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 |
|---|---|---|---|---|---|---|
2018AandA...615L..16F__Gal_et_al._(2014)_Instance_1 | Nitrogen chemistry mainly consists of three competing processes: (i) the conversion of atomic N to N2 in the gas phase, (ii) destruction of N2, for instance, via photodissociation and reaction with He+, and (iii) freeze-out of atomic N and N2 onto dust grains followed by surface reactions (e.g., Daranlot et al. 2012; L... | [
"Le Gal et al. (2014)"
] | [
"According to the pseudo-time-dependent gas-phase astrochemical model under dense cloud conditions (104 cm−3, 10 K, 10 mag) by",
"the conversion of atomic N into N2 takes an order of Myr, depending on assumed elemental abundances. In the gas-ice model of Daranlot et al. (2012), under the similar physical conditio... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
634,
654
]
] | [
[
508,
633
],
[
656,
967
]
] |
2018MNRAS.481..138B__Mullaney_et_al._2013_Instance_1 | To mitigate this problem, several studies have suggested to use the width of the [O iii]λ5007 Å emission line (hereafter [O iii]) originating in the narrow-line region (NLR) as a surrogate for σ⋆, assuming that the NLR is gravitationally bound to the bulge and thus, that the gas kinematics follows the bulge potential (... | [
"Mullaney et al. 2013"
] | [
"In particular, it is known to often display a blue wing (e.g.",
"generally interpreted as a signature of outflows with dust preferentially hiding one cone behind the stellar disc. For that reason, some studies have excluded the [O iii] blue wing"
] | [
"Motivation",
"Motivation"
] | [
[
969,
989
]
] | [
[
818,
879
],
[
1009,
1189
]
] |
2021AandA...653A..36M__Goulding_&_Alexander_(2009)_Instance_6 | The SFG sample was constructed using the Great Observatories All-Sky LIRG Survey (GOALS sample, Armus et al. 2009), from which we extracted 158 galaxies, with data from Inami et al. (2013), who report the fine-structure lines at high resolution in the 10 − 36 μm interval, and Stierwalt et al. (2014), who include the de... | [
"Goulding & Alexander (2009)"
] | [
"Both Bernard-Salas et al. (2009) and",
"reported data from the high-resolution Spitzer-IRS spectra."
] | [
"Similarities",
"Similarities"
] | [
[
2800,
2827
]
] | [
[
2763,
2799
],
[
2828,
2887
]
] |
2015ApJ...803...79L__Güsten_et_al._2006_Instance_1 | The number counts of the most massive clusters have the potential to constrain cosmological parameters. Unfortunately, these systems also tend to be most affected by the effects described above. Massive systems will produce the greatest gravitational lensing shear, and in our hierarchical universe, they are also common... | [
"Güsten et al. 2006"
] | [
"In this work, we aim to better understand how these considerations affect the observed SZE signals using high-resolution submillimeter and radio imaging of a representative sample of SZE-selected clusters.We present new observations at 345 GHz (19 2 resolution) with the Large APEX Bolometer Camera",
"on the Atac... | [
"Uses",
"Uses",
"Uses"
] | [
[
734,
752
]
] | [
[
361,
659
],
[
690,
732
],
[
754,
763
]
] |
2019ApJ...875...90L__Velli_et_al._2015_Instance_2 | When energy flows from the interior of the Sun outward into the solar atmosphere, why is the Sun’s outer atmosphere, the corona, much hotter than the inner atmosphere, the underlying chromosphere and photosphere? This is the long-standing problem of the coronal heating, which is one of the eight key mysteries in modern... | [
"Velli et al. 2015"
] | [
"Meanwhile, with the progress of observational studies, two groups of theoretical models, magnetic reconnection models and magnetohydrodynamic wave models, have traditionally attempted to explain coronal heating, but so far no models can address the key mystery perfectly"
] | [
"Motivation"
] | [
[
1997,
2014
]
] | [
[
1648,
1918
]
] |
2019MNRAS.488.4638L__Drabek-Maunder_et_al._2016_Instance_1 | In Fig. 10, we plot the variation of the ratio of the outflow contribution to the FWHM and turbulent energy. The ratio of the outflow contribution = 1 – ‘non-outflow contribution’/‘all contributions’. We observe that the outflow has a contribution in the FWHM: about 20 per cent in the local region at the H ii region (... | [
"Drabek-Maunder et al. 2016"
] | [
"It has a contribution of at least 15 per cent in the clump at early stages of massive star formation, which is lower than that reported in previous studies"
] | [
"Differences"
] | [
[
753,
779
]
] | [
[
579,
734
]
] |
2018AandA...619A.177B__Mayne_(2010)_Instance_1 | The wealth of precise all-sky data from the Gaia Data Release 2 (DR2) revealed a new feature in the Herzsprung–Russell diagram (HRD), namely a gap in the mid-M dwarf main sequence (Jao et al. 2018). The gap appears at a magnitude MG ∼ 10 and colour GBP – GRP ∼ 2.3−2.5 in the Gaia filter system. It is observed in optica... | [
"Mayne (2010)"
] | [
"Interestingly,",
"was the first to suggest the existence of an observational signature for the transition between fully and partly convective structures for pre-main sequence stars and predicted that it would result in a HRD gap. This author explored signatures of this transition in young clusters and linked the... | [
"Background",
"Background"
] | [
[
615,
627
]
] | [
[
600,
614
],
[
628,
1086
]
] |
2015AandA...584A..76S__Bernstein_et_al._(1995)_Instance_1 | The only gas-phase process, which is predicted to efficiently lead to products, is the process involving ionized methanimine. According to the model by Vuitton et al. (2007), the amount in the upper atmosphere of Titan of ionized methanimine is small, but not negligible. The products of the reaction CH2NH + CH2NH+ all ... | [
"Bernstein et al. (1995)"
] | [
"As for the experiment on ice by",
"it is well known that reaction barriers possibly present in gas-phase reactions are not significantly reduced when moving to ice-mediated reactions"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1187,
1210
]
] | [
[
1155,
1186
],
[
1212,
1359
]
] |
2019AandA...629A.134G__Leitherer_et_al._2010_Instance_1 | We used the combination of models from STARBURST99 and our model for the contribution from stripped stars to represent the radiation of a full stellar population in which stripped stars are formed. We made our models publicly available on the STARBURST99 online interface2, providing the addition from stripped stars to ... | [
"Leitherer et al. 2010"
] | [
"We chose to compare to the",
"spectral models from WM-BASIC for OB-stars"
] | [
"Uses",
"Uses"
] | [
[
944,
965
]
] | [
[
732,
758
],
[
877,
919
]
] |
2019MNRAS.485.3288I__Tsao,_Silberberg_&_Barghouty_1998_Instance_1 | Coming back to the flux values given in Table 1, it is tempting to explain the deficiency of the measured fluxes at energies ∼68 and ∼78 keV compared to the fluxes measured at 1.157 MeV as a consequence of an additional component of the flux at 1.157 MeV, which is generated by the interaction of low-energy cosmic rays ... | [
"Tsao, Silberberg & Barghouty 1998"
] | [
"However, considering that little or nothing is known about the LECR fluxes in the Cas A SNR and uncertainties in the generally small cross-sections for the relevant reactions to produce either ${}^{44}_{}\\mathrm{Ti}$ or excited ${}^{44}_{}\\mathrm{Ca}^{*}$",
"the validity of such an interpretation of the discr... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
850,
883
]
] | [
[
557,
813
],
[
886,
1098
]
] |
2015AandA...577A..43S__Odstrčil_&_Karlický_(1997)_Instance_1 | The initialization of solar flares remains an unsolved problem. Early ideas on how the initialization might occur were described by Norman & Smith (1978). They argued that flare process cannot start in the entire flare volume at one instant, and proposed that the flare onset was localized in a small part of an active r... | [
"Odstrčil & Karlický (1997)"
] | [
"These triggering processes were numerically studied by Karlický & Jungwirth (1989) and"
] | [
"Background"
] | [
[
869,
895
]
] | [
[
