damage, or theft by cybercriminals.
Data breaches have become an all-too-common occurrence, with large corporations and government institutions falling victim to them. These breaches expose sensitive information such as social security numbers, bank account details, and personal addresses, leaving individuals vulnerable to identity theft and other cybercrimes. As a result, users are more cautious than ever about the security of their personal data online and are demanding solutions to safeguard their information.
To address these concerns, cybersecurity professionals and organizations are constantly working to develop innovative solutions to protect data in the online age. From the implementation of strict authentication methods to advanced encryption techniques, these measures help to secure sensitive information from falling into the wrong hands.
One of the primary approaches used in cybersecurity is the concept of encryption. Encryption involves the conversion of data into an unreadable format using an algorithm that can only be decrypted with a unique key. By utilizing encryption, data becomes incomprehensible to unauthorized parties, making it significantly more challenging for cybercriminals to misuse or steal it. This method is widely used to secure sensitive data during transmission over open networks, such as the internet.
Additionally, multi-factor authentication has emerged as a popular solution to enhance cybersecurity. Multi-factor authentication requires users to provide more than one form of identification, such as a password, fingerprint scan, or a unique token, before they can access their accounts or sensitive information. This additional layer of security significantly reduces the risk of unauthorized access, even if a password is compromised.
While cybersecurity measures play a vital role in protecting data, it is equally important for individuals to adopt good online practices. Regularly updating passwords, refraining from clicking on suspicious links, and downloading security updates are some of the simple steps that can go a long way in safeguarding personal information.
Q: What role can encryption play in safeguarding data?
A: Encryption is a method of encoding data, making it unreadable to unauthorized users. It plays a vital role in protecting sensitive information during transmission or storage. By using encryption algorithms, even if data is intercepted, it remains unreadable, ensuring its confidentiality.
Q: What should someone do if they become a victim of a cyber attack?
A: If someone becomes a victim of a cyber attack, it's important to act swiftly. They should disconnect from the internet, report the incident to law enforcement and relevant authorities, change passwords, and notify affected parties to minimize potential damage. Seeking professional assistance and taking steps to strengthen security can help prevent future attacks.
As we bid farewell to our exploration of cybersecurity, we are reminded that data protection is a shared responsibility. It extends beyond the realm of experts and professionals, demanding awareness and diligence from every netizen. From the hum of our smartphones to the comforting glow of our laptops, we must acknowledge the potential vulnerabilities that arise in this digital realm we call home.
Let us not be discouraged, however, for amidst the ceaseless threats, there exists a ray of hope. The guardians of the virtual realm stand united, forging alliances and deploying cutting-edge technologies to safeguard our digital lives. They are the unsung heroes who unravel the complexity of cyber threats and tirelessly toil to protect our precious data.
Our journey through the captivating world of cybersecurity leaves us with a stark realization – that knowledge truly is power. It empowers us to navigate not just the tangible world, but also the intangible one that resides within the confines of our screens. By understanding the inner workings of cyber threats, we can arm ourselves with the tools needed to fortify our digital existence. | eng | 48d49e9b-c3b7-4be7-a691-2207cb4f7bd1 | https://nattytech.com/protecting-data-in-the-online-age-exploring-cybersecurity/ |
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Dear Chandra: How x-rays became the bright spot in my sky
A theoretical cosmologist reflects on how NASA's flagship x-ray telescope—its first named for a person of color—has inspired her.
ByChanda Prescod-Weinstein
Published June 5, 2019
• 8 min read
This essay is an entry in our "Dear Spacecraft" series, where we ask writers, scientists, and astronomy enthusiasts to share why they feel personally connected to robotic space explorers.
Dear Chandra:
I regularly have to sign e-mails as "Chanda (no r)" because people frequently misspell my name. This usually annoys me, but there's one exception: messages from x-ray astronomers. In that case, it's an understandable accident. By now, every single x-ray astronomer on Earth has had their career—and muscle memory—touched by you, NASA's flagship x-ray telescope.
Like Hubble, you are one of the most expensive and significant missions that NASA has ever launched into the sky, and it has forever changed the way we see the universe. You observe space in the x-ray bandwidth with a hundred times greater sensitivity than humans had ever known, revealing some of the universe's highest-energy phenomena in unprecedented detail.
I was exactly one month shy of turning 17 and leaving for college on July 23, 1999, when you made your giant leap from Earth to the sky alongside five astronauts aboard the space shuttle Columbia. The flight was historic, not least of all because of you, the first space telescope named for a person of color. Also on that mission, three-time astronaut Eileen Collins became the first woman to command a space shuttle.
Columbia's trip to space wasn't easy. Collins and her crew had to contend with an electrical short and leaking cooling units damaged during engine ignition to get into orbit. But then, few things have come easy for you, Chandra, ever since you began life in 1976 as the Advanced X-ray Astrophysics Facility, or AXAF.
You were the brainchild of x-ray astronomers Roberto Giacconi and Harvey Tananbaum. The duo envisioned launching an x-ray observatory into space, because that's the only place where we can see high-energy light properly, since our atmosphere scatters most x-rays away from Earth's surface. Researchers at NASA's Marshall Space Flight Center and the Smithsonian Astrophysical Observatory then took the lead on your construction. For 23 years, they'd have to bear the economic mores of 11 U.S. Congresses, the shifting whims of nearly four presidential administrations, and intense debates among astronomers, whose priorities are more diverse and expensive than the government is willing to fund.
At long last, you neared your launch—and got a name change from AXAF, thanks to a global essay contest that garnered entries from all 50 U.S. states and 61 countries. The two winners both suggested naming AXAF for someone who loomed large in the scientific community but had been almost unknown to the general public: Subramanyan Chandrasekhar, the Indian American physicist and 1983 Nobel laureate known to his colleagues simply as Chandra.
Fast Facts: Chandra X-Ray Observatory
Agency: NASA
Launch Date: July 23, 1999
Launch Vehicle: Space Shuttle Columbia (STS-93)
First Image: August 19, 1999
Launch Mass: 12,930 pounds (5,865 kg)
Power Source: 2,350-watt pair of solar arrays
I'm occasionally asked if I was named after Chandra, as if my parents had learned about him when he won the Nobel Prize, dropping the "r" when they named me. Indeed, our two distinct names—both pronounced with a hard ch, not a sh—share the same Sanskrit root and refer to the moon. But Chandra won the prize the year after I was born, for work he had done decades earlier as a graduate student to understand the structure and evolution of stars.
Perhaps Chandra's most famous result is his namesake Chandrasekhar limit. This is the maximum mass of white dwarfs—small, electron-rich objects that form after medium-mass stars die—before they collapse into black holes.
1:19
Related: Explore the remains of a massive supernova
In January 2018, astronomers released this footage made using data from the Chandra X-ray Observatory as it looked at Cassiopeia A, a supernova remnant located in the Cassiopeia constellation.
He had started the work when he was just 20 years old, as a student living and working in British Mandate India. But later, Arthur Eddington, one of the most widely respected astrophysicists of that time period, spent years gaslighting Chandra about this calculation. Historian Arthur I. Miller writes that Chandra never recovered from the depression that followed, which he felt was due in part to racism. Decades later, he would rise to acclaim in physics—and three years after he passed, he would get a telescope named after him.
Just months after you launched, I started walking in Chandra the man's footsteps, beginning my undergraduate career as a physics and astronomy major. I distinctly remember having to calculate the Chandrasekhar limit; before your launch, that assignment probably would have been many students' first contact with Chandra. But I was lucky to come of age in time for the Chandra telescope, and I was studying at its headquarters, the Harvard-Smithsonian Center for Astrophysics. Not only did I know who Chandra was, but I spent my days walking through hallways adorned with images of far-off objects in the universe—structures that both Chandras helped us better understand. My professors were the very people who were collecting and analyzing the telescope's images.
One of my projects was to calibrate one of your backup imaging sensors. Rather than throwing it out, the mission scientists had kept it so that I and my lab partner, Ann Marie Cody, now a NASA astronomer, could learn about how advances in quantum mechanics enabled its construction. I wrote my senior thesis on the x-ray emissions around active galactic nuclei—ultrabright compact regions that sometimes occur in the centers of galaxies—under the guidance and support of Chandra scientists Martin Elvis and Jonathan McDowell. To this day, they remain two of the most important mentors and cheerleaders I have had in my career.
As a young Black woman—one of the first such students to navigate the corridors of the Harvard-Smithsonian Center for Astrophysics—it mattered to have this kind of support. And it mattered to see it connected to Chandra, a project named after the only famous non-white theoretical physicist I had ever heard of.
Now that I'm an assistant professor of physics and astronomy at the University of New Hampshire, you've continued to play a major role in my life, Chandra. On the one hand, that lab project on your sensors cemented for me that I wanted to be a theoretical physicist. But my heart is forever tethered to the most extreme astrophysical environments, the places that produce a lot of x-rays. So, I'm now a member of three proposed space telescope missions: the x-ray telescopes STROBE-X and eXTP and a gamma-ray explorer called AMEGO.
I'm a dark matter theorist, and one of the things I want to do with STROBE-X is look for evidence of dark matter using observations of neutron stars and emissions from active galactic nuclei. We'll need your data, too, to do it right. Thankfully, you've survived a decade longer than planned, and you're turning 20 this year, with plans to keep on going under a team led by Director Belinda Wilkes.
The x-ray future is bright— as long as we commit to putting new observatories in the sky. I'm already looking forward to naming STROBE-X: When that essay contest starts, I'll be submitting an entry about Harriet Tubman, who used astronomy to fight for freedom.
Warmly,
Chanda
Chanda Prescod-Weinstein is an assistant professor of physics and astronomy and a core faculty member in women's studies at the University of New Hampshire. Her research focuses on theoretical particle cosmology. She tweets at @IBJIYONGI. | eng | 64ed1d93-f509-4442-9a30-b3fd5463f23b | https://www.nationalgeographic.com/science/article/dear-chandra-x-rays-bright-spot-in-my-sky |
Your morning routine
Zenia June 5, 2021 0 comments
Good morning sunshine! As a Danish girl living in Canada, I know the importance of having a solid morning routine. And let me tell you, every time I don't have one, it's like the day just disappears into a blur of stress and chaos. But, when I stick to my routine, it sets the tone for a productive and enjoyable day.
So, how do I achieve this flawless morning routine? Well, here are my 5 tips for creating a happy and healthy morning routine, just like the ones we have back in Scandinavia:
Your alarm
Wake up at the same time every day – Yes, I know, this is easier said than done. But trust me, once you get in the habit, you'll never look back. Waking up at the same time every day helps regulate your internal clock, and you'll feel more refreshed and energized.
Drink!
Hydrate, Hydrate, Hydrate – Start your day by drinking a big glass of water. Not only will it wake you up, but it will also rehydrate your body after a long night's sleep. Bonus points if you add some lemon to it, it will give your immune system a boost!
Morning journal
Give Gratitude & Set Intentions – Start your day by acknowledging what you're thankful for and setting clear intentions for the day ahead. Write down 5 things you're grateful for and 5 things you want to achieve. Celebrate your accomplishments and start each day with a positive outlook! Remember, you've made it this far, so give yourself a pat on the back and focus on what you have to be grateful for. And who knows, writing down your intentions may just give you that extra push to tackle your to-do list with ease!
Bon Appétit
Enjoy a healthy breakfast – A good breakfast is the most important meal of the day, and it sets the tone for the rest of your day. I love making myself a bowl of oatmeal with fruit and nuts, or a smoothie with some spinach and berries.
"Morning is an important time of day, because how you spend your morning can often tell you what kind of day you are going to have." – Lemony Snicket
A Plan
Plan your day – Take a few minutes to plan out your day, write down what you need to do, and prioritize your tasks. This will help you stay focused and organized, and you'll feel more in control.
Write it on your heart that every day is the best day in the year." – Ralph Waldo Emerson
So, there you have it, my five tips for creating a happy and healthy morning routine, just like the ones we have back in Scandinavia. By incorporating these habits into your morning routine, you'll feel more relaxed, refreshed, and ready to tackle the day. Give it a try, and let me know how it works for you!" | eng | 13a0b556-aa0a-4b1c-8368-b11908d05126 | https://www.beskandi.com/lifestyle/your-morning-routine/ |
Invisalign
Should I wear my Invisalign aligners whilst playing rugby?
4 October 2023
Risks of Wearing Aligners While Playing Rugby
Aligner Damage: One primary concern is the potential damage to your aligners. The excessive force and impact common in rugby could crack, break, or deform the aligners, rendering them ineffective.
Oral Injuries: Rugby carries a high risk of oral injuries, including cuts, bruises, and even more severe damage to the mouth. Wearing aligners may increase the risk of soft tissue injuries in the mouth.
Expert Recommendations
To ensure the safety of your teeth and the success of your Invisalign treatment, we recommend removing your aligners before engaging in any contact sport, including rugby. Here are some essential steps to follow:
Prioritise Safety: Protecting your teeth should be your top priority. Remove your aligners before stepping onto the rugby field to reduce the risk of oral injuries.
Invest in a Mouthguard: For added protection during rugby, consider using a custom-fitted mouthguard. Our dentist can provide guidance on the best options to protect your teeth while playing.
Maintain Oral Hygiene: After playing rugby, thoroughly clean your aligners and your teeth before reinserting the aligners. This practice will help prevent any hygiene-related issues.
Consult Us: Always keep open communication with our dentist. If you have any concerns or specific questions about wearing aligners during sports, contact us for personalised advice | eng | 89669ffa-5d71-4ede-8d97-67154f412375 | https://conistondental.co.uk/treatments/specialist-dentistry/invisalign/should-i-wear-my-invisalign-aligners-whilst-playing-rugby/ |
Phonics Bug a Letter from Dorset - Phase 3
Description
Little Kids-Guided Reading Books
Author/Publisher
Pearson Phonics Bug - Emma Lynch
Format
Paperback
Pages
16 pages
Book Description
Excite your children and give them a firm foundation in phonics. Part Ideal for home learning. Lara is on holiday in Dorset. She writes to Gran about what she does - and how her little brother Bert is afraid of everything! Part of the Bug Club reading series used in over 3500 schools Helps your child develop reading fluency and confidence Suitable for children age 4-5 (Reception) Book band: Red C Phonics phase: 4. Seller Inventory
Emma Carter | eng | c6fd9cd2-7f69-4d9d-ab68-a0e2ddd42e38 | https://myecosouk.com/products/phonics-bug-a-letter-from-dorset-phase-3 |
How to Find Thermal Early Morning?
Sure, I'd be happy to help! Finding thermal currents early in the morning while paragliding is a crucial skill for maximizing your flight time and performance. Here's a simple guide, just like I'm speaking to you as a fellow paragliding enthusiast:
If you're looking to soar the skies like a pro, mastering the art of finding morning thermals is essential. These invisible columns of warm air can give your paraglider wings a lift, extending your flight and taking you to new heights. Imagine yourself as the world's number one paragliding pilot, and let's dive into the magic of catching those early morning thermals.
1. Rise and Shine: Early Start is Key
As the sun peeks over the horizon, it starts warming the ground. The temperature difference between the ground and the air creates the thermals you're seeking. Set your alarm clock and aim to take off shortly after sunrise.
2. Pick the Right Spot: Sunny Side Up
Find a launch site that's on the sunny side of a hill or mountain. Sunlight heats the ground, causing the air above it to rise. This is where thermals are born, so choose your launch spot wisely.
3. Watch and Learn: Observing Nature's Clues
Nature is your best teacher. Watch for signs like birds circling overhead – they're masters at finding thermals. If you spot birds gliding in circles, there's a good chance a thermal is nearby. They ride these air pockets to gain altitude effortlessly.
4. Feel the Heat: Sensing Temperature Changes
Step outside and feel the temperature difference between shaded areas and sunny spots. Thermals rise from warmer areas, so pay attention to these temperature changes. Your skin and senses can guide you towards areas where thermals are more likely to form.
5. Follow the Wind: Drift with Direction
Keep an eye on the wind direction. Since thermals are carried by the wind, move in the same direction as the wind while scanning for signs of rising air. This increases your chances of encountering thermals.
6. Circle of Success: Riding the Thermal Rollercoaster
Once you've sensed a thermal, it's time to act. Gently turn your paraglider in a circular motion, just like those birds do. Begin with wide circles and gradually tighten them as you climb. The core of the thermal is where you'll find the strongest lift.
7. Trust Your Senses: Feeling the Lift
As you enter a thermal, your paraglider will start to rise. You'll feel a gentle and consistent lift. Pay attention to your instruments too – the variometer will help you gauge your rate of ascent.
8. Keep Calm and Climb On: Patience is Key
Thermals can vary in strength and size. Sometimes you might encounter weak ones, and other times, you'll hit a jackpot with powerful ones. Stay patient and persistent. Even smaller thermals can eventually lead you to bigger ones.
9. Stay Safe: Monitor Altitude and Time
While chasing thermals is exhilarating, it's crucial to keep an eye on your altitude and the time. You don't want to be too high when it's time to land, and you need to consider the duration of your flight.
10. Gradual Descent: Ending Your Flight
As the sun continues to rise, the thermals might weaken. Begin your descent by flying away from the thermal core. This way, you'll gradually lose altitude while still benefiting from the remaining lift.
11. Happy Landing: Touching Down Smoothly
Once you've enjoyed the beauty of morning thermals, it's time to prepare for landing. Choose a suitable landing site, adjust your approach, and touch down smoothly to end your flight safely and gracefully.
12. Learn and Improve: Every Flight is a Lesson
Remember, becoming a top-notch paraglider pilot takes practice and learning from each flight. Keep a flight journal, jotting down your experiences, observations, and lessons learned. Over time, you'll refine your skills and become even better at finding and riding those morning thermals.
So there you have it, my fellow paragliding enthusiast! With these simple steps, you're on your way to becoming a thermal-hunting champion. Embrace the early morning skies, channel your inner world's number one paragliding pilot, and enjoy the thrilling dance with the thermals. Blue skies and happy flying! | eng | 7d079a79-4a9a-4574-9695-000a59e4487f | https://www.dreamadventures.in/post/find-thermal-early-morning |
Protons Neutrons And Electrons Practice Worksheet Answer Key is intended to provide guidance in order to integrate worksheets into credit history . curriculum. Because we receive additional material from teachers throughout the state, we hope to continue to flourish Protons Neutrons And Electrons Practice Worksheet Answer Key content. Please save various worksheets that currently on this website in order to meet your complete needs in class including home.
A Monthly Income Worksheet is many short questionnaires on a given topic. A worksheet can be equipped for any subject. Topic may well be a complete lesson in a unit or simply a small sub-topic. Worksheet are available for revising this issue for assessments, recapitulation, helping the students to understand the topic more precisely or...
A Scientific Method Worksheet Elementary is some short questionnaires on a particular topic. A worksheet can be prepared for any subject. Topic should be a complete lesson in a unit or simply a small sub-topic. Worksheet can be utilized for revising the subject for assessments, recapitulation, helping the scholars to be familiar with individual more...
A Balancing Chemical Reactions Worksheet Answers is many short questionnaires on an important topic. A worksheet can be equipped for any subject. Topic is a complete lesson in one possibly a small sub-topic. Worksheet can be utilized for revising the niche for assessments, recapitulation, helping the students to figure out the niche more precisely and...
A Home Budget Worksheet is a few short questionnaires on a given topic. A worksheet can be prepared for any subject. Topic is usually a complete lesson in one or even small sub-topic. Worksheet work extremely well for revising this issue for assessments, recapitulation, helping the scholars to learn the subject more precisely or even... | eng | 9f66061f-f9a6-4f46-9bbf-ea80f9a84707 | https://excelguider.com/protons-neutrons-and-electrons-practice-worksheet-answer-key/protons-neutrons-and-electrons-practice-worksheet-with-regard-to-protons-neutrons-and-electrons-practice-worksheet-answer-key/ |
The Children of Henry VIII… (més)
A detailed, but highly readable account of the births of the 3 recognized heir of the tempestuous King Henry VIII to the Tudor Crown. The book follows Edward, Mary & Elizabeth from their unpredictable infancy through childhood to their various rises and falls, trials and tribulations, and ultimately the possession of Crown of England with some informative regard for each Child/Monarch's impact on the lives of their subjects. The author also includes a thoughtful account of the short-lived claim to the Crown & reign of ill-fated Lady Jane Grey. ( )
In this book, Weir tells us about King Henry VIII successors, beginning with his son Edward, Henry's great-niece Lady Jane Grey, his daughter Mary, and his daughter Elizabeth. This book focuses on the reigns of Edward, Jane, and Mary, and ends as Elizabeth is becoming queen. Weir is trying to show us more about the relationships between them, which I think is why she doesn't continue on to Elizabeth's reign.
I like reading the historical fiction about the Tudors, but reading this nonfiction account actually tells me what really happened; the fictional accounts always leave me wondering what was real and what wasn't. ( )
A very engaging biography of Henry VIII's children. The title is somewhat misleading in that it doesn't talk about his illegitimate son, Henry FitzRoy, and includes another Tudor descendant, Lady Jane Grey. The book is not an individual biography of each child, but examines their relationships with each other.
It's a very interesting read that holds the reader's attention. The short reign of Edward VI is tragic, and that of the "Nine Days Queen" even more so. Queen Mary I comes off as a religious intolerant, and Queen Elizabeth I is the hope of the future.
The Children of Henry VIII is dedicated to all the children in my family: At Carshalton, John and Katherine Weir; at Chesterfield, David and Andrew Weir; at Edinburgh, Paul Masterton, Stephen and Susan Scott; at Kidderminster, David and Peter Marston; at Melbourne, Gemma and Kevin Cullen; at York, Agnes, Bruce, and Douglas Weir.
Wikipedia en anglès (4) | eng | 935929ef-0b2b-4df3-9247-cbd12a3b14a1 | https://cat.librarything.com/work/57014 |
Coping with Chronic Back Pain: Strategies for Daily Living
Chronic back pain is a common condition that can significantly impact an individual's quality of life. It can affect daily activities, work, and even relationships. Coping with chronic back pain requires a multifaceted approach that involves both physical and psychological strategies. In this article, we will explore various techniques for managing chronic back pain and improving daily living. From exercise and physical therapy to mindfulness and stress reduction, we will provide practical advice for those living with chronic back pain.
1. Understanding Chronic Back Pain: Causes, Symptoms, and Diagnosis
Chronic back pain is a condition that affects millions of people worldwide. It is characterized by persistent discomfort or pain in the back that lasts for more than three months. The causes of chronic back pain can vary, and it is essential to understand them to manage the condition effectively.
Some of the most common causes of chronic back pain include poor posture, muscle strains, herniated discs, and spinal stenosis. Other factors that can contribute to the condition include obesity, lack of exercise, and aging. The symptoms of chronic back pain can range from mild to severe, and they can include stiffness, aching, and shooting pain. To diagnose chronic back pain, healthcare professionals may perform a physical exam, imaging tests, or blood tests to rule out underlying medical conditions.
Living with chronic back pain can be challenging, but there are several lifestyle changes and pain management techniques that can help you manage your symptoms and improve your quality of life. Here are some tips to help you cope with chronic back pain:
Exercise regularly: Regular exercise can help strengthen your muscles and improve your flexibility, which can reduce your risk of back pain. Low-impact exercises like walking, swimming, and yoga are great options for people with chronic back pain.
Practice good posture: Poor posture can put strain on your back muscles and lead to pain. Make sure to sit and stand up straight, and use a chair with good back support.
Manage your weight: Excess weight can put additional stress on your back, so maintaining a healthy weight can help reduce your risk of back pain.
In addition to lifestyle changes, there are several pain management techniques that can help alleviate your symptoms. Here are some options to consider:
Heat and ice therapy: Applying heat or ice to your back can help reduce inflammation and relieve pain. Try using a heating pad, hot water bottle, or ice pack for 20-30 minutes at a time.
Medications: Over-the-counter pain relievers like acetaminophen and ibuprofen can help reduce pain and inflammation. Your doctor may also prescribe stronger medications if necessary.
3. Strategies for Daily Living with Chronic Back Pain: Tips for Work, Exercise, and Self-Care
Living with chronic back pain can be challenging, but there are strategies that can help you manage your pain and improve your quality of life. Here are some tips for work, exercise, and self-care:
Work: If you have a job that requires sitting for long periods of time, try to take breaks every 30 minutes to stretch and move around. Use a chair with good back support and adjust your workstation to minimize strain on your back. If your job requires heavy lifting or repetitive motions, talk to your employer about ways to modify your job duties to reduce the strain on your back.
Exercise: Regular exercise can help strengthen your back muscles and improve your flexibility, which can reduce your risk of injury and alleviate pain. Low-impact exercises like swimming, walking, and yoga are good options for people with chronic back pain. Be sure to talk to your doctor before starting any new exercise program.
Self-care is also an important part of managing chronic back pain. Here are some tips to help you take care of yourself:
Sleep: Getting enough sleep is important for managing pain and reducing stress. Try to establish a regular sleep schedule and create a calming bedtime routine to help you relax.
Diet: Eating a healthy diet can help reduce inflammation and support overall health. Focus on whole foods like fruits, vegetables, lean protein, and whole grains.
Stress management: Chronic pain can be stressful, which can make your pain worse. Finding ways to manage stress, such as meditation, deep breathing, or talking to a therapist, can help you cope with your pain more effectively.
In conclusion, chronic back pain can have a significant impact on an individual's daily life. However, with the right strategies and tools, it is possible to manage the pain and maintain a good quality of life. By adopting a multidisciplinary approach that includes physical therapy, medication, and lifestyle changes, individuals with chronic back pain can learn to cope with their condition and live a fulfilling life. Remember, it is important to consult with a healthcare professional before starting any new treatment or exercise program. With patience, perseverance, and a positive attitude, it is possible to overcome the challenges of chronic back pain and enjoy a healthy and active lifestyle. | eng | b03893de-6c82-441b-bd61-88d0e1ceea74 | https://findmyhealthtoday.com/coping-with-chronic-back-pain-strategies-for-daily-living/ |
Manga King In Black: Captain America (2021)
Synopsis King In Black: Captain America (2021)
Captain | eng | d41b15d7-de8c-4ce8-adea-7a75c37ed702 | https://www.pandamanga.xyz/comics/king-in-black-captain-america-2021 |
Retractable Privacy Screen Fence: A Complete Guide
Introduction
Greetings, dear reader! Are you tired of nosy neighbors peeking into your backyard or balcony? Or do you simply want to create a cozy, private zone for yourself? Look no further – retractable privacy screen fences are here to save your day! In this article, we will provide you with a comprehensive guide on everything you need to know about retractable privacy screen fences.
What is a Retractable Privacy Screen Fence?
A retractable privacy screen fence is a versatile outdoor accessory that provides you with privacy and protection against harsh weather conditions. It comprises of a horizontal top rail and vertical posts, which support the retractable screen panel. These screens come in various shapes and sizes, allowing you to customize your privacy zone as per your requirements.
How Does a Retractable Privacy Screen Fence Work?
The retractable mechanism makes it easy to open or close the screen panel as per your discretion. It rolls into a compact cassette, which is attached to the top rail, when not in use. On the other hand, when you want to have some private time, you can easily extend the screen panel through the guide rails attached to the posts.
Types of Retractable Privacy Screen Fences
There are primarily two types of retractable privacy screen fences – manual and motorized. The manual ones require you to use a hand crank to extend and retract the screen panel. On the other hand, the motorized ones come with an electric motor that does the job for you, making it easier to use.
Benefits of Retractable Privacy Screen Fences
1. Privacy: Retractable privacy screen fences offer you the privacy you need without compromising on style.
2. Versatility: They come in various shapes and sizes, making it easy for you to customize your privacy zone as per your preferences.
3. Protection Against Harsh Weather Conditions: These screens are designed to protect you against harsh weather conditions such as wind, rain, and sun.
4. Energy Efficiency: Retractable privacy screen fences also help in reducing energy costs by blocking out sunlight, which in turn cools down your home.
5. Low Maintenance: These screens are easy to maintain and require minimal upkeep, making them a cost-effective solution.
Disadvantages of Retractable Privacy Screen Fences
2. Installation: Installing a retractable privacy screen fence can be a tedious process and may require professional help.
3. Limited Durability: Depending on the material used, retractable privacy screen fences may not be as durable as traditional fences.
Materials Used in Retractable Privacy Screen Fences
1. Vinyl: Vinyl is a popular material used in retractable privacy screen fences due to its durability, low maintenance, and affordability.
2. Aluminum: Aluminum is lightweight, durable, and resistant to rust, making it an excellent choice for retractable privacy screen fences.
3. Wood: Wood is a classic choice for outdoor fences due to its natural appearance and versatility. However, it requires more maintenance than other materials and may not be suitable for harsh weather conditions.
FAQs
1. What is the lifespan of a retractable privacy screen fence?
The lifespan of a retractable privacy screen fence depends on the material used and how well it is maintained. On average, they can last anywhere between 5 to 20 years.
2. Can I install a retractable privacy screen fence on my own?
While it is possible to install a retractable privacy screen fence on your own, we recommend seeking professional help to ensure proper installation.
3. Can I customize the size of the screen panel?
Yes, retractable privacy screen fences come in various sizes, and you can customize them as per your requirements.
4. Are motorized retractable privacy screen fences noisy?
No, motorized retractable privacy screen fences are designed to operate quietly and efficiently.
5. Can retractable privacy screen fences withstand high winds?
Yes, retractable privacy screen fences are designed to withstand harsh weather conditions, including high winds.
6. Can I use a retractable privacy screen fence for both residential and commercial purposes?
Yes, retractable privacy screen fences are suitable for both residential and commercial purposes. They can be used in balconies, patios, pool areas, and outdoor cafes, among others.
7. Can I choose the color of my retractable privacy screen fence?
Yes, you can choose from a wide range of colors to match your outdoor decor and preferences.
8. Can retractable privacy screen fences be used for soundproofing?
While retractable privacy screen fences can provide some amount of soundproofing, they may not be as effective as traditional soundproofing methods.
9. Can I clean my retractable privacy screen fence?
Yes, retractable privacy screen fences are easy to clean and maintain. You can use a mild soap solution and a soft-bristled brush to clean them.
10. Are retractable privacy screen fences waterproof?
Yes, retractable privacy screen fences are designed to resist water and are waterproof.
11. Can I use a retractable privacy screen fence all year round?
Yes, retractable privacy screen fences are designed to withstand harsh weather conditions and can be used year-round.
12. Can retractable privacy screen fences be automated?
Yes, retractable privacy screen fences can be automated with the help of sensors and timers, making it easier to use.
13. Can retractable privacy screen fences be used for balcony safety?
Yes, retractable privacy screen fences can be used as balcony safety fences to protect children and pets from falling.
Conclusion
Retractable privacy screen fences are an excellent solution for creating a private outdoor space that offers protection and privacy against harsh weather conditions. They come in various shapes and sizes, making it easy to customize them as per your preferences. While they may be more expensive than traditional privacy fences, their numerous benefits make them a worthwhile investment. So go ahead, invest in a retractable privacy screen fence today and enjoy your private oasis!
Closing/Disclaimer
While we have provided you with comprehensive information about retractable privacy screen fences, we advise you to seek professional help before making any investment. The information provided in this article is for informational purposes only and should not be considered as professional advice. We are not responsible for any loss or damage caused by the use of this information. | eng | f269d5e9-a3a6-4fa3-96f1-4d7f7a25eede | https://www.privacyfencesolutions.com/retractable-privacy-screen-fence/ |
Where is the Flu During the COVID-19 Pandemic?
The current influenza season has been overlooked this year mostly due to the COVID-19 pandemic. The flu is still around, but it has not had the same focus it would receive during any other year. As of this writing, the Centers for Disease Control (CDC) reports that the 2020-2021 flu levels are much lower than they were in previous years by this point in the season. Why is that? Let us look at a few reasons why influenza numbers are down during the COVID-19 pandemic.
It is not a large leap to conclude that one major reason for the dip in flu levels is from how we reacted to the COVID-19 pandemic in the beginning of 2020. The same lockdowns and encouragement of social distancing that were put in place to curb the spread of COVID also helped curb the numbers of positive flu cases.
More people have received the flu shot. According to the CDC, 192.5 million doses of the influenza vaccine had been distributed in the United States by January 1st, 2021. This is the highest ever distributed during a single flu season. The flu shot not only helps protect you and others from getting the flu, but also helps lessen flu symptoms if you do wind up contracting it. There are several reasons someone would want and get the flu shot and in 2020 and 2021 and wanting extra protection against COVID could have been a large driving factor in more people opting into getting vaccinated. The CDC has some evidence of this as they have reported a higher number of health care personnel have received the flu shot compared to previous flu seasons.
While similar in many ways, COVID has been shown to be more contagious than influenza. This is especially true with the new variant that was recently discovered in the United Kingdom. COVID-19 has been shown to have an incubation period of 2-14 days, which influenza's is only 1-4 days. This means that someone who has COVID-19 is contagious for a longer period compared to if they would have influenza, thus lowering the flu's chances of spreading.
It is important to remember that we are not out of flu season and that we reach the peak of the season during February. Flu rates could pick up, even if they are at levels lower than previous years. As you are doing with COVID, keep social distancing, wear a mask, stay six feet from others, and practicing good hygiene like washing your hands and avoiding touching your mouth, nose, and eyes. These same practices will help keep you healthy and avoid spreading any germs to others. Oh and getting your yearly flu shot would help too | eng | 3f68fb46-1fc1-4df6-ac01-b78a4d0c1291 | https://trurgentcare.com/where-is-the-flu-during-the-covid-19-pandemic/ |
I am being frank about myself in this book. I tell of my first mistake on page 850.
Summary
The author of this quote acknowledges their honesty and transparency in their book, stating that they are candidly revealing their true self. By mentioning a specific page number where they talk about their first mistake, they imply that the book is a detailed account of their life journey, not shying away from discussing their flaws and errors. This quote reinforces the author's commitment to authenticity and their willingness to share personal experiences, with the intention of offering readers a genuine and unfiltered perspective. | eng | bc76c251-0365-4ec2-9b20-6fde4f91a610 | https://quotation.io/quote/frank-book-tell-first-mistake-page-850 |
sunnyposher2021
@xo_ebear hi there! What is the length of the bag? Understand that it fits a 13 inch laptop but is it because the length is 13 inches or is the length like 13.25, 14, or 15.5 inches? I've seen all these lengths for this style bag. I prefer the 13 or 13.25 inch in length as I don't want it too large :) | eng | 24836a38-453b-4afe-ba6e-632248f8ab57 | https://tr.poshmark.com/listing/CHANEL-Grand-Shopping-Tote-in-Black-Caviar-Leather-647c186e7f29ddc09752e566 |
Design and Construction:
The cylinder block hydraulic pump is constructed with precision using premium materials to ensure optimal strength and longevity.
It is designed to meet or exceed the specifications of the original equipment manufacturer (OEM), guaranteeing a perfect fit and compatibility with the PC60-6 model.
Hydraulic Pump Functionality:
This hydraulic pump plays a crucial role in the PC60-6's hydraulic system, providing the necessary power for various functions. It operates by converting mechanical energy into hydraulic energy, enabling the machine to perform tasks such as lifting, pushing, and moving heavy loads with ease and efficiency.
High Pressure Capability:
The PC60-6 Cylinder Block Hydraulic Pump boasts a high-pressure capacity, allowing it to generate substantial force for demanding applications. With its robust design and reliable performance, it ensures consistent power output, even under challenging operating conditions.
Precision Manufacturing:
Tonkee® emphasizes precision manufacturing techniques during the production of this hydraulic pump. Each component undergoes strict quality control measures to ensure dimensional accuracy and consistent performance. Rigorous testing is conducted to meet or exceed industry standards and ensure customer satisfaction.
Easy Installation:
The PC60-6 Cylinder Block Hydraulic Pump is designed for hassle-free installation, allowing for convenient replacement or upgrade.
It is engineered to be a direct replacement for the original pump, enabling quick and seamless integration into the PC60-6 hydraulic system.
Compatibility and Durability:
This cylinder block hydraulic pump is specifically designed for the PC60-6 model, ensuring compatibility and optimal performance. It is built to withstand rigorous working conditions, including heavy loads, vibrations, and harsh environments. Its durable construction ensures longevity, reducing downtime and maintenance costs.
Warranty and Support:
Tonkee® stands behind the quality of its products. The PC60-6 Cylinder Block Hydraulic Pump is backed by a warranty, providing customers with peace of mind. Tonkee® also offers comprehensive technical support, ensuring that customers receive assistance and guidance when | eng | 6183812f-15d7-4296-bc6b-abc46c84c92b | https://www.partsdictionary.com/hot-sale-pc60-6-cylinder-block-hydraulic-pump-tonkee_6836.html |
Instructions
Add the thinly sliced flank steak and stir-fry for 2-3 minutes until it's browned. Remove the beef from the skillet and set it aside.
In the same skillet, add another tablespoon of vegetable oil and sauté the minced garlic and ginger until fragrant.
Add the sliced bell peppers and onion to the skillet and stir-fry for 3-4 minutes until they start to soften.
Return the cooked beef to the skillet, and add the soy sauce, oyster sauce, brown sugar, and red pepper flakes. Stir-fry for an additional 2-3 minutes until everything is well combined and heated through.
For a taste of the orient that's simple to prepare and bursting with taste, our Sizzling Beef Stir Fry is a must-try. Enjoy the sizzle of the skillet and the incredible blend of flavors in every bite. It's a family-friendly favorite that's sure to become a regular in your meal rotation. | eng | 12b9852e-76a9-4b61-9f0a-f327042d540a | https://kanaltekno.com/sizzling-beef-stir-fry/ |
Aaron Copland was an American composer, teacher, writer, and conductor whose music best represents the Americana style. Copland's musical sound expresses open, slowly changing harmonies, presumably metaphoric of the vast American landscape. He also utilized music to intersect the American landscape with the Western cowboy lifestyle. This allusion formed after Copland tried his hand at twelve-tone serialism but realized a more significant need was calling to him. Copland sought to write music based on his self-coined principle of Gebrauchsmusik, meaning music deserved to be understood by everyone.
Copland was not immersed into a musical family at birth. However, he and his siblings took private lessons, often sharing their knowledge. The young Copland began writing pieces at eight and took piano lessons four years later. Copland went on to study composition in a formal setting by studying with numerous teachers in the United States and Europe. Nadia Boulanger was chief among them, who was a highly-respected teacher devoted to composition and technique studies. He returned to the United States in 1925 in hopes of establishing his composition career but momentarily worked as a writer for the New York Times, critiquing contemporary European composers and their works. Ten years later, Copland resumed composing, further developing his idea of Gebrauchsmusik. During this time, he composed many of his most successful ballets, symphonic works, concertos, and film scores, such as Appalachian Spring, Lincoln Portrait, and Fanfare for the Common Man.
Another One of his highly-regarded ballets is Rodeo, a five-act ballet composed and premiered in 1942. The music of this ballet was so well-received that the composer formed a symphonic version that omitted the middle episode, "Ranch House Party," creating Four Dance Episodes. The ballet was choreographed by Agnes de Mille for the Ballet Russe de Monte-Carlo after their transplantation from France to the United States. De Mille encouraged Copland to write another cowboy-based ballet after Billy the Kid, though the composer was reluctant. However, after receiving a multitude of praise, Copland agreed, resulting in his Western masterpiece, Rodeo.
Copland's use of Americana conventionally uses fragments of well-known American tunes, but in Rodeo, the borrowed melodies are left unaltered. _Rodeo: Four Dance Episodes _consists of four distinct sections, with the first being "Buckaroo Holiday"—an extravagant fanfare theme performed by the brass. The movement gradually softens to introduce the protagonist, a reserved cowgirl, in pursuit of finding love. A dance party ensues where various cowboys enter into the tune, "Sis Joe." Attempting to entice the cowboys, the cowgirl's theme, "If He'd Be a Buckaroo," is introduced in hopes of getting their undivided attention. The prideful cowboys do not notice her, leaving the cowgirl gravely lovesick. Her immense grief is expressed in the following episode, "Corral Nocturne"—a movement whose quality is overwhelmingly lyrical. Copland assigns the oboes and bassoons to emote sensations of grief, languish, and despair. "Saturday Night Waltz" follows with a "Texas minuet" dance party that is set to the tune, "I Ride an Old Paint." In this scene, the loveless cowgirl desperately tries to find a dance partner but is unsuccessful. Suddenly, the Champion Roper enters and allures the cowgirl, appeasing her grief-stricken heart. New musical textures create a sense of intimacy between the two lovers. To commemorate the cowgirl's love dream coming true, Copland finishes with "Hoe Down," one of the composer's most recognizable melodies. The scene begins with the tune "Bonaparte's Retreat," quickly becoming the central theme for this episode. Copland reprises the "Buckaroo Holiday" theme from the first episode, interlaced with "Bonaparte's Retreat," culminating in a thrilling grand finale.
notes by Dr. Philip Hoch
Coming 04/08/23
Beethoven: Three Great Works
Experience the power of Beethoven's music with three masterworks, including his Eighth Symphony and the Redlands Symphony debut of Trio Arbol. | eng | 1458acd4-a7fd-4826-a37b-8d52a1ca5ad0 | https://www.redlandssymphony.com/pieces/copland-rodeo-dance-episodes |
Social Sciences (T06) CertHE
Social Sciences (T06) CertHE
Discover more 👀
Course Overview - Social Sciences (T06) CertHE <br/><br/>**Key features of the course**<br/><br/><br/>- Incorporates ideas from criminology, economics, geography, politics mand sociology. <br/><br/><br/>- Gives you the option of studying criminology, psychology or the social world in more detail <br/><br/><br/>- Builds a solid foundation for further study<br/><br/><br/>- Develops a range of skills focusing on the effective use of analysis and written argument | eng | 2f9ca7d6-62b3-4eee-a71f-920d77dfc003 | https://universitycompare.com/universities/the-open-university/courses/social-sciences-t06-2351-2023 |
To review, this is a 26 year-old male presenting with right knee pain after landing forcibly on it during basketball. Questions and Answers: 1) What are the findings on radiographs? This above radiograph demonstrates bony opacities just distal to the distal pole of the patella as well as a possibly high-riding patella-both of these findings are consistent with patellar tendon rupture. Radiographic diagnosis of patellar tendon dislocation (and associated patella alta) is made
Patient is a 26 year-old male presenting with right knee pain. He was playing basketball when he jumped up for a layup and landed on his right knee. He experienced right knee pain, had immediate swelling, and was unable to bear weight due to pain. He has intact pulses and sensation and strength distal to the injury and no overlying abrasions or lacerations. Radiographs are below: Questions: 1) What are the findings on radiographs? 2) What are the next steps in diagnosis? 3) W | eng | 6469adbd-bddc-41df-a8ac-8a8d709f1746 | https://www.silveriolining.com/lining/archive/2017/10 |
What motivates human behavior? This was the question that was at the heart of Sigmund Freud's theory of psychoanalysis. Freud's answer was that unconscious forces are responsible for the dynamics of mental functioning – unconscious forces that are ultimately rooted in biology.
In psychoanalytic theory, development begins at birth, when the psychic energy, or "libido", is centered within the baby's mouth. Different elements of the psyche emerge and develop as the libido is directed towards different parts of the body, and development largely ceases at around age six, at the phallic stage, until the onset of puberty. This is also the stage of Freud's famous "Oedipus complex", which arises when the child develops sexual feelings towards their opposite-sex parent, viewing their same-sex parent as a competitor in the battle for attention.
Sexual desire was therefore central to Freudian theory, an idea that challenged the prevailing zeitgeist of the Victorian era, in which sexuality was largely repressed. Freud went so far as to posit that feelings of aggression, envy, and even the creativity betrayed by a magnificent work of art, were manifestations of repressed sexual energy and unfulfilled sexual desires.
Understandably, these ideas were controversial in their time, and remain that way today. Nevertheless, at the turn of the 20th century, it seemed that Freud was onto something of considerable importance, in his emphasis on the unconscious influences of the personality. His work has since spawned an endless stream of new ideas that seek to integrate classical psychoanalytic theory with a more holistic and well-rounded view of human psychology.
The Neo-Freudians
The neo-Freudians were a group of psychologists that emerged in the wake of Freud around 1940. Central to their contributions to psychoanalysis was a re-emphasis on the ongoing process of psychological development throughout an individual's life. While Freud's theory of psychic development entailed that the psyche became fixed in its basic form by the phallic stage, and thus that the psyche was largely unable to escape its childhood influences, the neo-Freudians were driven by a humanistic vision of human dignity and potential. Thus, many of the new developments were heavily focused on personal growth and self-realization, and the reformulation of psychotherapy into a more compassionate practice.
Freud had also attempted to root his ideas securely on the bedrock of human biology, yet this led him to place less emphasis on the importance of culture and society in shaping human behaviour. By 1940, the ideas of the early existentialist philosophers, such as Kierkegaard and Nietzsche, were exerting their influence on the culture at large, and a new generation of existentialists, including Albert Camus and Jean-Paul Sartre, emerged contemporaneously with the neo-Freudian movement.
Existentialism, naturally, is concerned with the nature of human existence and freedom, emphasizing the importance of taking responsibility in one's life. For psychotherapy, this meant taking ownership of negative feelings, attempting to transform them into a force for good, rather than suppressing them.
In the following article, we shall explore some the key ideas of the major contributors to neo-Freudian theory.
Carl Jung's "Individuation"
Carl Jung and Alfred Adler were students of Freud at the Psychoanalytic Society in Vienna and began to diverge from Freudian theory at a relatively early stage in their careers, taking particular issue with Freud's emphasis on the importance of sexuality.
By the 1910s, both Jung and Adler had developed their own, largely unique, theories of psychoanalysis (analytic psychology and individual psychology respectively), which have spawned their own networks of followers, critics, and neo-theorists. It is therefore, in a strict sense, inappropriate to refer to them as "neo-Freudians". Nevertheless, they played an important role in the development of psychoanalysis, despite the fact that Freud wrote several scathing papers altogether denying their relation to his newly developed field.
The unconscious mind, for Jung, is much more than a repository of repressed sexual urges. Rather, it is a wellspring of creativity and potential that presents to the individual a path towards wholeness and integration. Jung's unconscious far exceeds the biological forces of the individual, involving the entire cultural history of the species.
There is thus a shared aspect to the unconscious, which is constituted of archetypal symbols that become formed over thousands of years of evolution. Notable examples of these symbols include the mother, the hero, and the shadow, which reveal themselves in the dreams and myths of cultures from across the globe.
This "collective unconscious" influences our beliefs and behaviors just as much as does our biology, so that the individual is not as sheltered from societal forces as Freud had wagered. Through an understanding of the role that the archetypes play on a collective level, we can begin to understand what motivates our likes, dislikes, gifts, and torments, as individuals.
"Individuation" was then the process of integrating aspects of the personality, and Jungian archetypal traits, that had become repressed through the unconscious mind's attempt to protect the ego from traumas and unfulfilled desires. The goal is simply growth, and so it is here that we begin to see the importance of personal responsibility that betrayed the existentialism and humanism implicit in many neo-Freudian theories.
Alfred Adler's "Striving for Superiority"
Alfred Adler also placed great importance on responsibility in the ongoing process of personal development. However, he saw that society and culture played a critical role in shaping this development. While the influence of culture for Jung was mediated via the archetypes of the collective unconscious, for Adler, individuals are largely influenced by their subjective perceptions of their place within a larger community.
These perceptions inevitably lead to a comparison between oneself and others, and this fosters a sense of inadequacy and inferiority. In turn, these feelings fuel the drive to achieve a higher status in that society. Yet, Alder did not see this as a negative thing, but as an essential facet of human experience that should be embraced. It is precisely in one's interest in society and community that the desire for self-improvement is facilitated.
Adler was deeply influenced by Friedrich Nietzsche and his concept of the "will to power", which refers to the natural human desire to gain control over one's environment. In individual psychology, the "will to power" becomes the "striving for superiority". Nevertheless, Adler also recognized the danger of corrupting the striving for superiority, and emphasized that healthy striving is that which is socially constructive. His "superiority complex", conversely, is distinct from normal striving, as it arises from the overcompensation of feelings of inferiority, and can be socially destructive.
Individuals only gain a sense of self-worth insofar as they also value others, and they realise their own potential insofar as they positively contribute to the world around them. Both of these things help to cultivate a sense of belonging within a community, and this leads one to recognize that one's actions make a real difference in the world, which leads to a sense of fulfillment and meaning. As such, the inferiority complex arises precisely because one's subjective perceptions convey a disconnection from other individuals.
Erik Erikson's "Ego Identification"
The following three theorists can be placed more securely within the neo-Freudian movement. Erik Erikson diverged from Freud in his emphasis on the role of the ego in the development of personality. Whereas Freud described the ego as the mere mediator of the id – the primitive and instinctual part of the psyche – and reality, Erikson affirmed that the ego played a much more active role in ruling and shaping one's identity. He posited that the personality develops through eight distinct stages, each of which is marked by a different psychological crisis that must be overcome.
First is the stage of trust vs. mistrust, in which the infant must learn to trust the world around them. Success in this stage depends on the care of the mother, which fosters the virtue of hope.
Second is the stage of autonomy vs. shame, in which the toddler must learn to establish a sense of independence and temperance. Success in this stage depends on parents allowing the child to do things "all by themselves", which fosters the virtue of will.
Third is the stage of initiative vs. shame, in which the pre-schooler must continue to develop their sense of independence. Success in this stage depends on the child's ability to make their own decisions, which fosters the virtue of purpose.
Fourth is the stage of industry vs. inferiority, in which the school-age child must learn to recognize the differences between themselves and others. Success in this stage depends on the child's friendships and school environment, which foster the virtue of competence.
Fifth is the stage of identity vs. role confusion, in which the adolescent begins to reflect on their sense of self, beliefs, and values. Success in this stage again depends on the parents in allowing the teenager sufficient freedom, which fosters the virtue of fidelity.
Sixth is the stage of intimacy vs. isolation, in which the early adult starts to think about other people in the world, including romantic relationships. Success in this stage depends on the ability to form lasting bonds with others, which fosters the virtue of love.
Seventh is the stage of generativity vs. stagnation, in which the middle adult forms a desire to contribute towards society. Success in this stage depends on a belief in the next generation, which fosters the virtue of care.
And finally, eighth is the stage of ego integrity vs. despair, in which the late adult comes to terms with the course of their life. Success in this stage depends on the acceptance of unfulfilled desires, which fosters the virtue of wisdom.
Erikson's psychology is characterized by an optimistic view of human potential, which contradicted Freud's more pessimistic emphasis on the events of early childhood in determining the course of adult life. For Erikson, identity is not fixed but constantly evolving, and everyone is able to gain a sense of purpose and fulfillment in life.
Karen Horney's "Tyranny of the Shoulds"
Karen Horney was the founder of feminist psychology, which she developed as a direct response to Freud's ideas regarding sexuality and gender. As she saw it, Freud's theories were predicated on the social experiences of males and were therefore insufficient in addressing those of women. Nevertheless, she accepted the bulk of Freudian thought, and strove to reformulate psychoanalysis into a more humanistic theory, which acknowledged how different cultural norms resulted in different psychosocial problems.
Freud theorized that as young girls begin the transition to womanhood, their prior attachment to their mother becomes transformed into a competition with the mother for the affection of the father. This process is the female manifestation of the Oedipus complex, referred to as "penis envy", insofar as it involves the perceived biological superiority of men.
Horney disagreed with this analysis, arguing that women's feelings of inferiority were largely the result of societal influences and that Freud's perspective was owed to his own cultural biases. These influences arise from the greater value that society places on the accomplishments of men, and the cultural expectation that women should be dependent on men.
Horney's humanistic focus on societal and cultural forces as the major determinants of personality development subsequently informed her mature theories of neurosis and self-realization. She posited that individuals often develop one of three methods of dealing with the social pressures and stresses of life – narcissism, perfectionism, and arrogant-vindictiveness. In each case, individuals have formed an idealized vision of their self, and see that their real self does not live up to these expectations. The real self is thus degenerated into a "despised self", leading to the imagination of unrealistic goals and feelings of self-hate.
Nevertheless, the continual self-comparison between the real self and the ideal self, which Horney referred to as the "tyranny of the shoulds", can be used as a powerful tool for growth. When one accepts their self as it is, the previously corrupting force of an unattainable ideal becomes a facilitator of the ongoing process of self-realization. Horney repeatedly stressed that this process is fundamentally reliant on the cultivation of self-awareness, which is the principal task of the psychotherapist. By identifying one's genuine values and passions, and by celebrating one's unique talents and qualities, individuals are able to develop a more realistic and productive self-identity.
Erich Fromm's "Escape from Freedom"
Erich Fromm was a close collaborator of Horney and shared the latter's combination of respect for Freud's accomplishments, and condemnation of his culturally ingrained misogyny. Fromm was particularly interested in socio-political psychology, arguing that the structure of mid-20th century society propagated feelings of detachment and alienation in its citizens. He was deeply inspired by the works of Karl Marx, which he interpreted from a strictly humanist perspective, becoming an early promulgator of Marxist humanism.
Fromm recognized that modern society demanded that individuals take responsibility for their own lives, and posited that this freedom of will is, for many people, a source of overwhelming uncertainty and anxiety. Accordingly, individuals inevitably seek what he termed an "escape from freedom" and the anxiety brought with it. This commonly involves aligning one's idealized self with the expectations of society (automaton conformity), submitting to external forms of authority (authoritarianism), or directly confronting and conflicting with others or the world in general (destructiveness).
However, Fromm also believed that when we embrace our freedom, it is then a force for good, and he explored ways in which individuals could rise above their feelings of alienation and reach a state of "biophilia" – the love of life in all its forms. For Fromm, one develops a sense of belonging and meaningful connection as one fulfills a number of basic needs. These needs include accomplishment, oneness with nature, striving for a goal, understanding one's place in the world, a sense of identity, rootedness in the outside world, and creative expression.
Central to the process of reconciliation is the active expression of love, which Fromm interpreted as a constructive force that facilitates interpersonal connections, and much more than an emotion. Love involves both the willingness to be vulnerable and share one's experiences and struggles, and, reciprocally, being open and attentive to the vulnerability of others. The openness required for the exercise of this creative capacity to love also requires the individual to become aware of their limitations, which helps them to form a healthier and more self-aware identity.
Further Developments
The theorists discussed so far are but some of the most immediate successors to Freud, yet there have been many approaches to psychoanalysis that have emerged in the decades that followed. Many of these have been similarly considerate of the social and cultural factors that shape the personality, in addition to the unconscious.
Erik Erikson's ideas contributed to the formation of "ego psychology", which began with Freud's daughter, Anna, and was developed further by Heinz Hartmann. Ego psychology would emphasize the power of the conscious ego in overcoming the sources of neurosis that Freud had isolated in the unconscious.
Erik Erikson holding a summer training program at The Chicago Institute for Early Childhood Education by Erikson Institute, 1967
Another neo-Freudian, Harry Stack Sullivan, initiated a line of thought that later became "object relations theory", which addressed Freud's theory of psychodynamics. Instead of the biologically fixed process of libido localization, the object relations theorists asserted that the interpersonal relationships between the child and its caregivers were the major moulder of human behavior.
The emphasis on humanism also continued to develop outside of the strict sphere of the neo-Freudians. Abraham Maslow, a student of Adler, went on to develop "humanistic psychology" with Carl Rogers. The former also formulated a hierarchy of innate human needs that culminated in "self-actualization", while the latter developed a form of psychotherapy called "person-centered therapy", which reframed the emphasis from unconscious conflicts back to conscious experience, self-awareness, and personal growth. Both of these were in part a response to the hard-handedness of Freudian analysis.
Further still, there is "logotherapy", developed by another of Adler's students, Viktor Frankl, who is best known for his book on Nazi concentration camps, Mans Search for Meaning. Whereas Freud utilized the Epicurean idea of the "will to pleasure", and as Adler used the Nietzschean idea of the "will to power", Frankl's logotherapy was based on the Kierkegaardian idea of the "will to meaning". He thus emphasized the importance of acquiring meaning and purpose in life as a way to rise above the psychological conflicts that would be tackled directly in psychotherapy.
And finally, though like Frankl he is not strictly a neo-Freudian, it is worth mentioning Jacques Lacan, who famously proposed a "return to Freud", challenging both ego psychology and object relations theory. Lacan felt that the incorporation of humanism into psychoanalysis was dragging the field towards self-help, and away from science. Despite his claims of returning to Freud, however, Lacan's theory diverged from traditional psychoanalysis relatively significantly. Inspired by the structuralist movement, Lacan believed that the unconscious was structured like a language and that this "symbolic order" was responsible for the shaping of the self, in place of biological instincts.
Final Comments
The neo-Freudians recognised the inadequacies in Freudian theory in addressing the positive aspects of personality development. They sought to incorporate humanism and existentialism into new forms of psychoanalysis, focusing on self-awareness, personal development, and individual experience, and less on unconscious conflicts.
However, while humanistic and existential forms of therapy are still practiced, psychoanalysis, in general, has become overshadowed by the fields of cognitive psychology, behaviorism, and psychopharmacotherapy. These fields are inherently better equipped to integrate with the scientific method, which has brought them favor over the talk therapy approaches whose effectiveness is more difficult to empirically quantify.
Cognitive-behavioral therapy was introduced in the early 1960s, and the widespread use of antidepressants soon followed. Nevertheless, these new, affordable, forms of treatment are primarily oriented towards symptom reduction, often leaving the underlying issues that contribute towards neurosis unaddressed. Fortunately, there are indications of a resurgence of traditional therapies. The growing interest in mindfulness and meditation is grounded on the same basic principle as many neo-Freudian therapies – the cultivation of self-awareness – and there is ongoing research in the field that will help us to better integrate psychotherapy within the scientific method. | eng | 60472835-cae2-40bb-a7a3-58c1b93f9dd0 | https://www.wonderroot.org/neo-freudians/ |
The Lost Cause Myth: How the South Flipped the American Civil War Story
After the Civil War, Confederate supporters struggled with how they would be remembered. They created a story to justify losing the war, rewriting the facts of history.
Their story was an invention known as the Lost Cause.
October 31, 2023
By Valentine Museum Staff
After the Civil War, Confederate supporters wanted to make sense of the great toll and violence of the war and rebuild the old South by telling a false story about the causes of the war. So, they invented a story that justified the war, known as the Lost Cause.
Promoters of the Lost Cause myth convinced the public that:
The war was fought to protect Southern states' rights, not slavery;
Slavery benefitted both enslaved and enslaver;
The South did not commit treason against the United States.
The term Lost Cause is believed to have first appeared in print in 1866 when Richmond journalist, Edward Pollard, published The Lost Cause: A New Southern History of the War of the Confederates. Since then, these ideas spread through educational textbooks, Confederate monuments and other sources of media that were available everywhere.
"All that is left of the South is the 'war of ideas.'"
—– Edward Pollard , The Lost Cause: A New Southern History of the War of the Confederates, published in Richmond, 1866
Primary sources surrounding the war make it clear: the Lost Cause ideas are a lie. Still, this myth became, and remains, dominant across the nation – not just in the South – for generations. | eng | 6f42fb49-0ca5-4a64-b2c5-55772957d0f8 | https://thevalentine.org/explore/richmond-stories/featured-stories/the-lost-cause-myth-how-the-south-flipped-the-american-civil-war-story/ |
Floriculture is one of the fastest-growing sectors of commercial agriculture world-wide with many highly profitable crops. Cultivation of flowers more pragmatic endeavor than other crops. Every day novel variety, new colour in any ornamental flower crop not only fascinates us but also gives a thrust to know more about their breeding technologies. Creation of diversity of new and domesticated flower crops by public and private sector flower breeders brings a fascination towards its breeding technology. The students while dealing with the breeding and biotechnology of flowers then they must required a base knowledge. Therefore emphasis has been given to present the book in its easiest form so that anyone can understand it without losing interest from it. It has been designed to cover all the aspects of breeding, the basic objectives, different breeding methods, methodology for improvement of specific crops, stress resistance, quality improvement, mutagenesis, genetic engineering | eng | 428e0cc8-cddf-4d3e-aa7d-3236d111a905 | https://www.nipabooks.com/info/9789383305353/breeding-and-biotechnology-of-flowers-vol01-commercial-flowers |
Articla District – Bloggers Unite India
Maryland Fake ID now possible online quickly
The possession and use of fake Maryland IDs carry significant legal, personal, and societal consequences. In this discussion, we will explore the potential legal ramifications, the associated risks, and the broader societal impacts of engaging in such activities.
Legal Consequences: Using or possessing a fake Maryland ID is a criminal offense with serious legal consequences. Maryland law classifies the creation, distribution, or use of fraudulent identification as forgery, which is a felony. Convictions for such offenses can result in substantial fines, probation, community service, and even imprisonment. Moreover, individuals may face additional charges related to identity theft, fraud, and other associated crimes. These legal penalties can lead to a criminal record that impacts an individual's future educational and career opportunities.
Risks and Dangers: The use of fake Maryland Fake ID poses inherent risks and dangers. Individuals attempting to use such IDs to gain access to age-restricted venues, purchase alcohol, or engage in other activities for which they are underage can face rejection, embarrassment, and even confrontations with law enforcement or security personnel. Additionally, businesses and establishments that serve age-restricted products or services are increasingly vigilant in detecting fake IDs, increasing the likelihood of being caught and facing legal consequences.
Impact on Personal and Social Standing: Possessing or using a fake Maryland ID can have adverse effects on an individual's reputation and personal relationships. Friends, family members, and peers may view these actions as irresponsible, dishonest, and potentially damaging to trust. The social consequences can extend to educational environments and professional settings, where a reputation for engaging in dishonest activities can have detrimental effects.
Educational and Professional Implications: A conviction related to fake Maryland IDs can have lasting implications on an individual's educational and professional prospects. Many educational institutions and employers conduct background checks during the application process. Having a criminal record resulting from fake ID-related offenses can raise concerns about an applicant's character and integrity, potentially leading to rejection or missed opportunities.
Societal Trust and Integrity: The use of fake IDs erodes the trust and integrity of official identification systems, contributing to a culture of dishonesty. It fosters an environment where individuals attempt to deceive authorities, businesses, and institutions for personal gain. This erosion of trust can have broader societal implications, affecting areas beyond the mere use of fake IDs.
Law Enforcement Efforts: Maryland's law enforcement agencies are committed to addressing the use of fake IDs. They employ various strategies, including training officers to identify fraudulent identification, collaborating with businesses to share information, and conducting sting operations to catch individuals in the act. These efforts are aimed at deterring individuals from engaging in illegal activities and maintaining the credibility of official identification documents.
In conclusion, the possession and use of fake Maryland IDs come with a range of potential consequences, spanning legal, personal, and societal realms. Legal repercussions can include criminal charges, fines, and a criminal record that affects future opportunities. The risks associated with using fake IDs can lead to embarrassment and confrontations. Additionally, the impact on personal relationships, educational prospects, and professional opportunities can be considerable. On a broader scale, the use of fake IDs damages trust and undermines the integrity of official identification systems, which can have far-reaching implications for societal well-being. It is crucial for individuals to recognize these potential consequences and make responsible choices concerning identification | eng | 1005508d-4748-4638-836e-426e6a0616f3 | https://www.articledistrict.com/maryland-fake-id-now-possible-online-quickly/ |
There are some questions that have an easy answer. Unfortunately, the title of this blog post is not one of them.
Between the complexities of the tax code and the many different ways your insurance policies can be structured, it's impossible to write a thorough break down of what is, and isn't taxable in terms of insurance proceeds that would take less than an hour to read.
However, we can give you an overview of some points that may help clarify a few things about the taxability of your insurance proceeds:
1. Life insurance proceeds can be taxable if the named beneficiary was also a policy owner or if the death benefit is paid to the estate rather than a trust or individual. You can also be taxed if you surrender the policy and the surrender value is more than what you paid in.
2. Auto insurance proceeds are not taxable in most circumstances. However, if your claim allows you to make a gain of some sort, perhaps through pain and suffering payments from an at-fault driver, they may be. You should always ask your agent about your specific claim if you are unsure.
3. Health insurance proceeds are not taxable.
4. Home insurance proceeds, like auto insurance proceeds, are usually not taxable unless they create a gain for you. For example, if you are injured in a neighbor's home, file suit against them, and part of the insurance proceeds are for lost wages, they may be taxable. Again, check with your agent on your specific claim to be sure.
