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 |
|---|---|---|---|---|---|---|
2022MNRAS.515.2188H__Rorai_et_al._2018_Instance_1 | In this work, we follow the method for measuring the IGM thermal state based on Voigt profile decomposition of the Ly α forest (Schaye et al. 1999; Ricotti et al. 2000; McDonald et al. 2001). In this approach, a transmission spectrum is treated as a superposition of multiple discrete Voigt profiles, with each line desc... | [
"Rorai et al. 2018"
] | [
"The majority of past applications of this method constrained the IGM thermal state by fitting the low-b-$N_{\\rm H\\, {\\small I}}$ cutoff of the $b-N_{{{{\\rm H\\, {\\small I}}}}{}}$ distribution"
] | [
"Background"
] | [
[
1027,
1044
]
] | [
[
640,
830
]
] |
2016ApJ...826..117Y__Roux_&_Webb_2009_Instance_2 | Traditionally, the Parker transport equation (Parker 1965) was used to model pickup ion acceleration at the SWTS when using a transport theory approach. However, interesting Voyager results, such as strongly fluctuating pitch-angle anisotropies upstream, the detection of highly anisotropic intensity spikes at the SWTS,... | [
"le Roux & Webb 2009"
] | [
"Furthermore, statistical variations in the observed magnetic field direction near the SWTS were included as a time series to model time variations in the injection and DSA of pickup ions to simulate the highly volatile nature of actual DSA at the SWTS"
] | [
"Compare/Contrast"
] | [
[
1901,
1920
]
] | [
[
1617,
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2022MNRAS.515.5629D__Dubber_et_al._2021_Instance_1 | In the previous sections, we have shown the difficulty in balancing follow-up time with large numbers of unconfirmed candidate companions from single-epoch photometry. This follow-up dilemma was the motivation for designing the K-peak filter: can we optimize the observing time required to determine the nature of a targ... | [
"Dubber et al. 2021"
] | [
"In previous work",
"we used a custom filter centred on the deep 1.45 µm feature present in YPMOs to distinguish between them and background sources. In the 2–5 µm range covered by NIX, such water features are far less dominant, and there are strong telluric features across some of this range that would make a si... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
857,
875
]
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[
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818
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[
878,
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2021MNRAS.507.5882S__Mackereth_et_al._2018_Instance_2 | Cosmological hydro dynamical N-body simulations offer another possibility to investigate the origin of the bimodality in the ([Fe/H], [α/Fe]) plane. Earlier simulations, e.g. full N-body simulations by Loebman et al. (2011), Brook et al. (2012) or hybrid simulations in which a semi-analytic chemical evolution was added... | [
"Mackereth et al. (2018)"
] | [
"Clarke et al. (2019) and Buck (2020) suggest that bimodality should be common in disc galaxies, whereas",
"suggest that it is rare."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1680,
1703
]
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2021ApJ...910...78Z__Condon_et_al._2017_Instance_2 | The multiwavelength spectral data of 13 SNRs with hard γ-ray spectra. The γ-ray spectra are fitted with a hadronic model with the normalization of the individual spectrum as free parameters. The model assumes that protons have a single power-law energy distribution with an exponential high-energy cutoff. Note that the ... | [
"Condon et al. 2017"
] | [
"RCW 86:",
"GeV"
] | [
"Uses",
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1312,
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2022AandA...668A..50S__Ginski_et_al._(2016)_Instance_2 | To test IADI, we made a model of a disk in scattered light. This model is 400 × 400 pixels, each pixel having a physical size of 1 × 1 au. Multiple rings are implemented, inspired by observations of disks (e.g., HD 97048 Ginski et al. 2016; RX J1615 de Boer et al. 2016 and TW Hydrae van Boekel et al. 2017), see panel a... | [
"Ginski et al. (2016)"
] | [
"For our disk model, we are using the power-law profile for the scattering surface height H and the separation r found by",
"for the disk around HD 97048. This profile describes the flaring discovered in this source reasonably well up to a separation of ~270 au."
] | [
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] | [
[
851,
871
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850
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[
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2021MNRAS.507.6012Z__Kendrick_2018_Instance_1 | Being a benchmark system H + H2, H + HD, and their isotopic counterparts have received much attention over the last several decades (Marinero et al. 1984; Zhang & Miller 1989; D’Mello et al. 1991; Harich et al. 2002; Gao et al. 2015; Yuan et al. 2018a, b, 2020). Most early experimental and theoretical investigations we... | [
"Kendrick 2018"
] | [
"These PESs have also been able to account for even subtle effects such as the GP"
] | [
"Background"
] | [
[
940,
953
]
] | [
[
798,
878
]
] |
2016MNRAS.461.4406A__Santos_et_al._2015_Instance_1 | However, we note that the quoted eccentricity for the inner planet in HD 155358 is 0.17 ± 0.03 (Robertson et al. 2012a). The mean value is exceeded for the standard run at 4000 orbits after going into resonance with the implication that the planets could not have been in resonance longer than this time. If this is the ... | [
"Tadeu dos Santos et al. 2015"
] | [
"This is likely to need to be considered for different possible exterior disc models and in addition the planets may have built up their masses as they went (see e.g.",
"These considerations are beyond the scope of this paper."
] | [
"Future Work",
"Future Work"
] | [
[
669,
697
]
] | [
[
503,
668
],
[
700,
756
]
] |
2016ApJ...827...75L__Nishizawa_&_Nakamura_2014_Instance_1 | According to general relativity, in the limit in which the wavelength of gravitational waves is small compared to the radius of curvature of the background spacetime, the waves propagate with the velocity of light, i.e., c (see Will 1998, and references therein). In other theories, the speed
could differ from c.... | [
"Nishizawa & Nakamura 2014",
"Nishizawa & Nakamura 2014"
] | [
"However, there is no theoretical argument (or pathology) against GWs propagating faster than light (see",
"and references therein)"
] | [
"Uses",
"Uses"
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[
841,
866
],
[
1663,
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[
737,
840
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886,
909
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2018MNRAS.476.1835F__Danforth_et_al._2010_Instance_1 | In the classical unified model, blazars constitute a class of active galactic nuclei (AGNs) viewed at small angles from the jet axis (Blandford & Rees 1978; Antonucci 1993; Urry & Padovani 1995). Traditionally, blazars have been further splitted into two subclasses based on the strength of the features present in their... | [
"Danforth et al. 2010"
] | [
"In past years, several alternatives have been proposed to constrain the redshift of BL Lac objects, including",
"or from the neutral hydrogen in the intergalactic medium (e.g."
] | [
"Background",
"Background"
] | [
[
1348,
1368
]
] | [
[
1033,
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[
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2022AandA...663A..50B__Seibert_et_al._2005_Instance_1 | In the absence of dust, the spectral emission of a normal star-forming galaxy is dominated by stellar populations of different ages with superimposed nebular emission, mainly in the form of recombination lines as well as continuum. The interaction with dust has a dramatic effect, both dimming and reddening the emission... | [
"Seibert et al. 2005"
] | [
"While this approach initially appeared to work remarkably well in the case of starburst galaxies",
"there is now ample evidence that there is no tight universal relation between the UV slope and the"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2028,
2047
]
] | [
[
1773,
1869
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[
1892,
1990
]
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2021MNRAS.501.4148L__Hatzes_2014_Instance_1 | If the separation between the period of the planet and all the other periodic signals is large enough, and the RV signal has a similar or larger semi-amplitude, it is possible to determine the RV semi-amplitude for a USP planet without any assumptions about the number of planets in the system or the activity of the hos... | [
"Hatzes 2014"
] | [
"Such an approach, also known as floating chunk offset method (FCO;",
"has proven extremely reliable even in the presence of complex activity signals, as shown by Malavolta et al. (2018)."