782,
868
]
] |
2019MNRAS.482.3656R__Kashi_&_Soker_2011_Instance_1 | Several evolutionary channels have been proposed that lead to a SNIa explosion. For a comprehensive review, see Livio & Mazzali (2018) and Wang (2018). Among these, the two classical scenarios are the single- and the double-degenerate channels. In the single-degenerate channel a white dwarf (WD) in a binary system accr... | [
"Kashi & Soker 2011"
] | [
"Additional evolutionary channels for SNIa include",
"the core-degenerate channel"
] | [
"Background",
"Background"
] | [
[
1037,
1055
]
] | [
[
754,
803
],
[
965,
992
]
] |
2020MNRAS.497.4231R__Brown,_Vasil_&_Zweibel_2012_Instance_1 | Application of linear theory to investigate IGWs has been done extensively in the field of oceanography (Sutherland 2010). The general idea is to linearize hydrodynamical equations and introduce a wave-like ansatz to solve the linearized equations. In the context of stellar parameters, one of the earliest works was don... | [
"Brown, Vasil & Zweibel 2012"
] | [
"We ignore the pressure term in equation (4), which leads to a set of equations that conserve energy"
] | [
"Uses"
] | [
[
1049,
1076
]
] | [
[
948,
1047
]
] |
2019ApJ...886...14F__Urquhart_et_al._2014_Instance_1 | Figure 6(a) shows the 1.3 mm continuum and C18O(J = 2–1) distribution around the Papillon Nebula. The extended 1.3 mm continuum emission around the Papillon Nebula YSO roughly agrees with the distribution of Hα emission and has no counterparts of molecular gas, indicating that the continuum emission seems to be dominat... | [
"Urquhart et al. 2014"
] | [
"The peak column densities and total masses of both sources deduced from the 1.3 mm continuum emission are ∼1 × 1024 cm−2, and ∼2 × 102 M⊙, respectively, with an assumption",
"and a uniform dust temperature of 20 K, which is typically adapted/estimated for galactic high-mass star-forming dust clumps (e.g.,"
] | [
"Uses",
"Uses"
] | [
[
1325,
1345
]
] | [
[
839,
1010
],
[
1193,
1324
]
] |
2017ApJ...850...97B__Tamburro_et_al._2009_Instance_2 | The H i mass fraction of every gas particle in the baryonic runs is calculated based on the particle’s temperature and density and the cosmic UV background radiation flux while including a prescription for self-shielding of H2 and dust shielding in both H i and H2 (Christensen et al. 2012). This allows for the straight... | [
"Tamburro et al. 2009"
] | [
"Dispersions are thought to be driven at least partially by thermal velocities or supernovae"
] | [
"Compare/Contrast"
] | [
[
1100,
1120
]
] | [
[
1007,
1098
]
] |
2015ApJ...801...88S__Liu_et_al._2008_Instance_1 | There are several different effects that have been considered to explain the observed offset in the [O iii]λ5007/Hβ vs. [N ii]λ6584/Hα BPT diagram among high-redshift galaxies. First, there are the physical parameters describing the H ii regions contributing to the integrated line ratios from galaxies. These include th... | [
"Liu et al. 2008"
] | [
"Early work highlighting the issue of the high-redshift offset in the [O iii]λ5007/Hβ vs. [N ii]λ6584/Hα BPT diagram focused on these parameters (e.g.,"
] | [
"Background"
] | [
[
631,
646
]
] | [
[
435,
585
]
] |
2022MNRAS.510.3479B__Perucho_et_al._2010_Instance_1 | Our simulations, despite probing quite different jet velocities and resolution levels, point to a very unstable nature of the structure resulting from the jet–wind–orbit interaction in HMMQ. Although this was already suggested, our numerical calculations strongly endorse this possibility. Our results, not being an exte... | [
"Perucho et al. 2010"
] | [
"In fact, the jet–wind interaction alone can already perturb the jet"
] | [
"Background"
] | [
[
1208,
1227
]
] | [
[
1111,
1178
]
] |
2016AandA...589A.132B__Sarangi_&_Cherchneff_2013_Instance_1 | Extensive modelling efforts have been undertaken to explain observations and the formation of dust in local and high redshift SNe. While some studies use the classical nucleation theory (CNT) to describe dust formation under equilibrium conditions in shocked environments (Kozasa et al. 1989; Todini & Ferrara 2001; Noza... | [
"Sarangi & Cherchneff 2013"
] | [
"other studies describe the formation of both molecules and dust clusters from the shocked gas by assuming a chemical kinetic approach under non-equilibrium conditions and the subsequent coalescence and coagulation of these clusters to form dust grains"
] | [
"Background"
] | [
[
668,
693
]
] | [
[
360,
611
]
] |
2018ApJ...866...48U__Plagge_et_al._2013_Instance_1 | RX J1347.5–1145 is one of the most luminous X-ray galaxy clusters and is located at a redshift of z = 0.451. It was thought to be a relaxed cluster when it was discovered in the ROSAT all sky survey (Schindler et al. 1997). Komatsu et al. (1999) made the first measurements of the Sunyaev–Zel’dovich effect (SZE: Sunyaev... | [
"Plagge et al. 2013"
] | [
"The presence of the substructure has been confirmed by Chandra and XMM-Newton",
"as well as by more recent SZE measurements"
] | [
"Background",
"Background"
] | [
[
915,
933
]
] | [
[
703,
780
],
[
831,
873
]
] |
2021ApJ...912..106Y__Minchev_et_al._2013_Instance_1 | Our analysis on the LAMOST-RC stars by dissecting the MAPs shows that the chemical bimodality is observed throughout the Galactic disk, and the high- and low-[α/Fe] sequences are corresponding to the thick and thin disks of the Milky Way, respectively. How to explain the formation mechanism of the stellar thin and thic... | [
"Minchev et al. 2013"
] | [
"Our flared vertical profiles for the thin and thick disks",
"and are consistent with the number simulations of the chemodynamical evolution in Galactic disks formed in the cosmological context"
] | [
"Similarities",
"Similarities"
] | [
[
789,
808
]
] | [
[
486,
543
],
[
656,
787
]
] |
2020AandA...640A.121G__Nakajima_1983_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... | [
"Nakajima 1983"
] | [
"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"
] | [
[
719,
732
]
] | [
[
463,
653
]
] |
2018AandA...617A.116L__Hendecourt_&_Allamandola_(1986)_Instance_1 | Information about the composition and structure of astrophysical ices, and in particular the presence of solid methanol, is obtained by comparing astrophysical observations in the infrared to laboratory data (Dartois et al. 1999; Pontoppidan et al. 2003; Boogert et al. 2008; Bottinelli et al. 2010). The main infrared a... | [
"d’Hendecourt & Allamandola (1986)"
] | [
"The laboratory data most widely used for comparison to observations are those provided by",
"The first reference gives IR spectra and band strengths of methanol ice at 10 K in the 2.5–20 μm range."
] | [
"Uses",
"Uses"
] | [
[
640,
673
]
] | [
[
550,
639
],
[
725,
828
]
] |
2019AandA...622A.106M__Lanz_et_al._(2010)_Instance_1 | The standard single-frequency detection methods for point sources in the CMB and far IR are based on wavelet techniques (Vielva et al. 2003; Barnard et al. 2004; González-Nuevo et al. 2006) or on the matched filter (or MF hereafter, Tegmark & de Oliveira-Costa 1998; Herranz et al. 2002; Barreiro et al. 2003; López-Cani... | [
"Lanz et al. 2010"
] | [
"However, over the last few years a number of multifrequency compact source detection techniques have been proposed in the literature"
] | [
"Background"
] | [
[
1867,
1883
]
] | [
[
1691,
1823
]
] |
2020ApJ...901...21B__Cane_2000_Instance_1 | In general, the most important effect of the ICME passage in generating major FDs is ascribable to the energetic interplanetary shock/sheath region, although it has been proposed that the MC effect could even be dominant (e.g., Sanderson et al. 1990). Intense shocks are associated with the fast ICME propagation and may... | [
"Cane 2000"
] | [
"A statistical study was performed by Richardson & Cane (2011) on more than 300 ICMEs, showing that 80% of them is associated with an FD, detected by the anticoincidence guard data on the International Monitoring Platform (IMP-8;",
"and that the minimum GCR intensities occur within the MC."