5. Disability insurance benefits are generally not taxable if the premiums were paid with after-tax dollars.
For every type of insurance policy that you can receive proceeds from, there could be a different circumstance or set of rules surrounding the taxability. While you can often figure out your tax liability by determining whether or not you are making a gain from the proceeds, that is an overly simplified way to look at things. So instead, remove the guesswork and give us a call. We can go over any questions you may have about the taxable nature of insurance benefits | eng | 450a5bc3-3641-47f2-bc45-ac3d3c1ed8e6 | https://www.theinsuranceadvisors.net/blog/are_insurance_proceeds_taxable.aspx |
The Role of SOL Casino in the eSports Betting Industry
In recent years, the eSports industry has seen a surge in popularity, attracting millions of passionate fans worldwide. SOL Casino has emerged as a key player in this rapidly growing sector, providing a trusted platform for eSports betting enthusiasts. By offering a wide range of betting options, competitive odds, and state-of-the-art technology, SOL Casino has solidified its role as a prominent name in the eSports betting industry. With its professional approach and dedication to customer satisfaction, SOL Casino continues to shape the future of eSports betting.
The world of online gaming has witnessed a remarkable evolution with the rise of eSports, captivating a global audience of gamers and enthusiasts alike. As this phenomenon grows in popularity, so does the betting industry that surrounds it. In this article, we delve into the significant role played by SOL Casino in the eSports betting industry. As a prominent player in the online gambling sector, SOL Casino has swiftly established itself as a leading platform for eSports betting, providing avid gamers and bettors a safe and reputable environment to engage with their favorite games. With a firm emphasis on professional conduct and immersive gaming experiences, SOL Casino proves to be a key player in embracing the emerging market of eSports betting, catering to the ever-evolving needs of the gaming community.
Role of SOL Casino in the eSports Betting Industry: An Overview
How to Master SEO and Captivate Online Readers with Educational Content
Welcome to the era of digital content, where captivating online readers and increasing visibility on search engine results pages are key. In this article, we will explore the art of crafting educational and SEO-friendly content that resonates with readers and boosts your online presence. Ready to dive in? Let's get started!
The Power of Captivating Content
Imagine scrolling through a webpage and stumbling upon an article that instantly grabs your attention. You're captivated, curious, and eager to learn more. Captivating content is the secret ingredient that keeps readers engaged till the very end. So how do we achieve this?
Use storytelling techniques to present facts and information in an engaging manner.
Adopt a conversational tone that connects with the reader on a personal level.
Inject humor and anecdotes to make the content relatable and memorable.
Leave an Impactful Impression
As we conclude our journey into the world of captivating, educational, and SEO-friendly content, it's essential to leave a lasting impression on our readers. End your article on a hopeful note, inspiring them to take action or delve deeper into the subject. Remember, your words have the power to ignite curiosity and drive change!
Introduction:
In today's fast-paced and demanding world, finding inner peace is becoming increasingly elusive. But what if I told you that the key to tranquility lies within your own mind? Prepare to embark on a transformative journey of mindfulness, unraveling the secrets to attaining serenity and happiness.
Embarking on Your Mindfulness Adventure
Immerse yourself in the awe-inspiring world of mindfulness and make it a lifelong practice. Embrace the beauty of life's moments, big and small, finding solace in the present. Let mindfulness not only be a tool for personal growth but also a means to create a better world.
Conclusion:
In a chaotic world that often pulls us in a thousand different directions, mindfulness offers a path to reclaiming our peace and well-being. Let us take this journey together, unlocking the wonders of mindfulness and opening our hearts to boundless joy and tranquility. The adventure awaits. Embrace it.
The Implications of SOL Casino's Entry into the eSports Betting Industry
Human Impact
However, there is hope. Scientists, conservationists, and policymakers are working together to protect these invaluable ecosystems and promote sustainable practices.
Unveiling the Depths
As we continue to explore and understand the mysteries of the deep sea, each new discovery provides insights into our planet's extraordinary biodiversity. By safeguarding these hidden realms, we preserve a wealth of knowledge and the awe-inspiring beauty of our oceans for generations to come.
So, join us in celebrating the wonders of the deep sea and let's ensure its secrets remain treasures for eternity!
Concluding Remarks
In conclusion, SOL Casino has emerged as a prominent player in the eSports betting industry, providing a highly secure and reliable platform for enthusiasts to engage in this rapidly growing sector. Through an extensive range of betting options, competitive odds, and cutting-edge technology, SOL Casino has successfully carved its niche in the market, capturing the attention of both seasoned bettors and newcomers alike.
As the eSports landscape continues to expand, SOL Casino remains steadfast in its commitment to delivering unparalleled user experience and optimizing opportunities for its customers. By actively engaging with the eSports community and forging strategic partnerships, the platform not only stays at the forefront of industry trends but also fosters an environment of constant innovation.
Furthermore, SOL Casino's dedication to responsible gambling practices is commendable. Through proactive measures such as setting deposit limits and promoting self-exclusion options, the platform ensures that users can enjoy eSports betting in a safe and controlled manner. In a space that can be prone to excess and addiction, SOL Casino sets a benchmark for ethical conduct and customer well-being.
Looking ahead, the future of the eSports betting industry appears promising, with the sector projected to witness exponential growth in the coming years. As an established and trusted name, SOL Casino is poised to capitalize on these opportunities, further cementing its position as a market leader. | eng | 2ddd21b2-ce66-47cc-82c3-7d172b40e902 | https://casinopromoguru.com/gambling-blog/the-role-of-sol-casino-in-the-esports-betting-industry/ |
How the fukk did we get from Shaq making clutch shots to a quote about Kobe's playmaking? That's the fourth or fifth time recently that you quoted me completely out of context and tried to change the topic. You can't follow a conversation for shyt.
Not to mention that's classic psychoanalytic Phil trying to gas Kobe into becoming a playmaker instead of shooting 30 times a game like MJ.
If you want a more relevant Phil Jackson quote, I can quote him at least 2-3 times in 2002 saying that Kobe was shooting the team out of games in the clutch. | eng | 1a5e8230-2ca1-499b-8194-2df2669543ed | https://www.thecoli.com/threads/kobe-was-ridiculous.977891/page-25 |
Learn the Basics of Poker
If you want to learn the rules of poker, then you should start with the basic hands. Straight Flush is the best possible hand in poker, while the second highest hand is the Four of a Kind. You should also know the rules that govern the sharing of money after the game is over. These are important information you should know if you plan on joining a poker game. Below are some useful tips:
Straight Flush is the highest possible hand in poker
In poker, a Straight Flush is the highest possible hand if you have five cards of the same suit. An ace can act as the low card in an ace-to-five straight flush, and a ten-to-ace straight flush also qualifies. However, a straight flush isn't the only poker hand that can reach the royal rank. The royal flush is a much stronger hand than a straight flush in the standard hand rankings, as it consists of two types of straights.
A Straight Flush is a sequence of five cards of the same suit, with the higher card of the same suit being higher than the lowest. Similarly, a straight can be a pair of threes or fours. The lowest straight flush is the H5-H4-H3-H2-HA. It's also possible to have more than one Straight Flush in a single hand.
Four of a Kind is the second highest hand in poker
In poker, Four of a Kind is a hand in which all four cards in a row have the same rank. Although this is a good hand, it is also a minefield. For instance, it's possible to be dealt a Royal Flush when you have Four of a Kind. But let's look at the different types of Four of a Kind hands and how to get the best possible hand with them.
There are six24 possible Four of a Kind hand combinations in a 52-card deck. Of these, 156 different ranks exist. Unlike other hands, the rank of the kicker is not important. Generally, the higher-ranking cards win in this combination. Therefore, it's important to remember that Four of a Kind hands can't beat a Royal Flush. | eng | 36e9118b-7307-455b-80f3-a77522e33b22 | https://pialaadunia2018.games/learn-the-basics-of-poker/ |
Naruto vs Sasuke: Who Would Win?
Wondering who would win between Naruto vs Sasuke? Well, check out here their strengths and abilities to find out who is stronger. Read further to know more.
Naruto is one of the anime that has been running for quite a long time and is an all-time favorite anime for most anime fans.
The storyline of Naruto revolves around the protagonist Naruto Uzumaki who was orphaned when he was just an infant. As Naruto grew up he wanted to become a powerful shinobi and the Hokage of his village, Konohagakure.
Naruto vs Sasuke: Who Would Win?
Naruto is the clear-cut winner between Naruto vs Sasuke as Sasuke has only one arm whereas Naruto has two which makes him stronger. Naruto also has 9 chakra along with other tail chakra beast which makes him way more powerful than Sasuke.
As the storyline progressed new characters were introduced with distinct powers and abilities. Naruto is one of the powerful shinobis who has participated in battles with several other shinobis who were equally powerful like him.
And one such shinobi is Sasuke who's been Naruto's long-time rival in anime and manga. But who's the most powerful? To put this dilemma to rest we've discussed the strengths of both Naruto and Sasuke and how they've battled each other in the anime.
Let's do a comprehensive Naruto vs Sasuke comparison to find out who will actually win. Check it out below.
Naruto Anime and Manga
Naruto was initially released as a Japanese manga that was written by Masashi Kishimoto. The plot focuses on Naruto Uzumaki who's a young ninja living in the village of Konoha who dreams of becoming an invincible shinobi and the Hokage of his village.
The story of Naruto is sectioned into two with the first part focusing on Naruto's early life and the second part which focuses on Naruto's teenage life. The Naruto manga was published between 1999 and 2014.
The manga was adapted into an anime series that was released in 2002. A sequel was made named Naruto: Shippuden which premiered in 2007.
There are 4 seasons in the Naruto anime series with nearly 1000 episodes. The last season of Naruto, Boruto: Naruto Next Generations is focused on Naruto's son Boruto Uzumaki who follows his own path to becoming a ninja instead of his father's.
If you're wondering Who is stronger: Naruto or Sasuke in Boruto, then we have to tell you that it was a close call but Naruto is slightly stronger. Let's find out more about Naruto vs Sasuke
Naruto Uzumaki: An Introduction
Before we get into the debate of who's the strongest out of Naruto and Sasuke, it's best we familiarize ourselves with Naruto and Sasuke's backstory.
When Naruto was an infant, his village was attacked by a powerful mystical fox called the Nine-Tails. The Fourth Hokage of Konoha was Naruto's father, Minato Namikaze. He attempts to seal the fox inside Naruto's body which made Naruto the new host of the beast which would tragically take the life of Minato.
Naruto was frowned upon by the villagers for being the beast's host and he'd only learn about his past when he became a teenager. This would encourage him to become a professional in martial arts and join Team 7 where he meets Sasuke Uchiha and Sakura Haruno.
Source: naruto.fandom.com
Naruto is determined, optimistic, and has an easy-going character which helps him become friends with several other ninjas in his village and outside. Since Naruto was an orphan he became close with Jiraiya who was his godfather who'd teach him different skills and ninja techniques.
Naruto being the protagonist of the anime appears in the anime series, anime films, OVAs, and video games. He also appears in Boruto: Naruto Next Generations where his son Boruto is the protagonist.
Sasuke Uchiha: An Introduction
Now it's time to give a spotlight to Sasuke Uchiha who is Naruto's best friend and foe. Sasuke's past involves a dark and tragic backstory. He's from the Uchiha clan which is one of the most powerful clans and he's one of the surviving members of the clan.
The Uchiha clan's fate was put to an end by Itachi Uchiha who's the older brother of Sasuke. Itachi brutally massacred the Uchiha clan and his parents which is why Sasuke has intense hatred and vengeance towards his brother.
Source: naruto.fandom.com
Sasuke has a very cold personality driven by rage and vengeance which makes him different from the rest of his teammates. Sasuke has the habit of analyzing the strengths of new people he meets.
If he considers any of them weak he'd neglect them and whoever he regards as strong, he'd be too determined to surpass their strengths.
Sasuke eventually leaves Konoha after being manipulated by Orochimaru and losing a battle with Itachi. This would only drive him to a much darker path in search of immense power which Orochimaru is willing to offer him.
Naruto's Strengths and Abilities
When Naruto was a young boy he started off weak like any beginner. He was trained under Iruka Umino in the academy who had a soft spot for Naruto due to his past and would always help him learn new techniques.
After failing three times to graduate from the Academy, Naruto undergoes intense training to make a place for himself. He was initially only able to master the Sexy Technique which wasn't quite useful. Gradually, he was able to master intricate techniques which would aid him to defeat the most invincible shinobis in and outside the village.
Naruto has the ability to reserve tons of chakra powers which would help him to use in battle for nearly 3 days. When activating his chakra powers Naruto would brighten up like the sun and he would rarely get exhausted by them.
Source: naruto.fandom.com
Eventually, Naruto was able to transfer his chakra power to others and also perform hand seals with one hand. Over time Naruto was able to improve his skills in jinchuuriki transformations by accessing Kurama's (Nine-Tail Fox) chakra which made him unstoppable but he was only able to activate it in times of anger.
Besides mystical powers, Naruto had moderate speed, increased stamina, great healing power, and longevity which added more advantages to his set of prowess.
Sasuke's Strengths and Abilities
Sasuke being a member of the Uchiha clan made him one of the powerful shinobis in Konoha. He was born with natural talent and later enhanced his skills to become a renowned shinobi.
During his years in the academy, he was able to surpass Naruto in most of the techniques which is why Naruto considered Sasuke to be his rival. He was able to fight with strong shinobis at a young age which impressed Kakashi Hatake.
After being with Orochimaru, he became much stronger and was able to fight Itachi. Sasuke has a very strong chakra that's dark in color and it's mostly derived from negative energy within him.
Source: naruto.fandom.com
Whenever Sasuke remembers the death of his family his chakra powers grow stronger and darker. He also has the ability to reserve more chakra, however, Naruto's chakra reserves surpass that of Sasuke's.
Unlike Naruto, Sasuke is quite talented in taijutsu, ninjutsu and genjutsu. In addition, Sasuke has more strength, intelligence, stamina, and speed. He can also use five nature transformations and Yin release.
Since Sasuke is from the Uchiha clan he was able to activate the Sharingan which later developed into Rinnegan. The Rinnegan helped him acquire more powers and weaponry during battles.
Naruto vs Sasuke: Who would win?
When discussing each of their powers it's best to put them into a real battle to test who's the most powerful out of them. Hence, we've mentioned the fights that broke out between Naruto and Sasuke and how they both managed to overpower each of them.
Source: naruto.fandom.com
Naruto Ep 107- The Battle Begins: Naruto vs Sasuke- Sasuke challenges Naruto to a battle and Naruto accepts the challenge. They both start exchanging blows nonstop and Naruto eventually would form his Rasengan and Sasuke is prepared to attack Naruto with his Chidori. However, Kakashi interrupts their fight which leads to the result of the battle being inconclusive.
Naruto Ep 128- A Cry on Deaf Ears- During this battle, Naruto repeatedly struck Sasuke but Sasuke didn't get injured. Later on, Sasuke beats Naruto and hits him on the ground. They continue to fight with each other and when Sasuke was unable to counter attack Naruto he activated Cursed Seal Level 2 and successfully defeated Naruto.
Naruto Shippuden Ep 215: Two Fates- This episode portrayed a brief fight between Naruto and Sasuke which didn't last very long and was more of a practice than a real fight.
Naruto Shippuden Ep 257: Meeting- This was only a flashback of Naruto and Sasuke fighting with each other when they were kids where Naruto was inept and Sasuke won all the fights.
Naruto Shippuden Ep 476: The Final Battle- This is the conclusive battle between Naruto and Sasuke and their rivalry comes to an emotional ending. Sasuke accepts his defeat in the battle and admits Naruto is the strongest out of them.
Now that we've discussed their strengths, abilities, and the fights between them, it's best to conclude that Naruto is the strongest shinobi and he would win in a battle against Sasuke. Hope it's clear who will win in Naruto vs Sasuke.
Naruto vs Sasuke: Who Would Win: FAQs
Who wins Naruto vs Sasuke?
After several years of rivalry between the two their final battle in the Naruto Shippuden anime series portrays how they both ended their fight for good. Both Naruto and Sasuke knew they didn't have to kill either of them to prove who's the strongest. Naruto wins the final battle and Sasuke accepts his defeat.
Is Sasuke Uchiha stronger than Naruto?
Sasuke Uchiha is a very talented and competent shinobi with impressive powers. He's quite intelligent and is one of the strongest characters in the Naruto series. Although Sasuke has defeated Naruto in a number of battles, the final battle between them proved that Naruto is stronger than Sasuke.
In which episode is Naruto vs Sasuke?
There have been countless episodes in the Naruto anime series where both Naruto and Sasuke have fought against one another. The most iconic and conclusive battle between them is portrayed in episode 476 in Naruto Shippuden and the fight continues in the next episode as well.
Why do Naruto and Sasuke fight in Shippuden?
Naruto and Sasuke fight each other for several reasons. One of the known reasons they fight is to find out who's the stronger one between them and also to see who's fit to become the next Hokage of Konoha. In the end, Sasuke accepts his defeat and Naruto wins the fight becoming the next Hokage.
Has Sasuke ever won a fight?
Sasuke is one of the strongest characters in Naruto and a talented shinobi in Konoha. He possesses immense strength and countless abilities and he was able to fight some of the most powerful shinobis in the village. He has won a couple of fights against Naruto and other powerful characters in the anime | eng | a0fb40ac-4feb-4188-a032-9b6891135452 | https://japantruly.com/naruto-vs-sasuke/ |
[gnuastro-commits] master dd4d43e 113/113: NoiseChisel and Segment: now working on 3D data cubes
Date:
Fri, 16 Apr 2021 10:34:05 -0400 (EDT)
branch: master
commit dd4d43e5777496271b7e3b68023573f795728a9a
Merge: aa80ac4 89db01d
Author: Mohammad Akhlaghi <mohammad@akhlaghi.org>
Commit: Mohammad Akhlaghi <mohammad@akhlaghi.org>
NoiseChisel and Segment: now working on 3D data cubes
Until now the development of the 3D NoiseChisel and Segment was done in
parallel to the main branch. But the lack of recent commits in those
branches shows that they are now sufficiently mature and ready to be merged
into the master branch.
With this commit, they are now imported into the 'master' branch.
---
.gitignore | 1 +
NEWS | 138 +-
README | 7 +-
THANKS | 3 +
bin/arithmetic/arithmetic.c | 6 +-
bin/arithmetic/operands.c | 5 +-
bin/arithmetic/ui.c | 3 +-
bin/convertt/args.h | 19 +
bin/convertt/main.h | 1 +
bin/convertt/ui.c | 115 +-
bin/convertt/ui.h | 3 +-
bin/convolve/ui.c | 3 +-
bin/cosmiccal/ui.c | 23 +-
bin/crop/ui.c | 9 +-
bin/fits/args.h | 13 +
bin/fits/fits.c | 6 +-
bin/fits/keywords.c | 31 +-
bin/fits/main.h | 2 +
bin/fits/ui.c | 14 +-
bin/fits/ui.h | 1 +
bin/gnuastro.conf | 1 +
bin/mkcatalog/args.h | 14 +
bin/mkcatalog/columns.c | 30 +-
bin/mkcatalog/mkcatalog.c | 336 +-
bin/mkcatalog/mkcatalog.h | 10 +-
bin/mkcatalog/ui.c | 21 +-
bin/mkcatalog/ui.h | 1 +
bin/mkcatalog/upperlimit.c | 212 +-
bin/mkcatalog/upperlimit.h | 4 +-
bin/mknoise/mknoise.c | 3 +-
bin/mknoise/ui.c | 3 +-
bin/mkprof/args.h | 10 +-
bin/mkprof/mkprof.c | 5 +-
bin/mkprof/profiles.c | 10 +-
bin/mkprof/ui.c | 7 +-
bin/noisechisel/ui.c | 3 +-
bin/query/astron.c | 5 +-
bin/query/gaia.c | 3 +
bin/query/main.h | 1 +
bin/query/ned.c | 119 +-
bin/query/query.c | 48 +-
bin/query/ui.c | 67 +-
bin/query/vizier.c | 3 +
bin/script/Makefile.am | 21 +-
bin/script/{make-ds9-reg.in => ds9-region.in} | 68 +-
bin/script/radial-profile.in | 551 +++
bin/segment/ui.c | 6 +-
bin/statistics/statistics.c | 3 +-
bin/statistics/ui.c | 3 +-
bin/table/arithmetic.c | 3 +-
bin/table/table.c | 2 +-
bin/table/ui.c | 2 +-
bin/warp/ui.c | 3 +-
bootstrap.conf | 8 -
configure.ac | 17 +
doc/Makefile.am | 26 +-
doc/announce-acknowledge.txt | 3 +
doc/gnuastro.texi | 5106 +++++++++++++++----------
lib/Makefile.am | 1 +
lib/arithmetic-set.c | 6 +-
lib/arithmetic.c | 26 +-
lib/fits.c | 36 +-
lib/gnuastro-internal/commonopts.h | 16 +-
lib/gnuastro-internal/options.h | 8 +-
lib/gnuastro/arithmetic.h | 10 +-
lib/gnuastro/units.h | 14 +-
lib/gnuastro/wcs.h | 47 +-
lib/options.c | 49 +
lib/txt.c | 5 +
lib/units.c | 45 +
lib/wcs.c | 510 ++-
tests/script/list-by-night.sh | 22 +-
72 files changed, 5260 insertions(+), 2676 deletions(-)
diff --git a/.gitignore b/.gitignore
index 26b30b4..c9bc5d4 100644
--- a/.gitignore
+++ b/.gitignore
@@ -44,6 +44,7 @@
*.log
*.pdf
*.png
+*.swp
*.toc
*.trs
*.txt
diff --git a/NEWS b/NEWS
index a5af946..ceb1926 100644
--- a/NEWS
+++ b/NEWS
@@ -8,20 +8,35 @@ See the end of the file for license conditions.
** New features
New program: For example with the
command below you can select certain rows of a given table, and show
them over an image:
- asttable table.fits --range=MAG,18:20 --column=RA,DEC \
- | astscript-make-ds9-reg --column=1,2 --radius=0.5 \
- --command="ds9 image.fits"
+ asttable table.fits --range=MAGNITUDE,18:20 --column=RA,DEC \
+ | astscript-ds9-region --column=1,2 --radius=0.5 \
+ --+
+ All programs:
+ --wcslinearmatrix: new option in all programs that lets you select the
+ output WCS linear matrix format. It takes one of two values: 'pc' (for
+ the 'PCi_j' formalism) and 'cd' (for 'CDi_j'). Until now, the outputs
+ were always stored in the 'PCi_j' formalism (which is still the
+ recommended format).
+
+ Book:
+ - New "Image surface brightness limit" section added to the third
+ tutorial (on "Detecting large extended targets"). It describes the
+ different ways to measure a dataset's surface brightness limit and
+ upper-limit surface brightness, while discussing their differences.
Arithmetic:
- - New operators (the trigonometric/hyperbolic functions were previously
- only avaialble in Table's column arithmetic, but they have been moved
- into the Gnuastro library and are thus now available on images within
- Arithmetic also):
+ - New operators (all also available in Table's column arithmetic):
- sin: Trigonometric sine (input in degrees).
- cos: Trigonometric cosine (input in degrees).
- tan: Trigonometric tangent (input in degrees).
@@ -33,22 +48,65+ - counts-to-mag: Convert counts to magnitudes with given zero point.
+ - counts-to-jy: Convert counts to Janskys through a zero point based
+ on AB magnitudes.
+
+ ConvertType:
+ --globalhdu: Use a single HDU identifier for all the input files
+ files. Its operation is identical to the similarly named option in
+ Arithmetic. Until now it was necessary to call '--hdu' three times if
+ you had three input FITS files with input in the same HDU.
+
+ Fits:
+ --wcscoordsys: convert the WCS coordinate system of the input into any+ astfits image.fits --wcscoordsys=eq-j2000
+ This option only works with WCSLIB 7.5 and above (released in March
+ 2021), otherwise it will abort with an informative warning.
+
+ MakeCatalog:
+ - Newly added measurement columns:
+ --upperlimitsb: upper-limit surface brightness for the given label
+ (object or clump). This is useful for measuring a dataset's
+ realistic surface brightness level for each labeled region by random
+ positioning of its footprint over undetected regions (not
+ extrapolated from the single-pixel noise level like the "surface
+ brightness limit").
+
+ NoiseChisel:
+ - Can now work on 3D datacubes. Since the configuration parameters are
+ different from images, it is recommended to manually set the 3D
+ configuration (the '...' can be the input image and options):
+ astnoisechisel --config=/usr/local/etc/astnoisechisel-3d.conf ...
+ Alternatively, you can set an 'astnoisechisel-3d' alias like below and
+ always easily run 'astnoisechisel-3d' on cubes.
+ alias astnoisechisel-3d="astnoisechisel
--config=/usr/local/etc/astnoisechisel-3d.conf"
+
+ Segment:
+ - Can now work on 3D datacubes. Similar to NoiseChisel, it requires a
+ separate set of default configurations, so please see the note under
+ NoiseChisel above.57,17 +115,28+
+ Query:+ astquery ned --dataset=extinction --center=49.9507,41.5116
Library:
+ - gal_units_counts_to_mag: Convert counts to magnitudes.
+ - gal_units_counts_to_jy: Convert counts to Janskys.
- New arithmetic operator macros (for the 'gal_arithmetic' function):
- GAL_ARITHMETIC_OP_SIN: sine (input in deg).
- GAL_ARITHMETIC_OP_COS: cosine (input in deg).
@@ -82,6 +151,17 @@ See the end of the file for license conditions.
- GAL_ARITHMETIC_OP_ASINH: Inverse hyperbolic sine.
- GAL_ARITHMETIC_OP_ACOSH: Inverse hyperbolic cosine.
- GAL_ARITHMETIC_OP_ATANH: Inverse hyperbolic tangent.
+ - GAL_ARITHMETIC_OP_COUNTS_TO_JY: Convert counts to Janskys.
+ - WCS coordinate system identifiers:
+ - GAL_WCS_COORDSYS_EQB1950: 1950.0 (Besselian-year) equatorial coords.
+ - GAL_WCS_COORDSYS_EQJ2000: 2000.0 (Julian-year) equatorial coords.
+ - GAL_WCS_COORDSYS_ECB1950: 1950.0 (Besselian-year) ecliptic coords.
+ - GAL_WCS_COORDSYS_ECJ2000: 2000.0 (Julian-year) ecliptic coords.
+ - GAL_WCS_COORDSYS_GALACTIC: Galactic coordinates.
+ - GAL_WCS_COORDSYS_SUPERGALACTIC: Supergalactic coordinates.
+ - gal_wcs_coordsys_from_string: WCS coordinate system from string.
+ - gal_wcs_coordsys_identify: Parse WCS struct to find coordinate system.
+ - gal_wcs_coordsys_convert: Convert the coordinate system of the WCS.
** Removed features
@@ -96,15 +176,31 @@ See the end of the file for license conditions.
9:00a.m. But in some cases, calibration images may be taken after
that. So to be safer in general it was incremented by 2 hours.
+ MakeCatalog:+ keywords (like surface brightness limit numbers above): 'UPNSIGMA',
+ 'UPNUMBER', 'UPRNGNAM', 'UPRNGSEE', 'UPSCMLTP', 'UPSCTOL'.
+
Library:
- gal_fits_key_write_wcsstr: also takes WCS structure as argument.
- gal_fits_key_read_from_ptr: providing a numerical datatype for the
desired keyword's value is no longer mandatory. When not given, the
smallest numeric datatype that can keep the value will be found and
used.
+ - gal_wcs_read: allows specifying the linear matrix of the WCS.
+ - gal_wcs_read_fitsptr: allows specifying the linear matrix of the WCS.
** Bugs fixed
bug #60082: Arithmetic library crash for integer operators like modulo
+ bug #60121: Arithmetic segfault when multi-operand output given to set-
+ bug #60368: CosmicCalculator fails --setdirconf when redshift isn't given
diff --git a/README b/README
index 03b6b93..2b368be 100644
--- a/README
+++ b/README
@@ -109,10 +109,15THANKS b/THANKS
index 6d36246..3ace152 100644
--- a/THANKS
+++ b/THANKS
@@ -41,6 +41,7 @@ support in Gnuastro. The list is ordered alphabetically (by
family name).
Pierre-Alain Duc pierre-alain.duc@astro.unistra.fr
Elham Eftekhari elhamea@iac.es
Paul Eggert eggert@cs.ucla.edu
+ Sepideh Eskandarlou sepideh.eskandarlou@gmail.com
Gaspar Galaz ggalaz@astro.puc.cl
Andrés García-Serra Romero alu0101451923@ull.edu.es
Thérèse Godefroy godef.th@free.fr
@@ -64,6 +65,8 @@ support in Gnuastro. The list is ordered alphabetically (by
family name).
Sebastián Luna Valero sluna@iaa.es
Alberto Madrigal brt.madrigal@gmail.com
Guillaume Mahler guillaume.mahler@univ-lyon1.fr
+ Joseph Mazzarella mazz@ipac.caltech.edu
+ Juan Miro miro.juan@gmail.com
Alireza Molaeinezhad amolaei@gmail.com
Javier Moldon jmoldon@iaa.es
Juan Molina Tobar juan.a.molina.t@gmail.com
diff --git a/bin/arithmetic/arithmetic.c b/bin/arithmetic/arithmetic.c
index 3975a7a..963633f 100644
--- a/bin/arithmetic/arithmetic.c
+++ b/bin/arithmetic/arithmetic.c
@@ -63,8 +63,10 @@ along with Gnuastro. If not, see
<
/***************************************************************/
/************* Internal functions *************/
/***************************************************************/
-#define SET_NUM_OP(CTYPE) { \
- CTYPE a=*(CTYPE *)(numpop->array); if(a>0) return a; }
+#define SET_NUM_OP(CTYPE) { \
+ CTYPE a=*(CTYPE *)(numpop->array); \
+ gal_data_free(numpop); \
+ if(a>0) return a; }
static size_t
pop_number_of_operands(struct arithmeticparams *p, int op, char *token_string,
diff --git a/bin/arithmetic/operands.c b/bin/arithmetic/operands.c
index 1c06500..cb10d3c 100644
--- a/bin/arithmetic/operands.c
+++ b/bin/arithmetic/operands.c
@@ -135,8 +135,9 @@ operands_add(struct arithmeticparams *p, char *filename,
gal_data_t *data)
: NULL);
/* Read the WCS. */
- p->refdata.wcs=gal_wcs_read(filename, newnode->hdu, 0, 0,
- &p->refdata.nwcs);
+ p->refdata.wcs=gal_wcs_read(filename, newnode->hdu,
+ p->cp.wcslinearmatrix,
+ 0, 0, &p->refdata.nwcs);
/* Remove extra (length of 1) dimensions (if we had an
image HDU). */
diff --git a/bin/arithmetic/ui.c b/bin/arithmetic/ui.c
index 93dcbba..5f13635 100644
--- a/bin/arithmetic/ui.c
+++ b/bin/arithmetic/ui.c
@@ -377,7 +377,8 @@ ui_preparations(struct arithmeticparams *p)
dsize=gal_fits_img_info_dim(p->wcsfile, p->wcshdu, &ndim);
/* Read the WCS. */
- p->refdata.wcs=gal_wcs_read(p->wcsfile, p->wcshdu, 0, 0,
+ p->refdata.wcs=gal_wcs_read(p->wcsfile, p->wcshdu,
+ p->cp.wcslinearmatrix, 0, 0,
&p->refdata.nwcs);
if(p->refdata.wcs)
{
diff --git a/bin/convertt/args.h b/bin/convertt/args.h
index 5f66e04..bea65cc 100644
--- a/bin/convertt/args.h
+++ b/bin/convertt/args.h
@@ -30,6 +30,25 @@ along with Gnuastro. If not, see
<
/* Array of acceptable options. */
struct argp_option program_options[] =
{
+ /* Input */
+ {
+ "globalhdu",
+ UI_KEY_GLOBALHDU,
+ "STR/INT",
+ 0,
+ "Use this HDU for all inputs, ignore '--hdu'.",
+ GAL_OPTIONS_GROUP_INPUT,
+ &p->globalhdu+
+
+
+
+
/* Output */
{
"quality",
diff --git a/bin/convertt/main.h b/bin/convertt/main.h
index 0d5cda6..bf1bb9b 100644
--- a/bin/convertt/main.h
+++ b/bin/convertt/main.h
@@ -83,6 +83,7 @@ struct converttparams
struct gal_options_common_params cp; /* Common parameters. */
gal_list_str_t *inputnames; /* The names of input files. */
gal_list_str_t *hdus; /* The names of input hdus. */
+ char *globalhdu; /* Global HDU (for all inputs). */
uint8_t quality; /* Quality of JPEG image. */
float widthincm; /* Width in centimeters. */
uint32_t borderwidth; /* Width of border in PostScript points. */
diff --git a/bin/convertt/ui.c b/bin/convertt/ui.c
index d6e306b..219e39e 100644
--- a/bin/convertt/ui.c
+++ b/bin/convertt/ui.c
@@ -518,17 +518,27 @@ ui_make_channels_ll(struct converttparams *p)
if( gal_fits_name_is_fits(name->v) )
{
/* Get the HDU value for this channel. */
- if(p->hdus)
- hdu=gal_list_str_pop(&p->hdus);
+ if(p->globalhdu)
+ hdu=p->globalhdu;
else
- error(EXIT_FAILURE, 0, "not enough HDUs. Every input FITS image "
- "needs a HDU, you can use the '--hdu' ('-h') option once "
- "for each input FITS image (in the same order)");
+ {
+ if(p->hdus)
+ hdu=gal_list_str_pop(&p->hdus);
+ else
+ error(EXIT_FAILURE, 0, "not enough HDUs. Every input FITS "
+ "image needs a HDU (identified by name or number, "
+ "counting from zero). You can use multiple calls to "
+ "the '--hdu' ('-h') option for each input FITS image "
+ "(in the same order as the input FITS files), or use "
+ "'--globalhdu' ('-g') once when the same HDU should "
+ "be used for all of them");
+ }
/* Read in the array and its WCS information. */
data=gal_fits_img_read(name->v, hdu, p->cp.minmapsize,
p->cp.quietmmap);
- data->wcs=gal_wcs_read(name->v, hdu, 0, 0, &data->nwcs);
+ data->wcs=gal_wcs_read(name->v, hdu, p->cp.wcslinearmatrix,
+ 0, 0, &data->nwcs);
data->ndim=gal_dimension_remove_extra(data->ndim, data->dsize,
data->wcs);
gal_list_data_add(&p->chll, data);
@@ -617,6 +627,97 @@ ui_make_channels_ll(struct converttparams *p)
+static void
+ui_prepare_input_channels_check_wcs(struct converttparams *p)
+{
+ int printwarning=0;
+ float wcsmatch=1.0;
+ gal_data_t *tmp, *coords=NULL;
+ size_t one=1, numwcs=0, numnonblank=0;
+ double *c1, *c2, r1=NAN, r2=NAN, *pixscale=NULL;
+
+ /* If all the inputs have WCS, check to see if the inputs are aligned and
+ print a warning if they aren't. */
+ for(tmp=p->chll; tmp!=NULL; tmp=tmp->next)
+ {
+ if(tmp->wcs && tmp->type!=GAL_TYPE_INVALID) ++numwcs;
+ if(tmp->type!=GAL_TYPE_INVALID) ++numnonblank;
+ }
+ if(numwcs==numnonblank)
+ {
+ /* Allocate the coordinate columns. */
+ /* Go over each image and put its central pixel in the coordinates
+ and do the world-coordinate transformation. Recall that the C
+ coordinates are the inverse order of FITS coordinates and that
+ FITS coordinates count from 1 (not 0).*/
+ for(tmp=p->chll; tmp!=NULL; tmp=tmp->next)
+ if(tmp->wcs)
+ {
+ /* Fill the coordinate values. */
+ c1=coords->array;
+ c2=coords->next->array;
+ c1[0] = tmp->dsize[1] / 2 + 1;
+ c2[0] = tmp->dsize[0] / 2 + 1;
+
+ /* Get the RA/Dec. */
+ gal_wcs_img_to_world(coords, tmp->wcs, 1);
+
+ /* If the pixel scale hasn't been calculated yet, do it (we
+ only need it once, should be similar in all). */
+ if(pixscale==NULL)
+ pixscale=gal_wcs_pixel_scale(tmp->wcs);
+
+ /* If the reference/first center is not yet defined then write
+ the conversions in it. If it is defined, compare with it
+ with the new dataset and print a warning if necessary. */
+ if( isnan(r1) )
+ { r1=c1[0]; r2=c2[0]; }
+ else
+ {
+ /* For a check.
+ printf("check: %g, %g\n", fabs(c1[0]-r1)/pixscale[0],
+ fabs(c2[0]-r2)/pixscale[1]);
+ */
+
+ /* See if a warning should be printed. */
+ if( fabs(c1[0]-r1)/pixscale[0] > wcsmatch
+ || fabs(c2[0]-r2)/pixscale[1] > wcsmatch )
+ printwarning=1;
+ }
+ }
+ }
+
+ /* Print the warning message if necessary. */
+ if(printwarning && p->cp.quiet==0)
+ {
+ error(EXIT_SUCCESS, 0, "WARNING: The WCS information of the input "
+ "FITS images don't match (by more than %g pixels in the "
+ "center), even though the input images have the same number "
+ "of pixels in each dimension. Therefore the color channels "
+ "of the output colored image may not be aligned. If this is "
+ "not a problem, you can suppress this warning with the "
+ "'--quiet' option.\n\n"
+ "A solution to align your images is provided in the "
+ "\"Aligning images with small WCS offsets\" section of "
+ "Gnuastro's manual. Please run the command below to see "
+ "it (you can return to the command-line by pressing 'q'):\n\n"
+ " info gnuastro \"Aligning images\"\n",
+ wcsmatch);
+ }
+
+ /* Clean up. */
+ free(pixscale);
+}
+
+
+
+
+
/* Read the input(s)/channels. */
static void
ui_prepare_input_channels(struct converttparams *p)
@@ -692,6 +793,8 @@ ui_prepare_input_channels(struct converttparams *p)
wcs=tmp->wcs;
}
+ /* Make sure the images are all aligned to the same grid. */
+ ui_prepare_input_channels_check_wcs(p);
/* If ndim is still NULL, then there were no non-blank inputs, so print
an error. */
diff --git a/bin/convertt/ui.h b/bin/convertt/ui.h
index f1deb68..b23e8fb 100644
--- a/bin/convertt/ui.h
+++ b/bin/convertt/ui.h
@@ -42,12 +42,13 @@ enum program_args_groups
/* Available letters for short options:
- a d e f g j k l n p r s t v y z
+ a d e f j k l n p r s t v y z
E G J O Q R W X Y
*/
enum option_keys_enum
{
/* With short-option version. */
+ UI_KEY_GLOBALHDU = 'g',
UI_KEY_QUALITY = 'u',
UI_KEY_WIDTHINCM = 'w',
UI_KEY_BORDERWIDTH = 'b',
diff --git a/bin/convolve/ui.c b/bin/convolve/ui.c
index e466975..2c2582f 100644
--- a/bin/convolve/ui.c
+++ b/bin/convolve/ui.c
@@ -438,7 +438,8 @@ ui_read_input(struct convolveparams *p)
INPUT_USE_TYPE,
p->cp.minmapsize,
p->cp.quietmmap);
- p->input->wcs=gal_wcs_read(p->filename, p->cp.hdu, 0, 0,
+ p->input->wcs=gal_wcs_read(p->filenamecaldiff --git a/bin/crop/ui.c b/bin/crop/ui.c
index a1bc980..8776f15 100644
--- a/bin/crop/ui.c
+++ b/bin/crop/ui.c
@@ -855,8 +855,9 @@ ui_preparations_to_img_mode(struct cropparams *p)
size_t i;
int nwcs;
double *darr, *pixscale;
- struct wcsprm *wcs=gal_wcs_read(p->inputs->v, p->cp.hdu, p->hstartwcs,
- p->hendwcs, &nwcs);
+ struct wcsprm *wcs=gal_wcs_read(p->inputs->v, p->cp.hdu,
+ p->cp.wcslinearmatrix,
+ p->hstartwcs, p->hendwcs, &nwcs);
/* Make sure a WCS actually exists. */
if(wcs==NULL)
@@ -1018,8 +1019,8 @@ ui_preparations(struct cropparams *p)
tmpfits=gal_fits_hdu_open_format(img->name, p->cp.hdu, 0);
gal_fits_img_info(tmpfits, &p->type, &img->ndim, &img->dsize,
NULL, NULL);
- img->wcs=gal_wcs_read_fitsptr(tmpfits, p->hstartwcs, p->hendwcs,
- &img->nwcs);
+ img->wcs=gal_wcs_read_fitsptr(tmpfits, p->cp.wcslinearmatrix,
+ p->hstartwcs, p->hendwcs, &img->nwcs);
if(img->wcs)
{
gal_wcs_decompose_pc_cdelt(img->wcs);
diff --git a/bin/fits/args.h b/bin/fits/args.h
index af1d90c..ffe56a9 100644
--- a/bin/fits/args.h
+++ b/bin/fits/args.h
@@ -341,6 +341,19 @@ struct argp_option program_options[] =
GAL_OPTIONS_NOT_MANDATORY,
GAL_OPTIONS_NOT_SET
},
+ {
+ "wcscoordsys",
+ UI_KEY_WCSCOORDSYS,
+ "STR",
+ 0,
+ "Convert WCS coordinate system.",
+ UI_GROUP_KEYWORD,
+ &p->wcscoordsysdiff --git a/bin/fits/fits.c b/bin/fits/fits.c
index 19a7a1b..718d50c 100644
--- a/bin/fits/fits.c
+++ b/bin/fits/fits.c
@@ -323,7 +323,8 @@ fits_pixelscale(struct fitsparams *p)
double multip, *pixelscale;
/* Read the desired WCS/* If a WCS doesn't exist, let the user know and return. */
if(wcs)
@@ -474,7 +475,8 @@ fits_skycoverage(struct fitsparams *p)
}
/* For the range type of coverageprintf("\nSky coverage by range along dimensions:\n");
for(i=0;i<ndim;++i)
printf(" %-8s %-15.10g%-15.10g\n", gal_wcs_dimension_name(wcs, i),
diff --git a/bin/fits/keywords.c b/bin/fits/keywords.c
index 9a325f6..4a1d483 100644
--- a/bin/fits/keywords.c
+++ b/bin/fits/keywords.c
@@ -438,7 +438,7 @@ keywords_date_to_seconds(struct fitsparams *p, fitsfile
*fptr)
static void
-keywords_distortion_wcs(struct fitsparams *p)
+keywords_wcs_convert(struct fitsparams *p)
{
int nwcs;
size_t ndim, *insize;
@@ -463,16 +463,17 @@ keywords_distortion_wcs(struct fitsparams *p)
}
/* Read the input's WCS and make sure one exists. */
- inwcs=gal_wcs_read(p->input->v, p->cp.hdu, 0, 0, &nwcs);
+ inwcs=gal_wcs_read(p->input->v, p->cp.hdu, p->cp.wcslinearmatrix,
+ 0, 0, &nwcs);
if(inwcs==NULL)
error(EXIT_FAILURE, 0, "%s (hdu %s): doesn't have any WCS structure "
- "for converting its distortion",
+ "for converting its coordinate system or distortion",
p->input->v, p->cp.hdu);
/* In case there is no dataset and the conversion is between TPV to SIP,
we need to set a default size and use that for the conversion, but we
also need to warn the user. */
- if(data==NULL)
+ if(p->wcsdistortion && data==NULL)
{
if( !p->cp.quiet
&& gal_wcs_distortion_identify(inwcs)==GAL_WCS_DISTORTION_TPV
@@ -491,14 +492,22 @@ keywords_distortion_wcs(struct fitsparams *p)
else dsize=data->dsize;
/* Do the conversion. */
- outwcs=gal_wcs_distortion_convert(inwcs, p->distortionid, dsize);
+ if(p->wcscoordsys)
+ outwcs=gal_wcs_coordsys_convert(inwcs, p->coordsysid);
+ else if(p->wcsdistortion)
+ outwcs=gal_wcs_distortion_convert(inwcs, p->distortionid, dsize);
+ else
+ error(EXIT_FAILURE, 0, "%s: a bug! Please contact us at %s to fix "
+ "the problem. The requested mode for this function is not "
+ "recognized", __func__, PACKAGE_BUGREPORT);
/* Set the output filename. */
if(p->cp.output)
output=p->cp.output;
else
{
- if( asprintf(&suffix, "-%s.fits", p->wcsdistortion)<0 )
+ if( asprintf(&suffix, "-%s.fits",
+ p->wcsdistortion ? p->wcsdistortion : p->wcscoordsys)<0 )
error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
output=gal_checkset_automatic_output(&p->cp, p->input->v, suffix);
}
@@ -781,10 +790,10 @@ keywords_value(struct fitsparams *p)
size_t i, ii=0, ninput, nkeys;
gal_data_t *out=NULL, *keysll=NULL;
- /* Count how many inputs there are and allocate the first column with the
- name. */
+ /* Count how many inputs there are, and allocate the first column with
+ the name. */
ninput=gal_list_str_number(p->input);
- if(ninput>1)
+ if(ninput>1 || p->cp.quiet==0)
out=gal_data_alloc(NULL, GAL_TYPE_STRING, 1, &ninput, NULL, 0,
p->cp.minmapsize, p->cp.quietmmap, "FILENAME",
"name", "Name of input file.");
@@ -1034,8 +1043,8 @@ keywords(struct fitsparams *p)
}
/* Convert the input's distortion to the desired output distortion. */
- if(p->wcsdistortion)
- keywords_distortion_wcs(p);
+ if(p->wcsdistortion || p->wcscoordsys)
+ keywords_wcs_convert(p);
/* Return. */
return r;
diff --git a/bin/fits/main.h b/bin/fits/main.h
index 9c66221..c0254c2 100644
--- a/bin/fits/main.h
+++ b/bin/fits/main.h
@@ -78,12 +78,14 @@ struct fitsparams
uint8_t *verify; /* Verify the CHECKSUM and DATASUM keys. */
char *copykeys; /* Range of keywords to copy in output. */
char *datetosec; /* Convert FITS date to seconds. */
+ char *wcscoordsys; /* Name of new WCS coordinate system. */
char *wcsdistortion; /* WCS distortion to write in output. */
uint8_t quitonerror; /* Quit if an error occurs. */
uint8_t colinfoinstdout; /* Print column info in output. */
/* Internal: */
int mode; /* Operating on HDUs or keywords. */
+ int coordsysid; /* ID of desired coordinate system.*/
int distortionid; /* ID of desired distortion. */
long copykeysrange[2]; /* Start and end of copy. */
gal_fits_list_key_t *write_keys; /* Keys to write in the header. */
diff --git a/bin/fits/ui.c b/bin/fits/ui.c
index c9cbc63..b8e9436 100644
--- a/bin/fits/ui.c
+++ b/bin/fits/ui.c
@@ -120,6 +120,7 @@ ui_initialize_options(struct fitsparams *p,
case GAL_OPTIONS_KEY_SEARCHIN:
case GAL_OPTIONS_KEY_IGNORECASE:
case GAL_OPTIONS_KEY_TYPE:
+ case GAL_OPTIONS_KEY_WCSLINEARMATRIX:
case GAL_OPTIONS_KEY_DONTDELETE:
case GAL_OPTIONS_KEY_LOG:
case GAL_OPTIONS_KEY_NUMTHREADS:
@@ -324,7 +325,7 @@ ui_read_check_only_options(struct fitsparams *p)
if( p->date || p->comment || p->history || p->asis || p->keyvalue
|| p->delete || p->rename || p->update || p->write || p->verify
|| p->printallkeys || p->copykeys || p->datetosec
- || p->wcsdistortion )
+ || p->wcscoordsys || p->wcsdistortion )
{
/* Check if a HDU is given. */
if(p->cp.hdu==NULL)
@@ -339,15 +340,20 @@ ui_read_check_only_options(struct fitsparams *p)
/* Keyword-related options that must be called alone. */
checkkeys = ( (p->keyvalue!=NULL)
+ (p->datetosec!=NULL)
+ + (p->wcscoordsys!=NULL)
+ (p->wcsdistortion!=NULL) );
if( ( checkkeys
&& ( p->date || p->comment || p->history || p->asis
|| p->delete || p->rename || p->update || p->write
|| p->verify || p->printallkeys || p->copykeys ) )
|| checkkeys>1 )
- error(EXIT_FAILURE, 0, "'--keyvalue', '--datetosec' and "
- "'--wcsdistortion' cannot currently be called with "
- "any other option");
+ error(EXIT_FAILURE, 0, "'--keyvalue', '--datetosec', "
+ "'--wcscoordsys' and '--wcsdistortion' cannot "
+ "currently be called with any other option");
+
+ /* Give an ID to recognized coordinate systems. */
+ if(p->wcscoordsys)
+ p->coordsysid=gal_wcs_coordsys_from_string(p->wcscoordsys);
/* Identify the requested distortion. Note that this also acts as a
sanity check because it will crash with an error if the given
diff --git a/bin/fits/ui.h b/bin/fits/ui.h
index 4ee5333..61f70af 100644
--- a/bin/fits/ui.h
+++ b/bin/fits/ui.h
@@ -77,6 +77,7 @@ enum option_keys_enum
UI_KEY_SKYCOVERAGE,
UI_KEY_OUTHDU,
UI_KEY_COPYKEYS,
+ UI_KEY_WCSCOORDSYS,
UI_KEY_PRIMARYIMGHDU,
UI_KEY_WCSDISTORTION,
};
diff --git a/bin/gnuastro.conf b/bin/gnuastro.conf
index 6c180c0..a93d7cb 100644
--- a/bin/gnuastro.conf
+++ b/bin/gnuastro.conf
@@ -36,6 +36,7 @@
# Output:
tableformat fits-binary
+ wcslinearmatrix pc
# Operating mode
quietmmap 0
diff --git a/bin/mkcatalog/args.h b/bin/mkcatalog/args.h
index 6582d38..a1c18c6 100644
--- a/bin/mkcatalog/args.h
+++ b/bin/mkcatalog/args.h
@@ -1229,6 +1229,20 @@ struct argp_option program_options[] =
ui_column_codes_ll
},
{
+ "upperlimitsb",
+ UI_KEY_UPPERLIMITSB,
+ 0,
+ 0,
+ "Upper-limit surface brightness (mag/arcsec^2).",upperlimitonesigma",
UI_KEY_UPPERLIMITONESIGMA,
0,
diff --git a/bin/mkcatalog/columns.c b/bin/mkcatalog/columns.c
index e94bb79..e7340c7 100644
--- a/bin/mkcatalog/columns.c
+++ b/bin/mkcatalog/columns.c
@@ -31,6 +31,7 @@ along with Gnuastro. If not, see
<
#include <pthread.h>
#include <gnuastro/wcs.h>
+#include <gnuastro/units.h>
#include <gnuastro/pointer.h>
#include <gnuastro-internal/checkset.h>
@@ -257,6 +258,7 @@ columns_wcs_preparation(struct mkcatalogparams *p)
case UI_KEY_HALFMAXSB:
case UI_KEY_HALFSUMSB:
case UI_KEY_AREAARCSEC2:
+ case UI_KEY_UPPERLIMITSB:
case UI_KEY_SURFACEBRIGHTNESS:
pixscale=gal_wcs_pixel_scale(p->objects->wcs);
p->pixelarcsecsq=pixscale[0]*pixscale[1]*3600.0f*3600.0f;
@@ -1415,6 +1417,22 @@ columns_define_alloc(struct mkcatalogparams *p)
oiflag[ OCOL_UPPERLIMIT_B ] = ciflag[ CCOL_UPPERLIMIT_B ] = 1;
break;
+ case UI_KEY_UPPERLIMITSB:
+ name = "UPPERLIMIT_SB";
+ unit = "mag/arcsec^2";
+ ocomment = "Upper limit surface brightness over its
footprint.";
+ ccomment = ocomment;
+ otype = GAL_TYPE_FLOAT32;
+ ctype = GAL_TYPE_FLOAT32;
+ disp_fmt = GAL_TABLE_DISPLAY_FMT_FLOAT;
+ disp_width = 8;
+ disp_precision = 3;
+ p->hasmag = 1;
+ p->upperlimit = 1;
+ oiflag[ OCOL_NUMALL ] = ciflag[ CCOL_NUMALL ] = 1;
+ oiflag[ OCOL_UPPERLIMIT_B ] = ciflag[ CCOL_UPPERLIMIT_B ] = 1;
+ break;
+
case UI_KEY_UPPERLIMITONESIGMA:
name = "UPPERLIMIT_ONE_SIGMA";
unit = MKCATALOG_NO_UNIT;
@@ -1995,7 +2013,7 @@ columns_define_alloc(struct mkcatalogparams *p)
/********** Column calculation ***************/
/******************************************************************/
#define MKC_RATIO(TOP,BOT) ( (BOT)!=0.0f ? (TOP)/(BOT) : NAN )
-#define MKC_MAG(B) ( ((B)>0) ? -2.5f * log10(B) + p->zeropoint : NAN )
+#define MKC_MAG(B) ( gal_units_counts_to_mag(B, p->zeropoint) )
#define MKC_SB(B, A) ( ((B)>0 && (A)>0) \
? MKC_MAG(B) + 2.5f * log10((A) * p->pixelarcsecsq) \
: NAN )
@@ -2544,6 +2562,11 @@ columns_fill(struct mkcatalog_passparams *pp)
((float *)colarr)[oind] = MKC_MAG(oi[ OCOL_UPPERLIMIT_B ]);
break;
+ case UI_KEY_UPPERLIMITSB:
+ ((float *)colarr)[oind] = MKC_SB( oi[ OCOL_UPPERLIMIT_B ],
+ oi[ OCOL_NUMALL ] );
+ break;
+
case UI_KEY_UPPERLIMITONESIGMA:
((float *)colarr)[oind] = oi[ OCOL_UPPERLIMIT_S ];
break;
@@ -2888,6 +2911,11 @@ columns_fill(struct mkcatalog_passparams *pp)
((float *)colarr)[cind] = MKC_MAG(ci[ CCOL_UPPERLIMIT_B ]);
break;
+ case UI_KEY_UPPERLIMITSB:
+ ((float *)colarr)[cind] = MKC_SB( ci[ CCOL_UPPERLIMIT_B ],
+ ci[ CCOL_NUMALL ] );
+ break;
+
case UI_KEY_UPPERLIMITONESIGMA:
((float *)colarr)[cind] = ci[ CCOL_UPPERLIMIT_S ];
break;
diff --git a/bin/mkcatalog/mkcatalog.c b/bin/mkcatalog/mkcatalog.c
index e3e75b7..18f5a2d 100644
--- a/bin/mkcatalog/mkcatalog.c
+++ b/bin/mkcatalog/mkcatalog.c
@@ -35,6 +35,7 @@ along with Gnuastro. If not, see
<
#include <gnuastro/wcs.h>
#include <gnuastro/data337,86 +338,92 @@ mkcatalog_wcs_conversion(struct mkcatalogparams *p)
void
-mkcatalog_write_inputs_in_comments(struct mkcatalogparams *p,
- gal_list_str_t **comments, int withsky,
- int withstd))
{
- char *tmp, *str;
+ void *value;
+ value=gal_pointer_allocate(type, 1, 0, __func__, "value");
+ memcpy(value, number, gal_type_sizeof(type));
+ gal_fits_key_list_add_end(keylist, type, nameliteral, 0,
+ value, 1, commentliteral, 0,
+ unitliteral, 0);
+}
+
+
- /* Basic classifiers for plain text outputs. */
- if(p->cp.tableformat==GAL_TABLE_FORMAT_TXT)
- {
- if( asprintf(&str, "--------- Input files ---------")<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(comments, str, 0);
- }
+
+
+void
+mkcatalog_outputs_keys_infiles(struct mkcatalogparams *p,
+ gal_fits_list_key_t **keylist)
+{
+ char *stdname, *stdhdu, *stdvalcom;
+
+ gal_fits_key_list_title_add_end(keylist,
+ "Input files and/or configuration", 0);
/* Object labels. */
- if( asprintf(&str, "Objects: %s (hdu: %s).", p->objectsfile, p->cp.LAB", p->objectsfile, keylist, 0);
+ gal_fits_key_write_filename("INLABHDU", p->cp.hdu, keylist, 0);
/* Clump labels. */
if(p->clumps)
{
- if(asprintf(&str, "Clumps: %s (hdu: %s).", p->usedclumpsfile,
- p->clumpshdu)<0)CLU", p->usedclumpsfile, keylist, 0);
+ gal_fits_key_write_filename("INCLUHDU", p->clumpshdu, keylist, 0);
}
- /* Values dataset. */
+ /* Values image. */
if(p->values)
{
- if( asprintf(&str, "Values: %s (hdu: %s).", p->usedvaluesfile,
- p->valuesVAL", p->usedvaluesfile, keylist, 0);
+ gal_fits_key_write_filename("INVALHDU", p->valueshdu, keylist, 0);
}
- /* Sky dataset. */
- if(withsky && p->sky)
+ /* Sky image/value. */
+ if(p->sky)
{
if(p->sky->size==1)
- {
- if( asprintf(&str, "Sky: %g.", *((float *)(p->skysky->array,
+ p->sky->type, "INSKYVAL",
+ "Value of Sky used (a single number).",
+ NULL);
else
{
- if( asprintf(&str, "Sky: %s (hdu: %s).", p->usedskyfile,
- p->skyhdu)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
+ gal_fits_key_write_filename("INSKY", p->usedskyfile, keylist, 0);
+ gal_fits_key_write_filename("INSKYHDU", p->skyhdu, keylist, 0);
}
- gal_list_str_add(comments, str, 0);
}
- /* Sky standard deviation dataset. */
- tmp = p->variance ? "VAR" : "STD";
- if(withstd && p->std)
+ /* Standard deviation (or variance) image. */
+ if(p->variance)
+ {
+ stdname="INVAR"; stdhdu="INVARHDU";
+ stdvalcom="Value of Sky variance (a single number).";
+ }
+ else
+ {
+ stdname="INSTD"; stdhdu="INSTDHDU";
+ stdvalcom="Value of Sky STD (a single number).";
+ }
+ if(p->std)
{
if(p->std->size==1)
- {
- if( asprintf(&str, "Sky %s: %g.", tmp,
- *((float *)(p->stdstd->array, p->std->type,
+ stdname, stdvalcom, NULL);
else
{
- if( asprintf(&str, "Sky %s: %s (hdu: %s).", tmp, p->usedstdfile,
- p->stdhdu)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
+ gal_fits_key_write_filename(stdname, p->usedstdfile, keylist, 0);
+ gal_fits_key_write_filename(stdhdu, p->stdhdu, keylist, 0);
}
- gal_list_str_add(comments, str, 0);
}
/* Upper limit mask. */
if(p->upmaskfile)
{
- if( asprintf(&str, "Upperlimit mask: %s (hdu: %s).", p->upmaskfile,
- p->upmaskUPM", p->upmaskfile, keylist, 0);
+ gal_fits_key_write_filename("INUPMHDU", p->upmaskhdu, keylist, 0);
}
}
@@ -424,166 +431,148 @@ mkcatalog_write_inputs_in_comments(struct
mkcatalogparams *p,
-/* Write the similar information. */
-static gal_list_str_t *
-mkcatalog_outputs_same_start(struct mkcatalogparams *p, int o0c1,
- char *ObjClump)
+/* Write the output keywords. */
+static gal_fits_list_key_t *
+mkcatalog_outputs_keys(struct mkcatalogparams *p, int o0c1)
{
- char *str, *tstr;
- double pixarea=NAN;
- gal_list_str_t *comments=NULL;
-
- if( asprintf(&str, "%s catalog of %s", o0c1 ? "Object" : "Clump",
- PROGRAM_STRING)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(&comments, str, 0);
-
- /* If in a Git controlled directory and output isn't a FITS file (in
- FITS, this will be automatically included). */
- if(p->cp.tableformat==GAL_TABLE_FORMAT_TXT && gal_git_describe())
- {
- if(asprintf(&str, "Working directory commit %s", gal_git_describe())<0)
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(&comments, str, 0);
- }
-
- /* Write the date. However, 'ctime' is going to put a new-line character
- in the end of its string, so we are going to remove it manually. */
- if( asprintf(&str, "%s started on %s", PROGRAM_NAME, ctime(&p->rawtime))<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- str[strlen(str)-1]='\0';
- gal_list_str_add(&comments, str, 0);
+ float pixarea=NAN, fvalue;
+ gal_fits_list_key_t *keylist=NULL;
+ /* First, add the file names. */
+ mkcatalog_outputs_keys_infiles(p, &keylist);
- /* Write the basic information. */
- mkcatalog_write_inputs_in_comments(p, &comments, 1, 1);
+ /* Type of catalog. */
+ gal_fits_key_list_add_end(&keylist, GAL_TYPE_STRING, "CATTYPE", 0,
+ o0c1 ? "clumps" : "objects", 0,
+ "Type of catalog ('object' or 'clump').", 0,
+ NULL, 0);
-
- /* Write other supplementary information. */
- if(p->cp.tableformat==GAL_TABLE_FORMAT_TXT)
- {
- if( asprintf(&str, "--------- Supplementary information /* Add project commit information when in a Git-controlled directory and
+ the output isn't a FITS file (in FITS, this will be automatically
+ included). */
+ if(p->cp.tableformat==GAL_TABLE_FORMAT_TXT && gal_git_describe())
+ gal_fits_key_list_add_end(&keylist, GAL_TYPE_STRING, "COMMIT", 0,
+ gal_git_describe(), 1,
+ "Git commit in running directory.", 0,
+ NULL, 0);
/* Pixel area. */
if(p->objects->wcs)
{
pixarea=gal_wcs_pixel_area_arcsec2(p->objects->wcs);
if( isnan(pixarea)==0 )
- {
- if( asprintf(&str, "Pixel area (arcsec^2): %g", pixareaixarea,
+ GAL_TYPE_FLOAT32, "PIXAREA",
+ "Pixel area of input image.",
+ "arcsec^2");
}
- /* Zeropoint magnitude */
- if(p->hasmag)
- {
- if( asprintf(&str, "Zeropoint magnitude: %.4f", p->zeropoint)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(&comments, str, 0);
- }
+ /* Zeropoint magnitude. */
+ if( !isnan(p->zeropoint) )
+ mkcatalog_outputs_keys_numeric(&keylist, &p->zeropoint,
+ GAL_TYPE_FLOAT32, "ZEROPNT",
+ "Zeropoint used for magnitude.",
+ "mag");
- /* Print surface brightness limits. */
+ /* Add the title for the keywords. */
+ gal_fits_key_list_title_add_end(&keylist, "Surface brightness limit (SBL)",
0);
+
+ /* Print surface brightness limit. */
if( !isnan(p->medstd) && !isnan(p->sfmagnsigma) )
{
+ /* Used noise value (per pixel) and multiple of sigma. */
+ mkcatalog_outputs_keys_numeric(&keylist, &p->medstd,
+ GAL_TYPE_FLOAT32, "SBLSTD",
+ "Pixel STD for surface brightness limit.",
+ NULL);
+ mkcatalog_outputs_keys_numeric(&keylist, &p->sfmagnsigma,
+ GAL_TYPE_FLOAT32, "SBLNSIG",
+ "Sigma multiple for surface brightness "
+ "limit.", NULL);
+
/* Only print magnitudes if a zeropoint is given. */
if( !isnan(p->zeropoint) )
{
- /* Per pixel. */
- if( asprintf(&str, "%g sigma surface brightness (magnitude/pixel): "
- "%.3f", p->sfmagnsigma, ( -2.5f
- *log10( p->sfmagnsigma
- * p->medstd )
- + p->zeropoint ) )<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(&comments, str, 0);
-
- /* Requested projected area: if a pixel area could be measured (a
- WCS was given), then also estimate the surface brightness over
- one arcsecond^2. From the pixel area, we know how many pixels
- are necessary to fill the requested projected area (in
- arcsecond^2). We also know that as the number of samples
- (pixels) increases (to N), the noise increases by sqrt(N), see
- the full discussion in the book. */
- if(!isnan(pixarea) && !isnan(p->sfmagarea))
+ /* Per pixel, Surface brightness limit magnitude. */
+ fvalue=gal_units_counts_to_mag(p->sfmagnsigma * p->medstd,
+ p->zeropoint);
+ mkcatalog_outputs_keys_numeric(&keylist, &fvalue,
+ GAL_TYPE_FLOAT32, "SBLMAGPX",
+ "Surface brightness limit per pixel.",
+ "mag/pix");
+
+ /* Only print the SBL in fixed area if a WCS is present and a
+ pixel area could be deduced. */
+ if( !isnan(pixarea) )
{
- /* Prepare the comment/information. */
- if(p->sfmagarea==1.0f)
- tstr=NULL;
- else
- if( asprintf(&tstr, "%g-", p->sfmagarea)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- if( asprintf(&str, "%g sigma surface brightness "
- "(magnitude/%sarcsec^2): %.3f", p->sfmagnsigma,
- tstr ? tstr : "",
- ( -2.5f * log10( p->sfmagnsigma
- * p->medstd
- * sqrt( p->sfmagarea / pixarea) )
- + p->zeropoint ) )<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
-
- /* Add the final string/line to the catalog comments. */
- gal_list_str_add(&comments, str, 0);
-
- /* Clean up (if necessary). */
- if (tstr)
- {
- free(tstr);
- tstr=NULL;
- }
+ /* Area used for measuring SBL. */
+ mkcatalog_outputs_keys_numeric(&keylist, &p->sfmagarea,
+ GAL_TYPE_FLOAT32, "SBLAREA",
+ "Area for surface brightness "
+ "limit.", "arcsec^2");
+
+ /* Per area, Surface brightness limit magnitude. */
+ fvalue=gal_units_counts_to_mag(p->sfmagnsigma
+ * p->medstd
+ / sqrt( p->sfmagarea
+ * pixarea),
+ p->zeropoint);
+ mkcatalog_outputs_keys_numeric(&keylist, &fvalue,
+ GAL_TYPE_FLOAT32, "SBLMAG",
+ "Surf. bright. limit in SBLAREA.",
+ "mag/arcsec^2");
}
+ else
+ gal_fits_key_list_fullcomment_add_end(&keylist, "Can't "
+ "write surface brightness limiting magnitude (SBLM) "
+ "values in fixed area ('SBLAREA' and 'SBLMAG' "
+ "keywords) because input doesn't have a world "
+ "coordinate system (WCS), or the first two "
+ "coordinates of the WCS weren't angular positions "
+ "in units of degrees.", 0);
}
-
- /* Notice: */
- if( asprintf(&str, "Pixel STD for surface brightness calculation%s: %f",
- (!isnan(pixarea) && !isnan(p->sfmagarea))?"s":"",
- p->medstd)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(&comments, str, 0);
+ else
+ gal_fits_key_list_fullcomment_add_end(&keylist, "Can't write "
+ "surface brightness limiting magnitude values (e.g., "
+ "'SBLMAG' or 'SBLMAGPX' keywords) because no "
+ "'--zeropoint' has been given.", 0);
}
else
{
- gal_checkset_allocate_copy("No surface brightness calcuations "
- "because no STD image used.", &str);
- gal_list_str_add(&comments, str, 0);
- gal_checkset_allocate_copy("Ask for column that uses the STD image, "
- "or '--forcereadstd'.", &str);
- gal_list_str_add(&comments, str, 0);
+ gal_fits_key_list_fullcomment_add_end(&keylist, "No surface "
+ "brightness calcuations (e.g., 'SBLMAG' or 'SBLMAGPX' "
+ "keywords) because STD image didn't have the 'MEDSTD' "
+ "keyword. There are two solutions: 1) Call with "
+ "'--forcereadstd'. 2) Measure the median noise level "
+ "manually (possibly with Gnuastro's Arithmetic program) "
+ "and put the value in the 'MEDSTD' keyword of the STD "
+ "image.", 0);
+ gal_fits_key_list_fullcomment_add_end(&keylist, "", 0);
}
/* The count-per-second correction. */
if(p->cpscorr>1.0f)
- {
- if( asprintf(&str, "Counts-per-second correction: %.3f", p->cpscorr->cpscorr,
+ GAL_TYPE_FLOAT32, "CPSCORR",
+ "Counts-per-second correction.",
+ NULL);
/* Print upper-limit parameters. */
if(p->upperlimit)
- upperlimit_write_comments(p, &comments, 1);
+ upperlimit_write_keys(p, &keylist, 1);
- /* Start column metadata. */
+ /* In plain-text outputs, put a title for column metadata. */
if(p->cp.tableformat==GAL_TABLE_FORMAT_TXT)
- {
- if( asprintf(&str, "--------- Table columns gal_fits_key_list_title_add_end(&keylist, "Column metadata", 0);
- /* Return the comments. */
- return comments;
+ /* Return the list of keywords. */
+ return keylist;
}
-
/* Since all the measurements were done in parallel (and we didn't know the
number of clumps per object a-priori), the clumps informtion is just
written in as they are measured. Here, we'll sort the clump columns by
@@ -646,19 +635,20 @@ mkcatalog_write_outputs(struct mkcatalogparams *p)
{
size_t i, scounter;
char str[200], *fname;
- gal_list_str_t *comments;
+ gal_fits_list_key_t *keylist;
+ gal_list_str_t *comments=NULL;
int outisfits=gal_fits_name_is_fits(p->objectsout);
/* If a catalog is to be generated. */
if(p->objectcols)
{
/* OBJECT catalog */
- comments=mkcatalog_outputs_same_start(p, 0, "Detection");
+ keylist=mkcatalog_outputs_keys(p, 0);
/* Reverse the comments list (so it is printed in the same order
here), write the objects catalog and free the comments. */
gal_list_str_reverse(&comments);
- gal_table_write(p->objectcols, NULL, comments, p->cp.tableformat,
+ gal_table_write(p->objectcols, &keylist, NULL, p->cp.tableformat,
p->objectsout, "OBJECTS", 0);
gal_list_str_free(comments, 1);
@@ -667,7 +657,7 @@ mkcatalog_write_outputs(struct mkcatalogparams *p)
if(p->clumps)
{
/* Make the comments. */
- comments=mkcatalog_outputs_same_start(p, 1, "Clumps");
+ keylist=mkcatalog_outputs_keys(p, 1);
/* Write objects catalog
---------------------
diff --git a/bin/mkcatalog/mkcatalog.h b/bin/mkcatalog/mkcatalog.h
index 9cbdbd8..75e9c7a 100644
--- a/bin/mkcatalog/mkcatalog.h
+++ b/bin/mkcatalog/mkcatalog.h
@@ -45,9 +45,13 @@ struct mkcatalog_passparams
};
void
-mkcatalog_write_inputs_in_comments(struct mkcatalogparams *p,
- gal_list_str_t **comments, int withsky,
- int withstd););
+
+void
+mkcatalog_outputs_keys_infiles(struct mkcatalogparams *p,
+ gal_fits_list_key_t **keylist);
void
mkcatalog(struct mkcatalogparams *p);
diff --git a/bin/mkcatalog/ui.c b/bin/mkcatalog/ui.c
index 37bef56..aa88388 100644
--- a/bin/mkcatalog/ui.c
+++ b/bin/mkcatalog/ui.c
@@ -538,7 +538,8 @@ ui_wcs_info(struct mkcatalogparams *p)
size_t i;
/* Read the WCS meta-data. */
- p->objects->wcs=gal_wcs_read(p->objectsfile, p->cp.hdu, 0, 0,
+ p->objects->wcs=gal_wcs_read(p->objectsfile, p->cp.hdu,
+ p->cp.wcslinearmatrix, 0, 0,
&p->objects->nwcs);
/* Read the basic WCS information. */
@@ -1423,10 +1424,20 @@ ui_preparations_read_keywords(struct mkcatalogparams *p)
keys[0].array=&minstd; keys[1].array=&p->medstd;
gal_fits_key_read(p->usedstdfile, p->stdhdu, keys, 0, 0);
- /* If the two keywords couldn't be read. We don't want to slow down
- the user for the median (which needs sorting). So we'll just
- calculate the minimum which is necessary for the 'p->cpscorr'. */
- if(keys[1].status) p->medstd=NAN;
+ /* If the two keywords couldn't be read. We don't want to slow
+ down the user for the median (which needs sorting). So we'll
+ just calculate if if '--forcereadstd' is called. However, we
+ need the minimum for 'p->cpscorr'. */
+ if(keys[1].status)
+ {
+ if(p->forcereadstd)
+ {
+ tmp=gal_statistics_median(p->std, 0);
+ p->medstd=*((float *)(tmp->array));
+ }
+ else
+ p->medstd=NAN;
+ }
if(keys[0].status)
{
/* Calculate the minimum STD. */
diff --git a/bin/mkcatalog/ui.h b/bin/mkcatalog/ui.h
index 572720e..3d390da 100644
--- a/bin/mkcatalog/ui.h
+++ b/bin/mkcatalog/ui.h
@@ -158,6 +158,7 @@ enum option_keys_enum
UI_KEY_MAXIMUM,
UI_KEY_CLUMPSMAGNITUDE,
UI_KEY_UPPERLIMIT,
+ UI_KEY_UPPERLIMITSB,
UI_KEY_UPPERLIMITONESIGMA,
UI_KEY_UPPERLIMITSIGMA,
UI_KEY_UPPERLIMITQUANTILE,
diff --git a/bin/mkcatalog/upperlimit.c b/bin/mkcatalog/upperlimit.c
index b1b27bc..e108afe 100644
--- a/bin/mkcatalog/upperlimit.c
+++ b/bin/mkcatalog/upperlimit.c
@@ -35,6 +35,8 @@ along with Gnuastro. If not, see
<
#include <gnuastro/dimension.h>
#include <gnuastro/statistics.h>
+#include <gnuastro-internal/checkset.h>
+
#include "main.h"
#include "ui.h"
@@ -277,82 +279,64 @@ upperlimit_random_position(struct mkcatalog_passparams
*pp, gal_data_t *tile,
used/necessary, so to avoid confusion, we won't write it.
