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 |
|---|---|---|---|---|---|---|
2022AandA...662A..34D__Hyde_&_Bernardi_2009_Instance_1 | The marginalized probability for Mgal and Mhalo is shown in Fig. 6. The contours correspond to the 68% and 95% intervals and the black dot marks the position of the best model. We note that the best model is outside the 68% region of the marginalized probability. The N-dimensional likelihood near the best model forms a... | [
"Hyde & Bernardi 2009"
] | [
"The inferred mass of the galaxy (baryons) in the best model (5.4 × 1010 M⊙) is marginally consistent with the estimated stellar mass derived from the velocity dispersion – stellar mass correlation"
] | [
"Similarities"
] | [
[
1063,
1083
]
] | [
[
865,
1061
]
] |
2020ApJ...892...53A__Connolly_et_al._2018_Instance_1 | These new limits, in conjunction with the inconsistency of isotropic flux interpretations, leave no room for an astrophysical interpretation of AAEs in the context of the standard model for time windows as short as 103 s. However, it has been shown that these events can be explained using physics beyond the standard mo... | [
"Connolly et al. 2018"
] | [
"These new limits, in conjunction with the inconsistency of isotropic flux interpretations, leave no room for an astrophysical interpretation of AAEs in the context of the standard model for time windows as short as 103 s. However, it has been shown that these events can be explained using physics beyond the standa... | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
477,
497
]
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[
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[
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2020MNRAS.494.3413T__Shidatsu_&_Done_2019_Instance_2 | The existence of winds is shown by blueshifted absorption lines from highly ionized ions. These are only seen in soft state but not in hard state (Ponti et al. 2012), anticorrelated with the radio jet which is seen in the hard state but not in the soft. This was thought to be evidence that the wind was magnetically dri... | [
"Shidatsu & Done 2019"
] | [
"These simulations were tailored to the BHB system H1743−332, where there is Chandra high-resolution data in both states giving detailed spectral information on the wind or its absence"
] | [
"Uses"
] | [
[
1488,
1508
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[
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2022AandA...659A.124H__Liu_et_al._(2013b)_Instance_2 | Combining different samples from various instruments at different redshifts therefore inevitably introduces ENLR size–luminosity relations with different slopes α depending on the details of target selection and analysis approaches. Slopes ranging from α = 0.22 ± 0.04 (Greene et al. 2012), α = 0.25 ± 0.02 (Liu et al. 2... | [
"Liu et al. (2013b)"
] | [
"The slopes solely inferred from the CARS data are consistent with those reported by Greene et al. (2012) and",
"and are therefore on the shallower side of previous estimates."
] | [
"Similarities",
"Similarities"
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[
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[
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2019AandA...630A.151P__Gallerani_et_al._(2011)_Instance_1 | Capturing the full information content of the cosmic large-scale structure requires a field-based approach to infer the entire three-dimensional cosmic large-scale structure from observations. This poses a particular challenge for the analyses of Ly-α forest observations, which provide sparse inherently one-dimensional... | [
"Gallerani et al. (2011)"
] | [
"and Kitaura et al. (2012) proposed a Gibbs sampling scheme to jointly infer density and velocity fields and corresponding power-spectra.",
"However, these approaches assume matter density amplitudes to be log-normally distributed. The log-normal distribution reproduces one- and two-point statistics but fails to ... | [
"Background",
"Compare/Contrast"
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[
613,
636
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2016AandA...586A..16B__Mol_&_Defrise_(2004)_Instance_1 | The problem we are facing consists in the reconstruction of two maps of a given region of an astrophysical object: the former consists in point sources, such as stars, of very high intensity, the latter of smooth structures surrounding these sources. The standard approach, i.e. simply solving Eq. (2), fails since the p... | [
"De Mol & Defrise (2004)"
] | [
"Hence, the main idea is to consider the object x as the sum of two components, namely x = xP + xE, where xP represents the point sources and xE the extended source. This approach was proposed for the first time in",
"assuming that the positions of the point sources are known."
] | [
"Uses",
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[
621,
644
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646,
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2022ApJ...926..155S__Umehata_et_al._2017_Instance_1 | However, the sensitivity limits of most current submillimeter surveys only allow for the study of the most extremely star-bursting systems (e.g., Asboth et al. 2016; Geach et al. 2017; Simpson et al. 2019), which may represent merely a tip of an iceberg of dust-obscured star formation in the early Universe. A potential... | [
"Umehata et al. 2017"
] | [
"Several ALMA blind surveys have been performed and allowed to detect and characterize the faint SMGs across cosmic times (e.g.,"
] | [
"Background"
] | [
[
830,
849
]
] | [
[
642,
769
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2018ApJ...860...24P__Warmuth_2015_Instance_2 | Figure 13 shows the temporal evolution of the density, ρ, plasma flow velocity, vx, position of the wave crest, PosA, phase speed, vw, and magnetic field component in the z-direction, Bz, for the primary waves in every different case of initial amplitude, ρIA. In Figure 13(a), we observe that the amplitude of the densi... | [
"Warmuth 2015"
] | [
"One can see that the larger the initial amplitude, ρIA, the stronger the decrease of the primary wave’s amplitude, which is consistent with observations"
] | [
"Similarities"
] | [
[
922,
934
]
] | [
[
729,
881
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] |
2018ApJ...866...93L___2012c_Instance_1 | Interestingly, from ∼11:33:40 UT, the PAD of the suprathermal electrons changes to cigar type, in association with a dramatic drop of electron flux (Figure 2(a)). This change of electron PAD and flux is related to a magnetic dip structure that is manifested by a conspicuous decrease of the magnetic field strength (Figu... | [
"Fu et al.",
"2012c"
] | [
"The observed electron cigar distribution and the associated magnetic dip are a strong indication of the betatron cooling effect. This betatron-mediated cigar distribution has been suggested in previous studies",
"but never clearly observed. These observations, for the first time, show a direct link between the c... | [
"Similarities",
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[
776,
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[
793,
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565,
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2018AandA...616L...2K__Frew_et_al._(2016)_Instance_1 | The distances to planetary nebulae (PNe) have always faced the difficulty that nearby targets were lacking that could be reached well by direct methods. Trigonometric parallaxes have been obtained in a homogeneous long time-line campaign by the US Naval Observatory (USNO; Harris et al. 2007) and from the Hubble Space T... | [
"Frew et al. (2016)"
] | [
"Another model-independent method for distances to PNe are a cluster membership, as studied extensively by Majaess et al. (2007, 2014), and as discussed in"
] | [
"Background"
] | [
[
731,
749
]
] | [
[
576,
730
]
] |
2019MNRAS.489.4669S__Bigiel_et_al._2010_Instance_2 | In Fig. 7 we compare UGC 1378’s SFR density versus gas surface density (the Schmidt–Kennicutt relation) to data in the literature. The gas surface density corresponds to H i calculated from the 0th moment map from Mishra et al. (2017) in the same areas as SFR density. Points for the HSB and LSB discs are plotted as bla... | [
"Bigiel et al. 2010"
] | [
"Similar deviations are observed in",
"outer parts of HSB spiral galaxies"
] | [
"Similarities",
"Similarities"
] | [
[
1862,
1880
]
] | [
[
1719,
1753
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[
1826,
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]
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2022ApJ...928...51B__Yadav_et_al._2016_Instance_1 | Relatively few such global convective dynamo studies have been conducted in the domain of M-dwarf stars. Early work by Browning (2008) considering lower mass FC M dwarfs found that the deep CZ could support very strong nonaxisymmetric fields, which strongly quenched the star’s differential rotation. Later, more turbule... | [
"Yadav et al. 2016"
] | [
"A still slower rotating model",
"built large-scale, axisymmetric, cycling magnetic fields of somewhat lower amplitude which did not eliminate the star’s differential rotation, reminiscent of the distributed αΩ-type dynamos prevalent in solar-like contexts."
] | [
"Background",
"Background"
] | [
[
801,
818
]
] | [
[
770,
799
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[
820,
1043
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] |
2017ApJ...836L...4S__Scholer_&_Burgess_2007_Instance_2 | At quasi-perpendicular shocks, the average shock structure is dominated by a foot of reflected ions, which is upstream of the shock ramp where the major thermalization and deceleration occurs. Non-stationarity in the form of rippling of the surface or steepened whistler waves (Moullard et al. 2006; Lobzin et al. 2007) ... | [
"Scholer & Burgess 2007"
] | [
"kinetic instabilities such as the Buneman and modified two-stream instability (e.g.,"
] | [
"Background"
] | [
[
1111,
1133
]
] | [
[
943,
1027
]
] |
2016AandA...588A..25M__Weiss_&_Ferguson_2009_Instance_1 | There are some indications that available models of the post-AGB and CSPN phases are not accurate enough. First, the two available grids of post-AGB models (Vassiliadis & Wood 1994; Blöcker 1995a) do not agree with each other on the predicted timescales (Zijlstra et al. 2008). Second, consistency between the masses of ... | [
"Weiss & Ferguson 2009"
] | [
"Lastly, post-AGB stellar evolution models, computed with updated physics in a reduced mass range",
"show a strong disagreement with the previous grids."