] | [
"Background",
"Background"
] | [
[
1219,
1228
]
] | [
[
990,
1218
],
[
1231,
1288
]
] |
2021ApJ...915...86A__Troja_et_al._2017_Instance_1 | In addition to confirming the origin of some short GRBs, combining data from observations of GW170817 and GRB 170817A allowed for the inference of basic properties of short GRB jets. These include the isotropic equivalent luminosity of the jet, determined through a redshift measurement made possible by the optical foll... | [
"Troja et al. 2017"
] | [
"Indeed, the scientific debate about the emission profile of the jet and the subsequent gamma-ray production mechanism of GRB 170817A is still ongoing"
] | [
"Motivation"
] | [
[
932,
949
]
] | [
[
714,
863
]
] |
2021ApJ...912..163B__Davis_et_al._2018_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... | [
"Davis et al. 2018"
] | [
"For the refractory and main component elements in CC chondrites, we examine the elemental and isotopic compositions of Ti and Cr, respectively, because these are lithophile elements whose isotopic compositions have been measured precisely for a large number of chondrites and their components"
] | [
"Motivation"
] | [
[
1540,
1557
]
] | [
[
1137,
1429
]
] |
2022MNRAS.509.3427D__Díaz_et_al._2017_Instance_1 | Unlike BH–BH mergers, binary neutron star (BNS) merger mechanisms are expected to yield an optical counterparts powered by the radioactive decay of rapid neutron capture process (r-process) elements synthesized in the merger ejecta (Li & Paczyński 1998; Metzger et al. 2010) or by the cooling of shock-heated material ar... | [
"Díaz et al. 2017"
] | [
"GRB 170817A was followed by the discovery of the optical counterpart Swope Supernova Survey 17a [SSS17a (AT 2017gfo)] ∼11 h later in the galaxy NGC 4993",
"and later confirmed by others teams"
] | [
"Background",
"Background"
] | [
[
895,
911
]
] | [
[
622,
774
],
[
797,
832
]
] |
2016AandA...595A..16T__Eggleton_et_al._(2006)_Instance_1 | We used the theoretical models by Eggleton et al. (2008), Charbonnel & Lagarde (2010), and Lagarde et al. (2012) for the comparison. They provide quantitative values representing the first dredge-up, thermohaline (TH), and thermohaline and rotation (TH+V) induced mixing. Eggleton et al. (2008) estimated the mixing spee... | [
"Eggleton et al. (2006)"
] | [
"The model of Charbonnel & Lagarde (2010) of thermohaline instability induced mixing and the model by Eggleton et al. (2008) are both based on the ideas of"
] | [
"Background"
] | [
[
886,
908
]
] | [
[
731,
885
]
] |
2018AandA...614A..72V__Bocquet_et_al._2015_Instance_1 | Cluster cosmology requires jointly modelling the physical parameters describing the evolution of the intra-cluster medium (ICM) alongwith the impact of selection procedure. While the first self-consistent methods have followed a backward modelling of the recovered cosmology-dependent, mass function (e.g. Vikhlinin et a... | [
"Bocquet et al. 2015"
] | [
"Cluster number counts from Sunyaev-Z’eldovich surveys are routinely modelled in terms of the signal-to-noise ratio (S/N) or the Compton parameter of the detections, which can be related to the cluster mass via scaling relations from X-ray, lensing, or velocities (e.g."
] | [
"Background"
] | [
[
844,
863
]
] | [
[
505,
773
]
] |
2022AandA...661A..71H__Liu_et_al._2020_Instance_1 | While using the Padé(2,1) approximation, we checked the influence of the quasar relation on the cosmological constraints. We first provide the constraints considering a free quasar relation. Then combining that with the following two special cases, the effect of the slope parameter γ is studied. One case is the fitting... | [
"Liu et al. 2020"
] | [
"This result is consistent with previous research within a 1σ error",
"Here, it is worth noting that the 1σ errors of the γ best fit from previous research are both larger than 0.01."
] | [
"Similarities",
"Differences"
] | [
[
1018,
1033
]
] | [
[
862,
928
],
[
1054,
1165
]
] |
2021MNRAS.507.2766S__Sumiyoshi_et_al._2005_Instance_2 | In order to make a linear analysis, first we have to prepare the PNS models as a background. The PNS properties depend on not only the density and pressure profiles but also the distributions of temperature (or entropy per baryon) and electron fraction inside the PNS, while such profiles can be determined only via the ... | [
"Sumiyoshi et al. 2005"
] | [
"For the collision term associated with neutrino emission, absorption, and scattering with leptons, nucleons, and nuclei handles, the basic neutrino reactions are adopted"
] | [
"Uses"
] | [
[
1312,
1333
]
] | [
[
1128,
1297
]
] |
2020AandA...641A.126B__Jones_&_Hardee_1979_Instance_1 | Many low-luminosity active galactic nuclei (LLAGN) display prominent jets and compact cores that are sources of highly nonthermal continuum radio emission (see, e.g., Heeschen 1970; Wrobel & Heeschen 1991). The observational signatures of the compact cores have been reproduced using models that produce self-absorbed sy... | [
"Jones & Hardee 1979"
] | [
"In the optically thin limit, the emission is significantly polarized",
"an effect that has been observed in higher-luminosity AGN sources"
] | [
"Background",
"Similarities"
] | [
[
728,
747
]
] | [
[
658,
726
],
[
750,
815
]
] |
2022MNRAS.513.4464T__Hopkins_et_al._2020_Instance_1 |
Galactic winds: Galactic winds driven by CRs have often been simulated in two limits: a diffusion-dominated regime, due possibly to ‘extrinsic confinement’, where CRs are scattered by extrinsic turbulence, and/or due to various wave damping mechanisms (e.g. ion neutral damping) and streaming-dominated ‘self confinemen... | [
"Hopkins et al. 2020"
] | [
"It is also much better at driving winds, because the CRs do not suffer strong energy losses via Alfven wave heating"
] | [
"Uses"
] | [
[
849,
868
]
] | [
[
711,
826
]
] |
2016ApJ...821..107G__Schwadron_et_al._2011_Instance_1 | We repeated the plasma pressure calculation presented by Schwadron et al. (2011) and Fuselier et al. (2012) for the new ENA energy spectrum. The results for the downwind hemisphere and for the Voyager 1 region are summarized in Table 3. The measured intensity
j
ENA
of neutralized hydrogen at a given energ... | [
"Schwadron et al. (2011)"
] | [
"We repeated the plasma pressure calculation presented by",
"and Fuselier et al. (2012) for the new ENA energy spectrum."
] | [
"Uses",
"Uses"
] | [
[
57,
80
]
] | [
[
0,
56
],
[
81,
140
]
] |
2018ApJ...859..115W__Luo_et_al._2016_Instance_1 | We futher examine the distributions of the radial number fraction of satellites with different colors in different LSE in Figure 5 to study the role central galaxies play in SCA. It can be seen, in general, that the intersections of these lines for each subsample are located between
to
, and with a mean va... | [
"Luo et al. 2016"
] | [
"Such evolutionary behavior is consistent with “strangulation” wherein cold gas that could be used for star formation is depleted as satellites are accreted (e.g.,"
] | [
"Similarities"
] | [
[
685,
700
]
] | [
[
481,
643
]
] |
2019MNRAS.489.4429R__Lada_et_al._2008_Instance_1 | In the currently accepted model of star formation, most stars form in families of star clusters within giant molecular clouds (GMCs). However, clusters and their families can be quite diverse, and there is no consensus yet on a general model for cluster formation. An additional complication is that once stars are born,... | [
"Lada et al. 2008"
] | [
"The Pipe Nebula,",
"has played a workhorse role in a number of previous studies (e.g.",
"Many of these works have the common goal of determining how GMCs are organized in the stages that precede their collapse and the consequent conversion of gas into stars."
] | [
"Background",
"Background",
"Background"
] | [
[
914,
930
]
] | [
[
574,
590
],
[
770,
835
],
[
1079,
1248
]
] |
2021ApJ...916...70Z__Millon_et_al._2020_Instance_1 | For the uncertainty from the Fermat potential, which is determined by lens modeling, source host galaxies without dazzling AGNs are conducive to the reconstruction of the mass distribution of the lens galaxies in lensed FRB systems. Simulations show that the Fermat potential component contributes approximately ∼0.8% un... | [
"Millon et al. 2020"
] | [
"For instance, the TDCOSMO collaboration",
"has achieved ∼2% in the inference of H0 from time-delay cosmography under the assumption that the radial-mass distribution of the lens can be described by a power-law mass profile or a composite of a dark-matter halo",
"and baryon matter."
] | [
"Background",
"Background",
"Background"
] | [
[
1041,
1059
]
] | [
[
1000,
1039
],
[
1061,
1277
],
[
1300,
1318
]
] |
2017AandA...602A..26L__Robrade_&_Schmitt_2005_Instance_1 | Along with the flare related changes, we also examine possible orbital variations by dividing the overall quiescent spectra in periods dubbed as “Quiet 1” and “Quiet 2” (the time bins for the spectra are as shown in Fig. 1) and model the pn, MOS and RGS X-ray spectra. We specifically determine the temperatures, emissio... | [
"Robrade & Schmitt 2005"
] | [
"As is often observed",
", we require multi-temperature components to achieve an adequate description of the observed coronal spectra."
