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 |
|---|---|---|---|---|---|---|
2015MNRAS.449.1018Y__Essey_et_al._2010_Instance_1 | VHE gamma-rays from distant blazars suffer serious EBL absorption. For instance, the attenuation factor of the flux at ∼1 TeV emitted at z = 0.6 due to EBL absorption is ∼10−4 (Domínguez et al. 2011). If VHE gamma-rays from a blazar are produced in its jet, the intrinsic VHE spectrum after de-absorption would be very h... | [
"Essey et al. 2010"
] | [
"Alternatively, it is recently proposed that VHE gamma-rays from distant blazars may be the secondary gamma-rays produced in the rectilinear propagation of the UHECRs escaping from these blazars (e.g.",
"In the latter case, UHECRs interact with background photons, i.e. EBL photons and microwave background (CMB) p... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1079,
1096
]
] | [
[
857,
1056
],
[
1099,
1533
]
] |
2018ApJ...853...12M__Weaver_et_al._1978_Instance_1 | There are numerous models which lay down nucleosynthesis yields from CCSN explosions (Burbidge et al. 1957; Woosley & Weaver 1986, 1995; Thielemann et al. 1996; Heger & Woosley 2002, 2010; Rauscher et al. 2002; Kobayashi et al. 2006; Nomoto et al. 2006; Woosley & Heger 2007; Pignatari et al. 2015; Sukhbold et al. 2016)... | [
"Weaver et al. 1978"
] | [
"whereas KEPLER was used to evolve the star along zero age main sequence and calculate nucleosynthesis yields and light curves"
] | [
"Uses"
] | [
[
786,
804
]
] | [
[
659,
784
]
] |
2018AandA...617A..94L__Joblin_et_al._2018_Instance_1 | In an interstellar cloud the spatial transition from atomic to molecular gas takes place in photon dominated regions (PDRs; see reviews by Hollenbach & Tielens 1997, 1999), which are also a source of a significant fraction of the far-infrared emission from the Milky Way and other galaxies. Exterior to the PDRs the gas ... | [
"Joblin et al. 2018"
] | [
"The observational analysis of PDRs, H II regions, and IBLs has improved considerably since the availability of far-infrared spectroscopic data from the Herschel Space Observatory (see"
] | [
"Background"
] | [
[
1176,
1194
]
] | [
[
930,
1113
]
] |
2019AandA...630A.123K__Kohutova_&_Verwichte_2016_Instance_1 | The coronal rain plasma can be distinguished from the prominence material by looking at their trajectories and average speeds. The timescale on which the coronal rain forms following the heating onset is much shorter than for the quiescent scenario; in the studied event condensations appear 10 min after the reconnectio... | [
"Kohutova & Verwichte 2016"
] | [
"The timescale on which the coronal rain forms following the heating onset is much shorter than for the quiescent scenario; in the studied event condensations appear 10 min after the reconnection event, whereas observations of quiescent rain suggests it recurs in the same loop of the order of hours"
] | [
"Compare/Contrast"
] | [
[
464,
489
]
] | [
[
127,
425
]
] |
2022MNRAS.512.3828B__Dokkum_&_Franx_2001_Instance_1 | Understanding the redshift dependence of galaxy evolution requires disentangling the evolution of an individual galaxy within a population from the evolution in the average properties of the population as a whole (due to the continual addition of newly formed galaxies with different properties to the extant population)... | [
"van Dokkum & Franx 2001"
] | [
"An individual star-forming galaxy is expected to evolve along the relation of star-forming galaxies in the mass–size plane",
"while the average size of the population as a whole increases with decreasing redshift due to processes such as mergers",
"and ’puffing up’ due to strong active galactic nuclei (AGNs) f... | [
"Background",
"Background",
"Background",
"Background"
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[
1006,
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]
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[
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[
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[
862,
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[
957,
1004
]
] |
2020MNRAS.499.5562Z__Miller_2015_Instance_1 | One explanation for the low effective temperatures is that the TDE thermal emission does not originate from the accretion disc, but from an outflow supported by radiation pressure from the disc’s super-Eddington accretion rate (e.g. Loeb & Ulmer 1997; Strubbe & Quataert 2009; Lodato & Rossi 2011; Metzger & Stone 2016; ... | [
"Miller 2015"
] | [
"These outflows can explain the nearly constant temperatures inferred from the spectrum of optically bright TDEs"
] | [
"Similarities"
] | [
[
692,
703
]
] | [
[
554,
665
]
] |
2015MNRAS.452.2731S__Stroe_et_al._2013_Instance_2 | The H α studies of Umeda et al. (2004) and Stroe et al. (2014a, 2015) are tracing instantaneous (averaged over 10 Myr) SF and little is known about SF on longer time-scales and the reservoir of gas that would enable future SF. An excellent test case for studying the gas content of galaxies within merging clusters with ... | [
"Stroe et al. 2013"
] | [
"There is evidence for a few additional smaller shock fronts throughout the cluster volume"
] | [
"Background"
] | [
[
1362,
1379
]
] | [
[
1271,
1360
]
] |
2019AandA...632A..40D__Sánchez-Fernández_et_al._2017_Instance_1 | An extreme example of a rapid decay is V404 Cyg. The parameters of the long Porb system were chosen to be close to those of V404 Cyg, whose last outburst lasted only a couple of weeks and showed a pronounced disc outflow, conjectured to be a thermal wind (Muñoz-Darias et al. 2016). The mass in the disc at the onset of ... | [
"Sánchez-Fernández et al. 2017"
] | [
"In support, observations of V404 Cyg do indicate the source",
"and was enshrouded by rapidly varying Compton-thick outflowing material"
] | [
"Similarities",
"Similarities"
] | [
[
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]
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[
1061,
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2015ApJ...813..109D__Górski_et_al._2005_Instance_1 | Photometric Calibration: Photometric calibration was performed using the stellar locus regression technique (SLR: Ivezić et al. 2004; MacDonald et al. 2004; High et al. 2009; Gilbank et al. 2011; Coupon et al. 2012; Desai et al. 2012; Kelly et al. 2014). Our reference stellar locus was empirically derived from the glob... | [
"Górski et al. 2005"
] | [
"We segmented the sky into equal-area pixels using the HEALPix scheme"
] | [
"Uses"
] | [
[
1090,
1108
]
] | [
[
1020,
1088
]
] |
2015ApJ...801..103G___2014_Instance_2 | Within the framework of the fireball shock model, Pe'er et al. (2007) proposed a method to infer central engine parameters using observed data. With the measured temperature and flux of an identified thermal component in the spectrum, along with a flux ratio between thermal and non-thermal components, one may infer th... | [
"Preece et al. 2014"
] | [
"The derived central engine parameters are sometimes ad hoc or inconsistent. For instance, the analyses",
"and for GRB 130427A",
"led to a curious conclusion that the bulk Lorentz factor of the outflow of different layers are decreasing with time. This would lead to no, or at most very inefficient, internal sho... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
832,
851
]
] | [
[
670,
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[
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[
853,
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2021AandA...655A.111K__Rojas-Arriagada_et_al._(2019)_Instance_1 | Over the last decade, the radial and vertical dependences of the metallicity-alpha-element distribution have been studied in more and more detail with increasingly larger samples (e.g., Bensby et al. 2011; Anders et al. 2014; Nidever et al. 2014; Hayden et al. 2015; Queiroz et al. 2020). Figure 6 is mostly consistent w... | [
"Rojas-Arriagada et al. (2019)"
] | [
"Conversely,",
"observe two sequences in the inner regions."
