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 |
|---|---|---|---|---|---|---|
2021ApJ...917...24Z__Hall_&_Evans_2019_Instance_1 | As Advanced LIGO and Virgo will upgrade while additional interferometers (KAGRA and LIGO-India) come online in the future, the detection horizon would be several hundred megaparsecs for BNS and BH–NS mergers with the localization accuracy reaching ∼10 deg2 for a network of these 2nd generation GW detectors (Abbott et a... | [
"Hall & Evans 2019"
] | [
"In contrast, higher localization accuracy would be obtained by networking of 3rd generation GW detectors"
] | [
"Compare/Contrast"
] | [
[
470,
487
]
] | [
[
330,
434
]
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2021AandA...646A..96C__Freundlich_et_al._2019_Instance_1 | Observations of cold molecular gas are more promising since any activity from the AGN (radiation, outflows, or jets) will have an impact on the molecular gas reservoir first, and then on the SFR, which previous studies have focused on. The molecular gas provides an instantaneous measure of the raw fuel from which stars... | [
"Freundlich et al. 2019"
] | [
"Over the last decade, large observational efforts have been devoted to map the molecular gas reservoir of galaxies (e.g.,",
"These studies are largely based on observations of carbon monoxide (CO) rotational emission lines, used as a tracer of cold molecular hydrogen H2 (the ground-state rotational transition in... | [
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771,
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2020MNRAS.492.5675C__Pérez-Montero_et_al._2019_Instance_1 | In regarding AGNs, the Te method tends to underestimate the oxygen abundance by an average value of about 0.6 dex in comparison to estimations based on strong-line methods and it produces subsolar O/H values for most of these objects (Dors et al. 2015; Dors, Freitas-Lemes & Âmores 2020). An alternative method to derive... | [
"Pérez-Montero et al. 2019"
] | [
"Along decades, results based on this indirect method have indicated Z near or slightly above the solar value in nuclear regions",
"in consonance with predictions of chemical evolution models",
"and with the use of strong-line methods"
] | [
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2017MNRAS.471...80S__Kalugina_et_al._2014_Instance_2 | The electronic computations were performed using the molpro (Molpro 2015, http://www.molpro.net) package. In a preliminary work, we used the complete active space self-consistent field (Knowles & Werner 1985; Werner & Knowles 1985) to examine the electronic wavefunction of the HNCO–He complex. These computations showed... | [
"Kalugina et al. 2014"
] | [
"Benchmarks by Hochlaf and co-workers",
"showed that results obtained from this highly correlated approach are close to those deduced using standard coupled cluster techniques extrapolated to the complete basis set (CBS) limit, whereas a strong reduction in CPU time and disc occupancy are observed."
] | [
"Similarities",
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[
1585,
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]
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1466,
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2021AandA...653A..83V__Krühler_et_al._(2015)_Instance_1 | The comparisons show that except for GRBs 060707 and 060605, which have a very high vpeak, the LAE-LGRBs fall in the same parameter space as LyC leakers and follow the correlations between the indirect indicators found by Verhamme et al. (2017). Following their study, we can cut these plots into two regions correspondi... | [
"Krühler et al. (2015)"
] | [
"In panel b of Fig. 12, we also superimpose the distribution of [OIII]/[OII] ratio for the GRB sample of",
"and GRB 081121 reported here.",
"For the majority of the GRBs, this ratio is about two, with seven cases at O32 > 4. GRB 021004 has a high value of O32 > 10 and is the strongest LAE of our golden sample (... | [
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2018MNRAS.475.1160H__Werk_et_al._2013_Instance_2 | 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"
] | [
"Additionally, CGM observations infer a significant amount of metals (e.g."
] | [
"Background"
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[
1863,
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[
1789,
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2019AandA...630A..30L__Hässig_et_al._(2015)_Instance_2 | The many unexpected surprises of comet 67P/Churyumov-Gerasimenko (hereafter 67P) revealed by the historic Rosetta mission highlight the importance of observing the evolution of comets throughout their orbits. One of the surprises was the drastic heterogeneity in both the major and minor volatile species in the coma tha... | [
"Hässig et al. 2015"
] | [
"The intensity variations in the major and minor volatile species were found to be periodic, and were dependent on both the observing sub-spacecraft latitude and longitude"
] | [
"Background"
] | [
[
1007,
1025
]
] | [
[
835,
1005
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2022MNRAS.513.5245A__Done_&_Jin_2016_Instance_2 | We assume the time-scales we observe here are generated in the corona itself (and note that longer time-scale changes will be driven by the disc outside of the corona) and are made visible by a changing electron temperature and density as a result of local turbulence and coupling to mass accretion rate propagations thr... | [
"Done & Jin 2016"
] | [
"Given the reported high spin values for these bright AGNs",
"we expect the ISCO to sit at ∼1.25Rg."
] | [
"Uses",
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[
1751,
1766
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1654,
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[
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2015MNRAS.450.3458C__Cichowolski_et_al._2001_Instance_4 | The kinetic energy stored in the CO shell can be estimated as $E_{\rm kin} = 0.5\, M_{\rm shell}\, V^2_{\rm exp}$, where Vexp is the expansion velocity of the shell and Mshell is the total (molecular, atomic, and ionized) shell mass. Adopting an expansion velocity equal to half the velocity interval where the structure... | [
"Cichowolski et al. 2001"
] | [
"Thus, we can compare now the new value obtained for Ekin with the mechanical energy deposited in the ISM by the wind of the WR star, Ew = (0.7–2.2) × 1050 erg"
] | [
"Compare/Contrast"
] | [
[
1012,
1035
]
] | [
[
852,
1010
]
] |
2020MNRAS.491..560D__Straten_&_Manchester_2004_Instance_1 | As MKT J170456.2–482100 is coincident with a star in a spectroscopic binary, it is possible that the companion star may be a pulsar or pulsating white dwarf, similar to AR Scorpii (Marsh et al. 2016). To investigate this possibility, we performed high-time resolution observations to search for pulsations over a range o... | [
"Hotan, van Straten & Manchester 2004"
] | [
"The data were recorded in psrfits format and processed using PSRCHIVE tools"
] | [
"Uses"
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[
901,
937
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] | [
[
824,
899
]
] |
2016AandA...585A..76W__Neau_et_al._2000_Instance_1 | The median value of the column density of OH in the first quadrant is 3.9 × 1014 cm-3 and for OH+ it is 0.68 × 1014 cm-3. In the fourth quadrant, the median column densities amount to 1.7 × 1014 cm-3 and 0.55 × 1014 cm-3, respectively. Column densities in excess of 1015 cm-2 (for OH) and above ~1014 cm-2 (for OH+) are ... | [
"Neau et al. 2000"
] | [
"determined by ion storage ring experiments,"
] | [
"Background"
] | [
[
961,
977
]
] | [
[
897,
940
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] |
2017AandA...605A..20C__Momjian_&_Sarma_2017_Instance_1 | In principle, when ΔνZ>δν, with δν being the observed full width at half maximun (FWHM) of the line, the complete set of information concerning the magnetic field B can be derived. However, for most of the Zeeman detections, the Zeeman splitting ΔνZ turns out to be significantly smaller than δν. Indeed, even if we negl... | [
"Momjian & Sarma 2017"
] | [
"The expected B values in star forming regions range from ~100 μG, for low-mass objects",
", to ~1 mG, as measured in regions hosting high-mass young stars (e.g.,"
] | [
"Uses",
"Uses"
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[
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[
973,
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2020ApJ...898...92C__Lawson_et_al._2012_Instance_1 | Neutral MF occurs as syn and anti conformers (also denoted Z and E rotamers) with Cs symmetry, with the syn rotamer being more stable (by ∼20 kJ mol−1) and well separated from the anti rotamer by a significant energy barrier of ∼35 kJ mol−1 for anti
syn isomerization (Wilmshurst 1957; Curl 1959; Blom & Günthard ... | [
"Lawson et al. 2012"
] | [
"Numerous mass spectrometric studies have investigated the production of H+MF via various ion–molecule reactions and its fragmentation by metastable decay and collisions"
] | [
"Background"
] | [
[
1459,
1477
]
] | [
[
1179,
1347
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] |
2022MNRAS.514.5192L__Borsa_et_al._2021_Instance_1 | We introduce the quantity ξ to represent a scaled product of equilibrium temperature (Teq) and surface gravity (g):
(14)$$\begin{eqnarray}
\xi = \left(\frac{T_{\text{eq}}}{1000~\text{K}}\right)\left(\frac{g}{g_{\rm J}}\right) ~,
\end{eqnarray}$$where gJ is the surface gravity of Jupiter. The calculated ξ values are l... | [
"Borsa et al. 2021)"
] | [
"The salmon-coloured points show recent results from other high-resolution spectrographs:",
"WASP-121b with ESPRESSO"
] | [
"Uses",
"Uses"
] | [
[
918,
936
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[
668,
756
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[
893,
916
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2017MNRAS.471.3856T__Tempel_et_al._2011_Instance_1 | It is important to note that we have not classified our simulated galaxies by morphology itself in this paper, and more detailed analysis of the morphology, including kinematical decomposition, will be made in future work. In Fig. 4, we show the distributions of our morphology indicators, ETGΔs, LTGΔs, ETGΔt, and LTGΔt... | [
"Tempel et al. 2011"
] | [
"Since mergers are strong drivers of morphological change, this implies that our high-mass galaxies are mostly elliptical, which is in good agreement with observational results for ellipticals and S0 galaxies (e.g."
