charlieoneill/embedding-saes
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12473133 | [
"Arca-Sedda, M.",
"Capuzzo-Dolcetta, R."
] | 2016MNRAS.461.4335A | [
"Globular clusters as tracers of the host galaxy mass distribution: the Fornax dSph test case"
] | 17 | [
"Department of Physics, Sapienza, University of Rome, Piazzale Aldo Moro 5, I-00185 Rome, Italy",
"Department of Physics, Sapienza, University of Rome, Piazzale Aldo Moro 5, I-00185 Rome, Italy"
] | [
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"2021MNRAS.503..... | [
"astronomy"
] | 1 | [
"methods: numerical",
"galaxies: individual: Fornax",
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"10.1093/mnras/stw1647",
"10.48550/arXiv.1607.01526"
] | 1607 | 1607.01526_arXiv.txt | The Fornax galaxy is the brightest dwarf spheroidal galaxy (dSph) satellite of the Milky Way (MW) and is, among all of the MW satellites, the only one that hosts five globular clusters, located within $1$ kpc from its center, named Fornax 1,2,3,4 and 5. Moreover, Fornax does not show any bright nucleus. As the other M... | \label{end} In this paper we revisited the so called ``timing problem'' for the stellar clusters in the Fornax dwarf spheroidal galaxy. Using two complementary approaches, a simple semi-analytic investigation of the dynamical friction decay times and a more sophisticated and detailed series of numerical simulations for... | 16 | 7 | 1607.01526 | The Fornax dwarf spheroidal galaxy is the most massive satellites of the Milky Way, claimed to be embedded in a huge dark matter halo, and the only among the Milky Way satellites hosting five globular clusters. Interestingly, their estimated masses, ages and positions seem hardly compatible with the presence of a signi... | false | [
"cuspy density profiles",
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"Fornax",
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"five globular clusters",
"the globular clusters",
"direct N-body simulations",
"the Fornax GC system",
"a huge dark matter halo",
"a standard density profile",
"the Milky Way satellites",
... | 10.009286 | 7.42452 | 167 |
5209849 | [
"Colombo, S.",
"Orlando, S.",
"Peres, G.",
"Argiroffi, C.",
"Reale, F."
] | 2016A&A...594A..93C | [
"Impacts of fragmented accretion streams onto classical T Tauri stars: UV and X-ray emission lines"
] | 15 | [
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy",
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy",
"INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134, Palermo, Italy; Dipartimento di Fisica & Chimica,... | [
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"2019ASSP...55...29D",
"2019ASSP...55...43O",
"2019arXiv190409156D",
"2020A&A...640A.... | [
"astronomy"
] | 3 | [
"accretion",
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"ultraviolet: stars",
"Astrophysics - Solar and Stellar Astrophysics"
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"10.1051/0004-6361/201628858",
"10.48550/arXiv.1607.03009"
] | 1607 | 1607.03009_arXiv.txt | Classical T Tauri Stars (CTTS) are young stars surrounded by \salvo{an accretion} disk. \salvo{According to the magnetospheric accretion scenario, gas from the disk accretes onto the star through accretion columns \citep{1991Apj...370L..39K}. Several lines of evidence support this picture especially in the optical and ... | \label{sec4} In this work we investigated the effects of \salvo{stream fragmentation} on C\,IV and O\,VIII emission lines. We developed a model that describes \salvo{a stream composed by a series of dense blobs} impacting onto the surface of a CTTS. Our model \salvo{takes} into account the stellar magnetic field, the ... | 16 | 7 | 1607.03009 | Context. The accretion process in classical T Tauri stars (CTTSs) can be studied through the analysis of some UV and X-ray emission lines which trace hot gas flows and act as diagnostics of the post-shock downfalling plasma. In the UV-band, where higher spectral resolution is available, these lines are characterized by... | false | [
"line profiles",
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"C IV",
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"speed",
"shocked upflows",
"impact regions",
"several plasma components",
... | 9.324092 | 12.202207 | 147 |
12586989 | [
"Schmidtmann, Birte",
"Winters, Andrew R."