] | [
"Similarities",
"Similarities"
] | [
[
607,
629
]
] | [
[
566,
586
],
[
651,
760
]
] |
2021MNRAS.504.3316B__than_2000_Instance_5 | WASP-43b is the most heavily scrutinized phase curve, with four analyses of this data set already published (Stevenson et al. 2017; Mendonça et al. 2018; Morello et al. 2019; May & Stevenson 2020). Our phase curve semi-amplitude, eclipse depth, and radius are consistent with all of these works. The more contentious iss... | [
"Stevenson et al. (2017)"
] | [
"May & Stevenson (2020) claimed that the differences between the retrieved phase offsets is the result of temporal binning which was not used by",
"and May & Stevenson (2020) but was used by Mendonça et al. (2018), Morello et al. (2019), and this work."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
963,
986
]
] | [
[
819,
962
],
[
987,
1091
]
] |
2018MNRAS.478.4986K__Greig_&_Mesinger_2017_Instance_1 | Various observational techniques, such as measuring the Gunn–Peterson optical depth from QSO spectra or the prevalence of Ly α emission in high-redshift galaxies, have placed very tight constraints on the volume filling fraction of neutral hydrogen in the intergalactic medium (IGM) towards the end of reionization at z∼... | [
"Greig & Mesinger 2017"
] | [
"Various observational techniques, such as measuring the Gunn–Peterson optical depth from QSO spectra or the prevalence of Ly α emission in high-redshift galaxies, have placed very tight constraints on the volume filling fraction of neutral hydrogen in the intergalactic medium (IGM) towards the end of reionization ... | [
"Background"
] | [
[
829,
850
]
] | [
[
0,
322
]
] |
2021AandA...649A.126T__Luck_(2018b)_Instance_1 | Studies of the radial n-capture-to-iron abundance gradients are very scarce so far. We can only search for a broad agreement of our results with several studies of abundance gradients with galactocentric distances (Rgc). da Silva et al. (2016) studied n-capture elements across the Galactic thin disc based on Cepheid va... | [
"Luck (2018b)"
] | [
"More recently,",
"also investigated the gradients of n-capture element abundance-to-iron ratios with respect to Rgc for a sample of 435 Cepheids."
] | [
"Background",
"Background"
] | [
[
1020,
1032
]
] | [
[
1005,
1019
],
[
1033,
1160
]
] |
2015MNRAS.451.2544P__Leitet_et_al._2011_Instance_1 | Observations are now probing galaxies in the middle of the reionization epoch, when the gas in the intergalactic medium was transformed from its initially neutral state into a hot, ionized plasma (e.g. McLure et al. 2011; Finkelstein et al. 2012; Bouwens et al. 2014). Most likely stars in galaxies are responsible for t... | [
"Leitet et al. 2011"
] | [
"Except for two objects",
"in the local Universe no ionizing radiation has been detected directly",
"although some objects show indirect evidence of photon leakage"
] | [
"Background",
"Background",
"Background"
] | [
[
1124,
1142
]
] | [
[
1100,
1122
],
[
1151,
1221
],
[
1270,
1332
]
] |
2019MNRAS.482.5651M__Schweizer_&_Middleditch_1980_Instance_1 | Therefore, the kinetics characteristics of the star could be the only piece to judge whether or not the SM star is the surviving companion of SN 1006. If its space velocity is significantly different from the other stars in the remnant of SN 1006, the probability to be the surviving companion would become high. Otherwi... | [
"Schweizer & Middleditch 1980"
] | [
"From the figure, it seems that there is not difference between the SM star and other stars in the remnant of SN 1006 in the aspect of proper motion, i.e. the proper motion of the SM star only slightly deviates from the median value of the proper motions of the stars at the direction of the SNR centre of SN 1006, a... | [
"Similarities"
] | [
[
868,
896
]
] | [
[
467,
866
]
] |
2022AandA...666A.134S__Rodríguez-Almeida_et_al._2021b_Instance_1 | A more puzzling task was the resolution of the fine and hyperfine structure. First, the A–E split structure attributed to the methyl internal rotation motion can be generally used as a molecular “fingerprint” to search for a molecule in an astronomical line survey (Cernicharo et al. 2016; Belloche et al. 2017). Moreove... | [
"Rodríguez-Almeida et al. 2021b"
] | [
"As an example, the analysis of the hyperfine structure of several N-bearing species, such as N-protonated isocyanic acid (H2NCO+,",
") which has been detected toward G+0693-0.027",
"was required for its conclusive line-by-line identification."
] | [
"Background",
"Background",
"Background"
] | [
[
776,
806
]
] | [
[
646,
775
],
[
806,
851
],
[
915,
975
]
] |
2021ApJ...912...92F__Feng_et_al._2021_Instance_1 | The sudden brightening of NGC 2617 provides a good opportunity to investigate the properties of CL-AGNs. In general, the CL processes can be interpreted as changes in obscuration or accretion rate. The obscuration model can be well applied to some X-ray selected CL-AGNs (e.g., Bianchi et al. 2005). The crossing time fo... | [
"Feng et al. 2021"
] | [
"The observational constraints of rdt and rdt/rBLR are discussed in estimating tcross for the double-peaked BEL CL-AGN NGC 3516, where rdt is a dust torus radius"
] | [
"Uses"
] | [
[
939,
955
]
] | [
[
777,
937
]
] |
2021MNRAS.506.3330W__Gronow_et_al._2020_Instance_1 | The majority of observational evidence based on studies of SN Ia populations thus points towards a DD scenario for most, if not all, SNe Ia. However, finding self-consistent progenitor and explosion models that recreate the observed luminosity function as well as correlations between luminosity, light-curve parameters,... | [
"Gronow et al. 2020"
] | [
"In recent years, attention directed towards explosions of sub-MCh WDs triggered by double detonations (primarily related to a DD scenario) has led to promising results (e.g."
] | [
"Background"
] | [
[
966,
984
]
] | [
[
725,
898
]
] |
2021AandA...653A.129C__Coutens_et_al._(2016)_Instance_1 | Figure 15 shows the comparison between pairs of molecular abundances, HC(O)NH2 and HNCO, CH3NCO and HNCO, and CH3NCO and HC(O)NH2. It is already known from previous observations that there is a correlation between HNCO and HC(O)NH2 (López-Sepulcre et al. 2015, 2019; Allen et al. 2020). In the top-left panel of Fig. 15 ... | [
"Coutens et al. (2016)"
] | [
"found that the deuteration (D/H ratio) of HC(O)NH2 in IRAS 16293 B is similar to that of HNCO, in agreement with the hypothesis that both species are chemically related via grain-surface reactions."
] | [
"Background"
] | [
[
1816,
1837
]
] | [
[
1838,
2035
]
] |
2019ApJ...875...68A__Clemens_&_Alexander_2002_Instance_1 | Associations between ULXs and star clusters have also been studied in interacting galaxies. The latter are known to host a higher average number (>5) of ULXs. Therefore, they are good candidates in which to examine the properties of the population of ULXs. Poutanen et al. (2013) extensively examined the significant ass... | [
"Clemens & Alexander 2002"
] | [
"Also, NGC 4490 has a giant H i envelope that probably originated from the star formation"
] | [
"Background"
] | [
[
1199,
1223
]
] | [
[
1109,
1197
]
] |
2019AandA...628A.110M__Kryukova_et_al._(2012)_Instance_1 | Deriving the completeness limits of the WISE photometry is mandatory to assess the reliability of our catalogue of starless cores. We examined the histograms of the number of mid-infrared (MIR) sources versus magnitude; taking into account the effects of the cuts required to fulfil the criteria of Koenig et al. (2012),... | [
"Kryukova et al. (2012)"
] | [
"Alternatively, one can compute the bolometric luminosity following"
] | [
"Uses"
] | [
[
1171,
1193
]
] | [
[
1104,
1170
]
] |
2021AandA...647A.186S__Shebalin_et_al._1983_Instance_1 | Chandrasekhar & Fermi (1953) assumed that “turbulent motions are isotropic”, and they adopted
$f\,{=}\,1/\sqrt{3}$f = 1/3
. If the field strength is weak, turbulent motions will drag the field lines in random directions and turbulence will be isotropic (super-Alfvénic turbulence). However, there is overwhelming obser... | [
"Shebalin et al. 1983"
] | [
"However, there is overwhelming observational evidence that magnetic fields in the ISM have well-defined directions, indicating that turbulence is sub, trans-Alfvénic and hence turbulent properties are highly anisotropic"
] | [
"Background"
] | [
[
549,
569
]
] | [
[
284,
503
]
] |
2021AandA...650A.155Z__Oh_et_al._2012_Instance_3 | Many factors can affect the prevalence of AGN activity. One important question is how gas is brought down to the galaxy center to fuel supermassive black holes (SMBHs). In the literature, two kinds of mechanisms are proposed. One is the internal secular evolution process. The torque induced by non-axisymmetric galactic... | [
"Oh et al. 2012"
] | [
"However, the question of whether galactic bars can significantly affect AGN activity is still under debate"
] | [
"Background"
] | [
[
903,
917
]
] | [
[
756,
862
]
] |
2015ApJ...811..129B__Pasachoff_et_al._2009_Instance_1 | An alternative possibility to coronal heating is that the release and dissipation of magnetic energy actually takes place in the chromosphere. In this scenario, the chromospheric plasma is directly heated to coronal temperatures, rather than by thermal conduction fronts that are driven into the lower atmosphere as a co... | [
"Pasachoff et al. 2009"
] | [
"N. E. Raouafi et al. (2015, in preparation) have argued that type II spicules have much more in common with so-called “classical” spicules",
"than do type I spicules. In particular, type II and classical spicules are both commonly observed in quiet Sun and coronal hole regions, whereas type I spicules appear to ... | [
"Similarities",
"Similarities"
] | [
[
772,
793
]
] | [
[
612,
750
],
[
795,
1008
]
] |
2019MNRAS.488.1728N__Kaiser_et_al._1995_Instance_1 | The mass estimate for each cluster was obtained by fitting a reduced tangential shear profile predicted by a projected Navarro–Frenk–White (NFW) profile (e.g. Bartelmann 1996) to the observed ellipticities. We derive the best-fitting profile parameters R200 and c200 by minimizing the merit function
(4)
\begin{eqnarra... | [
"Kaiser et al. 1995"
] | [
"The factor 1.08 is the multiplicative shear calibration bias of the used KSB+ pipeline",
"to convert from measured to true ellipticity."