] | [
"Similarities"
] | [
[
833,
851
]
] | [
[
597,
810
]
] |
2018MNRAS.479.3254V___2000_Instance_1 | The lifetime of molecular clouds (MCs) remains an active research topic in the study of the interstellar medium and star formation, and most recent studies, both observational and theoretical, place this lifetime at a few times 107 yr for clouds in the 105–106M⊙ mass range (e.g. Blitz & Shu 1980; Kawamura et al. 2009; ... | [
"Palla & Stahler",
"2000"
] | [
"For example, studies of young clusters embedded in moderate-mass MCs (∼104M⊙) (e.g.",
"have shown that their age histograms contain a large majority of young (1–2 Myr) objects, but also a tail of older (up to several Myr) ones suggesting an accelerating star formation activity, sometimes followed by a subsequent... | [
"Background",
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[
677,
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[
699,
703
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[
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[
725,
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2021MNRAS.503.6016K__Martocchia_et_al._2018a_Instance_1 | Observations of splits in the MS and at the eMSTO of young and (at least) moderately massive Magellanic Cloud star clusters have demonstrated the presence of complex stellar populations, suggestive of variations in their stellar rotation properties (Milone et al. 2018a). The effects of stellar rotation on stellar popul... | [
"Martocchia et al. 2018a"
] | [
"NGC 419, another young massive cluster with an age of 1.72 Gyr and a mass of ∼104 M⊙, are comparably massive with respect to other star clusters that show clear evidence of MPs"
] | [
"Differences"
] | [
[
766,
789
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[
588,
764
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2021AandA...656A..44R__Duc_2012_Instance_1 | In this work we aim to explore the presence and properties of LSBGs in the environment of the NGC 1052 group of galaxies. This region is of particular interest in light of the “exotic” properties that recent works claim for some LSBGs found in this region. For instance, van Dokkum et al. (2018a) in [KKS2000] 04 (more c... | [
"Duc 2012"
] | [
"the possibility that they are tidal dwarf galaxies – galaxies formed by strong interactions with recycled material from massive host galaxies, high in metals, and intrinsically born with a lack of dark matter (see e.g.,",
"– is ruled out."
] | [
"Differences",
"Differences"
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[
1116,
1124
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[
896,
1115
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[
1145,
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2016MNRAS.461.1719C__Fu_et_al._2012_Instance_1 | HATLAS12-00 had already been identified as a candidate gravitationally lensed galaxy as a result of its high submm flux (i.e. F500 > 100 mJy), red Herschel colours and the lack of a bright optical or radio counterpart (see e.g. Negrello et al. 2010 for a discussion of the selection of lens candidates in H-ATLAS and oth... | [
"Fu et al. 2012"
] | [
"A CO spectroscopic redshift of 3.26 was first suggested by Z-spec",
"observations, then subsequently confirmed by observations by",
"the Zpectrometer instrument",
"on the Greenbank Telescope"
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
725,
739
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409,
474
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[
498,
558
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[
619,
646
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[
668,
694
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] |
2019MNRAS.490.3875L__Onaka_et_al._1996_Instance_1 | Similar to Chen et al. (2017), we also follow Li & Draine (2001a) to derive upper limits on the abundance of the graphene C24 in the Galactic cirrus and in the diffuse ISM towards l = 44°20′, b = −0°20′ based on comparison of the observed IR emission with the calculated emission spectrum of C24. For the Galactic cirrus... | [
"Onaka et al. 1996"
] | [
"The Mid-Infrared Spectrograph (MIRS) aboard the Infrared Telescope in Space (IRTS) has also obtained the 4.7–11.7$\\, {\\rm \\mu m}$ spectrum for the diffuse ISM towards l = 44°20′, b = −0°20′"
] | [
"Uses"
] | [
[
788,
805
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] | [
[
597,
786
]
] |
2020ApJ...901...50E__Dame_et_al._2001_Instance_1 | Molecular hydrogen H2 is conventionally believed to make up 17% of the interstellar medium (ISM) by mass in the Galaxy (e.g., Draine 2011, Table 1.2, not including He), but, unlike atomic hydrogen H i (at 60% by mass), H2 is not generally detectable in the cold, diffuse conditions that predominate the volume of the ISM... | [
"Dame et al. 2001"
] | [
"The primary tracer for H2 in current use is the J = (1−0) ground-state rotational transition of 12CO at a wavelength of 3 mm. While this tracer has become widely adopted over the years (see, e.g.,",
"and has been often defended as a reliable large-scale tracer for molecules in the ISM, it also remains the primar... | [
"Background",
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] | [
[
667,
683
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[
451,
647
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[
685,
880
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2020MNRAS.495.2949F__Stauffer_et_al._2016_Instance_1 | Stellar rotation is known to be related to the activity level; e.g. faster rotators tend to have larger star-spot coverages (e.g. Paper I), and stronger chromospheric emissions (e.g. Stauffer et al. 1997; Douglas et al. 2014; Newton et al. 2017; Paper II) and X-ray emissions (e.g. Pizzolato et al. 2003; Mamajek & Hille... | [
"Stauffer et al. 2016"
] | [
"It is reasonable to connect the scatter to the stellar rotation rate diversity, considering the fact that there exist noticeable differences in rotation periods between stars of the same temperature in young open clusters (e.g."
] | [
"Uses"
] | [
[
759,
779
]
] | [
[
531,
758
]
] |
2022AandA...666L...5G__Ramos_et_al._2014_Instance_1 | More recently, García-Bernete et al. (2022) found that the PAH molecules responsible for the 11.3 μm PAH emission band are more resilient in the hard environments often present in AGN. In particular, the authors found larger 11.3/7.7 μm and 11.3/6.2 μm PAH ratios in AGN-dominated systems compared to SF galaxies, indica... | [
"Ramos et al. 2014"
] | [
"Previous sub-arcsecond angular resolution N-band (∼8–13 μm) ground-based spectroscopic studies investigated the 11.3 μm PAH feature in the nuclear and circumnuclear regions of AGN (e.g.,",
"However, these works were unable to provide definitive details regarding the effect of the AGN on the PAH molecules due to ... | [
"Background",
"Motivation"
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[
861,
878
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[
592,
778
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980,
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2020AandA...633A.147B__Xu_et_al._(2013)_Instance_1 | We used the position and distance of the MCs in the FQS catalogue to describe the structure of the Milky Way in this poorly known portion of the third quadrant. In Fig. 16 we show the distribution of the clouds projected onto the Milky Way plane. At any Galactic longitude the clouds are grouped in three well-separated ... | [
"Xu et al. (2013)"
] | [
"The pitch angle and the distance at a reference position of the three arms are taken from",
"for the Local arm",
"These authors used the positions of water masers derived from parallax measurements as part of the Bar and Spiral Structure Legacy (BeSSeL) survey to fit the parameters of the spiral arms.",
"We ... | [
"Uses",
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1021
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1317,
1440
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2015AandA...584A..75V__Essen_et_al._(2014)_Instance_1 | The data presented here comprise quasi-simultaneous observations during secondary eclipse of WASP-33 b around the V and Y bands. The predicted planet-star flux ratio in the V-band is 0.2 ppt, four times lower than the accuracy of our measurements. Therefore, we can neglect the planet imprint and use this band to measur... | [
"von Essen et al. 2014"
] | [
"Therefore, we can neglect the planet imprint and use this band to measure the stellar pulsations, and most specifically to tune their current phases (see phase shifts in"
] | [
"Uses"
] | [
[
418,
439
]
] | [
[
248,
417
]
] |
2021AandA...649A.126T__Luck_(2018b)_Instance_2 | 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)"
] | [
"It is interesting to note that the [Ba/Fe] versus Rgc slope according to this Cepheid sample is also negative, as in our study. [Ba/Fe] is the only n-capture element-to-iron ratio with a negative radial gradient in our sample of stars and in"
] | [
"Similarities"
] | [
[
1403,
1415
]
] | [
[
1161,
1402
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] |
