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.509.3599T__Du_et_al._2015_Instance_2 | Here we report the X-ray spectral and timing analysis of the joint XMM–Newton and NuSTAR observations of an IRAS 04416+1215, a nearby (z = 0.0889; Boller et al. 1992) hyper-Eddington AGN. The source is part of a XMM–Newton/NuSTAR campaign that aims to constrain the broad-band X-ray properties of eight super-Eddington A... | [
"Du et al. 2015"
] | [
"The dimensionless accretion rate",
"and black hole mass of the source are $\\log (\\dot{\\mathscr {M}})$ = $2.63^{+0.16}_{-0.67}$ and log (MBH/M⊙) = $6.78^{+0.31}_{-0.06}$ with the reverberation mapping technique",
"respectively, where $\\dot{\\mathscr {M}}\\equiv \\dot{M}_{\\bullet }c^2/L_{\\rm Edd}$, $\\dot{... | [
"Uses",
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"Uses"
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[
1696,
1710
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1471,
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1521,
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[
1713,
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2022ApJ...935..127H__Pan_et_al._2021_Instance_1 | Here we take the gravitational waveform of the nonrotating model with an observer viewed from the equatorial direction as an example for our HHT analysis. The gravitational waveforms of other models with different parameters are shown in the appendix (Figures B10–B20). Figure 6 (a) shows the simulated strains, followed... | [
"Pan et al. 2021",
"Pan et al. 2021"
] | [
"As this model is nonrotating and the proto-neutron star convection happens after the core bounce, the gravitational strain shows a loud bounce signal at time zero, and then it is followed by a low-frequency peak PNS oscillation, which could be caused by the g-mode oscillation although the nature remains controvers... | [
"Compare/Contrast",
"Similarities",
"Similarities"
] | [
[
812,
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1448,
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2018MNRAS.475.3613S__Stabenau,_Connolly_&_Jain_2008_Instance_1 | With the availability of such a wide range of photo-z codes and methods, comparisons of various implementations have been performed (Hildebrandt et al. 2010; Abdalla et al. 2011; Sanchez et al. 2014). No obvious best photo-z code was named since each code displays different strengths depending on the metrics used. The ... | [
"Stabenau, Connolly & Jain 2008"
] | [
"With regards to the inclusion of extra information, a recent example in template methods includes using surface brightness as a prior in spectral energy distribution templates",
", motivated by the knowledge of surface brightness dimming (1 + z)4.",
"In empirical methods this application is more straightforwar... | [
"Background",
"Background",
"Motivation"
] | [
[
900,
930
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] | [
[
704,
879
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[
931,
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[
1000,
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2020ApJ...904...20S__Woods_et_al._2008_Instance_1 | Comparison of the DAXSS two temperature (2T) model fits to DEM estimates from other instruments could help validate the DAXSS simple modeling approach. Moore et al. (2018) shows that the X123 response is primarily over the temperature range of 1 MK to 10 MK, so this comparison needs to be done over a similar range, suc... | [
"Woods et al. 2008"
] | [
"The primary DEMs for this analysis is the quiet Sun (QS) and active region (AR) DEMs as needed for estimating the daily variations of the solar XUV spectral irradiance for the XPS Level 4 product"
] | [
"Uses"
] | [
[
1090,
1107
]
] | [
[
893,
1088
]
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2017MNRAS.468.4992P__Lister_et_al._2016_Instance_1 | The intrinsic jet opening angles can be calculated as tan (αint/2) = tan (αapp/2) sin θ, where θ is the viewing angle to the jet axis. The latter, as well as the bulk Lorentz factor Γ, can be derived from apparent jet speed and Doppler factor using the following relations:
\begin{eqnarray*}
\theta = \arctan \frac{2\... | [
"Lister et al. 2016"
] | [
"For βapp and δvar we used the fastest measured radial, non-accelerating apparent jet speed from the MOJAVE kinematic analysis"
] | [
"Uses"
] | [
[
613,
631
]
] | [
[
486,
611
]
] |
2021MNRAS.501...50S__Gupta_et_al._2019_Instance_1 | 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"
] | [
"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."
] | [
"Background"
] | [
[
245,
257
],
[
264,
268
]
] | [
[
0,
165
]
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2015MNRAS.450..943T__Patterson_1984_Instance_1 | In order to recover the intrinsic SED, we employ the values for interstellar extinction E(B − V) from Schlafly & Finkbeiner (2011), collected on NASA's Infrared Science Archive (IRSA) web pages, to deredden the spectra. We use the relations derived by Cardelli, Clayton & Mathis (1989) as implemented in iraf, and a stan... | [
"Patterson 1984"
] | [
"Since CVs are intrinsically rather faint (typically, MV > 4 mag; e.g.",
", in general the correction for the interstellar extinction will represent an upper limit."
] | [
"Uses",
"Uses"
] | [
[
781,
795
]
] | [
[
711,
780
],
[
796,
886
]
] |
2021ApJ...922...85T__Porquet_et_al._2004_Instance_1 | When the primary X-ray continuum is scattered by distant matter at several thousands of gravitational radii, the line is narrow (FWHM 10,000 km s−1) and is unlikely to carry any information about the conditions in the accretion disk and the strong-gravity regime near the SMBH. Narrow lines have been detected in the gr... | [
"Porquet et al. 2004"
] | [
"In contrast, when the primary X-ray continuum is scattered close to the SMBH, Doppler and general relativistic effects combined may give rise to a significantly broader line (FWHM tens of thousands km s−1), reported in at least ∼36% of AGNs",
"see also, e.g.,"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1056,
1075
]
] | [
[
767,
1007
],
[
1040,
1055
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2021MNRAS.504.6198M__McCoy_et_al._2017_Instance_1 | Here, we present the GMC properties within the molecular disc of the closest giant elliptical galaxy, NGC 5128, which is the host of the radio-source Centaurus A (hereafter Cen A). Cen A is at a distance of only D ≃ 3.8 Mpc (Harris, Rejkuba & Harris 2010, 1 arcsec = 18 pc) and it is therefore by far the most adequate t... | [
"McCoy et al. 2017"
] | [
"Along the dust lane of the elliptical galaxy, there is a molecular gas component of mass ∼109 M⊙ as probed by various molecular lines"
] | [
"Background"
] | [
[
889,
906
]
] | [
[
641,
774
]
] |
2015ApJ...811L..32H__Hellinger_et_al._2013_Instance_1 | During the second phase, protons are heated. For negligible heat fluxes, collisions, and fluctuations, one expects the double adiabatic behavior or CGL (Chew et al. 1956; Matteini et al. 2012): the parallel and perpendicular temperatures (with respect to the magnetic field) are expected to follow
and
resp... | [
"Hellinger et al. 2013"
] | [
"Note that the perpendicular heating rate is a nonnegligible fraction of that observed in the solar wind, where"
] | [
"Uses"
] | [
[
1103,
1124
]
] | [
[
984,
1094
]
] |
2021MNRAS.503.2776Y__Ajith_et_al._2007_Instance_2 | In order to investigate the signal-to-noise ratio (SNR), ρ of NS–WD binaries for LISA-type space GW detectors, we calculate the averaged square SNR $\overline{\rho ^{2}}$ over the sky location, inclination, and polarization as
(30)$$\begin{eqnarray*}
\overline{\rho ^{2}} = \int _{f_{1}}^{f_{2}}\frac{4\cdot \frac{4}{5... | [
"Ajith et al. 2007"
] | [
"If f > fm, the index of the power-law relation between A(f) and f changes",
"and is beyond the scope of this study."
] | [
"Uses",
"Future Work"
] | [
[
1466,
1483
]
] | [
[
1391,
1464
],
[
1485,
1523
]
] |
2019MNRAS.484.2000D__Sandage_&_Fouts_1987_Instance_1 | To understand the distribution of Li-rich giants among different stellar components of the Galaxy, we have computed membership probability, based on the recipe given in Reddy, Lambert & Allende Prieto (2006) and references therein, for each of the stars in the selected RGB sample for belonging to one of the three main ... | [
"Sandage & Fouts 1987"
] | [
"Entire sample is shown in Toomre Diagram of rotational velocity (VLSR) and sum of quadrature of radial and vertical velocities ([$\\rm {\\it U}_{\\rm LSR}^2 + {\\it W}_{\\rm LSR}^2]^{1/2}$)"
] | [
"Uses"
] | [
[
994,
1014
]
] | [
[
808,
992
]
] |
2022AandA...659A.180G__Giannattasio_et_al._2013_Instance_1 | In the last few decades, the dynamic properties of the quiet Sun have been thoroughly investigated using a range of substantially different techniques, allowing us to elaborate a consistent picture of the photospheric dynamics by approaching the problem from different points of view. Particularly interesting and promis... | [
"Giannattasio et al. 2013"
] | [
"These studies are based on the hypothesis that magnetic fields are passively transported by the plasma flow and provide a characterisation of advection and diffusion processes in the quiet photosphere from granular to supergranular scales (see, e.g."
