Identifier stringlengths 37 82 | Paragraph stringlengths 1.95k 9.23k | Citation Text list | Functions Text list | Functions Label list | Citation Start End list | Functions Start End list |
|---|---|---|---|---|---|---|
2020AandA...635A.121M__Casassus_et_al._2018_Instance_1 | As scattered light imaging is sensitive to the stellar irradiation, it allows one to search for misalignments between various disk regions. While studying the morphology of the innermost disk region is challenging due to its very small radial extent, often marginally resolvable by optical interferometry (Lazareff et al... | [
"Casassus et al. 2018"
] | [
"In this scenario, depending on the misalignment angle, the outer disk image will show narrow shadow lanes (e.g.,"
] | [
"Compare/Contrast"
] | [
[
610,
630
]
] | [
[
434,
546
]
] |
2021MNRAS.507.4367C__Mazzali_et_al._2005_Instance_1 | In the previous section, we discussed how SNe Ia with blueshifted Na i D have broader light curves but this may be driven by their preference for late-type host galaxies and their differing environments. One of the main aims of this study was to investigate, for the first time, if there is a connection between the pres... | [
"Mazzali et al. 2005"
] | [
"The reason that high-velocity features are interesting to investigate in connection with blueshifted Na i D features is that there are suggestions that the high-velocity Ca ii features may be at least partially due to ejecta–CSM interaction (e.g.",
"Therefore, if a link between these quantities was identified, i... | [
"Motivation",
"Motivation"
] | [
[
1024,
1043
]
] | [
[
777,
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[
1066,
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]
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2019MNRAS.486.4671M__Webb_&_Hundhausen_1987_Instance_1 | CMEs are known for large-scale expulsion of magnetized plasma structures from closed magnetic field regions on the Sun. They were first detected in the coronagraphic images taken in 1971 by NASA’s OSO-7 spacecraft (Tousey 1973). However, some definite inferences for the solar wind (Eddington 1910; Birkeland 1916; Bierm... | [
"Webb & Hundhausen 1987"
] | [
"CMEs have been observed to occur often having spatial and temporal relation with solar flares, eruptive prominences"
] | [
"Background"
] | [
[
997,
1019
]
] | [
[
861,
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]
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2021AandA...646A..67W__Widrow_et_al._2014_Instance_1 | We consider time-varying dynamical effects, breaking the assumption of a steady state, to be the most probable reason for this unexpected result. We do see how local phase-space substructures can bias our result for individual stellar samples, most clearly for those of area cell B8. However, explaining the steep gravit... | [
"Widrow et al. 2014"
] | [
"In order to produce a steep gravitational potential at low |z|, there could be a breathing mode in the stellar disk",
"which is currently in its most compressed state."
] | [
"Uses",
"Uses"
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2016AandA...587A.159G__Tian_et_al._2014_Instance_1 | One has to be sure to rule out cases where inorganic chemistry can mimic the presence of life (“false positives”). Potential abiotic ozone production on Venus- and Mars-like planets has been discussed by Schindler & Kasting (2000, and references therein). While this is based on photolysis of e.g., CO2 and H2O and is th... | [
"Tian et al. 2014"
] | [
"Indeed, other studies confirm that abiotic buildup of ozone is possible (e.g.,"
] | [
"Similarities"
] | [
[
667,
683
]
] | [
[
572,
650
]
] |
2017MNRAS.469S..39F__Youdin_&_Goodman_2005_Instance_1 | At the disc age t ≈ 1.5 Myr, the decay of 26Al has sufficiently advanced to not melt forming planetesimals and dust from the inner disc has enriched the outer disc (Ciesla 2011). At rh = 30 au, we get τ ≈ 0.1 Myr and t0 ≈ 0.5 Myr because ρ(1 au)/ρ(30 au) = 170 and 1800 in the MMSN and Nice models, respectively (Zsom et... | [
"Youdin & Goodman 2005"
] | [
"The input of dust from the inner disc triggers a streaming instability in the outer disc",
"lasting ≈0.1 Myr and concentrating pebbles and fractals sticking to pebbles into filaments where the comet nucleus collapses by gravity at speeds 1 m s−1 into a randomly packed",
"aggregate of cm-sized pebbles, with the... | [
"Uses",
"Uses",
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930,
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[
1201,
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2018MNRAS.475.1160H__Zschaechner_et_al._2016_Instance_1 | Given their potentially profound impact on both the stellar and gas properties, galaxy mergers are often invoked to explain the presence of metals and low ionization species in the CGM at large impact parameters (e.g. Farina et al. 2013, 2014; Johnson, Chen & Mulchaey 2015b). Indeed, merger-induced tidal torques can gi... | [
"Zschaechner et al. 2016"
] | [
"In addition to morphological disturbances, galaxy mergers can trigger vigorous galactic outflows associated with feedback from the enhanced star formation (e.g."
] | [
"Background"
] | [
[
1148,
1171
]
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[
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972
]
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2016AandA...585A..48G__Mostardi_et_al._(2013)_Instance_1 | On the same SSA22 field, Nestor et al. (2011) and Nestor et al. (2013) show nine LBGs and 20 Lyman-α emitters (LAEs) with LyC detection out of a sample of 41 LBGs and 91 LAEs (all spectroscopically confirmed). They started from a different narrowband image centred at ~3640 Å, which is deeper than that used by Iwata et ... | [
"Mostardi et al. (2013)"
] | [
"Similar conclusions can be reached for the",
"sample where they adopt the same analysis as in Nestor et al. (2013)."
] | [
"Similarities",
"Similarities"
] | [
[
1164,
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]
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1121,
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[
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2022MNRAS.513..232N__Haywood_et_al._2013_Instance_1 | There are a plethora of data available in the form of spectra, astrometric, and photometric information, as well as multiwavelength maps with the advent of large-scale spectroscopic (Apache Point Observatory Galactic Evolution Experiment/APOGEE: Eisenstein et al. 2011, RAdial Velocity Experiment/RAVE: Steinmetz et al. ... | [
"Haywood et al. 2013"
] | [
"For example, star count observations in the solar neighbourhood",
"followed by its characterization as the old α-enhanced population in the double sequence exhibited by the solar neighbourhood stars in the [α/Fe] versus [Fe/H] plane"
] | [
"Background",
"Background"
] | [
[
1519,
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2017ApJ...840...98J__Nataf_et_al._2010_Instance_1 | Figure 1 shows our synthetic color–magnitude diagrams (CMDs) for the two RCs at four different metallicity regimes, which are almost identical to those presented in Figure 1 of Paper I, but here (
) CMDs are added in the right panels. We recall that in our models, the fRC and bRC are produced by G1 and G2, respect... | [
"Nataf et al. 2010"
] | [
"Following Paper I, we have also adopted a 0.2 dex difference in metallicity between G2 and G1, and assumed 12 and 10 Gyrs for the ages of G1 and G2, respectively, with the same population ratio for the two RCs"
] | [
"Uses"
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[
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2015ApJ...799...42D__Skemer_et_al._2014_Instance_1 | The Large Binocular Telescope (LBT) consists of two 8.4Â m aperture optical telescopes on a single ALT-AZ mount installed on Mount Graham in southeastern Arizona (at an elevation of 3192Â m) and operated by an international collaboration among institutions in the United States, Italy, and Germany (Hill et al. 2014; Vei... | [
"Skemer et al. 2014"
] | [
"Each deformable mirror uses 672 actuators that routinely correct 400 modes and provide Strehl ratios exceeding 80%, 95%, and 99% at 1.6âμm, 3.8âμm, and 10âμm, respectively"
] | [
"Background"
] | [
[
754,
772
]
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[
550,
730
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] |
2021AandA...652A..30S__Santini_et_al._2019_Instance_1 | This paper is the fourth in a series. In our first work (Merlin et al. 2018) we presented an accurate and conservative technique to single out passive galaxies at high redshift by means of spectral energy distribution (SED) fitting with a probabilistic approach. We selected 30 z > 3 candidates in the GOODS-S field. Pas... | [
"Santini et al. 2019"
] | [
"In our second work",
"S19 hereafter), we used a complementary approach and looked for evidence of the lack of star formation as seen in the sub-millimetre regime to confirm the passive classification of the high-z candidates selected in GOODS-S."