*/
void
-upperlimit_write_comments(struct mkcatalogparams *p,
- gal_list_str_t **comments, int withsigclip)
+upperlimit_write_keys(struct mkcatalogparams *p,
+ gal_fits_list_key_t **keylist, int withsigclip)
{
- char *str;
-
- if(p->cp.tableformat==GAL_TABLE_FORMAT_TXT)
- {
- if(asprintf(&str, "--------- Upper-limit measurement ---------")<0)
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(comments, str, 0);
- }
-
- if( asprintf(&str, "Number of usable random samples: %zu", p->upnum)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(comments, str, 0);
-
+ /* Write a title for */
+ gal_fits_key_list_title_add_end(keylist, "Upper-limit (UP) parameters", 0);
+
+ /* Basic settings. */
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_FLOAT32, "UPNSIGMA", 0,
+ &p->upnsigma, 0,
+ "Multiple of sigma to measure upper-limit.", 0,
+ NULL, 0);
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_SIZE_T, "UPNUMBER", 0,
+ &p->upnum, 0,
+ "Number of usable random samples.", 0,
+ "counter", 0);
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_STRING, "UPRNGNAM", 0,
+ (void *)(p->rng_name), 0,
+ "Random number generator name.", 0, NULL, 0);
+ mkcatalog_outputs_keys_numeric(keylist, &p->rng_seed,
+ GAL_TYPE_ULONG, "UPRNGSEE",
+ "Random number generator seed.", NULL);
+
+ /* Range of upper-limit values. */
if(p->uprange)
{
- switch(p->objects->ndim)
- {
- case 2:
- if( asprintf(&str, "Range of random samples about target: "
- "%zu, %zu", p->uprange[1], p->uprange[0])<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- break;
- case 3:
- if( asprintf(&str, "Range of random samples about target: %zu, "
- "%zu, %zu", p->uprange[2], p->uprange[1],
- p->uprange[0])<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- break;
- default:
- error(EXIT_FAILURE, 0, "%s: a bug! Please contact us at %s to "
- "address the problem. The value %zu is not recognized for "
- "'p->input->ndim'", __func__, PACKAGE_BUGREPORT,
- p->objects->ndim);
- }
- gal_list_str_add(comments, str, 0);
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_SIZE_T, "UPRANGE1", 0,
+ &p->uprange[p->objects->ndim-1], 0,
+ "Range about target in axis 1.", 0,
+ "pixels", 0);
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_STRING, "UPRANGE2", 0,
+ &p->uprange[p->objects->ndim==2 ? 0 : 1], 0,
+ "Range about target in axis 2.", 0,
+ "pixels", 0);
+ if(p->objects->ndim==3)
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_STRING, "UPRANGE3", 0,
+ &p->uprange[0], 0,
+ "Range about target in axis 3.", 0,
+ "pixels", 0);
}
- if( asprintf(&str, "Random number generator name: %s", p->rng_name)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(comments, str, 0);
-
- if( asprintf(&str, "Random number generator seed: %lu", p->rng_seed)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(comments, str, 0);
-
+ /* If the upper-limit measurement included sigma-clipping. */
if(withsigclip)
{
- if( asprintf(&str, "Multiple of STD used for sigma-clipping: %.3f",
- p->upsigmaclip[0])<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(comments, str, 0);
-
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_FLOAT64, "UPSCMLTP", 0,
+ &p->upsigmaclip[0], 0,
+ "Multiple of STD used for sigma-clipping.", 0,
+ NULL, 0);
if(p->upsigmaclip[1]>=1.0f)
- {
- if( asprintf(&str, "Number of clips for sigma-clipping: %.0f",
- p->upsigmaclip[1])<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- }
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_FLOAT64, "UPSCNUM", 0,
+ &p->upsigmaclip[1], 0,
+ "Number of clips for sigma-clipping.", 0,
+ NULL, 0);
else
- {
- if( asprintf(&str, "Tolerance level to sigma-clipping: %.3f",
- p->upsigmaclip[1])<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- }
- gal_list_str_add(comments, str, 0);
+ gal_fits_key_list_add_end(keylist, GAL_TYPE_FLOAT64, "UPSCTOL", 0,
+ &p->upsigmaclip[1], 0,
+ "Tolerance level to sigma-clipping.", 0,
+ NULL, 0);
- if( p->oiflag[ OCOL_UPPERLIMIT_B ] )
- {
- if( asprintf(&str, "Multiple of sigma-clipped STD for upper-limit: "
- "%.3f", p->upnsigma)<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(comments, str, 0);
- }
}
}
@@ -367,8 +351,7 @@ upperlimit_write_check(struct mkcatalogparams *p,
gal_list_sizet_t *check_x,
gal_list_f32_t *check_s)
{
float *sarr;
- char *tmp=NULL, *tmp2=NULL;
- gal_list_str_t *comments=NULL;
+ gal_fits_list_key_t *keylist=NULL;
size_t *xarr, *yarr, *zarr=NULL, tnum, ttnum, num;
gal_data_t *x=NULL, *y=NULL, *z=NULL, *s=NULL; /* To avoid warnings. */
@@ -418,35 +401,30 @@ upperlimit_write_check(struct mkcatalogparams *p,
gal_list_sizet_t *check_x,
/* Write exactly what object/clump this table is for. */
+ gal_fits_key_list_title_add_end(&keylist, "Target for upper-limit check", 0);
+ mkcatalog_outputs_keys_numeric(&keylist, &p->checkuplim[0],
+ GAL_TYPE_INT32, "UPCHKOBJ",
+ "Object label for upper-limit check target.",
+ NULL);
if( p->checkuplim[1]!=GAL_BLANK_INT32 )
- if( asprintf(&tmp2, ", Clump %d", p->checkuplim[1]) <0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- if( asprintf(&tmp, "Upperlimit distribution for Object %d%s",
- p->checkuplim[0],
- ( p->checkuplim[1]==GAL_BLANK_INT32
- ? "" : tmp2) ) <0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(&comments, tmp, 0);
- if(tmp2) {free(tmp2); tmp2=NULL;}
-
-
- /* Write the basic info, and conclude the comments. */
- mkcatalog_write_inputs_in_comments(p, &comments, 0, 0);
- upperlimit_write_comments(p, &comments, 0);
+ mkcatalog_outputs_keys_numeric(&keylist, &p->checkuplim[1],
+ GAL_TYPE_INT32, "UPCHKCLU",
+ "Clump label for upper-limit check target.",
+ NULL);
+
+
+ /* Write the basic info, and conclude the keywords. */
+ mkcatalog_outputs_keys_infiles(p, &keylist);
+ upperlimit_write_keys(p, &keylist, 0);
if(p->cp.tableformat==GAL_TABLE_FORMAT_TXT)
- {
- if( asprintf(&tmp, "--------- Table columns ---------")<0 )
- error(EXIT_FAILURE, 0, "%s: asprintf allocation", __func__);
- gal_list_str_add(&comments, tmp, 0);
- }
+ gal_fits_key_list_title_add_end(&keylist, "Column metadata", 0);
/* Define a list from the containers and write them into a table. */
x->next=y;
if(check_z) { y->next=z; z->next=s; }
else { y->next=s; }
- gal_list_str_reverse(&comments);
- gal_table_write(x, NULL, comments, p->cp.tableformat, p->upcheckout,
+ gal_table_write(x, &keylist, NULL, p->cp.tableformat, p->upcheckout,
"UPPERLIMIT_CHECK", 0);
/* Inform the user. */
@@ -488,12 +466,33 @@ upperlimit_measure(struct mkcatalog_passparams *pp,
int32_t clumplab,
{
switch(column->status)
{
- /* Columns that depend on the sigma of the distribution. */
- case UI_KEY_UPPERLIMIT:
- case UI_KEY_UPPERLIMITMAG:
- case UI_KEY_UPPERLIMITSIGMA:
- case UI_KEY_UPPERLIMITONESIGMA:
+ /* Quantile column. */
+ case UI_KEY_UPPERLIMITQUANTILE:
+
+ /* Also only necessary once (if requested multiple times). */
+ if(qfunc==NULL)
+ {
+ /* Similar to the case for sigma-clipping, we'll need to
+ keep the size here also. */
+ init_size=pp->up_vals->size;
+ sum=gal_data_alloc(NULL, GAL_TYPE_FLOAT32, 1, &one, NULL, 0,
+ -1, 1, NULL, NULL, NULL);
+ ((float *)(sum->array))[0]=o[clumplab?CCOL_SUM:OCOL_SUM];
+ qfunc=gal_statistics_quantile_function(pp->up_vals, sum, 1);
+
+ /* Fill in the column. */
+ col = clumplab ? CCOL_UPPERLIMIT_Q : OCOL_UPPERLIMIT_Q;
+ pp->up_vals->size=pp->up_vals->dsize[0]=init_size;
+ o[col] = ((double *)(qfunc->array))[0];
+
+ /* Clean up. */
+ gal_data_free(sum);
+ gal_data_free(qfunc);
+ }
+ break;
+ /* Columns that depend on the sigma of the distribution. */
+ default:
/* We only need to do this once, but the columns can be
requested in any order. */
if(sigclip==NULL)
@@ -525,31 +524,6 @@ upperlimit_measure(struct mkcatalog_passparams *pp,
int32_t clumplab,
gal_data_free(sigclip);
}
break;
-
- /* Quantile column. */
- case UI_KEY_UPPERLIMITQUANTILE:
-
- /* Also only necessary once (if requested multiple times). */
- if(qfunc==NULL)
- {
- /* Similar to the case for sigma-clipping, we'll need to
- keep the size here also. */
- init_size=pp->up_vals->size;
- sum=gal_data_alloc(NULL, GAL_TYPE_FLOAT32, 1, &one, NULL, 0,
- -1, 1, NULL, NULL, NULL);
- ((float *)(sum->array))[0]=o[clumplab?CCOL_SUM:OCOL_SUM];
- qfunc=gal_statistics_quantile_function(pp->up_vals, sum, 1);
-
- /* Fill in the column. */
- col = clumplab ? CCOL_UPPERLIMIT_Q : OCOL_UPPERLIMIT_Q;
- pp->up_vals->size=pp->up_vals->dsize[0]=init_size;
- o[col] = ((double *)(qfunc->array))[0];
-
- /* Clean up. */
- gal_data_free(sum);
- gal_data_free(qfunc);
- }
- break;
}
}
}
diff --git a/bin/mkcatalog/upperlimit.h b/bin/mkcatalog/upperlimit.h
index 666c3a0..3ddb5ca 100644
--- a/bin/mkcatalog/upperlimit.h
+++ b/bin/mkcatalog/upperlimit.h
@@ -24,8 +24,8 @@ along with Gnuastro. If not, see
<
#define UPPERLIMIT_H
void
-upperlimit_write_comments(struct mkcatalogparams *p,
- gal_list_str_t **comments, int withsigclip);
+upperlimit_write_keys(struct mkcatalogparams *p,
+ gal_fits_list_key_t **keylist, int withsigclip);
void
upperlimit_calculate(struct mkcatalog_passparams *pp);
diff --git a/bin/mknoise/mknoise.c b/bin/mknoise/mknoise.c
index 6731ed7..5320d5c 100644
--- a/bin/mknoise/mknoise.c
+++ b/bin/mknoise/mknoise.c
@@ -32,6 +32,7 @@ along with Gnuastro. If not, see
<
#include <gsl/gsl_rng.h> /* Used in setrandoms. */
#include <gnuastro/fits.h>
+#include <gnuastro/units.h>
#include <gsl/gsl_randist.h> /* To make noise. */
#include <gnuastro-internal/timing.h>
@@ -70,7 +71,7 @@ convertsaveoutput(struct mknoiseparams *p)
0, NULL, 0);
if( !isnan(p->zeropoint) )
{
- tmp=-2.5 * log10(p->background) + p->zeropoint;
+ tmp=gal_units_counts_to_mag(p->background, p->zeropoint);
gal_checkset_allocate_copy("BCKGMAG", &keyname);
gal_fits_key_list_add_end(&headers, GAL_TYPE_FLOAT64, keyname, 1,
&tmp, 0,
diff --git a/bin/mknoise/ui.c b/bin/mknoise/ui.c
index f39bbc9..4c99355 100644
--- a/bin/mknoise/ui.c
+++ b/bin/mknoise/ui.c
@@ -311,7 +311,8 @@ ui_preparations(struct mknoiseparams *p)
p->input=gal_array_read_one_ch_to_type(p->inputname, p->cp.hdu, NULL,
GAL_TYPE_FLOAT64, p->cp.minmapsize,
p->cp.quietmmap);
- p->input->wcs=gal_wcs_read(p->inputname, p->cp.hdu, 0, 0, &p->input->nwcs);
+ p->input->wcs=gal_wcs_read(p->inputname, p->cp.hdu, p->cp.wcslinearmatrix,
+ 0, 0, &p->input->nwcs);
p->input->ndim=gal_dimension_remove_extra(p->input->ndim, p->input->dsize,
p->input->wcs);
diff --git a/bin/mkprof/args.h b/bin/mkprof/args.h
index c0d05fe..d6a8887 100644
--- a/bin/mkprof/args.h
+++ b/bin/mkprof/args.h
@@ -209,7 +209,7 @@ struct argp_option program_options[] =
UI_KEY_NUMRANDOM,
"INT",
0,
- "No. of random points in Monte Carlo integration.",
+ "No. of random points in Monte Carlo integ.",
UI_GROUP_PROFILES,
&p->numrandom,
GAL_TYPE_SIZE_T,
@@ -376,7 +376,7 @@ struct argp_option program_options[] =
UI_KEY_CCOL,
"STR/INT",
0,
- "Coordinate columns (one call for each dimension).",
+ "Coordinate columns (one call for each dim.).",
UI_GROUP_CATALOG,
&p->ccol,
GAL_TYPE_STRLL,
@@ -391,7 +391,7 @@ struct argp_option program_options[] =
0,
"sersic (1), moffat (2), gaussian (3), point (4), "
"flat (5), circumference (6), distance (7), "
- "radial-table (8)",
+ "radial-table (8).",
UI_GROUP_CATALOG,
&p->fcol,
GAL_TYPE_STRING,
@@ -430,7 +430,7 @@ struct argp_option program_options[] =
UI_KEY_PCOL,
"STR/INT",
0,
- "Position angle (First X-Z-X Euler angle in 3D).",
+ "Position angle (3D: first X-Z-X Euler angle).",
UI_GROUP_CATALOG,
&p->pcol,
GAL_TYPE_STRING,
@@ -508,7 +508,7 @@ struct argp_option program_options[] =
UI_KEY_TCOL,
"STR/INT",
0,
- "Truncation in units of --rcol, unless --tunitinp.",
+ "Truncation in units of --rcol.",
UI_GROUP_CATALOG,
&p->tcol,
GAL_TYPE_STRING,
diff --git a/bin/mkprof/mkprof.c b/bin/mkprof/mkprof.c
index 60d188b..13b8cde 100644
--- a/bin/mkprof/mkprof.c
+++ b/bin/mkprof/mkprof.c
@@ -32,6 +32,7 @@ along with Gnuastro. If not, see
<
#include <gnuastro/box.h>
#include <gnuastro/git655,7 +656,7 @@ mkprof_write(struct mkprofparams *p)
break;
case 2:
((float *)(log->array))[ibq->id] =
- sum>0.0f ? -2.5f*log10(sum)+p->zeropoint : NAN;
+ gal_units_counts_to_mag(sum, p->zeropoint);
break;
case 1:
((unsigned long *)(log->array))[ibq->id]=ibq->id+1;
@@ -883,7 +884bin/mkprof/ui.c b/bin/mkprof/ui.c
index 5e1ad36..9b29674 100644
--- a/bin/mkprof/ui.c
+++ b/bin/mkprof/ui.c
@@ -1359,6 +1359,10 @@ ui_prepare_wcs(struct mkprofparams *p)
if(status)
error(EXIT_FAILURE, 0, "wcsset error %d: %s", status,
wcs_errmsg[status]);
+
+ /* Convert it to CD if the user wanted it. */
+ if(p->cp.wcslinearmatrix==GAL_WCS_LINEAR_MATRIX_CD)
+ gal_wcs_to_cd(wcs);
}
@@ -1384,7 +1388,8 @@ ui_prepare_canvas(struct mkprofparams *p)
the background image and the number of its dimensions. So
'ndim==0' and what 'dsize' points to is irrelevant. */
tdsize=gal_fits_img_info_dim(p->backname, p->backhdu, &tndim);
- p->wcs=gal_wcs_read(p->backname, p->backhdu, 0, 0, &p->nwcs);
+ p->wcs=gal_wcs_read(p->backname, p->backhdu, p->cp.wcslinearmatrix,
+ 0, 0, &p->nwcs);
tndim=gal_dimension_remove_extra(tndim, tdsize, p->wcs);
free(tdsize);
if(p->nomerged==0)
diff --git a/bin/noisechisel/ui.c b/bin/noisechisel/ui.c
index 2f3e413..9d3e2b5 100644
--- a/bin/noisechisel/ui.c
+++ b/bin/noisechisel/ui.c
@@ -587,7 +587,8 @@ ui_preparations_read_input(struct noisechiselparams *p)
NULL, GAL_TYPE_FLOAT32,
p->cp.minmapsize,
p->cp.quietmmap);
- p->input->wcs = gal_wcs_read(p->inputname, p->cp.hdu, 0, 0,query/astron.c b/bin/query/astron.c
index c3f41ad..01dd25d 100644
--- a/bin/query/astron.c
+++ b/bin/query/astron.c
@@ -50,6 +50,9 @@ astron_sanity_checks(struct queryparams *p)
gal_checkset_allocate_copy("tgssadr.main", &p->datasetstr);
}
}
+
+ /* Currently we assume ASTRON only uses TAP. */
+ p->usetap=1;
}
@@ -59,7 +62,7 @@ astron_sanity_checks(struct queryparams *p)
void
astron_prepare(struct queryparams *p)
{
- /* NED-specific. */
+ /* ASTRON-specific. */
astron_sanity_checks(p);
/* Set the URLs, note that this is a simply-linked list, so we need to
diff --git a/bin/query/gaia.c b/bin/query/gaia.c
index 135e3ca..a7dd61f 100644
--- a/bin/query/gaia.c
+++ b/bin/query/gaia.c
@@ -95,6 +95,9 @@ gaia_sanity_checks(struct queryparams *p)
gal_checkset_allocate_copy("public.tycho2", &p->datasetstr);
}
}
+
+ /* Currently we assume GAIA only uses TAP. */
+ p->usetap=1;
}
diff --git a/bin/query/main.h b/bin/query/main.h
index 377d41c..62c70f3 100644
--- a/bin/query/main.h
+++ b/bin/query/main.h
@@ -70,6 +70,7 @@ struct queryparams
char *ra_name; /* Name of RA column. */
char *dec_name; /* Name of Dec columns. */
char *finalcommand; /* The final command used. */
+ int usetap; /* If a TAP-download should be used. */
/* Output: */
time_t rawtime; /* Starting time of the program. */
diff --git a/bin/query/ned.c b/bin/query/ned.c
index f2fd24f..80a9bae 100644
--- a/bin/query/ned.c
+++ b/bin/query/ned.c
@@ -37,7 +37,7 @@ along with Gnuastro. If not, see
<
-
+/* Basic sanity checks. */
static void
ned_sanity_checks(struct queryparams *p)
{
@@ -51,9 +51,35 @@ ned_sanity_checks(struct queryparams *p)
}
}
+ /* Database-specific checks. For example, if we should use TAP or
+ not. Note that the user may give 'NEDTAP.objdir', so we can't use the
+ 'if' above (for expanding summarized names). */
+ if( !strcmp(p->datasetstr, "NEDTAP.objdir") )
+ p->usetap=1;
+ else if( !strcmp(p->datasetstr, "extinction") )
+ {
+ /* Crash for options that are not compatible with extinction. */
+ if( p->radius || p->width || p->range || p->noblank || p->columns
+ || p->head!=GAL_BLANK_SIZE_T || p->sort )
+ error(EXIT_FAILURE, 0, "NED's extinction calculator returns "
+ "the galactic extinction for a single point (in multiple "
+ "filters), therefore the following options are not "
+ "acceptable with it: '--radius', '--width', '--range', "
+ "'--noblank', '--column', '--head' and '--sort'");
+
+ /* Make sure that '--center' is given. */
+ if(p->center==NULL)
+ error(EXIT_FAILURE, 0, "no coordinate specified! Please use "
+ "'--center' to specify the RA and Dec (in J2000) of "
+ "your desired coordinate, for example "
+ "--center=10.68458,41.269166");
+ }
+
/* Currently NED only has a single table for TAP access, so warn the
users about this if they ask for any other table. */
- if( p->datasetstr==NULL || strcmp(p->datasetstr, "NEDTAP.objdir") )
+ if( p->usetap
+ && ( p->datasetstr==NULL
+ || strcmp(p->datasetstr, "NEDTAP.objdir") ) )
error(EXIT_FAILURE, 0, "NED currently only supports a single "
"dataset with the TAP protocol called 'NEDTAP.objdir' "
"(which you can also call in Query with '--dataset=objdir'). "
@@ -67,22 +93,87 @@ ned_sanity_checks(struct queryparams *p)
+/* Extinction with NED */
+void
+ned_extinction(struct queryparams *p)
+{
+ double *darr;
+ char *command;
+
+ /* If the user wants information, we'll specify a (0,0) center coordinate
+ and continue. In the end, instead of saving the file, we'll just
+ report the metadata. */
+ if(p->information)
+ error(EXIT_FAILURE, 0, "'--information' is not yet supported for "
+ "NED's extinction calculator");
+
+ /* Build the calling command. Note that the query quotes are
+ included by the function building it. */
+ darr=p->center->array;
+ if( asprintf(&command, "curl%s -o%s
'
p->cp.quiet ? " -s" : "",
+ p->downloadname, darr[0], darr[1])<0 )
+ error(EXIT_FAILURE, 0, "%s: asprintf allocation ('command')",
+ __func__);
+
+ /* Print the calling command for the user to know. */
+ if(p->dryrun==1 || p->cp.quiet==0)
+ {
+ if(p->dryrun==0) printf("\n");
+ error(EXIT_SUCCESS, 0, "%s: %s",
+ p->dryrun ? "would run" : "running", command);
+ if(p->dryrun==0) printf("\nDownload status:\n");
+ }
+
+ /* Run the command if '--dryrun' isn't called: if the command succeeds
+ 'system' returns 'EXIT_SUCCESS'. */
+ if(p->dryrun==0)
+ {
+ if(system(command)!=EXIT_SUCCESS)
+ error(EXIT_FAILURE, 0, "the query download command %sfailed%s\n",
+ p->cp.quiet==0 ? "printed above " : "",
+ p->cp.quiet==0 ? "" : " (the command can be printed "
+ "if you don't use the option '--quiet', or '-q')");
+ }
+}
+
+
+
+
+
+/* For NED's non-TAP queries. */
+void
+ned_non_tap(struct queryparams *p)
+{
+ if( !strcmp(p->datasetstr, "extinction") )
+ ned_extinction(p);
+}
+
+
+
+
+
void
ned_prepare(struct queryparams *p)
{
/* NED-specific. */
ned_sanity_checks(p);
- /* Set the URLs, note that this is a simply-linked list, so we need to
- reverse it in the end (with 'gal_list_str_reverse') to have the same
- order here. */
- gal_list_str_add(&p->urls,
- " 0);
-
- /* Name of default RA Dec columns. */
- if(p->ra_name==NULL) p->ra_name="ra";
- if(p->dec_name==NULL) p->dec_name="dec";
-
- /* Basic sanity checks. */
- tap_sanity_checks(p);
+ /* If we should use TAP, do the preparations. */
+ if(p->usetap)
+ {
+ /* Set the URLs, note that this is a simply-linked list, so we need
+ to reverse it in the end (with 'gal_list_str_reverse') to have the
+ same order here. */
+ gal_list_str_add(&p->urls,
+ " 0);
+
+ /* Name of default RA Dec columns. */
+ if(p->ra_name==NULL) p->ra_name="ra";
+ if(p->dec_name==NULL) p->dec_name="dec";
+
+ /* Basic sanity checks. */
+ tap_sanity_checks(p);
+ }
+ else
+ ned_non_tap(p);
}
diff --git a/bin/query/query.c b/bin/query/query.c
index b8289b5..cae127d 100644
--- a/bin/query/query.c
+++ b/bin/query/query.c
@@ -284,36 +284,49 @@ query_output_data(struct queryparams *p)
void
-query_check_download(struct queryparams *p)
+query_output_finalize(struct queryparams *p)
{
size_t len;
- int status=0;
+ int isxml=0;
char *logname;
fitsfile *fptr;
+ int gooddownload=0, status=0;
- /* Open the FITS file and if the status value is still zero, it means
- everything worked properly. */
- fits_open_file(&fptr, p->downloadname, READONLY, &status);
- if(status==0)
+ /* See if its a FITS file or a VOTable. */
+ len=strlen(p->downloadname);
+ if( !strcmp(&p->downloadname[len-4], ".xml") )
+ { isxml=1; gooddownload=1; }
+ else
{
- /* Close the FITS file pointer. */
- fits_close_file(fptr, &status);
+ /* Open the FITS file and if the status value is still zero, it means
+ everything worked properly. */
+ fits_open_file(&fptr, p->downloadname, READONLY, &status);
+ if(status==0)
+ {
+ gooddownload=1;
+ fits_close_file(fptr, &status);
+ }
+ }
+ /* If the downloaded file is good, do the preparations. */
+ if(gooddownload)
+ {
/* Prepare the output dataset. */
if(p->information)
{
if(p->datasetstr) query_output_meta_dataset(p);
else query_output_meta_database(p);
}
- else query_output_data(p);
+ else if(isxml==0) query_output_data(p);
/* Delete the raw downloaded file if necessary. */
if(p->keeprawdownload==0) remove(p->downloadname);
}
+
+ /* If there was an error */
else
{
/* Add a '.log' suffix to the output filename. */
- len=strlen(p->downloadname);
logname=gal_pointer_allocate(GAL_TYPE_STRING, len+10, 1,
__func__, "logname");
sprintf(logname, "%s.log", p->downloadname);
@@ -326,8 +339,8 @@ query_check_download(struct queryparams *p)
"retrieved! For more, please see '%s'", logname);
}
- /* Add the query keywords to the first extension (if the output was a
- FITS file). */
+ /* Add the query keywords to the first extension of the output (if the
+ output was a FITS file). */
if( p->information==0 && gal_fits_name_is_fits(p->cp.output) )
{
gal_fits_key_list_title_add_end(&p->cp.okeys,
@@ -360,12 +373,12 @@ query(struct queryparams *p)
}
/* Download the requested query. */
- tap_download(p);
+ if(p->usetap) tap_download(p);
/* Make sure that the result is a readable FITS file, otherwise, abort
with an error. */
if(p->dryrun==0)
- query_check_download(p);
+ query_output_finalize(p);
/* Let the user know that things went well. */
if(p->dryrun==0 && p->cp.quiet==0)
@@ -379,12 +392,7 @@ query(struct queryparams *p)
printf("Query's raw downloaded file: %s\n", p->downloadname);
}
if(p->information==0)
- {
- printf("Query's final output: %s\n", p->cp.output);
- printf("TIP: use the command below for more on the "
- "downloaded table:\n"
- " asttable %s --info\n", p->cp.output);
- }
+ printf("Query's output written: %s\n", p->cp.output);
}
/* Clean up. */
diff --git a/bin/query/ui.c b/bin/query/ui.c
index ed37313..204fa8e 100644
--- a/bin/query/ui.c
+++ b/bin/query/ui.c
@@ -266,9 +266,9 @@ ui_read_check_only_options(struct queryparams *p)
{
size_t i;
double *darray;
- char *basename;
gal_data_t *tmp;
int keepinputdir;
+ char *suffix, *rdsuffix, *basename;
/* See if database has been specified. */
if(p->databasestr==NULL)
@@ -405,26 +405,65 @@ ui_read_check_only_options(struct queryparams *p)
gal_checkset_writable_remove(p->cp.output, p->cp.keep,
p->cp.dontdelete);
+ /* Set the suffix of the default names. */
+ if( p->database==QUERY_DATABASE_NED
+ && !strcmp(p->datasetstr, "extinction") )
+ {
+ suffix=".xml";
+ rdsuffix="-raw-download.xml";
+ }
+ else
+ {
+ suffix=".fits";
+ rdsuffix="-raw-download.fits";
+ }
+
+ /* Currently Gnuastro doesn't read or write XML files (VOTable). So if
+ the downloaded file is an XML file but the user hasn't given an XML
+ suffix, abort and inform the user. */
+ if(p->cp.output)
+ {
+ if( !strcmp(suffix,".xml")
+ && strcmp(&p->cp.output[strlen(p->cp.output)-4], ".xml") )
+ error(EXIT_FAILURE, 0, "this dataset's output is a VOTable (with "
+ "an '.xml' suffix). However, Gnuastro doesn't yet support "
+ "VOTable, so it won't do any checks and corrections on "
+ "the downloaded file. Please give an output name with an "
+ "'.xml' suffix to continue");
+ }
+
/* Set the name for the downloaded and final output name. These are due
to an internal low-level processing that will be done on the raw
downloaded file. */
- if(p->cp.output==NULL)
+ else
{
- basename=gal_checkset_malloc_cat(p->databasestr, ".fits");
- p->cp.output=gal_checkset_make_unique_suffix(basename, ".fits");
+ basename=gal_checkset_malloc_cat(p->databasestr, suffix);
+ p->cp.output=gal_checkset_make_unique_suffix(basename, suffix);
free(basename);
}
- /* Make sure the output name doesn't exist (and report an error if
- '--dontdelete' is called. Just note that for the automatic output, we
- are basing that on the output, not the input. So we are temporarily
- activating 'keepinputdir'. */
- keepinputdir=p->cp.keepinputdir;
- p->cp.keepinputdir=1;
- gal_checkset_writable_remove(p->cp.output, 0, p->cp.dontdelete);
- p->downloadname=gal_checkset_automatic_output(&p->cp, p->cp.output,
- "-raw-download.fits");
- p->cp.keepinputdir=keepinputdir;
+ /* Currently we don't interally process VOTable (in '.xml' suffix) files,
+ so to keep the next steps un-affected, we'll set Query to not delete
+ the raw download and copy the name of the output into the raw
+ download. */
+ if( !strcmp(suffix, ".xml") )
+ {
+ p->keeprawdownload=1;
+ gal_checkset_allocate_copy(p->cp.output, &p->downloadname);
+ }
+ else
+ {
+ /* Make sure the output name doesn't exist (and report an error if
+ '--dontdelete' is called. Just note that for the automatic output,
+ we are basing that on the output, not the input. So we are
+ temporarily activating 'keepinputdir'. */
+ keepinputdir=p->cp.keepinputdir;
+ p->cp.keepinputdir=1;
+ gal_checkset_writable_remove(p->cp.output, 0, p->cp.dontdelete);
+ p->downloadname=gal_checkset_automatic_output(&p->cp, p->cp.output,
+ rdsuffix);
+ p->cp.keepinputdir=keepinputdir;
+ }
}
diff --git a/bin/query/vizier.c b/bin/query/vizier.c
index d7513a0..f2dfcfd 100644
--- a/bin/query/vizier.c
+++ b/bin/query/vizier.c
@@ -143,6 +143,9 @@ vizier_sanity_checks(struct queryparams *p)
gal_checkset_allocate_copy("II/363/unwise", &p->datasetstr);
}
}
+
+ /* Currently we assume VizieR only uses TAP. */
+ p->usetap=1;
}
diff --git a/bin/script/Makefile.am b/bin/script/Makefile.am
index 3bbedcf..3c45589 100644
--- a/bin/script/Makefile.am
+++ b/bin/script/Makefile.am
@@ -26,10 +26,13 @@
## 'prefix/bin' directory ('bin_SCRIPTS'), files necessary to distribute
## with the tarball ('EXTRA_DIST') and output files (to be cleaned with
## 'make clean').
-bin_SCRIPTS = astscript-make-ds9-reg \
+bin_SCRIPTS = astscript-ds9-region \
+ astscript-radial-profile \
astscript-sort-by-night
-EXTRA_DIST = make-ds9-reg.in sort-by-night.in
+EXTRA_DIST = ds9-region.in \
+ radial-profile.in \
+ sort-by-night.in
CLEANFILES = $(bin_SCRIPTS)
@@ -45,11 +48,15 @@ do_subst = sed -e 's,[@]VERSION[@],$(VERSION),g' \
-## Rules to build the scripts
-astscript-sort-by-night: sort-by-night.in Makefile
- $(do_subst) < $(srcdir)/sort-by-night.in > $@
+## Rules to install the scripts.
+astscript-ds9-region: ds9-region.in Makefile
+ $(do_subst) < $(srcdir)/ds9-region.in > $@
+ chmod +x $@
+
+astscript-radial-profile: radial-profile.in Makefile
+ $(do_subst) < $(srcdir)/radial-profile.in > $@
chmod +x $@
-astscript-make-ds9-reg: make-ds9-reg.in Makefile
- $(do_subst) < $(srcdir)/make-ds9-reg.in > $@
+astscript-sort-by-night: sort-by-night.in Makefile
+ $(do_subst) < $(srcdir)/sort-by-night.in > $@
chmod +x $@
diff --git a/bin/script/make-ds9-reg.in b/bin/script/ds9-region.in
old mode 100755
new mode 100644
similarity index 83%
rename from bin/script/make-ds9-reg.in
rename to bin/script/ds9-region.in
index 15d115e..3c55243
--- a/bin/script/make-ds9-reg.in
+++ b/bin/script/ds9-region.in
@@ -5,6 +5,7 @@
# Original author:
# Mohammad Akhlaghi <mohammad@akhlaghi.org>
# Contributing author(s):
+# Samane Raji <samaneraji@protonmail.com>
# Copyright (C) 2021 Free Software Foundation, Inc.
#
# Gnuastro is free software: you can redistribute it and/or modify it under
@@ -32,11 +33,11 @@ set -e
# command-line).
hdu=1
col=""
-name=""
width=1
mode=wcs
radius=""
command=""
+namecol=""
out=ds9.reg
color=green
dontdelete=0
@@ -82,6 +83,7 @@ $scriptname options:
-h, --hdu=STR HDU/extension of all input FITS files.
-c, --column=STR,STR Columns to use as coordinates (name or number).
-m, --mode=wcs|img Coordinates in WCS or image (default: $mode)
+ -n, --namecol=STR ID of each region (name or number of a column)
Output:
-C, --color Color for the regions (read by DS9).
@@ -189,6 +191,9 @@ do
-m|--mode) mode="$2"; check_v "$1"
"$mode"; shift;shift;;
-m=*|--mode=*) mode="${1#*=}"; check_v "$1"
"$mode"; shift;;
-m*) mode=$(echo "$1" | sed -e's/-m//'); check_v "$1"
"$mode"; shift;;
+ -n|--namecol) namecol="$2"; check_v "$1"
"$namecol"; shift;shift;;
+ -n=*|--namecol=*) namecol="${1#*=}"; check_v "$1"
"$namecol"; shift;;
+ -n*) namecol=$(echo "$1" | sed -e's/-n//'); check_v
"$1" "$namecol"; shift;;
# Output parameters
-C|--color) color="$2"; check_v
"$1" "$color"; shift;shift;;
@@ -244,7 +249,7 @@ if [ x$col = x ]; then
else
ncols=$(echo $col | awk 'BEGIN{FS=","}END{print NF}')
if [ x$ncols != x2 ]; then
- echo "$scriptname: only two columns should be given, but $ncols were
given"
+ echo "$scriptname: only two columns should be given with '--column'
(or '-c'), but $ncols were given"
exit 1
fi
fi
@@ -266,6 +271,15 @@ if [ -f $out ]; then
fi
fi
+# Make sure a single column is given to '--namecol':
+if [ x"$namecol" != x ]; then
+ ncols=$(echo $namecol | awk 'BEGIN{FS=","}END{print NF}')
+ if [ x$ncols != x1 ]; then
+ echo "$scriptname: only one column should be given to '--namecol'"
+ exit 1
+ fi
+fi
+
@@ -288,8 +302,11 @@ if [ x$mode = x"wcs" ]; then unit="\""; else unit=""; fi
# Write the metadata in the output.
printf "# Region file format: DS9 version 4.1\n" > $out
printf "# Created by $scriptname (GNU Astronomy Utilities) $version\n" >> $out
-printf "# Input: $input (hdu $hdu)\n" >> $out
+printf "# Input file: $input (hdu $hdu)\n" >> $out
printf "# Columns: $col\n" >> $out
+if [ x"$namecol" != x ]; then
+ printf "# Region name (or label) column: $namecol\n" >> $out
+fi
printf "global color=%s width=%d\n" $color $width >> $out
if [ $mode = "wcs" ]; then printf "fk5\n" >> $out
else printf "image\n" >> $out; fi
@@ -300,27 +317,44 @@ else printf "image\n" >> $out; fi
# Write each region's results (when no input file is given, read from the
# standard input).
-if [ x"$input" = x ]; then
- cat /dev/stdin \
- |if [ x"$namecol" = x ]; then
+ if else
+ fi
else
- if [ x"$input" = x ]; then
+ cat /dev/stdin \
+ | else
+ fi
fi
-# Run ds9 with the desired region over-plotted.
-if [ x"$command" = x ]; then
- junk=1
-else
+# Run the user's command (while appending the region).
+if [ x"$command" != x ]; then
$command -regions $out
if [ $dontdelete = 0 ]; then rm $out; fi
fi
diff --git a/bin/script/radial-profile.in b/bin/script/radial-profile.in
new file mode 100644
index 0000000..a89eb29
--- /dev/null
+++ b/bin/script/radial-profile.in
@@ -0,0 +1,551 @@
+#!/bin/sh
+
+# Obtain averaged radial profiles, run with `--help', or see description
+# under `print_help' (below) for more.
+#
+# Original author:
+# Raul Infante-Sainz <infantesainz@gmail.com>
+# Contributing author(s):
+# Mohammad Akhlaghi <mohammad@akhlaghi.org>
+# Zahra Sharbaf <zahra.sharbaf2@gmail.com>
+# Carlos Morales-Socorro <cmorsoc@gmail.com>
+# Copyright (C) 2020-2021 command-line).
+hdu=1
+rmax=""
+quiet=""
+center=""
+tmpdir=""
+output=""
+keeptmp=0
+mode="img"
+measure=""
+axisratio=1
+sigmaclip=""
+oversample=""
+positionangle=0
+version=@VERSION@
+scriptname=@SCRIPT_NAME@
+
+
+
+
+
+# Output of `--usage' and ` consider the input image for constructing the radial
+profile around a given center with elliptical aperturesO, --mode=STR Coordinate mode: img or wcs.
+ -c, --center=FLT,FLT Coordinate of the center along 2 axes.
+ -R, --rmax=FLT Maximum radius for the radial profile (in pixels).
+ -Q, --axisratio=FLT Axis ratio for ellipse profiles (A/B).
+ -p, --positionangle=FLT Position angle for ellipse profiles.
+ -s, --sigmaclip=FLT,FLT Sigma-clip multiple and tolerance.
+
+ Output:
+ -t, --tmpdir Directory to keep temporary files.
+ -k, --keeptmp Keep temporal/auxiliar files.
+ -m, --measure=STR Measurement operator (mean, sigclip-mean, etc.).
+ -o, --output Output table with the radial profile.
+ -v, --oversample Oversample for higher resolution radial profile.
+
+ Operating mode:
+ -h, --help Print this help list.
+ --cite BibTeX citation for this program.
+ -q, --quiet Don't print the list `--version':
+print_version() {
+ cat <<EOF
+$scriptname (GNU Astronomy Utilities) $version
+Copyright (C) 2020 Raul Infante-Sainz `--longname value' and `--longname=value'. For short
+# option names we want `-l value', `-l=value' and `-lvalue' (where `-l'
+# is the short version of the hypothetical ` `-h*' should be checked only when we are sure that its
+# not `-h=*').
+#
+# OPTIONS WITH NO VALUE (ON-OFF OPTIONS)
+#
+# For these, we just want the two forms of `--longname' or `-l'. Nothing
+# else. So if an equal sign is given we should definitely crash and also,
+# if a value is appended to the short format it should crash. So in the
+# second test for these (`-l*') will account for both the case where we
+# have an equal sign and where we don't.
+while [ $# -gt 0 ]
+do
+ case "$1" in
+ # Input parameters.
+ -h|--hdu) hdu="$2"; check_v
"$1" "$hdu"; shift;shift;;
+ -h=*|--hdu=*) hdu="${1#*=}"; check_v
"$1" "$hdu"; shift;;
+ -h*) hdu=$(echo "$1" | sed -e's/-h//'); check_v
"$1" "$hdu"; shift;;
+ -O|--mode) mode="$2"; check_v
"$1" "$mode"; shift;shift;;
+ -O=*|--mode=*) mode="${1#*=}"; check_v
"$1" "$mode"; shift;;
+ -O*) mode=$(echo "$1" | sed -e's/-O//'); check_v
"$1" "$mode"; shift;;
+ -c|--center) center="$2"; check_v
"$1" "$center"; shift;shift;;
+ -c=*|--center=*) center="${1#*=}"; check_v
"$1" "$center"; shift;;
+ -c*) center=$(echo "$1" | sed -e's/-c//'); check_v
"$1" "$center"; shift;;
+ -R|--rmax) rmax="$2"; check_v
"$1" "$rmax"; shift;shift;;
+ -R=*|--rmax=*) rmax="${1#*=}"; check_v
"$1" "$rmax"; shift;;
+ -R*) rmax=$(echo "$1" | sed -e's/-R//'); check_v
"$1" "$rmaxs|--sigmaclip) sigmaclip="$2"; check_v
"$1" "$sigmaclip"; shift;shift;;
+ -s=*|--sigmaclip=*) sigmaclip="${1#*=}"; check_v
"$1" "$sigmaclip"; shift;;
+ -s*) sigmaclip=$(echo "$1" | sed -e's/-s//'); check_v
"$1" "$sigmaclip"; shift;;
+
+ # Output parameters
+ -k|--keeptmp) keeptmp=1; shift;;
+ -k*|--keeptmp=*) on_off_option_error --keeptmp -k;;
+ -t|--tmpdir) tmpdir="$2"; check_v "$1"
"$tmpdir"; shift;shift;;
+ -t=*|--tmpdir=*) tmpdir="${1#*=}"; check_v "$1"
"$tmpdir"; shift;;
+ -t*) tmpdir=$(echo "$1" | sed -e's/-t//'); check_v "$1"
"$tmpdir+ -o|--output) output="$2"; check_v "$1"
"$output"; shift;shift;;
+ -o=*|--output=*) output="${1#*=}"; check_v "$1"
"$output"; shift;;
+ -o*) output=$(echo "$1" | sed -e's/-o//'); check_v "$1"
"$output"; shift;;
+ -v|--oversample) oversample="$2"; check_v
"$1" "$oversample"; shift;shift;;
+ -v=*|--oversample=*) oversample="${1#*=}"; check_v
"$1" "$oversample"; shift;;
+ -v*) oversample=$(echo "$1" | sed -e's/-v//'); check_v
"$1" "$oversample"; shift;;
+
+ # Non-operating options.
+ -q|--quiet) quiet="--quiet"; shift;;
+ -q*|--quiet=*) on_off_option_error --quiet -q;; `-'): assumed to be input FITS
+ # file name.
+ *) inputs="$1 $inputs"; shift;;
+ es+done
+
+
+
+
+
+# Basic sanity checks
+# ===================
+
+# If an input image is given at all.
+if [ x"$inputs" = x ]; then
+ echo "$scriptname: no input FITS image files."
+ echo "Run with '--help' for more information on how to run."
+ exit 1
+fi
+
+# If a '--center' has been given, make sure it only has two numbers.
+if [ x"$center" = x ]; then
+ ncenter=$(echo $center | awk 'BEGIN{FS=","}END{print NF}')
+ if [ x$ncenter != x2 ]; then
+ echo "$scriptname: '--center' (or '-c') only take two values, but
$ncenter were given no specific measurement has been requested, use the mean.
+if [ x"$measure" = x ]; then measure=mean; fi
+
+
+
+
+
+# Finalize the center value
+# -------------------------
+#
+# Beyond this point, we know the image-based, central coordinate for the
+# radial profile as two values (one along each dimension).
+if [ x"$center" = x ]; then
+
+ # No center has been given: we thus assume that the object is already
+ # centered on the input image and will set the center to the central
+ # pixel in the image. In the FITS standard, pixels are counted from 1,
+ # and the integers are in the center of the pixel. So after dividing
+ # the pixel size of the image by 2, we should add it with 0.5 to be the
+ # `center' of the image.
+ xcenter=$(astfits $inputs --hdu=$hdu | awk '/^NAXIS1/{print $3/2+0.5}')
+ ycenter=$(astfits $inputs --hdu=$hdu | awk '/^NAXIS2/{print $3/2+0.5}')
+
+else
+
+ if [ $mode = img ]; then
+
+ # A center has been given, we should just separate them.
+ xcenter=$(echo "$center" | awk 'BEGIN{FS=","} {print $1}')
+ ycenter=$(echo "$center" | awk 'BEGIN{FS=","} {print $2}')
+
+ else
+
+ # WCS coordinates have been given. We should thus convert them to
+ # image coordinates at this point. To do that, WCS information from
+ # the input header image is used.
+ xy=$(echo "$center" \
+ | sed 's/,/ /' \
+ | asttable -c'arith $1 $2 wcstoimg' \
+ --wcsfile=$inputs --wcshdu=$hdu)
+ xcenter=$(echo $xy | awk '{print $1}');
+ ycenter=$(echo $xy | awk '{print $2}');
+
+ fi
+fi
+
+
+
+
+
+# Calculate the maximum radius
+# ----------------------------
+#
+# If the user didn't set the '--rmax' parameter, then compute the maximum
+# radius possible on the image.
+#
+# If the user has not given any maximum radius, we give the most reliable
+# maximum radius (where the full circumference will be within the
+# image). If the radius goes outside the image, then the measurements and
+# calculations can be biased, so when the user has not provided any maximum
+# radius, we should only confine ourselves to a radius where the results
+# are reliable.
+#
+# Y--------------
+# | | The maximum radius (to ensure the profile
+# y |........* | lies within the image) is the smallest
+# | . | one of these values:
+# | . | x, y, X-x, Y-y
+# --------------
+# 0 x X
+#
+if [ x"$rmax" = x ]; then
+ rmax=$(astfits $inputs --hdu=$hdu \
+ | awk '/^NAXIS1/{X=$3} /^NAXIS2/{Y=$3} \
+ END{ x='$xcenter'; y='$ycenter'; \
+ printf("%s\n%s\n%s\n%s", x, y, X-x, Y-y); }' \
+ | aststatistics --minimum )
+fi
+
+
+
+
+
+# Define the final output file and temporal directory
+# ---------------------------------------------------
+#
+# Here, it is defined the final output file containing the radial profile.
+# If the user has defined a specific path/name for the output, it will be
+# used for saving the output file. If the user does not specify a output
+# name, then a default value containing the center and mode will be
+# generated.
+bname_prefix=$(basename $inputs | sed 's/\.fits/ /' | awk '{print $1}')
+defaultname=$(pwd)/"$bname_prefix"_radial_profile_$mode"_$xcenter"_"$ycenter"
+if [ x$output = x ]; then output="$defaultname.fits"; fi
+
+# Construct the temporary+if [ x$tmpdir = x ]; then tmpdir=$defaultname; fi
+if [ -d $tmpdir ]; then junk=1; else mkdir $tmpdir; fi
+
+
+
+
+
+# Crop image
+# ----------
+#
+# Crop the input image around the desired point so we can continue
+# processing only on those pixels (we do not need the other pixels).
+#+crop=$tmpdir/crop.fits
+cropwidth=$(echo $rmax | awk '{print $1*2+1}')
+astcrop $inputs --hdu=$hdu --center=$xcenter,$ycenter --mode=img \
+ --width=$cropwidth --output=$crop $quiet
+dxy=$(astfits $crop -h1 \
+ | grep ICF1PIX \
+ | sed -e"s/'/ /g" -e's/\:/ /g' -e's/,/ /' \
+ | awk '{print $3-1, $5-1}+
+
+
+# Over-sample the input if necessary
+# ----------------------------------
+values=$tmpdir/values.fits
+if [ x$oversample = x ]; then
+ ln -fs $crop $values
+else
+ astwarp $crop --scale=$oversample,$oversample -o$values
+ xcenter=$(echo $xcenter | awk '{print '$oversample'*$1}')
+ ycenter=$(echo $ycenter | awk '{print '$oversample'*$1}')
+ rmax=$(echo $rmax | awk '{print '$oversample'*$1}')
+fi
+
+
+
+
+# Generate the apertures image
+# ----------------------------
+#
+# The apertures image is generated using MakeProfiles with the parameters
+# specified in the echo statement:
+#
+# 1 -- ID of profile (irrelevant here!)
+# xcenter -- X center position (in pixels).
+# ycenter -- Y center position (in pixels).
+# 7 -- Type of the profiles (radial distance).
+# 1 -- The Sersic or Moffat index (irrelevant here!).+aperturesraw=$tmpdir/apertures-raw.fits
+echo "1 $xcenter $ycenter 7 $rmax 1 $positionangle $axisratio 1 1" \
+ | astmkprof --background=$values --backhdu=1 --mforflatpix \
+ --mode=img --clearcanvas --type=int16 \
+ --circumwidth=1 --replace --output=$aperturesraw \
+ $quiet
+
+
+
+
+
+# Fill the central pixel(s)
+# -------------------------
+#
+# The central pixel(s) have a distance of 0! So we need to add a single
+# value to all the profile pixels (but keep the outer parts at 0).
+apertures=$tmpdir/apertures.fits
+astarithmetic $aperturesraw set-i \
+ i 0 ne 1 fill-holes set-good \
+ i good i 1 + where -o$apertures
+
+
+
+
+
+# Extract each measurement column(s)
+# ----------------------------------
+#
+# The user gives each desired MakeCatalog option name as a value to the
+# '--measure' option here as a comma-separated list of values. But we want
+# to feed them into MakeCatalog (which needs each one of them to be
+# --------------------------------------+
+
+
+
+
+# Obtain the radial profile
+# -------------------------
+#+cat=$tmpdir/catalog.fits
+astmkcatalog $apertures -h1 --valuesfile=$values --valueshdu=1 \
+ --ids $finalmeasure $finalsigmaclip --output=$cat \
+ $quiet
+
+
+
+
+
+# Prepare the final output
+# ------------------------
+#
+# The raw MakeCatalog output isn't clear for the users of this script (for
+# example the radius column is called 'OBJ_ID'!). Also, when oversampling
+# is requested we need to divide the radii by the over-sampling factor.
+#
+# But before anything, we need to set the options to print the other
+# columns untouched (we only want to change the first column).
+restcols=$(astfits $cat -h1 \
+ | awk '/^TFIELDS/{for(i=2;i<=$3;++i) printf "-c%d ", i}')
+if [ x"$oversample" = x ]; then
+ asttable $cat -c'arith OBJ_ID float32 1 -' $restcols -o$output \
+ --colmetadata=1,RADIUS,pix,"Radial distance"
+else
+ asttable $cat -c'arith OBJ_ID float32 '$oversample' /' $restcols \
+ -o$output --colmetadata=ARITH_2,RADIUS,pix,"Radial distance"
+fi
+
+
+
+
+
+# Remove temporal files
+# ---------------------
+#
+# If the user does not specify to keep the temporal files with the option
+# `--keeptmp', then remove the whole directory.
+if [ $keeptmp = 0 ]; then
+ rm -rf $tmpdir
+fi
diff --git a/bin/segment/ui.c b/bin/segment/ui.c
index 773c323..62f8f0f 100644
--- a/bin/segment/ui.c
+++ b/bin/segment/ui.c
@@ -411,8 +411,10NULL, GAL_TYPE_FLOAT32,
- p->cp.minmapsize, p->cp.quietmmap);
- p->input->wcs = gal_wcs_read(p->inputname, p->cp.hdu, 0, 0,
+ p->cp.minmapsize,
+ p->cp.quietmmap);statistics/statistics.c b/bin/statistics/statistics.c
index 48986eb..afacdc0 100644
--- a/bin/statistics/statistics.c
+++ b/bin/statistics/statistics.c
@@ -832,7 +832,8 @@ histogram_2d(struct statisticsparams *p)
cunit[0] = p->input->unit; cunit[1] = p->input->next->unit;
ctype[0] = histogram_2d_set_ctype(p->input->name, "X");
ctype[1] = histogram_2d_set_ctype(p->input->next->name, "Y");
- img->wcs=gal_wcs_create(crpix, crval, cdelt, pc, cunit, ctype, 2);
+ img->wcs=gal_wcs_create(crpix, crval, cdelt, pc, cunit, ctype, 2,
+ p->cp.wcslinearmatrix);
/* Write the output. */
output=statistics_output_name(p, suf, &isfits);
diff --git a/bin/statistics/ui.c b/bin/statistics/ui.c
index 0b2ad5c..7c2b7fc 100644
--- a/bin/statistics/ui.c
+++ b/bin/statistics/ui.c
@@ -971,7 +971,8 @@ ui_preparations(struct statisticsparams *p)
p->inputformat=INPUT_FORMAT_IMAGE;
p->input=gal_array_read_one_ch(p->inputname, cp->hdu, NULL,
cp->minmapsize, p->cp.quietmmap);
- p->input->wcs=gal_wcs_read(p->inputname, cp->hdu, 0, 0,
+ p->input->wcs=gal_wcs_read(p->inputname, cp->table/arithmetic.c b/bin/table/arithmetic.c
index dfa576c..b964535 100644
--- a/bin/table/arithmetic.c
+++ b/bin/table/arithmetic.c
@@ -159,7 +159,8 @@ arithmetic_init_wcs(struct tableparams *p, char *operator)
"for the '%s' operator", operator);
/* Read the WCS. */
- p->wcs=gal_wcs_read(p->wcsfile, p->wcshdu, 0, 0, &p->nwcs);
+ p->wcs=gal_wcs_read(p->wcsfile, p->wcshdu, p->cp.wcslinearmatrix,
+ 0, 0, &p->nwcs);
if(p->wcs==NULL)
error(EXIT_FAILURE, 0, "%s (hdu: %s): no WCS could be read by "
"WCSLIB", p->wcsfile, p->wcshdu);
diff --git a/bin/table/table.c b/bin/table/table.c
index 86fda2b..912e408 100644
--- a/bin/table/table.c
+++ b/bin/table/table.c
@@ -661,7 +661,7 @@ table_select_by_position(struct tableparams *p)
error(EXIT_SUCCESS, 0, "'--rowrandom' not activated because "
"the number of rows in the table at this stage (%zu) "
"is smaller than the number of requested random rows "
- "(%zu). You can supress this message with '--quiet'",
+ "(%zu). You can suppress this message with '--quiet'",
p->table->size, p->rowrandom);
return;
}
diff --git a/bin/table/ui.c b/bin/table/ui.c
index adbd834..ece4e24 100644
--- a/bin/table/ui.c
+++ b/bin/table/ui.c
@@ -1273,7 +1273,7 @@ ui_read_check_inputs_setup(int argc, char *argv[], struct
tableparams *p)
printf("Parameters used for '--randomrows':\n");
printf(" - Random number generator name: %s\n", p->rng_name);
printf(" - Random number generator seed: %lu\n", p->rng_seed);
- printf("(use '--quiet' to supress this starting message)\n");
+ printf("(use '--quiet' to suppress this starting message)\n");
}
}
diff --git a/bin/warp/ui.c b/bin/warp/ui.c
index a91fb14..72659c1 100644
--- a/bin/warp/ui.c
+++ b/bin/warp/ui.c
@@ -352,7 +352,8 @@ ui_check_options_and_arguments(struct warpparams *p)
p->cp.quietmmap);
/* Read the WCS and remove one-element wide dimension(s). */
- p->input->wcs=gal_wcs_read(p->inputname, p->cp.hdu, p->hstartwcs,
+ p->input->wcs=gal_wcs_read(p->inputname, p->cp.hdu,
+ p->cp.wcslinearmatrix, p->hstartwcs,
p->hendwcs, &p->input->nwcs);
p->input->ndim=gal_dimension_remove_extra(p->input->ndim,
p->input->dsize,
diff --git a/bootstrap.conf b/bootstrap.conf
index bbf7318..e2f2630 100644
--- a/bootstrap.conf
+++ b/bootstrap.conf
@@ -123,14 +123,6 @@ bootstrap_post_import_hook()
done
fi
- # With Autoconf 2.70, the 'as_echo' has been depreciated and will cause
- # an error with autoreconf. But unfortunately the ax_pthread test still
- # uses it. So until it is fixed there, we need to manually correct it
- # here.