2018MNRAS.474.2277D__Oliveira,_Dottori_&_Bica_1998_Instance_1 | There are three possible explanations for the origin of these systems: (1) they formed from the fragmentation of the same molecular cloud (Elmegreen & Elmegreen 1983), (2) they were generated in distinct molecular clouds and then became bound systems after a close encounter leading to a tidal capture (Vallenari, Betton... | [
"de Oliveira, Dottori & Bica 1998"
] | [
"Dynamical models and N-body simulations (see, e.g.,",
"and references therein) have shown that, depending on the initial conditions, a bound pair of clusters may either become unbound, because of significant mass-loss in the early phases of stellar evolution, or merge into a single and more massive cluster on a ... | [
"Background",
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[
621,
653
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[
550,
601
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[
655,
991
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2022AandA...667A..82D__Lyne_et_al._(1985)_Instance_1 | Much of the progress in PPS has come from thorough Monte Carlo simulations that generate pulsars and test whether they fulfil the criteria for detection according to geometrical factors and sensitivity issues. It is then possible to develop and optimize a model for the underlying pulsar population, which informs us abo... | [
"Lyne et al. (1985)"
] | [
"Inspired by earlier studies from Taylor & Manchester (1977) and",
"Lorimer et al. (2006) applied the snapshot approach to the canonical3 pulsar population to determine best-fitting probability density functions in Galactocentric radius (R), luminosity (L), height with respect to the Galactic plane (z), and the p... | [
"Background",
"Background"
] | [
[
914,
932
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850,
913
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[
934,
1237
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2020MNRAS.495L..27H__Cao_et_al._2018_Instance_1 | Independent measurements of distances and redshifts, z, allow astronomers to constrain cosmological models, since they both define the distance–redshift relation. When it was determined that type Ia supernovae (SNIa) could be standardized and therefore used to measure distances, this led to the discovery of the acceler... | [
"Cao et al. 2018"
] | [
"For instance, we can use these model-independent measurements",
"to test natural constants such as the speed of light"
] | [
"Background",
"Background"
] | [
[
2624,
2639
]
] | [
[
2026,
2087
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[
2570,
2622
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2021ApJ...919...30D__Staguhn_et_al._2014_Instance_2 | The first SMGs were detected using SCUBA at 850 μm (Smail et al. 1997; Barger et al. 1998; Hughes et al. 1998), which remains one of the prime wavelengths to detect these galaxies (e.g., Geach et al. 2017), thanks to a combination of available instruments, spectral window, and the negative k-correction at that waveleng... | [
"Staguhn et al. 2014"
] | [
"Selecting SMGs from observations at longer wavelengths is thought to favor galaxies at higher redshifts (e.g.,",
"although it is difficult to compare the redshift distributions in an unbiased way",
"and account for intrinsic variations of galaxy far-IR spectral energy distributions (SEDs)."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
802,
821
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[
650,
760
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[
869,
950
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1001,
1092
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2022ApJ...931...70B__Gabrielse_et_al._2012_Instance_2 | RFs can propagate from the magnetotail to Earth over a long distance more than 10 R
E together with BBFs behind them (Runov et al. 2009; Cao et al. 2010). Studies have suggested that RFs are crucial regions for particle acceleration, pitch-angle evolution, wave–particle interactions, and electromagnetic energy conversi... | [
"Gabrielse et al. 2012"
] | [
"Possible mechanisms responsible for the energization of particles around RFs have been widely investigated based on both spacecraft observations and numerical simulations during the past decade. The strong convection electric field induced by the strong magnetic field gradient of RFs provides significant adiabatic... | [
"Background"
] | [
[
1811,
1832
]
] | [
[
1426,
1779
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] |
2017ApJ...835...25E__Rutten_1984_Instance_1 | We compare our results with a new reduction of observations from the Lowell Observatory SSS, which is running a long-term stellar activity survey complementary to the MWO HK Project. The SSS observes solar and stellar light with the same spectrograph, with the solar telescope consisting of an exposed optical fiber that... | [
"Rutten 1984"
] | [
"(simply K in other works) is the conversion factor from the MWO HKP-2 H & K flux (numerator of Equation (1)) to physical flux"
] | [
"Uses"
] | [
[
1020,
1031
]
] | [
[
893,
1018
]
] |
2019MNRAS.485L..78V__Chatterjee_et_al._2017_Instance_2 | The properties of the persistent radio source associated with FRB 121102 may be constrained independently of the Faraday-rotating medium. We assume equipartition between the relativistic gas and magnetic field as is common in synchrotron sources3 (Readhead 1994). The source becomes self-absorbed at $1.5$ GHz for radius... | [
"Chatterjee et al. 2017"
] | [
"We assume a power-law energy distribution of radiating electrons with somewhat shallow index of b = −1.5 that can account for the relatively flat spectrum of the source"
] | [
"Uses"
] | [
[
1306,
1328
]
] | [
[
1136,
1304
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] |
2020MNRAS.497.2941S__Loeb_&_Barkana_2001_Instance_1 | After the cosmological recombination, the universe went into the dark ages during which the density fluctuations in the matter distribution grew, and after reaching a threshold, the matter collapsed to make the first bound objects. The nature of dark matter sets the timeline and characteristics of these first bound obj... | [
"Loeb & Barkana 2001"
] | [
"The present observational probes that allow us to have a peak in this epoch are the absorption spectra of high-redshift quasars"
] | [
"Background"
] | [
[
819,
838
]
] | [
[
690,
817
]
] |
2022MNRAS.509.1959S__Ezzeddine_et_al._2019_Instance_1 | However, the transition between the two extremes of modern (metal-rich) and primordial (metal-poor) star formation, and in particular the role of dust coupling and stellar radiation feedback at low metallicity, has thus far received limited exploration. Krumholz (2011) present analytical models for radiation feedback a... | [
"Ezzeddine et al. 2019"
] | [
"However, these studies do not explore lower metallicities, despite available evidence for the existence of a low-metallicity ISM in the past through the discovery of stars with metallicities as low as $10^{-4}\\, \\rm {Z_{\\odot }}$",
"as well as several others with $\\rm {[Fe/H]} \\lt -5$"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1023,
1044
]
] | [
[
602,
831
],
[
879,
931
]
] |
2022MNRAS.509..903N__Murguia-Berthier_et_al._2014_Instance_1 | Binary neutron star (BNS) mergers have long been suspected to produce the central engines of short gamma-ray bursts (sGRBs) (Eichler et al. 1989). The link was firmly established in August 2017, after the combined detection of gravitational waves and an sGRB from the same BNS merger (Abbott et al. 2017a,b,c; Goldstein ... | [
"Murguia-Berthier et al. 2014"
] | [
"Recent relativistic (magneto-) hydrodynamics simulations",
"have illustrated the importance of the ambient medium in shaping the jet, thereby highlighting the importance of understanding the remnant structure and ejecta properties"
] | [
"Motivation",
"Background"
] | [
[
1837,
1865
]
] | [
[
1779,
1835
],
[
2141,
2311
]
] |
2016MNRAS.463.2716M__Cho_&_Lazarian_2007_Instance_2 | 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"
] | [
"It is, however, conceivable that the large grains in this source are not well aligned because the radiative torque mechanism does not operate efficiently on them: this could happen if the characteristic wavelength of the anisotropic component of the local radiation field were much smaller than the mid-plane grain ... | [
"Future Work"
] | [
[
3812,
3831
]
] | [
[
3485,
3811
]
] |
2021ApJ...910..124X__Leslie_et_al._2016_Instance_1 | What is the dominant mode of star formation for AGNs in general, and for quasars in particular? The main sequence gives a useful framework for discussing the evolutionary status of AGN host galaxies and their relation to the galaxy population at large. The existing literature in this field, however, is complicated enor... | [
"Leslie et al. 2016"
] | [
"While there is almost unanimous agreement that AGNs of low to moderate luminosity (Lbol ≲ 1045 erg s−1) at z ≈ 0–3 lie on or below the main sequence (e.g.,",
", no consensus exists for AGNs with Lbol > 1045 erg s−1."