] | [
"Background"
] | [
[
1095,
1119
]
] | [
[
645,
894
]
] |
2022ApJ...930..125L__Zimbardo_et_al._2017_Instance_1 | To this we can add that Zimbardo and coworkers reported in a series of papers that spacecraft observations of SEP intensity-time profiles ahead of interplanetary shocks yielded power laws instead of the exponential profiles predicted by standard DSA. They interpreted this as a sign of superdiffusive spatial SEP transpo... | [
"Zimbardo et al. 2017"
] | [
"To this we can add that Zimbardo and coworkers reported in a series of papers that spacecraft observations of SEP intensity-time profiles ahead of interplanetary shocks yielded power laws instead of the exponential profiles predicted by standard DSA. They interpreted this as a sign of superdiffusive spatial SEP tr... | [
"Compare/Contrast"
] | [
[
627,
647
]
] | [
[
0,
545
]
] |
2018ApJ...854...26L___2015a_Instance_4 | 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"
] | [
"As the hot Fe xxi line is absent in the non-flaring spectrum, the rest wavelength for the Fe xxi line (i.e., 1354.09 Å) is determined by averaging the line centers of the Fe XXI profiles which were used in the previous IRIS observations",
", while the rest wavelengths for the C i and Si iv lines, i.e., 1354.29 Å... | [
"Uses",
"Uses"
] | [
[
3057,
3066
],
[
3073,
3078
]
] | [
[
2530,
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[
2909,
3055
]
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2015MNRAS.454.1117S___2005_Instance_1 | One of the first models of MRI-driven accretion in protoplanetary discs was constructed by Gammie (1996), who proposed that Ohmic resistivity (due to weak coupling of charged species to the magnetic field) quenches the MRI in a ‘dead’ mid-plane region surrounded by ‘active layers’, which are ionized by cosmic rays. Thi... | [
"Salmeron & Wardle",
"2005"
] | [
"This layered-accretion scenario has been refined as additional non-thermal ionization sources (X-rays, UV radiation) and non-ideal magnetohydrodynamic (MHD) effects (ambipolar diffusion and the Hall effect) have been included (e.g."
] | [
"Background"
] | [
[
622,
639
],
[
646,
650
]
] | [
[
317,
548
]
] |
2020ApJ...896...59A__Henry_1989_Instance_1 | PNs are expanding shells of the luminous gas expelled by dying stars of low and intermediate masses (LIMS). They stem from objects that have lifetimes up to gigayears. The ionized gas surrounding the central star shows emission lines of highly ionized species from which the abundances can be derived. The neon abundance... | [
"Henry 1989"
] | [
"The neon abundance can be compared and related to the results from stellar abundance analysis, as neon (and oxygen) originates from primary nucleosynthesis in massive stars (≥10 M⊙) and is therefore nearly independent of the evolution of LIMS, the progenitor stars of PNs"
] | [
"Background"
] | [
[
575,
585
]
] | [
[
302,
573
]
] |
2020MNRAS.497..829F__Diaz-Miller,_Franco_&_Shore_1998_Instance_1 | In order to consider both the photoionization and radiation-pressure effects from the accreting protostar, we solve the frequency-dependent radiative transfer for stellar irradiation by the following method. We inject photons from the sink cell to the computational domain at the rate
(10)$$\begin{eqnarray*}
L_{\rm *}^... | [
"Diaz-Miller, Franco & Shore 1998"
] | [
"Assumption of the thermal blackbody radiation could overestimate the emissivity of ionizing photons at Z ∼ Z⊙ owing to the line-blanketing effect, especially for stars with M* ∼ 10 M⊙ (e.g."
] | [
"Uses"
] | [
[
952,
984
]
] | [
[
762,
951
]
] |
2021AandA...651A..71L__Samland_et_al._2017_Instance_1 | Both SHINE and GPIES surveys recently discovered three new exoplanets (Macintosh et al. 2015; Chauvin et al. 2017b; Keppler et al. 2018) and a few additional higher-mass brown dwarfs (Konopacky et al. 2016; Cheetham et al. 2018). Smaller surveys using SPHERE and GPI also discovered several substellar companions (Milli ... | [
"Samland et al. 2017",
"Samland et al. 2017"
] | [
"These surveys offer unprecedented detection, astrometric, and spectrophotometric capabilities that allow us to characterize fainter and closer giant planets, such as the recent discovery of 51 Eri b (2 MJup at 14 au, T5-type, of an age of 20 Myr;",
"Such surveys also provide key spectral and orbital characterisa... | [
"Background",
"Background"
] | [
[
643,
662
],
[
1136,
1155
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] | [
[
373,
619
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[
1014,
1114
]
] |
2019ApJ...883...73C__Engelbrecht_&_Burger_2013a_Instance_1 | Both Nel (2016) and Zhao et al. (2018) report that these parallel mean free paths are smaller during periods of high solar activity and larger during solar minima, with the opposite being true for the resulting perpendicular mean free paths. Zhao et al. (2018) also show that such solar cycle dependences would not be fu... | [
"Engelbrecht & Burger 2013a"
] | [
"were used as inputs for the turbulence quantities (e.g.,",
"Furthermore, mean free paths such as those discussed have,"
] | [
"Background",
"Similarities"
] | [
[
889,
915
]
] | [
[
832,
888
],
[
966,
1024
]
] |
2022MNRAS.516.3381J__Lindblom_&_Owen_2002_Instance_2 | Studying the dynamical properties of rotating neutron stars is a domain which brings out various interesting features when one assumes a perfect fluid. It is known that the centrifugal force of a rotating star counters gravitational force and hence one can expect massive stars to be fast rotors, at least in the initial... | [
"Lindblom & Owen 2002"
] | [
"Within these weak processes, although the modified Urca processes involving leptons are important, it has been shown that non-leptonic processes involving hyperons contribute more significantly towards bulk viscosity at temperatures lower than a few times 109 K"
] | [
"Compare/Contrast"
] | [
[
2311,
2331
]
] | [
[
2048,
2309
]
] |
2020AandA...642A..90M__Werner_et_al._2006_Instance_1 | Additional information can be derived from the abundance ratios measured in the ICM. For example, the Mn/Fe and Ni/Fe ratios are both sensitive to the electron capture rates during SNIa explosions, and are therefore crucial indicators of their progenitor channels (Seitenzahl et al. 2013a; Mernier et al. 2016a; Hitomi C... | [
"Werner et al. 2006"
] | [
"By pushing current observatories to their limit, recent studies derived constraints on the relative fraction of SN events that effectively contribute to the ICM enrichment. These measurements showed that SNIa and SNcc contribute relatively equally to the overall chemical enrichment in the ICM"
] | [
"Compare/Contrast"
] | [
[
818,
836
]
] | [
[
523,
816
]
] |
2016ApJ...825...10T__Brisken_et_al._2003_Instance_1 | Although this penalty is small, we can still provide a quantitative estimate based on a few assumptions. The observations of M15 that measured the parallax to VLA J2130+12 (K14) employed an interferometric technique where the position of a weaker potential in-beam calibrator source (M15 S1 and VLA J2130+12) can be meas... | [
"Brisken et al. 2003"
] | [
"Based on a literature review for papers where VLBI parallax measurements were determined using an in-beam calibrator, we find 24 similar measurements, the majority of which have been used to measure parallaxes to pulsars"
] | [
"Similarities"
] | [
[
742,
761
]
] | [
[
498,
718
]
] |
2016ApJ...833..192S__Champion_et_al._2008_Instance_1 | In recent years, several large-scale pulsar surveys have been undertaken to search for new pulsars (Cordes et al. 2006; Keith et al. 2010; Barr et al. 2013; Boyles et al. 2013; Deneva et al. 2013; Coenen et al. 2014; Stovall et al. 2014). One of the drivers for such surveys is the discovery of millisecond pulsars (MSPs... | [
"Champion et al. 2008"
] | [
"the study of binary systems such as eccentric MSPs like PSRs J1903+0327",
"which are interesting due to their peculiar binary evolution"
] | [
"Motivation",
"Motivation"
] | [
[
1096,
1116
]
] | [
[
1023,
1094
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[
1155,
1215
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2020AandA...641A.123H__Mikal-Evans_et_al._(2019)_Instance_1 | To confirm the importance of VO, water and an inversion layer (Evans et al. 2018; Mikal-Evans et al. 2019, 2020) obtained repeated HST observations of the transmission spectrum and the secondary eclipse using the STIS and WFC 3 instruments. The optical transmission spectrum displays rich variation, with multiple featur... | [
"Mikal-Evans et al. 2019"
] | [
"To confirm the importance of VO, water and an inversion layer",
"obtained repeated HST observations of the transmission spectrum and the secondary eclipse using the STIS and WFC 3 instruments.",