] | [
"Uses",
"Uses"
] | [
[
886,
904
]
] | [
[
798,
884
],
[
925,
970
]
] |
2018AandA...618L...3M__Greaves_&_Rice_(2010)_Instance_1 | One way to explain the observations is to postulate that the cores of planets are formed in the very first Myr of the protoplanetary disk evolution, or even in the embedded phase while the disk is still forming. The disks for which masses have been measured have ages >1 Myr, and a general trend of declining disk mass w... | [
"Greaves & Rice (2010)"
] | [
"Thus, it is possible that disks were massive enough to form the cores of planets at younger ages. This idea has been suggested by",
"Williams (2012), and Najita & Kenyon (2014), among others. In this scenario, the vast majority of the material composing planets must already be in the form of planetesimals, for r... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
525,
546
]
] | [
[
395,
524
],
[
548,
888
]
] |
2021MNRAS.507.5882S__Mackereth_et_al._2018_Instance_1 | Cosmological hydro dynamical N-body simulations offer another possibility to investigate the origin of the bimodality in the ([Fe/H], [α/Fe]) plane. Earlier simulations, e.g. full N-body simulations by Loebman et al. (2011), Brook et al. (2012) or hybrid simulations in which a semi-analytic chemical evolution was added... | [
"Mackereth et al. 2018"
] | [
"The bimodality has now been observed in some simulations"
] | [
"Similarities"
] | [
[
983,
1004
]
] | [
[
906,
962
]
] |
2020MNRAS.498.5116I__Andrews_et_al._2012_Instance_1 | It is now largely understood that the dust-to-gas mass ratio ϵ in protoplanetary discs is unlikely to match the canonical value in the interstellar medium of 0.01 (Mathis, Rumpl & Nordsieck 1977). For example, recent observations of CO isotopologues and dust continuum emission have found disc-averaged ϵ values to be mu... | [
"Andrews et al. 2012"
] | [
"There is also an observed discrepancy between the radial extents of the gas and dust components of protoplanetary discs, with dust discs being significantly more compact"
] | [
"Background"
] | [
[
664,
683
]
] | [
[
493,
662
]
] |
2018ApJ...858...13H___2009b_Instance_1 | It is widely accepted that an SN Ia is a thermonuclear explosion resulting from a binary system, of which one star is necessarily a degenerate carbon-oxygen (
) white dwarf (WD) (Hoyle & Fowler 1960) near the Chandrasekhar mass (
). Current research considers various progenitor configurations and final outcom... | [
"Wang et al.",
"2009b"
] | [
"This process can end up as a SN Ia, a highly magnetized WD (MWD), or an accretion-induced collapse"
] | [
"Background"
] | [
[
992,
1003
],
[
1011,
1016
]
] | [
[
744,
842
]
] |
2018ApJ...853...34Z__Giebels_et_al._2007_Instance_2 | Several well-studied TeV blazars show rich spectral behavior in X-rays, which may represent the general behavior of the synchrotron peak of all AGN jets. The X-ray spectra are usually curved (Massaro et al. 2004) and can only locally be fitted by a power law. The spectral variation with flux can be complex (Zhang et al... | [
"Giebels et al. 2007"
] | [
"The synchrotron peak usually moves to higher frequencies with increasing flux during outbursts",
"but no correlation between the break energy and the flux exists when a broken power law is adopted to fit the X-ray spectra"
] | [
"Background",
"Background"
] | [
[
814,
833
]
] | [
[
552,
646
],
[
673,
796
]
] |
2022AandARv..30....6M__Magliocchetti_et_al._2018b_Instance_2 | AGN While—starting from the very early works (e.g., Seldner and Peebles 1978; Longair and Seldner 1979; Hill and Lilly 1991; Peacock and Nicholson 1991; Allington-Smith et al. 1993; Zirbel 1997)—virtually all the studies presented in the literature converge at indicating that radio-AGN preferentially reside within over... | [
"Magliocchetti et al. 2018b"
] | [
"The reason for this discrepancy is not known, but it is likely related to the different redshift ranges probed by the two methods (much more local sources are considered in the second one), and/or—under the assumption of a strong correlation between radio luminosity and environmental density (e.g.,",
"but see fu... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1773,
1799
]
] | [
[
1451,
1750
],
[
1838,
1899
]
] |
2016ApJ...817...12P__Kleeorin_et_al._2000_Instance_1 | Large-scale magnetic fields with strength of the order of 1–10 μG have been observed in disk galaxies (e.g., Beck et al. 1996; Fletcher 2010; Beck 2012; Beck & Wielebinski 2013; Van Eck et al. 2015). The origin of these fields can be explained through mean-field dynamo theory (Ruzmaikin et al. 1988; Beck et al. 1996; B... | [
"Kleeorin et al. 2000",
"Kleeorin et al. 2000"
] | [
"To avoid catastrophic suppression of the dynamo action (α-quenching), the magnetic helicity due to the small-scale magnetic field should be removed from the system",
"Mechanisms suggested to produce these small-scale magnetic helicity fluxes are:",
"and through diffusive flux"
] | [
"Background",
"Background",
"Background"
] | [
[
946,
966
],
[
1432,
1452
]
] | [
[
752,
915
],
[
969,
1048
],
[
1404,
1430
]
] |
2020ApJ...896L..21R___2015_Instance_1 | Top left: the revised, CO(J = 1 → 0)-based Mgas from VLASPECS confirm that z = 2–3 galaxies detected in the ASPECS survey (green circles; tentative detections are marked with a plus sign) closely follow the “star formation law” (i.e., Mgas–SFR relation) at high redshift. CO-detected main-sequence galaxies at similar re... | [
"Sharon et al.",
"2015"
] | [
"Top right: the r31 brightness temperature ratio of VLASPECS galaxies (green circles) is similar to that of",
"and z > 2 dusty star-forming galaxies (DSFGs; blue squares; compilation from Sharon et al. 2016; including data from"
] | [
"Similarities",
"Similarities"
] | [
[
1291,
1304
],
[
1311,
1315
]
] | [
[
780,
886
],
[
1058,
1174
]
] |
2021MNRAS.502.5038N__Gosset_et_al._1994_Instance_1 | Several searches for high-frequency signals were performed in the past for WR stars, notably in the context of searches for compact companions (e.g. Marchenko et al. 1994). However, there were few cases of reported and confirmed periodicities. Focusing on our sample, the following detections were published. Blecha, Sch... | [
"Gosset et al. 1994"
] | [
"However, at the corresponding frequency of 138 d−1, the TESS high-cadence data (sector 10) show no signs of such a signal, confirming previous negative reports"
] | [
"Similarities"
] | [
[
603,
621
]
] | [
[
442,
601
]
] |
2018MNRAS.475.1160H__Werk_et_al._2013_Instance_1 | Galaxies are surrounded by vast gaseous haloes which extend well beyond the hosts’ stellar components: Early observations of quasar sight lines attributed the presence of absorption at multiple intermittent redshifts to gaseous haloes of intervening galaxies (e.g. Bergeron 1986; Bergeron & Boissé 1991; Lanzetta et al. ... | [
"Werk et al. 2013"
] | [
"The current model of the CGM suggests the presence of a clumpy multiphase medium which extends beyond the virial radius of the host galaxy, with a declining radial density profile, containing a substantial amount of gas and metals (e.g."