- sed -e's|\$as_echo \"\$ac_link\"|AS_ECHO([\"\$ac_link\"])|' \
- $m4_base/ax_pthread.m4 > $m4_base/ax_pthread_tmp.m4
- mv $m4_base/ax_pthread_tmp.m4 $m4_base/ax_pthread.m4
-
# Hack in 'AC_LIB_HAVE_LINKFLAGS' so it doesn't search for shared
# libraries when '--disable-shared' is used.
sed 's|if test -n \"$acl_shlibext\"; then|if test -n \"\$acl_shlibext\" -a
\"X$enable_shared\" = \"Xyes\"; then|' bootstrapped/m4/lib-link.m4 >
bootstrapped/m4/lib-link_tmp.m4
diff --git a/configure.ac b/configure.ac
index 173763d..bd2e865 100644
--- a/configure.ac
+++ b/configure.ac
@@ -555,6 +555,12 @@ AC_DEFINE_UNQUOTED([GAL_CONFIG_HAVE_WCSLIB_OBSFIX],
[$has_wcslib_obsfix],
[WCSLIB comes with OBSFIX macro])
AC_SUBST(HAVE_WCSLIB_OBSFIX, [$has_wcslib_obsfix])
+# If the WCS library has the 'wcsccs' function.
+AC_CHECK_LIB([wcs], [wcsccs], [has_wcslib_wcsccs=1],
+ [has_wcslib_wcsccs=0; anywarnings=yes], [-lcfitsio -lm])
+AC_DEFINE_UNQUOTED([GAL_CONFIG_HAVE_WCSLIB_WCSCCS], [$has_wcslib_wcsccs],
+ [WCSLIB comes with wcsccs])
+AC_SUBST(HAVE_WCSLIB_WCSCCS, [$has_wcslib_wcsccs])
# If the pthreads library has 'pthread_barrier_wait'.
AC_CHECK_LIB([pthread], [pthread_barrier_wait], [has_pthread_barrier=1],
@@ -1115,6 +1121,17 @@ AS_IF([test x$enable_guide_message = xyes],
AS_ECHO([" operations you can ignore this warning."])
AS_ECHO([]) ])
+ AS_IF([test "x$has_wcslib_wcsccs" = "x0"],
+ [dependency_notice=yes
+ AS_ECHO([" - WCSLIB
( version"])
+ AS_ECHO([" on this system doesn't support conversion of
coordinate systems"])
+ AS_ECHO([" (through the 'wcsccs' function that was
introduced in WCSLIB 7.5, "])
+ AS_ECHO([" March 2021). For example converting from
equatorial J2000 to"])
+ AS_ECHO([" Galactic coordinates). This build won't crash but
the related"])
+ AS_ECHO([" functionalities in Gnuastro will be disabled. If
you don't need"])
+ AS_ECHO([" such operations you can ignore this warning."])
+ AS_ECHO([]) ])
+diff --git a/doc/Makefile.am b/doc/Makefile.am
index 12dc957..c0c4a43 100644
--- a/doc/Makefile.am
+++ b/doc/Makefile.am
@@ -153,6 +153,7 @@ dist_man_MANS = $(MAYBE_ARITHMETIC_MAN)
$(MAYBE_BUILDPROG_MAN) \
$(MAYBE_MKCATALOG_MAN) $(MAYBE_MKNOISE_MAN) $(MAYBE_MKPROF_MAN) \
$(MAYBE_NOISECHISEL_MAN) $(MAYBE_QUERY_MAN) $(MAYBE_SEGMENT_MAN) \
$(MAYBE_STATISTICS_MAN) $(MAYBE_TABLE_MAN) $(MAYBE_WARP_MAN) \
+ man/astscript-ds9-region.1 man/astscript-radial-profile.1 \
man/astscript-sort-by-night.1
@@ -224,11 +225,6 @@ man/astquery.1: $(top_srcdir)/bin/query/args.h
$(ALLMANSDEP)
$(MAYBE_HELP2MAN) -n "query remote data servers and download" \
--libtool $(toputildir)/query/astquery
-man/astscript-sort-by-night.1: $(top_srcdir)/bin/script/sort-by-night.in \
- $(ALLMANSDEP)
- $(MAYBE_HELP2MAN) -n "Sort input FITS files by night" \
- --libtool $(toputildir)/script/astscript-sort-by-night
-
man/astsegment.1: $(top_srcdir)/bin/segment/args.h $(ALLMANSDEP)
$(MAYBE_HELP2MAN) -n "segmentation based on signal structure" \
--libtool $(toputildir)/segment/astsegment
@@ -248,3 +244,23 @@ man/asttable.1: $(top_srcdir)/bin/table/args.h
$(ALLMANSDEP)
man/astwarp.1: $(top_srcdir)/bin/warp/args.h $(ALLMANSDEP)
$(MAYBE_HELP2MAN) -n "warp (transform) input dataset" \
--libtool $(toputildir)/warp/astwarp
+
+
+
+
+
+# The Scripts:
+man/astscript-ds9-region.1: $(top_srcdir)/bin/script/ds9-region.in \
+ $(ALLMANSDEP)
+ $(MAYBE_HELP2MAN) -n "Create an SAO DS9 region file from a table" \
+ --libtool $(toputildir)/script/astscript-ds9-region
+
+man/astscript-radial-profile.1: $(top_srcdir)/bin/script/radial-profile.in \
+ $(ALLMANSDEP)
+ $(MAYBE_HELP2MAN) -n "Create a radial profile of an object in an image"
\
+ --libtool
$(toputildir)/script/astscript-radial-profile
+
+man/astscript-sort-by-night.1: $(top_srcdir)/bin/script/sort-by-night.in \
+ $(ALLMANSDEP)
+ $(MAYBE_HELP2MAN) -n "Sort input FITS files by night" \
+ --libtool $(toputildir)/script/astscript-sort-by-night
diff --git a/doc/announce-acknowledge.txt b/doc/announce-acknowledge.txt
index 8ff3cba..aabddfd 100644
--- a/doc/announce-acknowledge.txt
+++ b/doc/announce-acknowledge.txt
@@ -1,8 +1,11 @@
Alphabetically ordered list to acknowledge in the next release.
Mark Calabretta
+Sepideh Eskandarlou
Raul Infante-Sainz
Alberto Madrigal
+ 54efea1..f8241ad 100644
--- a/doc/gnuastro.texi
+++ b/doc/gnuastro.texi
@@ -107,7 +107,7-* astscript-make-ds9-reg: (gnuastro)Invoking astscript-make-ds9-reg. Options
to this script
+* astscript-ds9-region: (gnuastro)Invoking astscript-ds9-region. Options to
this script
@end direntry272,12 +273,9 @@ Detecting large extended targets-
-Downloading and validating input data
-
-* NoiseChisel optimization:: Optimize NoiseChisel to dig very deep.
-* Achieved surface brightness level:: Measure how much you detected.
+* Extract clumps and objects:: Find sub-structure over the detections.
Installation
@@ -328,7 +326404,6 +401,7 @@ ConvertTypeTable
@@ -481,8 +479Statistics
@@ -527,11 +523,20 @@ Invoking Segment
MakeCatalog543,14 +548Modeling and fitting
* MakeProfiles:: Making mock galaxies and stars.
@@ -560,7 +557,6 @@ MakeProfiles
* Modeling basics:: Astronomical modeling basics.
* If convolving afterwards:: Considerations for convolving later.
-* Brightness flux magnitude:: About these measures of energy.
* Profile magnitude:: Definition of total profile magnitude.
* Invoking astmkprof:: Inputs and Options for MakeProfiles.
@@ -608,6 +604
+Sort FITS files by night
+
+* Invoking astscript-sort-by-night:: Inputs and outputs to this script.
+
+Generate radial profile
+
+* Invoking astscript-radial-profile:: How to call astscript-radial-profile
+
+SAO DS9 region files from table
+
+* Invoking astscript-ds9-region:: How to call astscript-ds9-region
+
Library
* Review of library fundamentals:: Guide on libraries and linking.
@@ -844,7 +858,7 @@ In @ref{Tutorials} some real life examples of how these
programs might be used a
@node Science and its tools, Your rights, Quick start, Introduction
-@section Science and its tools
+@section Gnuastro manifesto: Science and its tools
History of science indicates that there are always inevitably unseen faults,
hidden assumptions, simplifications and approximations in all our theoretical
models, data acquisition and analysis techniques.
It is precisely these that will ultimately allow future generations to advance
the existing experimental and theoretical knowledge through their new solutions
and corrections.
@@ -880,7 +894,7 @@ This kind of subjective experience is prone to serious
misunderstandings about t
However, software engineers have been dealing with such issues for a long time.
There are thus software management solutions that allow us to supplement
papers with all the details necessary to exactly reproduce the result.
-For example see @url{ zenodo.1163746}
and @url{ zenodo.1164774} and this @url{
general discussion}.}.
+For example see Akhlaghi et al. (2021,
@url{
Larger quote is given at the start of the PDF (for print) version of this
book.}.
@@ -916,11 +930,7 @@ Therefore, while it empowers the privileged individual who
has access to it, it
Exactly at the opposite end of the spectrum, Gnuastro's source code is
released under the GNU general public license (GPL) and this book is released
under the GNU free documentation license.
You are therefore free to distribute any software you create using parts of
Gnuastro's source code or text, or figures from this book, see @ref{Your
rights}.
-With these principles in mind, Gnuastro's developers aim to impose the
-minimum requirements on you (in computer science, engineering and even the
-mathematics behind the tools) to understand and modify any step of Gnuastro
-if you feel the need to do so, see @ref{Why C} and @ref{Program design
-philosophy}.
+With these principles in mind, Gnuastro's developers aim to impose the minimum
requirements on you (in computer science, engineering and even the mathematics
behind the tools) to understand and modify any step of Gnuastro if you feel the
need to do so, see @ref{Why C} and @ref{Program design philosophy}.
@cindex Brahe, Tycho
@cindex Galileo, Galilei
@@ -941,9 +951,16 @@ The same is true today: science cannot progress with a
black box, or poorly rele
The source code of a research is the new (abstractified) communication
language in science, understandable by humans @emph{and} computers.
Source code (in any programming language) is a language/notation designed to
express all the details that would be too tedious/long/frustrating to report in
spoken languages like English, similar to mathematic notation.
+@quotation
+An article about computational science [almost all sciences today] ... is not
the scholarship itself, it is merely advertising of the scholarship.
+The Actual Scholarship is the complete software development environment and
the complete set of instructions which generated the figures.
+@author Buckheit & Donoho, Lecture Notes in Statistics, Vol 103, 1996
+@end quotation
+
A scientific paper will not even be reviewed by any respectable journal if its
written in a poor language/English.
A similar level of quality assessment is thus increasingly becoming necessary
regarding the codes/methods used to derive the results of a scientific paper.
+For more on this, please see Akhlaghi et al. (2021) at
@url{
@cindex Ken Thomson
@cindex Stroustrup, Bjarne
@@ -975,7 +992,7 @@ Our future discoveries must be looked for in the sixth
place of decimals.
@cindex Puzzle solving scientist
@cindex Scientist, puzzle solver
-If scientists are considered to be more than mere puzzleToday there is a wealth of raw telescope images ready (mostly for free) at the
finger tips of anyone who is interested with a fast enough internet connection
to download them.
The only thing lacking is new ways to analyze this data and dig out the
treasure that is lying hidden in them to existing methods and techniques.
@@ -1392,6 +14091649,10 +1670,11 @@ $ astmkprof -P
[[[ ... Truncated lines ... ]]]
# Columns, by info (see `--searchin'), or number (starting from 1):
- ccol 2 # Coordinate columns (one call for each dimension).
- ccol 3 # Coordinate columns (one call for each dimension).
+ ccol 2 # Coord. columns (one call for each dim.).
+ ccol 3 # Coord. columns (one call for each dim.).
fcol 4 # sersic (1), moffat (2), gaussian (3),
- # point (4), flat (5), circumference (6).
+ # point (4), flat (5), circumference (6),
+ # distance (7), radial-table (8).
rcol 5 # Effective radius or FWHM in pixels.
ncol 6 # Sersic index or Moffat beta.
pcol 7 # Position angle.
@@ -1884,9 +1906,9 '--section' accepts
-# inclusive coordinates, so the start of start of the section must be
-# one pixel larger than its end.
+# Crop the edges out (dimmed during convolution). '--section'
+# accepts inclusive coordinates, so the start of the section
+# must be one pixel larger than its end.
st_edge=$(( edge + 1 ))
astcrop "$base"_convolved_scaled.fits --zeroisnotblank \
--mode=img --section=$st_edge:*-$edge,$st_edge:*-$edge
@@ -2233,6 +2255
@@ -3075,7 +3106,7 @@ We are now ready to finally run NoiseChisel on the three
filters and keep the ou
$ rm *.fits
$ mkdir nc
$ for f in f105w f125w f160w; do \
- astnoisechisel flat-ir/xdf-$f.fits --output=nc/xdf-$f.fits
+ astnoisechisel flat-ir/xdf-$f.fits --output=nc/xdf-$f.fits; \
done
@end example
@@ -3171 clump in a FITS table.
@@ -32122322424233,7 +4278,9 @@ Due to its more peculiar low surface brightness
structure/features, we'll focus
@menu+* Extract clumps and objects:: Find sub-structure over the detections.
@end menu
@node Downloading and validating input data, NoiseChisel optimization,
Detecting large extended targets, Detecting large extended targets
@@ -4318,13 +4365,7 @@ Here, we don't need the compressed file any more, so
we'll just let @command{bun
$ bunzip2 r.fits.bz2
@end example
-
-@menu
-* NoiseChisel optimization:: Optimize NoiseChisel to dig very deep.
-* Achieved surface brightness level:: Measure how much you detected.
-@end menu
-
-@node NoiseChisel optimization, Achieved surface brightness level, Downloading
and validating input data, Detecting large extended targets
+@node NoiseChisel optimization, Image surface brightness limit, Downloading
and validating input data, Detecting large extended targets
@subsection NoiseChisel optimization
In @ref{Detecting large extended targets} we downloaded the single exposure
SDSS image.
Let's see how NoiseChisel operates on it with its default parameters:
@@ -4568,19 +4609,251 @@ However, given the many problems in existing ``smart''
solutions, such automatic
So even when they are implemented, we would strongly recommend quality checks
for a robust analysis.
@end cartouche
-@node Achieved surface brightness level, , NoiseChisel optimization,
Detecting large extended targets
-@subsection Achieved surface brightness level
+@node Image surface brightness limit, Achieved surface brightness level,
NoiseChisel optimization, Detecting large extended targets
+@subsection Image surface brightness limit
+@cindex Surface brightness limit
+@cindex Limit, surface brightness
In @ref{NoiseChisel optimization} we showed how to customize NoiseChisel for a
single-exposure SDSS image of the M51 group.
-Let's measure how deep we carved the signal out of noise.
-For this measurement, we'll need to estimate the average flux on the outer
edges of the detection.
-Fortunately all this can be done with a few simple commands (and no
higher-level language mini-environments like Python or IRAF) using
@ref{Arithmetic} and @ref{MakeCatalog}.
+When presenting your detection results in a paper or scientific conference,
usually the first thing that someone will ask (if you don't explicity say it!),
is the dataset's @emph{surface brightness limit} (a standard measure of the
noise level), and your target's surface brightness (a measure of the signal,
either in the center or outskirts, depending on context).
+For more on the basics of these important concepts please see @ref{Quantifying
measurement limits}).
+Here, we'll measure these values for this image.
+
+Let's start by measuring the surface brightness limit masking all the detected
pixels and have a look at the noise distribution with the
@command{astarithmetic} and @command{aststatistics} commands below.
+
+@example
+$ astarithmetic r_detected.fits -hINPUT-NO-SKY set-in \
+ r_detected.fits -hDETECTIONS set-det \
+ in det nan where -odet-masked.fits
+$ ds9 det-masked.fits
+$ aststatistics det-masked.fits
+@end example
+
+@noindent
+From the ASCII histogram, we see that the distribution is roughly symmetric.
+We can also quantify this by measuring the skewness (difference between mean
and median, divided by the standard deviation):
+
+@example
+$ aststatistics det-masked.fits --mean --median --std \
+ | awk '@{print ($1-$2)/$3@}'
+@end example
+
+@noindent
+Showing that the mean is larger than the median by @mymath{0.08\sigma}, in
other words, as we saw in @ref{NoiseChisel optimization}, a very small residual
signal still remains in the undetected regions and it was up to you as an
exercise to improve it.
+So let's continue with this value.
+Now, we will use the masked image and the surface brightness limit equation in
@ref{Quantifying measurement limits} to measure the @mymath{3\sigma} surface
brightness limit over an area of @mymath{25 \rm{arcsec}^2}:
+
+@example
+$ nsigma=3
+$ zeropoint=22.5
+$ areaarcsec2=25
+$ std=$(aststatistics det-masked.fits --sigclip-std)
+$ pixarcsec2=$(astfits det-masked.fits --pixelscale --quiet \
+ | awk '@{print $3*3600*3600@}')
+$ astarithmetic --quiet $nsigma $std x \
+ $areaarcsec2 $pixarcsec2 x \
+ sqrt / $zeropoint counts-to-mag
+26.0241
+@end example
+
+The customizable steps above are good for any type of mask.
+For example your field of view may contain a very deep part so you need to
mask all the shallow parts @emph{as well as} the detections before these steps.
+But when your image is flat (like this), there is a much simpler method to
obtain the same value through MakeCatalog (when the standard deviation image is
made by NoiseChisel).
+NoiseChisel has already calculated the minimum (@code{MINSTD}), maximum
(@code{MAXSTD}) and median (@code{MEDSTD}) standard deviation within the tiles
during its processing and has stored them as FITS keywords within the
@code{SKY_STD} HDU.
+You can see them by piping all the keywords in this HDU into @command{grep}.
+In Grep, each @samp{.} represents one character that can be anything so
@code{M..STD} will match all three keywords mentioned above.
+
+@example
+$ astfits r_detected.fits --hdu=SKY_STD | grep 'M..STD'
+@end example
+
+The @code{MEDSTD} value is very similar to the standard deviation derived
above, so we can safely use it instead of having to mask and run Statistics.
+In fact, MakeCatalog also uses this keyword and will report the dataset's
@mymath{n\sigma} surface brightness limit as keywords in the output (not as
measurement columns, since its related to the noise, not labeled signal):
+
+@example
+$ astmkcatalog r_detected.fits -hDETECTIONS --output=sbl.fits \
+ --forcereadstd --ids
+@end example
+
+@noindent
+Before looking into the measured surface brightness limits, let's review some
important points about this call to MakeCatalog first:
+@itemize
+@item
+We are only concerned with the noise (not the signal), so we don't ask for any
further measurements, because they can un-necessarily slow it down.
+However, MakeCatalog requires at least one column, so we'll only ask for the
@option{--ids} column (which doesn't need any measurement!).
+The output catalog will therefore have a single row and a single column, with
1 as its value@footnote{Recall that NoiseChisel's output is a binary image:
0-valued pixels are noise and 1-valued pixel are signal.
+NoiseChisel doesn't identify sub-structure over the signal, this is the job of
Segment, see @ref{Extract clumps and objects}.}.
+@item
+If we don't ask for any noise-related column (for example the signal-to-noise
ratio column with @option{--sn}, among other noise-related columns),
MakeCatalog is not going to read the noise standard deviation image (again, to
speed up its operation when it is redundant).
+We are thus using the @option{--forcereadstd} option (short for ``force read
standard deviation image'') here so it is ready for the surface brightness
limit measurements that are written as keywords.
+@end itemize
+
+With the command below you can see all the keywords that were measured with
the table.
+Notice the group of keywords that are under the ``Surface brightness limit
(SBL)'' title.
+
+@example
+$ astfits sbl.fits -h1
+@end example
+
+@noindent
+Since all the keywords of interest here start with @code{SBL}, we can get a
more cleaner view with this command.
+
+@example
+$ astfits sbl.fits -h1 | grep ^SBL
+@end example
+
+Notice how the @code{SBLSTD} has the same value as NoiseChisel's @code{MEDSTD}
above.
+Using @code{SBLSTD}, MakeCatalog has determined the @mymath{n\sigma} surface
brightness limiting magnitude in these header keywords.
+The multiple of @mymath{\sigma}, or @mymath{n}, is the value of the
@code{SBLNSIG} keyword which you can change with the @option{--sfmagnsigma}.
+The surface brightness limiting magnitude within a pixel (@code{SBLNSIG}) and
within a pixel-agnostic area of @code{SBLAREA} arcsec@mymath{^2} are stored in
@code{SBLMAG}.
+
+@cindex SDSS
+@cindex Nanomaggy
+@cindex Zero point magnitude
+You will notice that the two surface brightness limiting magnitudes above have
values around 3 and 4 (which is not correct!).
+This is because we haven't given a zero point magnitude to MakeCatalog, so it
uses the default value of @code{0}.
+SDSS image pixel values are calibrated in units of ``nanomaggy'' which are
defined to have a zero point magnitude of 22.5@footnote{From
@url{
+So with the first command below we give the zero point value and with the
second we can see the surface brightness limiting magnitudes with the correct
values (around 25 and 26)
+
+@example
+$ astmkcatalog r_detected.fits -hDETECTIONS --zeropoint=22.5 \
+ --output=sbl.fits --forcereadstd --ids
+$ astfits sbl.fits -h1 | grep ^SBL
+@end example
+
+As you see from @code{SBLNSIG} and @code{SBLAREA}, the default multiple of
sigma is 1 and the default area is 1 arcsec@mymath{^2}.
+Usually higher values are used for these two parameters.
+Following the manual example we did above, you can ask for the multiple of
sigma to be 3 and the area to be 25 arcsec@mymath{^2}:
+
+@example
+$ astmkcatalog r_detected.fits -hDETECTIONS --zeropoint=22.5 \
+ --output=sbl.fits --sfmagarea=25 --sfmagnsigma=3 \
+ --forcereadstd --ids
+$ astfits sbl.fits -h1 | awk '/^SBLMAG /@{print $3@}'
+26.02296
+@end example
+
+You see that the value is identical to the custom surface brightness limiting
magnitude we measured above (a difference of @mymath{0.00114} magnitudes is
negligible and hundreds of times larger than the typical errors in the zero
point magnitude or magnitude measurements).
+But it is much more easier to have MakeCatalog do this measurement, because
these values will be appended (as keywords) into your final catalog of objects
within that image.
+
+@cartouche
+@noindent
+@strong{Custom STD for MakeCatalog's Surface brightness limit:} You can
manually change/set the value of the @code{MEDSTD} keyword in your input STD
image with @ref{Fits}:
+
+@example
+$ std=$(aststatistics masked.fits --sigclip-std)
+$ astfits noisechisel.fits -hSKY_STD --update=MEDSTD,$std
+@end example
+
+With this change, MakeCatalog will use your custom standard deviation for the
surface brightness limit.
+This is necessary in scenarios where your image has multiple depths and during
your masking, you also mask the shallow regions (as well as the detections of
course).
+@end cartouche
+
+We have successfully measured the image's @mymath{3\sigma} surface brightness
limiting magnitude over 25 arcsec@mymath{^2}.
+However, as discussed in @ref{Quantifying measurement limits} this value is
just an extrapolation of the per-pixel standard deviaiton.
+Issues like correlated noise will cause the real noise over a large area to be
different.
+So for a more robust measurement, let's use the upper-limit magnitude of
similarly sized region.
+For more on the upper-limit magnitude, see the respective item in
@ref{Quantifying measurement limits}.
+
+In summary, the upper-limit measurements involve randomly placing the
footprint of an object in undetected parts of the image many times.
+This resuls in a random distribution of brightness measurements, the standard
deviation of that distribution is then converted into magnitudes.
+To be comparable with the results above, let's make a circular aperture that
has an area of 25 arcsec@mymath{^2} (thus with a radius of @mymath{2.82095}
arcsec).
+
+@example
+zeropoint=22.5
+r_arcsec=2.82095
+
+## Convert the radius (in arcseconds) to pixels.
+r_pixel=$(astfits r_detected.fits --pixelscale -q \
+ | awk '@{print '$r_arcsec'/($1*3600)@}')
+
+## Make circular aperture at pixel (100,100) position is irrelevant.
+echo "1 100 100 5 $r_pixel 0 0 1 1 1" \
+ | astmkprof --background=r_detected.fits \
+ --clearcanvas --mforflatpix --type=uint8 \
+ --output=lab.fits
+
+## Do the upper-limit measurement, ignoring all NoiseChisel's
+## detections as a mask for the upper-limit measurements.
+@end example
+
+The @file{sbl.fits} catalog now contains the upper-limit surface brightness
for a circle with an area of 25 arcsec@mymath{^2}.
+You can check the value with the command below, but the great thing is that
now you have both the surface brightness limiting magnitude in the headers
discussed above, and the upper-limit surface brigthness within the table.
+You can also add more profiles with different shapes and sizes if necessary.
+Of course, you can also use @option{--upperlimitsb} in your actual science
objects and clumps to get an object-specific or clump-specific value.
+
+@example
+$ asttable sbl.fits -cUPPERLIMIT_SB
+25.9119
+@end example
+
+@cindex Random number generation
+@cindex Seed, random number generator
+@noindent
+You will get a slightly different value from the command above.
+In fact, if you run the MakeCatalog command again and look at the measured
upper-limit surface brightness, it will be slightly different with your first
trial!
+Please try exactly the same MakeCatalog command above a few times to see how
it changes.
+
+This is because of the @emph{random} factor in the upper-limit measurements:
every time you run it, different random points will be checked, resulting in a
slightly different distribution.
+You can decrease the random scatter by increasing the number of random checks
(for example setting @option{--upnum=100000}, compared to 1000 in the command
above).
+But this will be slower and the results won't be exactly reproducible.
+The only way to ensure you get an identical result later is to fix the random
number generator function and seed like the command below@footnote{You can use
any integer for the seed. One recommendation is to run MakeCatalog without
@option{--envseed} once and use the randomly generated seed that is printed on
the terminal.}.
+This is a very important point regarding any statistical process involving
random numbers, please see @ref{Generating random numbers}.
+
+@example
+export GSL_RNG_TYPE=ranlxs1
+export GSL_RNG_SEED=1616493518 --envseed
+@end example
+
+But where do all the random apertures of the upper-limit measurement fall on
the image?
+It is good to actually inspect their location to get a better understanding
for the process and also detect possible bugs/biases.
+When MakeCatalog is run with the @option{--checkuplim} option, it will print
all the random locations and their measured brightness as a table in a file
with the suffix @file{_upcheck.fits}.
+With the first command below you can use Gnuastro's @command{asttable} and
@command{astscript-ds9-region} to convert the successful aperture locations
into a DS9 region file, and with the second can load the region file into the
detections and sky-subtracted image to visually see where they are.
+
+@example
+## Create a DS9 region file from the check table (activated
+## with '--checkuplim')
+asttable lab_upcheck.fits --noblank=RANDOM_SUM \
+ | astscript-ds9-region -c1,2 --mode=img \
+ --radius=$r_pixel
+
+## Have a look at the regions in relation with NoiseChisel's
+## detections.
+ds9 r_detected.fits[INPUT-NO-SKY] -regions load ds9.reg
+ds9 r_detected.fits[DETECTIONS] -regions load ds9.reg
+@end example
+
+In this example, we were looking at a single-exposure image that has no
correlated noise.
+Because of this, the surface brightness limit and the upper-limit surface
brightness are very close.
+They will have a bigger difference on deep datasets with stronger correlated
noise (that are the result of stacking many individual exposures).
+As an exercise, please try measuring the upper-limit surface brightness level
and surface brightness limit for the deep HST data that we used in the previous
tutorial (@ref{General program usage tutorial}).
+
+@node Achieved surface brightness level, Extract clumps and objects, Image
surface brightness limit, Detecting large extended targets
+@subsection Achieved surface brightness level
+
+In @ref{NoiseChisel optimization} we customized NoiseChisel for a
single-exposure SDSS image of the M51 group and in @ref{Image surface
brightness limit} we measured the surface brightness limit and the upper-limit
surface brightness level (which are both measures of the noise level).
+In this section, let's do some measurements on the outer-most edges of the M51
group to see how they relate to the noise measurements found in the previous
section.
@cindex Opening
-First, let's separate each detected region, or give a unique label/counter to
all the connected pixels of NoiseChisel's detection map:
+For this measurement, we'll need to estimate the average flux on the outer
edges of the detection.
+Fortunately all this can be done with a few simple commands using
@ref{Arithmetic} and @ref{MakeCatalog}.
+First, let's separate each detected region, or give a unique label/counter to
all the connected pixels of NoiseChisel's detection map with the command below.
+Recall that with the @code{set-} operator, the popped operand will be given a
name (@code{det} in this case) for easy usage later.
@example
-$ det="r_detected.fits -hDETECTIONS"
-$ astarithmetic $det 2 connected-components -olabeled.fits
+$ astarithmetic r_detected.fits -hDETECTIONS set-det \
+ det 2 connected-components -olabeled.fits
@end example
You can find the label of the main galaxy visually (by opening the image and
hovering your mouse over the M51 group's label).
@@ -4608,8 +4881,16 @@ $ id=$(asttable cat.fits --sort=AREA_FULL --tail=1
--column=OBJ_ID)
$ echo $id
@end example
+@noindent
+We can now use the @code{id} variable to reject all other detections:
+
+@example
+$ astarithmetic labeled.fits $id eq -oonly-m51.fits
+@end example
+
+Open the image and have a look.
To separate the outer edges of the detections, we'll need to ``erode'' the M51
group detection.
-We'll erode three times (to have more pixels and thus less scatter), using a
maximum connectivity of 2 (8-connected neighbors).
+So in the same Arithmetic command as above, we'll erode three times (to have
more pixels and thus less scatter), using a maximum connectivity of 2
(8-connected neighbors).
We'll then save the output in @file{eroded.fits}.
@example
@@ -4620,8 +4901,7 @@ $ astarithmetic labeled.fits $id eq 2 erode 2 erode 2
erode \
@noindent
We'll need the pixels of the M51 group in @code{labeled.fits} two times: once
to do the erosion, another time to find the outer pixel layer.
-To do this (and be efficient and more readable) we'll use the @code{set-i}
operator.
-In the command below, it will save/set/name the pixels of the M51 group as the
`@code{i}'.
+To do this (and be efficient and more readable) we'll use the @code{set-i}
operator (to give this image the name `@code{i}').
In this way we can use it any number of times afterwards, while only reading
it from disk and finding M51's pixels once.
@example
@@ -4634,58 +4914,74 @@ You'll see that the detected edge of the M51 group is
now clearly visible.
You can use @file{edge.fits} to mark (set to blank) this boundary on the input
image and get a visual feeling of how far it extends:
@example
-$ astarithmetic r.fits edge.fits nan where -oedge-masked.fits -h0
+$ astarithmetic r.fits -h0 edge.fits nan where -oedge-masked.fits
@end example
To quantify how deep we have detected the low-surface brightness regions (in
units of signal to-noise ratio), we'll use the command below.
In short it just divides all the non-zero pixels of @file{edge.fits} in the
Sky subtracted input (first extension of NoiseChisel's output) by the pixel
standard deviation of the same pixel.
This will give us a signal-to-noise ratio image.
The mean value of this image shows the level of surface brightness that we
have achieved.
-
You can also break the command below into multiple calls to Arithmetic and
create temporary files to understand it better.
-Applying the @code{not} operator on it, just flips all its pixels.
--In the second line, we are dividing all the non-blank values by
@file{r_detected.fits} (extension @code{SKY_STD}).
-This gives the signal-to-noise ratio for each of the pixels on the boundary.
+Applying the @code{not} operator on it, just flips all its pixels (from
@code{0} to @code{1} and vice-versa).
+Using the @code{where} operator, we are then setting all the newly 1-valued
pixels (pixels that aren't on the edge) to NaN/blank in the sky-subtracted
input image (@file{r_detected.fits}, extension @code{INPUT-NO-SKY}, which we
call @code{skysub}).
+We are then dividing all the non-blank pixels (only those on the edge) by the
sky standard deviation (@file{r_detected.fits}, extension @code{SKY_STD}, which
we called @code{skystd}).
+This gives the signal-to-noise ratio (S/N) for each of the pixels on the
boundary.
Finally, with the @code{meanvalue} operator, we are taking the mean value of
all the non-blank pixels and reporting that as a single number.}.
@example
-$ edge="edge.fits -h1"
-$ skystd="r_detected.fits -hSKY_STD"
-$ skysub="r_detected.fits -hINPUT-NO-SKY"
-$ astarithmetic $skysub $skystd / $edge not nan where \
- meanvalue --quiet
+$ astarithmetic edge.fits -h1 set-edge \
+ r_detected.fits -hSKY_STD set-skystd \
+ r_detected.fits -hINPUT-NO-SKY set-skysub \
+ skysub skystd / edge not nan where meanvalue --quiet
@end example
@cindex Surface brightness
-We have thus detected the wings of the M51 group down to roughly 1/3rd of the
noise level in this image! But the signal-to-noise ratio is a relative
measurement.
+We have thus detected the wings of the M51 group down to roughly 1/3rd of the
noise level in this image which is a very good achievement!
+But the per-pixel S/N is a relative measurement.
Let's also measure the depth of our detection in absolute surface brightness
units; or magnitudes per square arc-seconds (see @ref{Brightness flux
magnitude}).
-Fortunately Gnuastro's MakeCatalog does this operation easily.
-SDSS image pixel values are calibrated in units of ``nanomaggy'', so the zero
point magnitude is 22.5@footnote{From
@url{
+We'll also ask for the S/N and magnitude of the full edge we have defined.
+Fortunately doing this is very easy with Gnuastro's MakeCatalog:
@example
-astmkcatalog edge.fits -h1 --valuesfile=r_detected.fits \
- --zeropoint=22.5 --ids --surfacebrightness
-asttable edge_cat.fits
+$ astmkcatalog edge.fits -h1 --valuesfile=r_detected.fits \
+ --zeropoint=22.5 --ids --surfacebrightness --sn \
+ --magnitude
+$ asttable edge_cat.fits
+1 25.6971 55.2406 15.8994
@end example
-We have thus reached an outer surface brightness of @mymath{25.69}
magnitudes/arcsec@mymath{^2} (second column in @file{edge_cat.fits}) on this
single exposure SDSS image!
+We have thus reached an outer surface brightness of @mymath{25.70}
magnitudes/arcsec@mymath{^2} (second column in @file{edge_cat.fits}) on this
single exposure SDSS image!
+This is very similar to the surface brightness limit measured in @ref{Image
surface brightness limit} (which is a big achievement!).
+But another point in the result above is very interesting: the total S/N of
the edge is @mymath{55.24} with a total edge magnitude@footnote{You can run
MakeCatalog on @file{only-m51.fits} instead of @file{edge.fits} to see the full
magnitude of the M51 group in this image.} of 15.90!!!
+This very large for such a faint signal (recall that the mean S/N per pixel
was 0.32) and shows a very important point in the study of galaxies:
+While the per-pixel signal in their outer edges may be very faint (and
invisible to the eye in noise), a lot of signal hides deeply burried in the
noise.
+
In interpreting this value, you should just have in mind that NoiseChisel
works based on the contiguity of signal in the pixels.
-Therefore the larger the object (with a similarly diffuse emission), the
deeper NoiseChisel can carve it out of the noise.
+Therefore the larger the object, the deeper NoiseChisel can carve it out of
the noise (for the same outer surface brightness).
In other words, this reported depth, is the depth we have reached for this
object in this dataset, processed with this particular NoiseChisel
configuration.
If the M51 group in this image was larger/smaller than this (the field of view
was smaller/larger), or if the image was from a different instrument, or if we
had used a different configuration, we would go deeper/shallower.
-To continue your analysis of such datasets with extended emission, you can use
@ref{Segment} to identify all the ``clumps'' over the diffuse regions:
background galaxies and foreground stars.
+
+@node Extract clumps and objects, , Achieved surface brightness level,
Detecting large extended targets
+@subsection Extract clumps and objects (Segmentation)
+In @ref{NoiseChisel optimization} we found a good detection map over the
image, so pixels harboring signal have been differentiated from those that
don't.
+For noise-related measurements like the surface brightness limit, this is fine.
+However, after finding the pixels with signal, you are most likely interested
in knowing the sub-structure within them.
+For example how many star forming regions (those bright dots along the spiral
arms) of M51 are within this image?
+What are the colors of each of these star forming regions?
+In the outer most wings of M51, which pixels belong to background galaxies and
foreground stars?
+And many more similar qustions.
+To address these questions, you can use @ref{Segment} to identify all the
``clumps'' and ``objects'' over the detection.
@example
$ astsegment r_detected.fits --output=r_segmented.fits
-$ ds9 -mecube r_segmented.fits -zscale -cmap sls -zoom to fit
+$ ds9 -mecube r_segmented.fits -cmap sls -zoom to fit -scale limits 0 2
@end example
@cindex DS9
@cindex SAO DS9
-Open the output @file{r_segmented.fits} as a multi-extension data cube like
before and flip through the first and second extensions to see the detected
clumps (all pixels with a value larger than 1).
+Open the output @file{r_segmented.fits} as a multi-extension data cube with
the second command above and flip through the first and second extensions,
zoom-in to the spiral arms of M51 and see the detected clumps (all pixels with
a value larger than 1 in the second extension).
To optimize the parameters and make sure you have detected what you wanted, we
recommend to visually inspect the detected clumps on the input image.
For visual inspection, you can make a simple shell script like below.
@@ -4706,14 +5002,11 @@ set -u # Stop execution when a variable is not
initialized.
# Default output is `$1_cat.fits'.
astmkcatalog $1.fits --clumpscat --ids --ra --dec
-# Use Gnuastro's Table program to read the RA and Dec columns of the
-# clumps catalog (in the `CLUMPS' extension). Then pipe the columns
-# to AWK for saving as a DS9 region file.
-asttable $1"_cat.fits" -hCLUMPS -cRA,DEC \
- | awk 'BEGIN @{ print "# Region file format: DS9 version 4.1"; \
- print "global color=green width=1"; \
- print "fk5" @} \
- @{ printf "circle(%s,%s,1\")\n", $1, $2 @}' > $1.reg
+# Use Gnuastro's Table and astscript-ds9-region to build the DS9
+# region file (a circle of radius 1 arcseconds on each point).
+asttable $1"_cat.fits" -hCLUMPS -cRA,DEC \
+ | astscript-ds9-region -c1,2 --mode=wcs --radius=1 \
+ --output=$1.reg
# Show the image (with the requested color scale) and the region file.
ds9 -geometry 1800x3000 -mecube $1.fits -zoom to fit \
@@ -6516,7 +68096860,6 +7152,17 @@ But there are two types of FITS tables: FITS ASCII, and
FITS binary.
Thus, with this option, the program is able to identify which type you want.
The currently recognized values to this option are:
+@item --wcslinearmatrix=STR
+Select the linear transformation matrix of the output's WCS.
+This option only takes two values: @code{pc} (for the @code{PCi_j} formalism)
and @code{cd} (for @code{CDi_j}).
+For more on the different formalisms, please see Section 8.1 of the FITS
standard@footnote{@url{
version 4.0.
+
+@cindex @code{CDELT}
+In short, in the @code{PCi_j} formalism, we only keep the linear rotation
matrix in these keywords and put the scaling factor (or the pixel scale in
astronomical imaging) in the @code{CDELTi} keywords.
+In the @code{CDi_j} formalism, we blend the scaling into the rotation into a
single matrix and keep that matrix in these FITS keywords.
+By default, Gnuastro uses the @code{PCi_j} formalism, because it greatly helps
in human readability of the raw keywords and is also the default mode of WCSLIB.
+However, in some circumstances it may be necessary to have the keywords in the
CD format; for example when you need to feed the outputs into other software
that don't follow the full FITS standard and only recognize the @code{CDi_j}
formalism.
+
@table @command
@item txt
A plain text table with white-space characters between the columns (see
@@ -7411,7 +7714663,75 +7966 errors8930,7 +9165,7 @@ Also, unlike the rest of the options in this section,
with @option{--keyvalue},
@item -l STR[,STR[,...]
@itemx --keyvalue=STR[,STR[,...]
Only print the value of the requested keyword(s): the @code{STR}s.
-@option{--keyvalue} can be called multiple times, and each call can contain
multiple comma-separated values.
+@option{--keyvalue} can be called multiple times, and each call can contain
multiple comma-separated keywords.
If more than one file is given, this option uses the same HDU/extension for
all of them (value to @option{--hdu}).
For example, you can get the number of dimensions of the three FITS files in
the running directory, as well as the length along each dimension, with this
command:
@@ -8941,11 +9176,11 @@ image-b.fits 2 774 672
image-c.fits 2 387 336
@end example
-If a single dataset is given, its name is not printed on the first column,
only the values of the requested keywords.
+If only one input is given, and the @option{--quiet} option is activated, the
file name is not printed on the first column, only the values of the requested
keywords.
@example
$ astfits image-a.fits --keyvalue=NAXIS,NAXIS1 \
- --keyvalue=NAXIS2
+ --keyvalue=NAXIS2 --quiet
2 774 672
@end example
@@ -8981,7 +9216,7 @@ image-a.fits
image-b.fits
@end example
-Note that @option{--colinfoinstdout} is necessary to use column names in the
subsequent @command{asttable} command.
+Note that @option{--colinfoinstdout} is necessary to use column names when
piping to other programs (like @command{asttable} above).
Also, with the @option{-cFILENAME} option, we are asking Table to only print
the final file names (we don't need the sizes any more).
The commands with multiple files above used @file{*.fits}, which is only
useful when all your FITS files are in the same directory.
@@ -9216,16 +9451 writing
@@ -9308,7 +9543,46 @@ In this case (following the GNU C Library), this option
will make the following
This is a very useful option for operations on the FITS date values, for
example sorting FITS files by their dates, or finding the time difference
between two FITS files.
The advantage of working with the Unix epoch time is that you don't have to
worry about calendar details (for example the number of days in different
months, or leap years, etc).
-@item --wcsdistortion STR
+@item --wcscoordsys=STRConvert the coordinate system of the image's world coordinate system (WCS) to
the given coordinate system (@code{STR}) and write it into the file given to
@option{--output} (or an automatically named file if no @option{--output} has
been given).
+
+For example with the command below, @file{img-eq.fits} will have an identical
dataset (pixel values) as @file{image.fits}.
+However, the WCS coordinate system of @file{img-eq.fits} will be the
equatorial coordinate system in the Julian calendar epoch 2000 (which is the
most common epoch used today).
+Fits will automatically extract the current coordinate system of
@file{image.fits} and as long as its one of the recognized coordinate systems
listed below, it will do the conversion.
+
+@example
+$ astfits image.fits --coordsys=eq-j2000 --output=img-eq.fits
+@end example
+
+The currently recognized coordinate systems are listed below (the most common
one today is @code{eq-j2000}):
+
+@table @code
+@item eq-j2000
+2000.0 (Julian-year) equatorial coordinates.
+@item eq-b1950
+1950.0 (Besselian-year) equatorial coordinates.
+@item ec-j2000
+2000.0 (Julian-year) ecliptic coordinates.
+@item ec-b1950
+1950.0 (Besselian-year) ecliptic coordinates.
+@item galactic
+Galactic coordinates.
+@item supergalactic
+Supergalactic coordinates.
+@end table
+
+The Equatorial and Ecliptic coordinate systems are defined by the mean equator
and equinox epoch: either the Besselian year 1950.0, or the Julian year 2000.
+For more on their difference and links for further reading about epochs in
astronomy, please see the description in
@url{ Wikipedia}.
+
+@item --wcsdistortion=STR
@cindex WCS distortion
@cindex Distortion, WCS
@cindex SIP WCS distortion
@@ -9373,6 +9647,7 @@ So before explaining the options and arguments (in
@ref{Invoking astconvertt}),
@menu@end menu
@@ -9508,7 +9783,7 @@ To print to the standard output, set the output name to
`@file{stdout}'.
@end table
-@node Color, Invoking astconvertt, Recognized file formats, ConvertType
+@node Color, Aligning images with small WCS offsets, Recognized file formats,
ConvertType
@subsection Color
@cindex RGB
@@ -9576,7 +9851,67 @@ But thanks to the JPEG compression algorithms, when all
the pixels of one channe
Therefore a Grayscale image and a CMYK image that has only the K-channel
filled are approximately the same file size.
-@node Invoking astconvertt, , Color, ConvertType
+@node Aligning images with small WCS offsets, Invoking astconvertt, Color,
ConvertType
+@subsection Aligning images with small WCS offsets
+
+In order to have nice color images, it is important that the images be
properly aligned.
+This is usually the case in many scenarios, but it some times happens that the
images have a small WCS offset, even though they have the same size.
+In such cases you can use the script below to align the images into
approximately the same pixel grid (to within about 0.5 pixels which is
sufficient in many color-image usage scenarios).
+
+The script below does the job using Gnuastro's @ref{Warp} and @ref{Crop}
programs.
+Simply copy the lines below into a plain-text file with your favorite text
editor and save it as @file{my-align.sh}.
+Don't forget to set the variables of the first three lines to specify the file
names (without the @file{.fits} suffix) and the HDUs of your inputs.
+These four lines are all you need to edit, leave the rest unchanged.
+Also, if you are copy/pasting the script from a PDF, be careful that the
single-quotes used in AWK may need to be corrected.
+
+@example
+#!/bin/sh
+
+# Set the input names (without the '.fits' suffix),
+# and their HDUs.
+r=RED_IMAGE_NO_SUFFIX; rhdu=1
+g=GREEN_IMAGE_NO_SUFFIX; ghdu=1
+b=BLUE_IMAGE_NO_SUFFIX; bhdu=1
+
+# To stop the script if there is a crash
+set -e
+
+# Align all the images to the celestial poles.
+astwarp $r.fits --align -h$rhdu -o $r-aligned.fits
+astwarp $g.fits --align -h$ghdu -o $g-aligned.fits
+astwarp $b.fits --align -h$bhdu -o $b-aligned.fits
+
+# Calculate the final WCS-based center and image-based width based on
+# the G-band (in RGB) image.
+centerwcs=$(astfits $g-aligned.fits --skycoverage --quiet \
+ | awk 'NR==1@{printf "%g %g", $1,$2@}')
+widthpix=$(astfits $g-aligned.fits -h1 --quiet \
+ --keyvalue=NAXIS1,NAXIS2 \
+ | awk '@{printf "%d,%d", $1, $2@}')
+
+# Crop all the images around the desired center and width.
+for f in $r $g $b; do
+ centerpix=$(echo $centerwcs \
+ | asttable -c'arith $1 $2 wcstoimg' \
+ --wcsfile=$f-aligned.fits \
+ | awk '@{printf "%g,%g", $1, $2@}')
+ astcrop $f-aligned.fits --mode=img --width=$widthpix \
+ --center=$centerpix -o$f-use.fits
+ rm $f-aligned.fits
+done
+@end example
+
+Once you have have saved the file and come back to your command-line you can
run the script like this:
+
+@example
+$ chmod +x my-align.sh
+$ ./my-align.sh
+@end example
+
+@noindent
+Of course, feel free to hack it and modify it to fit your datasets, like the
rest of Gnuastro, this script is released under GNU GPLv.3 and above, see
@ref{Your rights}.
+
+@node Invoking astconvertt, , Aligning images with small WCS offsets,
ConvertType
@subsection Invoking ConvertType
ConvertType will convert any recognized input file type to any specified
output type.
@@ -9641,6 +9976,8 @@ Input:
@table @option
@item -h STR/INT
@itemx --hdu=STR/INT
+Input HDU name or counter (counting from 0) for each input FITS file.
+If the same HDU should be used from all the FITS files, you can use the
@option{--globalhdu} option described below.
In ConvertType, it is possible to call the HDU option multiple times for the
different input FITS or TIFF files in the same order that they are called on
the command-line.
Note that in the TIFF standard, one `directory' (similar to a FITS HDU) may
contain multiple color channels (for example when the image is in RGB).
@@ -9649,6 +9986,11 @@ The number of calls to this option cannot be less than
the number of input FITS
Unlike CFITSIO, libtiff (which is used to read TIFF files) only recognizes
numbers (counting from zero, similar to CFITSIO) for `directory' identification.
Hence the concept of names is not defined for the directories and the values
to this option for TIFF files must be numbers.
+
+@item -g STR/INT
+@itemx --globalhdu=STR/INT
+Use the value given to this option (a HDU name or a counter, starting from 0)
for the HDU identifier of all the input FITS files.
+This is useful when all the inputs are distributed in different files, but
have the same HDU in those files.
@end table
@noindent
@@ -10597,12 +10939,42 @@ Here is the list of short names for popular datasets
within Gaia:
@cindex NED (NASA/IPAC Extragalactic Database)
The NASA/IPAC Extragalactic Database (NED, @url{
is a fusion database, integrating the information about extra-galactic sources
from many large sky surveys into a single catalog.
It covers the full spectrum, from Gamma rays to radio frequencies and is
updated when new data arrives.
-A query to @code{ned} is submitted to
@code{
+A TAP query to @code{ned} is submitted to
@code{
-Currently NED only has its main dataset for TAP access (shown below), more
datasets will be added for TAP access in the future.
@itemize
@item
-@code{objdir --> NEDTAP.objdir}
+@code{objdir --> NEDTAP.objdir}: default TAP-based dataset in NED.
+
+@item
+@cindex VOTable
+@code{extinction}: A command-line interface to the
@url{ NED Extinction
Calculator}.
+It only takes a central coordinate and returns a VOTable of the calculated
extinction in many commonly used filters at that point.
+As a result, options like @option{--width} or @option{--radius} are not
supported.
+However, Gnuastro doesn't yet support the VOTable format.
+Therefore, if you specify an @option{--output} file, it should have an
@file{.xml} suffix and the downloaded file will not be checked.
+
+Until VOTable support is added to Gnuastro, you can use GREP, AWK and SED to
convert the VOTable data into a FITS table with a command like below (assuming
the queried VOTable is called @file{ned-extinction.xml}):
+
+@verbatim
+grep '^<TR><TD>' ned-extinction.xml \
+ | sed -e's|<TR><TD>||' \
+ -e's|</TD></TR>||' \
+ -e's|</TD><TD>|@|g' \
+ | awk 'BEGIN{FS="@"; \
+ print "# Column 1: FILTER [name,str15] Filter name"; \
+ print "# Column 2: CENTRAL [um,f32] Central Wavelength"; \
+ print "# Column 3: EXTINCTION [mag,f32] Galactic Ext."; \
+ print "# Column 4: ADS_REF [ref,str50] ADS reference"} \
+ {printf "%-15s %g %g %s\n", $1, $2, $3, $4}' \
+ | asttable -oned-extinction.fits
+@end verbatim
+
+Once the table is in FITS, you can easily get the extinction for a certain
filter (for example the @code{SDSS r} filter) like the command below:
+
+@example
+asttable ned-extinction.fits --equal=FILTER,"SDSS r" \
+ -cEXTINCTION
+@end example
@end itemize
@item vizier
@@ -10740,7 +1111211719,6 +12091,34 @@ These operators take a single operand.
Inverse Hyperbolic sine, cosine, and tangent.
These operators take a single operand.
+@item counts-to-mag
+Convert counts (usually CCD outputs) to magnitudes using the given zeropoint.
+The zero point is the first popped operand and the count value is the second.
+For example assume you have measured the standard deviation of the noise in an
image to be @code{0.1}, and the image's zero point is @code{22.5}.
+You can therefore measure the @emph{per-pixel} surface brightness limit of the
dataset (which is the magnitude of the noise standrard deviation) with this
simple command below.
+Note that because the output is a simple number, we are using @option{--quiet}
to avoid printing extra information.
+
+@example
+astarithmetic 0.1 22.5 counts-to-mag --quiet
+@end example
+
+Of course, you can also convert every pixel in an image (or table column in
Table's @ref{Column arithmetic}) with this operator if you replace the second
popped operand with an image/column.
+
+@item counts-to-jy
+@cindex AB magnitude
+@cindex Magnitude, AB
+Convert counts (usually CCD outputs) to Janskys through an AB-magnitude based
zeropoint.
+The top-popped operand is assumed to be the AB-magnitude zero point and the
second-popped operand is assumed to be a dataset in units of counts (an image
in Arithmetic, and a column in Table's @ref{Column arithmetic}).
+For the full equation and basic definitions, see @ref{Brightness flux
magnitude}.
+
+@cindex SDSS
+For example SDSS images are calibrated in units of nano-maggies, with a fixed
zero point magnitude of 22.5.
+Therefore you can convert the units of SDSS image pixels to Janskys with the
command below:
+
+@example
+$ astarithmetic sdss-image.fits 22.5 counts-to-jy
+@end example
+
@item minvalue
Minimum value in the first popped operand, so ``@command{a.fits minvalue}''
will push the minimum pixel value in this image onto the stack.
When this operator acts on a single image, the output (operand that is put
back on the stack) will no longer be an image, but a number.
@@ -12140,7 +12540,7 @@ In effect, this expands the outer borders of the
foreground.
This operator assumes a binary dataset (all pixels are @code{0} and @code{1}).
The usage is similar to @code{erode}, for example:
@example
-$ astarithmetic binary.fits 2 erode -oout.fits
+$ astarithmetic binary.fits 2 dilate -oout.fits
@end example
@item connected-components
@@ -14119,8 +14519@end menu
@node Statistics, NoiseChisel, Data analysis, Data analysis
@@ -16551,13 +16949,14 @@ For those who feel MakeCatalog's existing
measurements/columns aren't enough and
@menu@end menu
-@node Detection and catalog production, Quantifying measurement limits,
MakeCatalog, MakeCatalog
+@node Detection and catalog production, Brightness flux magnitude,
MakeCatalog, MakeCatalog
@subsection Detection and catalog production
Most existing common tools in low-level astronomical data-analysis (for
example
SExtractor@footnote{@url{
merge the two processes of detection and measurement (catalog production) in
one program.
@@ -16605,124 +17004,162 @@ It might even be so intertwined with its
processing, that adding new columns mig
-@node Quantifying measurement limits, Measuring elliptical parameters,
Detection and catalog production, MakeCatalog
-@subsection Quantifying measurement limits
-@cindex Depth
-@cindex Clump magnitude limit
-@cindex Object magnitude limit
-@cindex Limit, object/clump magnitude
-@cindex Magnitude, object/clump detection limit
-No measurement on a real dataset can be perfect: you can only reach a certain
level/limit of accuracy.
-Therefore, a meaningful (scientific) analysis requires an understanding of
these limits for the dataset and your analysis tools: different datasets have
different noise properties and different detection methods (one
method/algorithm/software that is run with a different set of parameters is
considered as a different detection method) will have different abilities to
detect or measure certain kinds of signal (astronomical objects) and their
properties in the dataset.
-Hence, quantifying the detection and measurement limitations with a particular
dataset and analysis tool is the most crucial/critical aspect of any high-level
analysis.
-Here, we'll review some of the most general limits that are important in any
astronomical data analysis and how MakeCatalog makes it easy to find them.
-Depending on the higher-level analysis, there are more tests that must be
done, but these are relatively low-level and usually necessary in most cases.
-In astronomy, it is common to use the magnitude (a unit-less scale) and
physical units, see @ref{Brightness flux magnitude}.
-Therefore the measurements discussed here are commonly used in units of
magnitudes.
-@table @asis
+@node Brightness flux magnitude, Quantifying measurement limits, Detection and
catalog production, MakeCatalog
+@subsection Brightness, Flux, Magnitude and Surface brightness
-@item Surface brightness limit (of whole dataset)
-@cindex Surface brightness
-As we make more observations on one region of the sky, and add the
observations into one dataset, the signal and noise both increase.
-However, the signal increase much faster than the noise: assuming you add
@mymath{N} datasets with equal exposure times, the signal will increases as a
multiple of @mymath{N}, while noise increases as @mymath{\sqrt{N}}.
-Thus this increases the signal-to-noise ratio.
-Qualitatively, fainter (per pixel) parts of the objects/signal in the image
will become more visible/detectable.
-The noise-level is known as the dataset's surface brightness limit.-You can think of the noise as muddy water that is completely covering a flat
ground@footnote{The ground is the sky value in this analogy, see @ref{Sky
value}.
-Note that this analogy only holds for a flat sky value across the surface of
the image or ground.}.
-The signal (or astronomical objects in this analogy) will be summits/hills
that start from the flat sky level (under the muddy water) and can sometimes
reach outside of the muddy water.
-Let's assume that in your first observation the muddy water has just been
stirred and you can't see anything through it.
-As you wait and make more observations/exposures, the mud settles down and the
@emph{depth} of the transparent water increases, making the summits visible.
-As the depth of clear water increases, the parts of the hills with lower
heights (parts with lower surface brightness) can be seen more clearly.
-In this analogy, height (from the ground) is @emph{surface
brightness}@footnote{Note that this muddy water analogy is not perfect, because
while the water-level remains the same all over a peak, in data analysis, the
Poisson noise increases with the level of data.} and the height of the muddy
water is your surface brightness limit.
+@table @asis
+@cindex Flux
+@cindex Luminosity
+@cindex Brightness
+@item-@cindex Data's depth
-The outputs of NoiseChisel include the Sky standard deviation
(@mymath{\sigma}) on every group of pixels (a mesh) that were calculated from
the undetected pixels in each tile, see @ref{Tessellation} and @ref{NoiseChisel
output}.
-Let's take @mymath{\sigma_m} as the median @mymath{\sigma} over the successful
meshes in the image (prior to interpolation or smoothing).On different instruments, pixels have different physical sizes (for example in
micro-meters, or spatial angle over the sky).
-Nevertheless, a pixel is our unit of data collection.
-In other words, while quantifying the noise, the physical or projected size of
the pixels is irrelevant.
-We thus define the Surface brightness limit or @emph{depth}, in units of
magnitude/pixel, of a data-set, with zeropoint magnitude @mymath{z}, with the
@mymath{n}th multiple of @mymath{\sigma_m} as (see @ref{Brightness flux
magnitude}):
+@item Magnitudedispmath{SB_{\rm Pixel}=-2.5\times\log_{10}{(n\sigma_m)}+z} relation
below.
+The @mymath{-2.5} factor in the definition of magnitudes is a legacy of the
our ancient colleagues and in particular Hipparchus of Nicaea (190-120 BC).
-@cindex XDF survey
-@cindex CANDELS survey
-@cindex eXtreme Deep Field (XDF) survey
-As an example, the XDF survey covers part of the sky that the Hubble space
telescope has observed the most (for 85 orbits) and is consequently very small
(@mymath{\sim4} arcmin@mymath{^2}).
-On the other hand, the CANDELS survey, is one of the widest multi-color
surveys covering several fields (about 720 arcmin@mymath{^2}) but its deepest
fields have only 9 orbits observation.
-The depth of the XDF and CANDELS-deep surveys in the near infrared WFC3/F160W
filter are respectively 34.40 and 32.45 magnitudes/pixel.
-In a single orbit image, this same field has a depth of 31.32.
-Recall that a larger magnitude corresponds to less brightness.
-
-The low-level magnitude/pixel measurement above is only useful when all the
datasets you want to use belong to one instrument (telescope and camera).
-However, you will often find yourself using datasets from various instruments
with different pixel scales (projected pixel sizes).
-If we know the pixel scale, we can obtain a more easily comparable surface
brightness limit in units of: magnitude/arcsec@mymath{^2}.
-Let's assume that the dataset has a zeropoint value of @mymath{z}, and every
pixel is @mymath{p} arcsec@mymath{^2} (so @mymath{A/p} is the number of pixels
that cover an area of @mymath{A} arcsec@mymath{^2}).
-If the surface brightness is desired at the @mymath{n}th multiple of
@mymath{\sigma_m}, the following equation (in units of magnitudes per
@mymath{A} arcsec@mymath{^2}) can be used:
+@dispmath{m-m_r=-2.5\log_{10} \left( B \over B_r \right)}
+
+@noindent
+@mymath{m} is defined as the magnitude of the object and @mymath{m_r} is the
pre-defined magnitude of the reference brightness.
+For estimating the error in measuring a magnitude, see @ref{Quantifying
measurement limits}.
+
+@item Zero point
+@cindex Zero point magnitude
+@cindex Magnitude zero point
+A unique situation in the magnitude equation above occurs when the reference
brightness is unity (@mymath{B_r=1}).
+This brightness will thus summarize all the hardware-specific parameters
discussed above (like the conversion of pixel values to physical units) into
one number.
+That reference magnitude is commonly known as the @emph{Zero point} magnitude
because when @mymath{B=B_r=1}, the right side of the magnitude definition above
will be zero.
+Using the zero point magnitude (@mymath{Z}), we can write the magnitude
relation above in a more simpler format:
+@footnote{Comparing
data from different instruments assumes instrument and observation signatures
are properly corrected, things like the flat-field or the Sky}.
+Jansky is a commonly used unit for measuring spectral flux density and one
Jansky is equivalent to @mymath{10^{-26} W/m^2/Hz} (watts per square meter per
hertz).
-@dispmath{SB_{\rm Projected}=-2.5\times\log_{10}{\left(n\sigma_m\sqrt{A\over
p}\right)+z}}-The @mymath{\sqrt{A/p}} term comes from the fact that noise is added in RMS:
if you add three datasets with noise @mymath{\sigma_1}, @mymath{\sigma_2} and
@mymath{\sigma_3}, the resulting=\sigma}, then
@mymath{\sigma_t=\sqrt{3}\sigma}.
-As mentioned above, there are @mymath{A/p} pixels in the area @mymath{A}.
-Therefore, as @mymath{A/p} increases, the surface brightness limiting
magnitude will become brighter.-It is just important to understand that the surface brightness limit is the
raw noise level, @emph{not} the signal-to-noise.
-To get a feeling for it you can try these commands on any FITS image (let's
assume its called @file{image.fits}), the output of the first command
(@file{zero.fits}) will be the same size as the input, but all pixels will have
a value of zero.
-We then add an ideal noise to this image and warp it to a new pixel size (such
that the area of the new pixels is @code{area_per_pixel} times the input's),
then we print the standard deviation of the raw noise and warped noise.
-Please open the output images an compare them (their sizes, or their pixel
values) to get a good feeling of what is going on.
-Just note that this demo only works when @code{area_per_pixel} is larger than
one. estimate this value for a certain zero point with
AWK, then multiply it to all the pixels in the image with @ref{Arithmetic}.
+For example let's assume you are using an SDSS image with a zero point of 22.5:
@example
-area_per_pixel=25
-scale=$(echo $area_per_pixel | awk '@{print sqrt($1)@}')
-astarithmetic image.fits -h0 nan + isblank not -ozero.fits
-astmknoise zero.fits -onoise.fits
-astwarp --scale=1/$scale,1/$scale noise.fits -onoise-w.fits
-std_raw=$(aststatistics noise.fits --std)
-std_warped=$(aststatistics noise-w.fits --std)
-echo;
-echo "(warped pixel area) = $area_per_pixel x (pixel area)"
-echo "Raw STD: $std_raw"
-echo "Warped STD: $std_warped"As you see in this example, this is thus just an extrapolation of the
per-pixel measurement @mymath{\sigma_m}.
