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 |
|---|---|---|---|---|---|---|
2019AandA...628A.110M__Kryukova_et_al._(2012)_Instance_3 | 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)"
] | [
"Equation (7) of",
"then yields Lbol ~ 1.7–2.8 L⊙, depending on whether the NIR flux is neglected (which may be the case) or extrapolated from γ = −2."
] | [
"Uses",
"Uses"
] | [
[
1440,
1462
]
] | [
[
1424,
1439
],
[
1463,
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2020MNRAS.496.3582C__Komacek_&_Showman_2016_Instance_1 | 3D General Circulation Models (GCMs) with simplified thermal forcing are one possible intermediate step between 3D GCMs with full coupling between radiation and dynamics like those used by Showman et al. (2009) and Amundsen et al. (2016), and shallow water models, i.e. atmosphere models with one atmosphere layer compri... | [
"Komacek & Showman 2016"
] | [
"They are, however, computationally much more expensive and their complexity makes it more difficult to test underlying modelling assumptions compared to GCMs with simplified thermal forcing. The latter are thus better suited to run simulations for various scenarios, to understand large-scale flow and circulation p... | [
"Compare/Contrast"
] | [
[
959,
981
]
] | [
[
502,
874
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2021ApJ...913...55H__Goldman_et_al._2017_Instance_2 | The short-plateau SNe 2006Y, 2006ai, and 2016egz most likely come from partially stripped massive progenitors,36
36
The lack of nebular spectra for SNe 2006Y and 2006ai remains a caveat.
but a remaining question is their exact formation channel. If it is single-star evolution as assumed in this work, the main theoret... | [
"Goldman et al. 2017"
] | [
"In addition, recent observational and theoretical studies on RSGs and SNe II indicate that RSG wind mass-loss rates may be independent from metallicity"
] | [
"Background"
] | [
[
988,
1007
]
] | [
[
835,
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2015ApJ...804..130C___2013_Instance_1 | We have developed the simplest spherical void lens model based on the recently developed embedded lens theory. We have assumed a uniform mass profile for the void, compensated by a thin bounding shell. The infinitesimally thin bounding shell was chosen for convenience (Maeda & Sato 1983a, 1983b). To investigate other v... | [
"Kantowski et al. 2013"
] | [
"It is also possible to build embedded void lens models with non-spherically symmetric density profiles given that the lowest-order embedded lens theory is applicable to any distributed lens"
] | [
"Background"
] | [
[
869,
890
]
] | [
[
678,
867
]
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2019ApJ...887..137S__Vekstein_2017_Instance_1 | As mentioned above, the magnetic reconnection is introduced as breaking and reconfiguration of the oppositely directed magnetic field lines in highly conducting plasma. The magnetic field lines collapse near the X-point and form an extended magnetic singularities known as a current sheet. There are two mechanism of the... | [
"Vekstein 2017"
] | [
"The first kind of current-sheet formation is associated with the MHD instabilities (e.g., resistive tearing mode and ideal kink mode) known as spontaneous magnetic reconnection (e.g.,"
] | [
"Background"
] | [
[
553,
566
]
] | [
[
346,
529
]
] |
2017AandA...606A..17M__Kennicutt_(1998)_Instance_1 | The SFR reported in Table C.1 refers to a stellar mass range from Mlow = 0.1M⊙ to Mup = 100M⊙, is averaged over the past Δt = 100 Myr, and was calculated using the standard SFR(LIR) relationship from Kennicutt (1998; here scaled to a Chabrier 2003, IMF) (1)\begin{equation} \label{eq:sfr} \textit{SFR}=10^{-10}\times L_{... | [
"Kennicutt (1998"
] | [
"he SFR reported in Table C.1 refers to a stellar mass range from Mlow = 0.1M⊙ to Mup = 100M⊙, is averaged over the past Δt = 100 Myr, and was calculated using the standard SFR(LIR) relationship from",
"here scaled to a Chabrier 2003, IMF) (1)\\begin{equation} \\label{eq:sfr} \\textit{SFR}=10^{-10}\\times L_{\\rm... | [
"Uses",
"Uses"
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[
200,
215
]
] | [
[
1,
199
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[
217,
407
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2017ApJ...835....2X___2003_Instance_1 | On the other hand, a clear physical interpretation of the observed pulse broadening phenomenon requires a good understanding of the interstellar electron density structure. A power-law model of electron density fluctuations is commonly adopted in theoretical constructions on radio wave propagation (Lee & Jokipii 1976; ... | [
"Cho & Lazarian",
"2003"
] | [
"Recent advances in understanding the properties of magnetohydrodynamic (MHD) turbulence",
"stimulate a renewed investigation on density statistics",
"which provide important insight into key physical processes such as star formation in the turbulent and magnetized ISM"
] | [
"Motivation",
"Motivation",
"Motivation"
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2018AandA...614A..86G__Hamann_et_al._(2006)_Instance_1 | In the supersonic part of WR outflows, the presence of instabilities and inhomogeneities should be taken into account. Invoking density inhomogeneities, or “clumping”, in stellar models has an influence on the mean opacity, due to the enhanced density in clumps (Moffat et al. 1988; Hamann & Koesterke 1998). However, a ... | [
"Hamann et al. (2006)"
] | [
"The surface temperatures of such hydrostatic, strongly inflated models computed with plane parallel grey atmospheres are then compared with the fictitious effective temperatures at τ = 20 of the atmosphere calculations performed by"
] | [
"Uses"
] | [
[
952,
972
]
] | [
[
720,
951
]
] |
2021MNRAS.508.4332M__Draine_1978_Instance_1 | As a first step, we need to specify the photoelectron sheath features. In this course, we first evaluate the steady state potential over the lunar surface (equation 4), and then after, we use this as a boundary condition to solve the Poisson equation (equation 2) and estimate the photoelectron sheath profile. In calcul... | [
"Draine 1978"
] | [
"Moreover, Draine’s formulation is accounted to determine the lunar surface’s photoelectric efficiency (",
") – its spectral dependence can be represented as ${\\chi _{\\nu r}} = {\\chi _o}[1 - ({\\phi _r}/{E_\\nu })]$."
] | [
"Uses",
"Uses"
] | [
[
819,
830
]
] | [
[
716,
819
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[
854,
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2015ApJ...815...15W__Dib_&_Kaspi_2014_Instance_1 | 1E 1841–045, located at the center of supernova remnant (SNR) Kes 73 (Vasisht & Gotthelf 1997), is another steady X-ray emitter. The source was monitored with NuSTAR between 2013 September 5 and 21, during which time six bursts were detected (An et al. 2015). In order to eliminate the contamination from the SNR, an ann... | [
"Dib & Kaspi 2014"
] | [
"Since the source emission has been stable for more than 15 years",
"we performed the joint fit with the longest, burst-free NuSTAR observations (ObsID = 30001025012) and XMM-Newton observations that were performed ∼11 years earlier."