] | [
"Differences",
"Differences"
] | [
[
737,
758
]
] | [
[
624,
720
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[
761,
812
]
] |
2019AandA...628A.110M__Kryukova_et_al._(2012)_Instance_2 | 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)"
] | [
"Starting from our completeness limit at 22 μm, after conservatively dereddening it by AV = 20, we assumed a spectral index γ = −2 (see Table 3 for definition) to compute the MIR luminosity from Eq. (6) of"
] | [
"Uses"
] | [
[
1400,
1422
]
] | [
[
1195,
1399
]
] |
2020ApJ...903....6M__Bueno_2010_Instance_1 | In this paper, we consider resonance scattering on a two-level atom with an infinitely sharp and unpolarized lower level. As for the frequency redistribution, we consider both CRD and angle-averaged PRD. In an unmagnetized one-dimensional spherically symmetric atmosphere, the polarized radiation field is axially symmet... | [
"Sampoorna & Trujillo Bueno 2010"
] | [
"From here on we present all the basic equations in the irreducible basis (see",
"for details)."
] | [
"Uses",
"Uses"
] | [
[
1006,
1037
]
] | [
[
928,
1005
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[
1038,
1051
]
] |
2015MNRAS.450..763M__Rieke_et_al._2004_Instance_1 | In this work, we focus on the 56 most massive (M* ≥ 1011 M⊙) galaxies at 1.4 ≤ z ≤ 2, 31 of which have spectroscopic redshifts. Two more objects entered the original sample, but they have been excluded from this study, because their WFC3/HST images are not available, or too noisy to perform SB fitting, due to the proxi... | [
"Rieke et al. 2004"
] | [
"The optical/near-IR photometry was then complemented with the 24 μm catalog",
", built as summarized in Section 2.1 from the Multi-Band Imaging Photometer for Spitzer (MIPS) images"
] | [
"Uses",
"Uses"
] | [
[
958,
975
]
] | [
[
749,
824
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[
855,
956
]
] |
2018MNRAS.473.2000T__Noutsios_et_al._2011_Instance_2 | The launch of the Fermi Gamma-ray Space Telescope has spurred on the search for pulsars in γ-rays (Grenier & Harding 2015), yielding over 2001 detections and triggering multiwavelength observations. While pulsars are common targets in the X-rays, they are very challenging targets in the optical and very few of them hav... | [
"Noutsios et al. 2011"
] | [
"Such a distance would make PSR J2043+2740 a viable target for deep optical observations, never carried out until now, and might be compatible with the debated association"
] | [
"Motivation"
] | [
[
2383,
2403
]
] | [
[
2211,
2381
]
] |
2017AandA...607A...9M__Weideman_1994_Instance_1 | Having a line list that is as complete as possible is crucial for doing proper radiative transfer computations in high temperature atmospheric environments. However, computing the line opacities for a large number of lines can be computationally challenging. For example, the ExoMol line list of CH4 contains on the orde... | [
"Weideman 1994"
] | [
"Computing the exact pressure and temperature broadened Voigt profile for each of these lines is computationally extremely demanding. There are several approximate methods for computing Voigt profiles available in the literature (e.g."
] | [
"Background"
] | [
[
614,
627
]
] | [
[
365,
598
]
] |
2019MNRAS.490.2155S__Blake_et_al._2016_Instance_1 | Modern optical imaging surveys measure the positions and ellipticities of millions of galaxies; from them, the galaxy overdensity field as well as the gravitational lensing shear field can be derived. The two-point auto and cross-correlations of these two fields are the two-point correlation functions of cosmic shear, ... | [
"Blake et al. 2016"
] | [
"Among the latter, Joudaki et al. (2018) recently performed a combined analysis of cosmic shear tomography, galaxy–galaxy lensing tomography, and redshift space multipole power spectra using data from KiDS-450 (∼450 deg2 of cosmic shear data from the KiDS survey) and two overlapping spectroscopic surveys, the 2-deg... | [
"Background"
] | [
[
1133,
1150
]
] | [
[
782,
1132
]
] |
2016AandA...596A..59F__Sobotka_et_al._1993_Instance_1 | Sunspot light bridges can be formed by the fragmentation of the umbra in the decay phase or during the merging of different magnetized areas during the formation of the sunspot in complex active regions (Bray & Loughhead 1964; Garcia de La Rosa 1987). At the last stages of a sunspot, the photospheric-like conditions ar... | [
"Sobotka et al. 1993",
"Sobotka et al. 1993"
] | [
"Previous studies have classified light bridges based on their morphological properties. Light bridges separating two umbral regions are called strong light bridges (e.g.,",
"Their brightness is similar to that of the penumbra, and they typically appear between two regions with the same polarity. Faint light brid... | [
"Background",
"Background",
"Background"
] | [
[
870,
889
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[
1101,
1120
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[
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[
1122,
1260
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2021AandA...655A..12T__Tang_et_al._2017b_Instance_5 | Using the RADEX3 non local thermodynamic equilibrium (LTE) modeling program (van der Tak et al. 2007) with collisional rate coefficients from Wiesenfeld & Faure (2013), we modeled the relation between the gas kinetic temperature and the measured average of para-H2CO 0.5 × [(322–221 + 321–220)/303–202] ratios, adopting ... | [
"Tang et al. (2017b)"
] | [
"Following the method applied by",
"in their Eq. (2), we plot the relation between the LTE kinetic temperature, TLTE, and the para-H2CO (3–2) line ratio in Fig. 5."
] | [
"Uses",
"Uses"
] | [
[
1558,
1577
]
] | [
[
1526,
1557
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[
1578,
1705
]
] |
2021ApJ...907...15H__Geiss_1982_Instance_1 | Figure 2 shows the ratios of the relative fluences (element/Mg) measured in Genesis bulk SW (Figure 2(a)) and regime targets (Figure 2(b)) after normalization to the respective solar abundance ratios (Table 7 in Appendix A.5). The bulk SW data for K and Fe in silicon (marked by asterisks in Figure 2(a)) are the prelimi... | [
"Geiss 1982"
] | [
"The bulk SW shows a fractionation of elemental abundances correlating with FIP, as previously observed by spacecraft (e.g.,",
"However, the better accuracy and element coverage of Genesis data compared to in situ measurements allows further insights into this FIP-related fractionation."
] | [
"Similarities",
"Compare/Contrast"
] | [
[
637,
647
]
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[
513,
636
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[
665,
824
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2022MNRAS.517.4986G__Chambers_1999_Instance_1 | Wang et al. (2017), motivated by the fact that previous studies on high-eccentricity migration focused only on the total efficiency of HJs formed, analyzed the efficiency of each high-eccentricity mechanism, trying to understand which mechanism is the dominant one in HJ formation. They considered multiplanetary systems... | [
"Chambers 1999"
] | [
"Their numerical simulations were performed using the classical version of the Mercury code",
"which does not include general relativity (GR) effects and tidal interaction with the central star. They studied how the initial number of planets, the spatial separation between them, and the location of the inner plan... | [
"Motivation",
"Motivation"
] | [
[
719,
732
]
] | [
[
627,
717
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[
735,
1434
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] |
2018AandA...620A..46M__Bergin_et_al._2000_Instance_1 | Astrochemical models have always dedicated special attention to molecular oxygen. With a cosmic abundance twice that of C, atomic O is the third most abundant element in space. In dense clouds, standard gas phase chemical models therefore suggest a comparable ratio of CO and O2 after times ≥ 3 × 105 yr (e.g. Woodall et... | [
"Bergin et al. 2000"
] | [
"Better agreement with observations can be obtained if freeze-out of O atoms onto dust grains is taken into account in gas-grain chemical models",
", with consequence surface production of H2O and O2, which may trap a significant fraction of oxygen, leaving only some atomic O and CO in the gas phase."