] | 2017JCoPh.330..566S | [
"Hybrid entropy stable HLL-type Riemann solvers for hyperbolic conservation laws"
] | 7 | [
"MathCCES, RWTH Aachen University, Schinkelstr. 2, 52062 Aachen, Germany",
"Mathematisches Institut, Universität zu Köln, Weyertal 86-90, 50931 Köln, Germany"
] | [
"2019JCoPh.378..477S",
"2019ShWav..29..755P",
"2020JCoPh.41609545T",
"2021ApJS..257...24L",
"2021ApJS..257...34F",
"2022JCoPh.46811521W",
"2023JCoPh.49312505H"
] | [
"astronomy",
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"10.1016/j.jcp.2016.10.034",
"10.48550/arXiv.1607.06240"
] | 1607 | 1607.06240_arXiv.txt | We consider the numerical solution of systems of hyperbolic conservation laws of the form \begin{equation} \label{eq:hypLaw} \pderivative{\vec{q}}{t} + \nabla\cdot\vec{f} = 0, \end{equation} on a domain $\Omega$. For a one-dimensional approximation we divide $\Omega$ into $K$ non-overlapping grid cells $C_i = [x_{i-1/2... | \label{scn:Conclusion} In this work we constructed two one-parameter families of hybrid entropy stable numerical fluxes. An advantage of the new numerical flux functions is that they remain applicable even when the eigenstructure of the flux Jacobian matrix is unknown. % The derivations and proofs in this work are kept... | 16 | 7 | 1607.06240 | It is known that HLL-type schemes are more dissipative than schemes based on characteristic decompositions. However, HLL-type methods offer greater flexibility to large systems of hyperbolic conservation laws because the eigenstructure of the flux Jacobian is not needed. We demonstrate in the present work that several ... | false | [
"hyperbolic conservation laws",
"entropy stability",
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"standard dissipation terms",
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"large systems",
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"dissipation",
"several HLL-type Riemann solvers",
"hybrid HLL-type methods",
"HLL-type schemes",... | 8.789782 | 4.468701 | 28 |
168897 | [
"Sayanagi, Kunio M.",
"Dyudina, Ulyana A.",
"Ewald, Shawn P.",
"Fischer, Georg",
"Ingersoll, Andrew P.",
"Kurth, William S.",
"Muro, Gabriel D.",
"Porco, Carolyn C.",
"West, Robert A."
] | 2013Icar..223..460S | [
"Dynamics of Saturn’s great storm of 2010-2011 from Cassini ISS and RPWS"
] | 74 | [
"Department of Atmospheric and Planetary Sciences, Hampton University, Hampton, VA 23668, USA; Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA",
"Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA",
... | [
"2013Icar..226..641L",
"2013Icar..226.1020D",
"2013JGRA..118.7246C",
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"2014Icar..241..313D",
"2014Icar..242..122T",
"2014MNRAS.444.1369H",
"2014Natur.505..625S",
"2015A&A...580A.... | [
"astronomy",
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] | 18 | [
"Astrophysics - Earth and Planetary Astrophysics"
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"10.1016/j.icarus.2012.12.013",
"10.48550/arXiv.1607.07246"
] | 1607 | 1607.07246_arXiv.txt | } Cumulus convecting storms on Saturn are known for their episodic behavior. Convective events on Saturn can be identified visually and through radio noise. The events occur intermittently within a small range of latitudes and are interspersed with quiescent periods that last for a year or longer \citep{Sromovsky_etal_... | We have reported the evolution of Saturn's latest planet-encircling storm of 2010-2011 using two of the instruments aboard Cassini spacecraft, ISS and RPWS. Our observational coverage enabled us to study the preconditions of the storm, in which we show that the storm erupted out of a previously known feature called the... | 16 | 7 | 1607.07246 | Saturn’s quasi-periodic planet-encircling storms are the largest convecting cumulus outbursts in the Solar System. The last eruption was in 1990 (Sánchez-Lavega, A. [1994]. Chaos 4, 341-353). A new eruption started in December 2010 and presented the first-ever opportunity to observe such episodic storms from a spacecra... | false | [
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"the SED radio signals",
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"Saturn’s quasi-periodic planet-encircling storms",
"RPWS",
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"... | 8.50624 | 15.511942 | 96 |
12408831 | [
"Leggett, S. K.",
"Cushing, Michael C.",
"Hardegree-Ullman, Kevin K.",
"Trucks, Jesica L.",
"Marley, M. S.",
"Morley, Caroline V.",
"Saumon, D.",
"Carey, S. J.",
"Fortney, J. J.",
"Gelino, C. R.",
"Gizis, J. E.",
"Kirkpatrick, J. D.",
"Mace, G. N."