] | [
"Uses",
"Uses"
] | [
[
1047,
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[
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2019MNRAS.488.5029H__Malhotra_et_al._2001_Instance_1 | For the first time, we detected [C ii] 158-μm emission from a GRB host galaxy at z > 2. This is the second detection of [C ii] 158-μm emission among known GRB host galaxies, following GRB 980425 (Michałowski et al. 2016). The [C ii] 158-μm fine structure line is the dominant cooling line of the cool interstellar medium... | [
"Malhotra et al. 2001"
] | [
"However, LC II/LFIR is not constant, but declines with increasing LFIR, known as the ‘[C ii] deficit’"
] | [
"Background"
] | [
[
943,
963
]
] | [
[
809,
910
]
] |
2016AandA...591A..38C__Roediger_et_al._(2011a)_Instance_1 | Despite the considerable scatter in both colors and color gradients (Peletier & Balcells 1996; Taylor et al. 2005; Roediger et al. 2011a), the tight correlation between color and stellar mass of the host galaxies holds true in both the region identified as intermediate and outer in Sect. 7. ETGs form a tight red sequen... | [
"Roediger et al. 2011a"
] | [
"Despite the considerable scatter in both colors and color gradients",
"the tight correlation between color and stellar mass of the host galaxies holds true in both the region identified as intermediate and outer in Sect. 7."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
115,
136
]
] | [
[
0,
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[
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2015AandA...581A..31S__Giodini_et_al._2013_Instance_1 | Although the origin and evolution of linear-scale clustering is well described by the concordance model (Spergel et al. 2007), gravitational clustering of matter on smaller scales (galaxy clusters and groups) belongs to a non-linear regime of structure formation. This regime is more difficult to understand and to simul... | [
"Giodini et al. 2013"
] | [
"Including baryon physics introduces some distortions in the scaling relations between the mass and other physical quantities such as temperature, X-ray, or optical luminosity"
] | [
"Background"
] | [
[
1007,
1026
]
] | [
[
818,
992
]
] |
2018ApJ...867..123M__Helling_&_Fomins_2013_Instance_1 | Regardless of their exact composition, particles suspended in these exoplanet environments likely undergo repeated particle–particle collisions in response to atmospheric circulation. Such dynamics have been inferred to drive efficient triboelectrification (e.g., Helling et al. 2013), resulting in electrified cloudy or... | [
"Helling & Fomins 2013"
] | [
"As happens within Earth’s clouds, exoplanet clouds are likely gravitationally stratified, meaning that smaller, lighter grains become concentrated at the top of the clouds, while larger, heavier grains remain at lower elevation"
] | [
"Uses"
] | [
[
631,
652
]
] | [
[
353,
580
]
] |
2022AandA...663A...5M__Andrae_et_al._2018_Instance_1 | With the real-time pipeline, we also frequently detect eclipsing binaries, due to their significant changes in brightness. Often, when we trigger these sources, PV light curves reveal potentially eclipsing behaviour. In these cases, we can attempt to verify the nature of the variable source by creating Lomb-Scargle per... | [
"Andrae et al. 2018"
] | [
"The source is a known source that appears in many sky survey catalogues, including Gaia, where its G-band magnitude is listed as 14.1 and its inferred temperature is ~5000 K (see",
"for how the listed temperature we extract from the Gaia catalogue is inferred from the Gaia data)."
] | [
"Uses",
"Uses"
] | [
[
977,
995
]
] | [
[
798,
976
],
[
996,
1094
]
] |
2015ApJ...815...39W__Frank_et_al._1996_Instance_1 | With improved resolution, in this work we have resolved corrugated swept-up shells as well as small blobs of mixed material in the wind region that were not seen in Paper I. The swept-up shells are much smoother in the simulations including poloidal field, which is related to the stabilization of shear instability by t... | [
"Frank et al. 1996"
] | [
"More complex and fragmented mixing structures are generated in the higher resolution simulation, which indicates that the process producing these structures is not completely resolved at the current resolution (see, e.g.,"
] | [
"Uses"
] | [
[
992,
1009
]
] | [
[
770,
991
]
] |
2021ApJ...908...95H__Sanders_&_Mirabel_1996_Instance_1 | Star-forming galaxies at redshifts z ∼ 1–3 probe the cosmic epoch when most of the stellar mass assembly in the universe took place (Madau & Dickinson 2014, and references therein). A better understanding of star formation (SF) during this epoch is therefore imperative to understand SF across cosmic time. Locally, less... | [
"Sanders & Mirabel 1996"
] | [
"These often-called starburst galaxies, with an IR luminosity LIR ∼ (0.1–5) × 1012 L⊙ (e.g.,",
"become increasingly more common at high z."
] | [
"Background",
"Background"
] | [
[
825,
847
]
] | [
[
733,
824
],
[
873,
915
]
] |
2020ApJ...895..128M__Zaldarriaga_et_al._2018_Instance_1 | We analyze the 10 BBH mergers reported by LIGO and Virgo in their O1 and O2 observing runs (Abbott et al. 2019a; LIGO Scientific Collaboration & Virgo Collaboration 2019). Before discussing results, it is useful to review expectations from the literature for the spin distributions resulting from different formation sce... | [
"Zaldarriaga et al. 2018"
] | [
"Although spin misalignments may be introduced by natal supernova kicks, episodes of mass transfer and tidal torques serve to realign component spins before the formation of the final black hole binary"
] | [
"Compare/Contrast"
] | [
[
721,
744
]
] | [
[
440,
640
]
] |
2019MNRAS.483.2362R__Calderone_et_al._2013_Instance_1 | Various types of AGNs are known and one among them are the narrow-line Seyfert 1 (NLSy1) galaxies, which are classified based on the presence of narrow Hβ emission line with full width at half-maximum (FWHM) 2000 km s−1 and weak [O iii] emission line, with F([O iii])/F(Hβ) 3 (Osterbrock & Pogge 1985; Goodrich 1989). Th... | [
"Calderone et al. 2013"
] | [
"However, from spectro-polarimetric observations of a γ-ray emitting NLSy1 galaxy, PKS 2004 − 447",
"and accretion disc modelling of a sample of 23 radio-detected NLSy1 galaxies",
"indicate that they have masses similar to the blazar class of AGNs."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
813,
834
]
] | [
[
618,
714
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[
735,
811
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[
836,
903
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2021MNRAS.507.6012Z__Kendrick_2018_Instance_2 | Being a benchmark system H + H2, H + HD, and their isotopic counterparts have received much attention over the last several decades (Marinero et al. 1984; Zhang & Miller 1989; D’Mello et al. 1991; Harich et al. 2002; Gao et al. 2015; Yuan et al. 2018a, b, 2020). Most early experimental and theoretical investigations we... | [
"Kendrick 2018"
] | [
"The GP effect, while not significant at temperatures relevant to astrophysics, is important below 1 K as illustrated in a series of calculations on H + HD (v, j) collisions for vibrational levels v = 4 − 9"
] | [
"Motivation"
] | [
[
1229,
1242
]
] | [
[
962,
1167
]
] |
2015MNRAS.453.2747M__Shaw_et_al._2008_Instance_1 | ΓCR can be expressed as the product of three factors – the total cosmic ray ionization rate per H nucleus ζH (including both primary and secondary ionizations), the average energy deposited into the medium per ionization ΔQ, and nH. Both ζH and ΔQ are rather uncertain and can vary considerably over different Galactic e... | [
"Shaw et al. 2008"
] | [
"Indriolo & McCall (2012) find a mean ζH of 1.8 × 10−16 s−1 in their sample of diffuse molecular sight lines, and values as large as ∼1 × 10−15 s−1 have been reported in the literature"