] | [
"Motivation",
"Motivation"
] | [
[
994,
1012
]
] | [
[
849,
992
],
[
1031,
1184
]
] |
2015MNRAS.451.4328K__Coddington_1994_Instance_1 | We estimate the DPL parameters in equation (9) via Monte Carlo simulations. We compare the real structure function of an AGN to simulations computed from mock light curves generated using the DPL model of equation (9). We generate ‘mock’ light curves using the Timmer & König (1995) method. To create a single mock light... | [
"Coddington 1994"
] | [
"To create a single mock light curve, pseudo-random numbers are generated using the Fast Mersenne Twister SFMT19937 generator seeded with hardware-generated random numbers (generated using Intel RDRAND instruction) to ensure that the random number sequences are free of artificial correlations",
"induced by poor r... | [
"Uses",
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] | [
[
585,
600
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] | [
[
291,
583
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[
602,
638
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2016MNRAS.461.1719C__Fu_et_al._2012_Instance_3 | 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"
] | [
"The submm photometry of HATLAS12-00 at 890 μm acquired with the Submillimeter Array (SMA) as part of this programme",
"is fully consistent with the 870 μm and 850 μm fluxes derived for this source from the LABOCA and SCUBA2 data to be presented here."
] | [
"Similarities",
"Similarities"
] | [
[
1503,
1517
]
] | [
[
1386,
1501
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[
1541,
1672
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2020AandA...635A..47H___2005_Instance_1 | Finally, the multiphase nature of galactic outflows implies that measurements of the outflow properties based on a single gas phase can lead to misleading conclusions (for a discussion, see e.g., Cicone et al. 2018b). Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on th... | [
"Rupke et al.",
"2005"
] | [
"Historically, systematic studies of galactic outflows in nearby and high-z galaxies have focused on the ionized gas",
"and the atomic phase – based on the Na D or Mg II lines in absorption (e.g."
] | [
"Background",
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[
680,
692
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[
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703
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[
218,
333
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[
582,
657
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2022AandA...663A.105P__Finoguenov_et_al._2010_Instance_1 | Cluster radio relics are usually found in the outskirts of merging galaxy clusters. They exhibit elongated morphologies and high degrees of polarisation above 1 GHz (up to 70%, Ensslin et al. 1998; Bonafede et al. 2014; Loi et al. 2019; de Gasperin et al. 2022). The resolved spectral index in radio relics shows a gradi... | [
"Finoguenov et al. 2010"
] | [
"Relics trace ICM shock waves with relatively low (M 3) Mach numbers"
] | [
"Background"
] | [
[
894,
916
]
] | [
[
823,
892
]
] |
2019MNRAS.490.3061V__Myers_2009_Instance_1 | On the other hand, the line-shift-absence conundrum of ZP74 is easily explained through geometrical considerations. Essentially, the arguments leading to this conundrum assume that the collapse is roughly spherically symmetric and monolithic, so that the infall motions are coherent, and directed towards a single collap... | [
"Myers 2009"
] | [
"This assumption is inconsistent with our current understanding of the structure of MCs, which are known to be far from spherically symmetric, and instead consist of an intricate and inhomogeneous network of filaments and clumps within them (e.g."
] | [
"Differences"
] | [
[
717,
727
]
] | [
[
371,
616
]
] |
2019AandA...630A..98S__Cenko_et_al._2012a_Instance_1 | The close approach of a star to a supermassive black hole (SMBH) can lead to the destruction of the stellar body in a process known as a tidal disruption event (TDE; Hills 1975). Gravitationally bound material returns to the black hole and is accreted, giving rise to a flare whose electromagnetic signature peaks in the... | [
"Cenko et al. 2012a"
] | [
"In recent years, large-area optical surveys have detected candidate TDEs emitting at temperatures of a few ×104 K"
] | [
"Background"
] | [
[
881,
899
]
] | [
[
742,
855
]
] |
2017ApJ...835..154H__Lee_et_al._2014_Instance_1 | The simplest explanation for these metal abundances, i.e., that they reflect the yields of normal core-collapse SNe (averaged over the stellar initial mass function (IMF)), fails to predict anything like the observed stellar abundances of the extremely metal-poor stars ([Fe/H] −3). Of course, at these low metallicitie... | [
"Lee et al. 2014"
] | [
"However, even with these degrees of freedom, the models still often fail to explain the abundances of certain individual species at the order-of-magnitude level (see, e.g.,",
", although they undoubtedly explain many of the observed abundance ratios."
] | [
"Differences",
"Similarities"
] | [
[
880,
895
]
] | [
[
665,
837
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[
916,
990
]
] |
2015MNRAS.446.1140T__Murray_et_al._2010_Instance_2 | Recently, forms of feedback that are fundamentally different from SNe have been shown to be essential to galaxy formation. Murray, Quataert & Thompson (2010) analysed the dynamical effects of several forms of stellar feedback on parent molecular clouds. In their models they include momentum input from ionized gas in H ... | [
"Murray et al. 2010"
] | [
"A variety of other studies have reached the same conclusions, placing the combination of RP and photoionization of gas by massive stars as the dominant mechanism for disruption of molecular clouds and internal regulation of the SF process"
] | [
"Background"
] | [
[
843,
861
]
] | [
[
554,
792
]
] |
2015ApJ...799..149J___2014_Instance_3 | With our joint analysis of stellar mass fraction and source size, we find a larger stellar mass fraction than earlier statistical studies. In Figure 2, we compare our determination of the stellar surface density fraction to a simple theoretical model and to the best fit of a sample of lens galaxies by Oguri et al. (2... | [
"Oguri et al. (2014)"
] | [
"as well as the best model using a Hernquist component for the stars and an NFW halo for the dark matter with and without adiabatic contraction, also from"
] | [
"Uses"
] | [
[
1193,
1213
]
] | [
[
1039,
1192
]
] |
2021MNRAS.502.1312C__Recchia,_Blasi_&_Morlino_2016_Instance_1 | The dynamical importance of CRs is even more uncertain. This is in part because most early work on this question focused only on galactic conditions similar to those found locally (Jokipii 1976; Badhwar & Stephens 1977; Ghosh & Ptuskin 1983; Chevalier & Fransson 1984; Boulares & Cox 1990; Ko, Dougherty & McKenzie 1991;... | [
"Recchia, Blasi & Morlino 2016"
] | [
"More recent numerical and analytic models have continued in this vein (e.g.",
"rather than address the question of whether CRs represent a significant contribution to the support of the neutral material that dominates the total mass budget and occupies at least $\\sim 50{{\\ \\rm per\\ cent}}$ of the volume",
... | [
"Background",
"Background",
"Background"
] | [
[
975,
1004
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] | [
[
715,
790
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[
1086,
1311
],
[
1337,
1356
]
] |
2021ApJ...919..140S__Bartos_et_al._2017_Instance_1 | 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"
] | [
"Previously, it has been argued that stars and BHs crossing the disk on low-inclination orbits get captured by Chandrasekhar dynamical friction into the disk"
] | [
"Background"
] | [
[
639,
657
]
] | [
[
481,
637
]
] |
2015AandA...573A.138B__Deubner_(1975)_Instance_1 | Solar-like oscillations are excited stochastically by motions in the convective envelope of stars. For low-mass stars, they are found in all evolutionary states, between the main sequence and horizontal branch of helium-core burning stars (e.g. Leighton et al. 1962; Frandsen et al. 2002; Carrier et al. 2003; Hekker et ... | [
"Deubner (1975)"
] | [
"It was shown by",
"that this ridge structure is governed by the degree of oscillation modes and resembles the predictions made by Ando & Osaki (1975)."
] | [
"Background",
"Background"
] | [
[
617,
631
]
] | [
[
601,
616
],
[
632,
763
]
] |
2017AandA...606A.113G__Carollo_et_al._(2013)_Instance_2 | In this context, massive (ℳ>1011 M⊙) PGs (MPGs) deserve particular attention. These systems are expected to evolve mainly through (dry) mergers (e.g. Hopkins et al. 2009; De Lucia & Blaizot 2007). If this is the case, in this mass range we should detect a stronger signal of the size-growth with respect to a lower mass ... | [
"Carollo et al. (2013)"
] | [
"found that the number density of massive quiescent and elliptical galaxies with Re 2.5 kpc decreases by about 30% from z~1 to z~0.2 and that their U−V colours are consistent with passive evolution. They concluded that the driving mechanism for the average size-growth of the whole population is the appearance at la... | [
"Background"
] | [
[
571,
592
]
] | [
[
593,
948
]
] |
2022MNRAS.515.2914E__Lada_&_Lada_2003_Instance_1 | Also addressing the evolution of a stellar cluster is work by Parker & Goodwin (2009) and Parker et al. (2009) in which N-body simulations are used to analyse the prevalence of planets susceptible to the Kozai effect from a binary companion, and the stability of binaries in a dense cluster environment respectively. Par... | [
"Lada & Lada 2003"
] | [
"This is not typical for embedded clusters, which have typical half mass radii of ∼0.8 pc",
", and therefore would have less frequent interactions between cluster stars and a particular binary."