] | [
"Uses",
"Compare/Contrast"
] | [
[
906,
917
]
] | [
[
839,
905
],
[
920,
1036
]
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2016ApJ...832...57P__Vasquez_&_Markovskii_2012_Instance_1 | We employ two types of kinetic codes, hybrid particle-in-cell (PIC) and full PIC simulations. Both types make use of the P3D family of codes (Zeiler et al. 2002), in hybrid PIC (e.g., Parashar et al. 2011) mode, and fully kinetic PIC mode (e.g., Wu et al. 2013b). All simulations discussed here are performed in the 2.5D... | [
"Vasquez & Markovskii 2012"
] | [
"The initial condition is the Orszag–Tang vortex (OTV) (e.g.,"
] | [
"Uses"
] | [
[
1196,
1221
]
] | [
[
1069,
1129
]
] |
2016ApJ...819...51L__Svensson_et_al._2010_Instance_1 | Further diagnostics are clearly needed to form firm conclusions. There are likely to be three routes through which this can come. The first is via spectroscopy of the bumps in any further examples. High quality spectroscopy, allied to detailed modeling can yield diagnostics even in the case of relatively weak or featur... | [
"Svensson et al. 2010"
] | [
"In the case of GRBs, approximately 1/6 of examples are consistent with a galaxy nucleus"
] | [
"Compare/Contrast"
] | [
[
1162,
1182
]
] | [
[
1051,
1138
]
] |
2017MNRAS.468.2206M__Ceplecha_(1951)_Instance_1 | The first identification of a possible meteor shower with a radiant point in the constellation of Ursa minor was by Denning (1912), occurring around the winter solstice. However, very few observations were subsequently made. Hoffmeister recorded its activity in 1914, but its existence was not confirmed until 1945 (Becv... | [
"Ceplecha (1951)"
] | [
"showed that the annual Ursid shower was related to comet 8P/Tuttle, a Jupiter family comet with a period of 13.6yr (JPL-HORIZONS, ssd.jpl.nasa.gov) and a perihelion distance slightly greater than 1au."
] | [
"Background"
] | [
[
759,
774
]
] | [
[
775,
975
]
] |
2019ApJ...879...52S__Wei_et_al._2010_Instance_1 | The lack of data at complementary wavelengths also makes resolved multiwavelength analyses applied to low-redshift galaxies, such as the Schmidt–Kennicutt relation (the correlation between galaxies’ SFR and gas mass surface densities; e.g., Schmidt 1959; Kennicutt 1989, 1998), significantly less common at high redshift... | [
"Wei et al. 2010"
] | [
"High-resolution CO observations are critical for evaluating where high-redshift galaxies fall on the true surface density version of the Schmidt–Kennicutt relation, where ΣSFR and Σgas can be compared on a pixel-by-pixel basis within individual galaxies (as done for local galaxies; e.g.,"
] | [
"Motivation"
] | [
[
660,
675
]
] | [
[
322,
610
]
] |
2022AandA...665A..68M__Kempen_et_al._2009_Instance_1 | Within a star-forming cloud core, the protostar is the main source of luminosity and heat due to the release of gravitational energy from contraction and material accretion. The amount of protostellar heating dictates the temperature structure of the cloud core. In an idealized spherical scenario, the temperature alone... | [
"van Kempen et al. 2009"
] | [
"Studies have shown that heating mainly escapes through the outflow cavity in deeply embedded sources"
] | [
"Background"
] | [
[
817,
839
]
] | [
[
715,
815
]
] |
2022MNRAS.515.2188H__Rorai_et_al._2018_Instance_3 | In this work, we follow the method for measuring the IGM thermal state based on Voigt profile decomposition of the Ly α forest (Schaye et al. 1999; Ricotti et al. 2000; McDonald et al. 2001). In this approach, a transmission spectrum is treated as a superposition of multiple discrete Voigt profiles, with each line desc... | [
"Rorai et al. 2018"
] | [
"Secondly, in practice, determining the location of the cutoff is vulnerable to systematic effects, such as contamination from the narrow metal lines"
] | [
"Background"
] | [
[
2097,
2114
]
] | [
[
1929,
2077
]
] |
2022AandA...666A..44K__Martig_et_al._2009_Instance_1 | Meanwhile, the quiescence of the stellar disks (albeit possibly not entirely passive), is the first indication of the presence of an apparent “outside-in” quenching mode in high-redshift massive galaxy populations, in contradiction to the classic “inside-out” configuration (Lang et al. 2014; Tacchella et al. 2015; Bred... | [
"Martig et al. 2009"
] | [
"The process of morphological quenching",
"where the formation of a stellar bulge stabilizes the disk against further star-formation, is also improbable."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
852,
870
]
] | [
[
812,
850
],
[
873,
983
]
] |
2021ApJ...921...19W__Arcones_&_Montes_2011_Instance_1 | The abundances for cold and hot tracers with different Ye treatments are shown in Figure 12 for model s15_F120_R006. In general, the abundances for cold and hot tracers show a clear iron peak. The cold component is characterized by the odd–even distribution from carbon to calcium, following the progenitor composition. ... | [
"Arcones & Montes 2011"
] | [
"The production of elements in the region of Sr, Y, and Zr is more efficient for slightly neutron-rich conditions, corresponding to RLn = 1.35",
"We observe a very similar behavior and dependency of abundances on the Ye distribution for all exploding models of the 15 M⊙ progenitor."
] | [
"Uses",
"Similarities"
] | [
[
780,
801
]
] | [
[
637,
778
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[
826,
962
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2022MNRAS.513L..78D__Marcos_2020_Instance_1 | The fields targeted by our proof-of-concept mini-survey were observed at relatively high airmasses (see Section 2). Therefore, it can be argued that our null result could be due to enhanced extinction caused by observing at such low elevations. However, this is likely not the case because the same EURONEAR collaboratio... | [
"de la Fuente Marcos & de la Fuente Marcos 2020"
] | [
"Atiras or Interior Earth Objects (IEOs) have aphelion distances 0.983 au and can only be observed at low solar elongations (often 70○); Vatiras have aphelia 0.718 au, are observed at very low solar elongations (typically 40○–45○), and just one such object is currently known"
] | [
"Background"
] | [
[
819,
865
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] | [
[
524,
798
]
] |
2017MNRAS.469.4933L__Friedmann_et_al._1996_Instance_1 | IC 59 has a lower surface brightness than IC 63, which may be the result of both lower column densities as well as a larger physical distance from the illuminating star (Blouin et al. 1997; Karr, Noriega-Crespo & Martin 2005) compared to IC 63. Because of their rare illumination geometry and proximity to Earth, these t... | [
"Friedmann et al. 1996"
] | [
"The distances of the nebulae from the illuminating star are about 1 pc, assuming that they are located near the plane of the sky occupied by γ Cas"
] | [
"Uses"
] | [
[
979,
1000
]
] | [
[
831,
977
]
] |
2021MNRAS.501.3046F__Thorstensen_et_al._1991_Instance_1 | Cataclysmic variables (CVs) are strong interacting binaries. They are systems with an accreting white dwarf (WD, the primary) and a red dwarf (the donor). The donor star is on a late-type main sequence, or sometimes in a slightly evolved state. An accretion disc forms and accreted material reaches the WD in the case in... | [
"Thorstensen et al. 1991"
] | [
"NLs have high accretion rates (∼10−8 M⊙ yr−1), so are in a persistent high state, and they gather above the period gap in the period distribution of CVs"
] | [
"Background"
] | [
[
1033,
1056
]
] | [
[
879,
1031
]
] |
2018ApJ...856..136P__Pingel_et_al._2013_Instance_1 | Depending on the specific driver, the characteristics of turbulence will then be imprinted within the ISM mainly as three-dimensional density and velocity fluctuations, and these fluctuations have been traditionally studied via correlation functions such as the spatial power spectrum (SPS) (e.g., Crovisier & Dickey 198... | [
"Pingel et al. 2013"
] | [
"In particular, the SPS approach has been applied to observations of various Galactic and extragalactic environments (e.g.,",
"showing power spectral slopes β roughly ranging from −2.7 to −3.7 depending on the tracers used (e.g., H i, carbon monoxide (CO), and dust)."
] | [
"Background",
"Compare/Contrast"
] | [
[
684,
702
]
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[
438,
560
],
[
705,
845
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] |
2022MNRAS.517..130P__Navarro,_Frenk_&_White_1996_Instance_1 | The catalogue represents a luminosity-complete sample of galaxies with r-band absolute magnitude Mr ≤ −19 in a (300h−1Mpc)3 comoving volume at z = 0. The mock contains both central and satellite galaxies, populated in dark matter haloes identified in an N-body simulation having 10243 particles with a flat ΛCDM WMAP7 co... | [
"Navarro, Frenk & White 1996"
] | [
"Since the halo concentration cannot be reliably measured for haloes with fewer than about ∼400 particles, we use the method presented by Ramakrishnan, Paranjape & Sheth (2021) to assign concentrations cvir (assuming",
"NFW profiles) conditioned on the mass and local tidal environment of individual haloes."