] | [
"Background",
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[
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2015AandA...584A.103S__Chamel_et_al._2007_Instance_1 | Before leaving this section, in Fig. 8 we display the spatial dependence of the self-consistent neutron and proton density profiles for the optimal solutions in spherical WS cells with average baryon densities nb = 0.0475 fm-3, 0.065 fm-3, and 0.076 fm-3. It is observed that in denser matter the size of the WS cell dec... | [
"Chamel et al. 2007"
] | [
"At high nb the density profile inside the WS cell extends towards the edge of the cell, pointing out that the WS approximation may be close to its limits of validity"
] | [
"Uses"
] | [
[
777,
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]
] | [
[
585,
750
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2022AandA...660A..56A__Myers_2009_Instance_1 | Recent theoretical models clearly demonstrate the role of expanding H I shells for the formation of molecular clouds (e.g., Hennebelle et al. 2008; Heitsch et al. 2009; Inoue & Inutsuka 2009). In particular, these models highlight the importance of multiple compressions for the formation of magnetized filamentary molec... | [
"Myers 2009"
] | [
"This matter replenishment may be channeled from within the cloud itself through molecular filaments",
"or toward hubs"
] | [
"Background",
"Background"
] | [
[
1340,
1350
]
] | [
[
1138,
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[
1324,
1338
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2022MNRAS.510.5676I__Faisst_et_al._2017_Instance_1 | The above finds an explanation within the context of the two-phases formation scenario of ETGs (Oser et al. 2010). According to this scenario, in the early (z ≳ 2) dissipative phase driven by wet major mergers (e.g. Hopkins et al. 2008) and/or violent disc instability (e.g. Barro et al. 2013; Dekel & Burkert 2014; Zolo... | [
"Faisst et al. 2017"
] | [
"Dry minor or intermediate mergers contribute little to the mass growth but promote substantial size growth (the accreted stars tend to be deposited mostly in the external regions), making spheroidal galaxies less compact and likely also less concentrated"
] | [
"Background"
] | [
[
1340,
1358
]
] | [
[
827,
1081
]
] |
2021MNRAS.500.4042S__Snellen_et_al._2010_Instance_1 | To highlight the evidence for CO2 in the transmission spectrum, in Fig. 18 we show three atmo model atmospheres: our best-fitting model from the free-chemistry retrieval; a model with all of the same parameters as the best fit, except the CO2 abundance, which is set to zero; and a third model with both CO and CO2 abund... | [
"Snellen et al. 2010"
] | [
"Theoretical models have found that CO should be the dominant carbon-bearing molecule for hydrogen-dominated atmospheres above 1000 K",
"and CO has been detected at high resolution in hot Jupiter atmospheres (e.g."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
848,
867
]
] | [
[
589,
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[
771,
847
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2021ApJ...922..268J__Bonoli_et_al._2021_Instance_1 | In the last decade, several projects have focused on collecting the deepest images of clusters and groups of galaxies. Among the most recent examples, we can mention the Frontier Fields initiative (Lotz et al. 2017), the Hyper Suprime-Cam Subaru Strategic Program (Aihara et al. 2018a, 2018b, 2019), the Fornax Deep Surv... | [
"Bonoli et al. 2021"
] | [
"In addition, technical development offers a new and barely explored perspective: a panchromatic, more detailed view of the universe through the use of narrowband filter systems, such as those from the J-PLUS and J-PAS surveys"
] | [
"Background"
] | [
[
678,
696
]
] | [
[
409,
634
]
] |
2020ApJ...891...28T__Antoja_et_al._2018_Instance_1 | With the release of Gaia DR2 (Gaia Collaboration et al. 2018; Katz et al. 2019), the proper motions of billions of stars are now available to the astronomical community. Combining with radial velocities from large spectroscopic surveys, like the Sloan Digital Sky Survey (Eisenstein et al. 2011; Blanton et al. 2017), Ga... | [
"Antoja et al. 2018"
] | [
"The discovery of snail shells in the phase-space distribution of MW disk stars",
"has inspired debates about their origin:"
] | [
"Background",
"Background"
] | [
[
680,
698
]
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[
600,
678
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[
700,
740
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2016MNRAS.461.3982B__Scheeres_2002_Instance_1 | Many studies have been done to understand the dynamics and origin of such systems since the discovery of the first binary asteroid system, Dactyl orbiting around (243) Ida in 1993 (Chapman et al. 1995). Based on the structure of ‘rubble pile’ asteroids (a collection of gravitationally bound boulders with a distribution... | [
"Scheeres 2002"
] | [
"Another model for their formation is by increasing their spin rates due to incident and remitted solar photons, known as the Yarkovsky–O'Keefe–Radzievskii–Paddack (YORP) effect. The YORP effect on contact binary asteroids has been studied"
] | [
"Background"
] | [
[
916,
929
]
] | [
[
635,
873
]
] |
2021MNRAS.505.2111L__Melia_et_al._2017_Instance_1 | Recently, quasars observed with multiple measurements, another potential cosmological probe with a higher redshift range that reaches to z ∼ 5, is becoming popular to constrain cosmological models in the largely unexplored portion of redshift range from z ∼ 2 to z ∼ 5. A sample that contains 120 angular size measuremen... | [
"Melia et al. 2017"
] | [
"A sample that contains 120 angular size measurements in intermediate-luminosity quasars from the very long baseline interferometry (VLBI) observations",
"has become an effective standard ruler, which have been extensively applied to test cosmological models"
] | [
"Background",
"Background"
] | [
[
563,
580
]
] | [
[
270,
420
],
[
442,
545
]
] |
2017AandA...599A...8V__Carbone_&_Veltri_1990_Instance_1 | At scales comparable with dp, a variety of observations in the solar wind have suggested that fluctuations may consist primarily of kinetic Alfvén waves (KAWs; Bale et al. 2005; Sahraoui et al. 2009). In the linear fluctuation terminology, KAWs are waves belonging to the Alfvén branch, at wavevectors k almost perpendic... | [
"Carbone & Veltri 1990"
] | [
"In the last decades, KAWs have received considerable attention due to their possible role in a normal mode description of turbulence. Indeed, theoretical studies (e.g.,",
"have shown that the turbulent cascade in magnetized plasma tends to develop mainly in directions perpendicular to B0."
] | [
"Background",
"Background"
] | [
[
755,
776
]
] | [
[
564,
732
],
[
799,
916
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] |
2021MNRAS.500.2209Z__Miyama,_Narita_&_Hayashi_1987_Instance_1 | There is growing observational and numerical evidence that star-forming regions may be in a state of global gravitational contraction; see Vázquez-Semadeni et al. (2019). The supersonic collisions of flows of warm diffuse atomic gas simulated with both self-gravity and cooling exhibit the hierarchical collapse of the t... | [
"Miyama, Narita & Hayashi 1987"
] | [
"The linear stability analysis of these idealized configurations",
"as well as the corresponding non-linear solutions (e.g.",
"confirms this view."
] | [
"Similarities",
"Similarities",
"Similarities"
] | [
[
1208,
1237
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] | [
[
936,
999
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[
1125,
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[
1306,
1325
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] |
2019ApJ...872...97L__Skokos_et_al._2002_Instance_1 | We find a similar dichotomy of bars in previous studies (Elmegreen & Elmegreen 1985, 1989; Baumgart & Peterson 1986; Elmegreen et al. 1996; Regan & Elmegreen 1997; Kim et al. 2015). They investigated two types of bars: flat and exponential profiles in surface brightness. Flat bars have nearly constant light distributio... | [
"Skokos et al. 2002"
] | [
"These properties can also be explained by the locations of resonances"
] | [
"Compare/Contrast"
] | [
[
945,
963
]
] | [
[
761,
830
]
] |
2019AandA...624A..92K___2017_Instance_1 | In Sects. 4.3 and 4.4 we showed that our image simulations match the actual data very well and that the re-weighting factors are close to unity for subsets of galaxies split by size and S/N, with fluctuations of the order of 10−4 or less. Consequently, the estimates of the shear biases presented in Table 2 should be ac... | [
"Hoekstra et al.",
"2017"
] | [
"Varying star densities can affect the results (e.g.",
"In this section we therefore explore the sensitivity of the shear measurement bias to various assumptions and simplifications made in the simulations."