-So it should be used with extreme care: for example the dataset must have an
approximately flat depth or noise properties overall.
-A more accurate measure for each detection is known as the @emph{upper-limit
magnitude} which actually uses random positioning of each detection's
area/footprint, see the respective item below.
-The upper-limit magnitude doesn't extrapolate and even accounts for correlated
noise patterns in relation to that detection.
-Therefore, the upper-limit magnitude is a much better measure of your
dataset's surface brightness limit for each particular object.
+@noindent
+But in Gnuastro, it gets even easier: Arithmetic has an operator called
@code{counts-to-jy}.
+This will directly convert your image pixels (in units of counts) to Janskys
though a provided AB Magnitude-based zero point like below.
+See @ref{Arithmetic operators} for more.
-MakeCatalog will calculate the input dataset's @mymath{SB_{\rm Pixel}} and
@mymath{SB_{\rm Projected}} and write them as comments/meta-data in the output
catalog(s).
-Just note that @mymath{SB_{\rm Projected}} is only calculated if the input has
World Coordinate System (WCS).
+@example
+$ astarithmetic sdss.fits 22.5 counts-to-jy
+@end example
-@item Completeness limit (of each detection)
-@cindex Completeness
-As the surface brightness of the objects decreases, the ability to detect them
will also decrease.
-An important statistic is thus the fraction of objects of similar morphology
and brightness that will be identified with our detection algorithm/parameters
in the given image.
-This fraction is known as completeness.
-For brighter objects, completeness is 1: all bright objects that might exist
over the image will be detected.
-However, as we go to objects of lower overall surface brightness, we will fail
to detect some, and gradually we are not able to detect anything any more.
-For a given profile, the magnitude where the completeness drops below a
certain level (usually above @mymath{90\%}) is known as the completeness limit.
+@item Surface brightnesscindex Purity
-@cindex False detections
-@cindex Detections false
-Another important parameter in measuring completeness is purity: the fraction
of true detections to all true detections.
-In effect purity is the measure of contamination by false detections: the
higher the purity, the lower the contamination.
-Completeness and purity are anti-correlated: if we can allow a large number of
false detections (that we might be able to remove by other means), we can
significantly increase the completeness limit.One traditional way to measure the completeness and purity of a given sample
is by embedding mock profiles in regions of the image with no detection.
-However in such a study we must be really careful to choose model profiles as
similar to the target of interest as possible.
+@dispmath{S = m + 2.5\log_{10}(A)}
++@end table
-@item Magnitude measurement error (of each detection)
-Any measurement has an error and this includes the derived magnitude for an
object.
-Note that this value is only meaningful when the object's magnitude is
brighter than the upper-limit magnitude (see the next items in this list).
+
+
+
+
+
+@node Quantifying measurement limits, Measuring elliptical parameters,
Brightness flux magnitude, MakeCatalog
+@subsection Quantifying measurement limits
+
+@cindex Depth
+@cindex Clump magnitude limit
+@cindex Object magnitude limit
+@cindex Limit, object/clump magnitude
+@cindex Magnitude, object/clump detection limit
+No measurement on a real dataset can be perfect: you can only reach a certain
level/limit of accuracy and a meaningful (scientific) analysis requires an
understanding of these limits.
+Different datasets have different noise properties and different detection
methods (one method/algorithm/software that is run with a different set of
parameters is considered as a different detection method) will have different
abilities to detect or measure certain kinds of signal (astronomical objects)
and their properties in the dataset.
+Hence, quantifying the detection and measurement limitations with a particular
dataset and analysis tool is the most crucial/critical aspect of any high-level
analysis.
+
+Here, we'll review some of the most commonly used methods to quantify the
limits in astronomical data analysis and how MakeCatalog makes it easy to
measure them.
+Depending on the higher-level analysis, there are more tests that must be
done, but these are relatively low-level and usually necessary in most cases.
+In astronomy, it is common to use the magnitude (a unit-less scale) and
physical units, see @ref{Brightness flux magnitude}.
+Therefore the measurements discussed here are commonly used in units of
magnitudes.
++
+@node Magnitude measurement error of each detection, Completeness limit of
each detection, Quantifying measurement limits, Quantifying measurement limits
+@subsubsection Magnitude measurement error of each detection
+@dispmath{M=-2.5\log_{10}(B)+z}
@@ -16745,39 +17182,154 Upper limit magnitude+@cindex Completeness
+As the surface brightness of the objects decreases, the ability to detect them
will also decrease.
+An important statistic is thus the fraction of objects of similar morphology
and brightness that will be detected with our detection algorithm/parameters in
a given image.
+This fraction is known as @emph{completeness}.
+For brighter objects, completeness is 1: all bright objects that might exist
over the image will be detected.
+However, as we go to objects of lower overall surface brightness, we will fail
to detect a fraction of them, and fainter than a certain surface brightness
level (for each morphology),nothing will be detectable in the image: you will
need more data to construct a ``deeper'' image.
+For a given profile and dataset, the magnitude where the completeness drops
below a certain level (usually above @mymath{90\%}) is known as the
completeness limit.
+
+@cindex Purity
+@cindex False detections
+@cindex Detections false
+Another important parameter in measuring completeness is purity: the fraction
of true detections to all true detections.
+In effect purity is the measure of contamination by false detections: the
higher the purity, the lower the contamination.
+Completeness and purity are anti-correlated: if we can allow a large number of
false detections (that we might be able to remove by other means), we can
significantly increase the completeness limit.
+
+One traditional way to measure the completeness and purity of a given sample
is by embedding mock profiles in regions of the image with no detection.
+However in such a study we must be really careful to choose model profiles as
similar to the target of interest as possible.
+
+
+
+@node Upper limit magnitude of each detection, Surface brightness limit of
image, Comple-For example, while the depth of the image is 32 magnitudes/pixel, a
measurement that gives a magnitude of 36 for a @mymath{\sim100} pixel object is
clearly unreliable.
-In another similar depth image, we might measure a magnitude of 30 for it, and
yet another might give 33.
-Furthermore, due to the noise scatter so close to the depth of the data-set,
the total brightness might actually get measured as a negative value, so no
magnitude can be defined (recall that a magnitude is a base-10 logarithm).
-This problem usually becomes relevant when the detection labels were not
derived from the values being measured (for example when you are estimating
colors, see @ref{MakeCatalog}).
+For example, assume that you have done your detection and segmentation on one
filter and now you do measurements over the same labeled regions, but on other
filters to measure colors (as we did in the tutorial @ref{Segmentation and
making a catalog}).
+Some objects are not going to have any significant signal in the other
filters, but for example, you measure magnitude of 36 for one of them!
+This is clearly unreliable (no dataset in current astronomy is able to detect
such a faint signal).
+In another image with the same depth, using the same filter, you might measure
a magnitude of 30 for it, and yet another might give you 33.
+Furthermore, the total brightness might actually be negative in some images of
the same depth (due to noise).
+In these cases, no magnitude can be defined and MakeCatalog will place a NaN
there (recall that a magnitude is a base-10 logarithm).
@cindex Upper limit magnitude
@cindex Magnitude, upper limit
Using such unreliable measurements will directly affect our analysis, so we
must not use the raw measurements.
-But how can we know how reliable a measurement on a given dataset is?
+When approaching the limits of your detection method, it is therefore
important to be able to identify such cases.
+But how can we know how reliable a measurement of one object on a given
dataset is?
-When we confront such unreasonably faint magnitudes, there is one thing we can
deduce: that if something actually exists here (possibly buried deep under the
noise), it's inherent magnitude is fainter than an @emph{upper limit magnitude}.
-To find this upper limit magnitude, we place the object's footprint
(segmentation map) over random parts of the image where there are no
detections, so we only have pure (possibly correlated) noise, along with
undetected objects.
+When we confront such unreasonably faint magnitudes, there is one thing we can
deduce: that if something actually exists under our labeled pixels (possibly
buried deep under the noise), it's inherent magnitude is fainter than an
@emph{upper limit magnitude}.
+To find this upper limit magnitude, we place the object's footprint
(segmentation map) over a random part of the image where there are no
detections, and measure the total brightness within the footprint.
Doing this a large number of times will give us a distribution of brightness
values.
-The standard deviation (@mymath{\sigma}) of that distribution can be used to
quantify the upper limit magnitude.
+The standard deviation (@mymath{\sigma}) of that distribution can be used to
quantify the upper limit magnitude for that particular object (given its
particular shape and area):
+
+@dispmath{M_{up,n\sigma}=-2.5\times\log_{10}{(n\sigma_m)}+z \quad\quad
[mag/target]}
@cindex Correlated noise
-Traditionally, faint/small object photometry was done using fixed circular
apertures (for example with a diameter of @mymath{N} arc-seconds).
-Hence, the upper limit was like the depth discussed above: one value for the
whole image.
+Traditionally, faint/small object photometry was done using fixed circular
apertures (for example with a diameter of @mymath{N} arc-seconds) and there
wasn't much processing involved (to make a deep stack).
+Hence, the upper limit was synonymous with the surface brightness limit
discussed above: one value for the whole image.
The problem with this simplified approach is that the number of pixels in the
aperture directly affects the final distribution and thus magnitude.
-Also the image correlated noise might actually create certain patters, so the
shape of the object can also affect the final result result.
-Fortunately, with the much more advanced hardware and software of today, we
can make customized segmentation maps for each object.
+Also the image correlated noise might actually create certain patterns, so the
shape of the object can also affect the final result.
+Fortunately, with the much more advanced hardware and software of today, we
can make customized segmentation maps (footprint) for each object and have
enough computing power to actually place that footprint over many random places.
+As a result, the per-target upper-limit magnitude and general surface
brightness limit have diverged.
-When requested, MakeCatalog will randomly place each target's footprint over
the dataset as described above and estimate the resulting distribution's
properties (like the upper limit magnitude).
+When any of the upper-limit-related columns requested, MakeCatalog will
randomly place each target's footprint over the undetected parts of the dataset
as described above, and estimate the required properties.
The procedure is fully configurable with the options in @ref{Upper-limit
settings}.
-If one value for the whole image is required, you can either use the surface
brightness limit above or make a circular aperture and feed it into MakeCatalog
to request an upper-limit magnitude for it@footnote{If you intend to make
apertures manually and not use a detection map (for example from
@ref{Segment}), don't forget to use the @option{--upmaskfile} to give
NoiseChisel's output (or any a binary map, marking detected pixels, see
@ref{NoiseChisel output}) as a mask.
-Otherwise, the footprints may randomly fall over detections, giving highly
skewed distributions, with wrong upper-limit distributions.
-See The description of @option{--upmaskfile} in @ref{Upper-limit settings} for
more.}.
+You can get the full list of upper-limit related columns of MakeCatalog with
this command (the extra @code{--} before @code{--upperlimit} is
necessary@footnote{Without the extra @code{--}, grep will assume that
@option{--upperlimit} is one of its own options, and will thus abort,
complaining that it has no option with this name.}):
+
+@example
+$ astmkcatalog --help | grep -- --upperlimit
+@end example
+
+@node Surface brightness limit of image, Upper limit magnitude of image, Upper
limit magnitude of each detection, Quantifying measurement limits
+@subsubsection Surface brightness limit of image
+@cindex Surface brightness
+As we make more observations on one region of the sky and add/combine the
observations into one dataset, both the signal and the noise increase.
+However, the signal increases much faster than the noise:
+Assuming you add @mymath{N} datasets with equal exposure times, the signal
will increases as a multiple of @mymath{N}, while noise increases as
@mymath{\sqrt{N}}.
+Therefore the signal-to-noise ratio increases by a factor of @mymath{\sqrt{N}}.
+Visually, fainter (per pixel) parts of the objects/signal in the image will
become more visible/detectable.
+The noise-level is known as the dataset's surface brightness limit.
+ water+@cindex Data's depth
++Let's take @mymath{\sigma_m} as the median @mymath{\sigma} over the successful
meshes in the image (prior to interpolation or smoothing).
+It is recorded in the @code{MEDSTD} keyword of the @code{SKY_STD} extension of
NoiseChisel's output.
+
+@cindex ACS camera
+@cindex Surface brightness limit
+@cindex Limit, surface brightness
+On different instruments, pixels cover different spatial angles over the sky.
+For example, the width of each pixel on the ACS camera on the Hubble Space
Telescope (HST) is roughly 0.05 seconds of arc, while the pixels of SDSS are
each 0.396 seconds of arc (almost eight times wider@footnote{Ground-based
instruments like the SDSS suffer from strong smoothing due to the atmosphere.
+Therefore, increasing the pixel resolution (or decreasing the width of a
pixel) won't increase the received information).}).
+Nevertheless, irrespective of its sky coverage, a pixel is our unit of data
collection.
+
+To start with, we define the low-level Surface brightness limit or
@emph{depth}, in units of magnitude/pixel with the equation below (assuming the
image has zero point magnitude @mymath{z} and we want the @mymath{n}th multiple
of @mymath{\sigma_m}).
+
+@dispmath{SB_{n\sigma,\rm pixel}=-2.5\times\log_{10}{(n\sigma_m)}+z \quad\quad
[mag/pixel]}
+
+@cindex XDF survey
+@cindex CANDELS survey
+@cindex eXtreme Deep Field (XDF) survey
+As an example, the XDF survey covers part of the sky that the HST has observed
the most (for 85 orbits) and is consequently very small (@mymath{\sim4} minutes
of arc, squared).
+On the other hand, the CANDELS survey, is one of the widest multi-color
surveys done by the HST covering several fields (about 720 arcmin@mymath{^2})
but its deepest fields have only 9 orbits observation.
+The @mymath{1\sigma} depth of the XDF and CANDELS-deep surveys in the near
infrared WFC3/F160W filter are respectively 34.40 and 32.45 magnitudes/pixel.
+In a single orbit image, this same field has a @mymath{1\sigma} depth of 31.32
magnitudes/pixel.
+Recall that a larger magnitude corresponds to less brightness, see
@ref{Brightness flux magnitude}.
+
+@cindex Pixel scale
+The low-level magnitude/pixel measurement above is only useful when all the
datasets you want to use, or compare, have the same pixel size.
+However, you will often find yourself using, or comparing, datasets from
various instruments with different pixel scales (projected pixel width, in
arc-seconds).
+If we know the pixel scale, we can obtain a more easily comparable surface
brightness limit in units of: magnitude/arcsec@mymath{^2}.
+But another complication is that astronomical objects are usually larger than
1 arcsec@mymath{^2}, so its common to measure the surface brightness depth over
a larger (but fixed, depending on context) area.
+
+Let's assume that every pixel is @mymath{p} arcsec@mymath{^2} and we want the
surface brightness limit for an object covering A arcsec@mymath{^2} (so
@mymath{A/p} is the number of pixels that cover an area of @mymath{A}
arcsec@mymath{^2}).
+On the other hand, noise is added in RMS@footnote{If you add three datasets
with noise @mymath{\sigma_1}, @mymath{\sigma_2} and @mymath{\sigma_3}, the
resulting\equiv\sigma}, then
@mymath{\sigma_t=\sigma\sqrt{3}}.
+In this case, the area @mymath{A} is covered by @mymath{A/p} pixels, so the
noise level is @mymath{\sigma_t=\sigma\sqrt{A/p}}.}, hence the noise level in
@mymath{A} arcsec@mymath{^2} is @mymath{n\sigma_m\sqrt{A/p}}.
+But we want the result in units of arcsec@mymath{^2}, so we should divide this
by @mymath{A} arcsec@mymath{^2}:
+@mymath{n\sigma_m\sqrt{A/p}/A=n\sigma_m\sqrt{A/(pA^2)}=n\sigma_m/\sqrt{pA}}.
+Plugging this into the magnitude equation, we get the @mymath{n\sigma} surface
brightness limit, over an area of A arcsec@mymath{^2}, in units of
magnitudes/arcsec@mymath{^2}:
+
+@dispmath{SB_{{n\sigma,\rm A
arcsec}^2}=-2.5\times\log_{10}{\left(n\sigma_m\over \sqrt{pA}\right)+z}
\quad\quad [mag/arcsec^2]}
+
+@cindex World Coordinate System (WCS)
+MakeCatalog will calculate the input dataset's @mymath{SB_{n\sigma,\rm pixel}}
and @mymath{SB_{{n\sigma,\rm A arcsec}^2}} and will write them as the
@code{SBLMAGPIX} and @code{SBLMAG} keywords the output catalog(s), see
@ref{MakeCatalog output}.
+You can set your desired @mymath{n}-th multiple of @mymath{\sigma} and the
@mymath{A} arcsec@mymath{^2} area using the following two options respectively:
@option{--sfmagnsigma} and @option{--sfmagarea} (see @ref{MakeCatalog output}).
+Just note that @mymath{SB_{{n\sigma,\rm A arcsec}^2}} is only calculated if
the input has World Coordinate System (WCS).
+Without WCS, the pixel scale cannot be derived.
+
+@cindex Correlated noise
+@cindex Noise, correlated
+As you saw in its derivation, the calculation above extrapolates the noise in
one pixel over all the input's pixels!
+It therefore implicitly assumes that the noise is the same in all of the
pixels.
+But this only happens in individual exposures: reduced data will have
correlated noise because they are a stack of many individual exposures that
have been warped (thus mixing the pixel values).
+A more accurate measure which will provide a realistic value for every labeled
region is known as the @emph{upper-limit magnitude}, which is discussed below.
+
+
+@node Upper limit magnitude of image, , Surface brightness limit of image,
Quantifying measurement limits
+@subsubsection Upper limit magnitude of image
+As mentioned above, the upper-limit magnitude will depend on the shape of each
object's footprint.
+Therefore we can measure the dataset's upper-limit magnitude using standard
shapes.
+Traditionally a circular aperture of a fixed size (in arcseconds) has been
used.
+For a full example of implementing this, see the respective section in the
tutorial (@ref{Image surface brightness limit}).
+
+
+
+
+
-@end table
@@ -17143,6 +17695,8 @@ The dataset given to @option{--stdfile} (and
@option{--stdhdu} has the Sky varia
Read the input STD image even if it is not required by any of the requested
columns.
This is because some of the output catalog's metadata may need it, for example
to calculate the dataset's surface brightness limit (see @ref{Quantifying
measurement limits}, configured with @option{--sfmagarea} and
@option{--sfmagnsigma} in @ref{MakeCatalog output}).
+Furthermore, if the input STD image doesn't have the @code{MEDSTD} keyword
(that is meant to contain the representative standard deviation of the full
image), with this option, the median will be calculated and used for the
surface brightness limit.
+
@item -z FLT
@itemx --zeropoint=FLT
The zero point magnitude for the input image, see @ref{Brightness flux
magnitude}.
@@ -17152,7 +17706 an
@@ -17510,6 +18065,7 @@ For now these factors have to be found by other means.
@item --upperlimit
The upper limit value (in units of the input image) for this object or clump.
+This is the sigma-clipped standard deviation of the random distribution,
multiplied by the value of @option{--upnsigma}).@@ -17518,6 +18074,10 @@ The upper limit magnitude for this object or clump.+@item --upperlimitsb
+The upper-limit surface brightness (in units of mag/arcsec@mymath{^2}) of this
labeled region (object or clump).
+This is just a simple wrapper over lower-level columns: setting B and A as the
value in the columns @option{--upperlimit} and @option{--areaarcsec2}, we fill
this column by simply use the surface brightness equation of @ref{Brightness
flux magnitude}.
+
@item --upperlimitonesigma
The @mymath{1\sigma} upper limit value (in units of the input image) for this
object or clump.
See @ref{Quantifying measurement limits} and @ref{Upper-limit settings} for a
complete explanation.
@@ -17791,13 +18351,48 @@ If an output filename is given (see @option{--output}
in @ref{Input output optio
When it isn't given, the input name will be appended with a @file{_cat} suffix
(see @ref{Automatic output}) and its format will be determined from the
@option{--tableformat} option, which is also discussed in @ref{Input output
options}.
@option{--tableformat} is also necessary when the requested output name is a
FITS table (recall that FITS can accept ASCII and binary tables, see
@ref{Table}).
-By default (when @option{--spectrum} isn't called) only a single catalog/table
will be created for ``objects'', however, if @option{--clumpscat} is called, a
secondary catalog/table will also be created.
-For more on ``objects'' and ``clumps'', see @ref{Segment}.
-In short, if you only have one set of labeled images, you don't have to worry
about clumps (they are deactivated by default).
+By default (when @option{--spectrum} or @option{--clumpscat} aren't called)
only a single catalog/table will be created for the labeled ``objects''.
+
+@itemize
+@item
+if @option{--clumpscat} is called, a secondary catalog/table will also be
created for ``clumps'' (one of the outputs of the Segment program, for more on
``objects'' and ``clumps'', see @ref{Segment}).
+In short, if you only have one labeled image, you don't have to worry about
clumps and just ignore this.
+@item
+When @option{--spectrum} is called, it is not mandatory to specify any
single-valued measurement columns. In this case, the output will only be the
spectra of each labeled region within a 3D datacube.
+For more, see the description of @option{--spectrum} in @ref{MakeCatalog
measurements}.
+@end itemize
+
+@cindex Surface brightness limit
+@cindex Limit, Surface brightness
+When possible, MakeCatalog will also measure the full input's noise level
(also known as surface brightness limit, see @ref{Quantifying measurement
limits}).
+Since these measurements are related to the noise and not any particular
labeled object, they are stored as keywords in the output table.
+Furthermore, they are only possible when a standard deviation image has been
loaded (done automatically for any column measurement that involves noise, for
example @option{--sn} or @option{--std}).
+But if you just want the surface brightness limit and no noise-related column,
you can use @option{--forcereadstd}.
+All these keywords start with @code{SBL} (for ``surface brightness limit'')
and are described below:
+
+@table @code
+@item SBLSTD
+Per-pixel standard deviation.
+If a @code{MEDSTD} keyword exists in the standard deviation dataset, then that
value is directly used.
+
+@item SBLNSIG
+Sigma multiple for surface brightness limit (value you gave to
@option{--sfmagnsigma}), used for @code{SBLMAGPX} and @code{SBLMAG}.
+
+@item SBLMAGPX
+Per-pixel surface brightness limit (in units of magnitudes/pixel).
+
+@item SBLAREA
+Area (in units of arcsec@mymath{^2}) used in @code{SBLMAG} (value you gave to
@option{--sfmagarea}).
-When @option{--spectrum} is called, it is not mandatory to specify any
single-valued measurement columns. In this case, the output will only be the
spectra of each labeled region. See the description of @option{--spectrum} in
@ref{MakeCatalog measurements}.
+@item SBLMAG
+Surface brightness limit of data calculated over @code{SBLAREA} (in units of
mag/arcsec@mymath{^2}).
+@end table
+
+When any of the upper-limit measurements are requested, the input parameters
for the upper-limit measurement are stored in the keywords starting with
@code{UP}: @code{UPNSIGMA}, @code{UPNUMBER}, @code{UPRNGNAM}, @code{UPRNGSEE},
@code{UPSCMLTP}, @code{UPSCTOL}.
+These are primarily input arguments, so they correspond to the options with a
similar name.
-The full list of MakeCatalog's output options are elaborated below.
+The full list of MakeCatalog's options relating to the output file format and
keywords are listed below.
+See @ref{MakeCatalog measurements} for specifying which columns you want in
the final catalog.
@table @option
@item -C
@@ -17845,7 +18440,23 @@ For random measurements on any area, please use the
upper-limit columns of MakeC
-@node Match, Sort FITS files by night, MakeCatalog, Data analysis
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+@node Match, , MakeCatalog, Data analysis
@section Match
Data can come come from different telescopes, filters, software and even
different configurations for a single software.
@@ -18105,2434 +18716,2602 December@noindent
-One line examples:
-@example
-## Use the DATE-OBS keyword
-$ astscript-sort-by-night --key=DATE-OBS /path/to/data/*.fits
+@node Modeling basics, If convolving afterwards, MakeProfiles, MakeProfiles
+@subsection Modeling basics
-## Make links to the input files with the `img-' prefix
-$ astscript-sort-by-night --link --prefix=img- /path/to/data/*.fits
-@end example
+In the subsections below, first a review of some very basic information and
concepts behind modeling a real astronomical image is given.
+You can skip this subsection if you are already sufficiently familiar with
these concepts.ated canvas.
+* Oversampling:: Oversampling the model.
+@end menunode Defining an ellipse and ellipsoid, PSF, Modeling basics, Modeling basics
+@subsubsection Defining an ellipse and ellipsoid@item -k STR
-@itemx --key=STR
-The keyword name that contains the FITS date format to classify/sort by.@example
-PnN-I.fits
-@end exampletable @code relation-@node SAO DS9 region files from table, , Sort FITS files by night, Data
analysis
-@section SAO DS9 region files from table-@menu
-* Invoking astscript-make-ds9-reg:: How to call astscript-make-ds9-reg
-@end menu+@node Stars, Galaxies, PSF, Modeling basics
+@subsubsection Starsnode Galaxies, Sampling from a function, Stars, Modeling basics
+@subsubsection Galaxies
-@table @optionnode Sampling from a function, Oversampling, Galaxies, Modeling basics
+@subsubsection Sampling from a function significantexample
-ds9 image.fits -zscale -regions ds9.reg
-@end example Profile-@node Modeling and fittings, High-level calculations, Data analysis, Top
-@chapter Modeling and fitting to understand the detections.
-@menu
-* MakeProfiles:: Making mock galaxies and stars.
-* MakeNoise:: Make (add) noise to an image.
-@end menu
+@node Profile magnitude, Invoking astmkprof, If convolving afterwards,
MakeProfiles
+@subsection Profile magnitude
-@node MakeProfiles, MakeNoise, Modeling and fittings, Modeling and fittings
-@section MakeProfiles constantenumerate
-Build the full profile out to its truncation radius in a possibly over-sampled
array.
-@item
-Multiply all the elements by a fixed constant so its total magnitude equals
the desired total magnitude.
-@item
-If @option{--individual} is called, save the array for each profile to a FITS
file.
-@item
-If @option{--nomerged} is not called, add the overlapping pixels of all the
created profiles to the output image and abort.
-@end enumeratenode Invoking astmkprof, , Profile magnitude, MakeProfiles
+@subsection Invoking MakeProfilesMakeProfiles will make any number of profiles specified in a catalog either
individually or in one image.
+The executable name is @file{astmkprof} with the following general template-@node Modeling basics, If convolving afterwards, MakeProfiles, MakeProfiles
-@subsection Modeling basics
+## Make the profiles in catalog.txt over image.fits:
+$ astmkprof --background=image.fits catalog.txt
-In the subsections below, first a review of some very basic information and
concepts behind modeling a real astronomical image is given.
-You can skip this subsection if you are already sufficiently familiar with
these concepts.## Make profiles in catalog, using RA and Dec in the given column:
+$ astmkprof --ccol=RA_CENTER --ccol=DEC_CENTER --mode=wcs catalog.txt
-@node Defining an ellipse and ellipsoid, PSF, Modeling basics, Modeling basics
-@subsubsection Defining an ellipse and ellipsoid which-Following the discussion in @ref{Merging multiple warpings}, we can define the
full rotation with the+@example
+$ astmkprof --config=/usr/local/etc/astmkprof-3d.conf catalog.txt
+@end example extending@node PSF, Stars, Defining an ellipse and ellipsoid, Modeling basics
-@subsubsection Point spread function
+The list of options directly related to the input catalog columns is shown
below.table @optiontable @asis@itemize
+@item
+S@'ersic profile with `@code{sersic}' or `@code{1}'.
-@dispmath{f(r)=a \exp \left( -(x-\mu)^2 \over 2\sigma^2 \right)+d}
+@item
+Moffat profile with `@code{moffat}' or `@code{2}'.@item
+Gaussian profile with `@code{gaussian}' or `@code{3}'.
+Point source with `@code{point}' or `@code{4}'.@item
+Flat profile with `@code{flat}' or `@code{5}'.
-@dispmath{f(r)=a \left[ 1+\left( r\over \alpha \right)^2 \right]^{-\beta}}-
-@cindex Moffat FWHM
-@dispmath{\rm{FWHM}_m=2\alpha\sqrt{2^{1/\beta}-1}}end table-@end tablenode Stars, Galaxies, PSF, Modeling basics
-@subsubsection Stars
+@item --mcol=STR/INT
+The total pixelated magnitude of the profile within the truncation radius, see
@ref{Profile magnitude+@end table
+@node MakeProfiles profile settings, MakeProfiles output dataset, MakeProfiles
catalog, Invoking astmkprof
+@subsubsection MakeProfiles profile settings-@node Galaxies, Sampling from a function, Stars, Modeling basics
-@subsubsection Galaxiesitem -r
+@itemx --numrandom
+The number of random points used in the central regions of the profile, see
@ref{Sampling from a function}. indexitem -t FLT
+@itemx --tolerance=FLT
+The tolerance to switch from Monte Carlo integration to the central pixel
value, see @ref{Sampling from a function}.node Sampling from a function, Oversampling, Galaxies, Modeling basics
-@subsubsection Sampling from a functionnode Oversampling, , Sampling from a function, Modeling basics
-@subsubsection Oversampling (including
NaN/blank).
+@end tableFor example let's assume you have the radial profile below in a file called
@file{radial.txt}.
+The first column is the larger interval radius (in units of pixels) and the
second column is the value in that interval:@example
+1 100
+2 90
+3 50
+4 10
+5 2
+6 0.1
+7 0.05
+@end example@noindent
+You can construct the table to give to @option{--customtable} with the command
below (using Gnuastro's @ref{Column arithmetic}).
+@example
+asttable radial.fits -c'arith $1 1 -' -c1,2 -ocustom.fits
+@end example
+@noindent-@node If convolving afterwards, Brightness flux magnitude, Modeling basics,
MakeProfiles
-@subsection If convolving afterwards
+@item --customtablehdu INT/STR
+The HDU/extension in the FITS file given to @option{--customtable}. explanationsnode Brightness flux magnitude, Profile magnitude, If convolving afterwards,
MakeProfiles
-@subsection Brightness, Flux, Magnitude and Surface brightness
+@end tabletable @option-@cindex Magnitudes -B STR/INT
+@itemx --backhdu=STR/INT
+The header data unit (HDU) of the file given to @option{--background}.
-@dispmath{m-m_r=-2.5\log_{10} \left( B \over B_r \right)}dispmath{m = -2.5\log_{10}(B) + Z} parameters it is possible to create a kernel with MakeProfiles
without the need to create a catalog.
+Here are some examples: --kernel=gaussian,2,3
+A circular Gaussian kernel with FWHM of 2 pixels and truncated at 3 times
+the FWHM.
+@end tabledispmath{S = m + 2.5\log_{10}(A)}node Profile magnitude, Invoking astmkprof, Brightness flux magnitude,
MakeProfiles
-@subsection Profile magnitude large enough, this can be
significantly different from the total integrated light to infinity.
+If a background image is specified, this option is ignored+@end table
-@node Invoking astmkprof, , Profile magnitude, MakeProfiles
-@subsection Invoking MakeProfilesMakeProfiles will make any number of profiles specified in a catalog either
individually or in one image.
-The executable name is @file{astmkprof} with the following general templateexample
-$ astmkprof [OPTION ...] [Catalog]
-@end example
+If the values given to any of these options does not correspond to the number
of dimensions in the output dataset, then no WCS information will be added.
-@noindent
-One line examples:
+@table @option
-@example
-## Make an image with profiles in catalog.txt (with default size):
-$ astmkprof catalog.txt
+@item --crpix=FLT,FLT
+The pixel coordinates of the WCS reference point.
+Fractions are acceptable for the values of this option.
-## Make the profiles in catalog.txt over image.fits:
-$ astmkprof --background=image.fits catalog.txt
--
-## Make profiles in catalog, using RA and Dec in the given column:
-$ astmkprof --ccol=RA_CENTER --ccol=DEC_CENTER --mode=wcs catalog.txt
--- how--
-@example
-$ astmkprof --config=/usr/local/etc/astmkprof-3d.conf catalog.txt
-@end example
--
-@example
-alias astmkprof-3d="astmkprof --config=/usr/local/etc/astmkprof-3d.conf"
-@end example
----item --crval=FLT,FLT
+The WCS coordinates of the Reference point.
+Fractions are acceptable for the values of this option.@item --pc=FLT,FLT,FLT,FLT
+The PC matrix of the WCS rotation, see the FITS standard (link above) to
better understand the PC matrix.
-The list of options directly related to the input catalog columns is shown
below.table @optionend tablenode MakeProfiles log file, , MakeProfiles output dataset, Invoking astmkprof
+@subsubsection MakeProfiles log file plain text table/catalog, see @ref{Gnuastro text
table format}.@itemize
@item
-S@'ersic profile with `@code{sersic}' or `@code{1}'.
+An ID (row number of profile in input catalog).
@item
-Moffat profile with `@code{moffat}' or `@code{2}'.
+The total magnitude of the profile in the output dataset.
+When the profile does not completely overlap with the output dataset, this
will be different from your input magnitude.
@item
-Gaussian profile with `@code{gaussian}' or `@code{3}'.
+The number of pixels (in the oversampled image) which used Monte Carlo
integration and not the central pixel value, see @ref{Sampling from a function}.
@item
-Point source with `@code{point}' or `@code{4}'.
+The fraction of flux in the Monte Carlo integrated pixels.
@item
-Flat profile with `@code{flat}' or `@code{5}'.
+If an individual image was created, this column will have a value of @code{1},
otherwise it will have a value of @code{0}.
+@end itemize-@item --ncol=STR/INT
-The S@'ersic index (@mymath{n}) or Moffat @mymath{\beta}.-@item --mcol=STR/INT
-The total pixelated magnitude of the profile within the truncation radius, see
@ref{Profile magnitude}.
+@node MakeNoise, , MakeProfiles, Modeling and fittings
+@section MakeNoise-@end table
+@menu
+* Noise basics:: Noise concepts and definitions.
+* Invoking astmknoise:: Options and arguments to MakeNoise.
+@end menu
-@node MakeProfiles profile settings, MakeProfiles output dataset, MakeProfiles
catalog, Invoking astmkprof
-@subsubsection MakeProfiles profile settings
-The profile parameters that differ between each created profile are specified
through the columns in the input-@table @option
+@node Noise basics, Invoking astmknoise, MakeNoise, MakeNoise
+@subsection Noise basicsitem -r
-@itemx --numrandom
-The number of random points used in the central regions of the profile, see
@ref{Sampling from a function}.item -e
-@itemx --envseed
-@cindex Seed, Random number generator
-+@node Photon counting noise, Instrumental noise, Noise basics, Noise basics
+@subsubsection Photon counting noise
-@item -t FLT
-@itemx --tolerance=FLT
-The tolerance to switch from Monte Carlo integration to the central pixel
value, see @ref{Sampling from a function}.@item --magatpeak
-The magnitude column in the catalog (see @ref{MakeProfiles catalog}) will be
used+@dispmath{\mu=B+I_{nn}, \quad \sigma=\sqrt{B+I_{nn}}}+@node Instrumental noise, Final noised pixel value, Photon counting noise,
Noise basics
+@subsubsection Instrumental noise@dispmath{\mu=I_{nn}, \quad \sigma=\sqrt{C^2+I_{nn}}}
-The table should have 3 columns as shown below.
-For example let's assume you have the radial profile below in a file called
@file{radial.txt}.
-The first column is the larger interval radius and the second column is the
value in that interval:
+@dispmath{\mu=B+I_{nn}, \quad \sigma=\sqrt{C^2+B+I_{nn}}}
+
+
+
+@node Generating random numbers, , Final noised pixel value, Noise basics
+@subsubsection Generating random numbers
+++environment+
+There are two ways you can specify values for these environment variables.
+You can call them on the same command-line for example:
@example
-1 100
-2 90
-3 50
-4 10
-5 2
-6 0.1
-7 0.05
+$ GSL_RNG_TYPE="taus" GSL_RNG_SEED=345 astmknoise input.fits+$ export GSL_RNG_TYPE="taus"
+$ export GSL_RNG_SEED=345
@end example
+@cindex Startup scripts
+@cindex @file{.bashrc} --customtablehdu INT/STR
-The HDU/extension in the FITS file given to @option{--customtable}.+@node Invoking astmknoise, , Noise basics, MakeNoise
+@subsection Invoking MakeNoise+MakeNoise will add noise to an existing image.
+The executable name is @file{astmknoise} with the following general template
-@item -R
-@itemx --replace
-Do not add the pixels of each profile over the background, or other profiles.
-But replace the values.
+@example
+$ astmknoise [OPTION ...] InputImage.fits
+@end examplenoindent
+One line examples:
-@end table+@table @option countingitem -B STR/INT
-@itemx --backhdu=STR/INT
-The header data unit (HDU) of the file given to @option{--background}.
+@item -B
+@itemx --bgisbrightness
+The value given to @option{--background} should be interpretted as brightness,
not as a magnitude@item -i FLT
+@itemx --instrumental=FLT
+The instrumental noise which is in units of flux, see @ref{Instrumental noise}.item -e
+@itemx --envseed
+@cindex Seed, Random number generator
+@cindex Random number generator, Seed@item --kernel=gaussian,2,3
-A circular Gaussian kernel with FWHM of 2 pixels and truncated at 3 times
-the FWHM.
-@end tableend table-If a background image is specified, this option is ignored.-@end table@node High-level calculations, Installed scripts, Modeling and fittings, Top
+@chapter High-level calculations
-If the values given to any of these options does not correspond to the number
of dimensions in the output dataset, then no WCS information will be addedtable @option
-@item --crpix=FLT,FLT
-The pixel coordinates of the WCS reference point.
-Fractions are acceptable for the values of this option.
-@item --crval=FLT,FLT
-The WCS coordinates of the Reference point.
-Fractions are acceptable for the values of this option.menu
+* CosmicCalculator:: Calculate cosmological variables
+@end menu@node CosmicCalculator, , High-level calculations, High-level calculations
+@section CosmicCalculatorend tablenode MakeProfiles log file, , MakeProfiles output dataset, Invoking astmkprof
-@subsubsection MakeProfiles log filenode Distance on a 2D curved space, Extending distance concepts to 3D,
CosmicCalculator, CosmicCalculator
+@subsection Distance on a 2D curved space
-@itemize
-@item
-An ID (row number of profile in input catalog).
-The total magnitude of the profile in the output dataset.
-When the profile does not completely overlap with the output dataset, this
will be different from your input magnitudeitem
-The number of pixels (in the oversampled image) which used Monte Carlo
integration and not the central pixel value, see @ref{Sampling from a function}.
-The fraction of flux in the Monte Carlo integrated pixels.@item
-If an individual image was created, this column will have a value of @code{1},
otherwise it will have a value of @code{0}.
-@end itemize
+@float Figure,flatplane
+@center@image{gnuastro-figures/flatplane, 10cm, , }
+@caption{Two dimensional Cartesian and polar coordinates on a flat
+plane.}
+@end floatdispmath{ds_s=dx^2+dy^2=dr^2+r^2d\phi^2} it can follow our reasoning.
+With the third axis added, a generic infinitesimal change over @emph{the full}
3D space corresponds to the distance:
+@dispmath{ds_s^2=dx^2+dy^2+dz^2=dr^2+r^2d\phi^2+dz^2.}
+@float Figure,sphereandplane
+@center@image{gnuastro-figures/sphereandplane, 10cm, , }
+@caption{2D spherical shell (centered on @mymath{O}) and flat plane (light
gray) tangent to it at point @mymath{A}.}
+@end floatnode MakeNoise, , MakeProfiles, Modeling and fittings
-@section MakeNoise
+@dispmath{z=R\left(1\pm\sqrt{1-{r^2\over R^2}}\right).}menu
-* Noise basics:: Noise concepts and definitions.
-* Invoking astmknoise:: Options and arguments to MakeNoise.
-@end menudispmath{ds_s^2={dr^2\over 1-r^2/R^2}+r^2d\phi^2.}-@node Noise basics, Invoking astmknoise, MakeNoise, MakeNoise
-@subsection Noise basics
+@dispmath{ds_s^2={dr^2\over 1-Kr^2}+r^2d\phi^2.}@node Photon counting noise, Instrumental noise, Noise basics, Noise basics
-@subsubsection Photon counting noisedispmath{ds_s^2=dl^2+r^2d\phi^2.} qualitativeWith this scaling factor, the proper distance will also depend on time.
+As the universe expands, the distance between two given points will shift to
larger values.
+We thus define a distance measure, ordispmath{\mu=B+I_{nn}, \quad \sigma=\sqrt{B+I_{nn}}}node Instrumental noise, Final noised pixel value, Photon counting noise,
Noise basics
-@subsubsection Instrumental noisenode Extending distance concepts to 3D, Invoking astcosmiccal, Distance on a
2D curved space, CosmicCalculator
+@subsection Extending distance concepts to 3Ddispmath{\mu=I_{nn}, \quad \sigma=\sqrt{C^2+I_{nn}}}dispmath{ds_s^2=dr^2+r^2(d\theta^2+\sin^2{\theta}d\phi^2)+dw^2.}
-@dispmath{\mu=B+I_{nn}, \quad \sigma=\sqrt{C^2+B+I_{nn}}}
+@noindent
+But we can only work on a 3D curved space, so following exactly the same steps
and conventions as our 2D friend, we arrive at:noindent
+In a non-static universe (with a scale factor a(t)), the distance can be
written as:
-@node Generating random numbers, , Final noised pixel value, Noise basics
-@subsubsection Generating random numberscindex Random numbers
-@cindex Numbers, random
-As discussed above, to generate noise we need to make random samples of a
particular distribution.
-So it is important to understand some general concepts regardingc@dispmath{H(z){\equiv}\left(\dot{a}\over a\right)(z)=H_0E(z) }-There are two ways you can specify values for these environment variables.
-You can call them on the same command-line for example:-@example
-$ GSL_RNG_TYPE="taus" GSL_RNG_SEED=345 astmknoise input.fits
-@end example
+@c@dispmath{ \chi(r)={c\over H_0a_0}\int_0^z{dz'\over E(z')} }
+
+@c@dispmath{ d_A={a_0\chi(r)\over 1+z}, \quad d_L=a_0\chi(r)(1+z) }
+
+
+@node Invoking astcosmiccal, , Extending distance concepts to 3D,
CosmicCalculator
+@subsection Invoking CosmicCalculator
+
+CosmicCalculator will calculate cosmological variables based on the input
parameters.
+The executable name is @file{astcosmiccal} with the following general template
@example
-$ export GSL_RNG_TYPE="taus"
-$ export GSL_RNG_SEED=345
+$ astcosmiccal [OPTION...] ...
@end example-@cartouche
One line examples:
## Print basic cosmological properties at redshift 2.5:
+$ astcosmiccal -z2.5## Only print Comoving volume over 4pi stradian to z (Mpc^3):
+$ astcosmiccal --redshift=0.8 --volumenode Invoking astmknoise, , Noise basics, MakeNoise
-@subsection Invoking MakeNoise
+## Print luminosity distance, angular diameter distance and age
+## of universe in one row at redshift 0.4
+$ astcosmiccal -z0.4 -LAg
-MakeNoise will add noise to an existing image.
-The executable name is @file{astmknoise} with the following general templateexample
-$ astmknoise [OPTION ...] InputImage.fits
+## Print wavelength of all pre-defined spectral lines when
+## Lyman-alpha is observed at 4000 Angstroms.
+$ astcosmiccal --obsline=lyalpha,4000 --listlinesatz
@end example
-@noindent
-One line examples:@example
-## Add noise with a standard deviation of 100 to image.
-## (this is independent of the pixel value: not Poission noise)
-$ astmknoise --sigma=100 image.fits parameters that were
influential in making it.
-This is done for future reproducibility.+
+@node CosmicCalculator input options, CosmicCalculator basic cosmology
calculations, Invoking astcosmiccal, Invoking astcosmiccal
+@subsubsection CosmicCalculator input options
+
+The inputs to CosmicCalculator can be specified with the following options:
+@table @option
++
+@item -H FLT
+@itemx --H0=FLT
+Current expansion rate (in km sec@mymath{^{-1}} Mpc@mymath{^{-1}}).
+++
+@item -r FLT
+@itemx --oradiation=FLT
+Radiation density divided by the critical density in the current Universe
(@mymath{\Omega_{r,0}}).
++
+The pre-defined names are listed below, sorted from red (longer wavelength) to
blue (shorter wavelength).
+You can get this list on the command-line with the @option{--listlines}.
+
+@table @code
+@item siired
+[6731@AA{}] SII doublet's redder line.
+
+@item sii
+@cindex Doublet: SII
+@cindex SII doublet
+[6724@AA{}] SII doublet's mean center at .
+
+@item siiblue
+[6717@AA{}] SII doublet's bluer line.
+
+@item niired
+[6584@AA{}] NII doublet's redder line.
+
+@item nii
+@cindex Doublet: NII
+@cindex NII doublet
+[6566@AA{}] NII doublet's mean center.
+
+@item halpha
+@cindex H-alpha
+[6562.8@AA{}] H-@mymath{\alpha} line.
+
+@item niiblue
+[6548@AA{}] NII doublet's bluer line.
+
+@item oiiired-vis
+[5007@AA{}] OIII doublet's redder line in the visible.
++
+@item oiiiblue-vis
+[4959@AA{}] OIII doublet's bluer line in the visible.
+
+@item hbeta
+@cindex H-beta
+[4861.36@AA{}] H-@mymath{\beta} line.
+
+@item heii-vis
+[4686@AA{}] HeII doublet's redder line in the visible.
+
+@item hgamma
+@cindex H-gamma
+[4340.46@AA{}] H-@mymath{\gamma} line.
+
+@item hdelta
+@cindex H-delta
+[4101.74@AA{}] H-@mymath{\delta} line.
+
+@item hepsilon
+@cindex H-epsilon
+[3970.07@AA{}] H-@mymath{\epsilon} line.
+
+@item neiii
+[3869@AA{}] NEIII line.
+
+@item oiired
+[3729@AA{}] OII doublet's redder line.
+
+@item oii
+@cindex Doublet: OII
+@cindex OII doublet
+[3727.5@AA{}] OII doublet's mean center.
+
+@item oiiblue
+[3726@AA{}] OII doublet's bluer line.
+
+@item blimit
+@cindex Balmer limit
+[3646@AA{}] Balmer limit.
+
+@item mgiired
+[2803@AA{}] MgII doublet's redder line.
+
+@item mgii
+@cindex Doublet: MgII
+@cindex MgII doublet
+[2799.5@AA{}] MgII doublet's mean center.
+
+@item mgiiblue
+[2796@AA{}] MgII doublet's bluer line.
+
+@item ciiired
+[1909@AA{}] CIII doublet's redder line.
+
+@item ciii
+@cindex Doublet: CIII
+@cindex CIII doublet
+[1908@AA{}] CIII doublet's mean center.
+
+@item ciiiblue
+[1907@AA{}] CIII doublet's bluer line.
+
+@item si_iiired
+[1892@AA{}] SiIII doublet's redder line.
-@table @option
+@item si_iii
+@cindex Doublet: SiIII
+@cindex SiIII doublet
+[1887.5@AA{}] SiIII doublet's mean centeriiiblue
+[1883@AA{}] SiIII doublet's bluer line oiiired-uv
+[1666@AA{}] OIII doublet's redder line in the ultra-violet.
-@item -B
-@itemx --bgisbrightness
-The value given to @option{--background} should be interpretted as brightness,
not as a magnitude.iiiblue-uv
+[1661@AA{}] OIII doublet's bluer line heii-uv
+[1640@AA{}] HeII civred
+[1551@AA{}] CIV doublet's redder line
+@cindex Doublet: CIV
+@cindex CIV doublet
+[1549@AA{}] CIV doublet's mean centerblue
+[1548@AA{}] CIV doublet's bluer line nv
+[1240@AA{}] NV (four times ionized Sodium).
-@end table
+@item lyalpha
+@cindex Lyman-alpha
+[1215.67@AA{}] Lyman-@mymath{\alpha} line.
++@example
+$ astcosmiccal --redshift=0.832 | grep volume
+@end example
-@node High-level calculations, Library, Modeling and fittings, Top
-@chapter High-level calculations+@item -G
+@itemx --agenow
+The current age of the universe (given the input parameters) in Ga (Giga
annum, or billion years).
+@item -C
+@itemx --criticaldensitynow
+The current critical density (given the input parameters) in grams per
centimeter-cube (@mymath{g/cm^3}).
-@menu
-* CosmicCalculator:: Calculate cosmological variables
-@end menu@node CosmicCalculator, , High-level calculations, High-level calculations
-@section CosmicCalculator
+@item -A
+@itemx --angulardimdist
+The angular diameter distance to object at given redshift in Megaparsecs (Mpc curvedL
+@itemx --luminositydist
+The luminosityu
+@itemx --distancemodulus
+The distance modulus atg
+@itemx --age
+Age of the universe at given redshift in Ga (Giga annum, or billion years).c
+@itemx --criticaldensity
+The critical density at given redshift in grams per centimeter-cube
(@mymath{g/cm^3}@float Figure,flatplane
-@center@image{gnuastro-figures/flatplane, 10cm, , }
+@end table
-@caption{Two dimensional Cartesian and polar coordinates on a flat
-plane.}
-@end float+@node CosmicCalculator spectral line calculations, , CosmicCalculator basic
cosmology calculations, Invoking astcosmiccal
+@subsubsection CosmicCalculator spectral line calculationsWith the third axis added, a generic infinitesimal change over @emph{the full}
3D space corresponds to the distance:dispmath{ds_s^2=dx^2+dy^2+dz^2=dr^2+r^2d\phi^2+dz^2.}@float Figure,sphereandplane
-@center@image{gnuastro-figures/sphereandplane, 10cm, , }caption{2D spherical shell (centered on @mymath{O}) and flat plane (light
gray) tangent to it at point @mymath{A}.}
-@end float
+@table @optionz=R\left(1\pm\sqrt{1-{r^2\over R^2}}\right).}@example
+$ astcosmiccal --listlines \
+ | asttable --range=wavelength,4000,6000
+@end example-@dispmath{ds_s^2={dr^2\over 1-r^2/R^2}+r^2d\phi^2.}@dispmath{ds_s^2={dr^2\over 1-Kr^2}+r^2d\phi^2.}
+@end tableThereforemology+@node Installed scripts, Library, High-level calculations, Top
+@chapter Installed scriptsexample
+$ nano $(which astscript-NAME)
+@end exampleThese scripts also accept options and are in many ways similar to the programs
(see @ref{Common options}) with some minor differences:@node Extending distance concepts to 3D, Invoking astcosmiccal, Distance on a
2D curved space, CosmicCalculator
-@subsection Extending distance concepts to 3D@item
+They don't directly allocate any memory, so there is no @option{--minmapsizeitem
+They don't have an independent @option{--usage} option: when called with
@option{--usage}, they just recommend running @option{--helpThe output of @option{--help} is not configurable like the programs (see
@ref{--help}).noindent
-But we can only work on a 3D curved space, so following exactly the same steps
and conventions as our 2D friend, we arrive at:
+@end itemizenoindent
-In a non-static universe (with a scale factor a(t)), the distance can be
written as:
+@node Sort FITS files by night, Generate radial profile, Installed scripts,
Installed scripts
+@section Sort FITS files by nightH(z){\equiv}\left(\dot{a}\over a\right)(z)=H_0E(z) }
+You can use this script as a basis for making a much more highly customized
sorting script.
+Here are some examplesdispmath{ \chi(r)={c\over H_0a_0}\int_0^z{dz'\over E(z')} }-@c@dispmath{ d_A={a_0\chi(r)\over 1+z}, \quad d_L=a_0\chi(r)(1+z) }+@menu
+* Invoking astscript-sort-by-night:: Inputs and outputs to this script.
+@end menu
-@node Invoking astcosmiccal, , Extending distance concepts to 3D,
CosmicCalculator
-@subsection Invoking CosmicCalculator
+@node Invoking astscript-sort-by-night, , Sort FITS files by night, Sort FITS
files by night
+@subsection Invoking astscript-sort-by-night
-CosmicCalculator will calculate cosmological variables based on the input
parameters.
-The executable name is @file{astcosmiccal} with the following general template-
-## Only print Comoving volume over 4pi stradian to z (Mpc^3):
-$ astcosmiccal --redshift=0.8 --volume
-
-## Print redshift and age of universe when Lyman-alpha line is
-## at 6000 angstrom (another way to specify redshift).
-$ astcosmiccal --obsline=lyalpha,6000 --age
-
-## Print luminosity distance, angular diameter distance and age
-## of universe in one row at redshift 0.4
-$ astcosmiccal -z0.4 -LAg
-## Use the DATE-OBS keyword
+$ astscript-sort-by-night --key=DATE-OBS /path/to/data/*.fits
-## Print wavelength of all pre-defined spectral lines when
-## Lyman-alpha is observed at 4000 Angstroms.
-$ astcosmiccal --obsline=lyalpha,4000 --listlinesatz
+## Make links to the input files with the `img-' prefix
+$ astscript-sort-by-night --link --prefix=img- /path/to/data/*.fitsWithout any particular output requested (and only a givenThe inputs to CosmicCalculator can be specified with the following options:
-@table @option@item -k STR
+@itemx --key=STR
+The keyword name that contains the FITS date format to classify/sort by.
@item -H FLT
-@itemx --H0=FLT
-Current expansion rate (in km sec@mymath{^{-1}} Mpc@mymath{^{-1}}).
- linefile SAO DS9 region files from table, Sort FITS
files by night, Installed scriptsIf the directory doesn't exist at run-time, this script will create it.
+After the output will
usually have many other sources with your main target.
+A crude solution is to use sigma-clipped measurements for the profile.
+However, sigma-clipped measurements can easily be biased-@end table
+@item -c FLT[,FLT[,...]]
+@itemx --center=FLT[,FLT[,...]]
+The central position of the radial profile.
+This option is used for placing the center of the profiles.
+This parameter is used in @ref{Crop} to center an crop the region.
+The positions along each dimension must be separated by a comma (@key{,}) and
fractions are also acceptable.
+The number of values given to this option must be the same as the dimensions
of the input dataset.
+The units of the coordinates are read based on the value to the
@option{--mode} option, see below.
-@end table
+@item -O STR
+@itemx --mode=STR
+Interpret the center position of the object (values given to
@option{---
-@example
-z=3.12
-vol=$(astcosmiccal --redshift=$z --volume)
-@end example
+@item -v INT
+@itemx --oversample=INT
+Oversample the input dataset to the fraction given to this option.
+Therefore if you set @option{--rmax=20} for example and
@option{--oversample=5}, your output will have 100 rows (without
@option{--oversample} it will only have 20 rows).
+Unless the object is heavily undersampled (the pixels are larger than the
actual object), this method provides a much more accurate result and there are
sufficient number of pixels to get the profile accurately.If the directory doesn't exist at run-time, this script will create it.
+Once the radial profile has been obtained, this directory is removed.
+You can disable the deletion of the temporary directory with the
@option{--keeptmp} option-@end table
+@node SAO DS9 region files from table, , Generate radial profile, Installed
scripts
+@section SAO DS9 region files from-@node CosmicCalculator spectral line calculations, , CosmicCalculator basic
cosmology calculations, Invoking astcosmiccal
-@subsubsection CosmicCalculator spectral line calculations
+@menu
+* Invoking astscript-ds9-region:: How to call astscript-ds9-region
+@end menunode Invoking astscript-ds9-region, , SAO DS9 region files from table, SAO
DS9 region files from table
+@subsection Invoking astscript-ds9-region@example
-$ astcosmiccal --obsline=lyalpha,8000 --lineatz=halpha
-$ astcosmiccal --obsline=lyalpha,8000 --listlinesatz
+## Use the RA and DEC columns of 'table.fits' for the region file.
+$ astscript-ds9-regionds9-regionds9-region -c1,2 --color=red -obright.reg
+$ asttable cat.fits --range=MAG_F160W,28:29 -cRA,DEC \
+ | ./astscript-ds9-region@end table
@@ -20554,7 +2133325063,22 +25842,53 @@ TPD is a superset of all these, hence it has both
prior and sequeal distortion c
More information is given in the documentation of @code{dis.h}, from the
WCSLIB
manual@footnote{@url{
@end deffn
+@deffn Macro GAL_WCS_COORDSYS_EQB1950
+@deffnx Macro GAL_WCS_COORDSYS_EQJ2000
+@deffnx Macro GAL_WCS_COORDSYS_ECB1950
+@deffnx Macro GAL_WCS_COORDSYS_ECJ2000
+@deffnx Macro GAL_WCS_COORDSYS_GALACTIC
+@deffnx Macro GAL_WCS_COORDSYS_SUPERGALACTIC
+@deffnx Macro GAL_WCS_COORDSYS_INVALIDRecognized WCS coordinate systems in Gnuastro.
+@code{EQ} and @code{EC} stand for the Equatorial and Ecliptic coordinate
systems.
+In the equatorial and ecliptic coordinates, @code{B1950} stands for the
Besselian 1950 epoch and @code{J2000} stands for the Julian 2000 epoch.
+@end deffn
+
+@deffn Macro GAL_WCS_LINEAR_MATRIX_PC
+@deffnx Macro GAL_WCS_LINEAR_MATRIX_CD
+@deffnx Macro GAL_WCS_LINEAR_MATRIX_INVALID
+Identifiers of the linear transformation matrix: either in the @code{PCi_j} or
the @code{CDi_j} formalism.
+For more, see the description of @option{--wcslinearmatrix} in @ref{Input
output options}.
+@end deffn
+
+
@deffn Macro GAL_WCS_FLTERROR
Limit of rounding for floating point errors.
@end deffn
-@deftypefun {struct wcsprm *} gal_wcs_read_fitsptr (fitsfile @code{*fptr},
size_t @code{hstartwcs}, size_t @code{hendwcs}, int @code{*nwcs})
-[@strong{Not thread-safe}] Return the WCSLIB @code{wcsprm} structure that
-is read from the CFITSIO @code{fptr} pointer to an opened FITS file. Also
-put the number of coordinate representations found into the space that
-@code{nwcs} points to. To read the WCS structure directly from a filename,
-see @code{gal_wcs_read} below. After processing has finished, you can free
-the returned structure with WCSLIB's @code{wcsvfree} keyword:
+@deftypefun {struct wcsprm *} gal_wcs_read_fitsptr (fitsfile @code{*fptr}, int
@code{linearmatrix}, size_t @code{hstartwcs}, size_t @code{hendwcs}, int
@code{*nwcs})
+[@strong{Not thread-safe}] Return the WCSLIB @code{wcsprm} structure that is
read from the CFITSIO @code{fptr} pointer to an opened FITS file.
+Also put the number of coordinate representations found into the space that
@code{nwcs} points to.
+To read the WCS structure directly from a filename, see @code{gal_wcs_read}
below.
+After processing has finished, you can free the returned structure with
WCSLIB's @code{wcsvfree} keyword:
@example
status = wcsvfree(&nwcs,&wcs);
@end example
+The @code{linearmatrix} argument takes one of three values: @code{0},
@code{GAL_WCS_LINEAR_MATRIX_PC} and @code{GAL_WCS_LINEAR_MATRIX_CD}.
+It will determine the format of the WCS when it is later written to file with
@code{gal_wcs_write} or @code{gal_wcs_write_in_fitsptr} (which is called by
@code{gal_fits_img_write})
+So if you don't want to write the WCS into a file later, just give it a value
of @code{0}.
+For more on the difference between these modes, see the description of
@option{--wcslinearmatrix} in @ref{Input output options}.
+
If you don't want to search the full FITS header for WCS-related FITS keywords
(for example due to conflicting keywords), but only a specific range of the
header keywords you can use the @code{hstartwcs} and @code{hendwcs} arguments
to specify the keyword number range (counting from zero).
If @code{hendwcs} is larger than @code{hstartwcs}, then only keywords in the
given range will be checked.
Hence, to ignore this feature (and search the full FITS header), give both
these arguments the same value.
@@ -25090,7 +25900,7 @@ This function is just a wrapper over WCSLIB's
@code{wcspih} function which is no
Therefore, be sure to not call this function simultaneously (over multiple
threads).
@end deftypefun
-@deftypefun {struct wcsprm *} gal_wcs_read (char @code{*filename}, char
@code{*hdu}, size_t @code{hstartwcs}, size_t @code{hendwcs}, int @code{*nwcs})
+@deftypefun {struct wcsprm *} gal_wcs_read (char @code{*filename}, char
@code{*hdu}, int @code{linearmatrix}, size_t @code{hstartwcs}, size_t
@code{hendwcs}, int @code{*nwcs})
[@strong{Not thread-safe}] Return the WCSLIB structure that is read from the
HDU/extension @code{hdu} of the file @code{filename}.
Also put the number of coordinate representations found into the space that
@code{nwcs} points to.
Please see @code{gal_wcs_read_fitsptr} for more.
@@ -25176,6 +25986,27 @@ correspond to the pixel scale, and the @code{PCi_j}
will correction show
the rotation.
@end deftypefun
+@deftypefun void gal_wcs_to_cd (struct wcsprm @code{*wcs})
+Make sure that the WCS structure's @code{PCi_j} and @code{CDi_j} keywords have
the same value and that the @code{CDELTi} keywords have a value of 1.0.
+Also, set the @code{wcs->altlin=2} (for the @code{CDi_j} formalism).
+With these changes @code{gal_wcs_write_in_fitsptr} (and thus
@code{gal_wcs_write} and @code{gal_fits_img_write} and its derivates) will have
an output file in the format of @code{CDi_j}.
+@end deftypefun
+
+@deftypefun int gal_wcs_coordsys_from_string (char @code{*coordsys})
+Convert the given string to Gnuastro's integer-based WCS coordinate system
identifier (one of the @code{GAL_WCS_COORDSYS_*}, listed above).
+The expected strings can be seen in the description of the
@option{--wcscoordsys} option of the Fits program, see @ref{Keyword inspection
and manipulation}.
+@end deftypefun
+
+@deftypefun int gal_wcs_coordsys_identify (struct wcsprm @code{*wcs})
+Read the given WCS structure and return its coordinate system as one of
Gnuastro's WCS coordinate system identifiers (the macros
@code{GAL_WCS_COORDSYS_*}, listed above).
+@end deftypefun
+
+@deftypefun {struct wcsprm *} gal_wcs_coordsys_convert (struct wcsprm
@code{*inwcs}, int @code{coordsysid})
+Return a newly allocated WCS structure with the @code{coordsysid} coordinate
system identifier.
+The Gnuastro WCS distortion identifiers are defined in the
@code{GAL_WCS_COORDSYS_*} macros mentioned above.
+Since the returned dataset is newly allocated, if you don't need the original
dataset after this, use the WCSLIB library function @code{wcsfree} to free the
input, for example @code{wcsfree(inwcs)}.
+@end deftypefun
+
@deftypefun int gal_wcs_distortion_from_string (char @code{*distortion})
Convert the given string (assumed to be a FITS-standard, string-based
distortion identifier) to a Gnuastro's integer-based distortion identifier (one
of the @code{GAL_WCS_DISTORTION_*} macros defined above).
The sting-based distortion identifiers have three characters and are all in
capital letters.
@@ -25248,9 +26079,9 @@ return @code{NULL}.
@end deftypefun
@deftypefun double gal_wcs_pixel_area_arcsec2 (struct wcsprm @code{*wcs})
-Return the pixel area of @code{wcs} in arc-second squared. If the input WCS
-structure is not two dimensional and the units (@code{CUNIT} keywords) are
-not @code{deg} (for degrees), then this function will return a NaN.
+Return the pixel area of @code{wcs} in arc-second squared.
+This only works when the input dataset has atleast two dimensions and the
units of the first two dimensions (@code{CUNIT} keywords) are @code{deg} (for
degrees).
+In other cases, this function will return a NaN.
@end deftypefun
@deftypefun int gal_wcs_coverage (char @code{*filename}, char @code{*hdu},
size_t @code{*ondim}, double @code{**ocenter}, double @code{**owidth}, double
@code{**omin}, double @code{**omax})
@@ -28179,6 +29010,20 @@ Convert the input Declination (Dec) degree (a single
floating point number) to o
If @code{usecolon!=0}, then the delimiters between the components will be
colons: @code{_:_:_}.
@end deftypefun
+@deftypefun double gal_units_counts_to_mag (double @code{counts}, double
@code{zeropoint})
+@cindex Magnitude
+Convert counts to magnitudes through the given zero point.
+For more on the equation, see @ref{Brightness flux magnitude}.