] | [
"Background"
] | [
[
1392,
1408
]
] | [
[
1155,
1391
]
] |
2015MNRAS.454..193B__Langhoff_et_al._1998_Instance_1 | Theoretical quantum chemical calculations help in narrowing down candidates for much more expensive laboratory experiments. Considering the high cost, time consumption and other constraints faced in laboratory, theoretical computational study can propose selected PAHs for which laboratory spectroscopy can most usefully... | [
"Langhoff et al. 1998"
] | [
"Density Functional Theory (DFT) has been used rigorously to calculate the harmonic frequencies and intensities of vibrational modes of PAHs in various forms including size, composition and charge states"
] | [
"Background"
] | [
[
610,
630
]
] | [
[
335,
537
]
] |
2015MNRAS.450.2404G__Fornasa_&_Sánchez-Conde_2015_Instance_1 | The extragalactic sky from any direction and at all frequencies is filled with radiation from discrete sources and from a diffuse (or unresolved) component known as the cosmic background. This pervasive radiation, discovered only in relatively recent times, is one of the most fundamental observables from the Universe, ... | [
"Fornasa & Sánchez-Conde 2015"
] | [
"The latest Fermi Large Area Telescope (Fermi-LAT) survey data are now providing strong evidence towards an origin mostly due to integrated radiation from blazars and radio galaxies (e.g."
] | [
"Background"
] | [
[
1096,
1124
]
] | [
[
877,
1063
]
] |
2017MNRAS.468.2590S__Fassnacht_et_al._2002_Instance_2 | We initiated the H0LiCOW (H0 Lenses in COSMOGRAIL's Wellspring) program with the aim of measuring the Hubble constant with better than 3.5 per cent precision and accuracy (in most background cosmological models), through a sample of five time-delay lenses. We obtain the key ingredients to each of the lenses through obs... | [
"Fassnacht et al. 2002"
] | [
"The unprecedented quality of the light curves combined with new curve-shifting algorithms",
"lead to time delays with typically ∼3 per cent accuracy"
] | [
"Uses",
"Uses"
] | [
[
996,
1017
]
] | [
[
817,
906
],
[
939,
994
]
] |
2017AandA...599A..13Y__Wimmer-Schweingruber_et_al._1997_Instance_1 | Figure 2 shows solar wind plasma and magnetic field measurements for a CIR that occurred between July 26 and 27, 2003 (days of year 207–208). Following Chotoo et al. (2000), Richardson et al. (1993), we marked four regions in the plot: the slow wind region (S), the compressed slow wind region (S′), the compressed fast ... | [
"Wimmer-Schweingruber et al. 1997"
] | [
"The stream interface (S′-F′) is indicated by the vertical line in Fig. 2 and is characterized by a drop of the O7+/O6+ abundance ratio measured with SWICS in the bulk solar wind"
] | [
"Uses"
] | [
[
712,
744
]
] | [
[
533,
710
]
] |
2019AandA...631A..88Y__Bohren_&_Huffman_(1998)_Instance_3 | Starting from the four aforementioned materials, we consider several composition mixtures and grain structures. For the sake of comparison, we first consider compact grains of purely a-Sil, a-C, or a-C:H. Subsequently, according to Köhler et al. (2015), we consider compact grains made of two thirds a-Sil and one third ... | [
"Bohren & Huffman (1998)"
] | [
"For grains surrounded by an ice mantle, the optical properties are derived with the core-mantle Mie theory using the BHCOAT routine given in"
] | [
"Uses"
] | [
[
3177,
3200
]
] | [
[
3036,
3176
]
] |
2021MNRAS.504.3316B__than_2000_Instance_2 | WASP-43b is the most heavily scrutinized phase curve, with four analyses of this data set already published (Stevenson et al. 2017; Mendonça et al. 2018; Morello et al. 2019; May & Stevenson 2020). Our phase curve semi-amplitude, eclipse depth, and radius are consistent with all of these works. The more contentious iss... | [
"Stevenson et al. (2017)"
] | [
"The more contentious issue is that of the phase curve’s phase offset and nightside temperature.",
"initially reported only a 2σ upper limit on the nightside temperature of 650 K, while all subsequent reanalyses (including ours) favour a significantly detectable nightside temperature of ∼800 K."
] | [
"Differences",
"Differences"
] | [
[
392,
415
]
] | [
[
296,
391
],
[
416,
611
]
] |
2022MNRAS.515.3299G__Tagawa_et_al._2020a_Instance_1 | In active galactic nuclei (AGNs), the gaseous accretion disc around the SMBH may facilitate binary formation and mergers of stellar-mass compact objects (McKernan et al. 2014; Bellovary et al. 2016; Bartos et al. 2017; Stone, Metzger & Haiman 2017; Tagawa, Haiman & Kocsis 2020a). In this scenario, BHs form in situ in t... | [
"Tagawa et al. 2020a"
] | [
"In this scenario, BHs form in situ in the vicinity of a GN and sink to the inner region due to mass segregation or they are delivered to these regions by infalling globular clusters",
"then get captured in the disc by hydrodynamic drag as they cross the disc (e.g."
] | [
"Background",
"Background"
] | [
[
759,
778
]
] | [
[
281,
462
],
[
607,
686
]
] |
2019ApJ...873...89M__Bourrier_et_al._2016_Instance_1 | Ultraviolet observations of the hot Jupiter HD 209458 b have found up to a 15% occultation in the wings of hydrogen Lyα, with effective Doppler shifts of up to ±150 km s−1, significantly larger than the 5% occultation observed at optical (Vidal-Madjar et al. 2003, 2008; Ben-Jaffel 2007; Ehrenreich et al. 2008). The hig... | [
"Bourrier et al. 2016"
] | [
"Similar outflows have been reported for",
"and for one hot Neptunian planet, GJ 435 b"
] | [
"Similarities",
"Similarities"
] | [
[
835,
855
]
] | [
[
463,
502
],
[
748,
790
]
] |
2016MNRAS.463.3637R__Mirabel,_Dottori_&_Lutz_1992_Instance_1 | In MS, the tidal tails host the formation of overdensities similar to TDGs (about 3 in each tail are visible in Fig. 3). Their associated phantom DM further favours their growth, while no such structure is visible in the stellar nor gaseous component of the NA model. The formation of TDGs in simulations is sensitive to... | [
"Mirabel, Dottori & Lutz 1992"
] | [
"Observations of the Antennae galaxies report only one TDG candidate, at the tip of the southern tail",
"but the exact nature of this structure is still questioned"
] | [
"Motivation",
"Motivation"
] | [
[
758,
786
]
] | [
[
656,
756
],
[
789,
847
]
] |
2015ApJ...805..115V__Robitaille_et_al._2006_Instance_1 | To classify the bursts in our models, we use the remaining mass in the envelope to define the boundary between the embedded and optically visible phases. Namely, we assume that the optically visible Class II begins when less than 10% of the initial core mass is left in the envelope. The boundary between the deeply embe... | [
"Robitaille et al. 2006"
] | [
"Our adopted classification scheme is based on physical properties of a young stellar object, such as envelope and disk masses (e.g.",
"rather than on observational signatures, such as submillimeter luminosities or effective temperatures"
] | [
"Uses",
"Differences"
] | [
[
592,
614
]
] | [
[
459,
590
],
[
643,
744
]
] |
2017MNRAS.464..183N__Iannuzzi_&_Dolag_2012_Instance_1 | Other important result we reported in Section 3.3 is the reversing behaviour of red and blue galaxies with respect to velocity and groupcentric distances segregation, with redshift. Regarding velocity segregation, the preceding paragraph provides a qualitative scenario. Now, to explain the spatial segregation, we shoul... | [
"Iannuzzi & Dolag 2012"
] | [
"Thus, both survival and replenishment of galaxies should be expected over the time, and two important factors come into play: (i) the accretion rate of galaxies; and (ii) the orbital dependence of galaxy properties (e.g."