] | [
"Compare/Contrast"
] | [
[
770,
786
]
] | [
[
565,
748
]
] |
2022AandA...658A.188S__Liu_et_al._(2013)_Instance_1 | The trends between the LF slope α and the aforementioned parameters, with the addition of the morphological T type, are shown in Fig. 4 together with their Spearman correlation coefficient (ρ) and their p value, indicating the probability that the two sets of data are uncorrelated. We summarize the properties for which... | [
"Liu et al. (2013)"
] | [
"It should be noted that only a handful of studies so far have looked at the correlation between α and global galaxy properties:",
"while",
"identified H II regions via Paα"
] | [
"Background",
"Background",
"Background"
] | [
[
960,
977
]
] | [
[
661,
788
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[
954,
959
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[
978,
1009
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2019MNRAS.490.5478W__Winter_et_al._2018b_Instance_1 | A growing body of work suggests that planet formation is strongly dependent on the birth environment of the host star. Stars preferentially form in groups (Lada & Lada 2003), and in sufficiently dense environments the evolution of a PPD can be significantly influenced by neighbours (de Juan Ovelar et al. 2012). Close s... | [
"Winter et al. 2018b"
] | [
"However, the stellar number densities required for tidal truncation are high, and in practice few observed regions satisfy this condition"
] | [
"Compare/Contrast"
] | [
[
735,
754
]
] | [
[
596,
733
]
] |
2018MNRAS.478.4357S__Barr_&_Hochberg_1988_Instance_1 | Since long cosmologists have felt motivated to look for alternative explanations for the DE beyond a rigid cosmological constant Λ. The scalar field paradigm was then profusely used also to make the cosmic vacuum dynamical: Λ = Λ(ϕ). In the old days, the main aim was to adjust the large value of Λ typically predicted i... | [
"Barr & Hochberg 1988"
] | [
"Since long cosmologists have felt motivated to look for alternative explanations for the DE beyond a rigid cosmological constant Λ. The scalar field paradigm was then profusely used also to make the cosmic vacuum dynamical: Λ = Λ(ϕ). In the old days, the main aim was to adjust the large value of Λ typically predic... | [
"Background"
] | [
[
518,
538
]
] | [
[
0,
379
]
] |
2016ApJ...817..173L__Takahashi_2004_Instance_1 | Horizon scale imaging promises to test basic predictions of GR and improves our understanding of the physics responsible for accretion and emission in a strong gravitational field. In particular, imaging a black hole shadow has been a long-standing goal of black hole astronomy. However, imaging the black hole shadow fe... | [
"Takahashi 2004"
] | [
"Second, while the predicted shadow feature is nearly independent of the spin or orientation of the black hole to within 10%",
"the emission region surrounding the black hole depends on the details of the underlying accretion process and is intrinsically time variable primarily due to the stochastic nature of mag... | [
"Background",
"Background"
] | [
[
834,
848
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[
695,
818
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[
851,
1130
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2015ApJ...801..112L__Kulsrud_1983_Instance_1 | The main goal of this paper was to further expand the recent transport theory of Zank et al. (2014) and thus, by default, earlier attempts by Drake et al. (2006, 2013) and Bian & Kontar (2013). In our approach, similar to Zank et al. (2014), the focus was on inertial-scale flux ropes that were modeled as quasi-2D ma... | [
"Kulsrud 1983"
] | [
"We adopt a different perspective in proceeding from the basic guiding center kinetic equation (e.g.,",
"instead of the transformed Vlasov equation (Skilling 1975) used by Zank et al. (2014)."
] | [
"Uses",
"Compare/Contrast"
] | [
[
643,
655
]
] | [
[
542,
642
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[
657,
744
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2021MNRAS.508.4512L__Fishbach_et_al._2019_Instance_1 | An EM counterpart is not strictly necessary to use compact binary mergers such as BBHs and BNSs as standard sirens. By matching the sky localization region of GW sources – which can be inferred from the GW measurements – with galaxy catalogues, one might in fact be able to extract complementary information on the redsh... | [
"Fishbach et al. 2019"
] | [
"It has already been tested with real data collected by the LIGO and Virgo detectors",
"though the constraints obtained so far with this ‘statistical’ method are not competitive with the ones derived from GW170817 and its EM counterpart, mainly because of the poor spatial resolution of the current network of grou... | [
"Background",
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] | [
[
720,
740
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[
635,
718
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831,
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2019MNRAS.487.3776P__Moriondo,_Giovanardi_&_Hunt_1998_Instance_1 | Driven by the influx of spatially resolved observations coming from integral field units (IFU), more recent investigations have focused on attempting to infer structural, dynamical, and/or chemical properties for localized regions of galaxies, by decomposing them into physically motivated components. In fact, this conc... | [
"Moriondo, Giovanardi & Hunt 1998"
] | [
"In fact, this concept pre-dates the large-scale use of IFU with works dealing with, for instance, photometric disc/bulge decompositions of surface brightness profiles (e.g. see"
] | [
"Background"
] | [
[
542,
574
]
] | [
[
302,
478
]
] |
2017AandA...601A.109W__Hoyt_et_al._1994_Instance_1 | The WSN/ISN series is based on the counts of both sunspot groups and individual sunspots, with the former being weighted with a factor of ten: (1)\begin{equation} R = k\cdot(10\cdot G + S), \end{equation}R=k·(10·G+S),where G and S are the numbers of sunspot groups and individual sunspots, respectively, and k is a corre... | [
"Hoyt et al. 1994"
] | [
"However, resolving individual spots may be imprecise with poor instrumentations, and a new series, based only on sunspot groups, was proposed, called the group sunspot number, GSN"
] | [
"Background"
] | [
[
545,
561
]
] | [
[
364,
543
]
] |
2015ApJ...800...62B___2014b_Instance_1 | We find that, even though the physical parameters such as kTe and Ïe are very well constrained by the data, it is still impossible to formally distinguish the geometry. The slab (disk-like) and the spherical geometries, as parameterized by the compTT and compPS models used here, both describe the MCGâ05-23-016 spect... | [
"Brenneman et al.",
"2014b"
] | [
"We note that a similar result was found in observations of the Seyfert 1.2 ICÂ 4329a and the narrow-line Seyfert 1 SWIFT J2127.4+5654 with NuSTAR"
] | [
"Similarities"
] | [
[
485,
502
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510,
515
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[
338,
483
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] |
2021AandA...656A..15G___1974_Instance_1 | The comparison between Ulysses and Pamela overlapping measurements revealed that the proton flux in the rigidity interval 1.6–1.8 GV (0.92–1.09 GeV, corresponding approximately to the median energy of the GCR spectrum at solar minimum) has a radial intensity variation of 2.7 ± 0.2% AU−1, and a latitudinal gradient of −... | [
"Marquardt & Heber (2019)"
] | [
"In the recent paper by",
"the Helios proton data radial gradients of the GCR flux were found to be 6.6 ± 4% above 50 MeV and 2 ± 2.5% between 250 and 700 MeV between 0.4 and 1 AU. These results are in agreement with those from Pamela/Ulysses (within the statistical and systematic errors)."