] | 2016ApJ...830..141L | [
"Observed Variability at 1 and 4 μm in the Y0 Brown Dwarf WISEP J173835.52+273258.9"
] | 31 | [
"Gemini Observatory, Northern Operations Center, 670 N. A'ohoku Place, Hilo, HI 96720, USA",
"The University of Toledo, 2801 West Bancroft Street, Mailstop 111, Toledo, OH 43606, USA",
"The University of Toledo, 2801 West Bancroft Street, Mailstop 111, Toledo, OH 43606, USA",
"The University of Toledo, 2801 W... | [
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"2018haex.bookE..94A",
"2019A&A...629A.145E",
"2019ApJ...874..111T",
"2019ApJ...875L..15M",
"2019ApJ...877..... | [
"astronomy"
] | 10 | [
"brown dwarfs",
"stars: atmospheres",
"stars: individual: WISEP J173835.52+273258.9",
"Astrophysics - Solar and Stellar Astrophysics"
] | [
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"2010arXiv1008.4... | [
"10.3847/0004-637X/830/2/141",
"10.48550/arXiv.1607.07888"
] | 1607 | 1607.07888_arXiv.txt | There are now more than twenty brown dwarfs known in the solar neighborhood that have effective temperatures ($T_{\rm eff}$) lower than 500~K (Cushing et al. 2011, 2014; Kirkpatrick et al. 2012; Liu et al. 2012; Luhman 2014; Luhman, Burgasser \& Bochanski 2011, Pinfield et al. 2014; Schneider et al. 2015; Tinney et al... | We obtained 12 hours of continuous {\em Spitzer} data on the Y0 brown dwarf W1738 at [3.6], followed by another 12 hours at [4.5]. Two sets of data were obtained four months apart, on June 30 and October 30 2013. We also obtained interspersed Gemini $Y$ and $J$ data on W1738, with about 1.4 hours on-source at $Y$ and 2... | 16 | 7 | 1607.07888 | We have monitored photometrically the Y0 brown dwarf WISEP J173835.52+273258.9 (W1738) at both near- and mid-infrared wavelengths. This ≲1 Gyr old 400 K dwarf is at a distance of 8 pc and has a mass around 5 M <SUB>Jupiter</SUB>. We observed W1738 using two near-infrared filters at λ ≈ 1 μm, Y and J, on Gemini Observat... | false | [
"large features",
"associated small changes",
"surface temperature",
"-infrared wavelengths",
"significant evolution",
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"atmospheric models",
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"variability",
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"The mid-infrared light curves",
"the solar system gas giants",
"a ∼3.0 hr period",
"Gemini... | 7.209815 | 12.589618 | 102 |
12518466 | [
"Bentum, Mark J.",
"Bonetti, Luca",
"Spallicci, Alessandro D. A. M."