] | [
"Similarities",
"Differences"
] | [
[
759,
777
]
] | [
[
472,
627
],
[
860,
916
]
] |
2017MNRAS.464.2545C__López-Corredoira_&_Molgó_2014_Instance_1 | One of the fundamental tasks of the Galactic studies is to estimate the structure parameters of the major structure components. Bahcall & Soneira (1980) fit the observations with two structure components, namely a disc and a halo. Gilmore & Reid (1983) introduce a third component, namely a thick disc, confirmed in the ... | [
"López-Corredoira & Molgó 2014"
] | [
"As the quantity and quality of data available continue to improve over the years, the model parameters derived have become more precise, numerically. Ironically, those numerically more precise results do not converge",
"table 2 of",
"The scatters in density law parameters, such as scale lengths, scale heights ... | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
785,
814
]
] | [
[
518,
734
],
[
774,
784
],
[
885,
1060
]
] |
2015AandA...579A.132P__Simha_et_al._(2009)_Instance_1 | A common feature of all previous models is that the relation between the central galaxy stellar mass and the halo mass reaches a maximum at halo masses ~1012 M⊙. According to Yang et al. (2012), below this threshold the mass accretion of the central galaxy is dominated by star formation. Thus, when the halo mass reache... | [
"Simha et al. (2009)"
] | [
"According to",
"the subhalos also retain their identity for quite some time after accreting a larger halo, so satellites in subhalos less massive than ~1012 M⊙ do not immediately see the effect of the hot gas in the larger halo and accrete in cold mode.",
"Thus, consistent with the results of Yang et al. (2012... | [
"Uses",
"Uses",
"Similarities"
] | [
[
872,
891
]
] | [
[
859,
871
],
[
893,
1130
],
[
1131,
1309
]
] |
2016MNRAS.457.2480C___2008_Instance_1 | A number of ideas have been put forward to explain the formation and early evolution of the compact Kepler and radial velocity systems, which in cases such as Gliese 581 and HD 69830 appear to contain in excess of ∼30 M⊕ of solid material within a few tenths of an au (Lovis et al. 2006; Udry et al. 2007). This concentr... | [
"Cresswell & Nelson",
"2008"
] | [
"N-body simulations, combined with either hydrodynamic simulations or analytic prescriptions for migration and eccentricity/inclination damping of planetary growth, have also been used to examine the origins of such systems"
] | [
"Background"
] | [
[
877,
895
],
[
902,
906
]
] | [
[
653,
875
]
] |
2017MNRAS.470..612F__Feng_etal._2016_Instance_2 | The millimetre bump in M87 as recently observed by the Atacama Large Millimeter/submillimeter Array can be naturally modelled by the synchrotron emission of the thermal electrons in the ADAF, which is different from the prediction of the jet model. Therefore, it provides an opportunity to explore the accretion process ... | [
"Feng etal. 2016)"
] | [
"It is still difficult to constrain the BH spin parameter from the modelling of the SED of M87 due to some degeneracy in model parameters (wind parameter, s, magnetic parameter ;"
] | [
"Compare/Contrast"
] | [
[
686,
702
]
] | [
[
508,
685
]
] |
2018MNRAS.473.1879R__Freudling_et_al._2011_Instance_1 | Cosmic H i gas density ($\Omega _{\rm {H}\,\small {I}}$) as a function of redshift (bottom axis) and lookback time (top axis). All measurements are corrected to the same cosmological parameters. Some DLA measurements adopted a different definition of the cosmic H i density taking into account neutral gas abundance (Ωga... | [
"Freudling et al. 2011"
] | [
"The open circle and square are the results from the Arecibo Ultra Deep Survey (AUDS)"
] | [
"Uses"
] | [
[
986,
1007
]
] | [
[
900,
984
]
] |
2018ApJ...863..194L__Kraft_et_al._1991_Instance_1 | Five XRT observations got only low exposure (i.e., much less than 1 ks) and the X-ray source was therefore undetected in these data sets. Surprisingly, we also found that the source was undetected in a “deep” observation taken on 2015 August 19 with an exposure time of about 1.6 ks (Table 2). Within a 47″ radius circul... | [
"Kraft et al. 1991"
] | [
"Using a Bayesian approach",
"we computed 95% upper limits for all the nondetections."
] | [
"Uses",
"Uses"
] | [
[
887,
904
]
] | [
[
860,
885
],
[
907,
962
]
] |
2019MNRAS.487.2412G__Weinberg_1993_Instance_1 | There are only three exceptions from the picture discussed above. In Fig. 2 we see that the model with the smallest number of objects, $N=40\, 000$, does not show abrupt dissolution. This model is characterized with the shortest initial relaxation time (among models considered in this paper), about 1.6 Gyr, and the sma... | [
"Weinberg 1993"
] | [
"The very fast dissolution of tidally filling models with low King model concentration was already extensively discussed in the literature (e.g."
] | [
"Background"
] | [
[
874,
887
]
] | [
[
730,
873
]
] |
2015ApJ...815..127W__Borucki_et_al._2010_Instance_1 | Since its launch in March of 2009, the NASA Kepler mission has been monitoring ∼160,000 stars in order to detect transiting extrasolar planets with high relative photometric precision (∼20 ppm in 6.5 hr, Jenkins et al. 2010). In 2013 May, the Kepler main mission ended with the failure of a second reaction wheel; howeve... | [
"Borucki et al. 2010"
] | [
"In 2013 May, the Kepler main mission ended with the failure of a second reaction wheel; however, the first four years of Kepler data have led to a wealth of planetary discoveries with a total of 4706 announced planet candidates"
] | [
"Background"
] | [
[
529,
548
]
] | [
[
226,
453
]
] |
2019MNRAS.484.1912R__Iyyani_et_al._2016_Instance_1 | Even though most of the energy released by a gamma-ray burst (GRB) is emitted during the prompt emission phase, the emission mechanism is still not understood. In order to determine the emission process typically, the low-energy spectral index, α, of the GRB spectrum is analysed. This analysis has not given a conclusiv... | [
"Iyyani et al. 2016"
] | [
"However, a large fraction (${\\sim } 28{{\\ \\rm per\\ cent}}$) was found to be inconsistent with the theoretical limit of −2/3 (‘line of death’;",
"and only specific physical scenarios remain plausible (large emitting radii and Lorentz factors of the flow,"
] | [
"Differences",
"Differences"
] | [
[
961,
979
]
] | [
[
567,
708
],
[
828,
936
]
] |
2018MNRAS.480.1639D__cent,_Ricci_et_al._2015_Instance_1 | Six out of the eight sources (75 per cent of the sample) show evidence for high obscuration by cold gas (column density NH≳ 1023 cm−2). The number of AGN with NH≳ 1024 cm−2 is in the range 2–4 when 90 per cent confidence errors on the column density are considered (see Table 4). Although our sample is definitely too sm... | [
"Ricci et al. 2015"
] | [
"Although our sample is definitely too small to make any strong conclusion in terms of statistical incidence of obscured AGN in dual systems, we note that the fraction of CT AGN in our sample of dual AGN is 25–50 per cent, i.e. higher than the fraction of hard X-ray selected CT AGN in isolated systems in a similar ... | [
"Compare/Contrast"
] | [
[
638,
655
]
] | [
[
280,
637
]
] |
2016ApJ...827...58S__Stern_et_al._2014_Instance_1 | The multiwavength UV to mid-IR SED of J1224+5555 supports the scenario of a highly obscured AGN, based on the empirically derived templates of Assef et al. (2010). These templates consist of a set of three galaxy templates and one AGN template. The galaxy templates, E, Sbc, and Im, are based on templates from Coleman e... | [
"Stern et al. 2014"
] | [
"This method has since been used to successfully uncover highly obscured and even Compton-thick AGNs in several other works thus far"
] | [
"Background"
] | [
[
887,
904
]
] | [
[
691,
822
]
] |
2017ApJ...845..160P__Camenzind_1986a_Instance_1 | It is a pressing question as to how the radiation that is observed in relativistic jets in active galactic nuclei (AGNs) is generated (e.g., Blandford & Königl 1979; Marscher 1980; Zensus 1997; Laing & Bridle 2002; Honda 2010; Levinson & Rieger 2011; Mościbrodzka et al. 2011; Ito et al. 2013; Mason et al. 2013; Potter ... | [
"Camenzind 1986a"
] | [
"In the case of collimated relativistic jets, magnetic fields must play an important role"
] | [
"Background"
] | [
[
1205,
1220
]
] | [
[
1115,
1203
]
] |
2016AandA...586A..81H__Massey_(2002)_Instance_1 |
Table 2
Catalogue description.
Column
Description
1
Source number
2−3
X-ray coordinates, right ascension and declination (epoch 2000.0)
4
Uncertainty of X-ray position [′′]. For XMM-Newton positions taken from Sturm et al. (2013c) the 1σ error includes a systematic uncertainty of 0.5′′.