] | [
"Uses",
"Uses"
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2022ApJ...930...32C__Pilbratt_et_al._2010_Instance_1 | Most DSFGs are discovered in wide-area observations using single-dish far-IR (FIR)/millimeter instruments such as the Submillimeter Common-User Bolometer Array (SCUBA/SCUBA-2) on the James Clerk Maxwell Telescope (JCMT; e.g., Smail et al. 1997; Hughes et al. 1998; Chapman et al. 2005; Koprowski et al. 2017; Simpson et ... | [
"Pilbratt et al. 2010"
] | [
"Most DSFGs are discovered in wide-area observations using single-dish far-IR (FIR)/millimeter instruments such as",
"the Herschel Space Observatory"
] | [
"Background",
"Background"
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2020AandA...644L...7G__Magdis_et_al._2020_Instance_1 | As in G18, we compiled existing constraints on the molecular gas fraction fgas of quiescent and pSB galaxies from recent literature, namely: local QGs consisting of the ATLAS3D (Young et al. 2011; Cappellari et al. 2013; Davis et al. 2014) and HRS (Boselli et al. 2014; Lianou et al. 2016) ETG samples as well as the sam... | [
"Magdis et al. 2020"
] | [
"In addition, we also included fgas estimates derived from the (median) stacked FIR spectral energy distributions of ETGs at",
"z ∼ 1.2, z ∼ 0.8, and z ∼ 0.5 (1394, 1536, and 563 galaxies, respectively;",
"hereafter M20"
] | [
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2018AandA...614A..31B__Nakajima_et_al._2012_Instance_1 | High-redshift z ≳ 2 galaxies with prominent Lyman-α emission (Partridge & Peebles 1967), referred to as Lyman-α emitters (LAEs), have become the subject of intense research over the last two decades. Since LAEs are believed to be powered at least partially by ongoing star formation, they are expected to belong to a rel... | [
"Nakajima et al. 2012"
] | [
"Increasing numbers of LAEs are being observed by surveys including narrow-band imaging (e.g.,"
] | [
"Background"
] | [
[
612,
632
]
] | [
[
518,
611
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] |
2021MNRAS.505.2561C__Michtchenko_et_al._2018_Instance_1 | Several mechanisms have been suggested to explain the formation of moving groups. A common explanation is that these velocity structures are the remnants of open clusters, or formed by interactions with a bar (Eggen 1965; Dehnen 2000). One problem with the cluster formation idea is that stars in moving groups can have ... | [
"Michtchenko et al. 2018"
] | [
"Recent work also finds that transient spiral structure",
"may lead to the formation of moving groups, as well as perturbations due to spiral arms in the MW"
] | [
"Background",
"Background"
] | [
[
943,
966
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[
770,
824
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[
844,
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2021AandA...650A.205V__Jones_et_al._2021_Instance_1 | The question of the evolution of exoplanet systems after the main sequence of their host is generally addressed by studying exoplanets around subgiants, RGB stars, and normal HB (RC) stars (hereafter the ’classical’ evolved stars). These classical evolved stars are typically very large stars, with radii ranging from ~ ... | [
"Jones et al. 2021"
] | [
"As a consequence, only large or massive planets are detected around the classical evolved stars",
"and references therein"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1109,
1126
]
] | [
[
1012,
1107
],
[
1128,
1150
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2022MNRAS.515.4520F__Rodriguez-Franco_&_Cuevas_2013_Instance_1 | The atmosphere above the Canary Islands, and especially the western islands Tenerife and La Palma, has been extensively characterized over the past 50 yr (Kiepenheuer 1972; McInnes & Walker 1974; Brandt & Righini 1985; Murdin 1985; Stickland et al. 1987; Whittet, Bode & Murdin 1987; Menéndez-Valdés & Blanco 1992; Jímen... | [
"Rodriguez-Franco & Cuevas 2013"
] | [
"The atmosphere above the Canary Islands, and especially the western islands Tenerife and La Palma, has been extensively characterized over the past 50 yr"
] | [
"Background"
] | [
[
603,
633
]
] | [
[
0,
153
]
] |
2021AandA...656A.126K__Lowry_et_al._2007_Instance_1 | Very small asteroids (VSAs) are objects with diameters D 150 m. They often rotate with periods shorter than 2 h enabling us to study their internal structure by comparing the centrifugal force with the material forces holding them together (Holsapple 2007). Because of their small sizes, VSAs are sensitive to the YORP ... | [
"Lowry et al. 2007"
] | [
"(54 509) was the first asteroid for which the effect of YORP has been observed"
] | [
"Background"
] | [
[
967,
984
]
] | [
[
887,
965
]
] |
2020MNRAS.499..710G__Assef_et_al._2015_Instance_1 | An alternative possibility to reduce the fraction of X-ray sources in the WISE R75 wedge is to allow a large fraction of heavily obscured AGN. This can be achieved for example, by increasing the fraction of Compton-thick AGN in the X-ray luminosity function above the current assumption of 34 per cent, or by increasing ... | [
"Assef et al. 2015"
] | [
"There is indeed evidence for a potentially large population of heavily obscured, possibly Compton-thick AGN, among the WISE population (e.g."
] | [
"Background"
] | [
[
716,
733
]
] | [
[
575,
715
]
] |
2018AandA...613L...1D__Salafia_et_al._2015_Instance_1 | Similarly to long bursts, short GRBs are thought to be produced by a relativistic jet with a typical half-opening angle θjet ~ 5–15 deg (Fong et al. 2016). However, whether or not BNS mergers can always efficiently produce a relativistic jet is still debated (Paschalidis et al. 2015; Ruiz et al. 2016; Kawamura et al. 2... | [
"Salafia et al. 2015"
] | [
"Alternatively, the jet could be (ii) structured, with a fast and energetic inner core surrounded by a slower, less energetic layer/sheath/cocoon (first proposed for long GRBs"
] | [
"Uses"
] | [
[
1044,
1063
]
] | [
[
827,
1001
]
] |
2015MNRAS.454.1644L__Kotze_&_Charles_2012_Instance_2 | The period candidates of other three ULXs may range from ∼100 to ∼600 d. Apart from noise and artefacts, all the candidate periods are only significant in a specific epoch. This suggests that they are not associated with any stable mechanism such as orbital motion. Instead, such long-term (> 100 d) X-ray quasi-periodic... | [
"Kotze & Charles 2012"
] | [
"In particular, there are two intermittent quasi-periodicities for both NGC 5408 X-1 and M81 X-6, suggesting that the quasi-periods are changing or evolving. They resemble some Galactic X-ray binaries that show similar behaviour (e.g. Cyg X–2 and SMC X–1;"
] | [
"Similarities"
] | [
[
957,
977
]
] | [
[
702,
956
]
] |
2020AandA...644A..59K__Pastorello_et_al._2019_Instance_1 | The year 2020 marks the 350 yr anniversary of the discovery of the eruption of Nova 1670 (or CK Vul) made by European astronomers (Shara et al. 1985). Their observations, predominantly performed with a naked eye, traced the object’s evolution on the sky in 1670−1672. From the archive records, we know that the eruption ... | [
"Pastorello et al. 2019"
] | [
"These characteristics resemble closest the behavior often observed in (luminous) red novae",
"a modern category of eruptive stars known from our and other galaxies (e.g."
] | [
"Background",
"Background"
] | [
[
754,
776
]
] | [
[
553,
643
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[
678,
753
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2015AandA...582A..22L__Todorov_et_al._2014_Instance_1 | Dust distribution:We employed the standard flared disk model with well-mixed gas and dust, which has been successfully used to explain the observed SEDs of a large sample of young stellar objects and BDs (e.g., Wolf et al. 2003; Sauter et al. 2009; Harvey et al. 2012a; Joergens et al. 2013; Liu et al. 2015). The struct... | [
"Todorov et al. 2014"
] | [
"J04221332+1934392 (a~7 AU,"
] | [
"Uses"
] | [
[
1160,
1179
]
] | [
[
1133,
1159
]
] |
2021AandA...649A..58L__Bemporad_et_al._(2018)_Instance_3 | The leading edges of the transients normally leave bright traces in the images of visible light, inspiring many methods that were developed to derive their locations and velocities, such as the icecream cone model (Fisher & Munro 1984), the graduated cylindrical shell (GCS) model (Thernisien 2011), geometric triangulat... | [
"Bemporad et al. (2018)"
] | [
"chose the propagating direction averaged over the whole CME derived by the polarization ratio technique to correct the radial speed in the 2D maps, but the key information along the LOS is still lacking."