] | [
"Uses"
] | [
[
854,
875
]
] | [
[
609,
829
]
] |
2015ApJ...807...91C__Moffat_1969_Instance_1 | The standard photometric analysis (see Dalessandro et al. 2008a, 2008b) has been performed on the “flc” images, which are corrected for flat field, bias, dark counts, and charge transfer efficiency. These images have been further corrected for “Pixel-Area-Map”10
10
For more details see the ACS Data Handbook.
with sta... | [
"Moffat 1969"
] | [
"The model has been chosen on the basis of a χ2 test and, in every image, the best fit is provided by a Moffat function"
] | [
"Uses"
] | [
[
709,
720
]
] | [
[
589,
707
]
] |
2018ApJ...864...51W__Lee_et_al._2014_Instance_1 | Understanding how, when, and where galaxies quench their star formation is one of the most muddled, outstanding problems in galaxy formation. Different models for galaxy formation and evolution often make very different assumptions and/or predictions. Among them, semi-analytic galaxy formation models (SAMs; e.g., White... | [
"Lee et al. 2014"
] | [
"Different models for galaxy formation and evolution often make very different assumptions and/or predictions. Among them, semi-analytic galaxy formation models (SAMs; e.g.,",
"are two powerful tools to trace galaxy formation and evolution in cosmological volumes. SAMs are phenomenological models that use an appr... | [
"Background",
"Background"
] | [
[
521,
536
]
] | [
[
142,
314
],
[
807,
1177
]
] |
2020MNRAS.493.2373D__Haghi_&_Amiri_2016_Instance_1 | The lack of detection of supersymmetric particles at Large Hadron Collider led alternative candidates for dark matter to rapidly gaining attention. Apart from other particles, modifications of the gravitational action also offer a new avenue to account for the dark matter. Among many theories, MOG has been successfully... | [
"Haghi & Amiri 2016"
] | [
"Nevertheless, a recent study of the dynamics of dwarf spheroidals orbiting around the Milky Way has shown some inconsistencies with previous results"
] | [
"Differences"
] | [
[
909,
927
]
] | [
[
759,
907
]
] |
2015MNRAS.451.2544P__Mesinger,_Furlanetto_&_Cen_2011_Instance_1 | Observations are now probing galaxies in the middle of the reionization epoch, when the gas in the intergalactic medium was transformed from its initially neutral state into a hot, ionized plasma (e.g. McLure et al. 2011; Finkelstein et al. 2012; Bouwens et al. 2014). Most likely stars in galaxies are responsible for t... | [
"Mesinger, Furlanetto & Cen 2011"
] | [
"The escape fraction is a key parameter in studies of the contribution of the observed galaxy population to reionization",
"semi-analytic modelling of reionization (e.g."
] | [
"Background",
"Background"
] | [
[
810,
841
]
] | [
[
508,
627
],
[
679,
724
]
] |
2021MNRAS.500.1817L__Abbott_et_al._2020b_Instance_1 | Since the errors of the LIGO-estimated rates are dominated by Poisson statistics (Abbott et al. 2020a,b), we approximate the PDF for the expected number of detections $\mathcal {N}=\mathcal {R}VT$ (from the surveyed space–time volume VT) by $\mathrm{d}P/\mathrm{d}\mathcal {N}\propto \mathcal {N}^{k-1/2}\mathrm{e}^{-\ma... | [
"Abbott et al. 2020",
"b"
] | [
"Since the errors of the LIGO-estimated rates are dominated by Poisson statistics",
"we approximate the PDF for the expected number of detections $\\mathcal {N}=\\mathcal {R}VT$ (from the surveyed space–time volume VT) by $\\mathrm{d}P/\\mathrm{d}\\mathcal {N}\\propto \\mathcal {N}^{k-1/2}\\mathrm{e}^{-\\mathcal ... | [
"Uses",
"Uses"
] | [
[
82,
100
],
[
102,
103
]
] | [
[
0,
80
],
[
106,
523
]
] |
2016AandA...591A..91P__Halpern_et_al._2014_Instance_2 | MSH 11-61A (also known as G290.1-0.8) is a mixed morphology SNR detected from radio to soft X-rays (up to ~3 keV) that was formed by the core collapse of a massive progenitor star (mass ≳25 M⊙; Filipović et al. 2005; Reynoso et al. 2006; García et al. 2012; Kamitsukasa et al. 2015; Auchettl et al. 2015a). Following th... | [
"Halpern et al. 2014"
] | [
"The estimated spin-down energy is Ė = 1.36 × 1036 erg s-1 and the surface dipolar magnetic field is 7.4 × 1011 G"
] | [
"Background"
] | [
[
991,
1010
]
] | [
[
877,
989
]
] |
2015ApJ...804..130C__Bertschinger_1985_Instance_3 | We have rigorously developed the embedded gravitational lensing theory for point mass lenses in a series of recent papers (Chen et al. 2010, 2011, 2015; Kantowski et al. 2010, 2012, 2013) including the embedded lens equation, time delays, lensing magnifications, shears, etc. We successfully extended the lowest-order em... | [
"Bertschinger 1985"
] | [
"The initial perturbation can be compensated or uncompensated, which leads to different void growth scenarios"
] | [
"Background"
] | [
[
2188,
2205
]
] | [
[
2078,
2186
]
] |
2015ApJ...807..101K__Sui_et_al._2005_Instance_1 | In a collisional thick-target model, the HXRs are produced by collisional bremsstrahlung during the passage of non-thermal electrons through denser plasma regions, in which the electrons are stopped completely by Coulomb collisions (Brown 1971; Brown et al. 2009; Kontar et al. 2011). Using the electron distribution par... | [
"Sui et al. 2005"
] | [
"An accurate determination of the low-energy cutoff to non-thermal electron distributions is crucial for the calculation of power and consequently non-thermal energy in solar flares"
] | [
"Motivation"
] | [
[
848,
863
]
] | [
[
666,
846
]
] |
2015AandA...583A..77L__Busso_et_al._2001_Instance_1 | During the past decade, significant information has been gathered on the chemical compositions of post-asymptotic giant branch (AGB) stars in the Milky Way. This has led to the discovery of a class of post-AGB stars that have C/O > 1 and display extreme enrichment in the abundances of the elements heavier than Fe produ... | [
"Busso et al. 2001"
] | [
"Since AGB stars can become C rich and have been confirmed both theoretically and observationally as the main stellar site for the s-process (see, e.g.,",
"it is natural to interpret these post-AGB observations as the signature of the nucleosynthesis and mixing events that occurred during the preceeding AGB phase... | [
"Background",
"Background"
] | [
[
598,
615
]
] | [
[
446,
597
],
[
618,
777
]
] |
2020AandA...643A.148G__Martin_et_al._1998_Instance_1 | Figure 11 shows that the distribution of the spectral index α (see Table A.1) is bimodal suggesting the existence of two populations (disc-bearing and discless stars) with approximately the same number of sources. We verified that the bimodality of the distribution of spectral indices is not an artefact caused by the d... | [
"Martin et al. 1998"
] | [
"Previous studies suggested that the early disappearence of circumstellar discs could be related to environmental effects imposed by the presence of massive stars that produce strong UV radiation, stellar winds, and supernova explosions (see e.g.",
"However, we see no dependency of the spectral index on the posit... | [
"Background",
"Differences"
] | [
[
827,
845
]
] | [
[
561,
806
],
[
848,
1020
]
] |
2016MNRAS.457.2569M__Binney_&_Piffl_2015_Instance_1 | The top-down dynamical approach consists in producing ab initio simulations of Milky Way-like galaxies in a cosmological context. This approach can be useful to understand some general features of galaxy formation (e.g. Minchev et al. 2014). However, it is not flexible enough to produce an acceptable model for the wide... | [
"Binney & Piffl 2015"
] | [
"To avoid the redundancy and computational waste of representing the orbits of every single particle in the model, one can use a phase-space distribution function (DF) to represent each population of constituent particles (typically, various stellar populations and dark matter; see e.g."