"The optical transmission spectrum displays rich variation, with multiple features consistent with VO absorption tha... | [
"Background",
"Background",
"Compare/Contrast"
] | [
[
82,
105
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[
0,
61
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[
113,
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241,
830
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2020ApJ...902...98G__Bournaud_et_al._2014_Instance_1 | On balance, a large abundance of baryon-dominated, dark matter cored galaxies at z ∼ 2, most strongly correlated with baryonic surface density, angular momentum, and central bulge mass, may be most naturally accounted for by the interaction of baryons and dark matter during the formation epoch of massive halos. Massive... | [
"Bournaud et al. 2014"
] | [
"This resulted in",
"formation of globally unstable disks, and radial gas transport by dynamical friction"
] | [
"Background",
"Background"
] | [
[
926,
946
]
] | [
[
584,
600
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[
759,
843
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2022MNRAS.512.4136C__Ventura_et_al._2013_Instance_1 | If we recall the tight, monotonic dependence of the position of galaxies along the SF sequence in the diagram with metallicity (as outlined in Section 3.1), we can interpret our global results of Figs 4 and 5 as a manifestation of the existence of an O/H versus N/O relation for SDSS star-forming galaxies, whose intrins... | [
"Ventura et al. 2013"
] | [
"A tight relationship between O/H and N/O abundances is indeed observed in both H ii regions and local galaxies,",
"and it is set by the predominant nucleosynthetic origin of nitrogen from CNO burning of pre-existing stellar carbon and oxygen in low- and intermediate-mass stars experiencing the AGB phase (i.e. th... | [
"Uses",
"Uses"
] | [
[
1023,
1042
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] | [
[
454,
565
],
[
747,
989
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] |
2021ApJ...912..163B__Brennecka_et_al._2020_Instance_1 | Braukmuller et al. (2018) proposed that all elements fall into one of four categories based on their condensation temperature: refractory elements (50% condensation temperature, Tc,50 > 1400 K), which exhibit approximately uniform enrichments in their Si-normalized concentrations in CC chondrites compared to CI chondri... | [
"Brennecka et al. 2020"
] | [
"For CC iron meteorites, we examine the isotopic compositions of Mo and Ni, respectively, because these are siderophile elements (so are therefore present in appreciable concentrations in iron meteorites, unlike Ti and Cr) whose compositions have also been relatively well studied in a number of iron meteorites as w... | [
"Motivation"
] | [
[
2123,
2144
]
] | [
[
1622,
1975
]
] |
2015MNRAS.449.4326P__Collaboration_2006_Instance_1 | We now consider upcoming spectroscopic surveys. We consider two cases for the CMB lensing map, including (1) the full Planck CMB lensing map and (2) the Advanced ACTPol5 CMB lensing map. In both cases, we assume that the CMB lensing maps will be estimated using the temperature map and both E and B polarization maps, an... | [
"Planck Collaboration 2006"
] | [
"We predict the noise in the Planck lensing map assuming the detector sensitivity and beam sizes listed in the Planck Bluebook"
] | [
"Uses"
] | [
[
490,
515
]
] | [
[
363,
488
]
] |
2022MNRAS.510.4943S__Murray_&_Dermott_1999_Instance_2 | The gravitational potential of an eccentric companion at the quadrupole order can be decomposed as a sum over circular orbits (e.g. Storch & Lai 2013; Vick, Lai & Fuller 2017):
(5)$$\begin{eqnarray*}
U\left(\boldsymbol{\mathbf {r}}, t\right) = \sum \limits _{m=-2}^2 U_{2m} \left(\boldsymbol{\mathbf {r}}, t\right) ,
\... | [
"Murray & Dermott 1999"
] | [
"The FNm can be written explicitly as an integral over the eccentric anomaly",
"F_{Nm} = \\frac{1}{\\pi }\\int \\limits _{0}^{\\pi } \\frac{\\cos \\left[N\\left(E - e\\sin E\\right) - mf(E)\\right]}{\\left(1 - e\\cos E\\right)^2}\\,\\,\\mathrm{d}E."
] | [
"Uses",
"Uses"
] | [
[
1390,
1411
]
] | [
[
1313,
1388
],
[
1457,
1607
]
] |
2018MNRAS.478..932H__Anjos_2001_Instance_1 | Although a correlation does exist, it is offset from the one-to-one line that one would expect, overestimating the number of spiral arms by approximately three. This may be due to how mass is assigned to the bulge and disc. We use photometric decompositions of Simard et al. (2011) and Mendel et al. (2014) to assign mas... | [
"Gadotti & dos Anjos 2001"
] | [
"The second issue is the pseudo- versus classical bulge argument – the model we use assumes an inner classical spherical bulge; bulges instead may be pseudo-bulges, which may not have a spherical shape, and profile well-described by a spherical Hernquist profile"
] | [
"Compare/Contrast"
] | [
[
852,
876
]
] | [
[
568,
829
]
] |
2015ApJ...806..152S__Ferraro_et_al._2001_Instance_1 | One of the most astonishing characteristics of Liller 1 is the extremely large value of the collision rate parameter. Verbunt & Hut (1987) showed that Liller 1 has the second-highest value of stellar encounter rate (after Terzan 5; see also Lanzoni et al. 2010) among all star clusters in the Galaxy, thus suggesting tha... | [
"Ferraro et al. 2001"
] | [
"In fact, it is commonly believed that dynamical interactions in GCs facilitate the formation of close binary systems and exotic objects such as cataclysmic variables (CVs), low-mass X-ray binaries (LMXBs), millisecond pulsars (MSPs), and blue straggler stars (BSSs) (e.g.,"
] | [
"Background"
] | [
[
721,
740
]
] | [
[
414,
686
]
] |
2022MNRAS.511.1121M__Reig_&_Nespoli_2013_Instance_1 | 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"
] | [
"The luminosity during the 2020 giant outburst reached a record high, which was significantly higher than the critical luminosity"
] | [
"Background"
] | [
[
611,
630
]
] | [
[
481,
609
]
] |
2022MNRAS.515.2188H__Rorai_et_al._2018_Instance_4 | 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"
] | [
"Lastly, the results from this approach critically depend on the choice of low-b cutoff fitting techniques, where different techniques might result in inconsistent T0 and γ measurements"
] | [
"Background"
] | [
[
2321,
2338
]
] | [
[
2117,
2301
]
] |
2017ApJ...838...67E__Derekas_et_al._2017_Instance_1 | In the present era of “high precision” cosmology (see Riess et al. 2016), it is important to exploit the full potential of Cepheids as precise extragalactic distance indicators for determining the expansion rate of the universe and setting constraints on cosmology models. To achieve these goals, a deeper understanding ... | [
"Derekas et al. 2017"
] | [
"Cepheids have also been found to show additional complications that include cycle-to-cycle variations in their light and radial velocity curves (see"
] | [
"Motivation"
] | [
[
890,
909
]
] | [
[
658,
806
]
] |
2018MNRAS.474.3280F__Sotomayor-Beltran_et_al._2013_Instance_1 | The ability to retrieve the polarized quantities of a radio source is entirely dependent on the ability to find radio sources within noisy images. It is of importance to planned future surveys to investigate suitable strategies for source-finding in linear polarization with interferometers such as LOFAR, which are very... | [
"Sotomayor-Beltran et al. 2013"
] | [
"It is of importance to planned future surveys to investigate suitable strategies for source-finding in linear polarization with interferometers such as LOFAR,",
"and with the ability to make precise Faraday rotation measurements"
] | [
"Background",
"Background"
] | [
[
702,
731
]
] | [
[
147,
305
],
[
634,
700
]
] |
2017ApJ...837...88B__High_et_al._2010_Instance_1 | With photometry in hand for the majority of our galaxy spectroscopy sample, we can also investigate velocity segregation effects as a function of galaxy luminosity. We use cluster galaxy brightness measurements in units relative to m*, a standard quantity that can be easily incorporated into both observational data and... | [
"High et al. 2010"
] | [
"Specifically, we use m* values computed from Bruzual & Charlot (2003) models in the same fashion as described in previous SPT publications"
] | [
"Similarities"
] | [
[
539,
555
]
] | [
[
399,
537
]
] |
2017AandA...602A.106B__Ehrenreich_et_al._2015_Instance_1 | About a quarter of the known exoplanets orbit at short distances (≲0.1 au) from their star (from the Exoplanet Encyclopaedia in December 2016; Schneider et al. 2011). Heating by the stellar energy can lead to the expansion of their upper atmospheric layers and their eventual escape. As a result of this expansion, the u... | [
"Ehrenreich et al. 2015"
] | [
"The warm Neptune GJ436b, which is the lowest mass planet found evaporating to date",
"), shows transit absorption depths up to 60% in the Ly-α line."