] | [
"Compare/Contrast"
] | [
[
2324,
2346
]
] | [
[
2347,
2550
]
] |
2020ApJ...898..143S__Shao_&_Li_2018_Instance_1 | In Figure 6, we plot the histogram distributions of the calculated number of Galactic BH–He XRBs as a function of the companion mass, BH mass, orbital period, and orbital eccentricity for Models A–D. Since the progenitor systems containing a BH and an OB star possess similar distributions of the OB star masses and the ... | [
"Shao & Li 2018"
] | [
"Some recent investigations showed that the mass-transfer process in the lobe-filling BH binaries is more stable than previously expected (e.g.,",
"; the maximal mass ratio of the donor star to the BH for stable mass transfer can reach as high as ∼6. Hence only a few BH–He XRBs with orbital periods of ≲1 day are ... | [
"Uses",
"Uses"
] | [
[
826,
840
]
] | [
[
658,
801
],
[
841,
1036
]
] |
2017MNRAS.470..626M__Robitaille_et_al._2012_Instance_1 | The opacity file used for the PAH/VSG population (draine_opac_new.dat) was computed by Bruce Draine (Draine & Li 2007) and is available at https://github.com/hyperion-rt/hyperion-pah/tree/master/PAH-Legacy/input. It was computed taking two lognormal size distributions, one with grain radii below 20 Å and another for gr... | [
"Robitaille et al. 2012"
] | [
"However, their emissivities can be computed based on specific energy absorbed in each grid cell and assuming that the emissivity is the function of the mean intensity of the radiation field, which approximates the spectral shape to the first order"
] | [
"Uses"
] | [
[
966,
988
]
] | [
[
717,
964
]
] |
2022ApJ...929..186L__Ferraro_et_al._2018b_Instance_2 | Our group is addressing this problem by combining a variety of complementary perspectives: (i) by constructing a new generation of high-quality star density profiles derived from star counts instead of surface brightness (see Lanzoni et al. 2007a, 2010, 2019; Miocchi et al. 2013; Pallanca et al. 2021); (ii) by investig... | [
"Ferraro et al. 2018b"
] | [
"In this context we promoted the ESO-VLT Multi-Instrument Kinematic Survey (hereafter the MIKiS survey;",
"a project specifically designed to characterize the kinematical properties of a sample of GGCs in different dynamical evolutionary stages from the radial velocities (RVs) of hundreds of individual stars dist... | [
"Motivation",
"Motivation"
] | [
[
1118,
1138
]
] | [
[
1015,
1117
],
[
1148,
1415
]
] |
2022AandA...667A.131B__Izumi_et_al._(2016)_Instance_2 | Molecular line ratio diagnostics are often used to investigate the physics and chemistry of the ISM in all of these environments. For example, as the gas chemistry located in the central, nuclear regions of galaxies is believed to be dominated by X-rays produced by the AGN, in so-called X-ray dominated regions (XDRs), ... | [
"Izumi et al. (2016)"
] | [
"observed a clear trend that AGNs, including the Seyfert composite galaxy NGC 1068, tend to show higher HCN/HCO+ and/or HCN/CS than in SB galaxies as long as the observations were at high enough spatial resolutions to separate energetically discrete regions."
] | [
"Background"
] | [
[
1151,
1170
]
] | [
[
1171,
1428
]
] |
2020MNRAS.499.1788W__Malhotra_et_al._2001_Instance_2 | Owing to their brightness at rest-frame FIR wavelengths, the ionized and neutral species of Carbon, Nitrogen, and Oxygen are powerful diagnostic lines for tracing the ISM of nearby and distant galaxies. When combined with photodissociation region (PDR) models (Tielens & Hollenbach 1985), measurement of the emission fro... | [
"Malhotra et al. 2001"
] | [
"The luminosity in these FIR lines generally exhibits a deficit in the most FIR luminous galaxies compared to the trend expected from lower luminosity galaxies (e.g."
] | [
"Compare/Contrast"
] | [
[
1832,
1852
]
] | [
[
1667,
1831
]
] |
2022AandA...661A..10B__Santos_et_al._2008_Instance_1 | It is also possible that these clusters have a smaller extent and can just be missed by our extent selection as our detection algorithm sets the extent to zero if it is smaller than 6 (Brunner et al. 2022). Following the method presented in Ghirardini et al. (2021a), we estimated several dynamical properties of the clu... | [
"Santos et al. 2008"
] | [
"The concentration parameter is defined as the ratio of the surface brightness within 0.1 R500 to the surface brightness within R500"
] | [
"Uses"
] | [
[
760,
778
]
] | [
[
602,
733
]
] |
2019MNRAS.482.2731Z__Perley_et_al._2008_Instance_1 | We searched the literature carefully and selected all published GRB-DLAs and QSO-DLAs sightlines conforming to our requirements which are as follows. The object must have spectral energy distributions (SEDs) and optical spectroscopic data available with measurements of AV, column densities of Zn ii and Fe ii, or of S i... | [
"Perley et al. 2008"
] | [
"Note that there is some degeneracy between broken power-law break frequency",
"and extinction, which could lead to inference of grey dust for some instances"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1000,
1018
]
] | [
[
800,
875
],
[
901,
978
]
] |
2017AandA...607A.103G__Gradie_&_Tedesco_(1982)_Instance_1 | In Fig. 4, 29 observations of 15B-type asteroids are presented. As shown by Gil-Hutton & Cañada-Assandri (2012) and Gil-Hutton et al. (2014), in any plot of the observations of B-type objects a dispersion always appears in the whole phase angle range and it seems that these objects do not follow a single phase-polariza... | [
"Gradie & Tedesco (1982)"
] | [
"The reason is probably that the asteroids classified by Bus & Binzel (2002) as members of this taxonomic class include objects that belong to the old F-class, originally proposed by",
"and included in the Tholen taxonomy, due to its flat spectrum and low albedo;"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
514,
537
]
] | [
[
332,
513
],
[
538,
615
]
] |
2018ApJ...864..158L__Drake_et_al._2006_Instance_1 | However, if the magnetic curvature contraction term (last term in Equation (15)) is dominated by the compression term (second-to-last term in Equation (15)) so that
, the contraction or merging is strongly compressible (∇ · VE 0), resulting in an increase in flux-rope magnetic energy instead. In this case the p... | [
"Drake et al. 2006"
] | [
"Although it appears that small-scale flux ropes tend to contract or merge predominantly incompressibly in discussions of particle simulations (e.g.,"
] | [
"Compare/Contrast"
] | [
[
625,
642
]
] | [
[
476,
624
]
] |
2015ApJ...806..152S__Ransom_et_al._2005_Instance_1 | One of the most astonishing characteristics of Liller 1 is the extremely large value of the collision rate parameter. Verbunt & Hut (1987) showed that Liller 1 has the second-highest value of stellar encounter rate (after Terzan 5; see also Lanzoni et al. 2010) among all star clusters in the Galaxy, thus suggesting tha... | [
"Ransom et al. 2005"
] | [
"In fact, it is commonly believed that dynamical interactions in GCs facilitate the formation of close binary systems and exotic objects such as cataclysmic variables (CVs), low-mass X-ray binaries (LMXBs), millisecond pulsars (MSPs), and blue straggler stars (BSSs) (e.g.,"
] | [
"Background"
] | [
[
755,
773
]
] | [
[
414,
686
]
] |
2019ApJ...872..143B__Seckel_et_al._1991_Instance_2 | The gamma-ray emission from the solar disk due to CR cascades in the solar atmosphere is denoted as a disk component. This secondary gamma-ray produced by the hadronic interaction of cosmic ray with the solar surface was first proposed by Dolan & Fazio (1965). While only upper limits were obtained by early measurements... | [
"Seckel et al. 1991"
] | [
"However, the measured solar disk emission flux was about a factor of seven higher than that predicted about this disk component by a “nominal” model"
] | [
"Differences"
] | [
[
1224,
1242
]
] | [
[
1074,
1222
]
] |
2019ApJ...887..118C__Joshi_et_al._2011_Instance_1 | Generally, solar eruptions release their prestored magnetic energy via three phases, namely the precursor, impulsive, and gradual phases (Zhang et al. 2001; Zhou et al. 2016). Thereinto, the latter two, jointly termed as the main phase, correspond to the impulsive acceleration of the erupting CME flux rope, while the l... | [
"Joshi et al. 2011"
] | [
"In the past, the limited observations showed that precursor activities of solar eruptions can come in various forms,",
"as well as nonthermal processes in microwave or hard X-ray wavelength",
"are most common ones."