5
Origin of... | [
"Massey (2002)"
] | [
"Optical coordinates, right ascension and declination (epoch 2000.0) for the identified counterpart from Zaritsky et al. (2002), or – when not available there – from"
] | [
"Uses"
] | [
[
1148,
1161
]
] | [
[
983,
1147
]
] |
2019ApJ...875...90L__Velli_et_al._2015_Instance_1 | 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"
] | [
"For about 80 yr since the discovery of the extremely hot corona around the late 1930s (Grotian 1939; Edlen 1945), people have worked hard on addressing this issue, and great advances have been made in observation and theoretical studies"
] | [
"Background"
] | [
[
785,
802
]
] | [
[
344,
580
]
] |
2021AandA...653A..85S__However,_Genovali_et_al._(2014)_Instance_1 | Figure 6 shows the orbital eccentricities as a function of [M/H] for the metal-rich disc sample. The solid lines correspond to the required eccentricity (see Eq. (2)) for different values of ISM radial metallicity gradients: −0.10 dex kpc−1 (black), −0.07 dex kpc−1 (our measured gradient for young stars in Table 1; see... | [
"Genovali et al. 2014"
] | [
"Cepheids analysis from",
"green"
] | [
"Uses",
"Uses"
] | [
[
423,
443
]
] | [
[
400,
422
],
[
445,
450
]
] |
2016ApJ...830...28P__Zank_et_al._2015_Instance_1 | Our basic model for acceleration is shown in Figure 1. The left panel shows a cartoon of the model for acceleration, transport, and radiation at the X-reconnection site in the corona. Acceleration can be by the second order Fermi (or stochastic) acceleration by turbulence (see, e.g., Petrosian & Liu 2004), by a standin... | [
"Zank et al. 2015"
] | [
"The latter model has been invoked as a possible mechanism in the downstream of the CME shock"
] | [
"Uses"
] | [
[
675,
691
]
] | [
[
560,
652
]
] |
2017ApJ...850..197P__Langer_2012_Instance_1 | In order to explode as an ECSN, several ingredients need to be in place. Nomoto (1984) argued that stars with helium cores between 2.0 and
(which corresponds roughly to initial masses between 8 and
) would explode as an ECSN. His models, however, did not develop a second dredge-up, which can significantly ... | [
"Langer 2012"
] | [
"Since then, several authors",
"have established precise initial mass ranges for ECSNe to occur, although these mass ranges are highly sensitive to the adopted convection criteria, overshooting, and mass-loss prescriptions"
] | [
"Background",
"Background"
] | [
[
814,
825
]
] | [
[
466,
493
],
[
577,
767
]
] |
2022AandA...666A.112L__Cormier_et_al._2015_Instance_2 | Local dwarf galaxies were the focus of large Herschel and Spitzer surveys (e.g., The Dwarf Galaxy Survey, DGS; Madden et al. 2006). Studies on both resolved and integrated-galaxy scales have highlighted some distinctively unique observational signatures of star-forming low-metallicity dwarf galaxies. A non-linear relat... | [
"Cormier et al. 2015"
] | [
"Other emission lines, however, such as the far-infrared [C ii]λl58 µm line, are strikingly enhanced on global scales in dwarf galaxies (e.g.,"
] | [
"Compare/Contrast"
] | [
[
1398,
1417
]
] | [
[
1256,
1397
]
] |
2022AandA...660A.135V__Nissen_2016_Instance_1 | The first study, to our knowledge, to notice the net increase in the abundance of slow (s) neutron capture elements in young stellar populations is D’Orazi et al. (2009), in which the abundance of barium in young star clusters was seen to be higher than in the older ones. Maiorca et al. (2011, 2012) added a few more el... | [
"Nissen 2016"
] | [
"Subsequently, a number of works have",
"and to use their abundances to estimate the ages of stars, often using neutron capture s-process elements in combination with other elements with opposite behaviours, such as α elements – that we indicate as chemical clocks – and thus maximising the dependence of the relat... | [
"Background",
"Background"
] | [
[
1021,
1032
]
] | [
[
465,
501
],
[
695,
996
]
] |
2018AandA...616A..43S__Breeveld_&_Puchnarewicz_1998_Instance_1 | Within the same scenario, Smith et al. (2004, 2005) have theoretically predicted that, when observed in polarized light, NLS1s should have a low polarization fraction, the polarization angle should change monotonically from one wing of the BELs to the other, and the BELs should be significantly broader than those obser... | [
"Breeveld & Puchnarewicz 1998"
] | [
"We assume that polarized BELs are scattered into the line of sight by material that is close to coplanar with the BLR (i.e. the torus). This prediction has been searched for in RQ-NLS1s, but many objects have not been detected in polarized light, and none of the detected show any significant broadening of the BELs... | [
"Compare/Contrast"
] | [
[
704,
732
]
] | [
[
367,
688
]
] |
2019MNRAS.490.4975R__Neilson_et_al._2012_Instance_1 | Fig. 6 displays the MLR for the investigated CCs whose intrinsic stellar parameters were derived from the best-fitting models listed in Table 1. These data are compared with the predicted canonical (no overshooting, no mass-loss) MLR (Bono et al. 2000; the solid lines) and with the relations obtained by increasing the ... | [
"Neilson et al. 2012"
] | [
"Inclusion of mass-loss and/or rotation would produce a similar increase in the Cepheid luminosity level at fixed mass (see",
"for details)."
] | [
"Uses",
"Uses"
] | [
[
663,
682
]
] | [
[
540,
662
],
[
684,
697
]
] |
2017MNRAS.472..876O__Rodono_et_al._1985_Instance_1 | Leitzinger et al. (2014) briefly compared the mass estimates of stellar mass ejection events and the estimated X-ray energies of their associated flares with the solar scaling. We extend their comparison here. Specifically, we consider the events observed as blueshifted extra emissions in Balmer lines on the active M d... | [
"Rodono et al. 1985"
] | [
"Doing so, we find EX ≈ EU ∼ 2 × 1032 erg for AD Leo"
] | [
"Uses"
] | [
[
897,
915
]
] | [
[
844,
895
]
] |
2022MNRAS.510.5088B__Faisst_et_al._2017_Instance_2 | In the expectation of a relationship between the observed IRX and the rest-frame UV slope there is the assumption that the stars and dust are well mixed, which leads to the coupling of any observed reddening in the UV to the FIR emission detected (e.g. Meurer et al. 1999; Charlot & Fall 2000; Calzetti 2001). If instead... | [
"Faisst et al. 2017"
] | [
"Evidence for offset dust continuum emission relative to the rest-UV has been identified in several high-redshift Lyman-break galaxies (LBGs;"
] | [
"Compare/Contrast"
] | [
[
1368,
1386
]
] | [
[
1204,
1344
]
] |
2017ApJ...844...17P__Xie_et_al._2004_Instance_1 | Observations by a single coronagraph allow us to obtain CME 2D images projected on the plane of the sky. Using the image sequences of CME expansions, we can determine CME 2D parameters such as speed and angular width. Such observations do have some limitations, mostly the projection effect. Kwon et al. (2015) showed th... | [
"Xie et al. 2004"
] | [
"In previous studies, geometrical models based on the assumption of different cone shapes were developed to obtain CME 3D parameters from single spacecraft observations"
] | [
"Background"
] | [
[
582,
597
]
] | [
[
413,
580
]
] |
2017ApJ...850...75S__Bugaev_et_al._2016_Instance_2 | A realistic EoS that is able to reproduce the properties of compact astrophysical objects has to fulfill several requirements. The possibility of including many particle species, which is known as multicomponent character, is of crucial importance for modeling the NS interiors, which in even the simplest treatment incl... | [
"Bugaev et al. 2016"
] | [
"Analysis of the particle yields produced in relativistic A+A collisions within statistical (thermal) models, i.e., the Hadron Resonance Gas (HRG) model",
"shows the importance of the particle hard core repulsion."
] | [
"Background",
"Background"
] | [
[
923,
941
]
] | [
[
770,
921
],
[
944,
1001
]
] |
2022MNRAS.509.3599T__Du_et_al._2015_Instance_3 | 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 is estimated by $\\dot{\\mathscr {M}}=20.1\\, \\ell _{44}^{3/2}M_7^{-2}$ from the Shakura–Sunyaev disc model",
"where ℓ44 is the 5100 Å luminosity in units of $10^{44}\\, {\\rm erg\\, s^{-1}}$ and $M_7=M_{\\bullet }/10^7\\, \\mathrm{M}_{\\odot }$."