] | 2017AdSpR..59..736B | [
"Dispersion by pulsars, magnetars, fast radio bursts and massive electromagnetism at very low radio frequencies"
] | 28 | [
"Universiteit van Twente, Faculteit van Elektrotechniek, Wiskunde en Informatica, Telecommunication Engineering Postbus 217, 7500 AE Enschede, The Netherlands; ASTRON, Postbus 2, 7900 AA Dwingeloo, The Netherlands",
"Université d'Orléans, Observatoire des Sciences de l'Univers en région Centre, 1A rue de la Férol... | [
"2017ApJ...842...23Y",
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"2018PhRvD..97l4016C",
"2019EPJC...79..590H",
"2019PhRvD..99l4001C",
"2019arXiv191206288S",
"2020RAA....20..... | [
"astronomy",
"physics"
] | 6 | [
"Photons",
"Radio astronomy",
"Satellites",
"Pulsars",
"Magnetars",
"Fast radio bursts",
"Astrophysics - Instrumentation and Methods for Astrophysics",
"Astrophysics - High Energy Astrophysical Phenomena",
"General Relativity and Quantum Cosmology",
"High Energy Physics - Phenomenology"
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"10.1016/j.asr.2016.10.018",
"10.48550/arXiv.1607.08820"
] | 1607 | 1607.08820_arXiv.txt | For many years, many of us have worked, see {\it e.g.}, \cite{spalliccietal2005}, for the opening of one of the gravitational wave windows on the universe, that has finally occurred \cite{abbottetal2016}, while for other windows we still have to wait \cite{spallicci2013}. Nevertheless, we can genuinely state that even ... | We have focused on the interest raised by the newly operating and future ground and space detectors at very low radio frequencies. The foundations of electromagnetism could be tested, confirming our beliefs or else contributing to establish new physics. Studies on dispersion appear crucial to unveil the causes of the e... | 16 | 7 | 1607.08820 | Our understanding of the universe relies mostly on electromagnetism. As photons are the messengers, fundamental physics is concerned in testing their properties. Photon mass upper limits have been earlier set through pulsar observations, but new investigations are offered by the excess of dispersion measure (DM), somet... | false | [
"unknown origin",
"pulsar observations",
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"OLFAR",
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"new investigations",
"dispersion measure",
"stable conditions",
"the proposed Orbiting Low Frequency Antennas",
"solar maxima",
"new avenues",
"dispersion",
"terrestrial interference",
... | 6.506097 | 3.84499 | -1 |
12406228 | [
"Eistrup, Christian",
"Walsh, Catherine",
"van Dishoeck, Ewine F."
] | 2016A&A...595A..83E | [
"Setting the volatile composition of (exo)planet-building material. Does chemical evolution in disk midplanes matter?"
] | 146 | [
"Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands",
"Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands ; School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK",
"Leiden Observatory, Leiden University, PO Box 9513, 2300 RA,... | [
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"2018A&A...611A.... | [
"astronomy"
] | 12 | [
"astrochemistry",
"planets and satellites: formation",
"protoplanetary disks",
"planets and satellites: atmospheres",
"molecular processes",
"Astrophysics - Earth and Planetary Astrophysics"
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"10.1051/0004-6361/201628509",
"10.48550/arXiv.1607.06710"
] | 1607 | 1607.06710_arXiv.txt | \label{intr} The discovery of more than 2000 extrasolar planets by the radial velocity and transiting techniques \citep[e.g.,][]{udry2007,borucki2011,batalha2013,fischer2014} has signaled the next phase in exoplanet research: the characterization of their atmospheres. Simple molecules such as CO, \ce{H2O} and perhaps ... | \label{conclusions} The models presented in this work have examined the importance of kinetic chemistry on the molecular composition (gas and ice) in protoplanetary disk midplanes. The main conclusions are listed below. \begin{itemize} \item The disk midplane composition reflects that of interstellar ices only for t... | 16 | 7 | 1607.06710 | Context. The atmospheres of extrasolar planets are thought to be built largely through accretion of pebbles and planetesimals. Such pebbles are also the building blocks of comets. The chemical composition of their volatiles are usually taken to be inherited from the ices in the collapsing cloud. However, chemistry in t... | false | [
"SUB>2</SUB",
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"grain surfaces",
"CO",
"initial abundances",
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"atomic H",
"intermediate disk radii",