] | [
"Similarities",
"Similarities"
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[
1150,
1174
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[
1127,
1149
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[
1176,
1439
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2019AandA...631A..35B__Bridges_et_al._(1996)_Instance_1 | The collision velocity dependence of the coefficient of restitution between particles was observed in experiments (Bridges et al. 1996; Higa et al. 1996) and is discussed in the literature (e.g., Ramírez et al. 1999; Zhang & Vu-Quoc 2002). However, the experiments by Heißelmann et al. (2010), used in the present paper ... | [
"Bridges et al. 1996"
] | [
"The collision velocity dependence of the coefficient of restitution between particles was observed in experiments"
] | [
"Background"
] | [
[
115,
134
]
] | [
[
0,
113
]
] |
2016ApJ...818...38S__Vanzella_et_al._2011_Instance_1 | As described in the introduction, spectroscopically confirmed Lyα emitters at high redshift (and the nonconfirmations from follow-up campaigns) have proven very valuable for studying the early universe and the environment at the epoch of reionization (Pentericci et al. 2011, 2014; Caruana et al. 2012, 2014; Treu et al.... | [
"Vanzella et al. 2011"
] | [
"Assuming a set of stellar population models",
"to generate spectral energy distributions for galaxies at the emission-line redshift, and fitting them to the available photometry, can give estimates of physical quantities of the galaxies like total stellar mass (the normalization between the observed flux and bes... | [
"Uses",
"Uses"
] | [
[
1041,
1061
]
] | [
[
550,
593
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[
640,
1021
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2019MNRAS.485.3088C__Cheng_et_al._2018_Instance_1 | As displayed in Fig. 1 and Supplementary Movie 1, the control torque τ, applied to the lander at rest, actuates it to pivot over the leading edge, and then the bottom side is dragged downwards in contact with the granular regolith, yielding a reaction force on to the lander (Allen et al. 2013). Given sufficient acceler... | [
"Cheng et al. 2018"
] | [
"Generally, during the hopping process, the acceleration first shows a gradual increase, and then decreases rapidly at the end of control torque, during which the reaction force is highly fluctuating due to intermittent transmissions of acoustic energy along force-chain-like networks",
"as illustrated in Fig 3."
... | [
"Background",
"Background"
] | [
[
1448,
1465
]
] | [
[
1131,
1414
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[
1468,
1492
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2022AandA...661A.129S__Rodríguez-Almeida_et_al._2021_Instance_2 | Radio astronomy is recognized as one of the most effective techniques to search for interstellar molecules. By comparing the spectra of candidate molecules in the laboratory with the spectra observed in astronomical surveys, we can determine whether these molecules exist in interstellar space. Therefore, it is necessar... | [
"Rodríguez-Almeida et al. 2021"
] | [
"Most recently, Rodriguez-Almeida reported the first unambiguous detection of ethanethiol in the ISM, toward the G+0.603-0.027 molecular cloud"
] | [
"Background"
] | [
[
1107,
1136
]
] | [
[
964,
1105
]
] |
2021AandA...655A..25Z__García-Burillo_et_al._2014_Instance_1 | Outflows are ubiquitous in both luminous AGN and in local Seyfert galaxies, and occur on a wide range of physical scales, from highly ionised semi-relativistic winds and jets in the nuclear region at subparsec scales to galactic scale outflows seen in mildly ionised, molecular, and neutral gas (Morganti et al. 2016; Fi... | [
"García-Burillo et al. 2014"
] | [
"On galactic scales massive molecular winds are common in local Seyfert galaxies (e.g."
] | [
"Background"
] | [
[
1204,
1230
]
] | [
[
1034,
1119
]
] |
2019ApJ...872...52C__Linsky_2017_Instance_1 | Studies aiming at measuring and modeling solar radiation and its variability are strongly motivated by the impact that solar irradiance (that is, the electromagnetic energy emitted by the Sun received at the top of Earth’s atmosphere in units of area and time), especially in the UV, has on the chemistry and physical pr... | [
"Linsky 2017"
] | [
"Unfortunately, measurements of UV radiation are strongly hampered by the interstellar medium absorption (up to 70%–90%), which is significant even for relatively close stars, so that estimates of stellar UV radiation strongly rely on modeling (see",
", for a recent review)."
] | [
"Background",
"Background"
] | [
[
1198,
1209
]
] | [
[
950,
1197
],
[
1209,
1232
]
] |
2015ApJ...806..118S__Moffatt_1978_Instance_1 | Magnetic fields observed in various astrophysical systems, such as the Earth, the Sun, disk galaxies, accretion disks, etc., possess large-scale magnetic fields in addition to a fluctuating component. The magnetic field survives for timescales much larger than the diffusion timescales in those systems, and therefore ar... | [
"Moffatt 1978"
] | [
"The standard model of such a turbulent dynamo producing a large-scale magnetic field involves the amplification of seed magnetic fields due to the usual α effect, where α is a measure of the net kinetic helicity in the flow (see, e.g.,"
] | [
"Background"
] | [
[
615,
627
]
] | [
[
379,
614
]
] |
2020ApJ...893...84B__Almeida_et_al._2014a_Instance_1 | Moreover, if mixing is effective over kiloparsec scales, then we would expect the neutral gas observed toward the QSO and the ionized gas seen toward the central H ii region to have the same metallicity. In which case, in order to find
, a significant fraction of the neutral gas must be many kiloparsecs a... | [
"Sánchez Almeida et al. 2014a"
] | [
"Our results are consistent with this idea and provide additional evidence for IGM gas feeding into galaxies through streams from the cosmic web (e.g.,"
] | [
"Similarities"
] | [
[
764,
792
]
] | [
[
613,
763
]
] |
2018AandA...610A..38F__Bisterzo_et_al._2017_Instance_2 | Similarly to the [α/Fe] ratio, the ratio of the slow (s-) neutron capture process elements to iron can be regarded as a cosmic clock. Ba, Sr, La, and Y are mainly s-process elements produced on long timescales by low mass AGB stars (Matteucci 2012). Since a low mass star must evolve to the AGB phase before the s-proces... | [
"Bisterzo et al. 2017"
] | [
"In the literature there are several theoretical works on the evolution of [Ba/Fe] and [Y/Fe] in the Galactic thin disc (e.g."