] | [
"Differences",
"Differences"
] | [
[
1366,
1395
]
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[
1354,
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[
1422,
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2018ApJ...862..150H__Cudlip_et_al._1982_Instance_1 | In Figure 1, we show the archival 850 μm polarization data from the legacy program of SCUPOL with the JCMT (Matthews et al. 2009) (effective 20″ beam ∼0.76 pc). Matthews et al. (2009) collected the JCMT data toward the GC, where the B-field is sampled on a 10″ grid. The linearly polarized light from dust grains is freq... | [
"Cudlip et al. 1982"
] | [
"The thermal emission from the aligned dust grains is then polarized with polarization segments perpendicular to the field lines"
] | [
"Uses"
] | [
[
605,
623
]
] | [
[
476,
603
]
] |
2021ApJ...920..147Z__Schneider_1959_Instance_1 | Mainly four mechanisms are considered to be causing the observed solar radio wave emissions: two causing incoherent and two causing coherent emissions. Incoherent emissions can be due to bremsstrahlung and gyrosynchrotron radiation. In them, every electron radiates independent on the others. The total emission is simpl... | [
"Schneider 1959"
] | [
"The two coherent emission mechanisms are",
"and electron cyclotron maser (ECM) emissions"
] | [
"Background",
"Background"
] | [
[
750,
764
]
] | [
[
540,
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[
678,
722
]
] |
2021ApJ...909...65K__Marsh_et_al._2016_Instance_1 | As mentioned in the previous section, if a magnetized WD rotates with a misalignment between its magnetic field and rotation axes (similar configuration to a pulsar), it can emit a continuous GW. We already provided a detailed discussion on GWs emitted from WDs with different magnetic field geometries and strengths in ... | [
"Marsh et al. 2016"
] | [
"Nevertheless, there are examples of weakly magnetized WD pulsars, which can be explained even in the GR framework, e.g.",
"and AR Scorpii",
"where magnetic fields hardly affect their mass–radius relations."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1498,
1515
]
] | [
[
1325,
1444
],
[
1482,
1496
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[
1518,
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2015MNRAS.448..822X__Steinmetz_et_al._2006_Instance_1 | Various methods have been developed in the past to derive stellar atmospheric parameters from large number of medium-to-low resolution spectra (Recio-Blanco, Bijaoui & de Laverny 2006; Lee et al. 2008a, Wu et al. 2011). The approaches generally fall into two main categories of method (Wu et al. 2011): the minimum dista... | [
"Steinmetz et al. 2006"
] | [
"Both categories of method have been applied to large stellar spectroscopic surveys, including",
"RAVE"
] | [
"Background",
"Background"
] | [
[
502,
523
]
] | [
[
371,
464
],
[
496,
500
]
] |
2016ApJ...832...41M__Helled_et_al._2011_Instance_1 | We first discuss the relative bulk enrichment. From internal structure models one can derive the MZ necessary to reproduce the observed mass and radius, and—for the Solar System planets—the gravitational moments. Studies inferring in this way eZ,rel,int of transiting exoplanets have found that eZ,rel,int decreases with... | [
"Helled et al. 2011"
] | [
"A similar decrease of eZ,rel,int with increasing mass is found for the bulk metal content of Solar System giants",
"where the mass where eZ,rel,int reaches 1 is extrapolated to be at about 11 MJup."
] | [
"Similarities",
"Similarities"
] | [
[
958,
976
]
] | [
[
821,
933
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[
979,
1060
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2020ApJ...888...46C__Singh_et_al._1995_Instance_2 | The theoretical models mentioned above have made assumptions. The validity of these assumptions needs to be examined. Besides, all these models involve parameters to be determined. These problems could be better understood through numerical simulations. Hurlburt et al. (1994) performed a two-dimensional numerical simul... | [
"Singh et al. 1995"
] | [
"The scaling laws derived from the numerical simulations of downward overshooting",
"agree well with Zahn’s analytical model."
] | [
"Similarities",
"Similarities"
] | [
[
1239,
1256
]
] | [
[
1157,
1237
],
[
1284,
1324
]
] |
2020MNRAS.496.1718E__Wong_et_al._2019_Instance_2 | (i) Our capability of reproducing the lensed images down to the noise level without fully correctly modelling the cored central mass density distribution of the lenses indicates some form of the source-position transformation (SPT; Schneider & Sluse 2014), in line with the previous findings by Unruh et al. (2017). As a... | [
"Wong et al. 2019"
] | [
"Together with the findings of Blum et al. (2020), our results have important implications for the analysis of time delays and a potential solution to the H0 tension"
] | [
"Compare/Contrast"
] | [
[
2258,
2274
]
] | [
[
2092,
2256
]
] |
2015MNRAS.446.2468E__Choi,_Shlosman_&_Begelman_2013_Instance_1 | The equations of motions and hydrodynamics are solved by the ramses code (Teyssier 2002). The gas follows a piecewise polytropic equation of state (EoS) fitting the heating/cooling equilibrium (see Kraljic et al. 2014, and references therein). A Jeans polytrope sets a pressure floor in the most refined volumes, to prev... | [
"Choi, Shlosman & Begelman"
] | [
"The resulting gas density probability distribution function",
"with an additional few per cent of the mass in a power-law tail at high density"
] | [
"Uses",
"Uses"
] | [
[
953,
978
]
] | [
[
649,
708
],
[
872,
951
]
] |
2019AandA...631A..35B__Bridges_et_al._(1996)_Instance_2 | The collision velocity dependence of the coefficient of restitution between particles was observed in experiments (Bridges et al. 1996; Higa et al. 1996) and is discussed in the literature (e.g., Ramírez et al. 1999; Zhang & Vu-Quoc 2002). However, the experiments by Heißelmann et al. (2010), used in the present paper ... | [
"Bridges et al. (1996)"
] | [
"This discrepancy in results might originate in the nature of the collisions studied in these different experiments:",
"and Higa et al. (1996) performed collisions of a particle with a flat surface, while Heißelmann et al. (2010) observed particle-particle collisions in a free-floating environment."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
621,
642
]
] | [
[
505,
620
],
[
643,
822
]
] |
2021MNRAS.501.2934C__Dong_&_Fung_2017_Instance_1 | Understanding how the diverse populations of protoplanetary discs in young stellar regions results in the range of exoplanet types and architectures found in the Galaxy is one of the major goals of planet-formation theory. This is an extremely challenging task due in part to the limited observational constraints availa... | [
"Dong & Fung 2017"
] | [
"The minimum gap-opening mass depends on the viscosity and scale-height of the disc",
"or even Earth-mass planets",
"could produce detectable gaps."
] | [
"Background",
"Background",
"Background"
] | [
[
1597,
1613
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] | [
[
1362,
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1548,
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[
1615,
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2020ApJ...889L..10M__McKay_et_al._2018_Instance_1 | As stated earlier, during review of this manuscript Croviser et al. announced in a CBET a tentative water production rate approximately five times larger than our reported value. While the brief nature of the CBET precludes a detailed comparison, we discuss some possible reasons for this discrepancy. At the high airmas... | [
"McKay et al. 2018"
] | [
"We confirmed that this is indeed negligible for [O i] 6300 Å emission based on observations of comet C/2012 S1 (ISON) that were performed at a similarly high airmass with ARCES, and found that the production rates derived from the ISON [O i] 6300 Å measurements were consistent with values determined using other me... | [
"Similarities"
] | [
[
937,
954
]
] | [
[
615,
935
]
] |
2021MNRAS.501...50S__Gupta_et_al._2019_Instance_2 | There have been rather strong claims of AGN QPOs in different bands of the electromagnetic spectrum, ranging from minutes through days through months and years (e.g. Gierliński et al. 2008; Lachowicz et al. 2009; Gupta, Srivastava & Wiita 2009; Gupta et al. 2018, 2019; King et al. 2013; Gupta 2014, 2018; Ackermann et a... | [
"Gupta et al. 2019"
] | [
"Among the better recent claims of QPOs in the gamma-ray band are of",
"and of ∼71 d in the blazar B2 1520+31",
"found as part of a continuing analysis of blazar Fermi–LAT observations."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Background"
] | [
[
825,
842
]
] | [
[
664,
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[
786,
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[
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2018ApJ...856...94Z__Bieber_et_al._1991_Instance_2 | 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"
] | [
"Matthaeus et al. (2007) presented a similar spectrum in different regimes: energy range, inertial range, and intermediate regime where the spectrum is proportional to k−1 to coincide with observations"
] | [
"Background"
] | [
[
2119,
2137
]
] | [
[
1917,
2117
]
] |
2019MNRAS.482.5430B__Salmonson_2003_Instance_1 | In light of this, the allowed structure of gamma-ray burst (GRB) jets and the efficiency at which it produces gamma-rays at large angles remains a topic of major importance, and it is useful to consider what types of jet structures are consistent with GRB observations (see also Beniamini et al. 2018b). Previous studies... | [
"Salmonson 2003"
] | [
"Previous studies have considered the implications of structure models",
"on the shape of the afterglow light curve"
] | [
"Background",
"Background"
] | [
[
683,
697
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] | [
[
304,
373
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[
598,
639
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] |
2022MNRAS.513.4361M__Vasudevan_&_Fabian_2007_Instance_1 | The photoionization of the disc surface is characterized by two main parameters: irradiating X-ray continuum flux and disc density. Thus the measurement of the disc ionization parameter can address various aspects of the disc/corona interplay. According to Ballantyne, McDuffie & Rusin (2011), the ionization parameter o... | [
"Vasudevan & Fabian 2007"
] | [
"coronal dissipation fraction fc ≈ 0.45"
] | [
"Uses"
] | [
[
914,
937
]
] | [
[
874,
912
]
] |
2019MNRAS.490.2071Y__Riess_et_al._2018_Instance_3 |
Set II: we now focus on the observational constraints on the model parameters after the inclusion of the local measurement of H0 by Riess et al. (2018) with the previous data sets (CMB, Pantheon, and CC) in order to see how the parameters could be improved with the inclusion of this data point. Since for this present ... | [
"Riess et al. 2018"
] | [
"However, comparing the observational constraints reported in Table 3 (without R18 data) and Table 4 (with R18), one can see that the inclusion of R18 data",
"does not seem to improve the constraints on the model parameters. In fact, the estimation of the Hubble constant H0 remains almost similar to what we found... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
837,
854
]
] | [
[
681,
835
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[
856,
1023
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2016ApJ...819L...7N___2015b_Instance_1 | The gap and ring resemble those in the HL Tau system, recently found by the ALMA long baseline campaign (ALMA Partnership et al. 2015). Our result shows that gaps and rings in the (sub)millimeter dust continuum can exist, not only in relatively young disks (0.1–1 Myr) but also in relatively old disks (3–10 Myr). One po... | [
"Kanagawa et al.",
"2015b"
] | [
"According to recent theoretical analyses of gap structure around a planet",
"the depth and width of the gap are controlled by the planetary mass, the turbulent viscosity, and the gas temperature."