] | [
"Differences",
"Differences"
] | [
[
1059,
1075
]
] | [
[
969,
1057
],
[
1076,
1176
]
] |
2020MNRAS.495.4508E__Heinke_et_al._2014_Instance_1 | Several qLMXBs have been identified in GCs and in the Galactic field (for some examples, see table 4 in Guillot et al. 2009 and references therein). While LMXBs in the field were detected following the onset of a bright accretion outburst, most qLMXBs in GCs, including all those with the highest flux at Earth, have not... | [
"Heinke et al. 2014"
] | [
"Previous works have confirmed that H-atmosphere models accurately describe the spectra of qLMXBs, with radii in the range 10–15 km, as expected for NSs, either from single sources (e.g."
] | [
"Background"
] | [
[
764,
782
]
] | [
[
505,
690
]
] |
2022MNRAS.511.5797M__Liu_&_Lai_2019_Instance_1 | A variety of formation channels have been proposed for binary black holes (BBHs; see e.g. Mapelli 2021 for a recent review): BBH mergers can be the outcome of isolated binary evolution via common envelope (Tutukov & Yungelson 1973; Bethe & Brown 1998; Portegies Zwart & Yungelson 1998; Belczynski, Kalogera & Bulik 2002;... | [
"Liu & Lai 2019"
] | [
"Alternatively, BBHs can form dynamically in",
"multiples (e.g."
] | [
"Background",
"Background"
] | [
[
1132,
1146
]
] | [
[
898,
941
],
[
1092,
1107
]
] |
2015AandA...584A..76S__Bernstein_et_al._(1995)_Instance_2 | 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)"
] | [
"Since in the experiment by",
"the ice was irradiated by VUV photons at the Lyman alpha wavelength, and we now know that methanimine can be efficiently ionized by those photons, we can also argue that ionization of several methanimine molecules can instead trigger the process in cold interstellar ices."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2260,
2283
]
] | [
[
2233,
2259
],
[
2284,
2556
]
] |
2020MNRAS.498.1319M__MacGregor_et_al._2017_Instance_1 | While most systems with exo-Kuiper belts do not have known planetary mass companions, in a few of these it has been possible to directly image one, thus enabling the study of planet–disc interactions in more detail. There are well-known examples such as β Pic with a massive planet possibly warping the disc (Mouillet et... | [
"MacGregor et al. 2017"
] | [
"While most systems with exo-Kuiper belts do not have known planetary mass companions, in a few of these it has been possible to directly image one, thus enabling the study of planet–disc interactions in more detail. There are well-known examples such as",
"and Fomalhaut having a narrow and eccentric planetesimal... | [
"Background",
"Background"
] | [
[
887,
908
]
] | [
[
0,
253
],
[
757,
818
]
] |
2017AandA...599A..97H__Gratton_et_al._2012_Instance_1 | Amongst the oldest stellar systems known to exist in the Milky Way (MW) are metal-poor globular clusters (GCs). These accumulations of stars do not seem to have undergone substantial star formation for extended periods. Given the limited quality of the available data, for a long time color-magnitude diagrams (CMDs) of ... | [
"Gratton et al. 2012"
] | [
"Moreover, in recent years evidence has grown supporting the statement that GCs are generally composed of two or three chemically distinct populations. These subpopulations are separated by a few tens to hundreds of Myr in age and show vastly varying abundances of light elements such as C, N, O, Na, Mg, and Al (see... | [
"Background"
] | [
[
1342,
1361
]
] | [
[
996,
1318
]
] |
2022MNRAS.516.6194C__Tran_et_al._2001_Instance_1 | In this paper, we focus on the bright elliptical galaxy NGC 5813. This is the central dominant member of a subgroup, hereafter referred to as the NGC 5813 group with an extensive diffuse X-ray emission. While part of the well-isolated NGC 5846 group ($z$ = 0.006578; e.g. Mahdavi, Trentham & Tully 2005a; Machacek et al.... | [
"Tran et al. 2001"
] | [
"NGC 5813 itself has been assumed to be dynamically old",
"with no evidence of a recent major merger in its history, as indicated by the lack of any significant disturbances to its dusty circumnuclear disc"
] | [
"Background",
"Background"
] | [
[
648,
664
]
] | [
[
422,
476
],
[
500,
646
]
] |
2018AandA...620A..80M__Coutens_et_al._2018_Instance_2 | The comparison with other hot corinos is not easy since we have a limited number of lines, in contrast to well-known sources that have been more extensively observed with ALMA and NOEMA, such as IRAS 16293-2422 (Jørgensen et al. 2016), NGC1333 IRAS 2A and 4A (Taquet et al. 2015; López-Sepulcre et al. 2017). In general,... | [
"Coutens et al. 2018"
] | [
"These values are in the range of those observed towards the molecular clouds in the Galactic centre but lower than in Orion KL"
] | [
"Compare/Contrast"
] | [
[
1066,
1085
]
] | [
[
938,
1064
]
] |
2020MNRAS.497L..56Y__Verde,_Treu_&_Riess_2019_Instance_1 | Over the past decade, direct measurements of the Hubble constant have achieved few percent in precision (Freedman 2017). Among the conducted measurements, the Supernova H0 for the Equation of State (SH0ES) team challenged the well-believed Hubble constant (H0) value inferred from the Planck cosmic microwave background ... | [
"Verde, Treu & Riess 2019"
] | [
"To come to a robust conclusion, independent H0 probes with accuracy better than $2{{\\ \\rm per\\ cent}}$ are crucial"
] | [
"Motivation"
] | [
[
1257,
1281
]
] | [
[
1141,
1255
]
] |
2022MNRAS.517.2801W__Gallo_et_al._2014_Instance_2 | During the X-ray ‘hard’ state, the radio and X-ray behaviour of BHXBs is correlated and has been studied in depth for many sources using quasi-simultaneous observations (e.g. Corbel et al. 2003; Gallo, Fender & Pooley 2003; Coriat et al. 2011; Corbel et al. 2013), and is known as the radio:X-ray plane. It was thought t... | [
"Gallo et al. 2014"
] | [
"The underlying cause of the split tracks (see",
"for a clustering analysis into the statistical robustness of this split) for BHXBs is not known"
] | [
"Background",
"Background"
] | [
[
1341,
1358
]
] | [
[
1266,
1311
],
[
1400,
1495
]
] |
2016ApJ...818..141V__Sellwood_2014b_Instance_1 | Historically, the study of orbits in potentials has focused on periodic orbits. In systems like disk galaxies small perturbations to closed periodic orbits (e.g., the epicyclic and vertical perturbations of circular orbits) provided a good analytic description of most orbits. Self-consistent distribution functions are ... | [
"Sellwood 2014b"
] | [
"The retrograde x4 (stable) orbit family is also elongated perpendicular to the bar at small radii, but becomes rounder as it extends to larger radii (for detailed description of orbit families and how they are identified see",
"In the frame of reference rotating with the bar, all of these families are characteri... | [
"Background",
"Background"
] | [
[
1144,
1158
]
] | [
[
840,
1064
],
[
1161,
1362
]
] |
2020MNRAS.498.2575W__Tampo_et_al._2020_Instance_1 | The sample of DES RETs shows a preference for low-metallicity, strongly star-forming host environments. The PDF of their metallicities displays a strong similarity to the hosts of SESNe, as well as LGRBs. There is a clear difference to the PDF of SNe II, which follow SDSS field galaxies. The preference for low-metallic... | [
"Tampo et al. 2020"
] | [
"The approximate rate of RETs (≥10−6 Mpc−3 yr−1"
] | [
"Uses"
] | [
[
986,
1003
]
] | [
[
875,
921
]
] |
2019MNRAS.485..189O__Ogiya_&_Mori_2014_Instance_1 | Finally, we emphasize that although the parameter space covered by the DASH library is vast, it is by no means exhaustive. One obvious shortcoming, as discussed above, is that the DASH simulations are inadequate to describe major mergers with ${\cal M}\lesssim 100$. In those cases, dynamical friction due to the host, a... | [
"Ogiya & Mori 2014"
] | [
"Such cores can be created within the CDM paradigm by a variety of baryonic processes (e.g."