] | [
"Background",
"Background"
] | [
[
1096,
1118
]
] | [
[
1012,
1094
],
[
1118,
1180
]
] |
2015MNRAS.451.2663H___2005_Instance_1 | Galaxy formation theory has developed dramatically over the last three decades. Λ cold dark matter (ΛCDM) has been established as the standard model for cosmological structure formation, and its parameters have been increasingly tightly constrained by observations. In parallel, simulations of galaxy formation within th... | [
"Springel et al.",
"2005"
] | [
"Semi-analytic modelling is a particular simulation method which is optimized to connect the observed properties of the galaxy population – abundances, scaling relations, clustering and their evolution with redshift – to the astrophysical processes that drive the formation and evolution of individual galaxies (e.g.... | [
"Background"
] | [
[
959,
974
],
[
981,
985
]
] | [
[
477,
792
]
] |
2020ApJ...897..158S__Sherwood_et_al._2003_Instance_1 | For the study of each of the individual reactions we have characterized the stationary points on their respective potential energy surfaces by means of density functional theory (DFT) calculations. We have employed the mPWB1K exchange and correlation functional of Zhao & Truhlar (2004) in combination with the def2-TZVP... | [
"Sherwood et al. 2003"
] | [
"Minima and transition states (TSs) were optimized using the DL-FIND",
"program of the ChemShell suite"
] | [
"Uses",
"Uses"
] | [
[
616,
636
]
] | [
[
494,
561
],
[
584,
614
]
] |
2022ApJ...925...37W__Lentati_et_al._2015_Instance_1 | The stochastic gravitational-wave background (SGWB)—the primary goal of the search of the PTA collaborations—is expected to be dominant in the nanohertz band, which might originate from supermassive black hole binaries (SMBHBs; Rajagopal & Romani 1995; Sesana 2013), comic strings (Damour & Vilenkin 2005; Blanco-Pillado... | [
"Lentati et al. 2015"
] | [
"Over the last few decades, the PTA collaborations have not found GW signals, but the increasingly sensitive data sets offer increasingly stringent constraints on the SGWB"
] | [
"Background"
] | [
[
648,
667
]
] | [
[
428,
598
]
] |
2022ApJ...928L..16Y__Yang_&_Zhang_2018_Instance_1 | Fast radio bursts (FRBs) are cosmological radio transients with millisecond durations. Since the first FRB (FRB 010724, the Lorimer burst) was discovered in 2007 (Lorimer et al. 2007), hundreds of FRB sources have been detected, dozens of which are repeaters (e.g., the CHIME/FRB Collaboration et al. 2021). Recently, a ... | [
"Yang & Zhang 2018"
] | [
"which suggests that at least some FRBs originate from magnetars born from the core collapse of massive stars (e.g.,"
] | [
"Motivation"
] | [
[
745,
762
]
] | [
[
539,
654
]
] |
2019MNRAS.482.3550K__Weisz_et_al._2013_Instance_1 | The simplest approach to handling the problem of completeness is to be extremely conservative, and discard all data in regions of parameter space where the observations are not complete or nearly so. However, this invariably requires one to discard much of the available data. A somewhat more sophisticated approach is f... | [
"Weisz et al. 2013"
] | [
"Approaches of this type are widely used in astronomy, for example to infer star formation histories or stellar mass distributions from observed colour–magnitude diagrams (CMDs; e.g."
] | [
"Background"
] | [
[
927,
944
]
] | [
[
707,
888
]
] |
2019ApJ...871..243Y__Zhou_et_al._1993_Instance_1 | B335 is an isolated Bok globule with an embedded Class 0 protostar at a distance of 100 pc (Keene et al. 1980, 1983; Stutz et al. 2008; Olofsson & Olofsson 2009). The size of the dense core in B335 observed at millimeter wavelengths is ∼0.1 pc (Saito et al. 1999; Motte & André 2001; Shirley et al. 2002), and the core i... | [
"Zhou et al. 1993"
] | [
"Infalling and rotational motions on scales from 100 to 3000 au have been observed in molecular lines with single-dish telescopes and interferometers"
] | [
"Background"
] | [
[
546,
562
]
] | [
[
396,
544
]
] |
2016MNRAS.455..449H__Angus_et_al._2012_Instance_1 | The EFE mentioned in the previous section is due to the fact that the MOND equations (3) and (4) are non-linear and involve the total gravitational acceleration with respect to a pre-defined frame (e.g. the CMB frame). Decomposing the total gravitational field ∇Φ into an internal part $\boldsymbol g$ and an external fi... | [
"Angus et al. 2012"
] | [
"This must typically be done with a numerical Poisson solver"
] | [
"Uses"
] | [
[
664,
681
]
] | [
[
587,
646
]
] |
2021AandA...651A..24H__Simmons_&_Stewart_(1985)_Instance_1 | The two main problems arising when dealing with P are the typically low signal-to-noise ratio of the polarisation signal coming from ERS and the non-Gaussian distribution of its noise statistics. Regarding the former, as mentioned above, the typical polarisation fractions of ERS at frequencies below ∼10 GHz are at most... | [
"Simmons & Stewart (1985)"
] | [
"discussed four estimators which attempted to correct for biasing in the degree of linear polarisation in the presence of low signal-to-noise ratios."
] | [
"Background"
] | [
[
1101,
1125
]
] | [
[
1126,
1274
]
] |
2018ApJ...866...20D__Thompson_et_al._2012_Instance_1 | The physical processes involved in the formation of massive O-type stars and their feedback mechanisms are still under debate (Zinnecker & Yorke 2007; Tan et al. 2014). The energetics of O-type stars can affect the origin of new low-mass and massive stars (Deharveng et al. 2010). The massive stars are often surrounded ... | [
"Thompson et al. 2012"
] | [
"Note that the majority of the studies related to the MIR bubbles are mainly carried out for a single H ii region or several H ii regions on scales of a few parsecs (e.g.,"
] | [
"Compare/Contrast"
] | [
[
838,
858
]
] | [
[
531,
701
]
] |
2018MNRAS.475.4011B__Burrows_et_al._2011_Instance_1 | ASASSN-14li was discovered by the All Sky Automated Search for Supernova (ASASSN; Shappee et al. 2014) on ut 2014–11–22.63 (MJD 56983.6) as a 16.5 magnitude source in the V band (Jose et al. 2014; Holoien et al. 2016; Brown et al. 2017a). The position of the source was found to be consistent with the centre of the post... | [
"Burrows et al. 2011"
] | [
"Three events (Swift J1644+57;",
"have isotropic ∼5 GHz luminosities of between 1040 and 1042 erg s−1 whereas the rest",
"have luminosities in the range 1037 to 1039 erg s−1 at similar frequencies. The higher power events are believed to result from observing down the axis of a relativistic jet, resulting in th... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1152,
1171
]
] | [
[
1122,
1151
],
[
1265,
1349
],
[
1487,
1848
]
] |
2019AandA...627A.135B__Bessell_&_Brett_(1988)_Instance_1 | Optical color-magnitude and near-infrared (NIR) color-color diagrams are used to classify our variable candidates. The 2MASS JHKs data are available for 93 stars, while for the remaining two stars, photometric data are adopted from the UKIDSS Galactic Plane Survey (Lucas et al. 2008). The 2MASS photometry is transforme... | [
"Bessell & Brett (1988)"
] | [
"The sequence of dwarf and giants from",
"are also overplotted. The three parallel lines are the reddening vectors drawn from the tip of the giant branch (left), from the base of the MS branch (middle)"
] | [
"Uses",
"Uses"
] | [
[
696,
718
]
] | [
[
658,
695
],
[
777,
936
]
] |
2021MNRAS.502.2859N__Evans_&_Howarth_2008_Instance_1 | 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)"
] | [
"Given this deficit, we provide only a simplified estimate using radial velocities of OBA-type stars from",
"Since they belong to the same young population, we assume that they have a similar distance distribution and kinematics as the Cepheids."