] | [
"Uses",
"Uses"
] | [
[
2039,
2053
]
] | [
[
1900,
2037
],
[
2056,
2184
]
] |
2016AandA...592A..74S__Sobolewska_&_Papadakis_(2009)_Instance_2 | In Fig. B.1 we plot the soft X-ray light curves for our candidate highly variable AGN using available X-ray data taken by the satellite missions Einstein, ROSAT, XMM, Suzaku and Swift. The count rates were obtained from different archives including HEASARC, the XMM Science Archive, the Swift UKSSDC and from our own Swi... | [
"Sobolewska & Papadakis (2009)"
] | [
"The sample of",
"showed spectral changes with observed power-law slope varying between 1.0 and 2.0 (see their Fig. 7). For a typical Galactic absorption of 3 × 1020 cm-2 the change from slope of 1.0 to 2.0 would alter our estimated fluxes by −14% (ROSAT), −13% (XMM-Newton), +7% (Swift-XRT), +76% (Suzaku), +25% (... | [
"Uses",
"Uses"
] | [
[
1049,
1078
]
] | [
[
1035,
1048
],
[
1079,
1657
]
] |
2015ApJ...805...44S__Tanaka_&_Haiman_2009_Instance_1 | Pair-instability supernovae (PI SNe) are the most energetic thermonuclear explosions known and can be detected near the edge of the observable universe. They have now been studied by several groups for their potential to probe the properties of the first stars and galaxies (Greif et al. 2008, 2010, 2011, 2012; Johnson ... | [
"Tanaka & Haiman 2009"
] | [
"They can also shed light on the origins of supermassive black holes and early cosmological reionization and chemical enrichment"
] | [
"Motivation"
] | [
[
826,
846
]
] | [
[
562,
689
]
] |
2022MNRAS.511.4946N__Orr_&_Browne_1982_Instance_1 | In the standard AGN unification theory, the anisotropic radio emission produced by relativistic jets points to a description where properties like radio morphology and radio spectral index depend on orientation. Two widely used orientation indicators in the radio regime are the (a) core-to-lobe flux density ratio (R), ... | [
"Orr & Browne 1982"
] | [
"A high R-value suggests a small viewing angle to the jet axis, while a low R-value indicates more of an edge-on view to the quasar"
] | [
"Background"
] | [
[
768,
785
]
] | [
[
614,
744
]
] |
2020AandA...639A..46B__Štverák_et_al._(2009)_Instance_5 | The linear relationship that we observe between breakpoint energy and core temperature is in line with previous measurements (e.g. McComas et al. 1992; Štverák et al. 2009), for both the halo and strahl. According to Scudder & Olbert (1979), a linear trend in the halo relation also follows under the assumption that bin... | [
"Štverák et al. (2009)"
] | [
"These findings by",
", along with the discrepancy between our calculated ratio of Ebp/kBTc = 5.5 ± 0.1 and the prediction of Ebp/kBTc = 7, suggest that the model of Scudder & Olbert (1979) requires a minor update to either the theory or to the input parameters."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1488,
1509
]
] | [
[
1470,
1487
],
[
1509,
1749
]
] |
2021AandA...654L...5P__Beaugé_&_Nesvorný_2013_Instance_1 | Armstrong et al. (2020) recently announced the discovery of TOI-849b, a planet having a size comparable to the one of Neptune (
R
pl
=
3
.
45
−
0.12
+
0.16
R
⊕
$ R_{\mathrm{pl}} = 3.45^{+0.16}_{-0.12}\,R_{\oplus} $
), but an anomalously larger mass (
M
pl
=
40
.
8
−
2.5
+
2.4
M
⊕
$ M_{... | [
"Beaugé & Nesvorný 2013"
] | [
"With such properties, TOI-849b represents one of the few planets populating the hot Neptune desert, a region on the radius-orbital distance plane characterised by a surprising deficit of Neptune-sized planets on very short orbits (e.g."
] | [
"Background"
] | [
[
1077,
1099
]
] | [
[
813,
1048
]
] |
2022AandA...657A..50G__Qian_&_Wasserburg_2003_Instance_1 | Carbon-enhanced metal-poor (CEMP) stars form an important class of metal-poor giants, sub-giants, and dwarfs, with a large fraction of them showing enhanced abundances of heavy elements (see Beers & Christlieb 2005; Frebel 2018 for a general review). Among the different types of CEMP stars, the CEMP-s stars are enriche... | [
"Qian & Wasserburg 2003"
] | [
"In Goswami et al. (2021), we present a detailed analysis and discussion on the classification criteria of CEMP stars, as well as the formation scenarios of CEMP stars put forward by different authors"
] | [
"Background"
] | [
[
940,
962
]
] | [
[
702,
901
]
] |
2022ApJ...935....7L__Takeuchi_&_Kono_2020_Instance_1 | Among the GRB empirical correlations, the Amati correlation is a very popular one, which connects the spectral peak energy in the GRB cosmological rest frame and the isotropic equivalent radiated energy (E
p
− E
iso; Amati et al. 2002; Amati 2006a, 2006b; Amati et al. 2008, 2009; Amati & Della Valle 2013). Recently, ... | [
"Takeuchi & Kono 2020"
] | [
"Recently, we proposed an improved Amati correlation",
"by using the Gaussian copula, which is a powerful statistical tool capable of describing the dependence structures between multivariate random variables, and has been applied to various fields by the astronomical community"
] | [
"Background",
"Background"
] | [
[
727,
747
]
] | [
[
310,
361
],
[
380,
602
]
] |
2021ApJ...919..140S__Bartos_et_al._2017_Instance_2 | Resonant dynamical friction may have applications beyond the relaxation of IMBHs examined in this paper. It may affect all objects in stellar clusters much more massive than the individual constituents of the disk, if present, including massive stars, stellar mass black holes (BHs), or the center of mass of massive bin... | [
"Bartos et al. 2017"
] | [
"An interesting implication is that, if BHs settle into the disk, they interact dynamically and form BH–BH binaries efficiently, and frequent dynamical interactions and gas effects drive the BHs to merger, producing gravitational waves (GWs) detectable by LIGO, VIRGO, and KAGRA"
] | [
"Background"
] | [
[
1010,
1028
]
] | [
[
703,
980
]
] |
2019AandA...631A.167D__George_et_al._2013_Instance_1 | The applicability of mid-IR and far-IR FSL as diagnostic tools of the ISM has received a boost thanks to the publication of samples of nearby galaxies observed with the infrared space observatory (ISO) and Herschel (e.g. Brauher et al. 2008; Farrah et al. 2013; Sargsyan et al. 2014; Kamenetzky et al. 2014; Cormier et a... | [
"George et al. 2013"
] | [
"Deep Herschel/SPIRE spectroscopy has also revealed a number of FSL detections, either in individual objects"
] | [
"Background"
] | [
[
1631,
1649
]
] | [
[
1478,
1585
]
] |
2019ApJ...886...34F__Sahijpal_&_Goswami_1998_Instance_1 | If the variation in 10Be/9Be ratios of CAIs reflects those episodic accretion events, 10Be/9Be ratios of CH–CB CAIs observed in this study would give important constraints on the evolution of the solar protoplanetary disk. Astronomical observations suggest that FUori-type outbursts are confined to the first few hundred... | [
"Sahijpal & Goswami 1998"
] | [
"If 26Al was introduced into the solar system at the earliest stage of the disk evolution (e.g.,",
"differences in Be–B and Al–Mg systematics between CH–CB and CV CAIs imply that the injection of 26Al have occurred between the evolutionary stages class I and class II of the solar protoplanetary disk."
] | [
"Uses",
"Uses"
] | [
[
1148,
1171
]
] | [
[
1052,
1147
],
[
1174,
1375
]
] |
2021MNRAS.504.5575K__Cohen_et_al._2018_Instance_1 | First detected as a radio source during the Vermilion River Observatory Sky Survey (Dickel et al. 1967) and the Ohio Sky Survey (Kraus 1977), OJ 287 has been studied extensively in the radio regime. Its relativistic jet is pointing at us with an average viewing angle of ∼2° (Jorstad et al. 2005; Agudo et al. 2012) and ... | [
"Cohen et al. 2018"
] | [
"The inner jet",
"and displays strong and variable radio polarization (e.g."