] | [
"Uses"
] | [
[
875,
894
]
] | [
[
588,
874
]
] |
2019AandA...631A..35B__Bridges_et_al._(1996)_Instance_4 | 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)"
] | [
"While the composition of the target surface was different than in",
"and Higa et al. (1996) (fine granular material vs. solid ice), the similar behavior of the coefficient of restitution supports the fact that particle-surface collisions are very different from particle-particle collisions, and coefficients of r... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1639,
1660
]
] | [
[
1573,
1638
],
[
1661,
2065
]
] |
2022AandA...667A.131B__Izumi_et_al._(2016)_Instance_1 | Molecular line ratio diagnostics are often used to investigate the physics and chemistry of the ISM in all of these environments. For example, as the gas chemistry located in the central, nuclear regions of galaxies is believed to be dominated by X-rays produced by the AGN, in so-called X-ray dominated regions (XDRs), ... | [
"Izumi et al. (2016)"
] | [
"In particular, the “submillimeter-HCN diagram”, first proposed in Izumi et al. (2013) and later expanded upon in",
"is a very notable example of the use of molecular line ratios as a probe of AGN-galaxies; this diagram makes use of two line ratios, HCN(4−3)/HCO+(4−3) and HCN(4−3)/CS(7−6), where all of the molecu... | [
"Background",
"Background"
] | [
[
883,
902
]
] | [
[
770,
882
],
[
904,
1150
]
] |
2018MNRAS.475.3419A__Davis_et_al._1999_Instance_1 | If we consider for the bulk density the value 4500 kg m−3, which is one of the highest measured in the asteroid population out of those asteroids with good quality of data (see Carry 2012), it will strengthen the hypothesis that Psyche could be an exposed metal core of a differentiated asteroid (Elkins-Tanton et al. 20... | [
"Davis et al. 1999"
] | [
"One possibility to solve this issue is that the potential Psyche asteroid family was created at an early time, e.g. within the first 500 Myr of Solar system history",
"This would allow the family fragments to be ground down by collisional evolution and be unobservable today. The same models show that, even in th... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1531,
1548
]
] | [
[
1365,
1529
],
[
1551,
1815
]
] |
2019ApJ...886...34F__Bonal_et_al._2010_Instance_1 | Here, we report Li–Be–B and Al–Mg isotopic compositions of seven CAIs from Sayh al Uhaymir (SaU) 290 (CH) and one CAI from Isheyevo (CH/CB) chondrites, which are one of the most pristine (unmetamorphosed) meteorites in our collections (e.g., Bischoff et al. 1993; Weisberg et al. 2001; Krot et al. 2002). The CH and CH/C... | [
"Bonal et al. 2010"
] | [
"The CH and CH/CB (hereafter: CH–CB) chondrites and their components are characterized by enrichments in 15N (up to 1,100‰;"
] | [
"Background"
] | [
[
488,
505
]
] | [
[
305,
427
]
] |
2021AandA...655A..99D__Carigi_et_al._2005_Instance_1 | 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"
] | [
"Once metallicity starts to increase, low- and intermediate-mass stars release carbon and massive stars start to eject more carbon than oxygen"
] | [
"Background"
] | [
[
1301,
1319
]
] | [
[
1158,
1299
]
] |
2019ApJ...875L..31H__Leary_et_al._2006_Instance_2 | The recent detection of gravitational-wave (GW) emission from a merging neutron star binary (Abbott et al. 2017d) and merging black hole binaries (BHBs; Abbott et al. 2016a, 2016b, 2017a, 2017b, 2017c; The LIGO Scientific Collaboration & The Virgo Collaboration 2018) by the Laser Interferometer Gravitational-Wave Obser... | [
"O’Leary et al. 2006"
] | [
"Unlike LIGO/Virgo, which can only detect merging BHBs in the final inspiral phase before merger, LISA will be able to detect eccentric stellar-mass BHBs for long timescales before they merge in the LIGO/Virgo band (e.g.,"
] | [
"Compare/Contrast"
] | [
[
1971,
1990
]
] | [
[
1750,
1970
]
] |
2022AandA...659A...5Y__Mills_et_al._2018_Instance_2 | Since its discovery more than five decades ago (Cheung et al. 1968), ammonia (NH3) has been a most valuable molecule for investigating the physical properties of molecular clouds (e.g., Ho & Townes 1983). While thermally excited transitions in the centimeter-wavelength inversion transitions of ammonia are regarded as a... | [
"Mills et al. 2018"
] | [
"These have led to the discovery of metastable maser lines in 22 different regions"
] | [
"Background"
] | [
[
1445,
1462
]
] | [
[
933,
1014
]
] |
2016ApJ...832...52F__Harris_et_al._2012_Instance_1 | However, most Herschel sources are not SMGs; they are, instead, less luminous dusty star-forming galaxies at lower redshifts (z 2; Casey et al. 2012, 2014). To select Herschel sources that are likely to be SMGs, we chose only the subsample that satisfies the following criteria: (1) flux density peak at 350 μm (
... | [
"Harris et al. 2012"
] | [
"This is confirmed by the blind carbon monoxide (CO J = 1–0) survey of a subsample of the brightest 350 μm peakers (S350 ≥ 115 mJy), which has shown a strikingly similar redshift distribution as 850 μm selected SMGs (zCO = 2.5 ± 0.8;"
] | [
"Similarities"
] | [
[
808,
826
]
] | [
[
575,
807
]
] |
2019ApJ...885...81S__Grogin_et_al._2011_Instance_1 | We measured the apparent axial ratio on the IF814W-band data, which correspond to the rest-frame V band for galaxies at z ∼ 0.4 and the rest-frame B band for those at z ∼ 0.8. Such differences in the rest-frame wavelength could cause some biases in the morphological analysis due to the color differences between bulge a... | [
"Grogin et al. 2011"
] | [
"In order to check the effects of the morphological K-correction, we used publicly available HST/ACS VF606W-band data over a 0.05 deg2 region in the COSMOS field from the CANDELS survey"
] | [
"Uses"
] | [
[
727,
745
]
] | [
[
541,
725
]
] |
2021ApJ...912..163B__Kleine_et_al._2020_Instance_1 | Shortly after the ignition of the Sun, the solar system contained a colossal cloud of dust and gas known as the protoplanetary disk. Within just a few million years, trillions of submillimeter-scale solids formed from this disk and coalesced to create a spectrum of planetary bodies that included asteroids, comets, and ... | [
"Kleine et al. 2020"
] | [
"For instance, a number of measurements have revealed that the stable isotopic compositions of all meteorites fall into two distinct families"
] | [
"Background"
] | [
[
1354,
1372
]
] | [
[
1159,
1299
]
] |
2016MNRAS.457.2433P__Nolan_et_al._2012_Instance_2 | From the result of the χ2 minimization, we found that the minimized χ2 values agree with the expected values, i.e. the computed χ2 are typically in the range of ($\mathrm{d.o.f.}-\sqrt{2 \mathrm{d.o.f.}}$, $\mathrm{d.o.f.}+\sqrt{2 \mathrm{d.o.f.}}$), where d.o.f. is the number of degrees of freedom. This means that the... | [
"Nolan et al. 2012"
] | [
"Semiminor and semimajor axes of many 2FGL sources are derived with one order of magnitude higher uncertainties than those for Mrk 421 in the 2FGL catalogue"
] | [
"Compare/Contrast"
] | [
[
987,
1004
]
] | [
[
830,
985
]
] |
2016MNRAS.463.2716M__Cho_&_Lazarian_2007_Instance_1 | Returning to the case of HL Tau, where the possible contribution of an infalling envelope is not an issue, how can one reconcile the strong indication of a dominant radial field component in the polarization map with the expectation that the bulk of the mm-wavelength emission originates near the disc mid-plane, where t... | [
"Cho & Lazarian 2007"
] | [
"Perhaps a more likely possibility is that, even in this comparatively young source, the grains near the mid-plane, which dominate the total intensity, have already grown to sizes that exceed the maximum size $a_\\mathrm{max} = \\lambda /2\\pi$ for producing polarized emission at wavelength λ (e.g.",
"; for λ = 1... | [
"Uses",
"Uses"
] | [
[
1082,
1101
]
] | [
[
786,
1081
],
[
1101,
1134
]
] |
2015MNRAS.454.2003P__Paardekooper_&_Papaloizou_2009_Instance_1 | In both of these approaches, disc–planet interactions causing planet migration are modelled using analytical formulae for the disc torque experienced by the planet. This gravitational torque consists of two components. The differential Lindblad torque results from the angular momentum exchange between the planet and th... | [
"Paardekooper & Papaloizou 2009"
] | [
"It has been shown that for mildly positive surface density gradients or negative entropy gradients, a positive corotation torque can eventually counteract the effect of a negative differential Lindblad torque, which may stall or even reverse migration"
] | [
"Background"
] | [
[
1604,
1634
]
] | [
[
1321,
1572
]
] |
2021AandA...651A..87O__Brunthaler_et_al._2021_Instance_2 | To complement our study, we also analyzed GLOSTAR continuum images toward sites with maser emission. A full description of the GLOSTAR continuum data calibration and imaging is given in Brunthaler et al. (2021), while the full analysis of continuum images of Cygnus X will be presented in a forthcoming paper. Here, we b... | [
"Brunthaler et al. 2021"
] | [
"Continuum and methanol line maps from Effelsberg observations have also been obtained as part of the GLOSTAR survey"
] | [
"Uses"
] | [
[
1004,
1026
]
] | [
[
887,
1002
]
] |
2021AandA...652A..98G__Buta_et_al._(2009)_Instance_1 | On the CND scales displayed in Fig. 12, the CO(3–2) emission in this highly inclined (i = 59°; Appendix D) barred Seyfert 2 galaxy is detected at every single position inside r 200 pc. However, a sizeable fraction of the molecular gas appears concentrated in a nuclear ring of ∼200 pc (deprojected) radius. Molecular ga... | [
"Buta et al. (2009)"
] | [
"The bar, detected in the NIR by Quillen et al. (1997) and",
"shows a prominent boxy-shape morphology."
] | [
"Background",
"Background"
] | [
[
630,
648
]
] | [
[
572,
629
],
[
650,
690
]
] |
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