] | [
"Uses",
"Compare/Contrast"
] | [
[
307,
329
]
] | [
[
202,
306
],
[
331,
467
]
] |
2019ApJ...887....8H__Marty_et_al._2011_Instance_1 | Silicon carbide is the best-characterized presolar mineral. It was identified more than 30 yr ago (Bernatowicz et al. 1987) because it is tagged with noble gases of anomalous isotopic compositions (Lewis et al. 1994). Subsequently, it was found that the major elements C and Si, and numerous minor elements contained in ... | [
"Marty et al. 2011"
] | [
"The mainstream grains have 12C/13C ratios between 10 and 100 (solar: 89), and the 14N/15N ratios of most of them are higher than the solar ratio of 440, the ratio measured for the solar wind"
] | [
"Background"
] | [
[
982,
999
]
] | [
[
790,
980
]
] |
2015AandA...579A.102B__Boselli_et_al._2009_Instance_1 | Once corrected for dust attenuation, Hα luminosities can be transformed into star formation rates (SFR, in M⊙ yr-1) using a factor that depends on the assumed IMF and stellar model7: (10)\begin{equation} {SFR = k({\rm H}\alpha) \times L({\rm H}\alpha)_{\rm cor}} . \end{equation}SFR=k(Hα)×L(Hα)cor.We recall that this re... | [
"Boselli et al. 2009"
] | [
"We recall that this relation is valid only under the assumption that the mean star formation activity of the emitting galaxies is constant on a timescale of a few Myr, roughly comparable to the typical time spent by the stellar population responsible for the ionisation of the gas on the main sequence"
] | [
"Uses"
] | [
[
601,
620
]
] | [
[
298,
599
]
] |
2021AandA...656A..16C__Bruno_&_Carbone_2013_Instance_3 | 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"
] | [
"Velocity fluctuations have been studied thoroughly (see, e.g.,",
"although the kinetic scales still remain quite unexplored for instrumental limitations, most notably in the sampling time resolution."
] | [
"Background",
"Future Work"
] | [
[
1518,
1538
]
] | [
[
1428,
1490
],
[
1541,
1674
]
] |
2022MNRAS.514.3894O__Buxton_et_al._2012_Instance_1 | The GBHT outburst light curves could be very complicated, and while the so-called ‘the main outburst’ could go through the spectral states described above, some GBHTs also show rebrightening episodes during the outburst decay (Kalemci et al. 2013) and/or an increase in brightness several days after the X-ray flux goes ... | [
"Buxton et al. 2012"
] | [
"Detection of rebrightening during the outburst decay supports the argument that the formation of a compact jet and its interaction with the accretion environment are imprinted on the multiwavelength behaviour of the GBHTs"
] | [
"Similarities"
] | [
[
955,
973
]
] | [
[
683,
904
]
] |
2021ApJ...923L..22A__Cordes_&_Jenet_2012_Instance_1 | Pulsar timing experiments (Sazhin 1978; Detweiler 1979) allow us to explore the low-frequency (∼1–100 nHz) part of the gravitational-wave (GW) spectrum. By measuring deviations from the expected arrival times of radio pulses from an array of millisecond pulsars, we can search for a variety of GW signals and their sourc... | [
"Cordes & Jenet 2012"
] | [
"Orbiting SMBHBs produce a",
"and transient GW bursts"
] | [
"Background",
"Background"
] | [
[
1168,
1187
]
] | [
[
484,
509
],
[
1115,
1138
]
] |
2016MNRAS.461.4176H__Jaffe_&_Kaiser_1995_Instance_1 | The Bayesian approach is indeed robust and optimal, within the context mentioned above. It focuses on the reconstruction of the LSS within the framework of the standard model of cosmology and for a given data base. However, most previous studies have not addressed the question how consistent is the assumed cosmological... | [
"Jaffe & Kaiser 1995"
] | [
"The relevant methodology is straightforward and well established. One needs to calculate the likelihood function of the data given the model – namely the probability of the occurrence of the data within the framework of the assumed model"
] | [
"Uses"
] | [
[
1094,
1113
]
] | [
[
855,
1092
]
] |
2018MNRAS.480.4154C__Maisinger,_Hobson_&_Lasenby_2004_Instance_1 | Classical imaging techniques were developed in the field to solve the RI reconstruction problem, such as clean and its multiscale variants (Högbom 1974; Bhatnagar & Corwnell 2004; Cornwell 2008; Stewart, Fenech & Muxlow 2011). In particular, clean builds a model image by iteratively removing point source components fro... | [
"Maisinger, Hobson & Lasenby 2004"
] | [
"However, an optimal metric – expressed as an entropy functional – is not known in advance and therefore needs to be chosen individually"
] | [
"Uses"
] | [
[
1337,
1369
]
] | [
[
1180,
1315
]
] |
2020AandA...641A.155V__Spilker_et_al._(2016)_Instance_1 | The right panel of Fig. 7 shows the relation between ΣSFR and R52. For each object, we computed ΣSFR = SFR/(2πR2), where R is a representative value of the galaxy radius. The latter is rather arbitrary and it depends on the chosen tracer, the depth, resolution, and wavelength of the observations. Here we adopted the AL... | [
"Spilker et al. (2016)"
] | [
"For the SPT-SMGs, we used the sizes of"
] | [
"Uses"
] | [
[
806,
827
]
] | [
[
767,
805
]
] |
2022MNRAS.512.3137Z__Katz_et_al._1999_Instance_2 | However, it is not straightforward to explain H2 formation in astronomical sources even when the catalytic roles of dust grains are introduced into models. Interstellar species are believed to be formed on cold grain surfaces via the so called Langmuir–Hinshelwood mechanism (Watson & Salpeter 1972; Pickles & Williams 1... | [
"Katz et al. 1999"
] | [
"It was found that if we assume a single H desorption energy in models, the dust temperature range over which efficient H2 formation occurs is narrow (6–10 K for olivine grains)"
] | [
"Background"
] | [
[
1674,
1690
]
] | [
[
1496,
1672
]
] |
2020ApJ...900..100R__White_et_al._2019_Instance_1 | It is much harder to localize and track the formation of current sheets in realistic black hole accretion flows in a larger domain and for a longer period because of the effects of the more complicated global dynamics governed by the central object, and due to the turbulence induced by the MRI. Both the evolution of ac... | [
"White et al. 2019"
] | [
"In the magnetically arrested disk",
"scenario, the MRI and subsequent turbulence in the inner accretion disk are suppressed due to large-scale magnetic flux (see, e.g.,"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
817,
834
]
] | [
[
598,
631
],
[
685,
816
]
] |
2020ApJ...893..124Z__Tenbarge_&_Howes_2013_Instance_1 | In hydrodynamic and magnetohydrodynamic systems, different fluctuations interact with each other nonlinearly, generating turbulence (Matthaeus et al. 2015). One of the most important characteristics of turbulence is the existence of intermittency among various scales. Spatial intermittency manifests as coherent structu... | [
"Tenbarge & Howes 2013"
] | [
"Plenty of simulation works",
"have indicated that dissipation, acceleration, and thermalization of turbulent plasmas mainly take place near intermittent structures on kinetic scale, while the actual physical mechanisms behind dissipation remain unclear."
] | [
"Background",
"Background"
] | [
[
1002,
1023
]
] | [
[
928,
954
],
[
1067,
1290
]
] |
2018MNRAS.475.4011B__Zauderer_et_al._2011_Instance_1 | ASASSN-14li was discovered by the All Sky Automated Search for Supernova (ASASSN; Shappee et al. 2014) on ut 2014–11–22.63 (MJD 56983.6) as a 16.5 magnitude source in the V band (Jose et al. 2014; Holoien et al. 2016; Brown et al. 2017a). The position of the source was found to be consistent with the centre of the post... | [
"Zauderer et al. 2011"
] | [
"A small number (currently six) of confirmed TDEs, including ASASSN-14li, have also been detected at radio wavelengths and the population may form a bi-modal distribution, consisting of more common non-relativistic ‘thermal’ events and rarer relativistic jets. Three events (Swift J1644+57",
"have isotropic ∼5 GHz... | [
"Background",
"Background",
"Background"
] | [
[
1173,
1193
]
] | [
[
862,
1150
],
[
1265,
1332
],
[
1563,
1725
]
] |
2022ApJ...933..243F__Woosley_&_Bloom_2006b_Instance_1 | Gamma-ray bursts (GRBs) are among the most powerful gamma-ray sources in the universe. They could be generated from the merger of binary compact objects (BCOs; Duncan & Thompson 1992; Usov 1992; Thompson 1994; Metzger et al. 2011) or the death of massive stars (Woosley 1993; Paczyński 1998; Woosley & Bloom 2006a). The ... | [
"Woosley & Bloom 2006b"
] | [
"On the other hand, long-duration gamma-ray bursts (lGRBs",
"are associated with the core collapse (CC) of dying massive stars",
"leading to supernovae (SNe;"
] | [
"Background",
"Background",
"Background"
] | [
[
948,
969
]
] | [
[
705,
761
],
[
800,
865
],
[
901,
928
]
] |
2017ApJ...835....2X__Collins_et_al._2012_Instance_1 | On the other hand, a clear physical interpretation of the observed pulse broadening phenomenon requires a good understanding of the interstellar electron density structure. A power-law model of electron density fluctuations is commonly adopted in theoretical constructions on radio wave propagation (Lee & Jokipii 1976; ... | [
"Collins et al. 2012"
] | [
"Recent advances in understanding the properties of magnetohydrodynamic (MHD) turbulence",
"stimulate a renewed investigation on density statistics"
] | [
"Motivation",
"Motivation"
] | [
[
744,
763
]
] | [
[
420,
507
],
[
589,
644
]
] |
2017MNRAS.471.2917K__Glenn_et_al._2015_Instance_1 | The only way to access the transitions which trace warmer molecular gas is to get above the atmosphere as did the Herschel Space Observatory The Herschel SPIRE Fourier Transform Spectrometer (FTS) was simultaneously sensitive to the J = 4−3 (EJ = 4 = 55 K) up to the J = 13−12 (EJ = 13 = 503 K) line of CO for local gala... | [
"Glenn et al. 2015"
] | [
"Many studies of individual galaxies",
"have shown that the higher J lines of CO arise from warmer, denser gas than the cold gas responsible for the emission of for example CO J = 1−0."