] | [
"Background"
] | [
[
2101,
2121
]
] | [
[
1877,
2001
]
] |
2018MNRAS.480.5113M__Murgia_et_al._2009_Instance_1 | In this paper we extend previous work based on cosmological simulations by analysing the general magnetic field properties and the diffuse radio halo emission in galaxy clusters in the IllustrisTNG project, a set of cosmological magnetohydrodynamics simulations run with the moving-mesh code arepo (Springel 2010) that i... | [
"Murgia et al. 2009"
] | [
"The main and novel aspect of our work is the analysis of the diffuse radio emission resulting from radio haloes in galaxy clusters"
] | [
"Extends"
] | [
[
539,
557
]
] | [
[
380,
510
]
] |
2019ApJ...878...84M__Oppenheimer_et_al._2016_Instance_1 | These observations have identified a large reservoir of baryons surrounding galaxies. This circumgalactic gas extends to roughly the virial radius (Shull 2014) and contains a substantial fraction of the baryons (Werk et al. 2014; Bregman et al. 2018) and metals (Peeples et al. 2014) associated with the dark matter halo... | [
"Oppenheimer et al. 2016"
] | [
"In cosmological hydrodynamical simulations, the O vi absorbing gas lies behind the halo accretion shock and is maximal in L* galaxies because their virial temperature is close to the temperature T ≈ 105.5 K where the O+5 ionization fraction peaks"
] | [
"Uses"
] | [
[
920,
943
]
] | [
[
672,
918
]
] |
2020AandA...644A..59K__Pastorello_et_al._2019_Instance_2 | The year 2020 marks the 350 yr anniversary of the discovery of the eruption of Nova 1670 (or CK Vul) made by European astronomers (Shara et al. 1985). Their observations, predominantly performed with a naked eye, traced the object’s evolution on the sky in 1670−1672. From the archive records, we know that the eruption ... | [
"Pastorello et al. 2019"
] | [
"Red novae are recognized as manifestations of on-going mergers of non-compact stars such as main-sequence dwarfs, sub-giants, or red giants"
] | [
"Background"
] | [
[
985,
1007
]
] | [
[
779,
918
]
] |
2022MNRAS.512..186K__Chakraborty_et_al._2019a_Instance_1 | A widely used statistical property of the sky brightness distribution is its power spectrum (Lazarian 1995; Bharadwaj & Sethi 2001, and others). As the redshifted 21-cm signal is expected to be faint and hard to detect with imaging, estimating its power spectrum or equivalently intensity mapping gives a possible probe ... | [
"Chakraborty et al. 2019a"
] | [
"This method and its variants",
"have been used to estimate the angular power spectrum of the diffused galactic foreground",
"These works propagate the uncertainties in each visibility estimate and combine that with the sample variance error in measuring the power spectrum to quote uncertainties in the power sp... | [
"Background",
"Background",
"Background"
] | [
[
789,
813
]
] | [
[
487,
515
],
[
655,
744
],
[
977,
1180
]
] |
2021ApJ...912..132K__Abramowicz_&_Zurek_1981_Instance_1 | The magnetic field assumed in our models is normalized either to β = 100, which means thermally dominated accretion flows, or to β = 1, which means actually quite strong magnetization and equilibrium ratio of the magnetic and gas pressures. The gas pressure is set by the solution of the Bondi transonic accretion flow, ... | [
"Abramowicz & Zurek 1981"
] | [
"However, the theoretical works that describe the fundamental properties of the low angular momentum accretion and that usually treat the steady solution of the equations have so far been carried out only for nonmagnetized and usually also nonviscous flows"
] | [
"Background"
] | [
[
1485,
1508
]
] | [
[
1228,
1483
]
] |
2021AandA...655A..12T__Tang_et_al._2017b_Instance_7 | 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"
] | [
"The spatial density measured with para-H2CO (303–202) and C18O (2–1) in N113 and N159W is n(H2) ~ 105 cm−3 on a size of ~30″"
] | [
"Uses"
] | [
[
2099,
2116
]
] | [
[
1973,
2097
]
] |
2015ApJ...810..107M__LBGs_and_Ouchi_et_al._2008_Instance_1 | Here, we present a revised calculation of the emissivity of ionizing photons at z = 2.85 based on the analysis of the HST data in the HS1549 field. We estimate the comoving specific emissivity as
3
following the assumptions of M13 and Nestor et al. (2013). In this expression, L is the non-ionizing UV luminosity, Φ... | [
"Ouchi et al. 2008"
] | [
"We perform this emissivity calculation separately for the main sample of spectroscopically confirmed LBGs and LAEs from M13 (using the UV luminosity functions from",
"for LAEs),"
] | [
"Uses",
"Uses"
] | [
[
940,
957
]
] | [
[
745,
908
],
[
958,
968
]
] |
2015AandA...584A..32M__Smolčić_et_al._2015b_Instance_1 | Ikarashi et al. (2015) discussed that if both the radio and FIR continuum are tracers of star-forming regions, then the z ≳ 3 SMGs are more compact than the lower-redshift SMGs typically observed in radio continuum emission (e.g. Biggs & Ivison 2008). As shown in Fig. 7, our present VLA 3 GHz data do not suggest such a... | [
"Smolčić et al. 2015b"
] | [
"We note that Capak et al. (2011) found that AzTEC3 belongs to a spectroscopically confirmed protocluster containing eight galaxies within a 1 arcmin2 area, and therefore the environment might also play a role in the galaxy size evolution (see also",
"However, it is currently unclear whether the environmental eff... | [
"Background",
"Compare/Contrast"
] | [
[
877,
897
]
] | [
[
629,
876
],
[
900,
1076
]
] |
2022MNRAS.511.1362T__Tanikawa_et_al._2021a_Instance_1 | Among the main proposed formation channels for merging binary COs, we find: pairing of primordial BHs (e.g. Carr & Hawking 1974; Bird et al. 2016; Carr et al. 2016; Scelfo et al. 2018; De Luca et al. 2021); isolated binary evolution via common envelope (e.g. Tutukov & Yungelson 1973; Bethe & Brown 1998; Portegies Zwart... | [
"Tanikawa et al. 2021a"
] | [
"Among the main proposed formation channels for merging binary COs, we find:",
"via stable mass transfer (e.g."
] | [
"Background",
"Background"
] | [
[
861,
882
]
] | [
[
0,
75
],
[
704,
734
]
] |
2020MNRAS.497.2651K__Teuff,_Millar_&_Markwick_2000_Instance_1 | As the H ii regions S235 A and S235 C are deeply embedded in the molecular cloud, we cannot use published predictions from standard plane-parallel PDR models without foreground absorption (e.g. Kaufman et al. 1999). In order to understand how the observational view by SOFIA is matched by a ’classical’ model of expandin... | [
"Le Teuff, Millar & Markwick 2000"
] | [
"The gas-phase chemical network from Röllig et al. (2007) (mainly based on the UMIST99 ratefile;",
"allows us to reproduce the C+, CO, and HCO+ abundances in PDRs",
"so we use this network together with the ionization of the atomic species and corresponding recombinations in the H ii regions."
] | [
"Uses",
"Uses",
"Uses"
] | [
[
702,
734
]
] | [
[
606,
701
],
[
736,
798
],
[
829,
956
]
] |
2017ApJ...850...75S__Bugaev_et_al._2016_Instance_1 | 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"
] | [
"Another element of the realistic phenomenological hadronic EoS corresponds to the short-range repulsive interaction of the hard core nature between particles"
] | [
"Background"
] | [
[
749,
767
]
] | [
[
567,
724
]
] |
2022ApJ...935..136O__Ioppolo_et_al._2011_Instance_1 | HCOOH is the simplest carboxylic acid and has been observed toward high-mass and low-mass star-forming regions (e.g., Woods et al. 1983; Liu et al. 2001, 2002; Bisschop et al. 2007; Lefloch et al. 2017; Oya et al. 2017; Csengeri et al. 2019), protoplanetary disks (e.g., Favre et al. 2018), pre-stellar sources (e.g., Ir... | [
"Ioppolo et al. 2011"
] | [
"Although the production of HCOOH has also been investigated experimentally",
"its formation process and chemical link to nitrogen-bearing species are puzzling."