] | [
"Background",
"Background"
] | [
[
763,
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[
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791
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[
688,
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[
800,
918
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2018MNRAS.478.1884F__Widing_&_Feldman_2001_Instance_1 | Several studies indicate that the solar wind produced by the WTD mechanism has higher AHe and vαp, while the solar wind may have lower AHe and vαp when the RLO mechanism is at work. While it is challenging to obtain direct observations of the AHe in the solar corona, first ionization potential (FIP) bias measurements a... | [
"Widing & Feldman 2001"
] | [
"It is found that generally the FIP bias is higher in AR and QS regions (mainly occupied by closed loops) than in CH regions (generally taken up by open magnetic field lines)"
] | [
"Background"
] | [
[
522,
543
]
] | [
[
347,
520
]
] |
2021MNRAS.508.4512L__Haiman_2017_Instance_1 | The GW sources that LISA will observe at cosmological distances can be used as standard sirens. These include MBHBs, EMRIs, and SOBHBs. Unfortunately, only for the first of these types of sources are EM counterparts plausibly expected to be produced and observed by future EM facilities (Tamanini et al. 2016). MBHBs are... | [
"Haiman 2017"
] | [
"MBHBs are in fact expected to emit a large amount of EM radiation in different bands",
"and possibly even through pre-merger signals"
] | [
"Background",
"Background"
] | [
[
701,
712
]
] | [
[
311,
395
],
[
579,
623
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] |
2015MNRAS.453.3414A__Filippenko_&_Chornock_2001_Instance_2 | Filippenko & Chornock (2001) first presented the dynamical estimate of mass of the source to be around 7.4 ± 1.1 M⊙. Recently, Radhika & Nandi (2014) claimed that the mass of XTE J1859+226 is perhaps in between 6.58 and 8.84 M⊙ which is similar to the prediction of Shaposhnikov & Titarchuk (2009), although the lower ma... | [
"Filippenko & Chornock 2001"
] | [
"The distance of this source is around d ∼ 11 kpc"
] | [
"Uses"
] | [
[
496,
522
]
] | [
[
446,
494
]
] |
2016MNRAS.455.1905H__Shields_et_al._2003_Instance_1 | Galaxies hosting active galactic nuclei (AGN) are not only promising candidates for providing direct evidence for such a co-evolution, they can also be used to study the scaling relations over cosmic times. Many studies suggest that BH growth precedes spheroid assembly (Treu, Malkan & Blandford 2004; McLure et al. 2006... | [
"Shields et al. 2003"
] | [
"Many studies suggest that BH growth precedes spheroid assembly",
"however, other studies find no significant evolution with redshift (e.g."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
631,
650
]
] | [
[
207,
269
],
[
558,
630
]
] |
2022ApJ...936..102A__Williams_et_al._2006_Instance_1 | As regards the modeling of BGK modes, there are two main theoretical approaches: the integral solution or BGK methodology and the differential (or Schamel) technique. In the former method (BGK), one assumes that the initial particle distribution function and the electrostatic potential profiles are known, so these are ... | [
"Williams et al. 2006"
] | [
"Electrostatic solitary waves have been observed in Saturn’s magnetosphere"
] | [
"Background"
] | [
[
1699,
1719
]
] | [
[
1624,
1697
]
] |
2021ApJ...907...47L__Lee_et_al._2019_Instance_3 | In Figure 8, we also find small differences in the [Na, Al, O/Fe] abundance ratios between the stars in the bright and faint RC groups, although it is not as clear as in the case of [Na, Al, O/H] abundances. In particular, unlike Figure 7, stars in the bRC group are more enhanced in [Na/Fe] but appear to be more deplet... | [
"Lee et al. 2019"
] | [
"Because the relatively small [Na/Fe] variation is expected from the chemical evolution model for metal-rich bulge stars and the O-depletion is indistinct in some metal-rich GCs, such as NGC 6121 and 47 Tuc (see",
"the direct comparison of bulge stars with similarly metal-rich GCs on the Na–O plane would require ... | [
"Future Work",
"Future Work"
] | [
[
2439,
2454
]
] | [
[
2212,
2422
],
[
2457,
2617
]
] |
2017MNRAS.472.1361B__Salvo_&_Stella_2002_Instance_1 | Historically, the explanation of soft state spectra of NSs demanded the presence of a blackbody emission from the boundary layer of an NS (Mitsuda et al. 1984). For the harder states with a power-law tail in the energy spectrum, the need of Compton scattering became evident (White et al. 1986; Mitsuda et al. 1989). The... | [
"Di Salvo & Stella 2002"
] | [
"The fact that disc accretion rate was not the single factor that controlled the size or temperature of the Compton cloud, used to model the hard state spectra, lead to the conclusion that some unknown parameter, related to the truncation radius of the disc, is responsible for the hard X-ray tail"
] | [
"Background"
] | [
[
1278,
1300
]
] | [
[
946,
1242
]
] |
2018MNRAS.479.3254V___2000_Instance_2 | The lifetime of molecular clouds (MCs) remains an active research topic in the study of the interstellar medium and star formation, and most recent studies, both observational and theoretical, place this lifetime at a few times 107 yr for clouds in the 105–106M⊙ mass range (e.g. Blitz & Shu 1980; Kawamura et al. 2009; ... | [
"Palla & Stahler",
"2000"
] | [
"Vázquez-Semadeni, González-Samaniego & Colín (2017) have recently shown that the simulations of Colín et al. (2013) in fact produce stellar age histograms highly resemblant of the observed ones"
] | [
"Similarities"
] | [
[
2092,
2107
],
[
2114,
2118
]
] | [
[
1897,
2090
]
] |
2017AandA...602A..82D__Kirkpatrick_et_al._2012_Instance_1 | Brown dwarfs and giant exoplanets populate the same temperature range and share many physical properties, such as their molecule-dominated atmospheres and gradual cooling from ~3000 K at formation to ~100 K like the solar system gas-giant planets. Recent discoveries of very massive planets (Chauvin et al. 2005; Marois ... | [
"Kirkpatrick et al. 2012"
] | [
"On the other hand, the discovery of isolated L dwarfs in young clusters",
"and very cold very nearby Y dwarf objects (e.g.,",
"show that very low-mass isolated brown dwarfs exist and overlap with the planetary masses."