] | [
"Background",
"Background"
] | [
[
958,
975
]
] | [
[
641,
676
],
[
1239,
1383
]
] |
2022MNRAS.510.1043B__Kukula_et_al._1998_Instance_1 | The origin of the radio emission in radio-loud active galactic nuclei (RL AGN) is clear, luminous relativistic jets of magnetized plasma, which can extend far out, on the host galaxy scale and beyond. Conversely, radio-quiet (RQ) AGN are associated with radio emission which is typically 103 times weaker (as defined by ... | [
"Kukula et al. 199"
] | [
"The fewer radio studies of RQ AGN",
"generally lead to mixed results. This encourages to keep investigating it, as it indicates that the origin of the radio emission in RQ AGN is still an open question."
] | [
"Motivation",
"Motivation"
] | [
[
896,
913
]
] | [
[
766,
799
],
[
1128,
1293
]
] |
2019ApJ...882..144K__Berk_et_al._2001_Instance_1 | The FOCAS and NIRSPEC spectra of PSO J006+39 were obtained at two different epochs separated by 1 yr and 9 months (by slightly less than 3 months in the quasar rest frame). Previously, we found that the PS1 y-band light curve of PSO J006+39 shows brightness variations with a peak-to-peak amplitude of ∼0.7 mag over ∼4 y... | [
"Vanden Berk et al. 2001"
] | [
"The estimated continuum slope is consistent but somewhat flatter than the typical slope of luminous quasars"
] | [
"Compare/Contrast"
] | [
[
1084,
1107
]
] | [
[
954,
1061
]
] |
2020AandA...640A.121G__Swain_et_al._2009_Instance_1 | The planetary physical properties that can be derived from measurements with the two most successful exoplanet detection techniques, that is, with the radial velocity method and the transit method, are the planet radius (if the planet transits its star), mass (a lower limit if the planet does not transit its star), and... | [
"Swain et al. 2009"
] | [
"The upper atmospheres (above optically thick clouds) of giant exoplanets and those of smaller planets around M stars can be probed using spectroscopy during primary and/or secondary transits"
] | [
"Background"
] | [
[
673,
690
]
] | [
[
463,
653
]
] |
2020ApJ...900...45L__Helmi_et_al._2018_Instance_1 | Much of the recent work on this topic has focused on gathering observational evidence for hierarchical growth through the identification of stellar streams and tidal interactions, which are thought to be the hallmark of low-mass galaxies having been accreted by more massive galaxies. The Sagittarius dwarf galaxy (Ibata... | [
"Helmi et al. 2018"
] | [
"Recent data from the Gaia mission",
"and other large-scale surveys, as well as analyses that combine kinematic data with information about chemical abundances and/or specific stellar populations, have led to discoveries of additional substructures in the Galaxy and brought renewed attention to this topic (e.g.,"... | [
"Motivation",
"Motivation"
] | [
[
887,
904
]
] | [
[
501,
534
],
[
568,
843
]
] |
2015ApJ...806..167G__Daughton_&_Karimabadi_2007_Instance_1 | We envision a situation where intense current sheets are developed within a magnetically dominated plasma. Earlier work in nonrelativistic low-β plasmas has shown that the gradual evolution of the magnetic field can lead to formation of intense, nearly force-free current layers where magnetic reconnection may be trigge... | [
"Daughton & Karimabadi 2007"
] | [
"The full particle simulations are performed using",
"and NPIC code",
"both of which solve Maxwell equations and push particles using relativistic approaches. The VPIC code directly evolves electric and magnetic fields, whereas in the NPIC code the fields are advanced using the scalar and vector potentials.",
... | [
"Uses",
"Uses",
"Background",
"Similarities"
] | [
[
1566,
1592
]
] | [
[
1444,
1493
],
[
1529,
1542
],
[
1595,
1832
],
[
1833,
2005
]
] |
2019ApJ...877...35W__Hu_&_Yang_2014_Instance_1 | Here, for simplicity, computational convenience, and continuity with past works (Kopparapu et al. 2017; Haqq-Misra et al. 2018), we have assumed a slab ocean with zero ocean heat transport. Ocean heat transport may have a significant effect on climate and also the location of clouds (Way et al. 2018). Dynamic ocean hea... | [
"Hu & Yang 2014"
] | [
"Dynamic ocean heat transport on completely ocean-covered worlds (i.e., no continents) leads to warmer global mean temperatures and a reduction in day–night temperature differences on synchronously rotating planets",
"In future works, our group plans to couple our GCM with a dynamic ocean model to study the inter... | [
"Motivation",
"Future Work"
] | [
[
518,
532
]
] | [
[
303,
516
],
[
1717,
1885
]
] |
2021AandA...656A..63M__Shakura_&_Sunyaev_1973_Instance_1 | One possibility could be that the disk, since viewed at such high inclination, might create a “shadow” zone where part of the reflection incoming between Rin, 1 and Rin, 2 is obscured (see Fig. 10, panel a). As highlighted by the Figure, a jump in the scale height of the disk, located sufficiently far away from its inn... | [
"Shakura & Sunyaev 1973"
] | [
"In the outer regions of a Shakura-Sunyaev disk, the opacity is expected to be mainly due to free-free absorption, while Thomson scattering dominates the opacity in the inner regions of the disk (see Eqs. (2.16) and (2.19) of",
"The geometrical thickness of the disk scales with the radius R following a (slightly)... | [
"Uses",
"Uses"
] | [
[
1079,
1101
]
] | [
[
854,
1078
],
[
1104,
1596
]
] |
2022AandA...666A..60K__Gustafsson_et_al._2008_Instance_1 | High-precision photometric measurements have shown that the present treatment of limb darkening is not sufficiently accurate and leads to systematic errors in the derived parameters of the exoplanets (e.g., Espinoza & Jordán 2016; Morello et al. 2017a; Maxted 2018). Typically, limb darkening is represented by rather si... | [
"Gustafsson et al. 2008"
] | [
"Consequently, many libraries of limb-darkening coefficients covering a wide range of effective temperatures (Teff), surface gravity (log g), and metal-licities (M/H) have been produced",
"using various radiative transfer codes, such as",
"MARCS"
] | [
"Background",
"Background",
"Background"
] | [
[
1111,
1133
]
] | [
[
713,
897
],
[
971,
1018
],
[
1104,
1109
]
] |
2022MNRAS.511.2885B__Lu_et_al._2013_Instance_1 | One of our key results is that accounting for a complete stellar mass function can explain the post-starburst preference of TDE hosts. The alternative, currently most widespread explanation is that post-starburst galaxies are initially born with an extremely steep density profile (Stone et al. 2018). Fig. 6 compares th... | [
"Lu et al. 2013"
] | [
"In fact, Sanders (1998) points out that, too close to the MBH, molecular clouds should get disrupted by its gravitational field preventing star formation; even if the Milky Way nucleus features a population of young stars very close to the MBH",
"supporting instead the idea of possible central star formation, it... | [
"Background",
"Similarities"
] | [
[
1044,
1058
]
] | [
[
768,
1011
],
[
1061,
1178
]
] |
2018AandA...614A..48B__Keselman_&_Nusser_2012_Instance_1 | The driving mechanisms and chronology of the buildup of bulges in late-type galaxies (LTGs) is an issue of key relevance to our understanding of galaxy evolution. According to our current knowledge on bulge demographics in the local universe, a large fraction of LTGs host pseudo-bulges (PBs; e.g., Gadotti 2009; Fisher ... | [
"Keselman & Nusser 2012"
] | [
"Traditionally, bulges were thought to invariably form early-on via",
"or mergers",
"with the disk gradually building up around them.",
"Whereas this inside-out galaxy formation scenario appears consistent with important integral characteristics of CBs (e.g., their red colors), it does not offer a plausible e... | [
"Background",
"Background",
"Background",
"Compare/Contrast"
] | [
[
1391,
1413
]
] | [
[
1219,
1285
],
[
1338,
1348
],
[
1475,
1523
],
[
1524,
1752
]
] |
2016AandA...588A..44Y__Jones_et_al._2014_Instance_3 | The second issue concerns the fact that inside a given region, coreshine is not detected in all the dense clouds observed by Paladini (2014) and Lefèvre et al. (2014) and that the proportion of clouds exhibiting coreshine varies from one region to another. For instance, 75% of the dense clouds detected in Taurus exhibi... | [
"Jones et al. 2014"
] | [
"In transition regions from diffuse ISM to dense clouds",
"\\hbox{$0.7 \\leqslant A_{V} \\leqslant 1.2$}0.7 ⩽ AV⩽ 1.2 for the standard ISRF), better shielded from UV photons and where the amount of hydrogen is significantly higher, H-poor carbon can be transformed into H-rich carbon through H atom incorporation, ... | [
"Background",
"Background"
] | [
[
1849,
1866
]
] | [
[
1793,
1847
],
[
1868,
2381
]
] |
2021MNRAS.503.6155C__Lovisari_et_al._2017_Instance_2 | Galaxy clusters are the traces of the formation of the largest structures in the Universe and so reliable tools to investigate structures formation and evolution. In principle, this is possible only if and when we have full knowledge of the properties of these objects. The total mass (i.e. the total amount of the dark ... | [
"Lovisari et al. 2017"
] | [
"They exploit the maps with different apertures and efficiencies and are applied individually or combined together, even with different weights (see e.g."