"ionisation level",
"high ionisation levels",
"CO<SUB>2</SUB>",
"gases",
"key volatile species",
"CO. H<SUB>2</SUB>O ice",
"chemical evolution",
"pr... | 9.99878 | 13.158843 | -1 |
2774767 | [
"Law, David R.",
"Cherinka, Brian",
"Yan, Renbin",
"Andrews, Brett H.",
"Bershady, Matthew A.",
"Bizyaev, Dmitry",
"Blanc, Guillermo A.",
"Blanton, Michael R.",
"Bolton, Adam S.",
"Brownstein, Joel R.",
"Bundy, Kevin",
"Chen, Yanmei",
"Drory, Niv",
"D'Souza, Richard",
"Fu, Hai",
"Jones... | 2016AJ....152...83L | [
"The Data Reduction Pipeline for the SDSS-IV MaNGA IFU Galaxy Survey"
] | 359 | [
"Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA",
"Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA",
"Department of Physics and Astronomy, University of Kentucky, 505 Rose Street, Lexington, KY 40506-0... | [
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] | 32 | [
"methods: data analysis",
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"10.3847/0004-6256/152/4/83",
"10.48550/arXiv.1607.08619"
] | 1607 | 1607.08619.txt | Over the last twenty years, multiplexed spectroscopic surveys have been valuable tools for bringing the power of statistics to bear on the study of galaxy formation. Using large samples of tens to hundreds of thousands of galaxies with optical spectroscopy from the Sloan Digital Sky Survey \citep{york00,dr1.ref} for i... | \label{summary.sec} The 13th data release of the Sloan Digital Sky Survey includes the raw MaNGA spectroscopic data, the fully reduced spectrophotometrically calibrated data, and the pipeline software and metadata required for individual users to re-reduce the data themselves. In this work, we have described the frame... | 16 | 7 | 1607.08619 | Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) is an optical fiber-bundle integral-field unit (IFU) spectroscopic survey that is one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV). With a spectral coverage of 3622-10354 Å and an average footprint of ∼500 arcsec<SUP>2</SU... | false | [
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12585901 | [
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"Dark matter directional detection: comparison of the track direction determination"
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] | 1607 | 1607.08157_arXiv.txt | Weakly interacting massive particles are among the most studied candidates for Dark Matter (DM). The direct search for DM is performed by looking for elastic collisions of these WIMPs with target nuclei in a detector~\cite{goodman_1985}. For a 1\,GeV/c$^2$ to 1000\,GeV/c$^2$ DM particle, the kinetic energy of the recoi... | \label{sec:discussion} Using SRIM simulations, we compared how the recoil primary direction information is preserved in the detector materials for three different strategies for a Dark matter directional detection: anisotropic crystals, emulsion layers and low-pressure gaseous TPCs. Anisotropic crystals do not allow an... | 16 | 7 | 1607.08157 | Several directional techniques have been proposed for a directional detection of Dark matter, among others anisotropic crystal detectors, nuclear emulsion plates, and low-pressure gaseous TPCs. The key point is to get access to the initial direction of the nucleus recoiling due to the elastic scattering by a WIMP. In t... | false | [
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12509827 | [
"Obata, Ippei",
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"Oscillating chiral tensor spectrum from axionic inflation"
] | 42 | [
"Department of Physics, Kyoto University, Kyoto 606-8502, Japan",
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] | 1607 | 1607.01847_arXiv.txt | Inflation can be regarded as magnifier which allows us to probe microscopic world, namely, high energy physics through the cosmic microwave background (CMB) anisotropies or the large scale structures of the universe. Indeed, it is important to explore high energy physics such as string theory by means of inflation. It ... | We studied the oscillatory feature of tensor spectrum from axionic inflation. In the case of single-field monodromy inflation, the modulation in tensor spectrum is too small to be detected by DECIGO or BBO. On the other hand, in the case of aligned chromo-natural inflation, we can get the sizable modulation in one heli... | 16 | 7 | 1607.01847 | We study axionic inflation with a modulated potential and examine if the primordial tensor power spectrum exhibits oscillatory feature, which is testable with future space-based gravitational-wave experiments such as DECIGO and BBO. In the case of single-field axion monodromy inflation, it turns out that it is difficul... | false | [