] | [
"Background",
"Background",
"Background"
] | [
[
948,
965
]
] | [
[
424,
540
],
[
877,
946
],
[
1008,
1029
]
] |
2015MNRAS.454.1468K__Winckel_2003_Instance_3 | Owing to their dusty circumstellar environments, a large mid-infrared (mid-IR) excess is a characteristic feature of post-AGB stars and a detection of cold circumstellar material using mid-IR photometry can be used to identify these objects. The first extensive search for these objects was initiated in the mid-80's usi... | [
"Van Winckel et al. 2009"
] | [
"Moreover, these disc-sources are confirmed to be binaries and show orbital periods between 100 and 2000 d"
] | [
"Compare/Contrast"
] | [
[
2050,
2073
]
] | [
[
1943,
2048
]
] |
2019AandA...623A.140G__Dong_et_al._2018_Instance_1 | Planet formation occurs in disks around young stellar objects. Interactions between planets and disks are very complex. Young planets are expected to cause rings, cavities, spirals, and disturbances in the velocity field and other features in the disk, which in turn may be used to infer the presence of these young plan... | [
"Dong et al. 2018"
] | [
"The literature on indirect evidence of the presence of planets is now becoming very rich, and nearby young stars surrounded by gas-rich disks are intensively studied for this purpose. In most cases, available data cannot fully eliminate alternative hypotheses, or the data have ambiguous interpretations (see, e.g.,... | [
"Background"
] | [
[
1214,
1230
]
] | [
[
878,
1193
]
] |
2019AandA...623A..16S__Olano_&_Poeppel_1987_Instance_1 | Figure 10 (see also Figs. A.4 and A.5) compare the spatial distributions of the Hα and 857 GHz emission in the Taurus–California–Perseus region (e.g., Taurus, Auriga, California, and Perseus). The 857 GHz dust emission traces each molecular cloud and exhibits a hole-like structure. This hole-like structure can also be ... | [
"Olano & Poeppel 1987"
] | [
"The hole-like structure may result from the expansion of a large-scale supershell produced by a supernova in the Per OB2 association that compresses the Taurus cloud from the far side"
] | [
"Background"
] | [
[
922,
942
]
] | [
[
737,
920
]
] |
2019ApJ...883...73C__Ruffolo_et_al._2012_Instance_1 | Assuming that the force-field approach to the solution of the Parker (1965) cosmic-ray transport equation is valid, the connection between historic cosmic-ray intensities and the solar properties they encountered lies in the effective diffusion coefficient that is assumed in this approximation. Establishing such a conn... | [
"Ruffolo et al. 2012"
] | [
"The most likely candidates for this task, given their reasonable agreement with observations and numerical simulations of cosmic-ray diffusion coefficients, are the quasilinear theory (QLT) of Jokipii (1966), the weakly nonlinear theory (WNLT) of Shalchi et al. (2004b), and the nonlinear guiding center theory (NLG... | [
"Compare/Contrast"
] | [
[
853,
872
]
] | [
[
451,
803
]
] |
2018AandA...610A..44M__Krüger_&_Dreizler_(1992)_Instance_3 | The first investigations of the rotational spectra of ethyl isocyanide were carried out in 1966 by Bolton et al. (1966). The spectra of the first vibrational and torsional excited states were measured in the centimeter wave domain (Anderson & Gwinn 1968). In this initial study, the dipole moment was determined to be μa... | [
"Krüger & Dreizler (1992)"
] | [
"The global fits included",
"29 lines from"
] | [
"Uses",
"Uses"
] | [
[
1652,
1676
]
] | [
[
1569,
1593
],
[
1638,
1651
]
] |
2018ApJ...852L..20A__Prieto_et_al._2015_Instance_1 | J0815+4729 is a main-sequence star (T
eff
=
6215
±
82
K,
log
g
= 4.7±0.5) with a metallicity of [Fe/H] ≤ −5.8 dex. Finding unevolved stars at this extremely low metallicity is very important since their stellar surface composition is not expected to be significantly modified by any internal mixing p... | [
"Allende Prieto et al. 2015"
] | [
"The majority of extremely metal-poor stars shows overabundances of carbon, [C/Fe] > 0.7, and it appears that carbon-enhanced metal-poor (CEMP) stars split into two groups, with dramatically different carbon abundances (see, e.g.,"
] | [
"Compare/Contrast"
] | [
[
1579,
1605
]
] | [
[
1324,
1553
]
] |
2022MNRAS.515.1086L__Naoz,_Farr_&_Rasio_2012_Instance_1 | Regarding non-restricted hierarchical three-body systems, Krymolowski & Mazeh (1999) and Ford, Kozinsky & Rasio (2000) presented secular equations of motion (or Hamiltonian) up to the octupole order in semimajor axial ratio by using Hamiltonian perturbation techniques. Lee & Peale (2003) adopted both the octupole-level... | [
"Naoz, Farr & Rasio 2012"
] | [
"Based on this behaviour, it becomes possible to form hot Jupiters on retrograde orbits by combining the eccentric ZLK effect and tidal friction"
] | [
"Background"
] | [
[
1088,
1111
]
] | [
[
925,
1068
]
] |
2018ApJ...854...26L___2015a_Instance_1 | The hot emission line of Fe xxi 1354.09 Å and the cool emission line of Si iv 1402.77 Å have been used in many spectroscopic studies to investigate chromospheric evaporation (e.g., Tian et al. 2014, 2015; Li et al. 2015b, 2017a, 2017b; Brosius et al. 2016; Zhang et al. 2016a, 2016b). It is widely accepted that the forb... | [
"Li et al. 2015a"
] | [
"Those blended emission lines can be easily detected at the position of the flare ribbon, including known and unknown emission lines, such as the C i line at 1354.29 Å, the Fe ii lines at 1353.02 Å, 1354.01 Å, and 1354.75 Å, the Si ii lines at 1352.64 Å and 1353.72 Å, and the unidentified lines at 1353.32 Å and 135... | [
"Background"
] | [
[
1023,
1038
]
] | [
[
694,
1022
]
] |
2022ApJ...925...62K__Cohen_et_al._2020_Instance_1 | We noticed that the fast wind stream had He++ beams moving ahead of the protons, low number densities, and low heavy-ion charge state ratios, which are characteristic of coronal-hole-originated solar wind. It should be noted that although the solar wind stream originates from the same coronal hole, the speed and the st... | [
"Cohen et al. 2020"
] | [
"The timing of the coronal-hole-originated solar wind observation aligned well with the PSP orbit. PSP started passing through the leading edge of the high-speed stream, continued as the high-speed stream corotates over the spacecraft, and ended passing the trailing edge of the stream as seen in Figure 3, standing ... | [
"Motivation"
] | [
[
769,
786
]
] | [
[
418,
767
]
] |
2015AandA...580A...5L__Voit_1991_Instance_1 | The solutions in Sect. 3 show that it is possible for a high X-ray flux in galactic nuclei to alter the carbon ionization balance and reduce the C+ abundance and correspondingly the [C ii] luminosity. In the presence of a high flux of soft X-rays above 1 keV, a condition encountered in many AGNs (Stacey et al. 2010; Eb... | [
"Voit 1991"
] | [
"Furthermore, in galactic nuclei with a high X-ray flux we would expect to see an increase in the dust temperature and infrared luminosity",
"Therefore in galactic nuclei, and in particular in AGNs, we expect a reduction in [C ii] emission relative to FIR/IR emission depending on the relative contribution of diff... | [
"Uses",
"Uses"
] | [
[
881,
890
]
] | [
[
742,
879
],
[
893,
1111
]
] |
2022AandA...663A.172M___2012_Instance_1 | We note that Pavesi et al. (2019) derived a lower κs parameter log(κs) ≈ −1 for HZ10, by observing the CO(2-1) line, which implies a low star formation efficiency for this source. The conflict between the two results can be explained by the fact that Pavesi et al. (2019) estimated the gas mass by adopting a large CO-to... | [
"Narayanan et al.",
"2012"
] | [
"The conversion factor depends on the physical conditions of the gas in the ISM (temperature, surface density, dynamics, and metallicity), as well as the star formation and associated feedback"
] | [
"Compare/Contrast"
] | [
[
937,
953
],
[
960,
964
]
] | [
[
744,
935
]
] |
2019ApJ...875...61M__Jones_&_Boffin_2017_Instance_1 | A substantial fraction of metal-poor stars that have recently evolved off the MS, e.g., giants and planetary nebulae (PNe), have been influenced by binary interactions. The IMF is significantly weighted toward low-mass stars (Bastian et al. 2010; Kroupa et al. 2013), and the MW star formation rate was ≈3 times larger ≈... | [
"Jones & Boffin 2017"
] | [
"For example, the enhanced close binary fraction of metal-poor solar-type stars substantially strengthens the conclusion that the shaping of PN morphologies is the result of binary interactions"
] | [
"Similarities"
] | [
[
1017,
1036
]
] | [
[
787,
979
]
] |
2019ApJ...875L..31H__Leary_et_al._2006_Instance_1 | The recent detection of gravitational-wave (GW) emission from a merging neutron star binary (Abbott et al. 2017d) and merging black hole binaries (BHBs; Abbott et al. 2016a, 2016b, 2017a, 2017b, 2017c; The LIGO Scientific Collaboration & The Virgo Collaboration 2018) by the Laser Interferometer Gravitational-Wave Obser... | [
"O’Leary et al. 2006"
] | [
"These explanations can be very roughly divided into two main categories:",
"and mergers due to dynamical interactions (e.g.,"
] | [
"Background",
"Background"
] | [
[
815,
834
]
] | [
[
509,
581
],
[
723,
771
]
] |
2018MNRAS.479.4509R__Kingma_&_Ba_2014_Instance_2 | After each step of calculations, the network should optimize the model based on its current and previous states to improve the subsequent mapping. Our model utilizes a computationally memory efficient optimization due to its dependence to only the first-order gradients, namely the ‘adaptive moment estimation’ (or Adam)... | [
"Kingma & Ba 2014"
] | [
"Adam optimization, compared to other gradient-based optimization, is very suitable for noisy and sparse gradients, and for simulated data that show very large scatter with respect to a given quantity of parameter"
] | [
"Compare/Contrast"
] | [
[