] | [
"Compare/Contrast"
] | [
[
3224,
3244
]
] | [
[
2948,
3100
]
] |
2019ApJ...881...42J__Jørgensen_1999_Instance_1 | Stellar population evolution studies beyond z ≈ 1 have primarily focused on ages through studies of luminosity changes. Beifiori et al. (2017) used new data for 19 galaxies in z = 1.3–1.6 clusters obtained with the Very Large Telescope/KMOS to extend the redshift coverage of the results regarding the evolution of the m... | [
"Jørgensen 1999"
] | [
"The authors used their new results together with",
"and low-redshift reference data for the Coma cluster",
"to further solidify the evidence supporting passive evolution and a formation redshift zform ≈ 2."
] | [
"Background",
"Background",
"Background"
] | [
[
767,
781
]
] | [
[
383,
431
],
[
713,
765
],
[
806,
903
]
] |
2020ApJ...899L..10F__Tomida_et_al._2013_Instance_1 | Understanding of the low-mass star formation process has been intensively studied from decades ago, mainly by theoretical work at the beginning (e.g., Larson 1969; Shu 1977; Shu et al. 1987; Inutsuka 2012). They explained that the fragmentation and condensation of molecular clouds result in forming dense cores, which u... | [
"Tomida et al. 2013"
] | [
"According to the theoretical studies, dense cores eventually harbor the first protostellar cores, the first quasi-hydrostatic object during the star formation process (hereafter the first core; e.g.,",
"which provide the initial condition of star formation."
] | [
"Background",
"Background"
] | [
[
600,
618
]
] | [
[
365,
564
],
[
621,
675
]
] |
2020AandA...641A.155V__Puglisi_et_al._2019_Instance_3 | The scenario presented above has been formulated in various flavors to individually explain several of the properties reported here. The main addition of this work, namely the excitation of CO in distant main-sequence and starburst galaxies, fits in the general picture that we sketched. The ensemble of properties and c... | [
"Puglisi et al. 2019"
] | [
"Such transition might well imply an imminent increase of the SFR, driving the object in the realm of starbursts",
"or its cessation, bringing the system back onto or even below the main sequence",
"with the CO properties potentially able to distinguish between these two scenarios."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Future Work"
] | [
[
1447,
1466
]
] | [
[
1198,
1309
],
[
1338,
1417
],
[
1469,
1552
]
] |
2016ApJ...832..195N__Jin_et_al._2012_Instance_2 | We ignore the density stratification effect in Case I, II, and IIa, because the width of the horizontal current sheet in our simulations is much shorter than the length. The simulation domain extends from x = 0 to x = L0 in the x-direction, and from
y
=
−
0.5
L
0
to
y
=
0.5
L
0
in the y-dire... | [
"Jin et al.",
"2012"
] | [
"and the magnetic field can exceed 0.15 T in both the intranetwork and the network quiet region"
] | [
"Uses"
] | [
[
1637,
1647
],
[
1654,
1658
]
] | [
[
1477,
1571
]
] |
2015ApJ...802....8A__Susa_2013_Instance_1 | Early theoretical work on the formation of the first stars, mostly through high-resolution simulations, found that Pop III stars with mass MIII,* ≳ 100 M⊙ are born in isolation inside minihalos, and thus the “one massive Pop III star per minihalo” paradigm was established (Abel et al. 2002; Bromm et al. 2002; Yoshida e... | [
"Susa 2013"
] | [
"While the universality of the latter finding is in doubt",
"it certainly introduces very important subtleties to the old paradigm"
] | [
"Motivation",
"Motivation"
] | [
[
628,
637
]
] | [
[
532,
588
],
[
751,
820
]
] |
2018AandA...610A..44M__Krüger_&_Dreizler_(1992)_Instance_1 | The first investigations of the rotational spectra of ethyl isocyanide were carried out in 1966 by Bolton et al. (1966). The spectra of the first vibrational and torsional excited states were measured in the centimeter wave domain (Anderson & Gwinn 1968). In this initial study, the dipole moment was determined to be μa... | [
"Krüger & Dreizler (1992)"
] | [
"The most recent spectroscopic study is from",
"who reinvestigated the internal rotation measurements and also determined hyperfine coupling parameters due to the nitrogen quadrupole"
] | [
"Background",
"Background"
] | [
[
720,
744
]
] | [
[
676,
719
],
[
745,
879
]
] |
2021ApJ...908...15S__Scoville_et_al._2014_Instance_1 | Several methods are commonly used to estimate gas masses. The first method is using CO emission line fluxes (e.g., Daddi et al. 2010; Genzel et al. 2010; Tacconi et al. 2010, 2013). This method has uncertainties on the CO-to-H2 conversion factor, which changes depending on metallicity (Genzel et al. 2012), and on the C... | [
"Scoville et al. 2014"
] | [
"Gas masses can also be estimated with an empirically calibrated relation between single-band dust continuum flux at the Rayleigh–Jeans (R-J) tail and gas mass (e.g.,",
"These scaling relations are calibrated with local galaxies or with local galaxies and SMGs up to z ∼ 2. In this method, the gas-to-dust mass rat... | [
"Background",
"Background",
"Compare/Contrast"
] | [
[
1022,
1042
]
] | [
[
856,
1021
],
[
1071,
1301
],
[
1302,
1449
]
] |
2017AandA...597A.114B__Bergin_&_Tafalla_(2007)_Instance_1 | The band-merged Hi-GAL product catalogue (Elia et al. 2016) is built as in Elia et al. (2013) and provides spectral energy distribution (SED) fit parameters to the individual clumps. The average angular size of the clumps is 25′′ at 250 μm. Using the heliocentric distances provided in the Hi-GAL product catalogue (desc... | [
"Bergin & Tafalla (2007)"
] | [
"The catalogue explores a wide range of linear diameters and masses, from sub-parsec (≤ 0.1 pc) to parsec scale (1−5 pc) with masses from 1 M⊙ to 105M⊙. These wide ranges mean that we probably mix several types of objects, from single star-forming cores to clumps containing multiple cores, even to entire clouds, de... | [
"Uses"
] | [
[
906,
929
]
] | [
[
461,
905
]
] |
2022MNRAS.516.2641V__Soleri_&_Fender_2011_Instance_1 | The connection between the accretion flow and compact jets is routinely studied in the X-ray–radio luminosity (LX–LR) diagram. Here, the former traces the accretion luminosity and is a proxy for accretion rate, while the latter traces the jet and its brightness. Compact BH jets show an LX–LR correlation across ∼eight o... | [
"Soleri & Fender 2011"
] | [
"Compact BH jets show an LX–LR correlation across ∼eight orders of magnitude in X-ray luminosity",
"a subset of sources follows a radio-bright correlation with a power-law slope of β ≈ 0.6 (where $L_R \\propto L_X^{\\beta }$, while others follow a steeper correlation with β ≳ 1 at high X-ray luminosities, before ... | [
"Background",
"Background"
] | [
[
721,
741
]
] | [
[
263,
358
],
[
431,
700
]
] |
2016MNRAS.462.3441D__Namouni_1999_Instance_5 | 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"
] | [
"This is not the Kozai–Lidov resonance; in this case, the Kozai–Lidov domain (domain II in",
"is characterized by libration around $\\omega _{\\rm r}=0{^\\circ }$ (or 180°) which is only briefly observed at the end of the backwards integrations",
"see Fig. 6"
] | [
"Compare/Contrast",
"Compare/Contrast",
"Uses"
] | [
[
1851,
1863
]
] | [
[
1761,
1850
],
[
1865,
2012
],
[
2014,
2024
]
] |
2020AandA...643A..92S__Huang_et_al._2018a_Instance_1 | Our models show that high signal to noise ratio (S/N) spiral structures in the gas dynamics, together with a spiral seen in the dust continuum surface density, can put constraints on grain size comparing the observed amplitude of the spiral in the dust with that in the gas. There are multiple candidate sources that are... | [