] | [
"Background",
"Background",
"Background"
] | [
[
752,
775
]
] | [
[
488,
559
],
[
703,
751
],
[
790,
880
]
] |
2020MNRAS.498.1496M__Dopita_&_Sutherland_1996_Instance_1 | The spectra from Sloan Digital Sky Survey (SDSS) have enabled the detection of the relatively faint He ii λ4686 line in large samples of star-forming galaxies (e.g. Shirazi & Brinchmann 2012). These studies find that the observed He ii λ4686/H β intensity ratio does not drop at low metallicities. In fact, recent studie... | [
"Dopita & Sutherland 1996"
] | [
"Alternative mechanisms such as",
"shocks from supernova remnants",
"are often invoked."
] | [
"Background",
"Background",
"Background"
] | [
[
842,
866
]
] | [
[
686,
716
],
[
789,
819
],
[
948,
966
]
] |
2018MNRAS.478L..18T__Zhang_et_al._2004_Instance_1 | The discovery of GW170817 and its electromagnetic counterparts (GRB170817A and AT2017gfo; Abbott et al. 2017a; Coulter et al. 2017; Goldstein et al. 2017) ushered in a new era of multimessenger astrophysics, in which both gravitational waves and photons provide complementary views of the same source. While observations... | [
"Zhang et al. 2004"
] | [
"Based on this evidence, Troja et al. (2017) suggested that a structured jet model (e.g.",
"provided a coherent description of the entire broad-band data set. Within this framework, the peculiar properties of GRB170817A/AT2017gfo could be explained, at least in part, by its viewing angle"
] | [
"Uses",
"Uses"
] | [
[
1081,
1098
]
] | [
[
993,
1080
],
[
1147,
1343
]
] |
2022ApJ...924...42N__Cheng_et_al._1990_Instance_1 | It is generally thought that the emission from radio to medium energy gamma rays is generated by the injected electrons through the synchrotron radiative mechanism. The high-energy photon emission mainly comes from inverse Compton (IC) scattering of the high-energy electrons on the background seed photons, which includ... | [
"Cheng et al. 1990"
] | [
"On the other hand, it is also suggested that the gamma rays could be emitted by the hadronic processes. The relativistic protons accelerated in the Crab pulsar outer gap interact with the matter inside the nebula. and this process may contribute in the high-energy gamma-ray range (see, e.g.,"
] | [
"Motivation"
] | [
[
796,
813
]
] | [
[
503,
795
]
] |
2021AandA...645A..99C__analysis,_Uttley_et_al._(2011)_Instance_1 | X-ray reverberation in black hole X-ray binaries was first robustly detected in GX 339–4 by Uttley et al. (2011) when the source was in its hard state. Previous studies of GX 339–4 pointed to the approximate central mass being ≥6 M⊙ (e.g. Hynes et al. 2003) and a small disc inclination angle (De Marco et al. 2015). Mil... | [
"Uttley et al. (2011)"
] | [
"X-ray reverberation in black hole X-ray binaries was first robustly detected in GX 339–4 by",
"when the source was in its hard state."
] | [
"Background",
"Background"
] | [
[
92,
112
]
] | [
[
0,
91
],
[
113,
151
]
] |
2020AandA...635A..60D__Castelli_&_Kurucz_2003_Instance_1 | We further constrain the stellar parameters for HD 85628 using the Virtual Observatory SED Analyzer (VOSA)5 and fitting the Hα profile of the star’s CHIRON spectrum. We fit the spectral energy distribution (SED; Fig. 8) of HD 85628 using published photometry from Tycho (BT VT; ESA 1997), APASS (BV; Henden et al. 2016),... | [
"Castelli & Kurucz 2003"
] | [
"and fit Kurucz ATLAS9 stellar atmosphere models"
] | [
"Uses"
] | [
[
525,
547
]
] | [
[
476,
523
]
] |
2017MNRAS.469S.731L__Hearn_et_al._2011_Instance_1 | The optical, spectrocopic and infrared remote imaging system (OSIRIS) scientific imaging cameras on the Rosetta spacecraft have been monitoring the coma activity of comet 67P Churyumov–Gerasimenko (67P hereafter) since their orbital rendezvous in 2014 August (Lara et al. 2015; Lin et al. 2015; Sierks et al. 2015; Lin e... | [
"A’Hearn et al. 2011"
] | [
"Such mini-outbursts or night-side activities have been observed before at",
"and comet 103P/Hartley 2 by the EPOXI mission"
] | [
"Background",
"Background"
] | [
[
834,
853
]
] | [
[
640,
713
],
[
787,
832
]
] |
2017AandA...601A..72I__Kobayashi_&_Tanaka_2010_Instance_2 | Small grains, which contribute most to infrared emission, are removed by collisional fragmentation and blown out by radiation pressure. The removal timescale is much shorter than the ages of host stars. Disruptive collisions among underlying large bodies, which are called planetesimals, produce smaller bodies and colli... | [
"Kobayashi & Tanaka 2010"
] | [
"Under the assumption of the steady state of collisional cascade, the power-law size distribution of bodies is analytically obtained and the power-law index depends on the size dependence of the collisional strength of bodies (see Eq. (32) of"
] | [
"Uses"
] | [
[
1131,
1154
]
] | [
[
888,
1129
]
] |
2021MNRAS.502.2859N__Evans_&_Howarth_2008_Instance_2 | It is harder to evaluate the behaviour of the young stellar population along the line of sight, since radial velocity measurements for our sample of Cepheids, needed for a thorough study, do not exist. Given this deficit, we provide only a simplified estimate using radial velocities of OBA-type stars from Evans & Howar... | [
"Evans & Howarth 2008"
] | [
"The radial velocities show a distinct and well-known gradient across the SMC with higher velocities in the eastern part (see also fig. 5 of"
] | [
"Compare/Contrast"
] | [
[
846,
866
]
] | [
[
706,
845
]
] |
2017MNRAS.465..248J__Tristram_et_al._2007_Instance_1 | First direct evidence for the geometrical distribution of the dust was found by Jaffe et al. (2004) with the help of the mid-infrared interferometric instrument (MIDI; Leinert et al. 2003) at the Very Large Telescope Interferometer (VLTI). One of the best-studied parsec-sized dust distribution is harboured by the Circi... | [
"Tristram et al. 2007"
] | [
"High-resolution mid-infrared (MIR) interferometric observations have revealed a two-component morphology in the brightness distribution: (i) a larger scale, elongated component in direction of the ionization cone (along PA ≈ 107°) with a full-width at half-maximum (FWHM) size of roughly 0.8 × 1.9 pc, which is resp... | [
"Background"
] | [
[
1058,
1078
]
] | [
[
453,
1056
]
] |
2016MNRAS.456..512C__Kronberg_et_al._2004_Instance_2 | Extended radio emission in galaxies is associated with both radio jets and lobes and with outflows, seen often as aligned radio sources in the opposite directions with respect to the central compact radio core. Giant radio galaxies (GRG) are extreme cases of this phenomenology with jets and lobes extending on ∼ Mpc sca... | [
"Kronberg et al. 2004"
] | [
"and in the seeding of large-scale magnetic fields in the universe (e.g."
] | [
"Background"
] | [
[
730,
750
]
] | [
[
658,
729
]
] |
2018ApJ...853...50F__Bernard_et_al._2015b_Instance_1 | 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"
] | [
"These bright PNe seem to resemble the younger, metal-rich population in the outer stream of M31, as revealed by HST pencil-beam pointings on the Giant Stream"
] | [
"Similarities"
] | [
[
755,
775
]
] | [
[
576,
733
]
] |
2021MNRAS.500.5009M__Bono_et_al._2003_Instance_1 | RR Lyrae are old low-mass stars that, during the central helium-burning phase, show mainly radial pulsation while crossing the classical instability strip in the colour–magnitude diagram. From the observational point of view, they represent the most numerous class of pulsating stars in the Milky Way and, being associat... | [
"Bono et al. 2003"
] | [
"The properties that make RR Lyrae standard candles are",
"the period–luminosity relation in the near-infrared (NIR) filters and in particular in the K 2.2 μm band (see e.g."