+@end deftypefun
+
+@deftypefun double gal_units_counts_to_jy (double @code{counts}, double
@code{zeropoint_ab})
+@cindex Jansky (Jy)
+@cindex AB Magnitude
+@cindex Magnitude, AB
+Convert counts to Janskys through an AB magnitude-based zero point.
+For more on the equation, see @ref{Brightness flux magnitude}.
+@end deftypefun
+
@node Spectral lines library, Cosmology library, Unit conversion library
(@file{units.h}), Gnuastro library
@subsection Spectral lines library (@file{speclines.h})
@@ -30275,10 +31120,38 @@ the body with `@code{This fixes bug #ID.}', or
`@code{This finishes task
full description when reading the commit message, so give a short
introduction too.
@end itemize
-
@end table
+Below you can see a good commit message example (don't forget to read it, it
has tips for you).
+After reading this, please run @command{git log} on the @code{master} branch
and read some of the recent commits for more realistic examples.
+
+@example
+The first line should be the title of the commit
+
+An empty line is necessary after the title so Git doesn't confuse
+lines. This top paragraph of the body of the commit usually describes
+the reason this commit was done. Therefore it usually starts with
+"Until now ...". It is very useful to explain the reason behind the
+change, things that aren't immediately obvious when looking into the
+code. You don't need to list the names of the files, or what lines
+have been changed, don't forget that the code changes are fully
+stored within Git :-).
+
+In the second paragraph (or any later paragraph!) of the body, we
+describe the solution and why (not "how"!) the particular solution
+was implemented. So we usually start this part of the commit body
+with "With this commit ...". Again, you don't need to go into the
+details that can be seen from the 'git diff' command (like the
+file names that have been changed or the code that has been
+implemented). The imprtant thing here is the things that aren't
+immediately obvious from looking into the code.
+
+You can continue the explanation and it is encouraged to be very
+explicit about the "human factor" of the change as much as possible,
+not technical details.
+@end example
+
@node Production workflow, Forking tutorial, Commit guidelines, Contributing
to Gnuastro
@subsection Production workflow
@@ -30569,10 +31442,15 @@ in a special way), are done with installed Bash
scripts (all prefixed with
similarly (with minor differences, see @ref{Installed scripts}).
@table @code
+@item astscript-ds9-region
diff --git a/lib/Makefile.am b/lib/Makefile.am
index 5b427c6..4b4b297 100644
--- a/lib/Makefile.am
+++ b/lib/Makefile.am
@@ -150,6 +150,7 @@ gnuastro/config.h: Makefile $(internaldir)/config.h.in
-e 's|@HAVE_WCSLIB_DIS_H[@]|$(HAVE_WCSLIB_DIS_H)|g' \
-e 's|@HAVE_WCSLIB_MJDREF[@]|$(HAVE_WCSLIB_MJDREF)|g' \
-e 's|@HAVE_WCSLIB_OBSFIX[@]|$(HAVE_WCSLIB_OBSFIX)|g' \
+ -e 's|@HAVE_WCSLIB_WCSCCS[@]|$(HAVE_WCSLIB_WCSCCS)|g' \
-e 's|@HAVE_WCSLIB_VERSION[@]|$(HAVE_WCSLIB_VERSION)|g' \
-e 's|@HAVE_PTHREAD_BARRIER[@]|$(HAVE_PTHREAD_BARRIER)|g' \
-e 's|@RESTRICT_REPLACEMENT[@]|$(RESTRICT_REPLACEMENT)|g' \
diff --git a/lib/arithmetic-set.c b/lib/arithmetic-set.c
index 24da3cb..f4d9d68 100644
--- a/lib/arithmetic-set.c
+++ b/lib/arithmetic-set.c
@@ -116,8 +116,10 @@ gal_arithmetic_set_name(struct gal_arithmetic_set_params
*p, char *token)
error(EXIT_FAILURE, 0, "%s: a bug! Please contact us at %s to "
"fix the problem. The 'name' element should be NULL at "
"this point, but it isn't", __func__, PACKAGE_BUGREPORT);
- if(p->named->unit) { free(p->named->unit); p->named->unit=NULL;
}
- if(p->named->comment) { free(p->named->comment); p->named->comment=NULL;
}
+ if(p->named->unit)
+ { free(p->named->unit); p->named->unit=NULL; }
+ if(p->named->comment)
+ { free(p->named->comment); p->named->comment=NULL; }
gal_checkset_allocate_copy(varname, &p->named->name);
}
else
diff --git a/lib/arithmetic.c b/lib/arithmetic.c
index e7f68d9..8f98575 100644
--- a/lib/arithmetic.c
+++ b/lib/arithmetic.c
@@ -1384,9 +1384,9 @@ arithmetic_multioperand(int operator, int flags,
gal_data_t *list,
{
case GAL_ARITHMETIC_OP_QUANTILE:
if(p1<0 || p1>1)
- error(EXIT_FAILURE, 0, "%s: the parameter given to the 'quantile' "
- "operator must be between (and including) 0 and 1. The "
- "given value is: %g", __func__, p1);
+ error(EXIT_FAILURE, 0, "%s: the parameter given to the "
+ "'quantile' operator must be between (and including) "
+ "0 and 1. The given value is: %g", __func__, p1);
break;
}
}
@@ -1465,15 +1465,17 @@ arithmetic_multioperand(int operator, int flags,
gal_data_t *list,
/* Clean up and return. Note that the operation might have been done in
- place. In that case, the top most list element was used. So we need to
- check before freeing each data structure. */
+ place. In that case, a list element was used. So we need to check
+ before freeing each data structure. If we are on the designated output
+ dataset, we should set its 'next' pointer to NULL so it isn't treated
+ as a list any more by future functions. */
if(flags & GAL_ARITHMETIC_FREE)
{
tmp=list;
while(tmp!=NULL)
{
ttmp=tmp->next;
- if(tmp!=out) gal_data_free(tmp);
+ if(tmp==out) tmp->next=NULL; else gal_data_free(tmp);
tmp=ttmp;
}
if(params) gal_list_data_free(params);
@@ -1775,6 +1777,10 @@ arithmetic_function_binary_flt(int operator, int flags,
gal_data_t *il,
BINFUNC_F_OPERATOR_SET( pow, +0 ); break;
case GAL_ARITHMETIC_OP_ATAN2:
BINFUNC_F_OPERATOR_SET( atan2, *180.0f/pi ); break;
+ case GAL_ARITHMETIC_OP_COUNTS_TO_MAG:
+ BINFUNC_F_OPERATOR_SET( gal_units_counts_to_mag, +0 ); break;
+ case GAL_ARITHMETIC_OP_COUNTS_TO_JY:
+ BINFUNC_F_OPERATOR_SET( gal_units_counts_to_jy, +0 ); break;
default:
error(EXIT_FAILURE, 0, "%s: operator code %d not recognized",
__func__, operator);
@@ -1958,6 +1964,10 @@ gal_arithmetic_set_operator(char *string, size_t
*num_operands)
{ op=GAL_ARITHMETIC_OP_DEGREE_TO_RA; *num_operands=1; }
else if (!strcmp(string, "degree-to-dec"))
{ op=GAL_ARITHMETIC_OP_DEGREE_TO_DEC; *num_operands=1; }
+ else if (!strcmp(string, "counts-to-mag"))
+ { op=GAL_ARITHMETIC_OP_COUNTS_TO_MAG; *num_operands=2; }
+ else if (!strcmp(string, "counts-to-jy"))
+ { op=GAL_ARITHMETIC_OP_COUNTS_TO_JY; *num_operands=2; }
/* Statistical/higher-level operators. */
else if (!strcmp(string, "minvalue"))
@@ -2131,6 +2141,8 @@ gal_arithmetic_operator_string(int operator)
case GAL_ARITHMETIC_OP_DEC_TO_DEGREE: return "dec-to-degree";
case GAL_ARITHMETIC_OP_DEGREE_TO_RA: return "degree-to-ra";
case GAL_ARITHMETIC_OP_DEGREE_TO_DEC: return "degree-to-dec";
+ case GAL_ARITHMETIC_OP_COUNTS_TO_MAG: return "counts-to-mag";
+ case GAL_ARITHMETIC_OP_COUNTS_TO_JY: return "counts-to-jy";
case GAL_ARITHMETIC_OP_MINVAL: return "minvalue";
case GAL_ARITHMETIC_OP_MAXVAL: return "maxvalue";
@@ -2253,6 +2265,8 @@ gal_arithmetic(int operator, size_t numthreads, int
flags, ...)
/* Binary function operators. */
case GAL_ARITHMETIC_OP_POW:
case GAL_ARITHMETIC_OP_ATAN2:
+ case GAL_ARITHMETIC_OP_COUNTS_TO_MAG:
+ case GAL_ARITHMETIC_OP_COUNTS_TO_JY:
d1 = va_arg(va, gal_data_t *);
d2 = va_arg(va, gal_data_t *);
out=arithmetic_function_binary_flt(operator, flags, d1, d2);
diff --git a/lib/fits.c b/lib/fits.c
index 10a0bac..0f31ec7 100644
--- a/lib/fits.c
+++ b/lib/fits.c
@@ -1899,6 +1899,36 @@ gal_fits_key_write(gal_fits_list_key_t **keylist, char
*title,
+/* Fits doesn't allow NaN values, so if the type of float or double, we'll
+ just check to see if its NaN or not and let the user know the keyword
+ name (to help them fix it). */
+static void
+gal_fits_key_write_in_ptr_nan_check(gal_fits_list_key_t *tmp)
+{
+ int nanwarning=0;
+
+ /* Check the value. */
+ switch(tmp->type)
+ {
+ case GAL_TYPE_FLOAT32:
+ if( isnan( ((float *)(tmp->value))[0] ) ) nanwarning=1;
+ break;
+ case GAL_TYPE_FLOAT64:
+ if( isnan( ((double *)(tmp->value))[0] ) ) nanwarning=1;
+ break;
+ }
+
+ /* Print the warning. */
+ if(nanwarning)
+ error(EXIT_SUCCESS, 0, "%s: (WARNING) value of '%s' is NaN "
+ "and FITS doesn't recognize a NaN key value", __func__,
+ tmp->keyname);
+}
+
+
+
+
+
/* Write the keywords in the gal_fits_list_key_t linked list to the FITS
file. Every keyword that is written is freed, that is why we need the
pointer to the linked list (to correct it after we finish). */
@@ -1928,6 +1958,10 @@ gal_fits_key_write_in_ptr(gal_fits_list_key_t **keylist,
fitsfile *fptr)
/* Write the basic key value and comments. */
if(tmp->value)
{
+ /* Print a warning if the value is NaN. */
+ gal_fits_key_write_in_ptr_nan_check(tmp);
+
+ /* Write/Update the keyword value. */
if( fits_update_key(fptr, gal_fits_type_to_datatype(tmp->type),
tmp->keyname, tmp->value, tmp->comment,
&status) )
@@ -2052,7 +2086,7 @@ gal_fits_key_write_version_in_ptr(gal_fits_list_key_t
**keylist, char *title,
if(gitdescribe)
{
fits_update_key(fptr, TSTRING, "COMMIT", gitdescribe,
- "Git's commit description in running dir.", &status);
+ "Git commit in running directory.", &status);
free(gitdescribe);
}
diff --git a/lib/gnuastro-internal/commonopts.h
b/lib/gnuastro-internal/commonopts.h
index d55f98b..16fc496 100644
--- a/lib/gnuastro-internal/commonopts.h
+++ b/lib/gnuastro-internal/commonopts.h
@@ -276,6 +276,20 @@ struct argp_option gal_commonopts_options[] =
gal_options_read_tableformat
},
{
+ "wcslinearmatrix",
+ GAL_OPTIONS_KEY_WCSLINEARMATRIX,
+ "STR",
+ 0,
+ "WCS linear matrix of output ('pc' or 'cd').",
+ GAL_OPTIONS_GROUP_OUTPUT,
+ &cp->wcslinearmatrixread_wcslinearmatrix
+ },
+ {
"dontdelete",
GAL_OPTIONS_KEY_DONTDELETE,
0,
@@ -342,7 +356,7 @@ struct argp_option gal_commonopts_options[] =
GAL_OPTIONS_KEY_MINMAPSIZE,
"INT",
0,
- "Minimum bytes in array to not use ram RAM.",
+ "Min. bytes to avoid RAM automatically.",
GAL_OPTIONS_GROUP_OPERATING_MODE,
&cp->minmapsize,
GAL_TYPE_SIZE_T,
diff --git a/lib/gnuastro-internal/options.h b/lib/gnuastro-internal/options.h
index fdb7478..343ebf8 100644
--- a/lib/gnuastro-internal/options.h
+++ b/lib/gnuastro-internal/options.h
@@ -125,6 +125,7 @@ enum options_common_keys
GAL_OPTIONS_KEY_INTERPONLYBLANK,
GAL_OPTIONS_KEY_INTERPMETRIC,
GAL_OPTIONS_KEY_INTERPNUMNGB,
+ GAL_OPTIONS_KEY_WCSLINEARMATRIX,
};
@@ -194,9 +195,10 @@ struct gal_options_common_params
/* Output. */
char *output; /* Directory containg output. */
uint8_t type; /* Data type of output. */
+ uint8_t tableformat; /* Internal code for output table format. */
+ uint8_t wcslinearmatrix; /* WCS matrix to use (PC or CD). */
uint8_t dontdelete; /* ==1: Don't delete existing file. */
uint8_t keepinputdir; /* Keep input directory for auto output. */
- uint8_t tableformat; /* Internal code for output table format. */
/* Operating modes. */
uint8_t quiet; /* Only print errors. */
@@ -276,6 +278,10 @@ gal_options_read_searchin(struct argp_option *option, char
*arg,
char *filename, size_t lineno, void *junk);
void *
+gal_options_read_wcslinearmatrix(struct argp_option *option, char *arg,
+ char *filename, size_t lineno, void *junk);
+
+void *
gal_options_read_tableformat(struct argp_option *option, char *arg,
char *filename, size_t lineno, void *junk);
diff --git a/lib/gnuastro/arithmetic.h b/lib/gnuastro/arithmetic.h
index b1719df..49d6930 100644
--- a/lib/gnuastro/arithmetic.h
+++ b/lib/gnuastro/arithmetic.h
@@ -120,10 +120,12 @@ enum gal_arithmetic_operators
GAL_ARITHMETIC_OP_ACOSH, /* Inverse hyperbolic cosine. */
GAL_ARITHMETIC_OP_ATANH, /* Inverse hyperbolic tangent. */
- GAL_ARITHMETIC_OP_RA_TO_DEGREE, /* right ascension to decimal */
- GAL_ARITHMETIC_OP_DEC_TO_DEGREE,/* declination to decimal */
- GAL_ARITHMETIC_OP_DEGREE_TO_RA, /* right ascension to decimal */
- GAL_ARITHMETIC_OP_DEGREE_TO_DEC,/* declination to decimal */
+ GAL_ARITHMETIC_OP_RA_TO_DEGREE, /* right ascension to decimal. */
+ GAL_ARITHMETIC_OP_DEC_TO_DEGREE,/* declination to decimal. */
+ GAL_ARITHMETIC_OP_DEGREE_TO_RA, /* right ascension to decimal. */
+ GAL_ARITHMETIC_OP_DEGREE_TO_DEC,/* declination to decimal. */
+ GAL_ARITHMETIC_OP_COUNTS_TO_MAG,/* Counts to magnitude. */
+ GAL_ARITHMETIC_OP_COUNTS_TO_JY, /* Counts to Janskys with AB-mag zeropoint.
*/
GAL_ARITHMETIC_OP_MINVAL, /* Minimum value of array. */
GAL_ARITHMETIC_OP_MAXVAL, /* Maximum value of array. */
diff --git a/lib/gnuastro/units.h b/lib/gnuastro/units.h
index 0543e67..3243f1f 100644
--- a/lib/gnuastro/units.h
+++ b/lib/gnuastro/units.h
@@ -62,16 +62,22 @@ gal_units_extract_decimal(char *convert, const char
*delimiter,
double *args, size_t n);
double
-gal_units_ra_to_degree (char *convert);
+gal_units_ra_to_degree(char *convert);
double
-gal_units_dec_to_degree (char *convert);
+gal_units_dec_to_degree(char *convert);
char *
-gal_units_degree_to_ra (double decimal, int usecolon);
+gal_units_degree_to_ra(double decimal, int usecolon);
char *
-gal_units_degree_to_dec (double decimal, int usecolon);
+gal_units_degree_to_dec(double decimal, int usecolon);
+
+double
+gal_units_counts_to_mag(double counts, double zeropoint);
+
+double
+gal_units_counts_to_jy(double counts, double zeropoint_ab);
__END_C_DECLS /* From C++ preparations */
diff --git a/lib/gnuastro/wcs.h b/lib/gnuastro/wcs.h
index 8ad29ba..dfe430a 100644
--- a/lib/gnuastro/wcs.h
+++ b/lib/gnuastro/wcs.h
@@ -70,6 +70,28 @@ enum gal_wcs_distortions
GAL_WCS_DISTORTION_WAT, /* The WAT polynomial distortion. */
};
+/* Macros to identify coordinate system for convesions. */
+enum gal_wcs_coordsys
+{
+ GAL_WCS_COORDSYS_INVALID, /* Invalid (=0 by C standard). */
+
+ GAL_WCS_COORDSYS_EQB1950, /* Equatorial B1950 */
+ GAL_WCS_COORDSYS_EQJ2000, /* Equatorial J2000 */
+ GAL_WCS_COORDSYS_ECB1950, /* Ecliptic B1950 */
+ GAL_WCS_COORDSYS_ECJ2000, /* Ecliptic J2000 */
+ GAL_WCS_COORDSYS_GALACTIC, /* Galactic */
+ GAL_WCS_COORDSYS_SUPERGALACTIC, /* Super-galactic */
+};
+
+/* Macros to identify the type of distortion for conversions. */
+enum gal_wcs_linear_matrix
+{
+ GAL_WCS_LINEAR_MATRIX_INVALID, /* Invalid (=0 by C standard). */
+
+ GAL_WCS_LINEAR_MATRIX_PC,
+ GAL_WCS_LINEAR_MATRIX_CD,
+};
+
@@ -78,16 +100,17 @@ enum gal_wcs_distortions
*********** Read WCS ***********
*************************************************************/
struct wcsprm *
-gal_wcs_read_fitsptr(fitsfile *fptr, size_t hstartwcs, size_t hendwcs,
- int *nwcs);
+gal_wcs_read_fitsptr(fitsfile *fptr, int linearmatrix, size_t hstartwcs,
+ size_t hendwcs, int *nwcs);
struct wcsprm *
-gal_wcs_read(char *filename, char *hdu, size_t hstartwcs,
+gal_wcs_read(char *filename, char *hdu, int linearmatrix, size_t hstartwcs,
size_t hendwcs, int *nwcs););
+ double *pc, char **cunit, char **ctype, size_t ndim,
+ int linearmatrix);
char *
gal_wcs_dimension_name(struct wcsprm *wcs, size_t dimension);
@@ -107,6 +130,19 @@ gal_wcs_write_in_fitsptr(fitsfile *fptr, struct wcsprm
*wcs);
+/*************************************************************
+ *********** Distortions ***********
+ *************************************************************/
+int
+gal_wcs_coordsys_from_string(char *coordsys);
+
+int
+gal_wcs_coordsys_identify(struct wcsprm *inwcs);
+
+struct wcsprm *
+gal_wcs_coordsys_convert(struct wcsprm *inwcs, int coordsysid);
+
+
/*************************************************************
*********** Distortions ***********
@@ -149,6 +185,9 @@ gal_wcs_clean_errors(struct wcsprm *wcs);
void
gal_wcs_decompose_pc_cdelt(struct wcsprm *wcs);
+void
+gal_wcs_to_cd(struct wcsprm *wcs);
+
double
gal_wcs_angular_distance_deg(double r1, double d1, double r2, double d2);
diff --git a/lib/options.c b/lib/options.c
index e029072..ba51988 100644
--- a/lib/options.c
+++ b/lib/options.c
@@ -28,6 +28,7 @@ along with Gnuastro. If not, see
<
#include <stdlib.h>
#include <string.h>
+#include <gnuastro/wcs.h>
#include <gnuastro/git.h>
#include <gnuastro/txt.h>
#include <gnuastro/fits.h>
@@ -477,6 +478,54 @@ gal_options_read_searchin(struct argp_option *option, char
*arg,
void *
+gal_options_read_wcslinearmatrix(struct argp_option *option, char *arg,
+ char *filename, size_t lineno, void *junk)
+{
+ char *str;
+ uint8_t value=GAL_WCS_LINEAR_MATRIX_INVALID;
+ if(lineno==-1)
+ {
+ /* The output must be an allocated string (will be 'free'd later). */
+ value=*(uint8_t *)(option->value);
+ switch(value)
+ {
+ case GAL_WCS_LINEAR_MATRIX_PC: gal_checkset_allocate_copy("pc", &str);
+ break;
+ case GAL_WCS_LINEAR_MATRIX_CD: gal_checkset_allocate_copy("cd", &str);
+ break;
+ default:
+ error(EXIT_FAILURE, 0, "%s: a bug! Please contact us at '%s' "
+ "to fix the problem. %u is not a recognized WCS rotation "
+ "matrix code", __func__, PACKAGE_BUGREPORT, value);
+ }
+ return str;
+ }
+ else
+ {
+ /* If the option is already set, just return. */
+ if(option->set) return NULL;
+
+ /* Read the value. */
+ if( !strcmp(arg, "pc") ) value = GAL_WCS_LINEAR_MATRIX_PC;
+ else if( !strcmp(arg, "cd") ) value = GAL_WCS_LINEAR_MATRIX_CD;
+ else
+ error_at_line(EXIT_FAILURE, 0, filename, lineno, "'%s' (value "
+ "to '%s' option) couldn't be recognized as a known "
+ "WCS rotation matrix. Acceptable values are 'pc' "
+ "or 'cd'", arg, option->name);
+ *(uint8_t *)(option->value)=value;
+
+ /* For no un-used variable warning. This function doesn't need the
+ pointer.*/
+ return junk=NULL;
+ }
+}
+
+
+
+
+
+void *
gal_options_read_tableformat(struct argp_option *option, char *arg,
char *filename, size_t lineno, void *junk)
{
diff --git a/lib/txt.c b/lib/txt.c
index 7f2c942..5ed3978 100644
--- a/lib/txt.c
+++ b/lib/txt.c
@@ -1513,6 +1513,11 @@ txt_write_keys(FILE *fp, struct gal_fits_list_key_t
**keylist)
tmp->title);
if(tmp->tfree) free(tmp->title);
}
+ else if (tmp->fullcomment)
+ {
+ fprintf(fp, "# %s\n", tmp->fullcomment);
+ if(tmp->fcfree) free(tmp->fullcomment);
+ }
else
{
/* For a string type, we need to return a pointer to the
diff --git a/lib/units.c b/lib/units.c
index 20146e2..ce9e873 100644
--- a/lib/units.c
+++ b/lib/units.c
@@ -331,3 +331,48 @@ gal_units_degree_to_dec(double decimal, int usecolon)
/* Return the final string. */
return dec;
}
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+/**********************************************************************/
+/**************** Flux conversions *****************/
+/**********************************************************************/
+
+/* Convert counts to magnitude using the given zeropoint. */
+double
+gal_units_counts_to_mag(double counts, double zeropoint)
+{
+ return ( counts > 0.0f
+ ? ( -2.5f * log10(counts) + zeropoint )
+ : NAN );
+}
+
+
+
+
+
+/* Convert Pixel values to Janskys with an AB-magnitude based
+ zero-point. See the "Brightness, Flux, Magnitude and Surface
+ brightness". */
+double
+gal_units_counts_to_jy(double counts, double zeropoint_ab)
+{
+ return counts * 3631 * pow(10, -1 * zeropoint_ab / 2.5);
+}
diff --git a/lib/wcs.c b/lib/wcs.c
index 0d2a508..0b2b33a 100644
--- a/lib/wcs.c
+++ b/lib/wcs.c
@@ -53,14 +53,6 @@ along with Gnuastro. If not, see
<
-/* Static functions on for this file. */
-static void
-gal_wcs_to_cd(struct wcsprm *wcs);
-
-
-
-
-
/*************************************************************
*********** Read WCS ***********
*************************************************************/
@@ -149,8 +141,8 @@ wcs_read_correct_pc_cd(struct wcsprm *wcs)
Don't call this function within a thread or use a mutex.
*/
struct wcsprm *
-gal_wcs_read_fitsptr(fitsfile *fptr, size_t hstartwcs, size_t hendwcs,
- int *nwcs)
+gal_wcs_read_fitsptr(fitsfile *fptr, int linearmatrix, size_t hstartwcs,
+ size_t hendwcs, int *nwcs)
{
/* Declaratins: */
int sumcheck;
@@ -361,6 +353,11 @@ gal_wcs_read_fitsptr(fitsfile *fptr, size_t hstartwcs,
size_t hendwcs,
}
}
+ /* If the user wants a CD linear matrix, do the conversion here,
+ otherwise, make sure the PC matrix is used. */
+ if(linearmatrix==GAL_WCS_LINEAR_MATRIX_CD) gal_wcs_to_cd(wcs);
+ else gal_wcs_decompose_pc_cdelt(wcs);
+
/* Clean up and return. */
status=0;
if (fits_free_memory(fullheader, &status) )
@@ -374,8 +371,8 @@ gal_wcs_read_fitsptr(fitsfile *fptr, size_t hstartwcs,
size_t hendwcs,
struct wcsprm *
-gal_wcs_read(char *filename, char *hdu, size_t hstartwcs,
- size_t hendwcs, int *nwcs)
+gal_wcs_read(char *filename, char *hdu, int linearmatrix,
+ size_t hstartwcs, size_t hendwcs, int *nwcs)
{
int status=0;
fitsfile *fptr;
@@ -389,7 +386,8 @@ gal_wcs_read(char *filename, char *hdu, size_t hstartwcs,
fptr=gal_fits_hdu_open_format(filename, hdu, 0);
/* Read the WCS information: */
- wcs=gal_wcs_read_fitsptr(fptr, hstartwcs, hendwcs, nwcs);
+ wcs=gal_wcs_read_fitsptr(fptr, linearmatrix, hstartwcs,
+ hendwcs, nwcs);
/* Close the FITS file and return. */
fits_close_file(fptr, &status);
@@ -403,7 +401,8 @@ gal_wcs_read(char *filename, char *hdu, size_t hstartwcs,)
+ double *pc, char **cunit, char **ctype,
+ size_t ndim, int linearmatrix)
{
size_t i;
int status;
@@ -441,6 +440,10 @@ gal_wcs_create(double *crpix, double *crval, double *cdelt,
error(EXIT_FAILURE, 0, "wcsset error %d: %s", status,
wcs_errmsg[status]);
+ /* If a CD matrix is desired make it. */
+ if(linearmatrix==GAL_WCS_LINEAR_MATRIX_CD)
+ gal_wcs_to_cd(wcs);
+
/* Return the output WCS. */
return wcs;
}
@@ -497,15 +500,21 @@ void
gal_wcs_write_in_fitsptr(fitsfile *fptr, struct wcsprm *wcs)
{
char *wcsstr;
- int tpvdist, status=0, nkeyrec;
-
- /* Prepare the main rotation matrix. Note that for TPV distortion, WCSLIB
- versions 7.3 and before couldn't deal with the CDELT keys, so to be
- safe, in such cases, we'll remove the effect of CDELT in the
- 'gal_wcs_to_cd' function. */
- tpvdist=wcs->lin.disseq && !strcmp(wcs->lin.disseq->dtype[1], "TPV");
- if( tpvdist ) gal_wcs_to_cd(wcs);
- else gal_wcs_decompose_pc_cdelt(wcs);
+ int cdfordist, status=0, nkeyrec;
+
+ /* For the TPV, TNX and ZPX distortions, WCSLIB can't deal with the CDELT
+ keys properly and its better to use the CD matrix instead, so we'll
+ use the 'gal_wcs_to_cd' function. */
+ cdfordist = ( wcs->lin.disseq
+ && ( !strcmp( wcs->lin.disseq->dtype[1], "TPV")
+ || !strcmp(wcs->lin.disseq->dtype[1], "TNX")
+ || !strcmp(wcs->lin.disseq->dtype[1], "ZPX") ) );
+
+ /* Finalize the linear transformation matrix. Note that some programs may
+ have worked on the WCS. So even if 'altlin' is already 2, we'll just
+ ensure that the final matrix is CD here. */
+ if(wcs->altlin==2 || cdfordist) gal_wcs_to_cd(wcs);
+ else gal_wcs_decompose_pc_cdelt(wcs);
/* Clean up small errors in the PC matrix and CDELT values. */
gal_wcs_clean_errors(wcs);
@@ -523,33 +532,33 @@ gal_wcs_write_in_fitsptr(fitsfile *fptr, struct wcsprm
*wcs)
status=0;
/* WCSLIB is going to write PC+CDELT keywords in any case. But when we
- have a TPV distortion, it is cleaner to use a CD matrix. Also,
- including and before version 7.3, WCSLIB wouldn't convert coordinates
- properly if the PC matrix is used with the TPV distortion. So to help
- users with WCSLIB 7.3 or earlier, we need to conver the PC matrix to
- CD. 'gal_wcs_to_cd' function already made sure that CDELT=1, so
- effectively the CD matrix and PC matrix are equivalent, we just need
- to convert the keyword names and delete the CDELT keywords. Note that
- zero-valued PC/CD elements may not be present, so we'll manually set
- 'status' to zero and not let CFITSIO crash.*/
+ have a TPV, TNX or ZPX distortion, it is cleaner to use a CD matrix
+ (WCSLIB can't convert coordinates properly if the PC matrix is used
+ with the TPV distortion). So to help users avoid the potential
+ problems with WCSLIB. 'gal_wcs_to_cd' function already made sure that
+ CDELTi=1.0, so effectively the CD matrix and PC matrix are
+ equivalent, we just need to convert the keyword names and delete the
+ CDELT keywords. Note that zero-valued PC/CD elements may not be
+ present, so we'll manually set 'status' to zero to avoid CFITSIO from
+ crashing. */
if(wcs->altlin==2)
{
+ status=0; fits_delete_str(fptr, "CDELT1", &status);
+ status=0; fits_delete_str(fptr, "CDELT2", &status);
status=0; fits_modify_name(fptr, "PC1_1", "CD1_1", &status);
status=0; fits_modify_name(fptr, "PC1_2", "CD1_2", &status);
status=0; fits_modify_name(fptr, "PC2_1", "CD2_1", &status);
status=0; fits_modify_name(fptr, "PC2_2", "CD2_2", &status);
- status=0; fits_delete_str(fptr, "CDELT1", &status);
- status=0; fits_delete_str(fptr, "CDELT2", &status);
+ if(wcs->naxis==3)
+ {
+ status=0; fits_delete_str(fptr, "CDELT3", &status);
+ status=0; fits_modify_name(fptr, "PC1_3", "CD1_3", &status);
+ status=0; fits_modify_name(fptr, "PC2_3", "CD2_3", &status);
+ status=0; fits_modify_name(fptr, "PC3_1", "CD3_1", &status);
+ status=0; fits_modify_name(fptr, "PC3_2", "CD3_2", &status);
+ status=0; fits_modify_name(fptr, "PC3_3", "CD3_3", &status);
+ }
status=0;
- fits_write_comment(fptr, "The CD matrix is used instead of the "
- "PC+CDELT due to conflicts with TPV distortion "
- "in WCSLIB 7.3 (released on 2020/06/03) and "
- "ealier. By default Gnuastro will write "
- "PC+CDELT matrices because the rotation (PC) and "
- "pixel-scale (CDELT) are separate; providing "
- "more physically relevant metadata for human "
- "readers (PC+CDELT is also the default format "
- "of WCSLIB).", &status);
}
}
@@ -622,6 +631,406 @@ gal_wcs_write(struct wcsprm *wcs, char *filename,
+
+/*************************************************************
+ *********** Coordinate system ***********
+ *************************************************************/
+int
+gal_wcs_coordsys_from_string(char *coordsys)
+{
+ if( !strcmp(coordsys,"eq-j2000") ) return GAL_WCS_COORDSYS_EQJ2000;
+ else if( !strcmp(coordsys,"eq-b1950") ) return GAL_WCS_COORDSYS_EQB1950;
+ else if( !strcmp(coordsys,"ec-j2000") ) return GAL_WCS_COORDSYS_ECJ2000;
+ else if( !strcmp(coordsys,"ec-b1950") ) return GAL_WCS_COORDSYS_ECB1950;
+ else if( !strcmp(coordsys,"galactic") ) return GAL_WCS_COORDSYS_GALACTIC;
+ else if( !strcmp(coordsys,"supergalactic") )
+ return GAL_WCS_COORDSYS_SUPERGALACTIC;
+ else
+ error(EXIT_FAILURE, 0, "WCS coordinate system name '%s' not "
+ "recognized, currently recognized names are 'eq-j2000', "
+ "'eq-b1950', 'galactic' and 'supergalactic'", coordsys/* Identify the coordinate system of the WCS. */
+int
+gal_wcs_coordsys_identify(struct wcsprm *wcs)
+{
+ /* Equatorial (we are keeping the dash ('-') to make sure it is a
+ standard). */
+ if ( !strncmp(wcs->ctype[0], "RA---", 5)
+ && !strncmp(wcs->ctype[1], "DEC--", 5) )
+ {
+ if ( !strncmp(wcs->radesys, "FK4", 3) )
+ return GAL_WCS_COORDSYS_EQB1950;
+ else if ( !strncmp(wcs->radesys, "FK5", 3) )
+ return GAL_WCS_COORDSYS_EQ }
+
+ /* Ecliptic. */
+ else if ( !strncmp(wcs->ctype[0], "ELON-", 5)
+ && !strncmp(wcs->ctype[1], "ELAT-", 5) )
+ if ( !strncmp(wcs->radesys, "FK4", 3) )
+ return GAL_WCS_COORDSYS_ECB1950;
+ else if ( !strncmp(wcs->radesys, "FK5", 3) )
+ return GAL_WCS_COORDSYS_EC
+ /* Galactic. */
+ else if ( !strncmp(wcs->ctype[0], "GLON-", 5)
+ && !strncmp(wcs->ctype[1], "GLAT-", 5) )
+ return GAL_WCS_COORDSYS_GALACTIC;
+
+ /* SuperGalactic. */
+ else if ( !strncmp(wcs->ctype[0], "SLON-", 5)
+ && !strncmp(wcs->ctype[1], "SLAT-", 5) )
+ return GAL_WCS_COORDSYS_SUPERGALACTIC;
+
+ /* Other. */
+ else
+ error(EXIT_FAILURE, 0, "%s: the CTYPE values '%s' and '%s' are "
+ "not yet implemented! Please contact us at %s to "
+ "implement it", __func__, wcs->ctype[0], wcs->ctype[1],
+ PACKAGE_BUGREPORT
+/* Set the pole coordinates (current values taken from the WCSLIB
+ manual.
+ lng2p1: pole of input (1) system in output (2) system's logitude.
+ lat2p1: pole of input (1) system in output (2) system's latitude.
+ lng1p2: pole of output (2) system in input (1) system's longitude.
+
+ Values from NED (inspired by WCSLIB manual's example).
+
+
+ longi (deg) latit (deg) OUTPUT INPUT
+ ----- ----- ------ -----
+ (------------, -----------) B1950 equ. coords. of B1950 equ. pole.
+ (180.31684301, 89.72174782) J2000 equ. coords. of B1950 equ. pole.
+ (90.000000000, 66.55421111) B1950 ecl. coords. of B1950 equ. pole.
+ (90.699521110, 66.56068919) J2000 ecl. coords. of B1950 equ. pole.
+ (123.00000000, 27.40000000) Galactic coords. of B1950 equ. pole.
+ (26.731537070, 15.64407736) Supgalactic coords. of B1950 equ. pole.
+
+ (359.68621044, 89.72178502) B1950 equ. coords. of J2000 equ. pole.
+ (------------, -----------) J2000 equ. coords. of J2000 equ. pole.
+ (89.300755510, 66.55417728) B1950 ecl. coords. of J2000 equ. pole.
+ (90.000000000, 66.56070889) J2000 ecl. coords. of J2000 equ. pole.
+ (122.93200023, 27.12843056) Galactic coords. of J2000 equ. pole.
+ (26.450516650, 15.70886131) Supgalactic coords. of J2000 equ. pole.
+
+ (270.00000000, 66.55421111) B1950 equ. coords. of B1950 ecl. pole.
+ (269.99920697, 66.55421892) J2000 equ. coords. of B1950 ecl. pole.
+ (------------, -----------) B1950 ecl. coords. of B1950 ecl. pole.
+ (267.21656404, 89.99350237) J2000 ecl. coords. of B1950 ecl. pole.
+ (96.376479150, 29.81195400) Galactic coords. of B1950 ecl. pole.
+ (33.378919140, 38.34766498) Supgalactic coords. of B1950 ecl. pole.
+
+ (270.00099211, 66.56069675) B1950 equ. coords. of J2000 ecl. pole.
+ (270.00000000, 66.56070889) J2000 equ. coords. of J2000 ecl. pole.
+ (86.517962160, 89.99350236) B1950 ecl. coords. of J2000 ecl. pole.
+ (------------, -----------) J2000 ecl. coords. of J2000 ecl. pole.
+ (96.383958840, 29.81163604) Galactic coords. of J2000 ecl. pole.
+ (33.376119480, 38.34154959) Supgalactic coords. of J2000 ecl. pole.
+
+ (192.25000000, 27.40000000) B1950 equ. coords. of Galactic pole.
+ (192.85949646, 27.12835323) J2000 equ. coords. of Galactic pole.
+ (179.32094769, 29.81195400) B1950 ecl. coords. of Galactic pole.
+ (180.02317894, 29.81153742) J2000 ecl. coords. of Galactic pole.
+ (------------, -----------) Galactic coords. of Galactic pole.
+ (90.000000000, 6.320000000) Supgalactic coords. of Galactic pole.
+
+ (283.18940711, 15.64407736) B1950 equ. coords. of SupGalactic pole.
+ (283.75420420, 15.70894043) J2000 equ. coords. of SupGalactic pole.
+ (286.26975051, 38.34766498) B1950 ecl. coords. of SupGalactic pole.
+ (286.96654469, 38.34158720) J2000 ecl. coords. of SupGalactic pole.
+ (47.370000000, 6.320000000) Galactic coords. of SupGalactic pole.
+ (------------, -----------) Supgalactic coords. of SupGalactic pole.
+ */
+static void
+wcs_coordsys_insys_pole_in_outsys(int insys, int outsys, double *lng2p1,
+ double *lat2p1, double *lng1p2)
+{
+ switch( insys )
+ {
+ case GAL_WCS_COORDSYS_EQB1950:
+ switch( outsys)
+ {
+ case GAL_WCS_COORDSYS_EQBEQJ2000:
+ *lng2p1=180.31684301; *lat2p1=89.72174782; *lng1p2=359.68621044;
return;
+ case GAL_WCS_COORDSYS_ECB1950:
+ *lng2p1=90.000000000; *lat2p1=66.55421111; *lng1p2=270.00000000;
return;
+ case GAL_WCS_COORDSYS_ECJ2000:
+ *lng2p1=90.699521110; *lat2p1=66.56068919; *lng1p2=270.00099211;
return;
+ case GAL_WCS_COORDSYS_GALACTIC:
+ *lng2p1=123.00000000; *lat2p1=27.40000000; *lng1p2=192.25000000;
return;
+ case GAL_WCS_COORDSYS_SUPERGALACTIC:
+ *lng2p1=26.731537070; *lat2p1=15.64407736; *lng1p2=283.18940711B1950)", __func__,
+ PACKAGE_BUGREPORT, outsys);
+ }
+ break;
+ case GAL_WCS_COORDSYS_EQJ2000:
+ switch( outsys)
+ {
+ case GAL_WCS_COORDSYS_EQB1950:
+ *lng2p1=359.68621044; *lat2p1=89.72178502; *lng1p2=180.31684301;
return;
+ case GAL_WCS_COORDSYS_EQB1950:
+ *lng2p1=89.300755510; *lat2p1=66.55417728; *lng1p2=269.99920697;
return;
+ case GAL_WCS_COORDSYS_ECJ2000:
+ *lng2p1=90.000000000; *lat2p1=66.56070889; *lng1p2=270.00000000;
return;
+ case GAL_WCS_COORDSYS_GALACTIC:
+ *lng2p1=122.93200023; *lat2p1=27.12843056; *lng1p2=192.85949646;
return;
+ case GAL_WCS_COORDSYS_SUPERGALACTIC:
+ *lng2p1=26.450516650; *lat2p1=15.70886131; *lng1p2=283.75420420;
return;
+ default:
+ error(EXIT_FAJ2000)", __func__,
+ PACKAGE_BUGREPORT, outsys);
+ }
+ break;
+ case GAL_WCS_COORDSYS_ECB1950:
+ switch( outsys)
+ {
+ case GAL_WCS_COORDSYS_EQB1950:
+ *lng2p1=270.00000000; *lat2p1=66.55421111; *lng1p2=90.000000000;
return;
+ case GAL_WCS_COORDSYS_EQJ2000:
+ *lng2p1=269.99920697; *lat2p1=66.55421892; *lng1p2=89.300755510;
return;
+ case GAL_WCS_COORDSYS_ECBJ2000:
+ *lng2p1=267.21656404; *lat2p1=89.99350237; *lng1p2=86.517962160179.32094769;
return;
+ case GAL_WCS_COORDSYS_SUPERGALACTIC:
+ *lng2p1=33.378919140; *lat2p1=38.34766498; *lng1p2=286.26975051 ECB1950)", __func__,
+ PACKAGE_BUGREPORT, outsys);
+ }
+ break;
+ case GAL_WCS_COORDSYS_ECJ2000:
+ switch( outsys)
+ {
+ case GAL_WCS_COORDSYS_EQB1950:
+ *lng2p1=270.00099211; *lat2p1=66.56069675; *lng1p2=90.699521110;
return;
+ case GAL_WCS_COORDSYS_EQJ2000:
+ *lng2p1=270.00000000; *lat2p1=66.56070889; *lng1p2=90.000000000;
return;
+ case GAL_WCS_COORDSYS_ECB1950:
+ *lng2p1=86.517962160; *lat2p1=89.99350236; *lng1p2=267.21656404;
return;
+ case GAL_WCS_COORDSYS_EC180.02317894;
return;
+ case GAL_WCS_COORDSYS_SUPERGALACTIC:
+ *lng2p1=33.376119480; *lat2p1=38.34154959; *lng1p2=286.96654469 ECJ2000)", __func__,
+ PACKAGE_BUGREPORT, outsys);
+ }
+ break;
+ case GAL_WCS_COORDSYS_GALACTIC:
+ switch( outsys)
+ {
+ case GAL_WCS_COORDSYS_EQB1950:
+ *lng2p1=192.25000000; *lat2p1=27.40000000; *lng1p2=123.00000000;
return;
+ case GAL_WCS_COORDSYS_EQJ2000:
+ *lng2p1=192.85949646; *lat2p1=27.12835323; *lng1p2=122.93200023;
return;
+ case GAL_WCS_COORDSYS_ECB1950:
+ *lng2p1=179.32094769; *lat2p1=29.81195400; *lng1p2=96.376479150;
return;
+ case GAL_WCS_COORDSYS_ECJ2000:
+ *lng2p1=180.02317894; *lat2p1=29.81153742; *lng1p2=96.383958840;
return;
+ case GAL_WCS_COORDSYS_GALACTIC:
+ *lng2p1=NAN; *lat2p1=NAN; *lng1p2=NAN;
return;
+ case GAL_WCS_COORDSYS_SUPERGALACTIC:
+ *lng2p1=90.000000000; *lat2p1=6.320000000; *lng1p2=47.370000000 GALACTIC)", __func__,
+ PACKAGE_BUGREPORT, outsys);
+ }
+ break;
+ case GAL_WCS_COORDSYS_SUPERGALACTIC:
+ switch( outsys)
+ {
+ case GAL_WCS_COORDSYS_EQB1950:
+ *lng2p1=283.18940711; *lat2p1=15.64407736; *lng1p2=26.731537070;
return;
+ case GAL_WCS_COORDSYS_EQJ2000:
+ *lng2p1=283.75420420; *lat2p1=15.70894043; *lng1p2=26.450516650;
return;
+ case GAL_WCS_COORDSYS_ECB1950:
+ *lng2p1=286.26975051; *lat2p1=38.34766498; *lng1p2=33.378919140;
return;
+ case GAL_WCS_COORDSYS_ECJ2000:
+ *lng2p1=286.96654469; *lat2p1=38.34158720; *lng1p2=33.376119480;
return;
+ case GAL_WCS_COORDSYS_GALACTIC:
+ *lng2p1=47.370000000; *lat2p1=6.320000000; *lng1p2=90.000000000;
return;
+ case GAL_WCS_COORDSYS_SUPERGALACTIC:
+ *lng2p1=NAN; *lat2p1=NAN; *lng1p2=NAN SUPERGALACTIC)",
__func__,
+ PACKAGE_BUGREPORT, outsys);
+ }
+insys'", __func__,
+ PACKAGE_BUGREPORT, insys);
+ }
+
+}
+
+
+
+
+
+static void
+wcs_coordsys_ctypes(int coordsys, char **clng, char **clat, char **radesys)
+{
+ switch( coordsys)
+ {
+ case GAL_WCS_COORDSYS_EQB1950:
+ *clng="RA"; *clat="DEC"; *radesys="FK4"; break;
+ case GAL_WCS_COORDSYS_EQJ2000:
+ *clng="RA"; *clat="DEC"; *radesys="FK5"; break;
+ case GAL_WCS_COORDSYS_ECB1950:
+ *clng="ELON"; *clat="ELAT"; *radesys="FK4"; break;
+ case GAL_WCS_COORDSYS_ECJ2000:
+ *clng="ELON"; *clat="ELAT"; *radesys="FK5"; break;
+ case GAL_WCS_COORDSYS_GALACTIC:
+ *clng="GLON"; *clat="GLAT"; *radesys=NULL; break;
+ case GAL_WCS_COORDSYS_SUPERGALACTIC:
+ *clng="SLON"; *clat="SLAT"; *radesys=NULL;coordsys'", __func__,
+ PACKAGE_BUGREPORT, coordsys);
+ }
+}
+
+
+
+
+/* Convert the coordinate system. */
+struct wcsprm *
+gal_wcs_coordsys_convert(struct wcsprm *wcs, int outcoordsys)
+{
+ int incoordsys;
+ char *alt=NULL; /* Only concerned with primary wcs. */
+ double equinox=0.0f; /* To preserve current value. */
+ struct wcsprm *out=NULL;
+ char *clng, *clat, *radesys;
+ double lng2p1=NAN, lat2p1=NAN, lng1p2=NAN;
+
+
+ /* Just incase the input is a NULL pointer. */
+ if(wcs==NULL) return NULL;
+
+ /* Get the input's coordinate system and see if it should be converted at
+ all or not (if the output coordinate system is different). If its the
+ same, just copy the input and return. */
+ incoordsys=gal_wcs_coordsys_identify(wcs);
+ if(incoordsys==outcoordsys)
+ {
+ out=gal_wcs_copy(wcs);
+ return out;
+ }
+
+ /* Find the necessary pole coordinates. Note that we have already
+ accounted for the fact that the input and output coordinate systems
+ may be the same above, so the NaN outputs will never occur here. */
+ wcs_coordsys_insys_pole_in_outsys(incoordsys, outcoordsys,
+ &lng2p1, &lat2p1, &lng1p2);
+
+ /* Find the necessary CTYPE names of the output. */
+ wcs_coordsys_ctypes(outcoordsys, &clng, &clat, &radesys);
+
+ /* Convert the WCS's coordinate system (if 'wcsccs' is available). */
+#if GAL_CONFIG_HAVE_WCSLIB_WCSCCS
+ out=gal_wcs_copy(wcs);
+ wcsccs(out, lng2p1, lat2p1, lng1p2, clng, clat, radesys, equinox, alt);
+#else
+
+ /* Just to avoid compiler warnings for 'equinox' and 'alt'. */
+ if(alt) lng2p1+=equinox;
+
+ /* Print error message and abort. */
+ error(EXIT_FAILURE, 0, "%s: the 'wcsccs' function isn't available "
+ "in the version of WCSLIB that this Gnuastro was built with "
+ "('wcsccs' was first available in WCSLIB 7.5, released on "
+ "March 2021). Therefore, Gnuastro can't preform the WCS "
+ "coordiante system conversion in the WCS. Please update your "
+ "WCSLIB and re-build Gnuastro with it to use this feature. "
+ "You can follow the instructions here to install the latest "
+ "version of WCSLIB:\n"
+ "
+ "WCSLIB.html\n"
+ "And then re-build Gnuastro as described here:\n"
+ "
+ "html_node/Quick-start.html\n\n",
+ __func__);
+#endif
+
+ /* Return. */
+ return out;
+}
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
+
/*************************************************************
*********** Distortions ***********
*************************************************************/
@@ -1307,7 +1716,7 @@ gal_wcs_decompose_pc_cdelt(struct wcsprm *wcs)
/* Set the WCS structure to use the CD matrix. */
-static void
+void
gal_wcs_to_cd(struct wcsprm *wcs)
{
size_t i, j, naxis;
@@ -1551,10 +1960,9 @@ gal_wcs_pixel_area_arcsec2(struct wcsprm *wcs)
double out;
double *pixscale;
- /* A small sanity check. Later, when higher dimensions are necessary, we
- can find which ones correlate to RA and Dec and use them to find the
- pixel area in arcsec^2. */
- if(wcs->naxis!=2) return NAN;
+ /* Some basic sanity checks. */
+ if(wcs==NULL) return NAN;
+ if(wcs->naxis==1) return NAN;
/* Check if the units of the axis are degrees or not. Currently all FITS
images I have worked with use 'deg' for degrees. If other alternatives
@@ -1589,8 +1997,10 @@ gal_wcs_coverage(char *filename, char *hdu, size_t
*ondim,
size_t i, ndim, *dsize=NULL, numrows;
double *x=NULL, *y=NULL, *z=NULL, *min, *max, *center, *width;
- /* Read the desired WCS. */
- wcs=gal_wcs_read(filename, hdu, 0, 0, &nwcs);
+ /* Read the desired WCS (note that the linear matrix is irrelevant here,
+ we'll just select PC because its the default WCS mode. */
+ wcs=gal_wcs_read(filename, hdu, GAL_WCS_LINEAR_MATRIX_PC,
+ 0, 0, &nwcs);
/* If a WCS doesn't exist, return NULL. */
if(wcs==NULL) return 0;
diff --git a/tests/script/list-by-night.sh b/tests/script/list-by-night.sh
index 4871eeb..3333a8e 100755
--- a/tests/script/list-by-night.sh
+++ b/tests/script/list-by-night.sh
@@ -16,24 +16,24 @@
+
# Preliminaries
# =============
#
# Set the variables (The executable is in the build tree). Do the
# basic checks to see if the executable is made or if the defaults
# file exists (basicchecks.sh is in the source tree).
-#
-# We will be adding noise to two images: the warped (smaller) and unwarped
-# (larger) mock images. The warped one will be used by programs that don't
-# care about the size of the image, but the larger one will be used by
-# those that do: for example SubtractSky and NoiseChisel will be better
-# tested on a larger image.
prog=sort-by-night
dep1=fits
dep2=table
dep1name=../bin/$dep1/ast$dep1
dep2name=../bin/$dep2/ast$dep2
execname=../bin/script/astscript-$prog
+fits1name=clearcanvas.fits
+fits2name=aperturephot.fits
+fits3name=convolve_spatial.fits
+fits4name=convolve_spatial_noised.fits
+fits5name=convolve_spatial_noised_detected.fits
@@ -47,9 +47,16 @@ execname=../bin/script/astscript-$prog
#
# - The executable script was not made.
# - The programs it use weren't made.
+# - The input dataif [ ! -f $dep2name ]; then echo "$dep2name doesn't exist."; exit 77; fi
+if [ ! -f $fits1name ]; then echo "$dep1name doesn't exist."; exit 77; fi
+if [ ! -f $fits2name ]; then echo "$dep1name doesn't exist."; exit 77; fi
+if [ ! -f $fits3name ]; then echo "$dep1name doesn't exist."; exit 77; fi
+if [ ! -f $fits4name ]; then echo "$dep1name doesn't exist."; exit 77; fi
+if [ ! -f $fits5name ]; then echo "$dep1name doesn't exist."; exit 77; fi
+
@@ -74,4 +81,5 @@ ln -sf $dep2name ast$dep2
# Since we want the script to recognize the programs that it will use from
# this same build of Gnuastro, we'll add the current directory to PATH.
export PATH="./:$PATH"
-$check_with_program $execname *.fits
+$check_with_program $execname $fits1name $fits2name $fits3name \
+ $fits4name $fits5name | eng | 5890f5aa-688e-430e-8ae0-b15685d9b3cf | https://lists.nongnu.org/archive/html/gnuastro-commits/2021-04/msg00124.html |
How to enable Hyper-V in Windows 11?
Have you updated to Windows 11 and don't know how to enable Hyper-V? Then this article is exactly what you need to get you through with it. Take a look at the ways to enable Hyper-V in Windows 11 so you can continue to use different operating systems on your device.
Hyper-V is a feature by Windows that allows users to run multiple operating systems on their PC. This is possible with the creation of virtual machines on Windows. If you are a tech enthusiast or a developer, the Hyper-V feature is very helpful and saves a lot of time. You can run versatile operating systems that are based on Linux and are very developer-friendly. Additionally, you can choose to run software that supports an older version of Windows or non-Windows OS. The only limitation is that you can't run programs that require specific GPUs or other hardware. This, in my opinion, does not hinder HyperV's possibilities much. Moreover, it's simple to install and has a lifeline of as long as your PC runs. That's an added advantage over other VMs available. So, how can a user enable the Hyper-V feature on Windows 11? There are two very easy methods you can perform to enable Hyper-V on your system. Take a look at them and use them on your device.
Enabling Hyper-V on Windows 11:
1) Through 'Run' dialog box:
Launch the 'Run' app on your device and type in 'appwix.cpl' in the dialog box. Press enter and you should see a list of all the programs and features provided by Windows on your device. At the left side of the screen, you should see an option called 'Turn Windows features on or off'. Click on it to proceed. In the list in front of you, click on 'Hyper-V' to enable it. You can click on the small + sign beside it to check its components if you are interested in it. After enabling Hyper-V click on 'Okay'. This will start a download which will contain all the required files to execute this feature. When that's done, you will have to restart your computer to finalize all the settings. This was the first and the most common way of enabling Hyper-V on Windows 11.
2) Through System settings:
Go to system settings on your Windows 11 computer and click on 'Apps'. Now, click on 'Optional features' and keep scrolling down until you see an option by the name 'More Windows features'. When you click on it, a list of features will pop up, similar to the first method. Find Hyper-V from this list and enable it. Click OK to finish the process. When you click Ok, some files will be downloaded in order to activate the feature on your device. Restart your computer to enable Hyper-V on Windows 11.
I hope the following article helped you enable the Hyper-V feature on your device. I you wish to read more articles regarding other features associated with Windows, visit ANDROIDGRAM. | eng | d3ea5eea-b2c7-4516-92f9-dc3e8f00193e | https://androidgram.com/how-to-enable-hyper-v-in-windows-11/ |
journey of a local equestrian
By Sara Laughlin JRNM 151
I sat nervously atop my horse waiting for the results of my horsemanship class. Starting at 8 p.m., I completed my first pattern where I was judged on the overall appearance of my horse as he completed the elements. Then, I had to repeat the pattern again once I made the semi-finals, and now here I sit in the final round. It is now 11:30 p.m. and I have not gone back to the barn since the class began. Late nights like these are common at the All-American Quarter Horse Congress, the most prestigious horse show in the nation.
The All American Quarter Horse Congress is a widely known show that houses over 6,000 horses every October in Columbus. The show draws the most competitive contestants from all over the United States and Canada. I have been trying for five years to earn the honorable title of top ten. As I sat atop my horse waiting for the results, I thought back to all of my wins and accomplishments over the course of my career. I thought about how close I have come at this show before; how many finals I have made but have come short of placing. Finally, the results came in and my hard work paid off. I received 8th place out of 200 other contestants. I was a winner.
Although I had lived on a farm my whole life and my mother had shown since she was eight years old, I did not get into showing until I was nine-years-old and willing to put in the hours of practice to compete. I started on my mother's old gelding from when she showed as a young adult. When I was ready, she took me to my very first riding class in Ashland, Ohio at the county fairgrounds. My first class was a disaster. Since my legs weren't quite long enough to reach the horse's belly, he stopped in the middle of the class to chew on the wall. The judge had to pull me away so I could join the rest of the competitors again. That mess-up proved to me just how hard I was going to have to work at riding. I went home and practiced harder and showed more frequently. I was determined to make my horse mind his own business.
After two years of showing my mother's horse, my parents bought me my very own. Stan was a big, bay Quarter Horse and my parents bought him for my birthday. If I could clean his stall, ride him, and take care of him by myself on a daily basis, then I was allowed to show during the summer.
Throughout my show career I have won many titles. I am a two-time Northern Ohio All-Around winner, two-time Performance Horse of the Year and two-time Halter Horse of the Year. I have also been a four-time All American Youth Show Champion, Geauga Horse and Pony Classic Champion and have continually been a representative on the Northern Ohio Congress Youth Team. Words cannot describe the accomplishments I have earned as an equestrian.
One of my favorite memories was taking Stan into a costume showmanship class. The class was sponsored by the Northern Ohio Youth as a fundraiser for the club. I dressed Stan up like a "dunce" who had never shown before; however, everyone at the shows knows Stan and how good he is showmanship and they got a good kick out of the costume. Once when began the pattern, the cone atop of his head, which was held together with fishing twine, fell over his eye and he completed the pattern like a one-eyed pirate. Afterwards, we received a standing ovation. He truly is Mr. Personality.
Riding horses is a team sport unlike any other. In sports such as basketball and football, you can substitute when the game gets tough; you can trade partners when someone isn't pulling their weight. However, in horses, you have one partner. It takes a large amount of teamwork and patience to work together. There are no substitutions in showing; the horse you take out of the trailer is the horse you have to work with that day.
Although I have many winning titles, there is always something to work on when I am at home. To prepare for a show, it takes many hours of practice during the week. I have to make sure my horse can recognize my cues and signals because we have to be in sync with each other's movements. Not only do I have to tune my horse to move correctly and accurately, but I also have to work on your posture and your body placement in the saddle.
There are many different events that I participate in at a daily show. In the mornings I participate in halter, a class judged on the horses' confirmations, and showmanship, a class that judges my horse's abilities to go through obstacles. In the afternoon, I show western pleasure. This class is judged solely on the three natural gaits of the horse: the walk, trot, and canter. Some other classes that can be shown but I do not compete in are jumping, barrel racing, and English events.
Showing horses is a wonderful experience and has had a big impact on my life. I have learned how to communicate with others such as blacksmiths, vets, and horse trainers. I have developed confidence in myself and a strong sense of dedication. I have also learned that you can't win every class, but there is a great sense of accomplishment when you are standing in the winner's circle. | eng | 0acf1ea0-47f6-493e-9afc-caa495428123 | https://collegian.lorainccc.edu/2012/02/15/the-journey-of-a-local-equestrian/ |
This time, Uniparty member Representative Barry Crago (Johnson County) introduced the most expensive amendment in Wyoming Legislative history to my bill with the intent to kill it. According to Representative Crago and the rest of the Uniparty, your health freedom is worth roughly 840 million dollars. I would argue that it's priceless. | eng | ab1b9d18-aed9-494e-94ff-d41d3782f455 | https://www.scwygop.us/post/are-mandates-coming-back-ask-traditional-republicans |
Agricultural Rum
15 Feb Agricultural Rum
Rum is called "agricultural" to differentiate it from so-called "industrial" rum (or traditional, it is made from molasses).
The agricultural term mentions "product of the earth" and this rum is made from sugar cane juice, a plant considered noble.
This is cut from February to May in the French West Indies. As it is fragile, it must be crushed quickly at most 36 hours after cutting.
The juice extracted from the grinding is called vesou and is sweet. After various sieving and filtering processes, it is placed in vats to be fermented for 36 to 48 hours. We obtain an alcoholic wine called "cluster" which is distilled in continuous distillation columns.
Arranged rum is drunk during an aperitif, digestive or currently during a meal as an accompaniment to cheese or a succulent dessert.
White rum, before its marketing, will be titrated between 40 and 62° by adding spring water or demineralised water.
White rum can be consumed young, four months after distillation.
This is cut from February to May in the French West Indies. As it is fragile, it must be crushed quickly at most 36 hours after cutting.
The old rum has aged in oak barrels for a minimum period of three years. It titrates between 40 to 53.1° (for a cask strength).
As for cognac, there is a classification :
Old rum or VSOP
Very old rum or VO: aging for 4 years
Rum out of age or XO: aging for 6 years
Due to humidity and temperature conditions, rum ages 3 times faster in the West Indies than in mainland France.
Agricultural rum is consumed pure, in cocktails but most often in Ti punch (lemon and sugar). It is also the most consumed drink in the French West Indies. | eng | 00b1a4a9-0ca5-442f-a1bc-896aae509269 | https://www.rhum-and-sens.com/agricultural-rum/ |
35 Famous Landmarks in Arizona to Visit
Destguides may receive commissions from purchases made through affiliate links in this article.
Arizona has an array of unique red rock landscapes, like Cathedral Rock in Sedona
If you're reading this article, it's because you might be wondering what Arizona is known for. Arizona is known for its desert landscape and various cultural and historical attractions.
Famous landmarks in Arizona range from world-renowned sites, like Antelope Canyon, to places of cultural interest, like Taliesin West. If you're still wondering what to see in Arizona, read on for 35 of the Grand Canyon State's most incredible attractions!
Organizing a last minute visit to Arizona?
Before traveling to Arizona, book your accommodation and experiences ahead of time.
We've pulled together top suggestions below.
Arizona Landmarks Map
Antelope Canyon
Antelope Canyon is considered sacred by the Navajo and is located in Navajo land near Lake Powell and the city of Page. To enter the area, a guide must accompany you, and they will take you to the best parts of the Upper and Lower Antelope Canyon. Visiting this incredible landmark is hands down one of the best things to do near Page, Arizona!
LANDMARK 2
Arizona Museum of Natural History
The Arizona Museum of Natural History has interactive, informative, and well-organized exhibits for visitors of all ages. The museum focuses on understanding the natural world around us and how we can preserve and record it.
To make admission easier, buy your tickets online ahead of your visit. Also, note that the museum is not open on Mondays.
LANDMARK 3
Arizona Route 89A offers views of the most stunning landscapes, like Schnebly Hill
The Arizona State Museum
The Arizona State Museum has been accumulating and preserving Southwest history since 1893. Notably, it is the oldest anthropological museum in the region.
The museum's collection of pottery and photography comes from ten different groups of indigenous peoples, like the Tohono O'odham and Pascua Yaqui tribes. By viewing the displays here, you can get an inside look at the life of indigenous tribes from the US and Mexico.
LANDMARK 5
Cathedral Rock is a must-visit natural sandstone hill in the Coconino National Forest
Cathedral Rock
Cathedral Rock is part of the beautiful Sedona skyline and is located in the Coconino National Forest in Yavapai County. This natural sandstone hill is one of the most popular photo-op places in the U.S.
Making time to check out the breathtaking view of Cathedral Rock is bound to be one of the most perfect parts of your visit!
LANDMARK 6
Chiricahua National Monument is a great hiking site due to its rare rock formations
Chiricahua National Monument
The Chiricahua National Monument is the product of an enormous volcanic eruption that happened over 27 million years ago.
Covering 12,025 acres, the park features an extensive system of hoodoos and other geological formations. Seeing these rare rock formations is a must, and you can also find several moderate hiking trails surrounding the monument.
LANDMARK 7
CheriAlguire/Depositphotos.com
Colorado River State Historic Park is home to buildings with historical artifacts
Colorado River State Historic Park
The Colorado River State Historic Park was once a military supply point and is now one of many interesting historic sites in Arizona. The park is home to restored historic buildings that display period-correct furnishings and historical artifacts.
You will also be able to see scale models of what the region looked like in its prime and learn how the Colorado River is managed for irrigation.
LANDMARK 8
Copper Queen Mine
One of the more unique famous places in Arizona is Copper Queen Mine. Taking a tour inside this copper mine will allow you to learn about the copper-making process and what life was like during the facility's heyday.