"Huang et al. 2018a"
] | [
"Out of the recent high-resolution Disk Substructures at High Angular Resolution Project (DSHARP) survey of 20 disks, 3 were found to harbor spirals: Elias 27, WaOph 6, and IM Lup"
] | [
"Uses"
] | [
[
708,
726
]
] | [
[
528,
706
]
] |
2016MNRAS.462.1415C__Bolzonella_et_al._2010_Instance_1 | Two major limitations, often neglected, affect this type of analysis: the adoption of oversimplified models to describe the wide variety of observed galaxy SEDs and the presence of ‘systematic’ model uncertainties. This second limitation has been addressed in several studies already (e.g. Charlot, Worthey & Bressan 199... | [
"Bolzonella et al. 2010"
] | [
"For example, most existing approaches rely on the adoption of a rigid physical model (e.g. analytic, two-parameter star formation histories combined with a standard dust attenuation curve and the assumption that all stars in a galaxy have the same metallicity) to describe galaxy SEDs (e.g.",
"this does not allow... | [
"Background",
"Compare/Contrast"
] | [
[
1410,
1432
]
] | [
[
1119,
1409
],
[
1825,
2013
]
] |
2018MNRAS.477.3520L__Abolfathi_et_al._2018_Instance_2 | 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"
] | [
"To illustrate this, we show examples of calibration vectors for SDSS",
"eBOSS DR14"
] | [
"Uses",
"Uses"
] | [
[
1011,
1032
]
] | [
[
837,
905
],
[
979,
989
]
] |
2018ApJ...854...73I__Schenker_et_al._2013_Instance_1 | The best-fit parameters are shown in Table 3. We find that the uncertainties in M* and
are considerably large due to a degeneracy between the two parameters when all parameters are variable. Plotted in Figure 1 is the faint-end slope α as a function of redshift. Our results indicate that the best-fit values of α... | [
"Schenker et al. 2013"
] | [
"We also plot the results of previous blank-field surveys"
] | [
"Uses"
] | [
[
834,
854
]
] | [
[
697,
753
]
] |
2020AandA...642A..19M__Tempel_et_al._(2014a)_Instance_1 | While this large-scale structure of the Universe (LSS) is also composed of dark matter and gas, it was through the galaxy distribution that it has started to be detected. Galaxy clusters were the first cosmic web features to be identified and studied because they are easily detectable through various techniques. Only w... | [
"Tempel et al. (2014a)"
] | [
"For example, Chen et al. (2016) and",
"have produced filament catalogues in the SDSS"
] | [
"Background",
"Background"
] | [
[
911,
932
]
] | [
[
875,
910
],
[
933,
978
]
] |
2020MNRAS.492..444Y__Proga_&_Begelman_2003_Instance_1 | In spite of these similarities, the angular profiles of these properties in two-dimensional simulations reveal a totally different accretion pattern. Within the stagnation radius, winds are mainly accreted in the polar region as a result of the low angular momentum there, whereas material with high angular momentum in ... | [
"Proga & Begelman 2003"
] | [
"This ‘funnel’ accretion scenario is also found in other simulations with a spherical-like distribution of rotationally accreting material"
] | [
"Similarities"
] | [
[
600,
621
]
] | [
[
461,
598
]
] |
2017ApJ...850...18H__Murase_et_al._2015_Instance_1 | The heating due to the reprocessing of non-thermal photons produced in the nebula can be efficient even at late times. Here, we treat these processes in a simple way as follows. At early times, electromagnetic cascades proceed in the saturation regime, leading to a flat energy spectrum up to ∼1 MeV (Metzger et al. 2014... | [
"Murase et al. 2015"
] | [
"At later times, the spectrum depends on the seed photon spectra, but it can roughly be estimated to be a flat spectrum from ∼1 eV to ∼0.1 TeV, while the supernova emission continues, which is expected based on more detailed calculations (e.g.,"
] | [
"Uses"
] | [
[
567,
585
]
] | [
[
323,
566
]
] |
2020ApJ...901...41S__Harrington_1973_Instance_1 | Observations have shown that the shape of the Lyα line is diverse. It includes broad damped absorption profiles, P-Cygni profiles, double-peak profiles, pure symmetric emission profiles, and combinations thereof (Kunth et al. 1998; Mas-Hesse et al. 2003; Shapley et al. 2003; Møller et al. 2004; Noll et al. 2004; Tapken... | [
"Harrington 1973"
] | [
"This variety can be understood through a detailed radiative transfer calculation, which is analytically solvable only for simple cases (e.g., a static, plane-parallel slab by"
] | [
"Background"
] | [
[
552,
567
]
] | [
[
377,
551
]
] |
2020MNRAS.496.1051A__Rudolph_et_al._2006_Instance_2 | The radial distribution of S/H ratios and the corresponding gradient are shown in panel (b) of Fig. 12. We obtain a slope of −0.035 ± 0.006 dex kpc−1 (very similar to the one we obtain with the ICF of ADIS20, as can be seen in Table 8), which is consistent with the one of −0.041 ± 0.014 dex kpc−1 estimated by Rudolph e... | [
"Rudolph et al. 2006"
] | [
"Recently, Fernández-Martín et al. (2017) reported a slope of −0.108 ± 0.006 dex kpc−1 using optical spectra for H ii regions located at RG between 5 and 17 kpc. That value of the slope is considerably much steeper than our determination and other previous estimates from the literature (e.g."
] | [
"Differences"
] | [
[
902,
921
]
] | [
[
530,
822
]
] |
2021ApJ...917...24Z__Coughlin_et_al._2020b_Instance_2 | 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"
] | [
"In view of the fact that the limiting magnitude of the follow-up wide-field survey projects is almost ≲21 mag (e.g.,",
"the maximum detectable distance for BH–NS kilonovae would be ≲200 Mpc, which can hardly cover the horizon of GW-triggered BH–NS merger events that O3 found (as shown in Figure 10)."
] | [
"Uses",
"Uses"
] | [
[
961,
982
]
] | [
[
801,
917
],
[
1026,
1206
]
] |
2022MNRAS.515.2188H__Rorai_et_al._2018_Instance_2 | 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"
] | [
"Therefore, by restricting attention to data in the distribution outskirts, this approach throws away information and reduces the sensitivity to the IGM thermal state significantly"
] | [
"Background"
] | [
[
1891,
1908
]
] | [
[
1710,
1889
]
] |
2018ApJ...867..101B___2018b_Instance_1 | To fully describe a population of streams, we need a realistic model of the Galaxy. The latest generation of hydrodynamical simulations have produced models that well reproduce a multitude of features observed in galaxies, both as individual objects (e.g., Wetzel et al. 2016) and as a population (e.g., Nelson et al. 20... | [
"Lilley et al.",
"2018b"
] | [
"In the classic study, Hernquist & Ostriker (1992) developed a set of basis functions for density and gravitational potential that can reproduce complex morphology of galaxies with a small number of terms (e.g.,",
"These expansions reproduce the force field of an N-body simulation with a precision of a few percen... | [
"Background",
"Motivation"
] | [
[
884,
897
],
[
905,
910
]
] | [
[
653,
863
],
[
913,
1262
]
] |
2021AandA...655A..99D__Carigi_et_al._2005_Instance_2 | 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)"
] | [
"This suggests that low-mass stars mostly contribute to carbon around solar metallicity, whereas at super-solar metallicities, massive stars produce carbon together with oxygen, thereby flattening or even decreasing the [C/O] ratio. This trend is in agreement with the metallicity dependent yields from",
"which pr... | [
"Similarities",
"Similarities"
] | [
[
1909,
1929
]
] | [
[
1607,
1908
],
[
1931,
2140
]
] |
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