] | [
"Background",
"Motivation"
] | [
[
514,
533
]
] | [
[
438,
512
],
[
661,
742
]
] |
2016MNRAS.457.3492H__Boylan-Kolchin_et_al._2009_Instance_1 | N-body simulations represent the most widely used and convenient method of exploring the highly non-linear regime of cosmic structure formation. Starting from a set of initial conditions, the numerical simulations follow the formation and evolution of structures from an early epoch down to present day. Motivated by the... | [
"Boylan-Kolchin et al. 2009"
] | [
"So far, the biggest efforts were focused into two, somewhat complementary approaches. The first is represented by simulations like",
"Millennium II (ms-II;",
"These follow structure formation in a large cosmological volume at the expense of having a medium or a low-mass resolution. Such simulations provide the... | [
"Background",
"Background",
"Background"
] | [
[
1323,
1349
]
] | [
[
1131,
1261
],
[
1301,
1322
],
[
1772,
2080
]
] |
2019AandA...632A..76N__Ni_2018_Instance_1 | The Juno spacecraft has measured Jupiter’s gravitational field to high precision through precise Doppler tracking in its polar orbit around Jupiter, compared with the previous values detected by Pioneer 10 and 11 and by Voyager 1 and 2 (Folkner et al. 2017; Bolton et al. 2017; Iess et al. 2018). These new gravity data ... | [
"Ni 2018"
] | [
"To accurately describe the shape and internal structure of Jupiter, various interior models with new ingredients, such as two-layer and three-layer structure models, have been established by several groups"
] | [
"Background"
] | [
[
939,
946
]
] | [
[
532,
737
]
] |
2018MNRAS.478...95K__Caselli_et_al._2002_Instance_1 | Strong controversies are however still present regarding the way stars form in gravitationally unstable cores, in particular high-mass stars. Whether it happens on approximately a free-fall time, as suggested in the competitive accretion scenario by Bonnell et al. (2001), or rather slowly, implying at least several fre... | [
"Caselli et al. 2002"
] | [
"A potentially powerful tool that was suggested in the literature is the measurement of deuteration fractions, which may be translated into time-scales via chemical models"
] | [
"Background"
] | [
[
761,
780
]
] | [
[
589,
759
]
] |
2016AandA...588A..44Y__Jones_et_al._2014_Instance_1 | As described in Köhler et al. (2015)2, we assume that the dust properties change with increasing local density through accretion and coagulation. First, in the transition between the diffuse ISM and dense clouds, a second mantle can form on the surface of the CM grains that is due to the coagulation of the small aromat... | [
"Jones et al. 2014"
] | [
"Such carbonaceous mantles are efficiently processed by UV photons",
"but can stay H-rich as long as the radiation field is attenuated"
] | [
"Background",
"Background"
] | [
[
641,
658
]
] | [
[
488,
553
],
[
575,
639
]
] |
2020AandA...644A..59K__Heays_et_al._2017_Instance_2 | Analyzing optical emission lines, emanating from within the northern lobe, Tylenda et al. (2019) found a reddening with EB − V ≈ 0.9 mag or AV ≈ 2.8 mag, which we assume is mainly circumstellar in origin. Hajduk et al. (2013) observed two stars shining through the southern lobe and found AV = 3.3 − 4.4 mag with unknown... | [
"Heays et al."
] | [
"We used shielding functions from",
"which include effects in lines."
] | [
"Uses",
"Uses"
] | [
[
878,
890
]
] | [
[
845,
877
],
[
892,
923
]
] |
2015AandA...576A...5C__Jørgensen_et_al._2012_Instance_2 | The relative abundances of the three species are derived from the column densities in Table 2 and are compared with other star-forming regions and comets in Table 3. The (CH2OH)2/CH2OHCHO abundance ratio of ~0.3–0.5 previously derived in IRAS 16293 by Jørgensen et al. (2012) was revised. Indeed, the assignment in Jørge... | [
"Jørgensen et al. (2012)"
] | [
"Indeed, the assignment in",
"was based on only one line of the gGg′ conformer of ethylene glycol about 200 cm-1",
"above the lowest-energy aGg′ conformer – and thus tentative."
] | [
"Differences",
"Differences",
"Differences"
] | [
[
315,
338
]
] | [
[
289,
314
],
[
339,
421
],
[
455,
515
]
] |
2021ApJ...914...52F__Dere_et_al._1997_Instance_1 | In Equations (24) and (25) the cumulative effect of all ions with Zi ≥ 2 is included in the term ζ(T, f), where a (rather weak) dependence on frequency f appears due to the Gaunt factor. The ζ(T, f) function depends both on the elemental abundances and on each element’s ionization state, which are different in equilibr... | [
"Dere et al. 1997"
] | [
"In this work, we will provide the ζ(T, f) function calculated under the assumption of ionization equilibrium using the CHIANTI spectral code",
"as detailed below. In this framework it is straightforward to users to replace the CHIANTI values for the equilibrium ion fractions by their own values calculated under ... | [
"Uses",
"Uses"
] | [
[
497,
513
]
] | [
[
355,
495
],
[
522,
763
]
] |
2020ApJ...903L..28S__Shivaei_et_al._2015_Instance_1 | The effectiveness of an IRX-β relation depends on its validity for different types of galaxies across cosmic time. While the original MHC99 IRX-β relation applies to majority of galaxies, large scatters around this relation have been observed. Theoretical studies have shown that the IRX-β scatter may depend on the type... | [
"Shivaei et al. 2015"
] | [
"Observations have shown that the IRX-β relation varies with",
"age"
] | [
"Background",
"Background"
] | [
[
764,
783
]
] | [
[
514,
573
],
[
721,
724
]
] |
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"
] | [
"In addition, several observational studies have suggested that the star formation rate (SFR) of the clouds appears to increase over their lifetimes. 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 M... | [
"Background",
"Background"
] | [
[
677,
692
],
[
699,
703
]
] | [
[
444,
676
],
[
725,
959
]
] |
2022MNRAS.517.1058H__Navarro-González_et_al._1989_Instance_1 | It is likely that some of these products are also formed in our experiments, but except for CO2, HNCO, and NCO−, they cannot be unequivocally identified with IR spectroscopy alone. Some of them have the same functional groups as urea and their IR spectra present absorptions in the same spectral regions, albeit with dif... | [
"Navarro-González et al. 1989"
] | [
"It is likely that some of these products are also formed in our experiments, but except for CO2, HNCO, and NCO−, they cannot be unequivocally identified with IR spectroscopy alone. Some of them have the same functional groups as urea and their IR spectra present absorptions in the same spectral regions, albeit wit... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
594,
622
]
] | [
[
0,
571
],
[
664,
802
]
] |
2018AandA...617A..86L__Li_et_al._2015b_Instance_1 | The IRIS spectra measure the flare in a “sit-and-stare” mode with a roll angle of 45∘. The spectral scale is ∼25.6 mÅ per pixel in the far-ultraviolet (FUV) wavelengths. The IRIS slit crosses the flaring loop and one ribbon (Fig. 1). Two red bars enclose the flaring loop region used to study the quasi-periodic oscillat... | [
"Li et al. 2015b"
] | [
"IRIS observations show that Fe XXI 1354.08 Å is a hot (∼11 MK) and broad emission line and is always blended with many narrow chromospheric lines at the flaring ribbons"
] | [
"Uses"
] | [
[
1003,
1018
]
] | [
[
833,
1001
]
] |
2018MNRAS.477.1664G__Behroozi,_Wechsler_&_Wu_2013_Instance_1 | We test our calibration procedure on the buzzard-v1.1 simulation, a mock DES Y1 survey created from a set of dark-matter-only simulations. The simulation and creation of the mock survey data are detailed in DeRose et al. (in preparation), Wechsler et al. (in preparation), and MacCrann et al. (2018), so we provide only ... | [
"Behroozi, Wechsler & Wu 2013"
] | [
"Haloes were identified using rockstar"
] | [
"Uses"
] | [
[
645,
673
]
] | [
[
606,
643
]
] |
2016AandA...593A..22R__Shibuya_et_al._2015_Instance_1 | Although it is a simple concept, obtaining galaxy sizes is not an easy task and is subject to a number of assumptions. The most common way to derive galaxy sizes is by performing light-profile fitting assuming a given shape of the surface brightness profile using a χ2 minimization (e.g. Simard et al. 1999; Peng et al. ... | [
"Shibuya et al. 2015"
] | [
"The most common way to derive galaxy sizes is by performing light-profile fitting assuming a given shape of the surface brightness profile using a χ2 minimization"
] | [
"Background"
] | [
[
673,
692
]
] | [
[
119,
281
]
] |
2017AandA...602A..75R__Kaneko_&_Yokoyama_(2015)_Instance_1 | We can see how this is consistent with the development of small scales via phase mixing by introducing local wavenumbers for the variation with α and β, (3)\begin{eqnarray} \xi \propto \exp {\rm i}\left[ \int \kappa_\alpha {\rm d}\alpha + \int \kappa_\beta {\rm d}\beta \right]\!. \label{number3} \end{eqnarray}ξ∝expi∫κα... | [
"Kaneko & Yokoyama (2015)"
] | [
"\\label{number5} \\end{eqnarray}kα=κα/hα, kβ=κβ/hβ.Equations (2) and (5) give a direct and elegant expression for the perpendicular wave vector as (7)\\begin{eqnarray} \\vec{k}_\\perp \\approx -(\\bdel \\omega_{\\rm c}) t, \\label{number6} \\end{eqnarray}k⊥≈−(∇ωc)t,which is a generalisation to three dimensions of ... | [
"Uses",
"Uses",
"Uses"
] | [
[
1905,
1929
]
] | [
[
1541,
1879
],
[
1901,
1904
],
[
1930,
2027
]
] |
2018MNRAS.480.2881M__Berkley,_Kazanas_&_Ozik_2000_Instance_1 | There has additionally been the concern that the optical light curves do not look as expected if they arise from reprocessing of X-ray emission from a small central corona, e.g. of size similar to that which we measure from microlensing observations, i.e. $\rm{\, \stackrel{\lt }{_\sim }\,}10 R_{G}$ (Dai et al. 2010; Mo... | [
"Berkley, Kazanas & Ozik 2000"
] | [
"The observed optical light curves are smoother than expected and an insufficient fraction of the X-ray emission hits the disc to power the optical variability (e.g."