] | [
"Background",
"Background"
] | [
[
2197,
2213
]
] | [
[
1648,
1702
],
[
2060,
2174
]
] |
2021AandA...656A..16C__Bruno_&_Carbone_2013_Instance_1 | Investigations of the turbulent nature of solar wind fluctuations have been ongoing for more than half a century (see, e.g., Bruno & Carbone 2016). Advances have been made consistently thanks to the increasingly accurate measurements of several dedicated space mission as well as to the enormous improvement of numerical... | [
"Bruno & Carbone 2013"
] | [
"Among these, the very nature of the turbulent cascade of the solar wind flow and its relationship with the small-scale processes still need to be described in full"
] | [
"Future Work"
] | [
[
826,
846
]
] | [
[
643,
806
]
] |
2021ApJ...917...24Z__Coughlin_et_al._2020b_Instance_1 | Our simulation results show that the median detectable distances of targeted GW events from BH–NS mergers for a single 2nd generation GW detector and a network of such detectors are ∼300 Mpc and ∼700 Mpc, respectively (see Table 4). For comparison, Figure 12 shows that the detection rate and detectable distance for HLV... | [
"Coughlin et al. 2020b"
] | [
"This is basically consistent with the detection rate and the distance distribution of BH–NS merger candidates detected during LVC O3 (e.g.,"
] | [
"Similarities"
] | [
[
584,
605
]
] | [
[
404,
543
]
] |
2020AandA...641A..85S__Dallacasa_et_al._2000_Instance_1 | Compact symmetric objects are very powerful (P1.4 GHz > 1025 W Hz−1), compact (linear size of 50–100 pc), and young (≲104 yr) objects with a rather symmetric radio structure and convex synchrotron radio spectra (Wilkinson et al. 1994; Murgia 2003; Polatidis & Conway 2003). The characterized convex synchrotron radio spe... | [
"Dallacasa et al. 2000"
] | [
"The characterized convex synchrotron radio spectrum peaks at around 100 MHz in the case of compact steep spectrum (CSS) sources, at about 1 GHz in the case of GHz-peaked spectrum (GPS) objects, and up to a few GHz (e.g., 5 GHz) in the case of high-frequency peakers (HFPs;"
] | [
"Background"
] | [
[
547,
568
]
] | [
[
274,
546
]
] |
2019AandA...630A.131M__Chartas_et_al._2009_Instance_1 | Comptonisation Monte Carlo code (MoCA; see Tamborra et al. 2018 for a detailed description of the code) is based on a single photon approach, working in a fully special relativistic scenario. MoCA allows for various and different physical and geometrical conditions of the accretion disc and of the Comptonising corona. ... | [
"Chartas et al. 2009"
] | [
"Even though arguments",
"microlensing",
"exist that favour a compact corona, we used extended coronae."
] | [
"Differences",
"Differences",
"Differences"
] | [
[
618,
637
]
] | [
[
520,
541
],
[
605,
617
],
[
709,
770
]
] |
2022MNRAS.517.4119T___2017_Instance_1 | SN 2011fe, discovered a mere ≈11 h after explosion (Nugent et al. 2011) by the Palomar Transient Facility (PTF; Law et al. 2009), is the brightest SN Ia since the advent of modern astronomical detectors. Located at just $d_L \approx 6.5~\rm {Mpc}$ (e.g. Shappee & Stanek 2011; Beaton et al. 2019), SN 2011fe exploded in ... | [
"Kundu et al. 2017"
] | [
"Stringent non-detections in radio",
"observations exclude nearby CSM at high significance."
] | [
"Background",
"Background"
] | [
[
960,
977
]
] | [
[
884,
917
],
[
1032,
1085
]
] |
2015AandA...580A.135D__Hunt_et_al._2010_Instance_1 | How does the propagation of radiation and the ISM composition affect ISM observables in low-metallicity galaxies? Addressing this question is important to understand the evolution of low-metallicity galaxies, which undergo more bursty star formation than normal galaxies. Nearby star-forming dwarf galaxies present disti... | [
"Hunt et al. 2010"
] | [
"Mid-IR (MIR) and far-IR (FIR) observations have revealed bright atomic lines from H ii regions ([S iii], [Ne iii], [Ne ii], [O iii], etc.) and PDRs ([C ii], [O i]) (e.g.,"
] | [
"Background"
] | [
[
790,
806
]
] | [
[
563,
733
]
] |
2018ApJ...854...26L__Tian_2017_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... | [
"Tian 2017"
] | [
"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"
] | [
[
1116,
1125
]
] | [
[
694,
1022
]
] |
2018ApJ...862....8T__Hull_et_al._2017a_Instance_1 | Interstellar turbulence is supposed to be one of the most important factors to regulate star formation activities. Shocks induced by supersonic turbulence dramatically increase the density and temperature in the post-shock layer and promote the structure formation, such as dense cores and protostars (e.g., Padoan 1995;... | [
"Hull et al. 2017a"
] | [
"Some multiscale polarization observations and numerical simulations suggest that turbulent motions, rather than magnetic fields, are dynamically important to form complex gas morphologies of protostellar envelopes"
] | [
"Background"
] | [
[
1343,
1360
]
] | [
[
1128,
1341
]
] |
2022ApJ...939..103R__Markwardt_2009_Instance_1 | We analysed the change as a function of time, by using annual groups of line intensities for each instrumental setup as independent data points d
i
. The baseline is taken as time t
0 = 2012.45, which is the mean time point of our original data, 16.31 years after the discovery of the event (Nakano et al. 1996). The to... | [
"Markwardt 2009"
] | [
"For the regression the mpfit library",
"was used, with the variable errors handled according to York (1966) in the implementation of Tellinghuisen (2020)."
] | [
"Uses",
"Uses"
] | [
[
1478,
1492
]
] | [
[
1440,
1476
],
[
1494,
1608
]
] |
2017ApJ...839...83W__Orlando_et_al._2016_Instance_1 | A closer look at the known ejecta-dominated SNRs supports the role of surrounding winds and/or shells, and may provide additional insight into why such remnants are so rare. Several, and perhaps all of them, are ones where the ejecta are expanding into a pre-SN stellar wind from the progenitor, or into a cavity carved ... | [
"Orlando et al. 2016"
] | [
"These are produced from the collapse of the helium core of a red supergiant that had lost most of its hydrogen envelope before exploding, so the ejecta expand into the stellar wind from the pre-SN star"
] | [
"Background"
] | [
[
729,
748
]
] | [
[
502,
703
]
] |
2017ApJ...835L...1W__Peixoto_&_Oort_1992_Instance_1 | In this work, we investigate how the climate of an Earth-like planet is affected when its orbit is perturbed by the presence of a nearby giant planet. For the first time, a GCM coupled with analytical equations that describe the orbital evolution of a terrestrial planet are used. An additional major difference between ... | [
"Peixoto & Oort 1992"
] | [
"We use a fully coupled ocean model because alongside atmospheric heat transport, ocean heat transport plays a vital role in the climate of Earth"
] | [
"Uses"
] | [
[
828,
847
]
] | [
[
682,
826
]
] |
2022ApJ...936..102A__Williams_et_al._2006_Instance_4 | As regards the modeling of BGK modes, there are two main theoretical approaches: the integral solution or BGK methodology and the differential (or Schamel) technique. In the former method (BGK), one assumes that the initial particle distribution function and the electrostatic potential profiles are known, so these are ... | [
"Williams et al. 2006"
] | [
"Importantly, the instrument on board Cassini, the Radio Plasma Wave Science instrument, does not have the ability to determine the polarity of the electric fields associated with the ESWs observed with 100% certainty as it lacks the ability to perform interferometry"
] | [
"Compare/Contrast"
] | [
[
3638,
3658
]
] | [
[
3370,
3636
]
] |
2021MNRAS.500.2564O__Ziurys_1987_Instance_1 | Phosphorus, which is isoelectronic with both nitrogen and the CH group, is a key element of living systems as a major component of nucleic acids and nucleotides, performing many relevant biochemical functions (Pasek & Lauretta 2005). Conversely, despite significant progress in the recent years (Jiménez-Serra et al. 201... | [
"Ziurys 1987"
] | [
"The first identified phosphorus compound in the ISM was PN through observations of its rotational transitions in Orion-KL, W51M, and Sgr B2"
] | [
"Background"
] | [
[
654,
665
]
] | [
[
492,
631
]
] |
2018ApJ...866...15N__Collet_et_al._2007_Instance_1 | We find that it is possible to infer
and
, at the precision of spectroscopy and relatively imprecise
and
for red-giant stars. We attempted to infer the [Fe/H]; this label is available from the apogee spectroscopy for our stars. However, this label failed and, on inspection, no pixels correlat... | [
"Collet et al. 2007"
] | [
"While we do not find the signature in the ACF amplitude, this does indicate that a [Fe/H] dependence might be expected, as was also suggested by 3D hydrodynamical simulations of convection"
] | [
"Similarities"
] | [
[
1010,
1028
]
] | [
[
820,
1008
]
] |
2016ApJ...823...20K__Xue_et_al._2011_Instance_1 | Ouchi et al. (2008) find that there is a possible excess of the Lyα LFs at z = 3.1 and 3.7 similar to the bright-end hump, and they claim that 100% of LAEs host AGNs at the bright ends of
and 43.4 erg s−1, respectively, based on the large-area LAE survey with the multiwavelength data set. Thus, the bright-end hu... | [
"Xue et al. 2011"
] | [
"For the X-ray data, we use",
"the Chandra 4 Ms source catalog in the CDFS field",
"The typical sensitivity limits of these X-ray data are",
"∼10−17 to 10−16 erg cm −2 s−1 for the CDFS and HDFN fields."