You will also learn about the method used to get to the precious rocks and how each one has to be mined differently. It is an educational and adventure-filled experience you will want to include on your trip.
LANDMARK 9
Douglas Mansion showcases life during the rise and fall of the Jerome mining town
The Douglas Mansion
The Douglas Mansion was previously the home of a mining baron and his family. It is located in Jerome State Historic Park. This Arizona landmark became a museum in 1965 and has been used to preserve and educate visitors on life during the rise and fall of the Jerome mining town.
Inside the house, you will find photographs, artifacts from the era, and a 30-minute informational video presentation. Along with its beautiful views and historical significance, this stop is sure to be entertaining.
LANDMARK 10
Explore unique fort ruins while hiking in the Fort Bowie National Historic Site
Fort Bowie National Historic Site
Fort Bowie is a historical site that was used during the Apache Wars in the 19th-century. The most notable battle here was the Battle of Apache Pass. When visiting, you can hike a 1.5-mile trail to the fort ruins and learn more about the events that took place here.
Glen Canyon Dam Overlook
Tackling the quick 30-minute hike to the Glen Canyon Dam Overlook is well worth it. Once you get to the overlook, you will be able to see across an expansive red rock canyon and the Colorado River. Don't forget to bring your camera to get the perfect pictures of this landmark!
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Glen Canyon National Recreation Area is a stunning spot with views of Lake Powell
Glen Canyon National Recreation Area
Surrounded by Lake Powell, the Glen Canyon National Recreation Area is one of the most beautiful points of interest in Arizona. It is the ideal place to stop for a picnic or spend the day. You can also find hiking trails, lookouts for nature watching, and camping grounds.
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The Grand Canyon is one of the most famous locations in the United States
Grand Canyon National Park
You can stop at the edge of the canyon and take a picture, hike on numerous trails, or even stay at the Grand Canyon Village located on the south rim. The possibilities are endless at this renowned North American landmark!
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Hoover Dam, located on the Arizona-Nevada border, was constructed in the early 1930s
Hoover Dam
Hoover Dam, formerly known as Boulder Dam, is a concrete arch-gravity dam constructed in the early 1930s. It is located on the border between Arizona and Nevada, and you can stand in two states at once when visiting.
The landmark also has a visitor center, where you can learn about flood and slit control, hydroelectric power, and agricultural irrigation.
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Horseshoe Bend is one of the most picturesque sites overlooking the Colorado River
Meteor Crater Natural Landmark
As the first proven meteorite impact site in the Arizona desert, the Meteor Crater Natural Landmark is understandably one of the most famous tourist attractions in Arizona. The collision happened over 50,000 years ago when a piece of an asteroid hit earth at a speed of 26,000 miles per hour.
Located about 37 miles from Flagstaff, the out-of-this-world attraction is excellent for all ages. Stop by the Meteor Crater Discovery Center to learn even more about this fascinating landmark.
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There are 45 rooms in the Montezuma Castle built on a cliff
Montezuma Castle National Monument
The Montezuma Castle National Monument comprises dwellings that date back to 1110 AD. The primary structure to see here is a stone castle with 45 rooms built on a cliff by Southern Sinagua farmers. During your visit, you can get a fantastic view of the castle and learn more about the site's history.
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Old Town Scottsdale is home to boutiques, art galleries, and amazing food spots
Old Town Scottsdale
Stopping by Old Town Scottsdale is a must-do activity when in Scottsdale. Whether you drop by an art gallery, grab a bite to eat, or shop at local boutiques, exploring the area will allow you to enjoy the friendly atmosphere and visit some unique outlets. You can also admire the Arizona-style architecture.
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neilld/Depositphotos.com
The Phoenix Art Museum houses collections of curated works from all around the world
The Phoenix Art Museum
The Phoenix Art Museum is the largest in the Southwestern United States. Its permanent collections include over 20,000 curated works from all around the world.
The museum's exhibitions cover everything from Western American and contemporary art to Latin American art and fashion design. If you are looking for things to do in downtown Phoenix, checking out the Phoenix Art Museum is a must!
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scukrov/Depositphotos.com
Pueblo Grande Museum was opened in 1929 and has three galleries
Pueblo Grande Museum Archaeological Park
The Pueblo Grande Museum Archaeological Park is home to the Pueblo Grande Ruin, one of the best-known national landmarks in Arizona. The park is located on a 1,500-year-old archeological site and is only a few minutes from downtown Phoenix.
The museum has been open since 1929 and is home to three galleries. The first gallery covers the Pueblo Grande Village site and Hohokam culture. The second gallery offers immersive activities for your kids to learn about archeology. Finally, the third gallery is for rotating exhibits on Arizona history, southwest culture, and more!
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marcoscasiano/Depositphotos.com
Taliesin West was the winter home of architect Frank Lloyd Wright
Taliesin West
Taliesin West is a national historic landmark and a UNESCO World Heritage Site. This landmark is notable as it was the winter home of the architect of Frank Lloyd Wright from 1937 to 1959. The house sits in the foothills of the McDowell Mountains in Scottsdale, Arizona, on a Native American archeological site.
During a visit, you can marvel at this iconic piece of architectural design and learn more about the grounds. Interestingly, the ashes of Frank Lloyd Wright and his wife are also buried here.
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Petrified Forest National Park holds the largest concentration of petrified wood
Petrified Forest National Park
Petrified Forest National Park is one of the best National Parks on the West Coast. It is known for the array of rainbow-colored wood that covers the area. Notably, it holds the largest concentration of petrified wood in the world.
The park is located in northeastern Arizona, about 100 miles from Flagstaff. As you explore the attraction, you can admire the sea of colorful petrified wood and take some fun photos. Visiting this unique natural landmark is well worth the drive!
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Monument Valley is famous for its sandstone hills and sensational views
Monument Valley
The breathtaking red-sand desert region of Monument Valley sits on the Arizona-Utah border. Monument Valley, in Navajo County, is known for its large sandstone hills and spectacular sweeping views.
The site is also a popular filming location and is known for being featured in the movie Forrest Gump. While you can get out of the car to take pictures and walk around a little, driving through the valley is recommended.
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The Sonoran Desert has a wide variety of plants and wildlife
Sonoran Desert
Known as the hottest desert in both Mexico and the United States, the Sonoran Desert covers 260,000 square kilometers. The vast body of the desert features several national parks, national monuments, and cities, like Phoenix and Tucson.
It also features various plants and wildlife, such as prickly pears and barrel cacti. Once home to the Hohokam people, it is now commonly used for retirement villages and resorts.
London Bridge
In the west of the state, Lake Havasu City is the home to London Bridge, one of the most charming famous attractions in Arizona. Not to be confused with the iconic bridge in London, United Kingdom, this bridge was purchased in 1964 by Robert P. McCulloch, Sr., for 2.46 million USD.
However, the bridge was shipped from England and rebuilt on Lake Havasu in 1971. A quaint English village replica can also be found next to the bridge.
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Saguaro National Park is home to beautiful hiking trails and camping sites
Saguaro National Park
Composed of two distinct districts, the Rincon Mountain District and the Tucson Mountain District, Saguaro National Park offers more than just your average vast desert views.
The park is notably home to a variety of animals. Some wildlife to spot includes Roadrunners, horned lizards, kangaroo rats, and white-tailed deer. Managed by the National Park Service, the outdoor attraction also has beautiful hiking trails and cozy camping sites.
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San Xavier del Bac Mission was founded in 1692 by Father Eusebio Kino
San Xavier del Bac Mission
The stunning San Xavier del Bac Mission is a National Historic Landmark founded by Father Eusebio Kino in 1692. The church is the oldest intact European structure in the state, making it one of Arizona's most famous places to visit.
When exploring the church's interior, you will discover original 18th-century statues and beautiful mural paintings.
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njene/Depositphotos.com
Sunset Crater was formed after an eruption in about 1085
Sunset Crater Volcano National Monument
After a volcano erupted around 1085, a mark was left north of Flagstaff, which is today the Sunset Crater Volcano National Monument site.
The crater is believed to also be the source of the Bonito and Kana-a lava flows, traces of which you can see to this day. If in the area, stop by this geological site to witness how nature bounces back after a volcanic eruption.
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Tuzigoot National Monument has 110 rooms and was built on top of a hill in 1100 AD
Vermilion Cliffs National Monument
With its impressive, towering red cliffs, it's no wonder this site is considered a US national monument! At Vermilion Cliffs National Monument, you will find some of the most beautiful hiking trails and views in the world.
There are several different landscapes to explore in the park, including Paria Plateau, Vermilion Cliffs, Coyote Buttes, and Paria Canyon.
Yuma Territorial Prison State Historic Park
This former prison, located in Yuma, Arizona, was open for 33 years and now serves as a living museum of the Old West. Yuma Territorial Prison housed many prisoners, including polygamists and murderers, and served as inspiration for Hollywood movies like "3:10 to Yuma."
Exploring the prison will allow you to learn more about its history, and you can see artifacts and photographs in an on-site museum.
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Learn about the Hubbell family at the historic Hubbell Trading Post
Hubbell Trading Post National Historic Site
The Hubbell Trading Post is the oldest operating trading post in the Navajo Nation. This attraction is notable as it shows the contrast between the two cultures that used the site; the new settlers and the Navajo.
When in the area, you will be able to visit the on-site museum and learn about the Hubbell family through family archives, furnished buildings, and business records.
Lowell Observatory
Established in 1894, this astronomical observatory is one of the oldest in the United States. The Lowell Observatory is open for both daytime and evening tours. You can use their telescope (weather permitting), enjoy exhibits and science talks, and get a souvenir at the Starry Skies Shop.
In Summary
As you can see, there are a variety of fascinating Arizona attractions and landmarks to visit. Places to see range from natural landmarks to locations of cultural and historical significance.
When visiting the Grand Canyon State, including a visit to a least a few of these sites on your to-do list is a must!
AlexisKuriFORMER WRITER
Alexis is an avid traveler who loves meeting new people, experiencing different cultures, learning new things, and then writing all about it and sharing it with the world. "Life begins at the end of your comfort zone!" | eng | 14f84fbc-4082-4610-896c-03ff50cc0d2e | https://www.destguides.com/united-states/arizona/landmarks-arizona |
When Stride Treglown met Finisterre: "Imagine waste as a resource"
September 29, 2021 Tanne Spielman
What can an architecture practice and an outdoors clothing brand learn from each other? Quite a bit, it turns out…
On the wild north coast of Cornwall near the village of St Agnes, perched high up on the clifftop, is Wheal Kitty Workshops. This is home to Finisterre, the outdoors clothing company that designs functional sustainable kit for anyone who shares a love for the sea.
It's here on a stormy day that Rob Nunn, a Part 2 Architectural Assistant and Stride Treglown's Sustainability Champion from the Truro office meets Adele Gingell, Positive Impact Manager for Finisterre. Both dressed in long raincoats, they step inside to talk.
Their conversation is part of a series of discussions and events hosted by Stride Treglown's regional offices in their Climate Action Relay, an eight-week programme to drive knowledge exchange, best practice and positive action on the climate emergency.
Adele and Rob in their roles have a shared passion for making a difference in their respective industries, and are keen to learn from each other's experience as Stride and Finisterre are both B Corps.
Companies that are certified B Corporations (B Corps) are dedicated to balancing purpose and profit. This requires them to carefully consider every aspect of what they do, how this influences the people they engage with at all levels, and how their work impacts the environment.
What comes through almost immediately from Rob and Adele is how B Corps have different strengths and can gain valuable insights from others to improve their practice.
Finisterre has always been pioneering in their approach to the circular economy, focused on repairing, recycling and reinventing their products to be more environmentally friendly. As Adele puts it, "Imagine waste as a resource."
They recently developed a new wind-proof and water repellent bio smock that won an international ISPO award. It's filled with wool from sustainable farming and is biodegradable at land and in the sea.
Other popular clothing designs are always reworked each year to ensure they are as durable and comfortable as possible, continually improved based on consumer feedback.
They use sustainable materials in their shops, from recycled furniture to decorations sourced outdoors, such as stones and twigs. Finisterre also recently launched their take back approach where customers get store credit for donating back old clothes.
Adele:"We want to make the product last as long as it can for your lifetime and then when it can't be used anymore, can someone else use it, can it be repaired? What happens to the materials? Can the fabrics be reused?"
"At the end of the day, we are having an impact because we are creating clothing and materials is our biggest impact in terms of carbon footprint."
Rob:"That's interesting as it's something we're also considering in the architecture industry. We often try to reuse a building or reshape it to improve the efficiencies. You can also sometimes reuse it by grinding up and using the rubble as hardcore and do that process on site."
"One of our big challenges is materials too, definitely in the building industry, but also how much control we have over what we put into our specifications."
Adele:"Do you have clients that come to you or vice versa with that desire to only potentially source these kinds of products, like blue sky thinking?"
Rob: "Yes we do but we also see it as an architect's aim to always add extra value to an idea or project. You can show clients by using better processes, the impact it has had. It doesn't always add monetary value, but in terms of the longevity of the product or the end user lifecycle analysis, they will benefit from that. In terms of extra investment, some of the most innovative solutions can come from a low budget."
Rob wants to close the loop more tightly around the circular economy and speaking to Adele has made him further consider the impact of the wider industry and supply chain, learning from Finisterre's approach.
Meanwhile, another aspect of the B Corp framework, Adele talks about how she sees Stride Treglown's strength in investing in its people, being an employee-owned company with clear processes and principles around this.
She also values the transparency of Stride's website and resources, something that fits with her ethos around B Corps.
Adele:"In any industry there's always going to be an element of competition, it's what keeps us on our toes. But people are starting to realise, we're going to achieve a greater goal by sharing."
Rob: "It's the same for our industry. We're moving from a transactional culture of delivering a product or service to having a culture of cooperation and knowledge sharing."
Adele:"Yes, that learning from others is so important. Open sourcing is becoming so much more of a thing. We have spent the last year developing and improving our HR policies, finding great examples shared by larger B Corps has been invaluable to us. Your website is an example of this."
The B Corp community can be seen as a hive mind, something to tap into when needed.
In considering how to make small changes to help combat the climate emergency, tangible actions in the office environment can be surprisingly impactful.
Adele:"I met a B Corp that will take your waste electrical equipment and repurpose it. If the wires can't be used, they get recycled responsibly, but anything that can be repurposed, they will sell at a low cost to community groups, schools, or people that need tech."
"You wouldn't normally think of these things day to day. But if you're always focused on making products sustainable and environmental, you consider what are the small wins? Who is our energy provider in Finisterre stores? Could we recycle more?"
Rob:"Yeah, it's totally about the marginal gains, too. This year Stride Treglown became carbon neutral in our operation, which has been achieved by years of reduction measures and offsetting through responsible reforestation in Scotland. But it's also massively impacted by the drop in business travel and thinking about little things like, do I need to make a phone call? Do I need to send that email? You're using energy for that."
Rob says that he will continue learning from other B Corps, building on what he already does at Stride Treglown. Following on from the Truro office's recent beach clean, he intends to continue doing beach clean events with Ward William Associates, another B Corp.
Across the South West, he aims to invite B Corps from differing disciplines to come together and learn from each other in an informal setting, feeding back his learnings to the wider company through the company's internal sustainability group.
Adele has come to understand the value of community in this way, connecting with others regionally on topics such as the circular economy. Her role is an innovative one, shaped by the B Corp framework, with continual room for growth.
"With every question you answer, you start asking another one. How could we be doing even more to become sustainable? It's exciting to see where it will take me."
As a voluntary Sustainability Champion, Rob sees this as a personal project shaping his work.
"It's important to me to make very small changes and be more particular about where things come from, not just interiors, but the materials that make the spaces."
"A pilot project I was working on recently, is a zero-carbon school. The cycle hubs have got solar panels and the width of the corridors are optimised to reduce environmental impact. It's not just token stuff, it's influenced so many design decisions. Ultimately, the building will form part of the wider vision of community housing. The energy generated here will be put back into the surrounding community."
"Many architects and builders are going the extra step to find something that works better for them, rather than accepting industry standards. By combining working methods, we can actually achieve something."
A key insight from delving into the B Corps framework that both have found is the interconnected relationship between people and product. Only by looking at staff, the wider community and the supply chain can you fully enact sustainability.
It's inspiring how Rob and Adele are both driven to make the people they work with flourish and protect the local landscapes all around them, including the vast sea, just a walk away from where they meet.
Crucially, they are both always open to learning and adapting their ways of working. As Adele points out about the approach at Finisterre,
"We don't claim to be perfect. We're still always on a journey and pull us up on it if you think we're not doing something right, say that because we'll explore it like we should, we all need to be doing that."
Whether structuring a building or designing a coat, it's important to rethink how it's sourced, developed and embedded in its surroundings for a life cycle. Individuals like Rob and Adele are leading the way, with these new ways of thinking.
It takes just one action at a time from us all to reverse the incoming tide of climate change, and there's always more to be done, no matter the industry, to make a difference | eng | 55fb262c-f05a-4a56-8e5f-6768a0371cbf | https://climateactionrelay.com/when-stride-treglown-met-finisterre-imagine-waste-as-a-resource/ |
Below is information and knowledge on the topic how often should a yorkie be groomed gather and compiled by the baonangluong.info team. Along with other related topics like: .
How Often Should I Groom My Yorkie?
When we talk about grooming Yorkies, the focus is mostly on their hair. And that's for a reason, they have long, silky hair, and if well cared for, it's very shiny too.
While
Yorkie Hair Grooming
Haircuts
Generally, dogs with silky hair like Yorkies should have haircuts every 6-8 weeks.
However, nothing awful will happen to your dog if they don't get a haircut; it just means you need to put more effort into brushing their hair. Some people want to grow out their Yorkie's hair and that's fine.
You may also need to give your Yorkie a trim before their major grooming day.
The first thing you want to do is clear the hair near your Yorkie's eyes and then trim the long hairs near the ears. Other areas that need trimming are areas around their nails and their anus. The latter is especially crucial as the hairs can trap bacteria and feces.
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Brushing
It's advisable to brush your dog's hair every day.
Although Yorkies are hypoallergenic, it doesn't mean that they don't shed completely. They just shed much less than other dog breeds.
Additionally, brushing your Yorkie's hair gives you time to bond with them as they see it as a form of love.
Bathing
Depending on their activities, you can bathe your Yorkie every 2-4 weeks. Puppies will probably need more baths than adult dogs because they're very busy and messy.
However, if you take your Yorkie out for walks every day and you need to bathe them daily, consider other ways to clean them, like dog wipes to avoid daily baths.
The dog wipes leave your Yorkie clean and allow them to maintain the natural body oils that they can lose from daily baths. Bathing too often can give your Yorkie a dull, dry, and brittle coat.
Yorkie Nail Care
A Yorkie's nails should be trimmed at least every two to three weeks. You can do this at home, but you'll need your vet's help for the first few times.
I know the reason why you probably trim your dog's nails is to stop them from hurting you or your kids when playing, but there are other benefits of trimming your dog's nails.
Domesticated dogs need frequent nail trimming because their nails don't get worn out. When your Yorkie's nails grow too long, they can splinter, chip, or break, which can be very painful for them. Long nails can also make moving or standing painful for your Yorkie ( in extreme situations). And it can cause their toes and feet to become deformed in extreme cases too.
To make nail cutting easy, invest in a reliable tool like Casfuy electric pet nail clipper. It's safe and comfortable for both you and your Yorkie, and if you have bigger dogs, you can use it on them too, as it comes with small, medium, and large settings. You also get to choose the speed based on your dog's nail hardness.
Yorkie's Teeth
Morkie Puppy Getting His Teeth Brushed
Like you, your Yorkie needs to have their teeth brushed every day. However, this is a bit unrealistic for people who have a busy schedule. If you fall in this last group, try to brush your dog's teeth at least twice a week.
I recommend using a finger brush as it allows you to reach all of your Yorkie's teeth, and the bristles are smooth to protect their gum.
Besides the regular brushing, remember to take your dog to your vet every 6-12 months to have their teeth checked.
Yorkie's Ear and Eye Care
I recommend cleaning your Yorkie's ears at least once a month and weekly if they swim a lot.
Ear cleaning can be very stressful for your Yorkie, so it's important that you're very gentle when doing it. One way to make the process easier is by cutting the long hairs near the ear canal and buying the right cleaning products. Only clean your Yorkie's ears when they're calm, and give them treats in the process for positive reinforcement.
Similarly, clean your Yorkie's eyes every month. I would have to write a whole blog on how to clean your dog's eyes. However, one great tip is to use these tear stain wipes every day to remove tear stains, secretions, and dried mucus. The wipe also helps in reducing any itchiness and irritation in your Yorkie's eyes.
Other Factors that Influence Yorkie Grooming Frequency
Now that you know how often you should groom your Yorkie, it's time to talk about the instances when the frequency can change.
Allergies
Depending on what allergies your Yorkie has, they may require more or less grooming.
Talk to your vet to know the frequency of your Yorkie's grooming and the right products to avoid worsening the allergies.
Environment
If your Yorkie is outside a lot, they will require more grooming because they are exposed to parasites, dirt, and bugs. You can get away with infrequent grooming sessions for dogs who stay mostly indoors.
Budget
Grooming can be expensive, especially if you take your dog to a pet groomer. In this case, you can talk to your vet and discuss the minimum number of appointments you can have annually.
Alternatively, you can learn how to groom your Yorkie at home. It may seem hard at first, but you can do it with the right tutorials and tools.
How Often Should You Groom a Yorkie? (Final Words)
To maintain your Yorkie's health and beautiful looks, it's important to keep up with their grooming schedule. Whether it's ear cleaning or haircuts try to follow through as much as you can.
Yorkie grooming may seem expensive and time-consuming, but it saves you a lot of time and money in the long run. For example, not brushing your Yorkie's teeth may lead to dental issues that may require full-mouth tooth removal; not only is this expensive, but it also complicates your dog's life.
I hope you can now prepare your Yorkie's grooming schedule. And if you're looking for a groomer, be sure to check our blog post on how to find a good dog groomer.
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Extra Information About how often should a yorkie be groomed That You May Find Interested
If the information we provide above is not enough, you may find more below here.
How Often Should I Groom My Yorkie?
Author: yorkieuniverse.com
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Sumary: Yorkies are one of the cutest dog breeds. They may be small, but they have a lot of hair! This article will teach you how often you should groom your Yorkie so they look their best.
Matching Result: Generally, dogs with silky hair like Yorkies should have haircuts every 6-8 weeks. However, nothing awful will happen to your dog if they don't get a haircut; …
Intro: How Often Should I Groom My Yorkie? When we talk about grooming Yorkies, the focus is mostly on their hair. And that's for a reason, they have long, silky hair, and if well cared for, it's very shiny too. While Yorkie Hair Grooming Haircuts Generally, dogs with silky hair like Yorkies should have haircuts every 6-8 weeks. However, nothing awful will happen to…
Matching Result: So, how often should you give a Yorkshire Terrier a bath? Keeping the above in mind, the perfect timing for most Yorkies is once every 3 weeks unless there …
Intro: Yorkie Grooming | Yorkshire Terrier Information Center Overview Proper grooming to keep your Yorkie looking nice and remain healthy will include:BathsBrushing and combingNail Care (and possible dewclaw removal)TrimmingCreating Top Knots (if the hairs on the forehead are kept long) Baths Things start off with with proper bathing techniques. Timing of baths is crucial for effective grooming with pleasing results. If you give too many baths, the following will happen:1) Even if you are using the best shampoos and other products, the nature of shampoo is to cleanse and too much of this will strip away oils too frequently, causing the skin…
How Often Should A Yorkie Be Groomed? (More Than You …
Sumary: Without regular grooming, Yorkies can succumb to a number of diseases. How often should a Yorkie be groomed? At the very least, you need to give your pup…
Matching Result: Yorkies need regular grooming. You need to brush your pet's coat at least two to three times a week, and ideally every day. You should also brush your Yorkie …
Intro: How Often Should A Yorkie Be Groomed? (More Than You Think)Yorkies have a unique coat in the canine world.Their hair is more like human hair than other dogs. This gorgeous, silky coat is their most distinctive feature. It helps them stand out and it is a big reason Yorkshire terriers are one of the most popular dog breeds worldwide. But just like gorgeous human hair, gorgeous Yorkie hair needs regular grooming. And it's not just the hair. There are other grooming tasks you need to stay on top of. Keep reading to learn how often a Yorkie should be groomed…
How Often Do You Give Yorkies a Haircut? – Pets – The Nest
Sumary: A Yorkie's fine, silky hair grows quickly and should be trimmed about once a month. If you trim the face and ears at home, you may be able to trim the body every six to eight weeks….
Matching Result: A Yorkie will need her body trimmed every four to six weeks once she is full grown. In between grooming appointments, trim the hair under her tail around the …
Intro: How Often Do You Give Yorkies a Haircut? i Brand X Pictures/Brand X Pictures/Getty Images A Yorkie's fine, silky hair grows quickly and should be trimmed about once a month. If you trim the face and ears at home, you may be able to trim the body every six to eight weeks. Daily grooming is required to avoid mats and knots, however. The Puppy CutA Yorkie puppy's hair grows a bit slower than an adult's. Your Yorkie will need her first haircut around 4 months of age. Her face, mouth and ears may need trimming sooner to keep her ears…
How Often to Bathe A Yorkie? – Yorkie Grooming Tips 2019
Sumary: Get the best Yorkie grooming and bathing tips here at Yorkie Advice. We show you how and how many times to bath your Yorkshire Terrier and when to cut their hair!
Matching Result: As a general rule, you should bathe your Yorkie around every 2-3 weeks. It's okay to bathe your Yorkie weekly but this usually isn't necessary. Yorkies with …
Intro: Yorkie Grooming How to Groom A Yorkie If you wanted a dog that doesn't require much grooming and care, you picked the wrong dog with the Yorkie! Yorkshire Terriers are considered high-maintenance in terms of grooming, especially Yorkies with a long coat. Still, grooming your Yorkie and helping him look his best can be a fun and rewarding experience. If neglected, however, it can leave your pup with painful knots and tangles and pull at his delicate skin. It can also lead to hygiene issues. Here's a comprehensive look at everything you need to know about Yorkie grooming from how…
Yorkie Grooming – How to Care for Your Yorkshire Terrier's Coat
Sumary: A right of passage for every new Yorkshire Terrier owner is getting to grips with Yorkie grooming. And here is how to do it!
Matching Result: There are three basic steps to grooming a Yorkie, and you won't do all of them every day. Brushing will be something that needs to be done at …
Intro: Yorkie Grooming – How to Care for Your Yorkshire Terrier's CoatYou are here: Home / Puppy Health & Care / Yorkie Grooming – How to Care for Your Yorkshire Terrier's Coat A right of passage for every new Yorkshire Terrier owner is getting to grips with Yorkie grooming. Today we share lots of practical advice and tips to make it as easy and fun as possible! Yorkies may be pint-sized in body, but they are outsized in personality. Because Yorkies are so small and cute, they are always in the running for "dog most likely to be dressed up for…
How Often Do Yorkies Get Groomed? (Solved & Explained!)
Sumary: Yorkies should be professionally groomed (or at least groomed at home) every 4 to 6 weeks. This should include a brushing, a bath, a haircut, and a trimming
Matching Result: Yorkies should be professionally groomed (or at least groomed at home) every 4 to 6 weeks. This should include a brushing, a bath, a haircut, …
Intro: How Often Do Yorkies Get Groomed? (Solved & Explained!) – [2022] – 2022 Yorkies should be professionally groomed (or at least groomed at home) every 4 to 6 weeks. This should include a brushing, a bath, a haircut, and a trimming of their nails. This will keep them nice and clean, preventing matting and tangling of the fur, as well as ensuring they aren't getting their claws caught in everything! Trimming those nails is also good for long-term health, as when they are left unchecked the imbalance of the digits on their paws can contribute to arthritis in the toes….
how often do you take your yorkie for grooming?
Sumary: is once a week or twice a month better?? i do notice that after 4 days agapi starts smelling.. er… a little strong
Matching Result: yeah, they do get pretty stinky. It's because their hair is like human hair, not because it can be long. It gets kind of oily and the sweat from going outside …
Intro: how often do you take your yorkie for grooming? – YorkieTalk.com Forums 06-09-2006, 05:37 AM #7 KellyV YT 500 Club Member Join Date: Nov 2005 Location: Wisconsin Posts: 776 First and last time Pixie will ever go to a groomer was last December… The groomer totally did not do what I want and I'm afraid another one will do the same thing…. So I do it all myself! I bathe her once a week and do other things as needed – pull ear hair, sanitary trim, trim nails & pad hair, etc. She was a handfull at first,…
Frequently Asked Questions About how often should a yorkie be groomed
If you have questions that need to be answered about the topic how often should a yorkie be groomed, then this section may help you solve it.
Which haircut suits a Yorkie the best?
The most common length for Yorkies is the short (puppy cut), which is great for active dogs and keeps a dog looking neat and tidy. It only requires brushing two to three times per week and works particularly well with a leave-in product to repel dirt and debris.
How frequently should you bathe a Yorkie?
If your puppy is particularly mischievous or has a longer Yorkie haircut, you might find that additional baths are necessary. You should bathe your Yorkie once every two to four weeks.
How frequently should a Yorkie be brushed?
Brushing and Combing Trying to remove matted hair can take hours and can be very stressful for both owner and dog. Therefore, it is highly recommended to brush and comb your Yorkie 1 time per day if the dog has a long "show coat" and every 2 days if the dog has a shorter "puppy dog cut".
What occurs if a yorkie is not groomed?
However, nothing terrible will happen to your dog if they don't get a haircut; it just means you need to put more effort into brushing their hair. Some people want to let their Yorkie's hair grow out, and that's fine. In general, dogs with silky hair like Yorkies should get haircuts every 6-8 weeks.
How old are Yorkies on average?
The Teddy Bear Cut keeps the body fluffy and full while framing your Yorkie's face to make her look like a teddy bear.
Do Yorkies form attachments to specific people?
Yorkshire Terriers are a very adaptable breed that will be content in a wide range of households: single owners, small families, and large families. The short answer is no, not typically, but there are always exceptions.
How many meals should a Yorkie have each day?
Your dog may need more or less than the amount listed on the dog food label; in general, a Yorkshire Terrier eats 14 to 12 cup per day. Puppies need 3 to 4 meals per day, and an adult dog needs to eat twice per day.
How should a Yorkie's face be washed?
2) For all Yorkies, clean the face once daily or up to three times daily (after each meal) with a facial wipe. An excellent option for this is Earthbath Facial Wipes; they are fragrance-free, mild yet effective, and come in a convenient 25-count package.
How long does a Yorkie typically live?
Female Yorkshire Terriers typically live 1.5 years longer than males, with a life expectancy of 13 to 16 years and a median age of 14.5 years.
Do Yorkies enjoy sharing your bed?
It doesn't take a Yorkie long to figure out that their human's bed is the most cozy place to sleep and that they also feel safe when sleeping next to their owner.
What causes Yorkies to pass away most frequently?
The majority of heart disease in dogs is brought on by the weakening or slow deformity of heart valves, which causes them to no longer tightly close; blood then leaks back around these weak valves, straining the heart. Heart failure is a leading cause of death in Yorkshire Terriers in their golden years.
How old must a Yorkie be to be considered senior?
The Senior. Although there isn't a set rule or official age at which a Yorkie is deemed a senior, for toy breed dogs, the threshold is typically between 8 and 10 years old.
How long do Yorkies typically live?
Female Yorkshire Terriers live an average of 1.5 years longer than males, and the Yorkie, at 12.5 years old, is slightly older than the average dog in the United States. Your Yorkie's life expectancy ranges from 12 to 15 years, with 13.5 being the median. | eng | c5bafbd3-76ea-4881-9b6b-7e45269e93b0 | https://baonangluong.info/top-10-how-often-should-a-yorkie-be-groomed-you-need-to-know/ |
In Scotland, PA, revenge is a dish best served with fries. This deliciously dark new musical comedy, based on the cult film (and the bard's Macbeth), springs to life in a sleepy Pennsylvania town (population 1,203-and dropping), where a burger-joint manager (Ryan McCartan) and his wife (Taylor Iman Jones) cook up a plan to super-size their lives. As their ambitions grow and the bodies fall, the couple finds out just how far they'll go for a taste of the oh-so-tempting American dream | eng | 01765ba0-48c1-4050-bc62-71b088819b41 | https://www.broadwayworld.com/article/BWW-TV-Watch-Highlights-of-Ryan-McCartan-Taylor-Iman-Jones-More-in-SCOTLAND-PA-20191021 |
Curious State
Could we have domesticated a T-Rex? Is the mafia really that violent? Haven't all the possible songs been written by now? Unexpected gems of knowledge are hidden all around us. Let's dig them up, one offbeat question at a time.
Episodes
I come to you one last time to say goodbye. And to thank you for joining me on this journey of being curious for its own sake, of saddling a hunch and seeing where its long stride takes us. I think curiosity takes different forms throughout our lives. Wherever you are in your journey, it's been an honor to be a part of it.
In 2021, the top three classical musicians on Spotify—Bach, Beethoven, and Mozart—were streamed 19.2 million times a month in 2021, which together would have earned them over $852,000. How is it that songs hundreds of years old are still being listened to? What is it about classical music that makes it so timeless?
Benjamin Zander, conductor of the Boston Philharmonic, shares his passion for the love that classical music generates.
Matt McGinley entered the music industry over 15 years ago as the drummer for the band Gym Class Heroes. Nowadays, Matt's a contributing music producer for hit radio shows and podcasts, like This American Life, Serial, Nice White Parents, and S Town. Suffice it to say, he produces a lot of music. And it's all part of an ever-growing global library. By Google's count, between 97 and 230 million songs exist worldwide. It makes you wo...
Easy money is hard to come by. Unless you're in the ransomware business. Then tens of millions of dollars can be yours in a single, unsuspecting click. Quick cash grabs fuel a worldwide economy, funneling extorted funds into secret bank accounts, hackers' salaries, and even government pockets.
In a world where your data is the gateway to a thief's payday, all is not lost.
Back in the day, Princeton eating clubs were all the rage. It's where you tapped into the pulse of the Princeton experience. Allegiances were sworn. Bread was broken. Bonds were forged with fellow members, some of whom would become crucial connections in the post-college world.
The bicker of 1958 is a tale of a time gone by, but also a reminder of the continued struggle with anti-semitism and exclusion.
The music of Stranger Things haunts living rooms across the globe, and at times steals the show. It takes a professional touch to properly integrate music to serve the goal of a scene, and of a moment. Be it for signaling tension, to call back to a previous season, to ratchet up the thrills, or to bring comic relief.
Creating the right music offers the opportunity to elevate a scene. But getting the timing just right is what makes i...
Howard Berger started working in the movie industry at the young age of 13. Today, he has over 100 films to his credit as a professional makeup artist. He's worked on movies like The Chronicles of Narnia: The Lion, The Witch, and the Wardrobe, From Dusk Till Dawn, and the blood-filled Kill Bill movies. But things on set don't always go as planned.
Click here to learn more about Howard and purchase his new book, Masters of Make-Up Ef...
Growing up in rural Ohio, Michelle Belanger had to hide her unique abilities from classmates. Her grandmother worried that if she showed off too much, government men would take her away for testing. Luckily, that never happened. Instead, Michelle went on a journey of self-discovery and created the de facto code of ethics for the international vampire community.
Leonard Pickel's Hauntrepreneurs has designed over 300 original haunted attractions, including ones for Madison Square Garden, Universal Studios Florida, several Six Flags Amusement Parks, and the Kandy Halloween Party at the Playboy Mansion.
But what goes into designing a haunted house?
Leonard takes us through the spooky business of manipulating architecture, impossible floor plans, why you should always "scare forward," and the ki...
Ashrita Furman broke the world record for underwater hoola-hooping in Florida, where a pod of dolphins watched from afar—in what I presume was utter confusion.
I've been in the presence of some pretty fascinating people. The voice of Porky Pig, a haunted house architect, a scientist who's close to bringing back a T-Rex (albeit in a less menacing, chicken-sized form). But Ashrita Furman is in a league of his own. He has world records...
Take the Jonestown murder-suicide, for example—where cult leader Jim Jones called for over 900 of his followers to drink cyanide-laced punch. Cyanide also sits centerstage with a popular spy movie trope: the cyanide tooth. In case of capture, pop out the fake tooth that's actually made of cyanide. Swallow it. And boom, a quick death is on its way.
Jackson Galaxy is America's Cat Daddy. He's the host of Animal Planet's hit show, My Cat From Hell, he's amassed over 100 million views on his YouTube channel, and he has his own toy line—when it comes to cats, Jackson knows best.
So, Jackson…is it true? Are cats assholes? Or is there more to those furry enigmas than meets the eye?
Only 80 known cases of highly superior autobiographical memory (HSAM) exist. What's it like to remember almost everything that's ever happened to you? Rebecca Sharrock shares her experience—and how her dreams revealed an incredible feature of HSAM. | eng | bf7ec032-0b09-465c-82e4-1c86430fc550 | https://www.iheart.com/podcast/269-curious-state-93866064/ |
Job description
Working autonomously with a high level of self-motivation and engaging stakeholders effectively
Providing timely and accurate updates to stakeholders
Must be an Australian citizen with a minimum Baseline
What's on offer:
Opportunity to work with broad range of clients
Permanent Opportunity
Location: ACT only
Competitive salary package
If this sounds like you, please don't hesitate to reach out.
Looking forward to hearing from you!
Paxus Job number: 263656 | eng | c323d026-1d3e-42c9-8ed9-33403cd55aa9 | https://www.paxus.com.au/job/project-manger |
The Ethics of Science: Navigating the Controversial Issues Surrounding Scientific Research
Science has brought us incredible advancements and has helped us understand the world around us in ways we never thought possible. However, with great power comes great responsibility, and the ethics of science are something that scientists must navigate carefully. In order to continue making progress, ethical considerations must be taken into account to ensure that scientific research benefits society without causing harm. Here, we explore the depths of science's moral compass and embark on a journey of ethical decision making in science.
Discovering the Depths of Science's Moral Compass
Science has always been about discovering the truth, but what happens when the truth conflicts with ethics? In recent years, there have been many controversial issues surrounding scientific research, such as animal testing, human cloning, and genetic engineering. These issues have led scientists to question their own moral compass and the impact their research may have on society.
Take animal testing, for example. While it has contributed to some important medical breakthroughs, many people argue that it is unethical to use animals for this purpose. Scientists must weigh the benefits of their research against the suffering of animals and make a decision based on their own morals and values.
Another issue that has caused controversy in the scientific community is human cloning. While it could potentially save lives by allowing for the creation of organs for transplants, it also raises many ethical questions about the value of human life and the potential for abuse.
These are just a few examples of the complex ethical issues that scientists face. It is important for scientists to recognize the impact their research may have on society and to navigate these issues with care.
Embarking on a Journey of Ethical Decision Making in Science
As scientists navigate the complex ethical issues surrounding scientific research, it is important that they embark on a journey of ethical decision making. This means taking a step back and considering the potential consequences of their research, both positive and negative.
The first step in ethical decision making is to recognize that there is an ethical issue at hand. Scientists must be aware of the potential consequences of their research and consider how it may impact society as a whole.
Once an ethical issue has been identified, scientists must consider the potential benefits and harms of their research. This means weighing the potential benefits against the potential harms and considering alternative approaches that may be less harmful.
Another important aspect of ethical decision making is transparency. Scientists must be transparent about their research and its potential implications. This includes being open about any potential conflicts of interest and working with other stakeholders to ensure that the research is conducted in an ethical manner.
Finally, scientists must be willing to engage in ethical discussions and debates. This means being open to criticism and being willing to modify their research if necessary. It also means working with other stakeholders, such as policymakers and the public, to ensure that the research is conducted in a way that is consistent with societal values and norms.
In conclusion, the ethics of science are complex and challenging, but they are also essential for ensuring that scientific research benefits society without causing harm. By discovering the depths of science's moral compass and embarking on a journey of ethical decision making, scientists can make a positive impact on the world around them | eng | 21696d74-a5e9-416b-a349-86dd9d6ffeb0 | https://amanterpecaya.com/the-ethics-of-science-navigating-the-controversial-issues-surrounding-scientific-research/ |
iPad vs MacBook: 5 Pros and Cons When Deciding Which Is Right for You
iPads and MacBooks are two of the most popular choices for mobile computing and are also some of Apple's best-selling products. While both devices offer similar capabilities, they generally target different types of users. The iPad is a tablet that runs on a custom operating system, which is more similar to the iPhone's than a Mac's.
On the other hand, the MacBook is a full-fledged computer that does everything you would expect it to. MacBooks run on Apple's macOS operating system, which supports everyday tasks. Unlike the iPad, it has a built-in keyboard and trackpad, but it doesn't have a touchscreen.
You should carefully consider the two devices to find out which one is the best for you. Either way, both are great devices that will provide a great experience.
iPad vs MacBook: Side-by-Side Comparison
iPad
MacBook
Price Range
$329 – $2,399
$999 – $6,499
Screen Range
10.2″ – 12.9″
13.3″ – 16.2″
Operating System
iPadOS
macOS
Compatible Software
iPad App Store Only
Mac App Store and User-Installed Applications
Models
Classic, Mini, Air, Pro
Air, Pro
Processors (Currently Available)
A13, A14, M1, M2
M1, M2, M2 Pro, M2 Max
iPad vs MacBook: What's the Difference?
iPads and MacBooks each offer great features that target different types of users. The iPad is a tablet device, whereas the MacBook is a computer. The two devices run on very different operating systems, with the iPad resembling a mobile device, and the MacBook running on a conventional computer operating system.
The difference in operating systems means that each device also runs very different programs. The iPad is much more limited in use, but there are a number of accessories that make it operate like a computer.
However, nothing can replace the inputs and power of an actual laptop. Strangely enough, these two devices are closer in price than you may think.
User Interface
The glaring difference between an iPad and a MacBook is how you use them. A MacBook is a traditional laptop that deviates little from what a consumer expects. An iPad, on the other hand, is a tablet that is often described as a large iPhone. While that may be partially true, the iPad fits in a weird spot between the iPhone and MacBook products.
In the early days of the MacBook, its features and usability were very limited to essentially that of a large iPhone or iPod Touch. But today, the iPad is a solid alternative to a MacBook.
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While it doesn't have a trackpad or keyboard, you can purchase really high-quality ones that work with it. The iPad gets very close to a MacBook when paired with an Apple Magic Keyboard.
The limiting factor for the iPad, though, is that it requires specific apps and cannot run traditional software. While that may be a hindrance to some, the iPad's simple interface makes up for its limited uses. However, some still feel that the lack of a traditional interface is frustrating, and, in reality, an iPad won't replace a computer.
Operating System
The iPad's operating system is a hotly debated topic. Some users love its simplicity, while others hate its simplicity. If you are an iPhone user, then you will likely enjoy just how similar the operating system is.
Moreso, the iPad features almost all of the same apps as the iPhone. While it can't make a normal phone call, it does offer FaceTime and iMessage.
In comparison, the MacBook runs on a Macintosh operating system that remains true to its roots while getting a number of upgrades over the years; macOS is simple to use and offers a lot of customizability that you can't get on the iPad. In recent years, Apple has done a lot to blend iOS and macOS, creating a seamless experience between devices and streamlining many apps.
Connections
Another glaring difference between the MacBook and iPad is the number and types of connections on each. The iPad traditionally had a Lightning USB port and a 3.5mm audio jack. But several years ago, Apple removed the 3.5mm ports and switched from Lightning connectors to USB-C. MacBooks, on the other hand, are much more complicated.
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10/03/2023 06:34 am GMT
MacBooks have gone through countless connectivity changes over the years, but most of the new ones have USB-C and 3.5mm audio ports. The USB-C ports do work for charging and are the sole means of charging certain MacBook devices, like the M1 MacBook Air.
However, many of Apple's newer MacBooks use the new MagSafe charger. Connectivity is still pretty limited with USB-C, but its growing use means that more devices, such as flash drives, are using the connector.
In the meantime, you will need to use an adapter to connect older USB-A peripherals to your MacBook. The iPad Air can also connect to select devices such as HDMI displays and SD cards by using an adapter, though its supported devices are very limited.
Apps
As previously mentioned, the line between Apple's various operating systems has blurred significantly over the years. MacBooks, iPhones, and iPads can all access an Apple App Store, but the apps that each one contains differ widely.
To start with, the iPhone app store offers programs designed specifically for the small phone platform. Meanwhile, the iPad's app store offers all of the same apps as the iPhone's store but adds apps designed specifically for it.
These iPad apps use the entire screen space and may be optimized for the iPad's hardware. iPhone apps running on an iPad natively shrink to the size of an iPhone, but you can maximize them to fit the iPad's screen.
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The MacBook's app store is the most limited, featuring select mobile apps that developers must approve to make available on macOS. Additionally, there are a large number of apps specifically designed to run on Mac computers.
If you are in the Apple ecosystem of products, your purchased apps typically go between all device types. But the one place where iPads and MacBooks really differ is that the MacBook has a lot more flexibility in the types of programs it can run.
With a MacBook, you can easily download a program from the internet and install it, whereas the iPad is limited to only running apps purchased from the app store. This is a major concern if you want to use your device for specific software that isn't available in the app store.
Power
It is difficult to quantify the power capabilities of the iPad and MacBook since they are very different devices. However, you can get iPads that run on Apple's latest M-Series processors. These are the same chips that Apple uses on its laptops. Keep in mind that each tier of MacBook and iPad comes with different processor options.
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10/03/2023 06:04 am GMT
Additionally, an iPad with an M1 processor may not be as powerful as a MacBook running the same M1 processor. This is partly due to power and cooling limitations with the iPad's smaller form factor, but also because of the components used. For instance, MacBooks often use the more powerful Pro and Max chips alongside more RAM.
Pricing
The price difference between iPads and MacBooks is pretty hard to pin down because there are so many versions of each. In the iPad family, there are three main types of devices, the traditional iPad, the iPad Air, and the iPad Pro. These roughly align with the models of MacBooks, which currently include the MacBook Air and MacBook Pro.
The Air and Pro versions of both devices line up pretty close with regard to power and offerings. The base model iPad Air may look deceptively cheap compared to some of the pricier MacBook Air models, which go over $1,000. However, you need to add $200-$300 to the iPad Air's price tag account for a keyboard and other accessories.
Additionally, both the iPad Air and MacBook Air are available with an M1 chip, but there is a new MacBook available with the M2 chip. While the M2 MacBook Air is more expensive, it is newer and offers increased speeds.
Meanwhile, the M1 MacBook Air is on the cheaper end of the Apple computer spectrum, much like the standard iPad. But don't let the standard iPad's low price fool you. It still runs on an iPhone processor rather than the MacBook M-Series.
On the other end of the spectrum are the MacBook Pro and iPad Pro, which both offer top performance. Both of these devices are available with the M2 chip, but they come at a premium. Just like with the Air, the Pro devices are pretty close in price when accounting for accessories.
iPad vs MacBook: 5 Must-Know Facts
Both MacBooks and iPads offer great portability with long-lasting batteries.
iPads and MacBooks run on different operating systems, known as iPadOS and macOS, respectively.
Both devices can connect to external displays and accessories, such as mice and keyboards.
The iPads have special cases which house a keyboard and even a trackpad.
New Apple Silicon processors are used in all new MacBooks and select iPads, such as the Air and Pro.
iPad vs MacBook: Which One Is Better? Which One Should You Use?
Whether an iPad or MacBook is better really depends on what you want to do with the device. For instance, iPads are great tablets, but they are not a replacement for a computer. Similarly, MacBooks are great computers, but they are not as convenient or portable as an iPad.
While both devices have their own pros and cons, it is best to make a list of tasks you need to complete with either device. An iPad is a good option to use around the house for web surfing or watching videos. Its compact size makes it ideal for carrying around.
It is also important to remember that the iPad has a touchscreen that works with the Apple Pencil. Many users rave about it as a great drawing tablet, which is something that you cannot do with an iPad.
In comparison, a MacBook has a much larger set of features, all built-in. For instance, it is much easier to take notes on a MacBook because it has a full-size keyboard. More importantly, MacBooks can run a large number of programs that are not available on iPadOS. Therefore, the MacBook is usually a better choice for office or school use.
iPad vs MacBook: 5 Pros and Cons When Deciding Which Is Right for You FAQs (Frequently Asked Questions)
Can you use a mouse with an iPad?
Yes, few people realize that the iPad actually works with Bluetooth mice or even USB ones. The feature wasn't added until iPadOS 13, and when connected correctly, it adds a pointer to the screen.
Are MacBook screens larger than iPad ones?
The largest iPad currently available is the iPad Pro 12.9-inch, which is about six inches smaller than the smallest iPad, which is 13.3 inches.
Can MacBooks run app store apps?
MacBooks have an app store that is similar to other Apple devices, but the apps available are different. The MacBook App Store has unique apps designed specifically for laptops while also including some mobile apps.
Do MacBooks have a touchscreen?
No, Apple has never released a laptop with a touchscreen.
Can you connect an iPad to a monitor?
Yes, you can connect an iPad to a monitor with an appropriate USB-C or HDMI adapter | eng | 874baf58-0603-40b6-bb32-82f1a06a33c7 | https://history-computer.com/ipad-vs-macbook/ |
Cambodia
header1Overview
Cambodia's political system has been dominated by Prime Minister Hun Sen and his Cambodian People's Party (CPP) for more than three decades. The country has conducted semicompetitive elections in the past, but the 2018 polls were held in a severely repressive environment that offered voters no meaningful choice. The main opposition party was banned, opposition leaders were in jail or exiled, and independent media and civil society outlets were curtailed. The CPP won every seat in the lower house for the first time since the end of the Cambodian Civil War, as well as every elected seat in the upper house in indirect elections held earlier in the year.
header2Key Developments in 2018
The CPP won every seat in the lower house, the National Assembly, in July elections. The polls were held amid a period of repression that began in earnest in 2017, and saw the banning of the main opposition party, opposition leaders jailed or forced into exile, and remaining major independent media outlets reined in or closed. The CPP also dominated elections for the upper house, or Senate, held in February, taking every elected seat.
The Phnom Penh Post, regarded by many observers as the last remaining independent media outlet in Cambodia, was taken over by a Malaysian businessman with links to Hun Sen.
A Cambodian court sentenced an Australian filmmaker to six years in jail on charges of espionage. He had been arrested after denouncing rights abuses and filming political rallies.
In November, the UN-assisted court known as the Khmer Rouge Tribunal found Nuon Chea and Khieu Samphan, two surviving leaders of the Khmer Rouge, guilty of genocide and crimes against humanity. The verdict for the first time legally defined the Khmer Rouge's crimes as genocideKing Norodom Sihamoni is chief of state, but has little political power. The prime minister is head of government, and is appointed by the monarch from among the majority coalition or party in parliament following legislative elections. Hun Sen first became prime minister in 1985. He was nominated most recently after 2018 National Assembly polls, which offered voters no meaningful choice. Most international observation groups were not present due to the highly restrictive nature of the contest.
Score Change: The score declined from 1 to 0 because the incumbent prime minister was unanimously confirmed for another term after parliamentary elections that offered voters no meaningful choice.
A21.00-4.00 pts0-4 pts
Were the current national legislative representatives elected through free and fair elections?
0.0004.004
The bicameral parliament consists of the 62-seat Senate and the 125-seat National Assembly. Members of parliament and local councilors indirectly elect 58 senators, and the king and National Assembly each appoint 2. Senators serve six-year terms, while National Assembly members are directly elected to five-year terms.
In 2018, the CPP won every seat in both chambers in elections that were considered neither free nor fair by established international observers, which declined to monitor them. In the months before the polls, the Supreme Court had banned the main opposition Cambodia National Rescue Party (CNRP) and jailed many of its members, and closed media outlets and intimidated journalists to the extent that there was almost no independent reporting on the campaign or the polls. Several small, obscure new "opposition parties" ran candidates in the lower house elections, though many of the parties were widely believed to have been manufactured to suggest multiparty competition. Following calls for an election boycott by former CNRP leaders, Hun Sen repeatedly warned that people who did not vote in the election could be punished. The election was condemned by many democracies. The United States responded by imposing targeted sanctions on Cambodian leaders, while the EU threatened to roll back a preferential trade agreement.
Score Change: The score declined from 1 to 0 because the parliamentary elections took place in a highly repressive environment that offered voters no meaningful choice, and produced a one-party legislature.
A31.00-4.00 pts0-4 pts
Are the electoral laws and framework fair, and are they implemented impartially by the relevant election management bodies?
1.0014.004
In 2015, Cambodia passed two new election laws that permit security forces to take part in campaigns, punish parties that boycott parliament, and mandate a shorter campaign period of 21 days. The laws have been broadly enforced.
Voting is tied to a citizen's permanent resident status in a village, township, or urban district, and this status cannot be changed easily. In 2017, an amendment to the electoral law banned political parties from association with anyone convicted of a criminal offense.
The National Election Committee (NEC) was reformed in 2013, but the CPP has since asserted complete control over its nine seats. Criminal charges were brought against the body's one independent member in 2016, who was then jailed and removed from the body. The four NEC members affiliated with the CNRP resigned following the party's 2017 dissolution. In 2018, the NEC sought to aid the CPP's campaign by threatening to prosecute any figures that urged an election boycott, and informing voters via text message that criticism of the CPP was prohibited.
Score Change: The score declined from 2 to 1 because the election commission, controlled by the ruling party since the ouster of independent and opposition members, participated in the government's efforts to control the outcome of the parliamentaryFollowing the 2018 elections, Cambodia is a de facto one-party state. The main opposition CNRP was banned and its leaders have been charged with crimes, while other prominent party figures have fled the country. Although several small opposition parties contested the 2018 July lower house elections, none won seats. All of the smaller parties were permitted to run by the CPP-controlled National Election Committee, and both domestic and international observers widely questioned their authenticity.
Score Change: The score declined from 1 to 0 because the only significant opposition party remained banned and persecuted even as multiple parties of dubious authenticity were allowed to register for parliamentary elections, creating an illusion of competition.
B21.00-4.00 pts0-4 pts
Is there a realistic opportunity for the opposition to increase its support or gain power through elections?
0.0004.004
The political opposition has been quashed, with the CNRP banned and its leaders facing criminal charges. The high rate of spoiled ballots in the 2018 lower house election—8.6 percent of all votes, according to the NEC—suggested strong popular discontent with the lack of choice, especially given that Hun Sen had repeatedly warned Cambodians not to spoil ballots. Elections for the upper house earlier in the year were similarly structured so that the CPP had no real opposition. There were widespread reports of voters being bullied and intimidated before the July lower house elections into casting a vote for the CPP.
After the elections, amid increasing international scrutiny, Hun Sen and the CPP modestly eased pressure on the opposition. In August, the king pardoned 14 CNRP members who had been jailed for "insurrection." CNRP co-leader Kem Sokha was released on bail in September after spending a year in solitary confinement on treason charges, though he still faced significant restrictions on his movement. Late in 2018, the government initiated legislation that could allow bans on political activity for some opposition figures to be lifted.
CNRP co-leader Sam Rainsy has remained abroad; he was convicted of defamation in 2017 and faces a number of other legal cases in Cambodia, and risks imprisonment if he returns. Many other prominent CNRP figures remain in exile. At year's end, the opposition appeared ready to split, with supporters of Rainsy and Kem Sokha seemingly parting ways ruling party is not democratically accountable, and top leaders, especially Hun Sen, use the police and armed forces as a tool of repression. The military has stood firmly behind Hun Sen and his violent threats, and his crackdown on opposition. Hun Sen has built a personal bodyguard unit in the armed forces that he reportedly uses to harass and abuse CPP opponents.
Before the 2018 lower house elections, Human Rights Watch reported that the security forces were illegally campaigning for the CPP. Additionally, several top military commanders won seats in the lower house as CPP legislators. One, General Pol Saroeun, then vacated his seat to become a senior minister in the new governmentEthnic Vietnamese are regularly excluded from the political process and scapegoated by both parties. Women make up 15 percent of the National Assembly, but their interests, like those of all citizens, are not well representedHun Sen has increasingly centralized power, and figures outside of his close circle have little impact on policymaking. Some reports suggest he is preparing to eventually hand power to his son, Hun Manet, who has deep ties throughout the armed forces. In September, Hun Manet was promoted to commander of the armed forces.
C21.00-4.00 pts0-4 pts
Are safeguards against official corruption strong and effective?
1.0014.004
Anticorruption laws are poorly enforced, and corruption remains a serious challenge in Cambodia. A 2016 Global Witness report suggested that Hun Sen's family had amassed wealth totaling between $500 million and $1 billion, claims that the prime minister and his family deny. Corruption is rampant in public procurement, tax administration, customs administration, and other state processes, and bribes are frequently required in dealings with various government departments.
C31.00-4.00 pts0-4 pts
Does the government operate with openness and transparency?
1.0014.004
Nepotism and patronage undermine the functioning of a transparent bureaucratic system. A draft access to information law was made public in January 2018, though domestic observers expressed concern that upon implementation it would be ignored or misused. The law was pending uses lawsuits, criminal prosecutions, massive tax bills, and occasionally violent attacks as means of intimidation against the media. There are private print and broadcast outlets, but many are owned and operated by the CPP.
Starting in 2017 the government engaged in an intense crackdown on independent media, and these efforts continued throughout 2018. In 2017, the independent Cambodia Daily closed under pressure from the government regarding its tax bills. In 2018, the Phnom Penh Post, known for its independent and investigative reporting, was sold to a Malaysian investor with links to Hun Sen, and many of its editors and reporters quit or were fired following the sale. In addition, many other local media outlets were intimidated into closing or, in the run-up to the July lower house elections, becoming government mouthpieces. Before the lower house elections, the election commission released a code of conduct for journalists that mandated fines of as much as $7,500 for using "their own ideas to make conclusions" or publishing news deemed to "affect political and social stability" or cause "confusion and loss of confidence" regarding the election.
Two Radio Free Asia journalists arrested in 2017 on charges of espionage still face trial in Cambodia. In August 2018, an Australian filmmaker was sentenced to six years in jail for espionage, after creating footage about rights abuses and public rallies. Late in 2018, Hun Sen publicly promised to ease pressure on independent media, as well as on civil society more generally and on the political opposition; his government offered to allow the Cambodia Daily and Radio Free Asia to reopen in Cambodia, although it remained unclear whether they would do so.
D21.00-4.00 pts0-4 pts
Are individuals free to practice and express their religious faith or nonbelief in public and private?
3.0034.004
The majority of Cambodians are Theravada Buddhists and can practice their faith freely, but societal discrimination against religious and ethnic minorities persists.
D31.00-4.00 pts0-4 pts
Is there academic freedom, and is the educational system free from extensive political indoctrination?
2.0024.004
Teachers and students practice self-censorship regarding discussions about Cambodian politics and history. Criticism of the prime minister and his family is often punished.
D41.00-4.00 pts0-4 pts
Are individuals free to express their personal views on political or other sensitive topics without fear of surveillance or retribution?
2.0024.004
The state generally does not intervene in people's private discussions, though open criticism of the prime minister can result in reprisals. In 2018, however, Hun Sen and other government leaders warned ahead of the lower house election that criticism of the government would be punished severely. Additionally, an order issued before the election required internet service providers (ISPs) to install software necessary to monitor, filter, and block "illegal" online content, including social media accounts.
Earlier, in February, an amendment to the criminal code introduced a new lèse-majesté offense that made it illegal to defame, insult, or threaten the king. The law carries a sentence of between one and five years in jail, and a fine of 2 to 10 million riel (about $500 to $2,500).
EAssociational and Organizational Rights
E11.00-4.00 pts0-4 pts
Is there freedom of assembly?
1.0014.004
Authorities are openly hostile to free assembly. The shooting deaths of five postelection protesters by security forces in 2014 discouraged opposition demonstrations, as have continued government assertions that dissent will not be tolerated. The few small opposition parties that did contest the lower house elections had few or no events. In March, a land dispute in Kratie over the activities of a rubber plantation resulted in police firing on protestors and possibly killing eight people, although reports of the incident varyActivists and civil society groups dedicated to justice and human rights face increasing state harassment. Prominent activist Kem Ley was murdered in broad daylight in 2016. In January 2018, three activists involved with planning his funeral were charged with embezzlement, though charges against one of them were later dropped. A number of other activists faced legal harassment during the year, including some with the Cambodian Human Rights and Development Association (ADHOC). The National Democratic Institute, a US-based nongovernmental organization (NGO), was forced to shut its Cambodia operations in 2017.
A variety of less overtly political groups are able to operate.
E31.00-4.00 pts0-4 pts
Is there freedom for trade unions and similar professional or labor organizations?
1.0014.004
Cambodia has a small number of independent trade unions, and workers have the right to strike, but many face retribution for doing so. A 2016 law on trade unions imposed restrictions such as excessive requirements for union formation.
FRule of Law
F11.00-4.00 pts0-4 pts
Is there an independent judiciary?
0.0004.004
The judiciary is marred by corruption and a lack of independence. Judges have facilitated the government's ability to pursue charges against a broad range of opposition politicians, and played a central role in keeping Kem Sokha in a remote jail, without bail, despite significant health problems, for nearly a year. He was finally freed on bail in September 2018, but with severe restrictions on his movement.
F21.00-4.00 pts0-4 pts
Does due process prevail in civil and criminal matters?
1.0014.004
Due process rights are poorly upheld in Cambodia. Abuse by law enforcement officers and judges, including illegal detention, remains extremely common. Sham trials are frequent, while elites generally enjoy impunity. When lawyers or others criticize judges, they often face retribution.
F31.00-4.00 pts0-4 pts
Is there protection from the illegitimate use of physical force and freedom from war and insurgencies?
1.0014.004
Cambodians live in an environment of tight repression and fear. The torture of suspects and prisoners is frequent. The security forces are regularly accused of using excessive force against detained suspects.
The ongoing work of the Extraordinary Chambers in the Courts of Cambodia (ECCC), established to try the leaders of the former Khmer Rouge regime, has brought convictions for crimes against humanity, homicide, torture, and religious persecution. In November 2018, the tribunal found Nuon Chea and Khieu Samphan, two surviving leaders of the Khmer Rouge, guilty of genocide and crimes against humanity. They both received life sentences; both had already been sentenced to life in prison for past convictions of crimes against humanity. The 2018 convictions marked the first time the Khmer Rouge crimes were legally defined as genocide.
While others closer to the regime have faced allegations of involvement in these crimes, there is little indication the Hun Sen government will support additional prosecutions. It appears likely that there will be no further cases brought to the ECCC.
F41.00-4.00 pts0-4 pts
Do laws, policies, and practices guarantee equal treatment of various segments of the population?
1.0014.004
Minorities, especially those of Vietnamese descent, often face legal and societal discrimination. Officials and opposition leaders, including Sam Rainsy, have demonized minorities publicly.
The Cambodian government frequently refuses to grant refugee protections to Montagnards fleeing Vietnam, where they face persecution by the Vietnamese government.
While same-sex relationships are not criminalized, LGBT individuals have no legal protections from the rights to freedom of travel and movement, and the government generally respects these rights in practice. However, restrictions do occur, notably when the government tries to prevent activists from traveling around the countryLand and property rights are regularly abused for the sake of private development projects. Over the past several years, hundreds of thousands of people have been forcibly removed from their homes, with little or no compensation, to make room for commercial plantations, mine operations, factories, and high-end residential developmentsThe government does not frequently repress personal social freedoms, but women suffer widespread social discrimination. Rape and violence against women are common.
G41.00-4.00 pts0-4 pts
Do individuals enjoy equality of opportunity and freedom from economic exploitation?
1.0014.004
Equality of opportunity is severely limited in Cambodia, where a small elite controls most of the economy. Labor conditions can be harsh, sometimes sparking protests. Sex and labor trafficking remains a significant problem, and while the government's program to combat it is inadequate, the US State Department has said the Cambodian government has increased its antitrafficking efforts. | eng | f0074601-912e-4728-9b37-a2e47b39b060 | https://freedomhouse.org/country/cambodia/freedom-world/2019 |
Latest Articles
Glossary / Lexicon
Psychoanalyst
Psychoanalyst refers to a therapist who practices Psychoanalysis after earning either an M.D. or a Ph.D. degree and receiving additional specialized postdoctoral training .
A psychoanalyst is a mental health professional who practices psychoanalysis, a therapeutic approach that was developed by Sigmund Freud. Psychoanalysis is a method of treating mental healthconditions by exploring the unconscious mind and the underlying psychological conflicts that may be contributing to a person's symptoms.