] | [
"Compare/Contrast"
] | [
[
613,
641
]
] | [
[
448,
612
]
] |
2022MNRAS.511.4333K__Gibbons_et_al._2014_Instance_1 | The first structures we consider are cosmic voids. Cosmic voids are defined as large underdense regions of the cosmic web, they are the largest structures in the Universe and make up most of its volume (Cautun et al. 2014; Falck & Neyrinck 2015). Historically, their existence was one of the earliest predictions of the ... | [
"Gibbons et al. 2014"
] | [
"Moreover, due to their low density, voids are naturally sensitive to dark energy and thus the interest to use them as probe of alternative Dark Energy models and modified gravity scenarios is increasing"
] | [
"Motivation"
] | [
[
1580,
1599
]
] | [
[
1264,
1466
]
] |
2021AandA...656A.137G__White_et_al._1997_Instance_1 | To determine the median spectral index and the variation within the sample we perform a bootstrap analysis, randomly drawing from our sample (with replacement) and median stacking both the LoTSS and FIRST cutouts independently to obtain a median peak pixel flux density measurement in each survey. This is then repeated ... | [
"White et al. 1997"
] | [
"The 16th and 84th percentile of the resulting peak flux density distributions, together with the systematic flux scale density uncertainty of 5%",
"for the FIRST and LoTSS survey, respectively, are used to determine the error on the spectral index."
] | [
"Uses",
"Uses"
] | [
[
567,
584
]
] | [
[
421,
565
],
[
622,
722
]
] |
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.490.1714P__Dolag_et_al._2009_Instance_1 | The E-MOSAICS project (Pfeffer et al. 2018; Kruijssen et al. 2019a) is a suite of cosmological, hydrodynamical simulations of galaxy formation in the Λ cold dark matter cosmogony that couples the MOSAICS model for star cluster formation and evolution (Kruijssen et al. 2011; Pfeffer et al. 2018) to the EAGLE model of ga... | [
"Dolag et al. 2009"
] | [
"Bound galaxies (subhaloes) were identified within the simulations using the subfind algorithm",
"in the same manner as in the EAGLE simulations"
] | [
"Uses",
"Similarities"
] | [
[
657,
674
]
] | [
[
540,
633
],
[
677,
723
]
] |
2017ApJ...847...42D__Purcell_et_al._2011_Instance_1 | The detailed kinematic reconstruction of the Sgr tidal debris by Law & Majewski (2010) used an initial total mass of
M⊙ for the Sgr satellite. However, several studies point to a Sgr remnant mass significantly exceeding that value. Ibata et al. (1997) and Ibata & Lewis (1998) estimate lower bounds of 109 M⊙ for ... | [
"Purcell et al. 2011"
] | [
"As a result, recent studies have shifted to using dark-matter halo masses as large as 1011 M⊙",
"based on halo abundance matching arguments."
] | [
"Background",
"Background"
] | [
[
639,
658
]
] | [
[
544,
637
],
[
679,
722
]
] |
2018MNRAS.478.3890B__Heckman_et_al._2017_Instance_4 | Rather than AGN feedback, it is possible that the effects we are seeing are from a different process coeval or prior to the onset of AGN accretion. Several works have pointed out that AGN activity coincides with a recent starburst, with the AGN having significant accretion events at least ∼200 Myr after the starburst h... | [
"Heckman et al. (2017)"
] | [
"However, the results of",
"show strong offsets in the kinematics of the gas from the host galaxy (≈100 km s−1;",
"whereas the COS-AGN sightlines do not (bottom panel of Fig. 6)"
] | [
"Differences",
"Differences",
"Differences"
] | [
[
1090,
1111
]
] | [
[
1066,
1089
],
[
1112,
1195
],
[
1234,
1296
]
] |
2016ApJ...825...47P__Krimm_et_al._2011a_Instance_1 | A tidal disruption event (TDE) is an astronomical phenomenon that occurs when a star gets too close to a supermassive black hole in the galaxy center and is disrupted by the tidal force of the black hole. Part of stellar material is bound and accreted by the central black hole, resulting in bright optical, UV, and soft... | [
"Krimm et al. 2011a"
] | [
"Recently, three unusual TDE candidates have been discovered by Swift, i.e., Swift J164449.3+573451, Swift J2058.4+0516, and Swift J1112.2-8238 (hereafter Sw J1644+57, Sw J2058+05, and Sw J1112-82 for short, respectively), which have very bright nonthermal hard X-ray and radio emissions"
] | [
"Motivation"
] | [
[
871,
889
]
] | [
[
543,
829
]
] |
2019ApJ...879...52S___2010_Instance_1 | Kennicutt & Evans (2012) present a compilation of disk-averaged SFR and gas mass surface densities whose values have been calculated in a uniform manner across different galaxy types (including normal disk galaxies and dusty starburst galaxies selected in the IR) and find a power-law index of n ∼ 1.4. However, this res... | [
"Bigiel et al.",
"2010"
] | [
"In analyses of the resolved star formation properties of nearby disks, a near-unity index for the Schmidt–Kennicutt relation is also found in regimes where the molecular gas dominates the total gas mass surface density (Σgas >9 M⊙ pc−2; e.g.,"
] | [
"Similarities"
] | [
[
1163,
1176
],
[
1183,
1187
]
] | [
[
920,
1162
]
] |
2022AandA...666A..83N__Chan_et_al._(2018)_Instance_1 | The detection criterion of having the full interval α ± σα inside the prior range [0.8, 1.2] (e.g., Ata et al. 2018; Chan et al. 2018) has commonly been employed in the literature. However, we can observe from these analyses that the distribution of the α parameter in general seems to be more Gaussian than what we find... | [
"Chan et al. (2018)"
] | [
"As pointed out by",
"and Abbott et al. (2022), a natural consequence from having a (approximate) Gaussian distribution is a reasonable concordance among the three different error measurements, that is, ⟨σα⟩∼σ68 ∼ σstd."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
828,
846
]
] | [
[
810,
827
],
[
847,
1044
]
] |
2019MNRAS.486.1608N__Cicone_et_al._2014_Instance_1 | The clearest examples of host–AGN interaction are arguably found in nearby brightest cluster galaxies. The AGN in these systems have been shown to deposit vast amounts of energy into the surrounding intracluster medium via heating and (mega-parsec scale) jets both observationally and by means of modelling (e.g. Binney ... | [
"Cicone et al. 2014"
] | [
"Direct observational evidence for AGN feedback on galactic scales in such environments remains sparse. More specifically, while outflows have been observationally detected in a number of instances around AGN in various gas phases, most of these detections have been made in ultra-luminous infrared galaxies or some ... | [