] | [
"Uses",
"Uses",
"Uses",
"Uses"
] | [
[
760,
775
]
] | [
[
547,
573
],
[
709,
758
],
[
850,
904
],
[
970,
1029
]
] |
2019MNRAS.485.4841R__Creminelli_et_al._2010_Instance_1 | Although, the standard form of Press–Schechter mass function with $f(\nu)=\sqrt{{2}/{\pi }} \nu \mathrm{ e}^{-\frac{\nu }{2}}$ which discussed in Press & Schechter (1974) and Bond et al. (1991) can provide a good approximation of the predicted number density of haloes, it fails by predicting approximation too many low-... | [
"Creminelli et al. 2010"
] | [
"However, the virialization of dark matter perturbations in the non-linear regime cannot be independent from the properties of DE"
] | [
"Uses"
] | [
[
2090,
2112
]
] | [
[
1922,
2050
]
] |
2016ApJ...829..120A__Perron_et_al._1988_Instance_1 | Annealing is sometimes used to avoid effects of temperature fluctuations during the etching and/or to remove a background consisting of tracks of light ions. We did not anneal samples before etching. The reason is that nanometric structure transformations of olivine along the heavy projectile trajectory provide enhance... | [
"Perron et al. 1988"
] | [
"This correlates with the analysis",
"which demonstrated that the preliminary track annealing led to unpredictable changes in track lengths, resulting in a lower accuracy of nuclear charge determination."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1987,
2005
]
] | [
[
1952,
1985
],
[
2008,
2173
]
] |
2022AandA...666A..95H__Hartman_et_al._2022_Instance_2 | Scaling relations for the core radii rc, core densities δc, and core masses Mc as functions of the total halo mass M200 were fitted to the simulated halo populations, which largely agree with hydrostatic considerations of the halo cores where rc is nearly constant, as well as velocity dispersion tracing in the halo env... | [
"Hartman et al. 2022"
] | [
"For SIBEC-DM given by the field Lagrangian in Eq. (1), the self-interaction is constrained to Rc 1 kpc, otherwise an early radiation-like period and a large comoving Jeans’ length washes out too much structure to be consistent with observations"
] | [
"Compare/Contrast"
] | [
[
1160,
1179
]
] | [
[
892,
1137
]
] |
2016ApJ...826...54D__Schlickeiser_1984_Instance_1 | In both models, the particles interact with magnetohydrodynamic (MHD) Alfvén waves in the plasma. If the Doppler-shifted wave frequency is a constant multiple of the particle gyrofrequency in the particle guiding center frame, then a resonant interaction between the particle and the transverse component of the electric... | [
"Schlickeiser 1984"
] | [
"This stochastic acceleration process typically causes the particle distributions to have a pronounced curvature in the energy spectrum"
] | [
"Uses"
] | [
[
937,
954
]
] | [
[
801,
935
]
] |
2018MNRAS.478.3890B__Heckman_et_al._2017_Instance_5 | Rather than AGN feedback, it is possible that the effects we are seeing are from a different process coeval or prior to the onset of AGN accretion. Several works have pointed out that AGN activity coincides with a recent starburst, with the AGN having significant accretion events at least ∼200 Myr after the starburst h... | [
"Heckman et al. 2017"
] | [
"see fig. 5 from"
] | [
"Uses"
] | [
[
1212,
1231
]
] | [
[
1196,
1211
]
] |
2020AandA...643A.128K__Younes_et_al._2015_Instance_1 | In order to allow us to compare the continuum shape with earlier analyses, we use phenomenological continuum models rather than more physically motivated models such as those by Becker & Wolff (2007)2 or Farinelli et al. (2016). As discussed by Müller et al. (2013), among others, phenomenological spectral models typica... | [
"Younes et al. 2015"
] | [
"Due to its simplicity and in order to allow comparison with previous work (e.g.,",
"), we used the cutoffpl model for all subsequent analysis."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1127,
1145
]
] | [
[
1046,
1126
],
[
1145,
1203
]
] |
2018MNRAS.478.4357S__Peebles_&_Ratra_2003_Instance_1 | Observations over the years seem to firmly support the current acceleration of the Universe and therefore the possible existence of a generic cause responsible for it which we call dark energy (DE; see e.g. Riess et al. 1998; Perlmutter et al. 1999; WMAP collaboration 2013; Planck collaboration XVI 2014; Planck collabo... | [
"Peebles & Ratra 2003"
] | [
"Cosmologists have worked hard to decipher the dark energy code, but we still ignore the physical nature of the DE and hence of the ultimate cause of the observed acceleration of the Universe. Such theoretical conundrum is the so-called Cosmological Constant Problem (CCP)"
] | [
"Background"
] | [
[
726,
746
]
] | [
[
394,
665
]
] |
2020MNRAS.492.3021R__Machacek,_Bryan_&_Abel_2001_Instance_1 | In Fig. 4, we plot the mass growth of each candidate DCBH halo as a function of redshift. In both the panels, we plot the mass of the halo versus the redshift. The left-hand panel contains haloes from the Normal simulation while the right-hand panel contains haloes from the Rarepeak simulation. The grey region in each ... | [
"Machacek, Bryan & Abel 2001"
] | [
"The dashed blue line is the limit above which a halo must grow in order to overwhelm the impact of LW radiation, Mmin, LW"
] | [
"Uses"
] | [
[
754,
781
]
] | [
[
631,
752
]
] |
2018AandA...612A..77M__Gromadzki_&_Mikołajewska_(2009)_Instance_2 | “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)"
] | [
"Using Eq. (1) from",
", we derived the precession time of T ≈ 530 yr.",
"This value is quite large for the wiggling waves that we see."