] | [
"Background"
] | [
[
976,
993
]
] | [
[
804,
894
]
] |
2021MNRAS.507.4316B__Tan_et_al._2014_Instance_1 | One of the main debates in the star formation community is whether the massive young stellar objects are a scaled-up version of low-mass young stellar objects (YSOs) where disc-accretion plays the dominating role for gaining the stellar mass. For the formation of low-mass stars, bipolar outflows driven by the accretion... | [
"Tan et al. 2014"
] | [
"However, on the other hand, understanding of the formation mechanism of massive stars is still elusive"
] | [
"Background"
] | [
[
651,
666
]
] | [
[
547,
649
]
] |
2019AandA...630A..26M__Wozniakiewicz_et_al._(2012)_Instance_1 | The majority of the particles collected by Stardust are olivine and pyroxene silicates with solar isotopic compositions, which suggests an origin in our solar system rather than an interstellar provenance. These polymineralic particles dominate those made of a single mineral even down to sizes smaller than 100 nm, indi... | [
"Wozniakiewicz et al. (2012)"
] | [
"Price et al. (2010) and",
"investigated the sizes of particles smaller than 10 μm that impacted the aluminum foils of the Stardust probe. The distribution peaks at about 175 nm, but if we assume that the particles areagglomerates of smaller subunits, as indicated by their common polymineralic nature, then the su... | [
"Uses",
"Uses"
] | [
[
791,
818
]
] | [
[
767,
790
],
[
819,
1161
]
] |
2019MNRAS.484.3307M__Hobbs_et_al._2005_Instance_1 | For most of our models, we can already determine, or at least extrapolate, the final neutron star properties quite well, barring the possibility of late-time fallback. Except for the $12.5 \, \mathrm{M}_\odot$ model, mass outflow already dominates over mass accretion on to the PNS, and the PNS mass has practically stab... | [
"Hobbs et al. 2005"
] | [
"while the models with higher He core masses are compatible with the typical kicks of young pulsars"
] | [
"Compare/Contrast"
] | [
[
1328,
1345
]
] | [
[
1191,
1289
]
] |
2016ApJ...827...31F__Lu_&_Yuan_1998_Instance_1 | While treated as fully relativistic under strong gravity, we note that the current model is time-independent based on axisymmetric plasma. This assumption makes it impossible for us to predict any temporal nature of the soft excess considered in this work, e.g., spectral time variabilities associated with shock compres... | [
"Lu & Yuan 1998"
] | [
"A more realistic shock process, on the other hand, is most likely accompanied by radiative cooling to some degree in which the post-shock plasma temperature may stay comparatively as cool as that of the upstream one, as in the isothermal shocks (e.g.,"
] | [
"Differences"
] | [
[
883,
897
]
] | [
[
631,
882
]
] |
2019ApJ...885...93F__McClintock_et_al._2006_Instance_1 | The vertical structure of an accretion disk has been investigated in detail by Abramowicz et al. (1997). A general accurate expression for the vertical hydrodynamical equilibrium that is valid both for a thin and a slim disk has been derived in their work. The hydrostatic balance in the vertical direction of the accret... | [
"McClintock et al. 2006"
] | [
"It has been pointed out that the widely used approximation for the vertical component of gravity, GMz/R3, is only valid for the thin disk with H/R ≪ 1, and a more accurate expression of vertical gravity should be adopted for a slim disk"
] | [
"Compare/Contrast"
] | [
[
1152,
1174
]
] | [
[
914,
1150
]
] |
2017AandA...605A..88L__Ceccarelli_et_al._2000_Instance_1 | Altogether, the approximately thirty molecules recently detected have confirmed the chemical complexity in the nebula, and generated our interest for the present study. Of these species, we will focus our attention on the seventeen species listed by molecular families in Table 1. As can be seen in this table, the WHISP... | [
"Ceccarelli et al. 2000"
] | [
"Because they are detected in a wide variety of interstellar sources – in hot cores",
"it is of prime importance to understand well how these precursor molecules form."
] | [
"Motivation",
"Motivation"
] | [
[
746,
768
]
] | [
[
642,
724
],
[
956,
1036
]
] |
2016MNRAS.458.3760S__Pettini_et_al._1994_Instance_1 | Plots of various characteristics of sub-DLAs and DLAs in the literature. Blue star points mark the detections presented in this work. The Xs mark detections from Péroux et al. (2011a, 2012). The points mark detections from previous studies in the literature. References: Pettini et al. 2000, Lacey et al. 2003, Junkkarin... | [
"Pettini et al. 1994"
] | [
"The points mark detections from previous studies in the literature. References:"
] | [
"Uses"
] | [
[
945,
964
]
] | [
[
191,
270
]
] |
2020AandA...639A..48S__Shulyak_et_al._2004_Instance_1 | In order to predict emission and transmission spectra of HJs we utilized the τ-REx (Tau Retrieval for Exoplanets) software package (Waldmann et al. 2015b,a). This package uses up-to-date molecular cross sections based on line lists provided by EXOMOL6 project (Tennyson & Yurchenko 2012) and HITEMP (Rothman et al. 2010)... | [
"Shulyak et al. 2004"
] | [
"All relevant numerical routines were extracted from the LLMODELS stellar model atmosphere code"
] | [
"Uses"
] | [
[
1650,
1669
]
] | [
[
1554,
1648
]
] |
2021MNRAS.507.4389G__Masters_et_al._2011_Instance_1 | Erwin (2018) showed that, in a sample drawn from the Spitzer Survey of Stellar Structure in Galaxies (S4G), the bar fraction is constant over a range of (g −r) colours and gas fractions. Their bar fraction does not increase, but rather decreases for stellar masses higher than ∼ 109.7M⊙. These results are in contrast to... | [
"Masters et al. (2011)"
] | [
"Nevertheless, the ‘combined’ bar fraction in Fig. 6 is not constant over (g −r) colour and agrees well with",
"for redder colours [(g −r) colour > 0.5]"
] | [
"Similarities",
"Similarities"
] | [
[
717,
738
]
] | [
[
609,
716
],
[
739,
779
]
] |
2015ApJ...814...73S__Soria_et_al._2004_Instance_1 | At a distance of 4.8 Mpc (Karachentsev et al. 2002), NGC 5408 X-1 is one of the best studied ULXs. It has been observed by several of the current generation of X-ray satellites, on a multitude of occasions. Observations include: an XMM-Newton large programme (e.g., Pasham & Strohmayer 2012); Swift XRT monitoring (Kaare... | [
"Soria et al. 2004"
] | [
"The flux variability of the source rules out an X-ray supernova remnant and confirms that it is powered by accretion onto a compact object"
] | [
"Compare/Contrast"
] | [
[
570,
587
]
] | [
[
410,
548
]
] |
2015AandA...579A..46M__Ilyushin_et_al._2010_Instance_1 | The Hamiltonian used in the present work is the so-called RAM (rho axis method) internal-rotation Hamiltonian based on the work of Kirtman (Kirtman 1962), Lees and Baker (Lees & Baker 1968), and Herbst et al. (Herbst et al. 1984). Since rather complete descriptions of this method, which takes its name from the choice o... | [
"Ilyushin et al. 2010"
] | [
"As for the main isotopolog",
"we employed the RAM36 (rho-axis-method for 3- and 6-fold barriers) code that uses the RAM approach for the molecules with the C3v top attached to a molecular frame of Cs or C2v symmetry and having 3- or 6-fold barriers to internal rotation, respectively"
] | [
"Uses",
"Uses"
] | [
[
1210,
1230
]
] | [
[
906,
932
],
[
955,
1208
]
] |
2021MNRAS.500.2336Y__Matonick_&_Fesen_1997_Instance_2 | Various surveys of SNRs in our Galaxy and nearby galaxies have been carried out at radio, X-ray, Infrared (IR), and optical wavelengths. The first extragalactic SNR candidates were identified in the LMC by Mathewson & Healey (1964) and later confirmed with a combination of radio and optical techniques by Westerlund & M... | [
"Matonick & Fesen 1997"
] | [
"Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S ii]/H α > 0.4–0.5"
] | [
"Background"
] | [
[
1264,
1285
]
] | [
[
1041,
1171
]
] |
2022AandA...658A.194P__Khata_et_al._2020_Instance_3 | The stellar photospheric parameters we collected from literature for the benchmark stars are summarized in Table A.1. Although most benchmark stars have v sini 2 km s−1 (Reiners et al. 2018), there are two stars with larger values: J07558+833 (12.1 km s−1) and J13005+056 (16.4 km s−1). These stars are useful to invest... | [
"Khata et al. 2020"
] | [
"the stellar radius and Teff"
] | [
"Background"
] | [
[
1837,
1854
]
] | [
[
1808,
1835
]
] |
2020AandA...644A..97C__Leroy_et_al._2013_Instance_3 | Major nearby galaxy cold gas mapping surveys (Regan et al. 2001; Wilson et al. 2009; Rahman et al. 2011; Leroy et al. 2009; Donovan Meyer et al. 2013; Bolatto et al. 2017; Sorai et al. 2019; Sun et al. 2018) have focused on observations of the molecular gas (through CO lines). Despite a few notable exceptions (e.g. Ala... | [
"Leroy et al. 2013"
] | [
"In some galaxies, the depletion time in the centres appear shorter"
] | [
"Background"
] | [
[
1756,
1773
]
] | [
[
1688,
1754
]
] |