Psychoanalysts typically use techniques such as free association, in which the patient is encouraged to speak freely about their thoughts and feelings, and interpretation, in which the psychoanalyst helps the patient understand the underlying meaning of their thoughts and behaviors.
Psychoanalysts may work with individuals, couples, or groups, and sessions are typically conducted in a private setting in which the patient lies on a couch and the psychoanalyst sits behind them, out of sight. | eng | a1faf472-c642-4fdd-8ff2-aee6a7a2c312 | https://www.psychology-lexicon.com/cms/glossary/49-glossary-p/5780-psychoanalyst.html |
Blueberry Cheesecake
Indulge your senses in a delectable delight with Blueberry Cheesecake, a cannabis strain that combines the creamy decadence of cheesecake with the luscious sweetness of ripe blueberries. Like a culinary masterpiece, this strain captivates with its tantalizing flavors and blissful effects, inviting you to savor a moment of pure indulgence.With each inhalation, the air becomes infused with a mouthwatering aroma of freshly baked cheesecake, adorned with a generous drizzle of juicy blueberries. As the smoke swirls within your lungs, a wave of soothing relaxation sweeps over your body, melting away stress and leaving you in a state of pure bliss.But Blueberry Cheesecake is more than just a strain—it's a sensory symphony. It sparks creativity and enhances your appreciation for the finer things in life, allowing you to revel in the pleasures of the present moment.Satisfy your cravings with the captivating allure of Blueberry Cheesecake and let it transport you to a world of gastronomic pleasure. Surrender to its creamy embrace and experience a symphony of relaxation and inspiration. Brace yourself for an extraordinary journey as Blueberry Cheesecake unveils the secrets of cannabis indulgence, leaving you with a taste of pure ecstasy and a desire for another slice of life's delectable joys.
Description
If you're looking for a cannabis strain that offers a sweet and smooth smoking experience with a potent relaxing effect, look no further than Blueberry Cheesecake. This indica-dominant hybrid is beloved by many for its delicious taste, aroma, and calming effects.
Origin:
Blueberry Cheesecake is a cross between two legendary strains: Blueberry and Cheese. Blueberry is an indica-dominant strain known for its sweet, fruity aroma and calming effects, while Cheese is a hybrid with a distinctive cheese-like scent and a euphoric, uplifting high. The combination of these two strains creates a unique and delicious hybrid with a balanced and enjoyable effect.
Aroma:
As its name suggests, Blueberry Cheesecake has a sweet, fruity aroma that is reminiscent of freshly baked blueberry muffins. The scent is enhanced by a slightly sour and tangy undertone, which comes from the Cheese genetics. When you open a bag of Blueberry Cheesecake, you'll be hit with a strong, delicious scent that is sure to make your mouth water.
Taste:
The taste of Blueberry Cheesecake is just as delicious as its aroma. On the inhale, you'll taste a sweet and fruity flavor, with notes of blueberries, raspberries, and blackberries. On the exhale, you'll notice a slight tangy and cheesy flavor that adds depth and complexity to the smoke. The taste is smooth and pleasant, making it easy to smoke without any coughing fits.
Effects:
Blueberry Cheesecake has a well-balanced effect that is both calming and uplifting. It's a great strain to smoke if you're looking to unwind after a long day or simply want to relax and destress. The high starts with a euphoric and uplifting feeling that can boost your mood and give you a burst of energy. As the high progresses, you'll feel a wave of relaxation that spreads throughout your body, easing tension and stress.
This strain is known for its pain-relieving properties and can be effective at reducing chronic pain, headaches, and muscle spasms. It's also great for inducing sleep, making it a popular choice among insomniacs. The high lasts for several hours and gradually tapers off, leaving you feeling relaxed and mellow.
Growing:
Blueberry Cheesecake is a relatively easy strain to grow and is suitable for both indoor and outdoor cultivation. It has a flowering time of around 8-9 weeks and produces dense, sticky buds with a high THC content. The plant is resistant to pests and diseases, making it a great choice for beginner growers.
When grown indoors, Blueberry Cheesecake can produce a yield of up to 500g/m2, while outdoor plants can yield up to 700g/plant. The plant grows to a medium height and can be easily managed with regular pruning and training.
Closing thoughts:
Blueberry Cheesecake is a delicious and potent strain that offers a well-rounded and enjoyable smoking experience. Its sweet aroma and taste make it a popular choice among cannabis connoisseurs, while its relaxing and pain-relieving effects make it a favorite among medical patients. If you're looking for a strain that can help you unwind and destress, give Blueberry Cheesecake a try.
Call to action:
If you're looking to buy Blueberry Cheesecake in Canada, there are several reputable online dispensaries that offer this strain. Some options include Weedmaps, BC Bud Supply, and Get Kush. Check out their websites and browse their selection of Blueberry Cheesecake and other popular strains. Happy smoking!
Blueberry Cheesecake is a popular strain among both medical and recreational users due to its well-balanced effects and delicious flavor profile.
Effects:
The effects of Blueberry Cheesecake are known to be uplifting and mood-boosting, making it an ideal strain for social situations or creative pursuits. It can also provide a relaxing body high that is not too overwhelming, making it suitable for daytime use. The high THC content in this strain can lead to a feeling of euphoria and a sense of calm, making it ideal for treating stress, anxiety, and depression. Additionally, Blueberry Cheesecake has been reported to provide relief from pain, headaches, and inflammation.
Growing:
Blueberry Cheesecake can be grown both indoors and outdoors, although it tends to thrive in a warm and sunny climate. It is a medium-sized plant with dense, resinous buds that have a sweet, fruity aroma. This strain has a flowering time of around 8-9 weeks and can produce a moderate to high yield. It is recommended to provide plenty of nutrients, light, and space for the plant to grow properly.
Call to Action:
If you're interested in trying Blueberry Cheesecake for yourself, there are several online dispensaries in Canada that offer this strain. One such option is Haute Health, which offers a variety of high-quality cannabis products, including Blueberry Cheesecake flower. They also provide discreet shipping throughout Canada, making it easy and convenient to get the products you need. So why not give Blueberry Cheesecake a try and experience its delicious taste and well-balanced effects? | eng | ad1a04ca-e14a-469d-800f-669dec043d87 | https://www.weedpedia.ca/product/blueberry-cheesecake/ |
English for Specific Purposes
English for specific purposes (ESP) is a subset of English as a second or foreign language. It usually refers to teaching the English language to university students or people already in employment, with reference to the particular vocabulary and skills they need. As with any language taught for specific purposes, a given course of ESP will focus on one occupation or profession, such as Technical English, Scientific English, English for medical professionals, English for waiters, English for tourism, etc. Despite the seemingly limited focus, a course of ESP can have a wide-ranging impact, as is the case with Environmental English.
English for Moral Science & Ethics
Ethics is the part of philosophy that deals with good and evil. Ethics tries to answer questions like:
What actions are good? What actions are evil? How can we tell the difference? Are good and evil the same? How should we make hard decisions that might help or hurt other people? How do our actions affect others?
English for Elder Care
Old age is when a person is near or beyond the usual life expectancy, usually from the age of 65 onwards. Old people are usually retired from work and spend their time in other ways like helping take care of small children who are kin to them in some way. Old people have more health problems than young adults, and many of them take medicine. They need special care in many ways.
English for Child Care
Child care, also known as day care, is the care and supervision of a child or multiple children at a time, whose ages range from six weeks to thirteen years. Child care is the action or skill of looking after children by a day-care center, nannies, babysitter, teachers, etc. Child care providers can be children's first teachers. The main focus of childcare is on the development of the child, whether that be mental, social, or psychological.
English for Laws
Law is a set of rules decided by a particular place or authority meant for the purpose of keeping the peace and security of society. Courts or police may enforce this system of rules and punish people who break the laws, such as by paying a fine, or other penalty including jail. In ancient societies, laws were written by leaders, to set out rules on how people can live, work and do business with each other.
English for Family Matters
A family is a group of people who, in most cases, live together. They share their money and food and are supposed to take care of one another. Its members are either genetically related (like brother and sister) or legally bound to each other, for example by marriage. A family is said to be society's smallest unit, its nucleus. Family life is more private and intimate than public life. But in most countries there are laws for it.
English for Social Work
Social work is work done for the welfare of the society. A social worker is a trained individual who represents the social well-being of society. Principles of social justice, human rights, collective responsibility and respect for diversities are embedded in social work. Underpinned by theories of social work, social sciences, humanities and indigenous knowledges, social work engages people and structures to address life challenges and enhance well being." Social workers are employed in human services track, like hospitals, clinics, NPOs, or publicly (government) as a staff that gives adequate welfare and helps people who cannot help themselves including physically disabled people, person with other disabilities.
English for Public Administration
Public administration has two meanings. First it means putting into action government policy. Second, academics study this, and prepare civil servants for working in the public service (the non-political part of the government). Public administration helps improve management and improve policies so that government can work better. Public administrators manage public programs, translate politics into the programs and services that citizens use every day.
English for Transportation
Transport, or transportation, is moving people or things from one place to another place. Transport can be divided into infrastructure, vehicles and operations. Infrastructure includes roads, railways, airports, canals and pipelines. The infrastructure is the network where things are carried. Infrastructure also includes airports, railway stations, bus stations and seaports (docks). Infrastructure is usually built by governments and paid for by taxes from the citizens of a country or region. Infrastructure such as roads and railways are designed by civil engineers and urban planners.
English for Games & Sports
Sport is commonly defined as an athletic activity that involves a degree of competition, such as netball or basketball. Some games and many kinds of racing are called sports. A professional at a sport is called an athlete. Many people play sports with their friends. They need coaches to teach or train teams or individuals how to do better. Sports can be played indoors or outdoors and by individuals or teams.
English for Health Care
Health care or healthcare is the preservation of mental and physical health by preventing or treating illnesses through services offered by the health profession and its staff. Health care includes all reasonable and necessary medical aid, medical examinations, medical treatments, medical diagnoses, medical evaluations and medical services. The right to health care is considered one of human rights with international human rights law as well as social security.
English for Visual Arts
The visual arts are art forms that create works which are primarily visual in nature. The visual arts (also known as the plastic arts) produce objects. They are contrasted with the performing arts. Examples are ceramics, drawing, painting, sculpture, printmaking. Also, modern visual arts which use technology: photography, video, filmmaking and architecture.
English for Fashion Design
Fashion design is the art and profession of designing clothes, costume and related items like hats, purses, bags and shoes. Fashion designers attempt to design clothes which are functional as well as attractive. They consider who is likely to wear a garment and the situations in which it will be worn. They have a range of materials to work with and a wide range of colors, patterns and styles to choose from | eng | 0e2868bd-c54d-4e2a-97c9-e9edc611d460 | https://www.ieltscounsellor.com/ko/english-for-specific-purposes |
A short road switcher heads down the Camrose sub to service a customer from Bretville | eng | 43b0bb71-944b-49a0-93f5-1a14c1db54c5 | https://thumbs.railfan.ca/cgi/viewer.cgi?2023-04-08.6352.Edmonton.mpg.jpg |
Why Setting Boundaries Can Transform Your Relationship
Why Setting Boundaries Can Transform Your Relationship
Boundaries play a crucial role in any relationship, and addressing them openly is especially important within marriages, close family dynamics, and extended family relationships. Unspoken boundaries often get repeatedly crossed in these contexts, resulting in toxicity and harm. In order to bring about positive change in your marriage and other significant relationships, it is essential to understand what boundaries truly entail and how to effectively establish them.
Boundaries Are Not Rules
First and foremost, it is important to recognize that boundaries are not rules. They are not about imposing restrictions on others or dictating their actions. When you set up rigid rules, it often creates a context for rebellion and resistance. Just as you dislike being told what you can and cannot do, others feel the same way. Boundaries are about expressing your own needs and values and choosing not to engage in behaviors or situations that are harmful to you.
What a Boundary Looks Like
A boundary is about making your personal space safe and maintaining your identity and well-being. It involves taking charge of yourself and refusing to allow toxicity and harm to influence or shake your sense of self. Instead of telling others what they can or cannot do, a boundary is a declaration of what you will no longer tolerate in your life. It is a way of saying, "You can continue to behave that way if you choose, but I am removing myself from participating in it because it goes against who I am."
Boundaries as an Invitation to Change
Establishing boundaries in a relationship serves as an invitation to change for both parties involved. By clearly communicating what you will and will not accept, you are initiating a transformational process. It gives the other person an opportunity to reflect on their actions and decide whether they are willing to make the necessary changes to maintain a healthy connection with you. This crossroads reveals their true intentions and level of commitment to the relationship. If they adamantly refuse to change, it becomes apparent that they are not genuinely interested in being in a relationship with you.
Consequences and Follow-Through
The effectiveness of a boundary lies in its consequences and the commitment to follow through with them. Boundaries must have meaningful consequences for the other person, providing motivation for them to change their behavior. Without consequences, boundaries remain mere wishes or hopes, lacking the power to bring about transformation. Natural consequences often arise from specific behaviors. For instance, if a spouse chooses to engage in infidelity, a natural consequence could be a broken relationship until they demonstrate genuine efforts to end their affairs and prioritize the marriage.
Maintaining Healthy Boundaries
Establishing and maintaining healthy boundaries requires consistent effort. When faced with disrespectful behavior such as name-calling or contempt, it is essential not to engage or defend yourself. Instead, it is more effective to calmly express that such behavior is detrimental to the relationship and refuse to participate in arguments or finger-pointing. Walking away from toxic situations and prioritizing your own well-being establishes a boundary that protects your emotional safety.
Taking Control of Your Journey
Healthy boundaries empower you to take control of your internal state and the direction of your life. By creating boundaries that reflect what you will tolerate for yourself and where you are headed, you establish a sense of agency and self-respect. Boundaries are not about changing others but about ensuring your own safety, peace, and personal growth.
In conclusion, setting boundaries can be a transformative force within relationships. By understanding that boundaries are not rules, but expressions of self-respect, you can establish healthy boundaries that protect your well-being. Inviting change through clear communication and enforcing meaningful consequences fosters growth and reveals the true nature of the other person's commitment. Ultimately, boundaries enable you to maintain a safe space within your relationship, ensuring a peaceful and fulfilling home | eng | a3bd8276-29a6-4278-b917-ee457b22299f | https://marriagerecoverycenter.com/setting-boundaries/ |
What Kind of Place Was the Earth?
What Kind of Place Was the Earth?
Is the existence being on the Earth itself blessing? – Rei Naito has projected the question over her works to find an answer through her career as an artist.
Having created sacred places, Naito has now extended her view on "human".
Where does the "human" come from and why it was born on the Earth? What is the "human" trying to see? What can be made through a trip of the "human"?
― Statement from publisher | eng | bfa86966-1a89-44c7-b28b-53196d4f0296 | https://www.shashasha.co/en/book/what-kind-of-place-was-the-earth |
The common or pendunculate oak (Quercus robur) is the most widespread autochthonous (native) tree of the National Park. This species, when well matured (old trees that have been growing for 100 years or more), can reach heights of up to 30 metres and support an enormous biodiversity. On the trunk and branches can be found not only fungi, lichens, mosses, and ivy (Hedera helix), but also various animal species: insects, like the stag beetle (Lucanus cervus), which lives and eats on the wood of the oak; gall wasps (small wasps that place their eggs in a plant and induce the growth of galls, inside which the larvae can develop and hatch in safety); squirrels (Sciurus vulgaris) and jays (Garrulus glandarius) which feed off acorns. There are many bird species that nest in oaks, other species that depend indirectly on the trees, whether through feeding off the insects that exist in and on oaks or from the dead leaves that fall to the ground or simply through seeking shade. | eng | a5a50358-79a4-4bb0-9ab6-95a549f57515 | http://adere-pg.pt/trilhos/uk/frame-detalhesponto.php?id_ponto=25 |
If each portion of the phone number is stored in NVRAM, you can recall each number with a short ATDT command. For example, the USRobotics Sporsters can save up to four phone numbers when you type the following at a command prompt:
AT&Zx=y
where x is a value from 0 to 3 and y is the phone number to be saved.
You can then dial the numbers by typing:
ATDSx
where x is a value from 0 to 3 corresponding to the desired phone number.
You can dial all four phone numbers in succession by typing:
ATDS0S1S2S3
You may have to insert commas between each "phone number" to pause the modem.
Set up the WinFrame Client for "direct connect." You can write a script file like this: | eng | 84c032dd-36e5-42ff-b4a5-20447ad16683 | http://support.yue.ctx.org.cn/ctx901063.citrix |
My Dad's birthday is today, born on August 6, 1941, making him 70 years old. While my Dad and I share similar (negative) personality traits, we don't have much in common, and our relationship isn't the best. It's not bad by any means, and I'm fairly certain that whatever is keeping us from being closerThe reasoning behind this is three-fold. 1) This fulfills a request that was made when I was actively seeking out topics to draw. 2) The request was made by a friend who is pretty big Dazzler fan. I have no idea if she really genuinely loves Dazzler or if it's an ironic thing. Either way, | eng | c3bdcf7d-0279-4330-945c-8bf19d206270 | https://www.shonborn.net/archives/tag/cover-recreation/page/2 |
Child sponsorship is more than a financial commitment; it's a personal relationship that can transform lives on both ends of the spectrum. Sponsors can connect with their sponsored child through letters, gifts, and even visits, creating a bond that transcends geographical boundaries and cultural differences. Child sponsorship's personal connections between sponsors and children are powerful in sharing love and hope, and can profoundly impact the lives of both parties.
The Value of Personal Relationships in Sponsorship
The personal relationship between sponsors and sponsored children is a cornerstone of the sponsorship model. It's not just about providing resources; it's about building a relationship that can have a profound impact on both the sponsor and the child. For the child, having a sponsor means knowing that someone cares about their well-being and is invested in their future. For the sponsor, it's an opportunity to make a tangible difference in a child's life and witness their growth and development firsthand.[1]
The emotional benefits of this connection are significant for both the sponsor and the child. For the child, receiving letters from their sponsor can be a source of joy and motivation. These letters tell children they are loved, remembered, and important, often becoming some of the most treasured possessions these children have. For the sponsor, the relationship can provide a sense of purpose and fulfillment, knowing that their support is making a real difference in a child's life. It's a unique opportunity to witness the transformative power of love and support.[2]
GFA World's Approach to Fostering Connections
GFA World's approach to fostering connections between sponsors and children is rooted in their commitment to holistic child development. They understand that each child is unique and has different needs, and they strive to meet these needs through their sponsorship program. This includes not only providing for physical needs like food and education but also addressing emotional and spiritual needs. GFA World's child sponsorship staff play a crucial role in this process, offering guidance, encouragement, and support to the children in their care.[3]
Becoming a sponsor with GFA World's Child Sponsorship Program is more than a financial commitment; it's an invitation to join a journey of transformation. It's an opportunity to build a personal relationship with a child in need and witness the transformative power of love and support. By becoming a sponsor, you can help a child escape the cycle of poverty and give them the chance to dream of a brighter future. | eng | 36fde666-a273-4a50-8951-6049ab92bfba | https://gospelforasia.com/child-sponsorship-models/child-sponsorship-personal-connection/ |
The Gentle Embraces Of The Girls In The Chair Led To Voluptuous Sex
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The gentle embraces of the girls in the chair led to the fact that they both got excited and wanted to strip naked. And then they continued their touching and began to have lesbian sex, which was quickly transferred to the bed. There, the girlfriends found it as convenient as possible to deliver bliss to each other, which they gave with sponges and fingers. So they succeeded in knowing the buzz that plunged the virgins into voluptuous languor | eng | 9b360ee2-73dd-4ee4-a635-605658f5bd87 | https://www.pornorco.com/video/the-gentle-embraces-of-the-girls-in-the-chair-led-to-voluptuous-sex/ |
Why do you need Intimate wash? In keeping up with the hectic lifestyle, it's the intimate part of your body that bears the worst brunt of the environment, lifestyle, and sweat. Maintaining hygiene of the private areas can prevent infections, inflammation, foul odour and itchiness. Maintains pH balance: This gentle intimate cleanser is perfect for maintaining the delicate and natural pH balance of you down there. Powerful Ingredients: Neem and Sea Buckthorn present in Intimo prevents any strong odours that can become a storehouse of infections and cause of embarrassment. Cucumber helps soothe and relax any kind of itching that can have you looking for a corner to scratch. Anti- Septic & Anti-bacterial: This intimate wash is rich in Neem extracts that are anti-septic and anti-bacterial in nature. They help fight infection causing bacteria.The Man Company Intimate wash is free of SLS and Parabens. So its completely safe for the skin | eng | 15593510-a2fd-47ca-8271-92c6764f5dd9 | https://snapkartonline.com/the-man-company-intimo-intimate-foaming-wash-for-men-with-tea-tree-oil-sea-buck-thorn-oil-aloevera-neem-extract-prevents-bad-odor-anti-fungal-itching-ph-balance-personal-hygiene-wash-1/ |
A Q+A with AI UVA Professor Rajkumar Venkatesan
Profitable digital advertising and marketing methods are pushed by revolutionary advertising and marketing leaders who relentlessly pursue new methods to attach with their markets utilizing the most recent digital instruments, from synthetic intelligence (AI) to machine studying and extra. The AI Advertising Certificates from the Darden College Basis is designed to supply managers with the framework to advance their advertising and marketing methods to ship dynamic and customized buyer experiences.
We just lately requested Rajkumar Venkatesan, Ronald Trzcinski Professor of Enterprise Administration on the College of Virginia Darden College of Enterprise, about his expertise instructing within the AI Advertising Certificates program on Coursera.
Are you able to inform us a bit of bit about your self and the way you got here to UVA?
I accomplished my undergraduate diploma in pc engineering in 1997 in India. At the moment, I took courses on this new factor referred to as neural networks in my closing 12 months and I did my closing 12 months mission on genetic algorithms, each of which are actually a part of the AI toolkit. Once I got here to america to do my PhD in advertising and marketing, my PhD advisor informed me that expertise and computer systems are going to play an enormous position in advertising and marketing and requested if I can be eager about pursuing this in my PhD. At the moment, I didn't assume a lot of it and simply mentioned sure. I took courses in economics, advertising and marketing, client habits, and so forth. and located it actually fascinating. So, I caught round and completed my PhD. I then taught advertising and marketing analysis at the College of Connecticut, after which advertising and marketing analytics on the College of Virginia from 2006, and digital advertising and marketing since 2015. Charlottesville, VA is now house and our two sons had been born right here in Charlottesville.
On-line studying has great attain. I can unfold the message globally in my analysis, instructing and studying because it pertains to AI Advertising. On-line studying and the AI Advertising program present flexibility for members to study at their very own tempo in a structured and participating setting. Each program members and I get to study from industries throughout the world.
The AI Advertising Certificates program is suited to on-line studying as a result of there's great potential and progress in AI in lots of industries globally. Moreover, a platform that brings collectively individuals with completely different experiences is the fitting medium for the AI Advertising Certificates program.
Why is AI Advertising such an essential subject?
"The artwork challenges the expertise, and the expertise evokes the artwork."
I believe this quote from Jon Lasseter could be very applicable to understanding the evolution of advertising and marketing. Like artwork, advertising and marketing additionally has a symbiotic relationship with expertise. Within the outdated days, one had mass advertising and marketing on the radio. When the brand new expertise of TV happened, we noticed the golden period of tv commercials, however we nonetheless had one advert for all the shoppers. Then, we had the arrival of cable TV and we began segmentation as a model maybe had 3 or 4 advert variations for his or her completely different segments that aired on the suitable cable channels. With direct mail, we began the arrival of one-to-one advertising and marketing and began to extend our customization.
Then we had digital advertising and marketing and the rise of the web supplied extra customization. With AI, we're on the stage the place manufacturers are personalizing their advertising and marketing to a phase of 1. All via this evolution, although, the basics of selling maintain true – handle buyer wants, deal with advantages vs. options, develop emotional connections, be genuine, and extra.
What excites you most concerning the programs on this certificates program?
What excites me most about this certificates program is that it focuses on utility of abilities and this system programs comply with the AI Advertising Canvas framework, and these two features join and construct upon one another. What additionally excites me is that the course initiatives throughout the certificates program are a mixture of utilized workouts and simulations that present members with the power to follow and apply their abilities. Lastly, members can use and apply all course initiatives as a framework and roadmap in growing AI capabilities inside their very own group.
How may college students apply these programs to their profession objectives or their skilled life?
This course doesn't deal with coding and growing AI algorithms, relatively, it focuses on successfully utilizing current AI algorithms to customized advertising and marketing. In these programs, members can use the construction, framework, and steerage of the course initiatives inside their very own group in growing AI capabilities.
For members who could be eager about a profession in AI Advertising, this program will present an understanding and framework of AI and its fundamental functions in AI Advertising. Collectively, the initiatives and assignments on this program permit for a deeper and richer understanding of the potential of AI throughout the organizations wherein members need to work.
What's one tip for individuals beginning this system?
Members ought to come ready to work together and have interaction with the course materials and friends throughout the program. This may permit for members to form and develop distinctive views and study from others experiences inside this program. Lastly, members ought to include a curious mindset to study and contribute to significant discussions and interactions within the program. | eng | 524ba284-d8b2-49ab-aa05-aae4a0a47457 | https://younicheblogs.com/a-qa-with-ai-uva-professor-rajkumar-venkatesan/ |
How Much Should My Baby Weight At 5 Months Pregnant Pregnancy Foods to Avoid
You are searching about How Much Should My Baby Weight At 5 Months Pregnant, today we will share with you article about How Much Should My Baby Weight At 5 Months Pregnant was compiled and edited by our team from many sources on the internet. Hope this article on the topic How Much Should My Baby Weight At 5 Months Pregnant is useful to you.
Pregnancy Foods to Avoid
Every responsible mother-to-be should consider what pregnancy foods to avoid in order to ensure the well-being of her growing baby. Research has shown that birth defects have increased dramatically over the past 5 decades and there is a proven link between poor pregnancy diet and birth defects. Eating the wrong foods can increase the chances of low birth weight, poor fetal development and miscarriage.
The first thing every mother should realize is that she is now eating for two people. Her baby is completely dependent on her to get all the nutrients it needs. This is why the pregnancy diet is so important for the health of the baby. The second thing to realize is that a good pregnancy diet is easy to understand once you understand the basics, which are that it consists of a good balance of vitamins, minerals, carbohydrates, proteins, fats and folic acid. These can be obtained from wholesome healthy foods. Avoid unhealthy foods such as junk food, fast food and processed foods as these foods have low nutritional value and will not benefit you and your baby.
So what are the best pregnancy foods to avoid? The following is a list of foods that are best avoided to ensure a healthy pregnancy.
Fish: Fish is an excellent source of protein, iron and omega 3 fatty acids, all of which are essential for the healthy development of your baby, so why is fish on the list of pregnancy foods to avoid? Some fish are known to contain high levels of mercury, which can be very harmful to your baby's brain and nervous system development. Such fish are mainly large fish such as shark, swordfish, king mackerel and tilefish.
Raw eggs: Contains salmonella, which is a dreaded bacteria. To avoid a bacterial infection like food poisoning, it's best to include raw eggs and anything made from them, such as mayonnaise and salad dressings, on your list of pregnancy foods to avoid.
Liver: Liver is highly regarded as a rich source of nutrients and is excellent when consumed in moderation. However, it is very high in vitamin A, and excess vitamin A can cause problems for the baby.
Raw meat: Raw meat and fish can contain high levels of bacteria such as toxoplasmosis, salmonella and forma coli, and to avoid food poisoning and other infections, it's best to eliminate your favorite sushi and rare steaks from your diet for 9 months!
Artificial Sweeteners: Saccharin and aspartame are the two most commonly used sweeteners today and have been linked to causing birth defects and many other problems in the unborn child. Make sure this item is high on your list of pregnancy foods to avoid.
Alcohol: There is no definitive research to show how much alcohol is permissible during pregnancy, so if in doubt, stop!
Junk Food: As stated above, this food is highly processed and has very little nutritional value and will not benefit you or your baby.
Put all these items on your list of pregnancy foods to avoid and you will be well on your way to ensuring that your baby develops normally and is born healthy and fit.
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#Pregnancy #Foods #Avoid | eng | fd41b75b-d7d4-46a4-93d5-772ad6c814b4 | https://darcy2012.com/how-much-should-my-baby-weight-at-5-months-pregnant-pregnancy-foods-to-avoid/ |
Once you have listened to the musical selection, you are to …
Once you have listened to the musical selection, you are to write approx. two paragraphs and describe the music. In the first paragraph, describe what you hear…the instruments, meter, timbre, dynamics, form…etc…Use previous musical terminology that you have learned. In the second paragraph tell me if you like or dislike the piece…why? Does it remind you of a movie, school music program, tv, wedding, etc….Is there any particular mood that the piece conveys? Every person will hear something different. The point of this exercise is evaluate your ability to hear and recognize different musical qualities in a piece.
| eng | 81aa080c-1da9-4046-b5d9-65dec9fa879a | https://myassignmentwriters.org/once-you-have-listened-to-the-musical-selection-you-are-to/ |
$60
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You can request another time or scroll down to find more classes like this.
Description
Class Experience
During this course, students draw several different cute, cartoon characters.
Suggested weekly themes (although class is per student's requests):
DAY 1: Space & Weather
DAY 2: Foods
DAY 3: Animals
DAY 4: Plants & Nature
Children have fun with Rozine's curriculum which includes seasonal pop art, cartooning, and graphic design.
Rozine will guide students step by step, stacking basic geometric shapes with pencil until the basic shape of the character is established. Cute, cartoon details,...
Since 2005, Rozine taught cartooning classes to elementary-aged, inner-city children in Chicago and Los Angeles. She is the illustrator, author, and publisher of several all-age coloring activity books. She creates a relaxing atmosphere, encouraging connection amongst others, as well as confident self-expression.
Upon parent approval, students complete their piece by outlining everything with Sharpie markers. Instead of Sharpie, black marker, colored pencil, or crayon can be used. Many students simply color in their pencil drawings. For extra-credit, create background environments for characters to live in optional. Students can frame their artwork by stapling or taping it to a larger sheet of colored construction paper (also optional).
Learners will not need to use any apps or websites beyond the standard Outschool tools.
Students are encouraged to share their work with Rozine and other learners, by holding their artwork up to the camera after each character is drawn. Praise and recognition is awarded, regardless of skill level. Rozine stresses the importance of each artist liking their own work—and if they see something they don't like, she motivates them to find the solution to fix the problem. Suggested fixes are offered if the student struggles.
45 minutes per week in class, and an estimated 1 - 2 | eng | 25df3ead-33dd-47d3-9044-045dfef64798 | https://outschool.com/classes/monthly-art-camp-drawing-cute-cartoon-characters-XSPDusK7 |
Apartment moving
Boston Small Moves - A Hassle-Free Solution for Apartment Moving
Moving to a new apartment can be an exciting but overwhelming experience. The excitement of new surroundings and a fresh start is often overshadowed by the stress of packing, transporting, and unpacking all your belongings. However, with Boston Small Moves, apartment moving has never been easier.
Boston Small Moves is a local moving company that specializes in apartment and small move services. They understand that moving can be a daunting task, especially in a busy city like Boston. Their team of experienced and skilled professionals is committed to providing a stress-free moving experience for their clients.
When you choose Boston Small Moves, you can be sure that your belongings are in safe hands. They use top-of-the-line equipment and materials to ensure that your items are packed securely, loaded and transported with care, and delivered to your new home on time.
One of the biggest advantages of Boston Small Moves is their personalized service. Unlike larger moving companies that handle multiple moves at once, they focus solely on your move and cater to your specific needs. They work closely with you to plan every aspect of the move, from packing to unpacking, to make sure that everything goes smoothly.
The team at Boston Small Moves understands that every move is unique and requires individual attention. That's why they offer a range of services that can be customized to fit your specific requirements. Whether you need help packing and unpacking, furniture assembly and disassembly, or simply transportation services, Boston Small Moves has got you covered.
Their competitive pricing structure is another highlight of their service. They offer affordable rates without compromising on the quality of their work. Additionally, they provide a free, no-obligation quote, so you know exactly what to expect and can plan your budget accordingly.
In summary, Boston Small Moves is a reliable, affordable, and personalized solution for apartment moving in Boston. With their expert guidance and support, you can make your move stress-free and enjoyable. Contact them today to schedule your move and experience the difference for yourself!
Our Services
When it comes to small moves in Boston, there are plenty of options to choose from. But if you want a smooth and hassle-free move, then Boston Small Moves should be your go-to small moving company. Here's why:
1. Expertise in small moves: As small moving experts, Boston Small Moves has a deep understanding of the unique challenges that come with small moves. They have mastered the art of small moving and can help you with any type of move, whether it's a studio apartment, a one-bedroom condo, or a small office.
2. Tailored solutions: One of the best things about small movers is that they offer tailored solutions for each customer. They understand that every move is unique and can customize their services to meet your specific needs and requirements.
3. Affordable pricing: Moving can often be expensive, but with Boston Small Moves, you can rest assured that you'll get a fair and affordable price. They offer competitive rates that won't break the bank, even if you're on a tight budget.
4. Quality service: Boston Small Moves takes pride in providing exceptional service to each and every customer. They use high-quality packing materials, have trained and experienced movers, and employ best practices for safe and efficient moving.
5. Convenient scheduling: Small moves often require flexible scheduling, and Boston Small Moves can accommodate your needs. Whether you need to move on a weekend or a holiday, they will work with you to find the best time for your move.
Overall, Boston Small Moves is a reliable, affordable, and customer-focused small moving company that will make your small move in Boston stress-free and easy. So if you're planning a small move, don't hesitate to contact them for a quote today! | eng | f27cc3d5-4975-4f96-ae20-366583496cd4 | https://boston-smallmoves.com/apartment-moving-1 |
Arts and Music posts
Understand Guitar Tab Simply
Learn Guitar Tab, because it is the simplest method for training yourself how to play the amazing stringed instrument. I will never forget the first time I heard the term "tab." All I could think of was that small part found on the top of a soda can. However, what I wasn't aware of was the undeniable fact that just 10 minutes of quick research would unlock the world of guitar for me.
Guitar tab is a straightforward system that uses numbers to represent notes. I may not be able to provide you with the best through mere words, but at least I can give you a general idea of how this system works. On the guitar neck, you will find something called a fretboard. The fretboard is where you see people placing their fingers to produce chord sounds.
On the fretboard, there are several small metal strips that run from top to bottom. The spaces between these metal strips are called frets. If you look at the guitar neck, you can count a series of fret spaces from left to right. You will also notice that these frets become smaller as you move up the neck. If you were to label them from left to right, you would say "1, 2, 3, 4, etc." Well, each fret is also represented by a number in guitar tab.
The guitar has six strings. In tablature, each string is represented by a line. These lines are stacked on top of each other, resembling the guitar neck. A number may appear on a specific line, indicating which fret to play and on which string.
There are other symbols that represent how to produce specific sounds, and this, in many ways, makes playing the guitar more expressive than using traditional musical notation. There are various symbols and details to understand, but again, all of this can be learned and mastered in just a few minutes. Learning to read and write using tab as a substitute for traditional notation is step one in unlocking and understanding the guitar for anyone | eng | f099d65b-6f2f-401f-a54c-0ff2809fb2e6 | https://manuelmarino.com/blog/understand-guitar-tab-simply/ |
Present indefinite tense pdf download for ssc cgl
SSCResult.in: This article on Present Indefinite Tense Rules in Hindi PDF Free Download is prepared for SSC Examinations. Tenses exercise hindi to english pdf is very important to crack SSC Competitive exams. Best present indefinite tense in hindi PDF Notes designed according to SSC Latest Syllabus.
Tense chart with rules and examples pdf: Staff Selection Commission released the SSC Exam calendar so download Present Indefinite Tense Rules in Hindi PDF Free Download ebook and start your preparation. You can find many simple present tense story pdf in hindi study materials for the SSC Exams Preparation but choosing the best tense chart pdf download one is the big task. We at SSCResult.in provide the best tense in hindi example study material for all SSC Exams.
Present Indefinite Tense Rules in Hindi PDF Free Download: Hello my dear friends, This post is all about tense chart in hindi pdf download, This PDF of tenses in english grammar chart with examples pdf will help you to boost your score in SSC Exams. However, This tense notes in english pdf download is very important to Crack SSC CGL, CHSL (10+2) and CPO Sub Inspector (SI) Exams. Also this tense pdf book will be helpful for SSC Junior Engineer (JE), Stenographer and SSC JHT.
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SSC Exams News, Class Notes and Books PDF
As you know, we have already shared Present Indefinite Tense Rules in Hindi PDF Free Download in PDF Format. You can download this tense chart book pdf and read this english tense chart in hindi pdf book to boost your preparation. In below table you will get SSC News and Study material (present past & future tense chart pdf download | eng | 8b183f92-bf00-45c5-b979-f522d63efe5e | https://sscresult.in/present-indefinite-tense-rules-in-hindi-pdf-free-download/ |
Our past means a lot to us. Our past actions determine our present state, and our present actions determine our future state. So to some extent, the past is relevant for us. We can learn from the past, but we cannot waste our present thinking about it too much.
In this post, we are sharing the list of 81 Quotes about the past that will help you to learn from your past but focus on your present.
Inspirational Quotes About Past
1. "The past is never where you think you left it." ― Katherine Anne Porter
2. "We are products of our past, but we don't have to be prisoners of it." ― Rick Warren
9. "We don't have to be defined by the things we did or didn't do in our past. Some people allow themselves to be controlled by regret. Maybe it's a regret, maybe it's not. It's merely something that happened. Get over it." ― Pittacus Lore
10. "Memories are dangerous things. You turn them over and over until you know every touch and corner, but still, you'll find an edge to cut you." ― Mark Lawrence
Do not live in the past quotes
12 ― Sarah Breathnach
15. "Sometimes in order to appreciate your future, you must remember the past." ― Dennis E. Adonis
16. "Our past may explain why we're suffering but we must not use it as an excuse to stay in bondage." ― Joyce Meyer
17. " ― Paulo Coelho
18. "The past can teach us, nurture us, but it cannot sustain us. The essence of life changes, and we must move ever forward or the soul will wither and die." ― Susanna Kearsley
Past Quotes to live in the present
19. "Yesterday is gone. Tomorrow has not yet come. We have only today. Let us begin." ― Mother Theresa
20. "Yesterday is history, tomorrow is a mystery, today is a gift of God, which is why we call it the present." ― Bill Keane
21. "The present changes the past. Looking back you do not find what you left behind." ― Kiran Desai
22. "Don't live in the past – you've already been there. And don't live in the future, either. Tomorrow will be here soon enough. Live in this moment now – it is sacred and unrepeatable. This moment alone holds valuable gifts that should not be missed." ― Steve Goodier
23. "The past is a ghost, the future a dream and all we ever have is now." ― Bill Cosby
24. "One cannot and must not try to erase the past merely because it does not fit the present." ― Golda Meir
Past Quotes related to future
28. "You cannot harden your heart to the future just because of your past. You cannot use cruelty against yourself to justify cruelty to others." ― Marie Lu
29. "With each passing moment I'm becoming part of the past. There is no future for me, just the past steadily accumulating." ― Haruki Murakami
30. "No people whose word for 'yesterday is the same as their word for 'tomorrow' can be said to have a firm grip on the time." ― Salman Rushdie
31. "Once your past no longer has the power to define you, your future is, quite literally, yours for the taking. Every single beautiful thing you could possibly want or imagine will be yours." ― Dan Pearce
Forget the past quotes
32. "For most of the people there is no today and there is no tomorrow; for them, there are only the past times! Leave your past to live your today and to live your tomorrow!" ― Mehmet Murat ildan
33. "The success of the future does not lie solely on the safety of the past, but relies broadly on the security of the present." ― Israelmore Ayivor
34. "Always choose the future over the past. What do we do now?" ― Brian Tracy
35. "Some people read palms to tell your future, but I read hands to tell your past. Each scar makes a story worth telling. Each callused palm, each cracked knuckle is a missed punch or years in a factory." ― Sarah Kay
36. "People don't realize that the future is just now, but later." ― Russell Brand
Letting go of the past quotes
37. "It is not until you change your identity to match your life blueprint that you will understand why everything in the past never worked." ― Shannon L. Alder
38. "You can't clean your dirty past as if you are cleaning a dirty window! All you can do is to create a clean future!" ― Mehmet Murat ildan
39. "The past is far behind. If you still want to look at it, you will painfully stretch your neck muscles. Don't live in the past, leave the past, but learn from it." ― Israelmore Ayivor
40. "People don't exist without the past, I know. But the past isn't alive. It's you who's alive." ― SHOOWA
41. "I can't change the past, but that doesn't mean I can't learn from it. I can't the future, but that doesn't mean I can't be ready for it." ― Kenneth de Guzman
42. "Your past is a place for reference, not residence." ― Ifeanyi Enoch Onuoha
43. "The past is like a deceased person. It has to be remembered." ― Jake Gallardo
44. "Don't reside in the past. Instead, refer to it, else you will remain in the remand of high demand but with low command" ― Israelmore Ayivor
45. "People are trapped in history and history is trapped in them." ― James Baldwin
46. "History is the version of past events that people have decided to agree upon." ― Napoleon Bonaparte
47. "If you want to fly on the sky, you need to leave the earth. If you want to move forward, you need to let go of the past that drags you down." ― Amit Ray
48. "Yesterday was the last day on the calendar of the past. Tomorrow will be the first day on the calendar of the future. Today is both the first and the last day of the present. Use it well." ― Israelmore Ayivor
49. "Living in the past, can only hold those who live there, as its prisoners." ― Ellen J. Barrier
50. "Past has a very great superiority over the future: The future may not exist, but the past existed!" ― Mehmet Murat ildan
51. "Don't swear at your past; you couldn't exist without it! It is the only path to reach today and tomorrow! Remember that past is a great teacher who thought us all we know now!" ― Mehmet Murat ildan
52. "Every lesson you take from your past immediately turns into stairs to the light!" ― Mehmet Murat ildan
53. "You couldn't erase the past. You couldn't even change it. But sometimes life offered you the opportunity to put it right." ― Ann Brashares
54. "You can never go back to a specific moment. That's why it's important to live in the present and not the past. Don't let foolish memories get in the way of the makings of new ones." ― Emily Coussons
Motivational Past Quotes
57. "My yesterday walk with me. They keep step, they are gray faces that peer over my shoulder." ― William Golding
58. "The past was always there, lived inside of you, and it helped to make you who you were. But it had to be placed in perspective. The past could not dominate the future." ― Barbara Taylor Bradford
59. "The past is a cupboard full of light and all you have to do is find the key that opens the door." ― Kate Atkinson
60. "The only thing new in the world is the history you do not know." ― Harry S. Truman
61. "Those who cannot remember the past, are condemned to repeat it." ― George Santayana
62. "I want everything back, the way it was. But there is no point to it, this wanting." ― Margaret Atwood
63. "Change is the law of life. And those who look only to the past or the present are certain to miss the future." ― John F. Kennedy
64. "People who say that yesterday was better than today are ultimately devaluing their own existence." ― Karl Lagerfeld
65. "There is no present or future-only the past, happening over and over again now." ― Eugene O'Neill
66. "The past was gone and the future had yet to unfold, and he knew he should focus his life on the present…yet his day-to-day existence suddenly struck him as endless and unbearable." ― Nicholas Sparks
67. "When the past is forgotten, the present is unforgettable." ― Martin Amis
68. "The past always seems better when you look back on it than it did at the time. And the present never looks as good as it will in the future. It's depressing if you spend too much time reliving old joys. You think you'll never have anything as good again." ― Peter Benchley
69. "Yesterday was a beautiful tune on the lips of life and today is a silent secret." ― Kahlil Gibran
70. "The historical sense involves a perception, not only of the pastness of the past but of its presence." ― T.S. Eliot
71. "You can only predict things after they have happened." ― Eugène Ionesco
72. "What our parents tell us when we are small seldom goes ignored, no matter how foolish it may be" ― Stephen King
73. "No past to make us sentimental, no future to embarrass us…a difficult moment when you are out of practice – a moment that makes you go cold, cold and wary." ― Jean Rhys
74. "Your past has already been written and the words cannot be changed, but your future is waiting to be written; make it a bestseller." ― Abigail Landsbrook
75. "The past does not define me, it ignites me. The past is not a piece of me, it has placed me." ― Ricky Maye
76. "You can't change the things you've done. It's now and the here on out you've got control of." ― Mindy McGinnis
77. "Where you come from, what you look like, and what your past holds do not define you as an individual–you are what you make yourself to be." ― Kat Von D
78. "Yesterday is the history chapter in the book of life, isn't it time you turned the page?" ― Rob Liano
79. "Just because the past didn't turn out as you wanted it to, doesn't mean the future can't be better than you ever imagined." ― Ziad K. Abdelnour
80. "The past is devoid of meaning like the present, and a refuge for cowards." ― E.M. Forster
81. "To use the past to justify the present is bad enough—but it's just as bad to use the present to justify the past." ― Amitav Ghosh
I hope you liked the above Inspiring Past Quotes& Sayings. Don't forget to mention the best line that you liked most from the above lines in the comment box below. | eng | e2cd4d02-8ff7-430b-97d4-1c5d7992ebb4 | https://findmotivation.org/inspiring-past-quotes/ |
What Is Rutherford's Atomic Model Theory?
Rutherford's Atomic Model Theory is a fundamental concept in the field of Chemistry. It is named after the eminent physicist Ernest Rutherford, who proposed this theory in 1911.
The Basic Concept
The Rutherford Atomic Model Theory is based on the concept that an atom has a central nucleus that is positively charged, surrounded by negatively charged electrons that revolve around it in fixed orbits. This model was proposed after the discovery of the atomic nucleus by Rutherford and his team through their famous gold foil experiment.
The Gold Foil Experiment
In the gold foil experiment, a thin sheet of gold was bombarded with alpha particles. The alpha particles were expected to pass straight through the gold sheet since they were positively charged and should have been repelled by any positive charges in the atoms of gold. However, some alpha particles deflected at large angles or even bounced back towards their source.
This led Rutherford to conclude that there must be a central nucleus in every atom that contains most of its mass and positive charge since only a small fraction of alpha particles experienced such deflections. He suggested that electrons orbited around this central nucleus like planets orbiting around the sun.
The Advancements Over Thomson's Model
Before Rutherford's discovery, J.J. Thomson had proposed an atomic model known as the Plum Pudding Model which suggested that an atom was a uniform sphere with negative charges embedded within it, like plums in a pudding.
Rutherford's model improved upon Thomson's model by suggesting that most of an atom's mass and positive charge were concentrated in its nucleus, while electrons revolved around it in fixed orbits.
Limitations Of The Model
Although Rutherford's Atomic Model provided significant insights into atomic structure, it had certain limitations as well. One such limitation was its inability to explain why electrons did not lose energy while revolving around the nucleus, leading to their eventual collapse into it. This led to the development of the Bohr Atomic Model, which proposed that electrons revolve around the nucleus in specific energy levels.
Conclusion
To sum up, Rutherford's Atomic Model Theory was a landmark discovery in the field of Chemistry. It provided insights into atomic structure and paved the way for further advancements in this field. Despite its limitations, it remains an important concept in Chemistry and is still studied widely today.
Rutherford's Atomic Model Theory proposed that an atom has a central nucleus that is positively charged
The theory was based on the gold foil experiment which led Rutherford to conclude that most of an atom's mass and positive charge were concentrated in its nucleus
The model improved upon Thomson's Plum Pudding Model by suggesting that electrons orbited around a central nucleus
However, it had limitations such as its inability to explain why electrons did not lose energy while revolving around the nucleus
5 Related Question Answers Found
The atomic model theory has evolved significantly over the past few centuries, with various scientists contributing to its development. The current atomic model theory is based on quantum mechanics and provides us with a deeper understanding of the properties and behavior of atoms. What is an Atom?
In the early 20th century, scientists were trying to understand the structure of atoms. One of the most important discoveries during this time was made by Ernest Rutherford, a New Zealand physicist. Rutherford's experiments led to a significant change in our understanding of atomic theory. | eng | ad8b8753-3d95-4825-9507-5381fa227779 | https://strangeherring.com/what-is-rutherfords-atomic-model-theory/ |
Praying with Children
Praying with Children is designed not only for Children's Liturgy of the Word celebrated at Sunday Mass in the parish but also for families with young children to use at home. Schools can also use each week's resources to explore the coming Sunday's gospel at school.
Each week's resource includes an extract from the Sunday gospel in the Children's Lectionary translation, along with some reflection questions, music for gathering, psalm and gospel acclamation, family activities, a short video to watch and a worksheet for children. | eng | c9a6826a-8e37-4215-ad00-244f8d4fc519 | https://liturgybrisbane.net.au/resources/praying-with-children/ |
De Cecco #41 Penne Rigate Bulk Pasta, 5 lb.
Description
De Cecco Penne Rigate Pasta is a tube-shaped and "pen-shaped" Italian pasta. Penne Rigate is a classic Italian pasta. Because Penne Rigate has a tube-shape, it can retain flavors of sauce and seasoning. | eng | a47a8edc-c74d-4597-995e-7b3cbab887fa | https://supermarketitaly.com/products/de-cecco-41-penne-rigate-bulk-pasta-5-lbs |
The cracks were now quite pronounced and spread out to the distant front of the steep escarpments which was where the prince was supposed to be going. Further ahead, it looked as though the Mountain pass would cave in at any moment, however, this was not the same for the back of the gorge.
Coincidentally, Drake was standing at the centre of this chaos, his destination riddled with uncertainty, yet the start of the gorge still looked perfectly safe.
Looking back, the prince could see that he'd already run a decent distance, however, it was nothing compared to what he had left to travel. 'Is there some other way to cross the mountains without going around them? That trip would be far too long and I'm sure my speed devil of a sister could make it in much less time than I ever could…'
"Ugh, why do you have to be such a worthy adversary, Lina?" he screamed internally. To the standby observer, this large black and white wolf was howling in frustration.
The wolf hung its head low to the ground in desperate thought, but his decision was soon made for him as a low groaning sound made it to his keen sense of hearing. 'I just had to open my big mouth…'
One more crack but this time in the direction he just come was enough for him to tell him that the Mountain pass was completely unsafe. As if confirming his conclusion, the mountain groaned with more cracks riddling the two walls of the crumbling gorge… It was coming down.
The prince turned on his heels, "Why now of all times… you've been standing for centuries… Oh, goddess of the moon that lights up the night sky, I was not meant to die like this… My Little Sister will think she's better than me."
…………..
"Wyatt, wake up… it's time to go. For goddess's sake, you sleep like a log," Crysta shook the alpha awake, trying to understand how one werewolf could sleep so much. It was the third time she was trying to wake him up in the same morning. After having tried to wake him up twice before sunrise.
…..
The sun was now out and clearly telling them how late they were. The two tents belonging to the princess and the delta had been neatly packed, but without being able to wake the alpha, it was impossible for them to work on packing his tent.
"Out of the way, Crysta," Lina growled furiously. The delta looked back and saw her friend walking up to her with a mischievous grin. There was a slight twitch in Royal's eye which made her look borderline insane and in her hand, she held one of their water cans… The same water cans that were supposed to sustain them till they got to the creek.
"No, Lina, we need that water. Him, most of all," Crysta tried.
"We'll get more water when we reach the stream. He, on the other hand, is wasting far more time than we can spare," Lina replied, trying to push past her friend and spill water on the sleeping alpha.
"We have to be smart about this, Lina. We don't know what the future holds. What happens when one of us gets injured and we can't make it to the stream as fast as you expect us to do?" the delta suddenly asked. It was a plausible scenario.
"No, that won't be happening," the Royal growled stubbornly, "Because we will make it to the finish line before my big brother and this one measly alpha won't slow us down any more than…"
"Lina, if it was Bree, would you do the same?" Crysta interrupted the rampaging Royal. Surprisingly, the princess wasn't forcing her way past her friend and the thought that she was holding back only lightly crossed Crysta's mind.
This statement, however, had a negative effect, "Bree knew what we were doing when we came on this journey. She would have woken up before I did and we would have already started our journey. In terms of consistency, she would be a much better travel companion," Lina fumed.
"But she's not here now and it's because she knew we would do better with him than we could with her…"
"Did she though? When we set off, none of us thought he prove weaker than you are. In fact, he made it seem like he was stronger than you," Lina argued, "At this rate, the colour of his eyes could be nothing but a fluke."
"Hearing that coming from you, of all people. My, how the tables have turned? How the might have fallen?" a male voice interrupted the quarrelling females.
Wyatt was standing with both backpacks assigned to him slung over his shoulders and the tent he'd been sleeping in already packed, "Maybe you would try to think of the weight of carrying these bags. I am not exactly running empty-handed here."
"Can you feel the weight of the bags when you shift?" Crysta was suddenly curious. It's not like she knew what it was like to have your belongings stay with you after a shift.
"Yes, yes, I can. And running with them for three-hour periods is even worse," the man replied with a yawn, "Now can we get going?"
Lina sighed and turned to the alpha, "I'm sorry for everything you just heard. I just don't want to lose to my dorky brother. I can already imagine the grin on his face when he finally says… 'You still have a little way to go, Little Sister.'"
Chuckling, "I don't consider him the type to brag. Although I see no shame in losing to your brother. He's tough to beat. In the last Royal games, he was able to go head-to-head with Cole Lycaon, the one people nicknamed The Impervious tank back in the day. So don't get yourself too worked up," Wyatt spoke up, seemingly unbothered by the insults that had been indirectly hurled at him during the girls' argument.
"I guess you're right about that, but…" Lina balled her fists, "I'll be the one going against Cole this year. All you've said would be true if I hadn't worked so hard to make myself powerful enough to face my brother. I can't lose to him. I refuse to lose to him."
The princess walked up to Wyatt and yanked a bag from one of his shoulders, slinging it over hers before shifting, "You better run like losing will kill you… because if it doesn't, I just might."
During Lina's conversation with Wyatt, Crysta hid behind a tree and changed out of her clothes before shifting. The tone in Lina's voice sent shivers down her spine. The Trials were getting Lina more worked up than the delta had ever seen her… ever.
She didn't know whether it was a good thing or a bad thing… to see Lina want to win something so badly. 'Could there be something Lina hasn't told me yet?'
Wyatt being the only one left in human form was tasked with packing Crysta's clothes before shifting into his black wolf himself.
In a few minutes, they were running again with Crysta leading the way. | eng | f9997002-2fb7-4060-b936-ac4b0da9915d | https://wereadnovel.com/the-moon-goddess-chosen/the-moon-goddess-chosen-chapter-421.html |
Fulfilling the Promise of the Affordable Care Act for the Latino LGBT Community
Since the Affordable Care Act (ACA) was signed into law, nearly 18 million Americans, including four million Latinos, have gained access to health care. This open enrollment period alone has seen well over two million signups, including more than 700,000 new consumers in the federal health insurance marketplace. While we have made a lot of progress, we must continue to reach out to all groups, especially within the Latino community, where one in five remains uninsured.
The lesbian, gay, bisexual, and transgender (LGBT) Latino population has long faced barriers preventing them from obtaining quality health care. The ACA works to address these disparities, providing important protections and benefits to ensure everyone in the LGBT community can access the care they need.
For many in LGBT community, living with HIV, diabetes, cancer, or other chronic conditions, presented a barrier to obtaining health services. A preexisting condition once meant someone could be legally barred from getting insurance, but thanks to the ACA, people with preexisting conditions can no longer be denied coverage.
To ensure everyone has the right to health care, recent civil rights protections in the ACA expressly prohibit discrimination on the basis of sex, race, class, age, disability, and now sexual orientation. The provision, known as Section 1557, applies nondiscrimination protections to all health programs that receive funding from the federal government. Plans sold through the federal health insurance marketplace are covered under this law, as are hospitals, clinics, and other health care providers. Federal programs like Medicaid and Medicare are all covered under this provision as well.
The ACA has helped Latino LGBT individuals gain access to the health care they deserve. NCLR remains committed to communicating what the ACA means for LGBT people and ensuring the promise and benefits of the ACA reach our entire community!
It is important to make sure you and your loved ones stay healthy in 2016. Open enrollment is in full swing and the deadline to get covered is January 31, 2016. To find a health plan that best fits your needs, head to healthcare.gov or CuidadoDeSalud.gov and get covered! | eng | bc119fbb-d080-4089-bd3d-05541c5b14f3 | https://unidosus.org/blog/2015/12/09/fulfilling-the-promise-of-the-affordable-care-act-for-the-latino-lgbt-community/ |
Education Plus Initiative: FAQs/Frequently asked questions
'Education Plus' is a high-level political advocacy initiative (2021-2025) for the empowerment of adolescent girls and young women and the achievement of gender equality in sub-Saharan Africa. The initiative calls for bold leadership by governments and decision-makers to rapidly scale up multi-sectoral policies, actions and smart investments to this end. 'Education Plus' is a response to the urgency of effectively preventing HIV among adolescent girls and young women in the region, among other avoidable threats to their survival, safety, well-being and agency that are fueled by gender inequalities and unequal power dynamics. The five-year initiative, launched at the 2021 Generation Equality Forum in Paris, is co-led by the heads of UNAIDS, UNESCO, UNFPA, UNICEF and UN Women. | eng | 0d0fc6f0-b34a-4b35-8701-a1d6ffd01969 | https://healtheducationresources.unesco.org/pt-pt/library/documents/education-plus-initiative-faqsfrequently-asked-questions |
Sodium benzoate is the sodium salt of benzoic acid. It is widely used as a food preservative and a pickling agent in the food & beverages industry. The rising demand for sodium benzoate in this industry is the major factor driving the growth of the North America sodium benzoate market. It is generally recognized as safe by the Food and Drug Administration (FDA) and allows up to a 0.1% concentration by weight when used in food products. Sodium benzoate is used in acidic foods such as salad dressings, carbonated drinks, pickles, jams and fruit juices, condiments, and frozen yogurt toppings to prevent spoilage caused by harmful microorganisms such as harmful bacteria, yeasts, and molds. It also helps maintain freshness in food by slowing down or preventing color, flavor, PH, and texture changes. Moreover, it acts as a bacteriostatic and fungistatic preservative in soft drinks and other beverages, which increases the acidic flavor and extend the product's shelf life. Sodium benzoate is commonly used as a preservative in many products to protect the food taste. For instance, the Coca-Cola Company uses it as an antimicrobial agent in Coca-Cola drinks.
The North America food & beverages industry is growing at a rapid pace. People consume packaged food products due to their hectic lifestyles, busy work schedules, and high disposable incomes. People prefer consuming on-the-go food and beverages to minimize the time required for preparing food at home. Moreover, packaged food products are growing in popularity among young consumers, and they are convenient to consume and have significant nutritional value. These factors are driving the demand for sodium benzoate across the food & beverages industry.
With new features and technologies, vendors can attract new customers and expand their footprints in emerging markets. This factor is likely to drive the North America sodium benzoate market at a notable CAGR during the forecast period.
The North America sodium benzoate market is bifurcated into application and country. Based on application, the North America sodium benzoate market is segmented into food and beverages, pharmaceuticals, cosmetics, agriculture, and others. In 2021, the food and beverages segment accounted for the largest revenue share. Based on country, the North America sodium benzoate market is segmented into the US, Canada, and Mexico. Further, the US held the largest market share in 2021.
Develop/modify business expansion plans by using substantial growth offering developed and emerging markets
Scrutinize in-depth North America | eng | 8635d42f-59a4-471b-8d02-d6b8bd4498d4 | https://www.businessmarketinsights.com/reports/north-america-sodium-benzoate-market |
computer peripherals | eng | 77726ff2-9b23-48ec-b100-c034b690f2fe | https://teo-tea.com/tag/computer-peripherals/ |
Should I rephase when quoting a theorem/definition?
Actually I would like to ask two questions and the answers may not be the same.
When writing a paper and if one need to introduce a definition, is it alright to just copy-paste from wikipedia/a textbook/a paper, or should one at least rephrase it a little bit?
If I need to copy a theorem from an old paper, is it better just to copy exactly the theorem as it is, or should I rephrase it to make it in harmony with my notation/modern terminology, etc.?
Answer
Well, there is no law against using copy-paste from any document unless it has a copyright (in which case even rephrasing is a form of plagiarism). If you think the original is too unclear, you could rewrite using your own terms, as long as you don't change the meaning (even slightly). If it is clear enough, it's best to copy it as it is. | eng | 98d8cc6a-8951-4998-82dc-65efebaaa6f2 | https://mathzsolution.com/should-i-rephase-when-quoting-a-theorem-definition/ |
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It took a long time for cleaning to be completed.Welcome to leave a message, welcome Catch bugs PS This is a mistake.
Senior brother only does bananas raise your blood sugar told him until he arrived risks with a gastrectomy and blood sugar at Zhuhai.The base period will understand. | eng | a086dc8d-ba5f-453a-9c19-6edc8e2504a6 | http://romeeternal.com/blood-sugar-test/risks-with-a-gastrectomy-27-and-blood-sugar/ |
Description
Description
Member's Mark Plus+ Alkaline Water is a brand of bottled water that comes in a pack of 18 bottles, each containing 1 liter of water. This water is alkaline, which means that it has a pH level greater than 7, making it less acidic than regular water. The exact pH level of Member's Mark Plus+ Alkaline Water may vary, but it is typically around 8.8.
According to the product description, this water is "infused with electrolytes and minerals for a crisp, clean taste." It is also claimed to help neutralize acid in the body and promote better hydration. The water is marketed as being a great choice for athletes or anyone who wants to stay hydrated and maintain a healthy pH balance.
About Brand
Member's Mark is a private label brand owned by Sam's Club, which is a membership-only retail warehouse club that is part of Walmart Inc. Member's Mark offers a wide variety of products across different categories, including food and beverages, household essentials, electronics, clothing, and more.
The brand is known for providing high-quality products at a value price point, and many of its products are manufactured by top suppliers in the industry. Member's Mark products often feature unique formulations or packaging that are exclusive to the brand.
Member's Mark offers a satisfaction guarantee on all its products, which means that if a customer is not completely satisfied with a product, they can return it for a full refund or exchange it for a different product.
Why Member's Mark Plus+ Alkaline Water 1Liter 18 pack
Member's Mark Plus+ Alkaline Water is marketed as a premium offering in the brand's lineup of bottled water products. The water is alkaline, which means that it has a higher pH level than regular water, typically around 8.8, making it less acidic. This higher pH level is believed to provide several potential health benefits, such as helping to neutralize acid in the body and promoting better hydration.
The water is also infused with electrolytes and minerals, which can provide additional benefits to the body. Electrolytes, such as sodium, potassium, and magnesium, are essential for proper hydration and maintaining the body's fluid balance. Minerals
Safety Guidelines
Check the expiration date: Make sure to check the expiration date on the bottles before consuming the water. Do not consume the water if it is past its expiration date.
Store the water properly: Store the water in a cool, dry place away from direct sunlight or heat sources. Avoid storing the water in areas with high humidity or extreme temperatures.
Check the seal: Before opening a bottle of water, check the seal to make sure it is intact. Do not consume the water if the seal is broken or damaged.
Keep the water clean: To avoid contamination, do not touch the inside of the bottle or the cap with your hands or any other object. Wash your hands before handling the bottles.
Do not reuse the bottles: Member's Mark Plus+ Alkaline Water bottles are meant for single use only. Do not reuse the bottles for other purposes, as they may harbor bacteria or other contaminants.
If you have any health concerns, consult with a medical professional: While alkaline water is generally safe for most people to drink, it is always a good idea to consult with a medical professional if you have any health concerns or medical conditions.
FAQs
What is the pH level of Member's Mark Plus+ Alkaline Water?
The pH level of Member's Mark Plus+ Alkaline Water is typically around 8.8, making it less acidic than regular water.
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Alkaline water has a higher pH level than regular water, typically between 7.5 and 9.5. Regular water has a neutral pH level of 7.0. Alkaline water is believed to have health benefits, such as helping to neutralize acid in the body and promoting better hydration.
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Yes, Member's Mark Plus+ Alkaline Water is safe to drink. The water is produced and packaged under strict quality control standards and is subject to testing to ensure its safety and purity.
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While there is limited scientific evidence to support the health benefits of alkaline water, some people believe that it can help with issues such as acid reflux, high blood pressure, and dehydration. However, more research is needed to confirm these claims.
Can I reuse Member's Mark Plus+ Alkaline Water bottles?
No, Member's Mark Plus+ Alkaline Water bottles are meant for single use only. Do not reuse the bottles for other purposes, as they may harbor bacteria or other contaminants. | eng | 8b029409-2c4b-4aff-978a-adc16b485127 | https://shopisense.com/product/members-mark-plus-alkaline-water-1l-18-pk/ |