] | [
"Uses",
"Uses"
] | [
[
698,
725
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] | [
[
482,
697
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[
727,
814
]
] |
2015ApJ...805..163D__Liang_et_al._2010_Instance_1 | In the field of GRBs, evidence of PFD jets has been collected independently in several directions. First, a prominent thermal emission component as expected in the fireball-internal-shock model (e.g., Mészáros & Rees 2000) has been seen only in a small fraction of GRBs (e.g., GRB 090902B, Ryde et al. 2010; Zhang et al.... | [
"Liang et al. 2010"
] | [
"Finally, the MFD internal shock (IS) model for GRBs also suffers some criticisms, such as",
"and inconsistency with some empirical (Amati/Yonetoku) relations"
] | [
"Differences",
"Differences"
] | [
[
1618,
1635
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] | [
[
1221,
1310
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[
1529,
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2021AandA...655A..72S___2019_Instance_3 | 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"
] | [
"their projected axis is oriented perpendicular to the disk midplane whose inclination with respect to the line-of-sight was estimated to be less than 30° (namely, the disk is seen approximately edge-on;"
] | [
"Background"
] | [
[
1699,
1711
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[
1718,
1722
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[
1496,
1698
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2018MNRAS.477.3520L__Abolfathi_et_al._2018_Instance_3 | Over time, the data releases have treated the Balmer line regions in different ways. The presence of the artificial curvature was first reported by Busca et al. (2013) in the context of the DR9 data release. To minimize this effect, a different scheme was used in DR12 (Alam et al. 2015, see their table 2) by using a li... | [
"Abolfathi et al. 2018"
] | [
"data release as well as calibration vectors for the MaNGA survey",
"DR14 data release",
"in Fig. 6.",
"In the upper panel, we show small-scale features in calibration vectors from the same plate (number 3647) processed by the DR9 (blue), DR12 (green), and DR14 (red) pipelines. The spectra are obtained by nor... | [
"Uses",
"Uses",
"Uses",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1138,
1159
]
] | [
[
1034,
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[
1119,
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[
1161,
1171
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[
1172,
1765
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[
1786,
1937
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] |
2020AandA...640L..11B__Segretain_1996_Instance_2 | Another possibly important cooling delay may arise from the phase separation of 22Ne during crystallization (Isern et al. 1991; Althaus et al. 2010). Our current best understanding is that at the small 22Ne concentrations typical of C/O white dwarfs (∼1% by number), the presence of 22Ne should not affect the phase diag... | [
"Segretain 1996"
] | [
"Given our very limited knowledge of the ternary C/O/Ne phase diagram",
"this effect cannot be quantitatively implemented in our evolution models.",
"However, we note that our current understanding of 22Ne phase separation is remarkably consistent with the missing cooling delay."
] | [
"Differences",
"Differences",
"Similarities"
] | [
[
1176,
1190
]
] | [
[
1106,
1174
],
[
1213,
1286
],
[
1287,
1416
]
] |
2016MNRAS.462.1508G__Gaur_et_al._2012c_Instance_1 | The new sample of HSPs gave us an opportunity to see the optical IDVs of HSPs and compare its properties with optical IDVs of LSPs. We started a dedicated project to search for optical IDV in HSPs and after doing 62 nights of IDV observations of HSPs which gave us 144 LCs (41 in B band, 62 in R band, and 41 in B−R colo... | [
"Gaur et al. 2012",
"c"
] | [
"Interestingly, we found that, four HSPs did not show any IDV"
] | [
"Compare/Contrast"
] | [
[
497,
513
],
[
515,
516
]
] | [
[
408,
468
]
] |
2018AandA...616L...2K__Frew_et_al._(2016)_Instance_2 | The distances to planetary nebulae (PNe) have always faced the difficulty that nearby targets were lacking that could be reached well by direct methods. Trigonometric parallaxes have been obtained in a homogeneous long time-line campaign by the US Naval Observatory (USNO; Harris et al. 2007) and from the Hubble Space T... | [
"Frew et al. (2016)"
] | [
"The newest model developed by",
"is based on similar ideas, but makes use of the optical Hα surface brightness and a wide set of various calibrators."
] | [
"Background",
"Background"
] | [
[
1523,
1541
]
] | [
[
1493,
1522
],
[
1542,
1658
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2020MNRAS.498.1801K__Hosler,_Jensen_&_Goldshlak_1957_Instance_1 | Water ice is ubiquitous in the cold regions of the Universe, owing to the fact that hydrogen and oxygen are the two most abundant elements to form a solid such as icy dust particles and comets. It is, therefore, commonly accepted that the essential component of dust particles and planetesimals in protoplanetary discs i... | [
"Hosler, Jensen & Goldshlak 1957"
] | [
"It is worthwhile noting that laboratory experiments on the coagulation growth of water-ice particles have a long history outside astronomy and planetary science, since coagulation is observed in daily life and is a plausible route to the formation of snowflakes (e.g."
] | [
"Background"
] | [
[
1024,
1055
]
] | [
[
742,
1009
]
] |
2017ApJ...835...79S__Wilson_et_al._1974_Instance_1 | The PN central white dwarf generates a significant ultraviolet (UV) radiation field during its transition from the proto-PN stage to the PN stage, typically ∼105 times that of the general interstellar medium (ISM), but decreasing to 10–100 as the remnant envelope expands and the luminosity of the white dwarf declines (... | [
"Wilson et al. 1974"
] | [
"Indeed, the first molecular searches of PNe turned up negative (e.g.,"
] | [
"Background"
] | [
[
612,
630
]
] | [
[
521,
590
]
] |
2019MNRAS.485.4343C__its_2018_Instance_1 | As of 2018, three multimeasurement catalogues including a substantial amount of redshift-independent extragalactic distance measurements have been released: HyperLEDA (Makarov et al. 2014), NED-D (Mazzarella & Team 2007; Steer et al. 2017), and Cosmicflows-3 (Tully, Courtois & Sorce 2016). HyperLEDA includes a homogeni... | [
"Mazzarella & Team (2007)"
] | [
"Treatment of errors for combining distance moduli across methods or across measurements is suggested by",
"and Tully et al. (2016) to be based on weighted estimates such as the uncertainty of the weighted mean, albeit with caution partly due to the heterogeneous origin of the compiled data and partly due to Malm... | [
"Uses",
"Uses"
] | [
[
1359,
1383
]
] | [
[
1255,
1358
],
[
1384,
1601
]
] |
2019MNRAS.486.5239D__Galli_et_al._2014_Instance_1 | The emission from both types of sources contaminates measurements of the Cosmic Microwave Background (CMB), which contains information on cosmological parameters. The measurement of the CMB polarization, particularly the E-mode damping tail, can help break some of the degeneracies between cosmological parameters. Measu... | [
"Galli et al. 2014"
] | [
"Further, the higher contrast of the acoustic features in EE power spectrum compared to astrophysical foregrounds",
"will ultimately provide independent and tighter constraints on the standard cosmological parameters, such as the scalar spectral index ns, than those from the temperature data alone."
] | [
"Future Work",
"Future Work"
] | [
[
690,
707
]
] | [
[
553,
665
],
[
709,
891
]
] |
2022MNRAS.511.3477E__Carter_&_Erdélyi_2008_Instance_1 | It has been cleared out in the observations that a coronal flux tube could consist of a twisted magnetic field (e.g. Kwon & Chae 2008; Aschwanden et al. 2012; Thalmann et al. 2014; Wang et al. 2015). In a magnetically twisted flux tube, the background magnetic field has an azimuthal component which causes the magnetic ... | [
"Carter & Erdélyi 2008"
] | [
"The role of twisted magnetic field in the MHD waves has been studied in many theoretical works (e.g."
] | [
"Background"
] | [
[
716,
737
]
] | [
[
516,
616
]
] |
2021MNRAS.506.5015H__Weinberg,_Miller_&_Lamb_2001_Instance_1 | Based purely on quality of fits of atmosphere model spectra to observed spectra obtained here, one composition is not preferred over another for the three older CCOs. The primary differences in fit results when the atmosphere is composed of carbon instead of hydrogen are a ∼40 per cent lower temperature and ∼3 times la... | [
"Weinberg, Miller & Lamb 2001"
] | [
"However, a hot region with radius 3–4 times smaller than R can still produce a pulsed fraction below current limits of 20–40 per cent in the spin period range 0.1–0.4 s of known CCOs (see Section 1; for pulsed fraction dependence on spot size, see, e.g."
] | [
"Uses"
] | [
[
977,
1005
]
] | [
[
664,
917
]
] |
2017MNRAS.469.2720G__Hernández-García_et_al._2015_Instance_1 | With all this in mind, our last question is: What powers soft X-rays and [O III] in LINERs? This has no clear answer, but both are not tracing the same mechanism, since none of them match in morphologies. This is a clear difference between type-2 Seyferts and LINERs. In favour of the soft X-ray emission being originate... | [
"Hernández-García et al. 2015"
] | [
"Indeed, the ultraviolet and X-ray variability detected for many of these LINERs",
"is in favour of a direct view of the AGNs (i.e. perpendicular to the disc under the UM). This is consistent with the fact that most of the [O III] morphologies found for LINERs are spheroids, if we assume that the [O III] traces t... | [
"Similarities",
"Similarities"
] | [
[
1078,
1106
]
] | [
[
979,
1058
],
[
1108,
1345
]
] |
2020AandA...642A.140G__Guilera_et_al._(2019)_Instance_1 | In addition, we also perform two new simulations changing the type I migration recipes from those of Tanaka et al. (2002) to those of Paardekooper et al. (2011) and Jiménez & Masset (2017). With this, we want to analyze whether or not the planet migration trap could be a robust result even using more sophisticated type... | [
"Guilera et al. (2019)"
] | [
"showed that the main differences between the migration recipes from Jiménez & Masset (2017) and Paardekooper et al. (2011) lie in the computation on the corotation torque."