] | [
"Background",
"Background"
] | [
[
724,
741
]
] | [
[
547,
560
],
[
647,
704
]
] |
2017ApJ...849...52N__Merloni_&_Fabian_2002_Instance_1 | The bolometric luminosity of 3C 84 is about 0.4% of the Eddington luminosity. Thus, the accretion flow of 3C 84 is likely to be a radiatively inefficient accretion flow (RIAF: Narayan & Yi 1995) rather than a standard disk (Shakura & Sunyaev 1973). However, we note that 3C 84 has a cold (
T
e
∼
10
4
... | [
"Merloni & Fabian 2002"
] | [
"A number of theoretical studies predicted that the accretion flow components of hot geometrically thick (RIAF-like) and cold geometrically thin can coexist in either horizontal or vertical stratification (e.g.,"
] | [
"Background"
] | [
[
759,
780
]
] | [
[
527,
737
]
] |
2022MNRAS.513.1623C__Koyama,_Taruya_&_Hiramatsu_2009_Instance_1 | Two-point statistics are central to many of the leading cosmological analyses of the large-scale structure searching for deviations from ΛCDM (Simpson et al. 2013; Song et al. 2015; Amon et al. 2018; Abbott et al. 2019a; Chudaykin, Dolgikh & Ivanov 2021; Lee et al. 2022; Muir et al. 2021; Tröster et al. 2021; Vazsonyi ... | [
"Koyama, Taruya & Hiramatsu 2009"
] | [
"Two-point statistics are central to many of the leading cosmological analyses of the large-scale structure searching for deviations from ΛCDM",
"and a great deal of effort has gone into accurately modelling the non-linear matter power spectrum in modified gravity and dark energy cosmologies – a theoretical ingre... | [
"Background",
"Background"
] | [
[
587,
618
]
] | [
[
0,
141
],
[
334,
586
]
] |
2019MNRAS.482.5597A__Bergeron_&_Stasińska_1986_Instance_1 | There have been many efforts in the past that have used the optical emission lines to understand the AGN and the host galaxy properties (e.g. Baldwin, Wampler & Burbidge 1981; Tadhunter et al. 1998). While broad and high ionization lines tend to arise from the immediate vicinity of the central massive black hole, low i... | [
"Bergeron & Stasińska 1986"
] | [
"Indeed, Mg ii is known as a good tracer of high column density H i gas in damped Lyman α absorbers (e.g."
] | [
"Background"
] | [
[
677,
702
]
] | [
[
572,
676
]
] |
2020AandA...638A..34J__Hardcastle_(2018)_Instance_1 | We stress that the age values discussed here should be taken with care as they are based on simulations which rely on a number of assumptions. One of these is the magnetic field which is typically computed using the often unrealistic equipartition conditions. For example, a factor two difference in the magnetic field v... | [
"Hardcastle (2018)",
"Hardcastle (2018)"
] | [
"on the other hand explored two types of models, with ages being either uniformly distributed between 0 and 1000 Myr, or linearly distributed in log space between 1 and 1000 Myr.",
"These latter authors found that the uniform-age models efficiently explain the size and luminosity statistics of bright sources obse... | [
"Differences",
"Compare/Contrast",
"Similarities",
"Similarities"
] | [
[
748,
765
],
[
1722,
1739
]
] | [
[
766,
943
],
[
944,
1173
],
[
1678,
1721
],
[
1740,
1833
]
] |
2022MNRAS.511.2105K__Husemann_et_al._2019_Instance_2 | The calculation of mass outflow rates, especially in the ionized gas phase, have often come from measurements using integrated fibre or long-slit spectra, where several assumptions are invoked in the outflow modelling. These assumptions, briefly described here, result in ‘time-averaged global mass outflow rate’ with la... | [
"Husemann et al. 2019"
] | [
"This can be mitigated by using integral field spectroscopy (IFS) which is being increasingly used for extragalactic studies (e.g.",
"although there could still be projection effects with the IFS data."
] | [
"Background",
"Background"
] | [
[
1561,
1581
]
] | [
[
1347,
1476
],
[
1635,
1702
]
] |
2017AandA...600A..47D__Becker_2015_Instance_1 | To check for the validity of this idea, the case of some PACWBs already investigated in X-rays deserves to be examined. Some systems, such as WR 140 (Williams et al. 1990; Pollock et al. 2005) or Cyg OB2 #8A (Harnden et al. 1979; De Becker et al. 2006), are indeed known to be both well-studied PACWBs and bright thermal... | [
"De Becker 2015"
] | [
"Recently, it has been demonstrated that its thermal X-ray spectrum is dominated by the colliding-wind region in the close binary, with only a weak/moderate contribution coming from the wind-wind interaction in the wide orbit"
] | [
"Background"
] | [
[
841,
855
]
] | [
[
615,
839
]
] |
2019ApJ...883..174X__Lattimer_&_Prakash_2000_Instance_1 | Both the magnitude and slope of nuclear symmetry energy contribute to the pressure of NS matter. For example, the pressure of npe matter in NSs at β equilibrium at density ρ and isospin asymmetry δ is explicitly
2
The first term is the SNM pressure
, while the last two terms are the isospin-asymmetric pressu... | [
"Lattimer & Prakash 2000"
] | [
"It is also well known that the radius R1.4 of canonical NSs is essentially determined by the pressure at densities around ρ0 ∼ 2.5ρ0",
"while the maximum mass of NSs is determined by the pressure at higher densities reached in the core."
] | [
"Uses",
"Uses"
] | [
[
1220,
1243
]
] | [
[
1086,
1218
],
[
1246,
1346
]
] |
2018MNRAS.478.4657P__Gadotti_2011_Instance_1 | We have studied a sample of 263 LSB galaxies observed by Green Bank Telescope (Schneider et al. 1992) which are in overlap with the SDSS footprint. We have performed two-component bulge-disc decomposition of 263 galaxies in the SDSS g, r and, i bands and investigated their structural properties in detail. We have found... | [
"Gadotti 2011"
] | [
"Our findings of bulges and bars suggest a considerable on-going evolution in the local LSB galaxies and the bars might as well be playing a role in the bulge growth"
] | [
"Compare/Contrast"
] | [
[
931,
943
]
] | [
[
740,
904
]
] |
2021MNRAS.508.4429C__McClintock_et_al._1976_Instance_1 | Vela X-1 (4U 0900−40) is an eclipsing high-mass X-ray binary (HMXB) discovered during rocket borne X-ray observations in 1967 (Chodil et al. 1967). It is located at a distance of ∼2.0 kpc (Sadakane et al. 1985; Nagase 1989) in the Vela constellation. Recent estimates using Gaia data infer distance of $2.42^{+0.19}_{-0.... | [
"McClintock et al. 1976"
] | [
"A fraction of the stellar wind is captured and channelled along the strong magnetic field",
"of the neutron star on to the magnetic poles, producing regular X-ray pulsations caused by the spin period ∼283 s",
"of the neutron star."
] | [
"Background",
"Background",
"Background"
] | [
[
1696,
1718
]
] | [
[
1377,
1466
],
[
1552,
1665
],
[
1720,
1740
]
] |
2021ApJ...920..145H__Damone_et_al._2018_Instance_3 | Over the past decade, many attempts to address this issue have been carried out, such as from the perspective of conventional nuclear physics and even exotic physics beyond the standard BBN framework (Angulo et al. 2005; Cyburt et al. 2008, 2016; Boyd et al. 2010; Pospelov & Pradler 2010; Fields 2011; Kirsebom & Davids... | [
"Damone et al. 2018"
] | [
"Recent experiments for key nuclear reactions like 7Be(n,p)7Li and 7Be(d,p)24He allow for a reduction of the 7Li production by about 12%",
"compared to previous calculations."
] | [
"Differences",
"Differences"
] | [
[
2364,
2382
]
] | [
[
2227,
2362
],
[
2403,
2437
]
] |
2015AandA...584A.103S__Potekhin_et_al._2013_Instance_3 | Douchin & Haensel (2001; DH) formulated a unified EoS for NS on the basis of the SLy4 Skyrme nuclear effective force (Chabanat et al. 1998), where some parameters of the Skyrme interaction were adjusted to reproduce the Wiringa et al. calculation of neutron matter (Wiringa et al. 1988) above saturation density. Hence, ... | [
"Potekhin et al. 2013"
] | [
"We shall adopt here the EoS of the BSk21 model",
"as a representative example of contemporary EoS for the complete NS structure,"
] | [
"Uses",
"Uses"
] | [
[
1785,
1805
]
] | [
[
1675,
1721
],
[
1828,
1906
]
] |
2022ApJ...929..186L__Lanzoni_et_al._2013_Instance_1 | Our group is addressing this problem by combining a variety of complementary perspectives: (i) by constructing a new generation of high-quality star density profiles derived from star counts instead of surface brightness (see Lanzoni et al. 2007a, 2010, 2019; Miocchi et al. 2013; Pallanca et al. 2021); (ii) by investig... | [
"Lanzoni et al. 2013"
] | [
"Our group is addressing this problem by combining a variety of complementary perspectives:",
"(iii) by characterizing the three-dimensional (3D) global velocity space through the analysis of the velocity dispersion profile and rotation curve from resolved star spectroscopy"
] | [
"Uses",
"Uses"
] | [
[
793,
812
]
] | [
[
0,
90
],
[
612,
791
]
] |
2016MNRAS.455.4426V__Smith_&_Dwek_1998_Instance_1 | It is interesting that the tracers of atomic and molecular hydrogen become maximum at distances ∼0.85 kpc, where no dust cloud is inferred from the Swift/XRT data (see Fig. 5). A fiducial dust cloud at the distance of ∼0.85 kpc would produce an X-ray ring with angular size ∼9 arcmin on MJD 57205.5. As this would fall w... | [
"Smith & Dwek 1998"
] | [
"A dust cloud composed by large grains ( ∼ 1 μm) would suppress the scattered intensity even at 1 keV, while it would significantly attenuate X-rays at ≤0.5 keV (e.g."