] | [
"Uses",
"Uses",
"Compare/Contrast"
] | [
[
1531,
1562
]
] | [
[
1512,
1530
],
[
1562,
1609
],
[
1610,
1671
]
] |
2016ApJ...819L...7N___2015b_Instance_2 | The gap and ring resemble those in the HL Tau system, recently found by the ALMA long baseline campaign (ALMA Partnership et al. 2015). Our result shows that gaps and rings in the (sub)millimeter dust continuum can exist, not only in relatively young disks (0.1–1 Myr) but also in relatively old disks (3–10 Myr). One po... | [
"Kanagawa et al.",
"2015b"
] | [
"Such a gap could be opened by a super-Neptune-mass planet, depending on the parameters of the disk, such as the turbulent viscosity"
] | [
"Compare/Contrast"
] | [
[
1779,
1794
],
[
1802,
1807
]
] | [
[
1646,
1777
]
] |
2019ApJ...885..165M__Wilman_et_al._2009_Instance_1 | Morphology, colors, and star formation rate (SFR) primarily depend on the small-scale (1 Mpc) environment (Hogg et al. 2004; Kauffmann et al. 2004; Wetzel et al. 2012). This result has been extended by studying galaxy group samples; they show that colors and SF history most directly depend on the properties of the host... | [
"Wilman et al. 2009"
] | [
"In this context, the investigation of the evolution of group members in the nearby universe acquires a great cosmological interest because more than half of galaxies reside in such environments. Furthermore, since the velocity dispersion of galaxies is significantly lower in groups than in clusters, the merger pro... | [
"Motivation"
] | [
[
1058,
1076
]
] | [
[
528,
1057
]
] |
2021ApJ...920..145H__Damone_et_al._2018_Instance_1 | Over the past decade, many attempts to address this issue have been carried out, such as from the perspective of conventional nuclear physics and even exotic physics beyond the standard BBN framework (Angulo et al. 2005; Cyburt et al. 2008, 2016; Boyd et al. 2010; Pospelov & Pradler 2010; Fields 2011; Kirsebom & Davids... | [
"Damone et al. 2018"
] | [
"Over the past decade, many attempts to address this issue have been carried out, such as from the perspective of conventional nuclear physics and even exotic physics beyond the standard BBN framework"
] | [
"Background"
] | [
[
631,
649
]
] | [
[
0,
199
]
] |
2022AandA...663A.105P__Brunetti_et_al._2008_Instance_2 | Regardless of the cluster orientation, the spectral index observed for the halo at all available frequencies suggests that it is a USSRH. Despite the number of detected USSRH is still low, radio halos with steep indices are being discovered more and more frequently in the last years thanks to the improved observational... | [
"Brunetti et al. 2008"
] | [
"If there is no break in the spectrum, the energy budget for these particles would be untenable"
] | [
"Compare/Contrast"
] | [
[
1575,
1595
]
] | [
[
1479,
1573
]
] |
2015ApJ...811...57A__Choi_et_al._2014_Instance_1 | Shown in Figures 2(a) and (b) are the z-component of the electric field, Ez, and y-component of the magnetic field, By, respectively. Panels 2(c)–(e) show the transversally averaged (in the yz-plane) electric and magnetic field components,
. The energy distribution (total of jet+ambient) and average energy along ... | [
"Choi et al. 2014"
] | [
"This electric field is generated by the density gradient and different mobilities of electrons and ions"
] | [
"Uses"
] | [
[
1605,
1621
]
] | [
[
1436,
1539
]
] |
2021ApJ...908..248D__Guseva_&_Martynenko_1981_Instance_1 | Where
is the straggle or standard deviation of the implantation distribution, D is the diffusion coefficient, and t is the irradiation time. In the case of gas implantation via ion irradiation, it is often assumed that irradiation damage produces enough defects to serve as trapping sites that the diffusion coeff... | [
"Guseva & Martynenko 1981"
] | [
"We can assume additional trapping due to the interaction of hydrogen with helium in the material, since helium bubbles serve as trapping sites for hydrogen atoms through synergistic effects",
", leading to a lower critical dose in the case of mixed hydrogen and helium exposure"
] | [
"Motivation",
"Motivation"
] | [
[
913,
937
]
] | [
[
617,
806
],
[
827,
911
]
] |
2016MNRAS.460..590F__Miralda-Escudé_et_al._1996_Instance_1 | It is important to note that the above procedure differs from the observational one, whereby Voigt profiles are fit to the absorption features in transmission spectra (e−τ) in order to extract column densities and Doppler broadening parameters. This approach enables deblending of multiple-component absorption, and take... | [
"Miralda-Escudé et al. 1996"
] | [
"The technique was originally devised under the premise that the intervening absorption lines in QSO spectra arose from discrete absorbing clouds, but this picture was challenged early by the smoothly distributed IGM captured in cosmological hydrodynamical simulations (e.g."
] | [
"Background"
] | [
[
764,
790
]
] | [
[
450,
723
]
] |
2017AandA...601A.143F___2015_Instance_1 | Although wind observations are very common in AGN (see Elvis 2000; Veilleux et al. 2005; and Fabian 2012, for reviews), most studies concern ionised gas and uncertain spatial scales. In the past few years the situation changed drastically. Several fast (vOF of the order of 1000 km s-1), massive outflows of ionised, neu... | [
"Feruglio et al.",
"2015"
] | [
"interferometric observations in the (sub)millmetre domain"
] | [
"Background"
] | [
[
937,
952
],
[
968,
972
]
] | [
[
873,
930
]
] |
2021MNRAS.503.4387A__Neronov_&_Vovk_2010_Instance_1 | Observations of large-scale magnetic fields offer clear insights about regular ordered patterns of the field lines, suggesting that mean-field dynamo processes are responsible for their order and structure, as well as the existence of additional transport processes carrying magnetic energy into huge regions of space (C... | [
"Neronov & Vovk 2010"
] | [
"In addition, observations of magnetic fields in voids provide bounds on their strength, depending on the analytical model: From the simplest ones, it is possible to obtain lower bounds, although when improving such models a bounded range of magnetic field strength values can be provided, ranging from 10−25 to 10−1... | [
"Compare/Contrast"
] | [
[
928,
947
]
] | [
[
607,
926
]
] |
2015MNRAS.448...42L__Shetrone_et_al._2003_Instance_1 | GCs formed in dwarf galaxies may differ from those found in the Galactic halo, depending on their age and metallicity. Dwarf galaxies show a wide variety of star formation histories (Hidalgo et al. 2011, 2013; Weisz et al. 2014) that are predicted to lead to variations in their metallicity distribution functions and ch... | [
"Shetrone et al. 2003"
] | [
"From observations, field stars in dwarf galaxies do exhibit different abundance ratios from MW field stars, e.g. lower [α/Fe] ratios and variations in neutron-capture element ratios at intermediate metallicities. However, these typically do not show up until [Fe/H] ∼ −1.5"
] | [
"Background"
] | [
[
1033,
1053
]
] | [
[
696,
968
]
] |
2016ApJ...827...75L__Gal-Yam_et_al._2006_Instance_1 | The coalescence of a binary compact object system (either a neutron star (NS) binary or a stellar-mass black hole (BH) and NS binary) has been widely suggested to account for short-duration gamma-ray burst (SGRB) events (Eichler et al. 1989; Narayan et al. 1992; Nakar 2007; Berger 2014) that last typically less than 2 ... | [
"Gal-Yam et al. 2006"
] | [
"Since 2006, it has been suspected that mergers of compact objects could also produce the so-called long–short GRBs (also known as the supernova-less long GRBs, which are apparently long-lasting but do not show any signal of supernovae down to very stringent limits), which share some properties of both long- and sh... | [
"Background"
] | [
[
731,
750
]
] | [
[
372,
704
]
] |
2018AandA...611A..85S__Schleicher_&_Dreizler_(2014)_Instance_1 | After the detection of V391 Peg b, some other planet or brown dwarf (BD) candidates orbiting sdB stars were proposed using different detection methods. From eclipse timing, about one-third of the known detached sdB/sdO + dM (dM = M-dwarf) post-common-envelope binaries (PCEB) are suspected to host planets/BDs: HW Vir (B... | [
"Schleicher & Dreizler (2014)"
] | [
"Interesting explorations on the origin of PCEB (and specifically sdB+MS/BD) circumbinary planets can be found in Zorotovic & Schreiber (2013),",
"Bear & Soker (2014), and Völschow et al. (2016)."
] | [
"Background",
"Background"
] | [
[
834,
862
]
] | [
[
691,
833
],
[
864,
912
]
] |
2020ApJ...889...29C__Kalapotharakos_et_al._2014_Instance_1 | The global magnetospheric structures for the oblique rotator are very similar to the aligned one. We show the structure of magnetic field lines and the distribution of the accelerating electric field E0 in the x–z plane for a 60° rotator with the pair multiplicity κ = {0, 1, 3} in Figure 4. As the pair multiplicity κ i... | [
"Kalapotharakos et al. 2014"
] | [
"In fact, the E0 distribution for the high κ solution is qualitatively similar to the FIDO one"
] | [
"Similarities"
] | [
[
811,
837
]
] | [
[
705,
798
]
] |
2015AandA...579A.132P__Simha_et_al._(2009)_Instance_2 | A common feature of all previous models is that the relation between the central galaxy stellar mass and the halo mass reaches a maximum at halo masses ~1012 M⊙. According to Yang et al. (2012), below this threshold the mass accretion of the central galaxy is dominated by star formation. Thus, when the halo mass reache... | [
"Simha et al. (2009)"
] | [
"which according to",
"is about of 0.5−1 Gyr after the merger"
] | [
"Uses",
"Uses"
] | [
[
1329,
1348
]
] | [
[
1310,
1328
],
[
1349,
1387
]
] |
2017AandA...598A..66P___2016_Instance_1 | In both models, as we will see, the thick disc scale length is about a factor of two shorter than that of the thin disc, in agreement with the results by Bovy et al. (2012a). The choice of presenting two mass models for the mass distribution of our Galaxy is mainly dictated by two reasons. First, the need to add a cent... | [
"Kunder et al.",
"2016"
] | [
"Secondly, there is growing evidence that the mass of any classical bulge, if present in the Milky Way, must be small",
"For these reasons, we prefer to present a second model, our Model II, which does not include any spherical central component, and which is still compatible with the rotation curve of the Galaxy... | [
"Background",
"Motivation"
] | [
[
1288,
1301
],
[
1308,
1312
]
] | [
[
1152,
1268
],
[
1344,
1570
]
] |
2021MNRAS.501.3781R___2017_Instance_1 | While spatially extended optical jets and bipolar CO molecular outflows have been observed in numerous Class 0/I protostars (e.g. Reipurth & Bally 2001; Bally 2016, and references therein), near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study ... | [
"Antoniucci et al.",
"2017"
] | [
"near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study the kinematics of the outflowing gas and physical properties at the base of the jet within a few hundred au of the driving source in Class 0/I protostars (e.g."