] | [
"Compare/Contrast"
] | [
[
1673,
1694
]
] | [
[
1695,
1866
]
] |
2022AandARv..30....6M__Ellison_et_al._2015_Instance_1 | In particular, two main scenarios have emerged: the first one attributes differences in radio morphology to the large-scale (i.e., host galaxy and environment, see also below in this Section) properties of radio-AGN which influence the interaction between the radio jet and the external medium (e.g., Kaiser and Best 200... | [
"Ellison et al. 2015"
] | [
"According to this framework, HERGs are powered by accretion of cold gas, provided by e.g., a recent merger with a gas-rich galaxy, while LERGs accrete hot intergalactic gas from dense environments at a low rate",
"with fuelling from major mergers strongly disfavoured by recent observations (e.g.,"
] | [
"Background",
"Background"
] | [
[
836,
855
]
] | [
[
510,
720
],
[
752,
835
]
] |
2020MNRAS.494.1045B__Raymond_et_al._2009_Instance_1 | In our simulations, we assumed that the growth of dust grains and planetesimals occurred during the first stages of planetary accretion. Thus, we used a bimodal disc composed of embryos (60 per cent of the disc’s mass) and planetesimals (40 per cent of the disc’s mass; Izidoro et al. 2015). It was assumed that embryos ... | [
"Raymond et al. 2009"
] | [
"he protoplanetary embryos masses scale as M ≈ r3(2 − x)/2Δ3/2",
"where Δ is the mutual Hill radii separations between embryos orbits."
] | [
"Uses",
"Uses"
] | [
[
782,
801
]
] | [
[
670,
731
],
[
825,
893
]
] |
2017MNRAS.469S.731L__Kolokolova_&_Kimura_2010_Instance_1 | The specific radiance received from the optically thin dust plume can be expressed as
(1)
\begin{equation}
L_\lambda =f_{\rm plume}\frac{p}{\pi } \frac{\phi (\alpha )}{\phi (0)} \frac{f_{\lambda }}{r_{\rm h}{^2}}
\end{equation}
where p is the geometric albedo of the dust particles at wavelength λ, ϕ(α) is the phas... | [
"Kolokolova & Kimura 2010"
] | [
"The flux ratio ϕ(α)/ϕ(0) can be derived by using the dust phase function"
] | [
"Uses"
] | [
[
896,
920
]
] | [
[
822,
894
]
] |
2016MNRAS.455..552B__Riess_et_al._1998_Instance_1 | The plethora of cosmological observations has turned cosmology into a quantitative science. From combining several probes that observe the Universe at different epochs and have different systematics and statistics, emerged the ‘concordance model’ of cosmology, a six parameter model, most of them measured to the accurac... | [
"Riess et al. 1998"
] | [
"Several SNe surveys have set strong constraints on cosmological models from the distance–redshift relation (e.g.",
"However the measured apparent magnitudes, have a residual scatter arising from its intrinsic scatter and effects due to line-of-sight (LOS) structures."
] | [
"Background",
"Background"
] | [
[
752,
769
]
] | [
[
639,
751
],
[
859,
1010
]
] |
2015MNRAS.451.2123T__King_&_Begelman_1999_Instance_1 | The results of Ivanova et al. (2003) are somewhat closer to ours. A remaining key difference is that Ivanova et al. (2003) find that their calculated mass-transfer rates for systems with initial orbital periods, Porb, i 0.4 d sometime exceed a critical mass-transfer rate, $\dot{M}_{\rm crit}$ related to the location o... | [
"King & Begelman 1999"
] | [
"In systems with very large super-Eddington mass-transfer rates, matter presumably piles up around the NS and forms a growing, bloated cloud engulfing a large fraction of the accretion disc. A system will only avoid a CE if it manages to evaporate the bulk of the transferred matter via the liberated accretion energ... | [
"Compare/Contrast"
] | [
[
992,
1012
]
] | [
[
420,
990
]
] |
2018MNRAS.478.2541F__Smith_&_Tombleson_2015_Instance_1 | Utilizing the full range of peak absolute magnitudes observed in LBV stars [M ≃ (−13)–(−9) mag; e.g. Smith et al. 2011b] provides a range of peak apparent magnitudes of m ≃ 16.5–20.5 mag, for a distance of D ≃ 8 Mpc (Table 1). Hence, if the transient source (m ≈ 21.0 mag; Section 2.1.2) is an LBV star, it must have b... | [
"Smith & Tombleson 2015"
] | [
"An LBV star provides an adequate explanation for the transient time-scale, the isolation (e.g.",
"the lack of a host H ii region (Fig. 2 and 3; see below, however), and the transient/main source offset (d ≈ 0.3 kpc, for D ≃ 8 Mpc; Table 1; see below, however)."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
647,
669
]
] | [
[
552,
646
],
[
684,
846
]
] |
2020MNRAS.494.5270Z__Pesnell,_Thompson_&_Chamberlin_2012_Instance_1 | In particular, the presence of slow magneto-acoustic-gravity waves (MAG waves, hereafter) guided by the magnetic field is supported by increasingly observational evidence in different atmospheric structures, e.g. photospheric flux tubes (Roberts & Ulmschneider 1997), sunspots (Jess et al. 2013; Freij et al. 2014; Khome... | [
"Pesnell, Thompson & Chamberlin 2012"
] | [
"As a result of the analysis of 3 min oscillations detected in observations from the Atmospheric Imaging Assembly instrument",
"on-board the Solar Dynamic Observatory (SDO;"
] | [
"Background",
"Background"
] | [
[
741,
776
]
] | [
[
547,
670
],
[
696,
740
]
] |
2021AandA...647A.144A__Bretherton_1966_Instance_2 | Understanding how inertial waves interact with co-rotation resonances is thus a key issue in quantifying tidal dissipation, especially since waves may deeply interact with the background flow at this particular location, which in turn may alter the background flow (as was proposed first by Eliassen & Palm 1961, for ter... | [
"Bretherton 1966"
] | [
"These studies all used an invariant quantity (the Reynolds stress or thewave action for rotating or magnetic flows) as a diagnostic tool to interpret the role of the critical level in terms of energy transmission and to quantify exchanges between the wave and the mean flow"
] | [
"Background"
] | [
[
2353,
2368
]
] | [
[
2056,
2329
]
] |
2018AandA...618A.145O__Codella_et_al._2016_Instance_1 | The chemical composition of protostellar envelopes and their properties along the evolutionary stage of protostars is an important topic in astrochemistry. Since the pioneering work by Cazaux et al. (2003) and Sakai et al. (2008), systematic chemical studies of solar-type protostars (see Ceccarelli et al. 2007; Caselli... | [
"Codella et al. 2016"
] | [
"Only a few hot corinos have been identified so far either with single dish or interferometric observations:",
"HH212"
] | [
"Background",
"Background"
] | [
[
987,
1006
]
] | [
[
687,
794
],
[
980,
985
]
] |
2022AandA...664A.117D__Peters_et_al._2015_Instance_1 | We mentioned that our light curves are characterized by two large gaps of one year and seven months plus eight months, as shown in Table 1. From the table, it is apparent that mean and median observed baseline values, computed for the sources in the main sample for each season, are very close to the maximum observed ba... | [
"Peters et al. 2015"
] | [
"Sparse and/or irregular sampling is a very common issue in SF analysis"
] | [
"Motivation"
] | [
[
986,
1004
]
] | [
[
886,
956
]
] |
2019AandA...631A.106S__Bordé_&_Traub_2006_Instance_1 | With a priori knowledge of speckle evolution lifetime (Milli et al. 2016), more evolved a posteriori algorithms may well calibrate the speckle pattern. However, any such method can directly benefit from an active technique that minimizes the static or quasi-static speckles in each science image during an observation. A... | [
"Bordé & Traub 2006"
] | [
"Active suppression of these speckles requires measurement of the electric field associated with the speckles directly from a coronagraphic image using a focal plane wavefront sensor (FPWFS). Several FPWFSs have been proposed such as phase diversity"
] | [
"Background"
] | [
[
569,
587
]
] | [
[
319,
567
]
] |
2015MNRAS.447.3243M__Middleton_et_al._2011b_Instance_1 | Ultraluminous X-ray sources (ULXs) have been widely observed in the local Universe, with inferred isotropic luminosities above 1039 erg s−1 (Roberts 2007; Feng & Soria 2011). Those below ∼3 × 1039 erg s−1 can be readily associated with accretion on to stellar mass black holes (BHs) (∼10 M⊙) accreting close to or at the... | [
"Middleton et al. 2011b"
] | [
"Observations of such ‘low-luminosity’ ULXs",
"have revealed changes in the disc emission that may imply the creation of a radiation pressure supported, larger scaleheight flow in the inner regions",
"or magnetic pressure support"
] | [
"Background",
"Background",
"Background"
] | [
[
845,
867
]
] | [
[
801,
843
],
[
912,
1062
],
[
1087,
1115
]
] |