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2775537 | [
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] | 2016ApJ...827L..27P | [
"A High-velocity Cloud Impact Forming a Supershell in the Milky Way"
] | 10 | [
"Department of Physics and Astronomy, Seoul National University Seoul 151-747, Korea",
"Department of Physics and Astronomy, Seoul National University Seoul 151-747, Korea",
"Korea Astronomy and Space Science Institute Daejeon 305-348, Korea",
"Department of Physics and Astronomy, Western Kentucky University ... | [
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"10.3847/2041-8205/827/2/L27",
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] | 1607 | 1607.07699_arXiv.txt | \label{sec:intro} Supershells are large gaseous shells of radius greater than a few hundred parsecs. They are distinct from other shell-like structures in their extraordinarily large energy requirement, i.e., $\ga 3\times 10^{52}$~erg, which corresponds to $\ga 30$ supernova (SN) explosions \citep{heiles1979,heiles198... | \label{sec:disc} \subsection{Formation of GS040 by the Collision of CHVC040} \label{sec:disc_sub1} The location of CHVC040 at the geometrical center of GS040 suggests that their physical association is very likely. The centroids of the CHVC emission and that of the GS040's hub emission overlap within $\sim 0.2$~degr... | 16 | 7 | 1607.07699 | Neutral atomic hydrogen (H I) gas in interstellar space is largely organized into filaments, loops, and shells, the most prominent of which are “supershells.” These gigantic structures, which require ≳ 3× {10}<SUP>52</SUP> erg to form, are generally thought to be produced by either the explosion of multiple supernovae ... | false | [
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4552757 | [
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"Oh, Kyuseok"
] | 2016MNRAS.461.4505J | [
"Diffuse gas in retired galaxies: nebular emission templates and constraints on the sources of ionization"
] | 28 | [
"Max-Planck Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany; Department of Biological and Environmental Sciences, University of Gothenburg, Medicinaregatan 18, SE-40530 Gothenburg, Sweden",
"Max-Planck Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85741 Garching, Germany; M... | [
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"10.1093/mnras/stw1668",
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] | 1607 | 1607.02243_arXiv.txt | 16 | 7 | 1607.02243 | We present emission-line templates for passively-evolving (`retired') galaxies, useful for investigation of the evolution of the interstellar medium in these galaxies, and characterization of their high-temperature source populations. The templates are based on high signal-to-noise (>800) co-added spectra (3700-6800... | false | [
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12410206 | [
"Shirokov, S. I.",
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"Gorokhov, V. L."
] | 2016ARep...60..563S | [
"Large-scale fluctuations in the number density of galaxies in independent surveys of deep fields"
] | 8 | [
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University, St. Petersburg, Russia",
"Saint-Petersburg State University of Architecture and Civil Engineering, St. Petersburg, Russia"
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"10.1134/S1063772916040107",
"10.48550/arXiv.1607.02596"
] | 1607 | 1607.02596_arXiv.txt | Modern observational cosmology has led to the discovery of very large structures with scales of order 100 Mpc in the spatial distribution of galaxies in the local Universe, at redshifts $z \sim 0.1$, and also in the spatial distribution of quasars at redshifts $z \sim 2$ $[1-6]$. Over the last decade, observations of t... | Our analysis of the radial distribution of galaxies in the COSMOS/UVISTA field shows that the real observed fluctuations in the spatial distribution of the galaxies appreciably exceed the predictions of the $\Lambda$CDM model for the evolution of non-baryonic dark matter, in both their amplitude and linear size. This m... | 16 | 7 | 1607.02596 | New arguments supporting the reality of large-scale fluctuations in the density of the visible matter in deep galaxy surveys are presented. A statistical analysis of the radial distributions of galaxies in the COSMOS and HDF-N deep fields is presented. Independent spectral and photometric surveys exist for each field, ... | false | [
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... | 11.750803 | 3.459156 | -1 |
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