] | [
"Background"
] | [
[
588,
605
],
[
618,
622
]
] | [
[
190,
479
]
] |
2019ApJ...871..243Y__Yen_et_al._2011_Instance_1 | There are two possibilities resulting in the different magnetic field strengths inferred from the polarimetric and molecular-line observations: (1) the rotational-to-gravitational energy βrot is overestimated, and (2) there are additional contributions in the polarized intensity from other mechanisms, such as dust scat... | [
"Yen et al. 2011"
] | [
"In our MHD simulations, βrot is adopted to be 0.4% based on the observational estimates of the core mass of ∼1 M and the angular speed of the core rotation of 4 × 10−14 s−1. The angular speed was estimated based on the global velocity gradient along the major axis of the dense core observed with single-dish telesc... | [
"Uses"
] | [
[
668,
683
]
] | [
[
328,
647
]
] |
2022AandA...662A..42M__Vázquez_2007_Instance_3 | A number of fundamental results have been rigorously proved in the mathematical literature concerning the asymptotic behaviour in time of some of the solutions of the porous medium equation and related equations (e.g. Kamin & Vázquez 1991; Bernis et al. 1993; Hulshof et al. 2001). What is of interest for us here is, pr... | [
"Vázquez 2007"
] | [
"A complementary result is the following: when the initial condition has positive net flux and its negative part has compact support, then the whole solution evolves into a positive function after a finite time",
"Theorem 18.29"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1509,
1521
]
] | [
[
1298,
1507
],
[
1523,
1536
]
] |
2021MNRAS.506.3313G__Surana_et_al._2020_Instance_1 | Deep learning (DL) is the paradigm of machine learning which uses multilayer neural networks. Neural networks are ML models inspired from the network of brain cells or neurons. The differentiating factor between DL and conventional ML is in the process of feature selection. In conventional ML, performance strongly depe... | [
"Surana et al. 2020"
] | [
"The Artificial Neural Networks (ANNs) have found application in not only the traditional tasks in extragalactic astronomy",
"but also in more specialized problems such as",
"estimation of star formation properties"
] | [
"Background",
"Background",
"Background"
] | [
[
1272,
1290
]
] | [
[
776,
897
],
[
1119,
1164
],
[
1231,
1270
]
] |
2019AandA...623A.156D__Cacciari_&_Clementini_2003_Instance_1 | Cepheids and RR Lyrae stars are primary standard candles of the cosmological distance ladder because they follow canonical relations linking their intrinsic luminosity to the pulsation period and/or the metal abundance. Specifically, for Cepheids the intrinsic luminosity (L) at any passband depends on the period (P) of... | [
"Cacciari & Clementini 2003"
] | [
"In the visual passband, the luminosity L depends on Z in the form of the so-called RR Lyrae luminosity–metallicity relation (see e.g."
] | [
"Background"
] | [
[
1838,
1864
]
] | [
[
1704,
1837
]
] |
2016MNRAS.458.3181C__Trujillo_et_al._2011_Instance_1 | To explain the observed evolution, the physical processes invoked have to result in a large growth in size but not in stellar mass, nor drastic increase in the star formation rate. Most plausible candidates are mass-loss driven adiabatic expansion (‘puffing-up’) (e.g. Fan et al. 2008, 2010; Ragone-Figueroa & Granato 20... | [
"Trujillo et al. 2011"
] | [
"In the former scenario, galaxies experience a mass-loss from wind driven by active galactic nuclei (AGNs) or supernovae feedback, which lead to an expansion in size due to a change in the gravitational potential. In the latter, mergers either major involving merging with another galaxy of comparable mass, or minor... | [
"Compare/Contrast"
] | [
[
866,
886
]
] | [
[
450,
864
]
] |
2020ApJ...903....8H__Finn_1987_Instance_1 | We note that during these encounters, energy is also lost due to tidal oscillations in the neutron star excited by the black hole (e.g., Press & Teukolsky 1977), and contributes to σ. To check whether we should include this effect in our calculations or whether it can be safely neglected, we approximate the tidal energ... | [
"Finn 1987"
] | [
"We approximate the NS as a polytropic star of index n = 0.5 (e.g.,"
] | [
"Uses"
] | [
[
822,
831
]
] | [
[
755,
821
]
] |
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... | [
"Compare/Contrast",
"Compare/Contrast",
"Differences"
] | [
[
2266,
2284
]
] | [
[
2141,
2265
],
[
2286,
2318
],
[
2319,
2469
]
] |
2022ApJ...924...42N__Cheng_et_al._1990_Instance_2 | It is generally thought that the emission from radio to medium energy gamma rays is generated by the injected electrons through the synchrotron radiative mechanism. The high-energy photon emission mainly comes from inverse Compton (IC) scattering of the high-energy electrons on the background seed photons, which includ... | [
"Cheng et al. 1990"
] | [
"and that of the gamma-ray emission about the hadronic process have been also investigated (see, e.g.,",
"However, with the establishment of more and more high-energy observatories, some telescopes have possessed the performance of observing photons of exceeding to the PeV from the astronomic objects."
] | [
"Background",
"Motivation"
] | [
[
1291,
1308
]
] | [
[
1189,
1290
],
[
1359,
1555
]
] |
2019MNRAS.489.2355D__Chevallard_et_al._2018a_Instance_1 | As a comparison, we also use the publicly available mock catalogue JAdes extraGalactic Ultradeep Artificial Realizations (JAGUAR; Williams et al. 2018) to derive the relation between UV and [O iii] + H β luminosity of simulated z ∼ 8 galaxies. The JAGUAR mock catalogue has been produced by matching luminosity and stell... | [
"Chevallard et al. 2018a"
] | [
"The JAGUAR catalogue provides emission line fluxes and EWs for the main lines based on modelling with the beagle code"
] | [
"Uses"
] | [
[
627,
650
]
] | [
[
481,
598
]
] |
2022ApJ...926..151Z__Jennings_et_al._2020_Instance_1 | Unlike the CMB, the 21 cm signal is highly non-Gaussian, because patchy, bubble-like structures of ionized hydrogen (H ii) regions are produced surrounding the ionizing sources. Thus, there is potentially a wealth of information in the 21 cm signal that is not contained in the 21 cm power spectrum, a two-point statisti... | [
"Jennings et al. 2020"
] | [
"Toward this goal, conventionally, new summary statistics that can only be measured with imaging have been proposed. These include the three-point correlation function"
] | [
"Background"
] | [
[
749,
769
]
] | [
[
559,
725
]
] |
2019ApJ...871..176X__Eldridge_et_al._2013_Instance_2 | The progenitors of SNe Ib/c have been thought to be Wolf-Rayet (W-R) stars with high initial masses (MZAMS ≳ 25 M⊙; Crowther 2007). Before core collapse, these stars usually have experienced severe mass loss through strong stellar winds or due to interaction with companion stars (van der Hucht 2006; Paxton et al. 2015)... | [
"Eldridge et al. 2013"
] | [
"Direct detection of progenitor stars is still elusive for SNe Ic, which prevents us from further testing the theoretical evolution of massive stars"
] | [
"Background"
] | [
[
2015,
2035
]
] | [
[
1866,
2013
]
] |
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