2018ApJ...856...19N__Isern_et_al._1991_Instance_1 | Models of the ECSN progenitor cores suggest the onset of the electron-capture instability occurs at a unique ONeMg core mass in the mass range of 1.366–1.377 M⊙. (Miyaji et al. 1980; Nomoto 1984, 1987; Podsiadlowski et al. 2005; Takahashi et al. 2013). Electron captures cause the core to contract, and O and Ne burning ... | [
"Isern et al. 1991"
] | [
"Whether the core collapses or the deflagration disrupts the core depends sensitively on the ignition density"
] | [
"Uses"
] | [
[
726,
743
]
] | [
[
616,
724
]
] |
2019MNRAS.482..560M__Kong_et_al._2004_Instance_1 | An empirical expression for FUV extinction based on UV reddening of a diverse, UV-selected sample of 200 galaxies (Seibert et al. 2005) is
(10)
\begin{eqnarray*}
A_{\rm FUV}(\beta)=3.978(m_{\rm FUV}-m_{\rm NUV})+0.143,
\end{eqnarray*}
where mFUV and mNUV are the respective GALEX AB magnitudes.13 The equation is sim... | [
"Kong et al. 2004"
] | [
"This is consistent with other results (e.g.",
"which have shown that galaxies having higher current SFR relative to their past averaged SFR are likely to deviate above the IRX–β relation, i.e. have larger AFUV(IRX) for a given AFUV(β).",
"Despite this qualitative agreement, the Kong et al. mean numerical relat... | [
"Similarities",
"Similarities",
"Differences"
] | [
[
909,
925
]
] | [
[
865,
908
],
[
955,
1143
],
[
1144,
1339
]
] |
2020ApJ...888..118M__Soto_et_al._2013_Instance_1 | To determine foreground and background contamination by star-forming galaxies, AGNs, shock emission, and extended PAH emission, as well as field stars, we performed the infrared color selection method described in Gutermuth et al. (2009). In Phase I of this method, we used only GLIMPSE sources that have photometry in a... | [
"Soto et al. 2013"
] | [
"We excluded stars with saturated photometry",
"by limiting the magnitudes of the detected VISTA/VVV sources to 13.8, 12.8, and 12.8, for the J, H, and KS bands, respectively."
] | [
"Uses",
"Uses"
] | [
[
1867,
1883
]
] | [
[
1822,
1865
],
[
1886,
2013
]
] |
2019ApJ...875..129K__Kovtyukh_&_Andrievsky_1999_Instance_1 | Finally, the final estimates depend slightly on whether very strong lines with X > −6 are used or not. In Figure 7, very strong lines clearly show a systematic tilt. These strong lines have an impact on the slopes, e.g., seen in Figure 4. The lower
values of the stronger lines in MB99 would give higher
va... | [
"Kovtyukh & Andrievsky 1999"
] | [
"While this is an important difference between the two line lists, generally speaking, it is suggested that using very strong lines often introduces complications such as non-LTE effects into a chemical abundance analysis (e.g.,"
] | [
"Uses"
] | [
[
709,
735
]
] | [
[
481,
708
]
] |
2021AandA...647A.137J__Beccari_et_al._2017_Instance_1 | The advent of the ESA Gaia satellite for the first time allows the study of young stellar populations on large scales (> 100 pc) in six-dimensional (6D) position and velocity space. For example, using Gaia Data Release 2 (DR2) (Gaia Collaboration 2018a), Kounkel et al. (2018) and Zari et al. (2019) demonstrated that th... | [
"Beccari et al. 2017"
] | [
"For example, using Gaia Data Release 2 (DR2)",
"Kounkel et al. (2018) and Zari et al. (2019) demonstrated that the Orion star-forming region is composed of a variety of populations with different spatial and kinematic properties each that are all likely generated in multiple events instead of in a progressive st... | [
"Background",
"Background",
"Background"
] | [
[
551,
570
]
] | [
[
182,
226
],
[
255,
550
],
[
616,
687
]
] |
2020MNRAS.498.6013A__Tonry_1998_Instance_1 | In this section, we describe our new compilation of SLS. To construct Dobs, we have chosen only systems with spectroscopically data well measured from different surveys. We have considered 19 SLS from the CASTLES, 107 from SLACS, 38 from BELLS, 4 from LSD, 35 from SL2S, and 1 system from the DES survey. The final list ... | [
"Tonry 1998"
] | [
"Many systems have not been taken into account due to several issues. For instance, the system PG1115+080",
"from the CASTLES survey has been discarded because the lens mass model is steeper than isothermal."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
709,
719
]
] | [
[
603,
707
],
[
721,
819
]
] |
2019AandA...629A.134G__Groh_et_al._2008_Instance_1 | The shape of the spectral energy distribution and the emission rates of ionizing photons (see Table 1 of Paper II) depend on the assumed wind mass-loss rates, wind speeds, and wind clumping. These parameters are uncertain. Theoretical predictions are now available (e.g., Krtička et al. 2016; Vink 2017), but they have n... | [
"Groh et al. 2008",
"Groh et al. 2008"
] | [
"Theoretical predictions are now available",
"but they have not yet been thoroughly tested against observations, because only very few stripped stars with sufficiently strong wind mass-loss have been identified and studied in detail so far (e.g.,"
] | [
"Background",
"Background"
] | [
[
506,
522
],
[
1076,
1092
]
] | [
[
223,
264
],
[
305,
505
]
] |
2021AandA...647A.144A__Bretherton_1966_Instance_1 | Understanding how inertial waves interact with co-rotation resonances is thus a key issue in quantifying tidal dissipation, especially since waves may deeply interact with the background flow at this particular location, which in turn may alter the background flow (as was proposed first by Eliassen & Palm 1961, for ter... | [
"Bretherton 1966"
] | [
"More generally, a body of work in various domains,",
"to geophysical fluid dynamics (e.g.",
"has tried to understand the properties of wave propagation and dissipation around co-rotation and, more generally, at all special locations in fluids that correspond to singularities in the linear wave propagation equa... | [
"Background",
"Background",
"Background"
] | [
[
828,
843
]
] | [
[
619,
669
],
[
792,
827
],
[
870,
1093
]
] |
2018MNRAS.473.2000T__Noutsios_et_al._2011_Instance_1 | The launch of the Fermi Gamma-ray Space Telescope has spurred on the search for pulsars in γ-rays (Grenier & Harding 2015), yielding over 2001 detections and triggering multiwavelength observations. While pulsars are common targets in the X-rays, they are very challenging targets in the optical and very few of them hav... | [
"Noutsios et al. 2011"
] | [
"Here, we report on Large Binocular Telescope (LBT) observations of an isolated pulsar, PSR J2043+2740",
"detected by",
"and Fermi"
] | [
"Background",
"Background",
"Background"
] | [
[
602,
622
]
] | [
[
389,
490
],
[
525,
536
],
[
573,
582
]
] |
2015AandA...582A..88W__Lamberts_et_al._2013_Instance_1 | For completeness, we also supplement our reaction scheme with grain-surface association reactions extracted from the publicly available Ohio State University (OSU) network3 (Garrod et al. 2008). For those species important in grain-surface chemical reaction schemes, e.g., the CH3O radical, which are not included in Rat... | [
"Lamberts et al. 2013"
] | [
"The grain-surface network has been further updated to include all studied routes to water formation under interstellar and circumstellar conditions"
] | [
"Uses"
] | [
[
597,
617
]
] | [
[
427,
574
]
] |
2018AandA...612A..77M__Gromadzki_&_Mikołajewska_(2009)_Instance_3 | “Wiggling” outflows are often observed among young stellar jets and protostellar molecular outflows (Eisloffel et al. 1996; Terquem et al. 1999). Terquem et al. (1999) investigated such binary systems where the accretion disk, from which the jet originates, is inclined to the binary orbital plane. They concluded that t... | [
"Gromadzki & Mikołajewska (2009)"
] | [
"We estimated the projected spatial wavelength λproj of the “wiggling” wave according to λ = λproj∕sin i, where i is the angle between the jet symmetry axis and the line of sight, and T = λ∕υ, where υ is the jet velocity, from"
] | [
"Uses"
] | [
[
1898,
1929
]
] | [
[
1672,
1897
]
] |
2016MNRAS.463.3783B__Reid_&_White_2011_Instance_1 | It is well known that a per cent level understanding of the anisotropy of the redshift-space galaxy clustering is needed to accurately recover cosmological information from the RSD signal in order to shed light on the issue of dark energy versus modified gravity. From a statistical point of view, the source of the anis... | [
"Reid & White 2011"
] | [
"State-of-the-art PT has proven successful in predicting the large-scale behaviour of the velocity PDF and the correspondent monopole and quadrupole of the redshift-space correlation function (e.g",
", at least for massive haloes, M ∼ 1013 M⊙."