] | [
"Uses"
] | [
[
678,
695
]
] | [
[
512,
677
]
] |
2019AandA...624A..60L__Dubernet_et_al._2016_Instance_1 | One of the main uncertainties in elemental abundances is the quality of the adopted atomic data used in spectral synthesis calculations (Bigot & Thevenin 2008). The Belgian repository of fundamental atomic data and stellar spectra (BRASS) aims to provide astronomers with quality information for the large amount of atom... | [
"Dubernet et al. 2016"
] | [
"Previously, we retrieved and cross-matched a large quantity of atomic data from several major atomic databases such as the",
"and providers within the Virtual Atomic and Molecular Data Centre (VAMDC;",
"in preparation for quality assessment work"
] | [
"Uses",
"Uses",
"Uses"
] | [
[
886,
906
]
] | [
[
519,
641
],
[
812,
885
],
[
909,
951
]
] |
2020ApJ...897..177P__Lister_et_al._2019_Instance_1 | Relativistic jets are the manifestation of the extreme processes that occur within the central regions of galaxies (see Blandford et al. 2019 for a review). Active galactic nuclei (AGNs) hosting relativistic jets closely aligned to the line of sight are called blazars. Due to their peculiar orientation, the relativisti... | [
"Lister et al. 2019"
] | [
"A few examples are",
"and superluminal motion and high brightness temperature"
] | [
"Background",
"Background"
] | [
[
791,
809
]
] | [
[
489,
507
],
[
709,
764
]
] |
2020MNRAS.493.4868L__Lazarian_&_Hoang_2007b_Instance_1 | Recently, polarized (sub)millimetre emission has been detected in an increasing number of discs by Atacama Large Millimeter/submillimeter Array (ALMA) with its high sensitivity and angular resolution. However, the origin of disc polarization remains uncertain, since grains do not have to be aligned with just the magnet... | [
"Lazarian & Hoang 2007b"
] | [
"They may also be aligned in the direction of",
"or the drift velocity of the grains relative to the ambient gas"
] | [
"Background",
"Background"
] | [
[
588,
610
]
] | [
[
370,
414
],
[
497,
560
]
] |
2021MNRAS.504.4626K__Kraljic_et_al._2020b_Instance_4 | Galaxies seem to retain a memory of their spin orientation with respect to the cosmic web filaments and walls, as suggested by the results from large-scale cosmological hydrodynamical simulations (Dubois et al. 2014; Codis et al. 2018; Wang et al. 2018; Ganeshaiah Veena et al. 2019; Kraljic, Davé & Pichon 2020b). The m... | [
"Kraljic et al. 2020b"
] | [
"In addition to the stellar mass, the spin-filament alignment was shown to depend on other internal properties of galaxies. Blue or rotation-supported galaxies were found to dominate the alignment signal at low stellar mass, while red or dispersion-dominated galaxies tend to show a preferential perpendicular alignm... | [
"Background"
] | [
[
1950,
1970
]
] | [
[
1593,
1911
]
] |
2017ApJ...839...26D__Conroy_et_al._2006_Instance_1 | One might hope that these global observations would strongly constrain the SFHs of individual galaxies, but this connection is not easily established. For example, average SFHs can be inferred by integrating the main sequence SFR over time (e.g., Leitner 2012), but this approach leads to inconsistencies (Leja et al. 20... | [
"Conroy et al. 2006"
] | [
"Instead, the most successful theoretical models link the growth of stellar mass to the growth of the dark matter halos that galaxies inhabit, for example, via subhalo abundance matching (e.g.,"
] | [
"Background"
] | [
[
540,
558
]
] | [
[
325,
517
]
] |
2020ApJ...891..111K__Howe_&_Burrows_2015_Instance_1 | To explore magma effects on sub-Neptune atmospheres, we assume the atmosphere equilibrates with a well-stirred magma ocean. Our model makes the following simplifications: (a) we consider only the elements Fe, Mg, Si, O, and H. Chemically reduced carbon compounds may also contain H; for simplicity, we omit consideration... | [
"Howe & Burrows 2015"
] | [
"This Tmai is at the low end of the Tmai output by thermal evolution models for multi-Gyr-old sub-Neptunes (e.g.,"
] | [
"Compare/Contrast"
] | [
[
803,
822
]
] | [
[
661,
773
]
] |
2017ApJ...848..126S__Luo_et_al._2017_Instance_1 | In Figure 2, we show the Chandra 0.3–8 keV images with SDSS contours overlaid for the six mergers in our sample. In Table 4 we list the number of counts detected in the 0.3–8 keV and 2–8 keV bands, and list the detection threshold, PB, associated with each position. There are a number of PB thresholds employed in the l... | [
"Luo et al. 2017"
] | [
"Based on weak sources in Chandra deep field images, the threshold for PB adopted based on a balance between reliability and completeness varies from 0.002 to 0.007"
] | [
"Uses"
] | [
[
559,
574
]
] | [
[
371,
534
]
] |
2021MNRAS.507.5053E__Johnston_et_al._2006_Instance_2 | Multiwavelength observations of the GC indicate that the number of pulsars in the central few parsecs should be high (Wharton et al. 2012) and conditions are highly favourable for relativistic binaries (Faucher-Giguère & Loeb 2011). The dense nuclear star cluster surrounding Sgr A* (see e.g. Genzel, Eisenhauer & Gilles... | [
"Johnston et al. 2006"
] | [
"Alternatively, the scarcity of detected pulsars might be caused by a more complex scattering structure towards the GC"
] | [
"Background"
] | [
[
1929,
1949
]
] | [
[
1764,
1881
]
] |
2017ApJ...844...14L__Lim_et_al._2016_Instance_1 | In order to see whether the CN- and HK′-strong stars in our study are also enhanced in Fe and s-process elements, we have compared our results with high-resolution spectroscopy by M15. In Figure 4, our δCN and δHK′ indices are plotted with [Na/Fe] and [Ca/Fe] abundances, respectively, for 33 common stars. In general, t... | [
"Lim et al. 2016"
] | [
"The upper panel of Figure 4 also shows a strong correlation between [Na/Fe] and the δCN index, which is in good agreement with previous studies"
] | [
"Similarities"
] | [
[
662,
677
]
] | [
[
497,
640
]
] |
2019MNRAS.485.4841R__Creminelli_et_al._2010_Instance_2 | Although, the standard form of Press–Schechter mass function with $f(\nu)=\sqrt{{2}/{\pi }} \nu \mathrm{ e}^{-\frac{\nu }{2}}$ which discussed in Press & Schechter (1974) and Bond et al. (1991) can provide a good approximation of the predicted number density of haloes, it fails by predicting approximation too many low-... | [
"Creminelli et al. 2010"
] | [
"Thus, in clustered DE scenarios, we should consider the contribution of perturbated DE components to the total mass of the haloes"
] | [
"Uses"
] | [
[
2272,
2294
]
] | [
[
2141,
2270
]
] |
2015AandA...576L..16P__Chandler_&_Sjouwerman_2014_Instance_1 | To constrain the size of outflows that we could have missed, we performed simple simulations. We placed artificial, unipolar secondary sources next to a primary point source model representing Sgr A* and compared the closure phases obtained from the resulting artificial visibility data with the observations. We conside... | [
"Chandler & Sjouwerman 2014"
] | [
"We used total fluxes of 0.2 Jy and 0.55 Jy for the artificial sources; these values ensure that our simulated outflows are sufficiently faint to not violate the constraints given by the known recent brightness evolution of Sgr A* (0.2 Jy from the mean variability of ≈15% from June 2013 to February 2014 at 41 GHz, ... | [
"Uses"
] | [
[
1065,
1091
]
] | [
[
676,
1064
]
] |
2015ApJ...798..104S___2000_Instance_1 | The Vela Molecular Ridge Cloud-D (hereafter VMR-D) (260° â² â â² 264°; |b| â² 1°) is part of a giant molecular complex located along the Galactic plane (260° â² â â² 272°; |b| â² 3°; Murphy & May 1991) and is then well suited to represent a typical star-forming region (SFR) of our Galaxy. For this reaso... | [
"Massi et al. 2000"
] | [
"For this reason a subregion of this cloud has been the subject of many previous papers, dealing with different observational aspects of the star formation (SF), such as",
"and clustering"
] | [
"Background",
"Background"
] | [
[
623,
641
]
] | [
[
306,
474
],
[
607,
621
]
] |
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