2022MNRAS.515.2698A__In_2018_Instance_1 | In the last few years, similar (though not identical) experimental developments to our method have been reported. In 2017, Wehres et al. (2017) described the design, construction, and operation of two laboratory broad-band emission spectrometers for gas-phase characterization of large molecules. The first is based on a... | [
"Tanarro et al. (2018)"
] | [
"In 2018, a new technique combining a Terahertz radiometer (41–49) GHz and a vacuum chamber was developed to observe the generation of cold plasma and UV photochemistry in the gas phase under low pressure as described by",
"However, in the context of the experiment described here, it is important to note that the... | [
"Background",
"Differences"
] | [
[
922,
943
]
] | [
[
702,
921
],
[
945,
1153
]
] |
2022AandA...665A..25C__Lambrechts_&_Johansen_2012_Instance_1 | Various theoretical studies employing numerical simulations have been performed to investigate planet formation through core accretion or gravitational instability in the low-stellar-mass regime. Payne & Lodato (2007) assessed planet formation around brown dwarfs adapting models for higher stellar masses based on core ... | [
"Lambrechts & Johansen 2012"
] | [
"Pebble accretion is a mechanism able to speed up significantly the giant planet formation process (i.e.,"
] | [
"Background"
] | [
[
777,
803
]
] | [
[
672,
776
]
] |
2021MNRAS.505..435S__Deming_et_al._2013_Instance_1 | Detections of ionic, atomic, and molecular species in exoplanetary atmospheres serve as a unique and strong diagnostic of those chemical and dynamical processes driving their formation and evolution. Their detection and abundance measurements could act as indicators of planetary formation scenarios and reveal connectio... | [
"Deming et al. 2013"
] | [
"A whole host of ions, atoms, and molecules have been detected through a variety of, often complementary, techniques, such as differential spectrophotometry using low-to-mid resolution spectroscopy (e.g."
] | [
"Background"
] | [
[
1109,
1127
]
] | [
[
880,
1082
]
] |
2021AandA...655A.104P__Draine_&_Li_2007_Instance_1 | This last, more technical aspect gave birth to a branch of research devoted to the problem of fitting a galaxy SED (Arnouts et al. 1999; Bolzonella et al. 2000; Cid Fernandes et al. 2005; Ilbert et al. 2006; Ocvirk et al. 2006; Tojeiro et al. 2007; Fritz et al. 2007, 2017; Franzetti et al. 2008; Pappalardo et al. 2010;... | [
"Draine & Li 2007"
] | [
"Historically, models reproducing the evolution of stellar populations and dust emission have been developed separately,",
"and a thorough comprehension of dust grains physics on the other"
] | [
"Background",
"Background"
] | [
[
934,
950
]
] | [
[
376,
495
],
[
791,
855
]
] |
2017ApJ...850...97B__Tamburro_et_al._2009_Instance_1 | 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"
] | [
"Velocity dispersions in dwarf galaxies can be on the order of the rotational velocity, ∼10–15 km s−1 (e.g.,"
] | [
"Compare/Contrast"
] | [
[
968,
988
]
] | [
[
834,
941
]
] |
2021ApJ...923L..22A__Dvorkin_&_Barausse_2017_Instance_1 | Pulsar timing experiments (Sazhin 1978; Detweiler 1979) allow us to explore the low-frequency (∼1–100 nHz) part of the gravitational-wave (GW) spectrum. By measuring deviations from the expected arrival times of radio pulses from an array of millisecond pulsars, we can search for a variety of GW signals and their sourc... | [
"Dvorkin & Barausse 2017"
] | [
"Orbiting SMBHBs produce a stochastic GW background (GWB"
] | [
"Background"
] | [
[
781,
804
]
] | [
[
484,
539
]
] |
2021ApJ...921..107B__Bellovary_et_al._2021_Instance_1 | A black hole mass this large in Leo I is not expected from extrapolation of any of the standard black hole−host galaxy correlations. Of course, these small systems do not necessarily need to follow the trends seen in normal galaxies, but the black hole mass reported here does stand out. Lützgendorf et al. (2015) explor... | [
"Bellovary et al. 2021"
] | [
"On the numerical side, van Wassenhove et al. (2010) consider different scenarios for formation of a black hole in Milky Way satellites and place the likelihood of one of them having a black hole around the size found here to be below 1%, but this result also depends on the initial seed mass (see also"
] | [
"Compare/Contrast"
] | [
[
824,
845
]
] | [
[
522,
823
]
] |
2016AandA...592A.157M__Mernier_et_al._2015_Instance_1 | As seen in Fig. 6 (right), the large MOS-pn discrepancy in the Ni/Fe abundance ratio prevents us from deriving a precise measurement. This discrepancy is worrying, but can be explained by imperfections in the cross-calibration of the two instruments. Alternatively, and perhaps more likely, the high energy band around t... | [
"Mernier et al. 2015"
] | [
"In particular, an instrumental line (Cu Kα) is known to affect pn at a rest-frame energy of ~8 keV",
"Despite our efforts to carefully estimate the background, that line might interfere with the Ni-K line in several observations, making a proper modelling of the Ni-K line impossible, and hence, boosting the Ni a... | [
"Uses",
"Uses"
] | [
[
739,
758
]
] | [
[
639,
737
],
[
761,
996
]
] |
2020AandA...643A..93H__Lin_et_al._2016a_Instance_1 | In recent years, type Ia supernovae (SNe Ia; Amanullah et al. 2010; Suzuki et al. 2012; Betoule et al. 2014; Scolnic et al. 2018) have been widely employed to test cosmic isotropy. Antoniou & Perivolaropoulos (2010) searched for the preferred direction of anisotropy for the Union2 sample by adopting the hemisphere comp... | [
"Lin et al. 2016a"
] | [
"Since then, these two methods have been widely used to explore the cosmic anisotropy",
"by investigating observational data of, for instance, the Union2.1 sample"
] | [
"Background",
"Background"
] | [
[
1038,
1054
]
] | [
[
689,
773
],
[
921,
994
]
] |
2018MNRAS.473.3810Y__Mitrushchenkov_et_al._2017_Instance_1 | The lack of data on inelastic processes due to collisions with neutral hydrogen atoms has been a major limitation on modelling of F-, G- and K-star spectra in statistical equilibrium, and thus to reliably proceeding beyond the assumption of local thermodynamic equilibrium (LTE) in analysis of stellar spectra and the de... | [
"Mitrushchenkov et al. 2017"
] | [
"Significant progress has been made in recent times through detailed full-quantum scattering calculations, based on quantum chemical data, for the cases of simple atoms such as Li, Na, Mg and Ca"
] | [
"Background"
] | [
[
797,
823
]
] | [
[
461,
654
]
] |
2019MNRAS.482.3803P__Schaerer_&_Vacca_1998_Instance_1 | The broad blue WR bump feature around 4686 Å was searched in all the star-forming regions in the galaxies. A clear detection of the broad blue WR bump was made only in two star-forming regions hosted by SBS 1222+614 as shown in Fig. 8. This detection is in good agreement with Shirazi & Brinchmann (2012), who have also ... | [
"Schaerer & Vacca 1998"
] | [
"The blue bump appears mainly due to the presence of late-type WN (WNL) and early-type WC (WCE) stars"
] | [
"Background"
] | [
[
744,
765
]
] | [
[
642,
742
]
] |
2020AandA...640A.133R___et_al._2017_Instance_1 | The full sample for which the circumstellar CO line emission will be modeled consists of the ∼180 C-, M-, and S-type AGB stars analyzed in Schöier & Olofsson (2001), González Delgado et al. (2003), and Ramstedt et al. (2006) together with additional sources presented in Danilovich et al. (2015). In this initial paper, ... | [
"Samus’ et al. 2017"
] | [
"The M-type sample consists of the non-Mira stars from the General Catalog of Variable Stars (GCVS;",
"with quality flag 3 in the IRAS 12, 25, and 60 μm bands and 60 μm flux ≳3 Jy"
] | [
"Uses",
"Uses"
] | [
[
1138,
1156
]
] | [
[
1039,
1137
],
[
1158,
1234
]
] |
2021MNRAS.504.2168G__Steiner_et_al._2011_Instance_1 | Finally, we attempt to characterize the reflection component using the full 2–35 keV spectra with a sophisticated model [M4: ${\tt{\rm constant}}$*${\tt{\rm TBabs}}$*(${\tt{\rm simplr}}$*${\tt {\rm kerrbb2}}$+${\tt{\rm kerrconv}}$*(${\tt{\rm ireflect}}$*${\tt{\rm simplc}}$)), to evaluate the impact on the spin measurem... | [
"Steiner et al. 2011"
] | [
"This model features a self-consistent treatment of the thermal, Compton scattering and the reflection component: ${\\tt {\\rm kerrbb2}}$ describes the thermal component and supplies the seed photons for ${\\tt{\\rm simplr}}$ (a modified version of ${\\tt{\\rm simpl}}$,",
"to generate the Compton component;"
] | [
"Uses",
"Uses"
] | [
[
690,
709
]
] | [
[
426,
689
],
[
711,
745
]
] |
2019MNRAS.484.1100M__Dekel_&_Birnboim_2006_Instance_1 | The stream velocity is proportional to the halo virial velocity, which can be related to the sound speed of gas at the virial temperature, yielding Mb ∼ 1. The density contrast is obtained by assuming pressure equilibrium between hot gas at Tb ∼ Tv, the virial temperature of an NFW halo, and cold gas at Ts ∼ 104K, set ... | [
"Dekel & Birnboim 2006"
] | [
"while the post-shock temperature in the hot halo near Rv may only be ∼0.5Tv",
", P18)."