] | [
"Background",
"Background"
] | [
[
1430,
1447
]
] | [
[
1233,
1428
],
[
1473,
1516
]
] |
2021MNRAS.507.4389G__Masters_et_al._2011_Instance_3 | Erwin (2018) showed that, in a sample drawn from the Spitzer Survey of Stellar Structure in Galaxies (S4G), the bar fraction is constant over a range of (g −r) colours and gas fractions. Their bar fraction does not increase, but rather decreases for stellar masses higher than ∼ 109.7M⊙. These results are in contrast to... | [
"Masters et al. 2011"
] | [
"However, the addition of weak bars in low-mass blue galaxies is insufficient to resolve the apparent disagreement between Erwin (2018) and many SDSS-based studies",
"which instead seems likely to be due to the very different sample selection of the S4G and SDSS galaxy samples."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1272,
1291
]
] | [
[
1108,
1270
],
[
1357,
1468
]
] |
2020AandA...644A..59K__Heays_et_al._2017_Instance_1 | Analyzing optical emission lines, emanating from within the northern lobe, Tylenda et al. (2019) found a reddening with EB − V ≈ 0.9 mag or AV ≈ 2.8 mag, which we assume is mainly circumstellar in origin. Hajduk et al. (2013) observed two stars shining through the southern lobe and found AV = 3.3 − 4.4 mag with unknown... | [
"Heays et al. 2017"
] | [
"We recalculated the lifetimes of molecules assuming AV = 3 mag, and with (1) standard dust properties (i.e. with composition and size distribution as of interstellar dust) or (2) with larger and less opaque grains, at the gas-to-dust mass ratio of 124 (see",
"for more details on the assumed dust properties)."
] | [
"Uses",
"Uses"
] | [
[
776,
793
]
] | [
[
519,
775
],
[
795,
844
]
] |
2020MNRAS.493.3045B__Jaisawal_&_Naik_2015a_Instance_3 | We have used 3.0–75.0 keV NuSTAR data to probe any cyclotron line feature. To describe the continuum of 4U 1700–37, we have applied the NPEX model [cons*TBpcf*(powerlaw*npex+gaus+gaus)], following the previous work of Jaisawal & Naik (2015a). The NPEX model has been created by adding two cutoffpl models with their cuto... | [
"Jaisawal & Naik 2015a"
] | [
"The 10.0–70.0 keV flux of the source is found to be (2.26 ± 0.01) × 10−9 erg cm-2s-1, much lower than the value (5.6 ± 0.3) × 10−9 erg cm-2s-1, previously reported from SUZAKU data"
] | [
"Differences"
] | [
[
2007,
2028
]
] | [
[
1825,
2005
]
] |
2019AandA...627A.114K__Robitaille_2010_Instance_1 | In the main simulation, we modeled a Cartesian cube 2000 AU in size with 150 grid points in each direction. The cell size of 13.3 AU is comparable to the size of the star, which was represented by a point source. Clumps A to D were simulated as 3D structures of a Gaussian density profile. The choice of a Gaussian distr... | [
"Robitaille 2010"
] | [
"To speed them up, we used the Modified Random Walk method implemented in RADMC-3D"
] | [
"Uses"
] | [
[
894,
909
]
] | [
[
811,
892
]
] |
2015ApJ...800...24K___2012_Instance_1 | Analyzing the fraction of quenched galaxies for centrals and satellites as a function of stellar mass and environmental parameters has emerged as a fruitful way of gaining insights into the phenomenology and the physical processes of quenching. However, one of the difficulties in interpreting this fraction is that many... | [
"Peng et al. 2012"
] | [
"For example, there is good evidence",
"that the local overdensity correlates with the group-centric distance (e.g.,"
] | [
"Background",
"Background"
] | [
[
645,
662
]
] | [
[
443,
478
],
[
568,
644
]
] |
2015ApJ...813...20B__Kim_2001_Instance_1 | In our investigation we were looking for alignment of galaxy clusters in a sample of 1056 low redshift ACO clusters with known Bautz–Morgan type. We found a statistically significant effect for structures with separation distance 30 R ≤ 45 h−1 Mpc. This allowed us to conclude that, for the analyzed clusters, the effec... | [
"Kim 2001"
] | [
"One should note that during studies of the isolated Abell groups",
"only a rudimentary alignment was found and related only to the brightest cluster members."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
706,
714
]
] | [
[
599,
663
],
[
748,
837
]
] |
2018AandA...617A..86L__Tian_2017_Instance_1 | The IRIS spectra measure the flare in a “sit-and-stare” mode with a roll angle of 45∘. The spectral scale is ∼25.6 mÅ per pixel in the far-ultraviolet (FUV) wavelengths. The IRIS slit crosses the flaring loop and one ribbon (Fig. 1). Two red bars enclose the flaring loop region used to study the quasi-periodic oscillat... | [
"Tian 2017"
] | [
"We also manually perform the absolute wavelength calibration using a relatively strong neutral line, O I 1355.60 Å (see"
] | [
"Uses"
] | [
[
821,
830
]
] | [
[
659,
778
]
] |
2018ApJ...853...50F__Bernard_et_al._2015b_Instance_3 | However, using the well-assessed new post-AGB evolutionary models, we confined the main-sequence ages of our halo sample to be mostly ∼2–5 Gyr, with the oldest being ∼6–8 Gyr, while the outer-disk sample are mostly ≲1–4 Gyr. We thus conjecture that our targets probably formed prior to the encounter with M33. Obviously,... | [
"Bernard et al. 2015b"
] | [
"The extended star formation history and the broad range of metallicity (−1.5 ≲ [Fe/H] ≲ 0.2) discovered in the stream fields can be explained by a disk galaxy progenitor"
] | [
"Uses"
] | [
[
1570,
1590
]
] | [
[
1372,
1541
]
] |
2020AandA...641A.151S__Spinoglio_et_al._(2002)_Instance_1 | The galaxy NGC 7213 benefits from a detailed SED decomposition performed by G16, which allowed us to disentangle the relative contributions of AGN and SF activity to the global IR outcome of the source, providing a characterisation of the host galaxy in terms of stellar and dust content (M⋆ and Mdust, respectively), an... | [
"Spinoglio et al. (2002)"
] | [
"In the case of NGC 7213, the photometric data included in the analysis are:",
"and the FIR photometry by"
] | [
"Uses",
"Uses"
] | [
[
1033,
1056
]
] | [
[
658,
733
],
[
1007,
1032
]
] |
2020ApJ...897...84T__Zhang_et_al._2019_Instance_1 | A comparison between the constraints in Figure 2 and those found from the analysis of the reflection spectrum of the disk of other sources in previous studies is not straightforward because these measurements are quite sensitive to the specific source and the quality of the data, so it may be dangerous to generalize th... | [
"Zhang et al. 2019"
] | [
"However, such a degeneracy can be broken when the inner edge of the disk is very close to the compact object"
] | [
"Compare/Contrast"
] | [
[
647,
664
]
] | [
[
508,
616
]
] |
2016MNRAS.462.3441D__Namouni_1999_Instance_4 | In principle, Fig. 5, central panel G, shows that (469219) 2016 HO3 may have been locked in a Kozai–Lidov resonance with ω librating about 270° for nearly 100 kyr and probably more. Because of the Kozai–Lidov resonance, both e (central panel E) and i (central panel F) oscillate with the same frequency but out of phase ... | [
"Namouni (1999)"
] | [
"Asteroid 469219 librates around $\\omega _{\\rm r}=-90{^\\circ }$ for Venus, the Earth, and Jupiter. This behaviour corresponds to domain III in",
"horseshoe-retrograde satellite orbit transitions and librations (around $\\omega _{\\rm r}=-90{^\\circ }$ or 90°). For a given cycle, the lower part corresponds to t... | [
"Uses",
"Uses"
] | [
[
1491,
1505
]
] | [
[
1349,
1490
],
[
1507,
1760
]
] |
2016MNRAS.458...84A__Larsson_et_al._2007_Instance_1 | While the properties of the SLSN hosts themselves are of interest, they are most diagnostic when compared to other classes of extragalactic transient whose progenitors are better understood. To this end, we employ a comparison sample of LGRB and CCSN3 host galaxies. In principle, CCSNe should trace all core-collapse ev... | [
"Larsson et al. 2007"
] | [
"Indeed, constraints from explosion parameters have shown the majority of CCSNe to be consistent with lower mass progenitors, as opposed to more massive Wolf–Rayet stars",
"GRBs likely represent a population with rather larger initial masses"
] | [
"Background",
"Background"
] | [
[
978,
997
]
] | [
[
708,
876
],
[
908,
976
]
] |
2015AandA...582A..41H__Davis_et_al._2014_Instance_1 | The snowlines of various volatiles (sublimation temperature Tsub ≲ 160 K) play a major role for planet formation. Beyond the snowline, the high abundances of solids allow for efficient sticking to form larger bodies, which is further enhanced by the presence of ices (e.g., Stevenson & Lunine 1988; Ros & Johansen 2013).... | [