598,
614
]
] | [
[
384,
596
]
] |
2019ApJ...882..168P__Hildebrand_1983_Instance_1 | In order to provide constraints on the gas masses in these galaxies independently from the CO measurements, we can use the Rayleigh–Jeans dust continuum emission. This will provide the first constraints to the αCO conversion factor in “normal” galaxies at z > 3 in the following. The Rayleigh–Jeans dust continuum emissi... | [
"Hildebrand 1983"
] | [
"The Rayleigh–Jeans dust continuum emission has been used to estimate dust and gas masses, assuming an average emissivity and dust temperature for the dominant cold dust component and a constant dust-to-gas ratio"
] | [
"Background"
] | [
[
493,
508
]
] | [
[
280,
491
]
] |
2022ApJ...935..135B__Mathur_1990_Instance_2 | All responses calculated in this paper only account for the direct response to a perturbing potential. In general, though, the response also has an indirect component that arises from the fact that neighboring regions in the disk interact with each other gravitationally. This self-gravity of the response, which we have... | [
"Mathur 1990"
] | [
"In the regime of stability, the normal modes are undamped oscillation modes in absence of lateral streaming"
] | [
"Uses"
] | [
[
1773,
1784
]
] | [
[
1664,
1771
]
] |
2016ApJ...821...19F__Fulle_et_al._2010_Instance_1 | GIADA characterizes individual dust particles by means of two independent sensors. At the instrument entrance the particle crosses a laser curtain, and is detected by photoelectric sensors (GDS, grain detection system) registering a signal (proportional to the particle cross section times the albedo) and the time at wh... | [
"Fulle et al. 2010"
] | [
"If the particle is too small to be detected by the GDS system, it may be detected by the IS sensor only (IS particles): in this case the particle momentum is converted to the mass assuming the mean value of the velocities of the GDS+IS particles in the same momentum bin, or assuming the velocities predicted by tai... | [
"Uses",
"Uses"
] | [
[
1135,
1152
]
] | [
[
810,
1133
],
[
1154,
1186
]
] |
2022MNRAS.512..186K__Dutta_&_Bharadwaj_2013_Instance_1 | A widely used statistical property of the sky brightness distribution is its power spectrum (Lazarian 1995; Bharadwaj & Sethi 2001, and others). As the redshifted 21-cm signal is expected to be faint and hard to detect with imaging, estimating its power spectrum or equivalently intensity mapping gives a possible probe ... | [
"Dutta & Bharadwaj 2013"
] | [
"This method and its variants",
"have been used to estimate",
"as well as the power spectrum of H i distribution in nearby galaxies",
"These works propagate the uncertainties in each visibility estimate and combine that with the sample variance error in measuring the power spectrum to quote uncertainties in t... | [
"Background",
"Background",
"Background",
"Background"
] | [
[
927,
949
]
] | [
[
487,
515
],
[
655,
681
],
[
838,
906
],
[
977,
1180
]
] |
2022ApJ...929...19G__Yu_et_al._2019_Instance_1 | From the theoretical point of view, we normalize the disk size to a fixed black hole mass and luminosity (thus to a fixed accretion rate; see Equations (14) and 17); therefore, we expect that the disk size τ
0 is independent of AGN properties. However, there are two possibilities that may cause the observed dependence ... | [
"Yu et al. 2019"
] | [
"Observational calibrations of the virial factor also tend to support this conclusion (e.g.,"
] | [
"Similarities"
] | [
[
837,
851
]
] | [
[
702,
793
]
] |
2022ApJ...939...43E__Protheroe_1999_Instance_1 | The multimessenger observations of NGC 1068 dictate the need for multiple emission zones. In this work, we will capture its inner microparsecs referring to a spherically symmetric structure for the corona of the AGN as well as an outer starburst ring with a radius of ∼1 kpc (see Figure 1). Note, that in between these t... | [
"Protheroe 1999"
] | [
"according to diffusive shock acceleration (DSA; e.g.,"
] | [
"Uses"
] | [
[
1765,
1779
]
] | [
[
1699,
1752
]
] |
2017MNRAS.471.3057M__Bovy_et_al._2016b_Instance_2 | We have performed the first detailed dissection of the stellar populations of the Milky Way disc in age, [Fe/H] and $\mathrm{[ \alpha \mathrm{/Fe]}}$ space, bridging the gap between the detailed observational understanding of MAPs (e.g. Bovy et al. 2012b, 2016b) and the plethora of studies of co-eval stellar population... | [
"Bovy et al. 2016b"
] | [
"The radial variation of the stellar surface density of the high $\\mathrm{[ \\alpha \\mathrm{/Fe]}}$ mono-age populations is found to have insignificant breaks, and they are better fit by a single exponential in this disc region. As these populations are the oldest, this may be a sign of the disc evolution washing... | [
"Similarities"
] | [
[
1780,
1797
]
] | [
[
1235,
1778
]
] |
2019MNRAS.487..364L__Kruijssen_et_al._2018_Instance_1 | It is well known that star formation is inefficient on galactic scales. The observed linear correlation between molecular gas surface density and star formation rate (SFR) surface density in normal star-forming galaxies suggests a nearly constant gas depletion time-scale around ∼2 Gyr, much longer than the dynamical ti... | [
"Kruijssen et al. 2018"
] | [
"The origin of this large scatter is usually explained as a combination of the time variability of the SFR during the course of cloud evolution and intrinsic scatter of SFEs due to the diversity of GMC properties"
] | [
"Background"
] | [
[
1081,
1102
]
] | [
[
779,
990
]
] |
2021ApJ...914L..38U__Dullemond_et_al._2001_Instance_1 | Snow lines of abundant volatile species are one of the possible origins of the observed substructures in dust continuum emission (Zhang et al. 2015; Okuzumi et al. 2016; Pinilla et al. 2017). Recent disk surveys have shown that the locations of the observed gap/ring structures do not seem to be related to the radial lo... | [
"Dullemond et al. 2001"
] | [
"To estimate the positions of the snow lines in observed disks, the temperature profile is often assumed to be a simple power law",
"which is broken if the disk has shadows on the disk surface"
] | [
"Uses",
"Uses"
] | [
[
641,
662
]
] | [
[
412,
540
],
[
580,
639
]
] |
2018AandA...615A.148D__Weidner_et_al._(2010)_Instance_1 | The last column in Table 1 reports the number of OB stars minus the “diffuse” population estimated from their density in the Reference field (22.5 stars per square degree): as is immediately seen, the M-star statistics is much larger than the OB star statistics. This can hardly be considered surprising, if an ordinary ... | [
"Weidner et al. 2010"
] | [
"The last column in Table 1 reports the number of OB stars minus the “diffuse” population estimated from their density in the Reference field (22.5 stars per square degree): as is immediately seen, the M-star statistics is much larger than the OB star statistics. This can hardly be considered surprising, if an ordi... | [
"Uses",
"Uses"
] | [
[
341,
360
]
] | [
[
0,
340
],
[
362,
403
]
] |
2022MNRAS.511.6218Z__Malkov,_Diamond_&_Sagdeev_2012_Instance_1 | To further reduce the number of fitting parameters, we assume that no source is unique in terms of the acceleration spectral shape, i.e. all the source components have the same H spectral index α, He spectral index, maximum rigidity Rm, and He-to-H Galactic injection flux ratio χ. The spectrum of He seems harder than t... | [
"Malkov, Diamond & Sagdeev 2012"
] | [
"The spectrum of He seems harder than that of H as indicated by many spectral studies, implying, e.g. time-dependent particle acceleration",
"or more efficient He injection in the shock acceleration process"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
507,
537
]
] | [
[
282,
419
],
[
441,
505
]
] |
2021AandA...655A..99D__Carigi_et_al._2005_Instance_3 | Another way of obtaining information about the nucleosynthesis processes involved in producing carbon is to compare it with other elements that are characterised by a well-known source of production, as in the case of oxygen. In Fig. 5, we show the variation of [C/O] as a function of [Fe/H], which serves as a first-ord... | [
"Carigi et al. 2005"
] | [
"The turning point of increased relative production of carbon from massive stars takes place at A(O) ~ 8.7 dex (see Fig. 2 of",
"which equals to [O/H] ~ 0.0 dex.",
"This observed behaviour of [C/O] is in contrast to the steady increase of [C/O] up to [Fe/H] ~ 0.3 dex found, for example, by Franchini et al. (202... | [
"Uses",
"Uses",
"Differences"
] | [
[
2266,
2284
]
] | [
[
2141,
2265
],
[
2286,
2318
],
[
2319,
2469
]
] |
2021MNRAS.507.2766S__Sumiyoshi_et_al._2005_Instance_1 | In order to make a linear analysis, first we have to prepare the PNS models as a background. The PNS properties depend on not only the density and pressure profiles but also the distributions of temperature (or entropy per baryon) and electron fraction inside the PNS, while such profiles can be determined only via the ... | [
"Sumiyoshi et al. 2005"
] | [
"In the simulations, hydrodynamics and neutrino transfer in general relativity are solved simultaneously"
] | [
"Uses"
] | [
[
761,
782
]
] | [
[
614,
717
]
] |
2019MNRAS.487.1210T__McNamara_&_Nulsen_2007_Instance_3 | On larger scales, the clusters in which BCGs reside can generally be divided into two categories: cool core clusters, which exhibit very peaked surface brightness distributions at X-ray wavelengths, and non cool core clusters, with similar overall X-ray luminosities but with smoother, less peaked X-ray surface brightne... | [
"McNamara & Nulsen 2007"
] | [
"Alone, the energy released by jetted outflows appears to be on the same order as the energy needed to offset cooling (e.g.",
"therefore suggesting that AGN feedback is a good candidate for solving the cooling flow problem."