] | [
"Uses",
"Uses"
] | [
[
726,
747
]
] | [
[
649,
724
],
[
747,
754
]
] |
2021AandA...653A..36M__Goulding_&_Alexander_(2009)_Instance_3 | 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)"
] | [
"It is worth noting that the original samples from",
"and Bernard-Salas et al. (2009) have spectra solely covering the central region of the galaxies."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1359,
1386
]
] | [
[
1309,
1358
],
[
1387,
1483
]
] |
2018AandA...613A...7Y__Kostogryz_et_al._(2016)_Instance_1 | where a is the area of the i, j pixel (constant for a regular grid), μ is the anglebetween the surface normal and the line of sight to the observer, ϕ is the polar angle of a system with the origin at the disk center, F is the total stellar flux, and q and u are normalized Stokes parameters. We note that the relative f... | [
"Kostogryz et al. (2016)"
] | [
"The center-to-limb variations ofintensity I(μij) and polarization P(μij) were found through trilinear interpolation using the look-up tables from Kostogryz & Berdyugina (2015) and",
", according to the selected wavelength, surface gravity, and temperature of a star."
] | [
"Uses",
"Uses"
] | [
[
581,
604
]
] | [
[
401,
580
],
[
604,
687
]
] |
2019MNRAS.484..814G__Tápai,_Zoltán_&_László_2015_Instance_1 | There are many methods, beyond those already employed here, that can be used to identify, and probe the masses of, black holes. This includes reverberation mappings of AGNs (e.g. Bahcall, Kozlovsky & Salpeter 1972; Blandford & McKee 1982; Netzer & Peterson 1997), the ‘fundamental plane of black hole activity’ (Merloni ... | [
"Tápai, Zoltán & László 2015"
] | [
"The Kamioka Gravitational Wave Detector",
"will be a 3-km-long underground interferometer in Japan capable of detecting the gravitational radiation emanating from collisions involving black holes with masses up to 200 M⊙"
] | [
"Background",
"Background"
] | [
[
1330,
1357
]
] | [
[
1086,
1125
],
[
1151,
1328
]
] |
2016ApJ...831...11S__Honeycutt_1992_Instance_1 | The secondary eclipses of the binary are 0.03–0.04 mag deep, and so relatively small data reduction issues can have large effects on the fidelity of the light curve. Our brightness measurements were derived from aperture photometry using DAOPHOT (Stetson 1987), although we took several additional steps to increase the ... | [
"Honeycutt 1992"
] | [
"We then attempted to unify the data for each filter to a consistent zero point by using ensemble photometry",
"This essentially uses all measured stars on the frame to determine magnitude offsets resulting from differences in exposure time, airmass, atmospheric transparency, and the like. Our implementation iter... | [
"Uses",
"Background"
] | [
[
653,
667
]
] | [
[
521,
628
],
[
670,
992
]
] |
2018AandA...615A.161M__Hartmann_1904_Instance_1 | δ Ori Aa+Ab = Mintaka Aa+Ab = 34 Ori Aa+Ab = HD 36486 A+B = BD −00 983 A+B = ALS 14 779 A+B. δ Ori is Orion’s Belt westernmost star and a multiple system at the center of the Mintaka cluster (Caballero & Solano 2008). It has two close bright visual components (Aa and Ab) and two distant dim ones (B and C) that will not... | [
"Hartmann 1904"
] | [
"Aa is itself composed of two spectroscopic components (Aa1+Aa2) in an eclipsing orbit with a5.7325 d period, while Ab is two magnitudes fainter than the two Aa components and located 0.′′ 267 away in 1993 and moving away from the primary"
] | [
"Background"
] | [
[
580,
593
]
] | [
[
341,
578
]
] |
2019MNRAS.489.4669S__Bigiel_et_al._2010_Instance_1 | In Fig. 7 we compare UGC 1378’s SFR density versus gas surface density (the Schmidt–Kennicutt relation) to data in the literature. The gas surface density corresponds to H i calculated from the 0th moment map from Mishra et al. (2017) in the same areas as SFR density. Points for the HSB and LSB discs are plotted as bla... | [
"Bigiel et al. 2010"
] | [
"We also plot the SFR in the outer regions of spiral galaxies",
"square symbols)."