"Davis et al. 2014"
] | [
"It is thought that the early pre-solar nebula was hot (>1500 K), such that both volatiles and refractories (Tsub ≳ 1400 K) are in the gas phase out to larger distances"
] | [
"Background"
] | [
[
812,
829
]
] | [
[
618,
785
]
] |
2021MNRAS.506.2181L__Qi_et_al._2019_Instance_1 | There are still several sources of systematics we do not consider in this paper. For instance, whether the use of a different mass distribution models for these lenses could significantly affect the final result. Therefore, we performed a sensitivity analysis and repeated the above calculation using the extend power la... | [
"Qi et al. 2019"
] | [
"Such lens model has found widespread astrophysical applications in the literature"
] | [
"Background"
] | [
[
600,
614
]
] | [
[
482,
563
]
] |
2019AandA...629L...4A__Arzoumanian_et_al._2011_Instance_1 | Herschel imaging observations have shown that filamentary structures are truly ubiquitous in the cold interstellar medium (ISM) of the Milky Way (Molinari et al. 2010), dominate the mass budget of Galactic molecular clouds at high densities (≳104 cm−3) (Schisano et al. 2014; Könyves et al. 2015), and feature a high deg... | [
"Arzoumanian et al. 2011"
] | [
"In particular, detailed analysis of the radial column density profiles indicates that, at least in the nearby clouds of the Gould Belt, molecular filaments are characterized by a narrow distribution of crest-averaged inner widths with a typical full width at half maximum (FWHM) value Wfil ∼ 0.1 pc and a disper... | [
"Background"
] | [
[
710,
733
]
] | [
[
361,
708
]
] |
2016MNRAS.461..248S__Munari_et_al._2013_Instance_4 | In Sifón et al. (2013), we used the σ–M200 scaling relation of Evrard et al. (2008) to estimate dynamical masses. As discussed in Section 1, the scaling relation of Evrard et al. (2008) was calibrated from a suite of N-body simulations using DM particles to estimate velocity dispersions. However, the galaxies, from whi... | [
"Munari et al. 2013"
] | [
"The different cosmologies used in the Millenium simulation (in particular, σ8 = 0.9; Springel et al. 2005) by Saro et al. (2013) and the simulations by",
"σ8 = 0.8) may also play a role."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2611,
2629
]
] | [
[
2458,
2609
],
[
2631,
2662
]
] |
2021AandA...655A.109B__Foreman-Mackey_et_al._2013_Instance_1 | When the size of the logarithmic redshift bin is small enough, we can use fluxes in place of luminosities, performing a test on the (non-)evolution with redshift that is completely independent from any assumption on cosmology. Risaliti & Lusso (2019) analysed in detail the choice of the bin size and verified that, as l... | [
"Foreman-Mackey et al. 2013"
] | [
"To perform the fitting to the data, we adopted the Python package emcee",
", a pure-Python implementation of Goodman & Weare’s Affine Invariant Markov chain Monte Carlo (MCMC) Ensemble sampler."
] | [
"Uses",
"Uses"
] | [
[
916,
942
]
] | [
[
843,
914
],
[
943,
1061
]
] |
2019ApJ...887...75T__Stritzinger_et_al._2012_Instance_1 | Figure 6 compares the IR SED of SN 2014C with the SEDs of all other interacting SNe for which observations beyond 5 μm are available in the literature. Apart from SN 2014C, only four other strongly interacting SNe IIn have been observed in the mid-IR. Three of these were observed at epochs comparable to the epoch at wh... | [
"Stritzinger et al. 2012"
] | [
"SN 2006jd was observed at 1638 days, an epoch very similar to that of SN 2014C, with Spitzer/IRAC and WISE",
"In all three cases, the photometry and spectra from 1 to 10 μm are well fitted by purely carbonaceous dust models, which we overplot in Figure 6 using dust parameters from the literature."
] | [
"Uses",
"Similarities"
] | [
[
731,
754
]
] | [
[
623,
729
],
[
956,
1143
]
] |
2019ApJ...887..137S__Vekstein_2017_Instance_2 | As mentioned above, the magnetic reconnection is introduced as breaking and reconfiguration of the oppositely directed magnetic field lines in highly conducting plasma. The magnetic field lines collapse near the X-point and form an extended magnetic singularities known as a current sheet. There are two mechanism of the... | [
"Vekstein 2017"
] | [
"The motion of the photospheric footpoints of the coronal magnetic field may also trigger the forced magnetic reconnection, which may be caused by the explosive solar coronal events (e.g.,"
] | [
"Background"
] | [
[
1551,
1564
]
] | [
[
1323,
1510
]
] |
2018ApJ...866...48U__Korngut_et_al._2011_Instance_1 | RX J1347.5–1145 is one of the most luminous X-ray galaxy clusters and is located at a redshift of z = 0.451. It was thought to be a relaxed cluster when it was discovered in the ROSAT all sky survey (Schindler et al. 1997). Komatsu et al. (1999) made the first measurements of the Sunyaev–Zel’dovich effect (SZE: Sunyaev... | [
"Korngut et al. 2011"
] | [
"The presence of the substructure has been confirmed by",
"as well as by more recent SZE measurements"
] | [
"Background",
"Background"
] | [
[
894,
913
]
] | [
[
703,
757
],
[
831,
873
]
] |
2021MNRAS.505.4289P__Vila-Costas_&_Edmunds_1993_Instance_1 | For decades, the metallicity and the above chemical abundance ratios have been estimated in samples of star-forming galaxies (SFGs), by using their emission line ratios to calculate the abundances of the different elements that originate them. Many techniques were developed for such studies, such as the use of the Te-m... | [
"Vila-Costas & Edmunds 1993"
] | [
"By using these techniques, some studies show a correlation between both 12 + log (O/H) and log (N/O)"
] | [
"Background"
] | [
[
585,
611
]
] | [
[
483,
583
]
] |
2018MNRAS.478.4336M__Porter_&_Raychaudhury_2007_Instance_1 | Recently filaments, in particular the warm hot intergalactic medium (WHIM) in filaments, have been the pivot of several studies. Using emission in the soft X-ray bands, such studies estimate the WHIM temperature in filaments to be ∼3–8 keV (Eckert et al. 2015; Akamatsu et al. 2017; Parekh et al. 2017; Tanimura et al. 2... | [
"Porter & Raychaudhury 2007"
] | [
"Studies of clusters and groups at $z$ ∼ 0 have evidently shown that outskirts of groups and clusters",
"and filaments of galaxies",
"are favourable sites for galaxy transformations."
] | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
1984,
2010
]
] | [
[
1593,
1693
],
[
1957,
1982
],
[
2112,
2160
]
] |
2020AandA...643A..58B__Trujillo_et_al._2001_Instance_1 | Adaptive optics (AO, Roddier 1999) is a game changer in the quest for high-angular resolution, especially for ground-based astronomical observations that face the presence of wavefront aberrations introduced by the atmosphere (Roddier 1981). Thanks to AO, the point spread function (PSF) delivered by an optical instrume... | [
"Trujillo et al. 2001"
] | [
"Still, some correction residuals persist and render the AO PSF shape complex to model. Consequently, standard parametric models that reliably reproduce the seeing-limited PSFs, such as a Moffat function",
"become inefficient at describing the AO PSF."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
657,
677
]
] | [
[
453,
655
],
[
693,
737
]
] |
2020AandA...642A...2R__Hyder_&_Lites_1970_Instance_1 | Investigation of solar wind outflow velocities is generally performed by the analysis of UV spectrometric observations. The UVCS/SOHO instrument has provided H I Lyα spectral line data over a longer time than a whole solar activity cycle (1996–2012), giving the possibility of studying coronal dynamics in different acti... | [
"Hyder & Lites 1970"
] | [
"One of the methods based on the synergy between UV and WL observations is the Doppler dimming technique"
] | [
"Uses"
] | [
[
650,
668
]
] | [
[
545,
648
]
] |
2021AandA...647A..67B__Cao_2011_Instance_1 | Keeping in mind the caveats discussed in Sect. 4.2, a relation between the properties of the jet collimation region and the properties of the accretion disk is suggested by Figs. 5 and 6. According to theoretical models and simulations, both thin disks (e.g., Blandford & Payne 1982; Fendt 2006; Liska et al. 2019) and g... | [
"Cao 2011"
] | [
"This result is in broad agreement with models of jet launching from ADAFs (e.g.,",
"which predict the formation of a thin and mildly-relativistic outer layer."