] | [
"Uses",
"Uses"
] | [
[
1857,
1879
]
] | [
[
1712,
1834
],
[
1913,
2009
]
] |
2020MNRAS.499.2575E__Pontzen_&_Governato_2014_Instance_1 | We note in passing that recent studies address improved satellite modellimg that ameliorates many of these issues, including the core–cusp issue via non-sphericity of the stellar velocity distribution (Hayashi, Chiba & Ishiyama 2020) and the detectability of MWG satellites (Nadler et al. 2020). Other proposed solutions... | [
"Pontzen & Governato 2014"
] | [
"Other proposed solutions include",
"or through dynamical feedback driven by starbursts or active galactic nuclei"
] | [
"Background",
"Background"
] | [
[
1099,
1123
]
] | [
[
296,
328
],
[
720,
796
]
] |
2022ApJ...940L..18Z__Perna_et_al._2022_Instance_1 | In addition to some fraction of BNS mergers masquerading as long GRBs, our sample used to constrain the DTD may suffer from other issues of incompleteness. As we rely on the modeling of host galaxies when constraining the DTD, we do not consider short GRBs that do not have a confident host association. Though the prope... | [
"Perna et al. 2022"
] | [
"For example, GRBs that are highly offset from their hosts may have afterglows with much lower luminosities, making precise localization (and therefore host identification) difficult"
] | [
"Compare/Contrast"
] | [
[
757,
774
]
] | [
[
574,
755
]
] |
2021AandA...653A.156F__Valentini_et_al._2007_Instance_1 | In general, hybrid-kinetic models have proved to be capable of satisfactorily catching the main kinetic physics at play for a large number of problems, ranging from fluid and kinetic instabilities (Hellinger & Matsumoto 2000; Matteini et al. 2006; Califano et al. 2008; Henri et al. 2013; Kunz et al. 2014) to collisionl... | [
"Valentini et al. 2007"
] | [
"The starting point is the “hybrid Vlasov–Maxwell” (HVM) code",
"which is already equipped with a fluid model in which electrons are described as an isotropic, isothermal fluid with finite inertia. The HVM code has recently been upgraded in order to implement a more sophisticated model for the electron fluid. Thi... | [
"Uses",
"Background"
] | [
[
936,
957
]
] | [
[
852,
912
],
[
960,
1546
]
] |
2021AandA...655A..72S___2019_Instance_2 | In this paper, we report on spectroscopic CH3CN, CH3OH (methanol), and dust continuum observations with the Atacama Large Millimeter/submillimeter Array (ALMA) at 349 GHz with an angular resolution of 0′′.1. We exploit the CH3CN (19K–18K) K-ladder, with excitation energies ranging from 168 K (for K = 0) to 881 K (for K... | [
"Sanna et al. 2019"
] | [
"We showed that molecular gas is falling in and slowly rotating with sub-Keplerian velocities down to radii of 500 au from the central star, where we measured a mass infall rate of 6 × 10−4 M⊙ yr−1",
"their Fig. 5)."
] | [
"Background",
"Background"
] | [
[
1287,
1304
]
] | [
[
1089,
1285
],
[
1306,
1320
]
] |
2022ApJ...937...62L__Xiao_et_al._2022_Instance_1 | However, the intrinsic effects caused by the unknown emission and acceleration mechanisms in the source could mitigate or enhance the LIV-induced time delay, which would impact the accuracy of the resulting constraints on LIV. A key challenge is then to distinguish an intrinsic time lag at the source from a delay induc... | [
"Xiao et al. 2022"
] | [
"while short GRBs are consistent with null or negligible intrinsic spectral lag and are therefore an ideal tool to measure the LIV effect"
] | [
"Motivation"
] | [
[
803,
819
]
] | [
[
612,
748
]
] |
2022MNRAS.510.4943S__Murray_&_Dermott_1999_Instance_1 | The gravitational potential of an eccentric companion at the quadrupole order can be decomposed as a sum over circular orbits (e.g. Storch & Lai 2013; Vick, Lai & Fuller 2017):
(5)$$\begin{eqnarray*}
U\left(\boldsymbol{\mathbf {r}}, t\right) = \sum \limits _{m=-2}^2 U_{2m} \left(\boldsymbol{\mathbf {r}}, t\right) ,
\... | [
"Murray & Dermott 1999"
] | [
"also denoted $X^N_{2m}$ in"
] | [
"Background"
] | [
[
1074,
1095
]
] | [
[
1047,
1073
]
] |
2022MNRAS.514.2010M__Feng_&_Holder_2018_Instance_1 | In the last few years, several experiments have reported upper limits on the power spectrum of 21-cm fluctuations during reionization (Parsons et al. 2014; Patil et al. 2017; Barry et al. 2019; Mertens et al. 2020; The HERA Collaboration 2021b) and the earlier cosmic-dawn era (Eastwood et al. 2019; Gehlot et al. 2019, ... | [
"Feng & Holder 2018"
] | [
"Similarly, stronger-than-expected 21-cm signals can arise if the cosmic radio background has contributions other than the CMB"
] | [
"Motivation"
] | [
[
806,
824
]
] | [
[
679,
804
]
] |
2021ApJ...908..220T__Milone_et_al._2020_Instance_1 | Recently, our knowledge of the MW formation and evolution has been revolutionized by the massive amount of data products from the Gaia mission and large spectroscopic surveys. Several dwarf galaxies are suggested to have been accreted by the MW since its formation (e.g., Helmi et al. 2018; Belokurov et al. 2018; Myeong... | [
"Milone et al. 2020"
] | [
"The existence of MPs in Pal 13 supports the statement that this phenomenon is not unique in Galactic GCs formed in situ (e.g.,"
] | [
"Similarities"
] | [
[
874,
892
]
] | [
[
727,
853
]
] |
2022MNRAS.515.2256V__Drury_1983_Instance_1 | SBs are complex environments. The hot rarefied plasma is spanned by primary shocks, which decay into turbulent motions and MHD waves. Collective effects such as re-acceleration processes contribute to the acceleration of particles. SBs are also delimited by a forward shock which expands into the ISM. While the size of ... | [
"Drury 1983"
] | [
"More generally, in the case of strong shocks, the velocity u is identified as the velocity of the shock, as it is precisely the velocity jump at the shock discontinuity which drives the acceleration of the particles via the DSA mechanism (e.g."
] | [
"Background"
] | [
[
733,
743
]
] | [
[
489,
732
]
] |
2016AandA...588A..44Y__Lehtinen_&_Mattila_(1996)_Instance_1 | All coreshine observations were obtained with the IRAC instrument on board the Spitzer observatory and are gathered in Paladini (2014) and Lefèvre et al. (2014), from which we selected 21 starless cores in the Taurus-Perseus, Chamaeleon, Cepheus, and L183/L134 regions (see their Fig. 9 and Table 1). Lefèvre et al. (201... | [
"Lehtinen & Mattila (1996)"
] | [
"After convolving our models with a 10″ FWHM Gaussian kernel to simulate the data analysis presented in Lefèvre et al. (2014) and following the",
"prescription to take into account the part of the ISRF+CM light that can be transmitted through the cloud3, we compute the synthetic photometry for each pixel along a ... | [
"Uses",
"Uses"
] | [
[
824,
849
]
] | [
[
681,
823
],
[
850,
1365
]
] |
2022ApJ...933..243F__Hajela_et_al._2022_Instance_1 | Recently, Fraija et al. (2021a) presented the afterglow light curves generated by the deceleration of sub-relativistic masses ejected from the merger of BCOs and the death of massive stars. The authors assumed that a PL velocity distribution describes the isotropic-equivalent kinetic energy of these masses and that the... | [
"Hajela et al. 2022"
] | [
"Inspired by the new observations of this GW event at 3.3 yr after the initial merger",
"in this paper, we extend the synchrotron model presented in Fraija et al. (2021a), including the continuous energy injection from the central engine (either a spinning magnetized NS or BH remnant) into the blast wave through ... | [
"Motivation",
"Motivation"
] | [
[
924,
942
]
] | [
[
838,
922
],
[
945,
1214
]
] |
2019AandA...622A..60C__Drake_et_al._2013a_Instance_1 | In order to establish the completeness and purity of the RR Lyrae stars confirmed by the SOS Cep&RRL pipeline and to estimate the number of new discoveries by Gaia, we performed a deep and careful comparison with the literature. As a first step, the catalogue of 140 784 confirmed sources was cross-matched against all m... | [
"Drake et al. 2013a"
] | [
"We primarily used the OGLE catalogues for RR Lyrae stars",
"but we also used RR Lyrae stars by CTRS",
"These cross-matches returned a list of 88 578 known RR Lyrae stars in our sample of 140 784 stars."