] | [
"Uses",
"Uses"
] | [
[
916,
934
]
] | [
[
854,
914
],
[
936,
952
]
] |
2021MNRAS.508.2019B__Gürkan_et_al._2018_Instance_1 | Assuming that non-jetted H ii galaxies are powered by SF, the relation between radio luminosities in such galaxies and MBH can be deciphered as a link between thermal/non-thermal SF luminosity and BH mass, in the form $L_{\rm SF} \propto M_{\rm BH}^{0.61}$, which has the largest scatter of the observed linear regressio... | [
"Gürkan et al. 2018"
] | [
"This unprecedented relation is likely the result of the observed link found between SF indicators such as radio, far-infrared, optical or line luminosities, and galaxy mass"
] | [
"Uses"
] | [
[
621,
639
]
] | [
[
421,
593
]
] |
2020ApJ...896..169P__Dullemond_&_Dominik_2004_Instance_1 | Pre-main-sequence stars are typically surrounded by protoplanetary disks, and since such disks are generally highly optically thick at optical/near-infrared (NIR) wavelengths, they may cast shadows on their surroundings. Such disk shadows have been observed on a wide range of angular scales; recently, high-contrast ima... | [
"Dullemond & Dominik 2004"
] | [
"Such shadows reveal that angular distortions are common in inner disks. This is consistent with the existence of a class of self-shadowed disks in which the inner disk scale height is higher than that of the outer disk, leading to a general shadowing and related cooling of the outer disk"
] | [
"Similarities"
] | [
[
776,
800
]
] | [
[
486,
774
]
] |
2021MNRAS.501.3781R___2017_Instance_2 | While spatially extended optical jets and bipolar CO molecular outflows have been observed in numerous Class 0/I protostars (e.g. Reipurth & Bally 2001; Bally 2016, and references therein), near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study ... | [
"Antoniucci et al.",
"2017"
] | [
"The mass accretion and loss rates for Class 0/I low-mass protostars span the range of 10−6–10−8 M⊙ yr−1, and the derived jet efficiencies (ratio between mass ejection and accretion rates) range between ∼1 per cent and 10 per cent (e.g.",
"These measurements are within the range predicted by the magnetohydrodynam... | [
"Background",
"Similarities"
] | [
[
1887,
1904
],
[
1917,
1921
]
] | [
[
1543,
1778
],
[
1956,
2053
]
] |
2021ApJ...916...57G__Gedalin_2017_Instance_1 | Collisionless shocks are one of the most ubiquitous phenomena in space plasmas. The directed flow energy is converted into other forms at the shock front: ion and electron heating, particle acceleration, and magnetic field enhancement. One of the most important problems of the collisionless shock physics is prediction ... | [
"Gedalin 2017"
] | [
"On larger scales or for measurements invoking substantial temporal and/or spatial averaging, the distributions become gyrotropic but can still remain anisotropic, since isotropization may be slow. The corresponding RH should take into account this anisotropy"
] | [
"Background"
] | [
[
1833,
1845
]
] | [
[
1557,
1815
]
] |
2020ApJ...899....4X__Zhou_et_al._2019_Instance_1 | It is also very encouraging to note that recent analyses of heavy-ion reaction experiments in terrestrial laboratories and properties of NSs from multiple messengers have led to some new progress in constraining the Esym(ρ) up to about twice the saturation density. For example, shown in Figure 1 are the values of symme... | [
"Zhou et al. 2019"
] | [
"For example, shown in Figure 1 are the values of symmetry energy at 2ρ0, that is, Esym(2ρ0), from",
"(6)",
"analyses of NS radii, tidal deformability, and maximum mass within an extended Skyrme Hartree–Fock approach (eSHF)",
"Despite the rather different assumptions and methods used in analyzing the differen... | [
"Uses",
"Uses",
"Uses",
"Similarities"
] | [
[
1184,
1200
]
] | [
[
266,
363
],
[
1032,
1035
],
[
1050,
1164
],
[
1517,
1830
]
] |
2017ApJ...834..135T__Zolotov_et_al._2015_Instance_1 | To explain the morphological transformation, two main evolutionary paths have been proposed in the literature. A slow cosmological path naturally follows from the strong redshift evolution of galaxy sizes,
(Mosleh et al. 2012; Newman et al. 2012; van der Wel et al. 2014b; Shibuya et al. 2015). Star-forming galax... | [
"Zolotov et al. 2015"
] | [
"A second, fast path involves a downward transition in the mass–size plane, at approximately constant redshift",
"This process requires a substantial “compaction” of the formally extended star-forming galaxies."
] | [
"Background",
"Background"
] | [
[
636,
655
]
] | [
[
478,
587
],
[
658,
754
]
] |
2018ApJ...865...22C__Criscuoli_et_al._2013_Instance_1 | The strong linearity between the two indices shown in Figure 5 must be ascribed to their strong temperature dependence and to the proximity of the Mg ii core and FUV formation heights on one side, and Mg ii continuum and MUV on the other. Most of the radiation contributing to the FUV and MUV originates in the higher ph... | [
"Criscuoli et al. 2013"
] | [
"In LTE, a linear dependence of the core/wing ratio is expected (e.g.,",
"but such dependence is probably less obvious for the Mg ii h and k line, whose cores form in NLTE conditions."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1244,
1265
]
] | [
[
1174,
1243
],
[
1268,
1377
]
] |
2021ApJ...923..105L__Owens_et_al._2013_Instance_2 | For the purpose of this study, we adopt the general concept that the global solar wind is generally composed of relatively steady high-speed solar winds from long-lived high latitude open coronal field regions. The high-speed solar winds from the northern and southern hemispheres are separated by a layer of—on average—... | [
"Owens et al. 2013"
] | [
"Weaker solar cycles and advanced imaging and modeling capabilities have raised the profile of pseudostreamers and their boundaries as contributors to the outflows within this slow wind layer"
] | [
"Motivation"
] | [
[
2877,
2894
]
] | [
[
2667,
2857
]
] |
2015ApJ...799...55G__Rosenvinge_et_al._2008_Instance_1 | We use data from instruments on board STEREO-A, STEREO-B, ACE, SOHO, Wind, the Geostationary Operational Environmental Satellites (GOES), MESSENGER and the Solar Dynamics Observatory (SDO). Remote-sensing observations of the CME and the activity phenomena over the solar surface were provided by the Sun Earth Connection... | [
"von Rosenvinge et al. 2008"
] | [
"Radio observations were provided by",
"and the High Energy Telescope"
] | [
"Uses",
"Uses"
] | [
[
1200,
1226
]
] | [
[
811,
846
],
[
1164,
1193
]
] |
2021MNRAS.507.1623C__Lesgourgues_2011_Instance_1 | To describe the H i bispectrum in redshift space, we apply the standard redshift space kernels (see Heavens et al. 1998; Scoccimarro et al. 1999 for derivations) such that
(10)$$\begin{eqnarray*}
B_\rm {H\,\small {I}}(\boldsymbol{k}_{1},\boldsymbol{k}_{2},\boldsymbol{k}_{3}) &=& 2\, \overline{T}_\rm {H\,\small... | [
"Lesgourgues 2011"
] | [
"Plin represents the real-space, linear matter power spectrum for which we use the CLASS Boltzmann solver"
] | [
"Uses"
] | [
[
915,
931
]
] | [
[
778,
882
]
] |
2017ApJ...840...91Y__Shatsky_&_Tokovinin_2002_Instance_1 | Another binary parameter is the stellar mass ratio distribution. The choice of the mass ratio can be called the pairing function, which is combining stars into binary systems. When random pairing is used (i.e., binary companions are randomly chosen from a given IMF), we find similar mass segregation results to those fo... | [
"Shatsky & Tokovinin 2002"
] | [
"When random pairing is used (i.e., binary companions are randomly chosen from a given IMF), we find similar mass segregation results to those for star clusters containing only single stars. However, random pairing is ruled out observationally, and there is also a lack of theoretical backing for a random pairing fu... | [
"Compare/Contrast"
] | [
[
499,
523
]
] | [
[
176,
497
]
] |
2020MNRAS.492..708M__Davidson_&_Fesen_1985_Instance_1 | Due to the high luminosity and seemingly long-term flux stability, the Crab pulsar and its pulsar wind nebula (PWN) is one of the most studied sources in the very high energy (VHE, $\rm {E} \gt 100$ GeV) regime. For many years, Crab has been used as a standard candle in X- and gamma-ray astronomy (Hester 2008). The Cra... | [
"Davidson & Fesen 1985"
] | [
"It has a (energy-dependent) angular size of ∼0.1° and its distance has been estimated to be ≈2.2 kpc, corresponding to a physical size of ≈3.8 pc"
] | [
"Background"
] | [
[
803,
824
]
] | [
[
642,
787
]
] |
2022ApJ...935..135B__Thomas_et_al._2019_Instance_1 | Disk galaxies typically reveal out-of-equilibrium features due to incomplete equilibration. These may appear in the form of bars and spiral arms, which are large-scale perturbations in the radial and azimuthal directions, responsible for a slow, secular evolution of the disk. In the vertical direction, disks often reve... | [
"Thomas et al. 2019"
] | [
"At large galactocentric radii (>10 kpc) this includes, among others,",
"and streams of stars kicked up from the disk that undergo phase mixing, sometimes referred to as “feathers” (e.g.,"
] | [
"Background",
"Background"
] | [
[
1044,
1062
]
] | [
[
761,
829
],
[
903,
1017
]
] |
2015AandA...574A..50J__Takeda_et_al._(2008)_Instance_1 | Several studies that analyzed the metallic content in the atmospheres of evolved stars hosting planets have been published in the last decade. The first results were based on small samples and/or the abundances were not obtained with a homogeneous technique. Schuler et al. (2005) derived the metallicity for one GWP and... | [
"Takeda et al. (2008)"
] | [
"with a sample of 322 giants, including 10 planet-hosts, did not find any metallicity offset."
] | [
"Compare/Contrast"
] | [
[
960,
980
]
] | [
[
982,
1074
]
] |
2022MNRAS.509..567S__Spinoso_et_al._2017_Instance_1 | When a galaxy is isolated, star formation quenching is mostly driven by internal processes (Larson 1974; Dekel & Silk 1986; Vulcani et al. 2021). Active galatic nuclei (AGNs) feedback create an outflow of gas preventing further hot gas accretion from the circumgalactic medium (Dalla Vecchia & Schaye 2008; Bongiorno et ... | [
"Spinoso et al. 2017"
] | [
"Bars in spiral galaxies may drive gas inflows, which enhance central star formation (bar-driven evolution;"
] | [
"Background"
] | [
[
641,
660
]
] | [
[
534,
640
]
] |
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