] | [
"Similarities",
"Similarities"
] | [
[
1567,
1575
]
] | [
[
1486,
1566
],
[
1623,
1697
]
] |
2022AandA...659A..85F__Jeffries_et_al._2014_Instance_2 | We apply our analysis to five open clusters of ages between ∼10 and 100 Myr that were observed within GES (25 Ori, Gamma Vel, NGC 2547, NGC 2451 B, and NGC 2516). These clusters were selected because they cover the age interval in which the effect of radius inflation could be significant, allowing us to investigate how... | [
"Jeffries et al. 2014"
] | [
"Both clusters host two kinematically distinct populations"
] | [
"Background"
] | [
[
1085,
1105
]
] | [
[
1026,
1083
]
] |
2018ApJ...854...26L___2015a_Instance_3 | 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"
] | [
"More details can be found in our previous papers"
] | [
"Background"
] | [
[
1823,
1838
]
] | [
[
1773,
1821
]
] |
2020AandA...642A..24W__Willingale_&_Mészáros_2017_Instance_1 | Selected as part of ESA’s Cosmic Vision programme, Athena will study the evolution of large scale structure through the detection of WHIM filaments to trace the missing baryons in the local universe. Athena aims to measure the local cosmological baryon density in the WHIM to better than 10% and to constrain structure f... | [
"Willingale & Mészáros 2017"
] | [
"A bright X-ray background source such as",
"or a GRB (e.g.",
"can be used to detect the WHIM by producing absorption features in its energy spectra"
] | [
"Background",
"Background",
"Background"
] | [
[
1151,
1177
]
] | [
[
1060,
1100
],
[
1136,
1150
],
[
1179,
1264
]
] |
2021ApJ...910...78Z__Condon_et_al._2017_Instance_1 | The multiwavelength spectral data of 13 SNRs with hard γ-ray spectra. The γ-ray spectra are fitted with a hadronic model with the normalization of the individual spectrum as free parameters. The model assumes that protons have a single power-law energy distribution with an exponential high-energy cutoff. Note that the ... | [
"Condon et al. 2017"
] | [
"References for the observational data are as follows: RX J0852.0−4622:",
"GeV"
] | [
"Uses",
"Uses"
] | [
[
965,
983
]
] | [
[
592,
662
],
[
960,
963
]
] |
2015ApJ...803...17Z__Campbell_&_Lattanzio_2008_Instance_1 | The metallicity calculated for HD 212869 is higher than that estimated prior to using high-resolution spectra. The iron abundance is found to be [Fe/H] =
0.2 dex on the basis of ionized lines that are almost free from NLTE effects. The carbon abundance was found to be high in the atmosphere of HD 112869,
... | [
"Campbell & Lattanzio 2008"
] | [
"With the obtained abundances [C/Fe] = +2.2 dex and [C/N] = +1.15, HD 112869 occupies the region of CEMP-s stars on the plots [C/Fe] versus [Fe/H] and [C/N] versus [Fe/H] (see Figures 5 and 6 in"
] | [
"Uses"
] | [
[
583,
608
]
] | [
[
389,
582
]
] |
2021AandA...646A..96C__Brusa_et_al._2018_Instance_1 | AGN-driven outflows. Another possible effect of the AGN activity on the molecular gas is through outflows. This possibility is supported by observations of individual objects: For example, Carniani et al. (2017), Brusa et al. (2018) and Loiacono et al. (2019) find low gas fractions in powerful AGN at cosmic noon hostin... | [
"Brusa et al. (2018)"
] | [
"Another possible effect of the AGN activity on the molecular gas is through outflows. This possibility is supported by observations of individual objects: For example, Carniani et al. (2017),",
"and Loiacono et al. (2019) find low gas fractions in powerful AGN at cosmic noon hosting high-velocity molecular and i... | [
"Background",
"Background"
] | [
[
213,
232
]
] | [
[
21,
212
],
[
233,
366
]
] |
2022MNRAS.511.1121M__Reig_&_Nespoli_2013_Instance_3 | Critical luminosity (Lcrit) is the luminosity above which a state transition from subcritical to supercritical takes place. The subcritical state (LX Lcrit) is known to be the low luminosity state whereas the supercritical state is high luminosity state (LX > Lcrit) (Becker et al. 2012). The critical luminosity is cruc... | [
"Reig & Nespoli 2013"
] | [
"During the transition from the subcritical to the supercritical regime, sources show two different branches in their hardness–intensity diagram (HID) which are known as horizontal branch (HB) and diagonal branch (DB)"
] | [
"Background"
] | [
[
1545,
1564
]
] | [
[
1327,
1543
]
] |
2019ApJ...885...50W__Falgarone_et_al._2009_Instance_1 | The physical conditions within giant molecular clouds (GMCs) establish the initial conditions for star formation, thus understanding the factors that determine molecular cloud properties is of major interest. A correlation between the size and line width, of the form σv ∝ Rα with α ≈ 0.5, has long been noted in samples... | [
"Falgarone et al. 2009"
] | [
"This correlation, hereafter referred to as the R–σv relation, is usually interpreted as the result of turbulent motions in the interstellar medium on all scales"
] | [
"Background"
] | [
[
585,
606
]
] | [
[
399,
559
]
] |
2018ApJ...856...94Z__Bieber_et_al._1991_Instance_1 | Figures 8 and 9 show the effects of solar activity on the CR parallel λ∥ (blue line), perpendicular λ⊥ (red line), and radial mean free path λrr (gray line) for a proton with rigidity 445 MV (corresponding to a 100 MeV proton) for the inwardly and outwardly directed IMF, respectively. As described in Zank et al. (1998)... | [
"Bieber et al. 1991"
] | [
"Observation of magnetic fluctuations in the SW indicates that omnidirectional power spectra approach a k−1 wavenumber dependence and that low-frequency turbulence exhibits some sunspot cycle variability"
] | [
"Background"
] | [
[
1303,
1321
]
] | [
[
1099,
1301
]
] |
2020ApJ...892L..10Y__Macchi_2013_Instance_1 | In this section, we consider the plasma properties under the propagation of strong waves. In strong waves, the motion of electrons in the plasma becomes relativistic. However, different from free electrons that have a relativistic drift velocity in the direction of the incident electromagnetic wave (see Section 3.1), i... | [
"Macchi 2013"
] | [
"For a circular polarized wave, the dispersion relation in the laboratory frame is given by (e.g.,"
] | [
"Uses"
] | [
[
1075,
1086
]
] | [
[
964,
1061
]
] |
2016ApJ...822...37S__Freeman_et_al._2001_Instance_1 | Each pulsar system in this analysis was observed with XMM-Newton (Jansen et al. 2001), using the European Photon Imaging Camera (EPIC) with the pn detector in full frame mode with thin filters (the data from the MOS and RGS detectors had insufficient counts for analysis). PSR J0337 was observed on 2013 August 1 (observ... | [
"Freeman et al. 2001"
] | [
"We measured 164 ± 13 background-subtracted counts between 0.2 and 2.0 keV, as determined using calc_data_sum in Sherpa"
] | [
"Uses"
] | [
[
725,
744
]
] | [
[
605,
723
]
] |
2022AandA...667A..69S__Hut_1985_Instance_1 | Finally, it is worth noting that two-body relaxation and tidal interactions affect the IMF in different ways. The former causes mass segregation with higher-mass stars moving inward and lower-mass stars outward, which enables the lower-mass stars to evaporate from the cluster (see also, e.g., Chandrasekhar 1942; Spitze... | [
"Hut 1985"
] | [
"The cluster then forms a dense core of high-mass stars and once it starts to collapse, binaries form in the centre. These perturb their neighbours, and we begin to observe massive stars escaping from the mass segregated core"
] | [
"Background"
] | [
[
600,
608
]
] | [
[
353,
577
]
] |
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