] | [
"Uses",
"Uses",
"Uses"
] | [
[
535,
553
]
] | [
[
380,
436
],
[
494,
533
],
[
992,
1090
]
] |
2021ApJ...909..172Z__Read_&_Lebonnois_2018_Instance_2 | Atmospheric superrotation is characterized by eastward wind at the equator, which means the atmosphere there has a higher angular momentum than the solid surface. Atmospheric superrotation is a common phenomenon across the universe. In the solar system, superrotation exists in the atmospheres of Venus, Titan, Saturn, a... | [
"Read & Lebonnois 2018"
] | [
"This up-gradient transport into the jet can result from Rossby waves, coupled Rossby–Kelvin waves, mixed Rossby–gravity waves, wave–jet resonance, barotropic instability, or baroclinic instability"
] | [
"Background"
] | [
[
1355,
1376
]
] | [
[
778,
974
]
] |
2021AandA...649A.168D__Oh_&_Escuti_2008_Instance_1 | A critical property of the phase mask is that it needs to be able to image subapertures in off-axis interferograms. The off-axis interferograms are rather large, with size scaling with λ/Dsub, where λ is the wavelength and Dsub is the diameter of the subaperture. Therefore, imaging multiple interferograms onto separate... | [
"Oh & Escuti 2008"
] | [
"This property enables the creation of steep phase ramps that efficiently diffract light into a single order without scattering"
] | [
"Uses"
] | [
[
779,
795
]
] | [
[
651,
777
]
] |
2018MNRAS.473.2144B__Nakamura_&_Li_2007_Instance_1 | The problem of the balance between driving and decay for magnetized turbulence is most acute in molecular clouds. Since these have linewidths indicating the presence of supersonic flow, the fast dissipation of turbulence found by these simulations necessitates a mechanism to reinject the energy equally quickly. A numbe... | [
"Nakamura & Li 2007"
] | [
"The problem of the balance between driving and decay for magnetized turbulence is most acute in molecular clouds. Since these have linewidths indicating the presence of supersonic flow, the fast dissipation of turbulence found by these simulations necessitates a mechanism to reinject the energy equally quickly. A ... | [
"Background",
"Background"
] | [
[
517,
535
]
] | [
[
0,
365
],
[
471,
495
]
] |
2021MNRAS.507.5053E__Johnston_et_al._2006_Instance_1 | Multiwavelength observations of the GC indicate that the number of pulsars in the central few parsecs should be high (Wharton et al. 2012) and conditions are highly favourable for relativistic binaries (Faucher-Giguère & Loeb 2011). The dense nuclear star cluster surrounding Sgr A* (see e.g. Genzel, Eisenhauer & Gilles... | [
"Johnston et al. 2006"
] | [
"Despite this only six radio pulsars have been discovered within half a degree of Sgr A*"
] | [
"Background"
] | [
[
911,
931
]
] | [
[
822,
909
]
] |
2021MNRAS.503..324M__Zhao_et_al._2019_Instance_3 | We first determined the orbital parameters for RS Ser, V449 Per, and V1095 Her. Further, we updated the parameters for V593 Cen and MR Del. Using the formula f = (Ωin – Ω1)/(Ωin – Ωout), we calculated the contact factors f for RS Ser, V593 Cen, and V1095 Her as 6.5 per cent, 40 per cent, and 53 per cent, respectively.... | [
"Zhao et al. 2019"
] | [
"For MR Del, we revised the absolute parameters using its full light curve and the published radial velocities, which are similar to those published previously"
] | [
"Similarities"
] | [
[
1148,
1164
]
] | [
[
988,
1146
]
] |
2022ApJ...935..137K__Tegler_et_al._1995_Instance_1 | In Figure 2, the reduced AKARI IRC spectra of all protostars are presented; the absorption features of the H2O, CO2, and CO ices are clearly detected. All of our targets show deep and broad absorption features of H2O ice in the wavelength range 2.7–3.4 μm. In the case of AFGL 7009S, strong extinction toward the source ... | [
"Tegler et al. 1995"
] | [
"Many near-infrared observations have revealed the same feature on the blue wing part of the CO absorption feature",
"which was suggested as an absorption feature of XCN ice."
] | [
"Similarities",
"Background"
] | [
[
1085,
1103
]
] | [
[
970,
1083
],
[
1195,
1251
]
] |
2020AandA...643A..35P__Irwin_et_al._2007_Instance_1 | In order to achieve high photometric accuracy and be sensitive to low amplitude undulations, we adopted techniques from the exoplanet community, with the purpose of eliminating the systematic errors. When performing differential photometry (Sect. 3), accurate bias-subtraction and flat-fielding are of major importance. ... | [
"Irwin et al. (2007)"
] | [
"According to",
", the Poisson noise is 200 e− for a typical detector with a gain of a few e− ADU−1 and the flat illumination level is of 20 000 ADU pixel−1 = 40 000 e− pixel−1. Thus, a typical photometric aperture with a radius of 3 pixels contributes ∼1 mmag photon noise."
] | [
"Uses",
"Uses"
] | [
[
333,
352
]
] | [
[
320,
332
],
[
352,
609
]
] |
2021AandA...654A..88W__Bordoloi_et_al._2014_Instance_1 | The CGM (see Tumlinson et al. 2017, for a detailed review) is now understood to be a key component in disentangling the feedback processes in active galaxies. It links the smaller-scale interstellar medium (ISM) of the galaxy to the larger-scale intergalactic medium (IGM), not only in a geometrical way but also by acti... | [
"Bordoloi et al. 2014"
] | [
"This complex environment is multiphase and has been observed in numerous surveys",
"at low redshift."
] | [
"Background",
"Background"
] | [
[
628,
648
]
] | [
[
517,
597
],
[
691,
707
]
] |
2015AandA...584A..75V__Essen_et_al._(2014)_Instance_2 | The data presented here comprise quasi-simultaneous observations during secondary eclipse of WASP-33 b around the V and Y bands. The predicted planet-star flux ratio in the V-band is 0.2 ppt, four times lower than the accuracy of our measurements. Therefore, we can neglect the planet imprint and use this band to measur... | [
"von Essen et al. (2014)"
] | [
"Hence, to reduce the number of 24 free parameters and the values they can take, we use prior knowledge about the pulsation spectrum of the star that was acquired during"
] | [
"Uses"
] | [
[
781,
804
]
] | [
[
612,
780
]
] |
2019MNRAS.485.5453S__Sahal-Brechot_et_al._1996_Instance_1 | Here we give a simple estimate for the population of 2s-state hydrogen atoms by considering a three-level system (1s, 2s, and 3p). We set the rate equation for the 2s population as
(1)
\begin{eqnarray*}
n_{\rm H,1s}C_{\rm 1s,2s}+n_{\rm H,3p}A_{\rm 3p,2s}-n_{\rm H,2s}A_{\rm 2s,1s}=0,
\end{eqnarray*}
where nH, j is t... | [
"Sahal-Brechot et al. 1996"
] | [
"For a collision at a velocity ∼108 cm s−1, which is a typical velocity scale for young SNR shocks, the cross-section is ∼10−13 cm2, giving a reaction rate ∼10−5 cm3 s−1 (e.g.",
"Thus, if the density is ∼106 cm−3, the collisional depopulation becomes important."
] | [
"Uses",
"Uses"
] | [
[
1181,
1206
]
] | [
[
978,
1152
],
[
1209,
1291
]
] |
2019AandA...622A..91G__Genzel_&_Stutzki_1989_Instance_1 | Among the species studied in this work, the detection of broad (Δv > 30 km s−1) line-wing H2O (312-221) emission implies the presence of shocked gas activity (e.g., van Dishoeck et al. 2011, 2013). Indeed, we only detect H2 O and CH3OH rotationally excited lines toward Orion S and BN/KL (Figs. 2 and B.1). Both species ... | [
"Genzel & Stutzki 1989"
] | [
"In OMC-1, the low- and high-velocity outflows from BN/KL plunge into the ambient molecular cloud",
"producing hot (from Tk ≃ 200–2000 K) and dense (up to n(H2) ≃ 106–107 cm−3) post-shocked gas in H2 Peaks 1 and 2"
] | [
"Uses",
"Uses"
] | [
[
754,
775
]
] | [
[
656,
752
],
[
777,
889
]
] |
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