"Background",
"Background",
"Motivation"
] | [
[
1311,
1329
]
] | [
[
711,
1061
],
[
1144,
1310
],
[
1347,
1534
]
] |
2017ApJ...834..178Y__Tachihara_et_al._2007_Instance_1 | In order to investigate the gas kinematics at an early evolutionary stage and the formation of Keplerian disks, we conduct ALMA observations toward three candidate young protostars, Lupus 3 MMS, IRAS 15398−3559, and IRAS 16253−2429. They are selected from our SMA sample (Yen et al. 2015a). These three protostars all ha... | [
"Tachihara et al. 2007"
] | [
"Lupus 3 MMS is a Class 0 protostar with a bolometric luminosity (Lbol) of 0.41 L⊙ and a bolometric temperature (Tbol) of 39 K in the Lupus 3 cloud at a distance of 200 pc"
] | [
"Background"
] | [
[
776,
797
]
] | [
[
604,
774
]
] |
2022MNRAS.517.5032D__Dihingia_et_al._2021_Instance_1 | In our study, we consider that the accretion disc is threaded by the poloidal magnetic field lines. The initial poloidal field lines are prescribed by implementing a vector potential Aϕ following Zanni et al. (2007) and Vourellis et al. (2019). The functional form of the vector potential is given by
(6)$$\begin{eqnarra... | [
"Dihingia et al. 2021"
] | [
"The parameter m play crucial role in the launching of Blandford–Payne type wind from the accretion disc"
] | [
"Background"
] | [
[
724,
744
]
] | [
[
595,
698
]
] |
2019MNRAS.482.3950S__Shultz_et_al._2015_Instance_1 | As a first step to analysis of NU Ori’s magnetic field, least-squares deconvolution (LSD) profiles were extracted using a line mask developed from an extract stellar request from the Vienna Atomic Line Database 3 (VALD3; Piskunov et al. 1995; Ryabchikova et al. 1997, 2015; Kupka et al. 1999, 2000) using the stellar par... | [
"Shultz et al. 2015"
] | [
"While He lines are often removed due to substantial differences between magnetometry results obtained from He versus metallic lines (e.g.",
"in this case He lines were left in the mask since the majority of the Stokes V line flux comes from these lines, and the Stokes V profiles extracted using a line mask with ... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1033,
1051
]
] | [
[
895,
1032
],
[
1082,
1319
]
] |
2020ApJ...891...28T__Lind_et_al._2015_Instance_1 | Most GCs are now found to host multiple populations through photometry and spectroscopy (e.g., Carretta et al. 2010b; Mészáros et al. 2015; Milone et al. 2015; Piotto et al. 2015; Tang et al. 2017, 2018). Chemical abundances from spectroscopic data suggest that GCs have a group of so-called “second generation” (SG) sta... | [
"Lind et al. 2015"
] | [
"Thanks to large spectroscopic surveys, the search for these chemically peculiar stars is becoming more efficient. Using high spectral resolution surveys, multiple elements, like C, N, O, Na, Mg, and Al, can be measured, depending on the wavelength range and signal-to-noise ratio. Toward this,",
"and Gaia-ESO sur... | [
"Background",
"Background"
] | [
[
1108,
1124
]
] | [
[
638,
931
],
[
1022,
1106
]
] |
2017AandA...601A..64Z__Milosavljević_&_Nakar_2006_Instance_1 | The distribution function of the electrons inside the precursor can be formally determined through a Lorentz transform of the corresponding distribution function in the shock frame, and the latter can be obtained by solving a stationary transport equation with a loss term corresponding to the finite residence time spen... | [
"Milosavljević & Nakar 2006"
] | [
"The residence time can be calculated as the time it takes to deflect the accelerated electron by an angle ~1/Γsh"
] | [
"Uses"
] | [
[
1295,
1321
]
] | [
[
1157,
1269
]
] |
2021AandA...650A.155Z__Oh_et_al._2012_Instance_2 | Many factors can affect the prevalence of AGN activity. One important question is how gas is brought down to the galaxy center to fuel supermassive black holes (SMBHs). In the literature, two kinds of mechanisms are proposed. One is the internal secular evolution process. The torque induced by non-axisymmetric galactic... | [
"Oh et al. 2012"
] | [
"In addition, there is evidence demonstrating that bars can enhance star formation in the central regions of galaxies (e.g."
] | [
"Background"
] | [
[
720,
734
]
] | [
[
597,
719
]
] |
2015AandA...584A..32M__Sargent_et_al._2010_Instance_1 | Nearly all of the cm-wavelength radio emission from star-forming galaxies, such as SMGs, is non-thermal synchrotron radiation from relativistic electrons accelerated in supernova (SN) remnants produced by the short-lived, high-mass OB-type stars (M ≳ 8 M⊙; main-sequence lifetime τMS ≲ 30 Myr). Because SNe trace the rec... | [
"Sargent et al. 2010"
] | [
"This connection between radio emission and star formation is strongly supported by the close infrared (IR)-radio correlation observed in galaxies (e.g."
] | [
"Background"
] | [
[
755,
774
]
] | [
[
464,
615
]
] |
2022ApJ...926...85S__Ehrenreich_et_al._2020_Instance_2 | As in Flowers et al. (2019), to compare our model transmission spectra directly against the Ehrenreich et al. (2020) results, we must calculate the transmission spectra as a function of orbital phase throughout the duration of transit. To account for orbital phase dependencies, we apply the following procedure:1.Accoun... | [
"Ehrenreich et al. (2020)"
] | [
"We use the quadratic limb-darkening coefficients reported by",
"to establish the stellar center-to-limb intensity profile,"
] | [
"Uses",
"Uses"
] | [
[
919,
943
]
] | [
[
858,
918
],
[
944,
1002
]
] |
2022MNRAS.513.4464T__Hopkins_et_al._2020_Instance_2 |
Galactic winds: Galactic winds driven by CRs have often been simulated in two limits: a diffusion-dominated regime, due possibly to ‘extrinsic confinement’, where CRs are scattered by extrinsic turbulence, and/or due to various wave damping mechanisms (e.g. ion neutral damping) and streaming-dominated ‘self confinemen... | [
"Hopkins et al. 2020"
] | [
"However, to date only the FIRE collaboration has implemented the two moment method (capable of dealing with CR streaming) in such simulations, and – in contrast to, for instance, van de Voort et al. (2021) – the plasma β in their winds is too high for the acoustic instability to develop"
] | [
"Compare/Contrast"
] | [
[
2490,
2509
]
] | [
[
2201,
2488
]
] |
2016ApJ...826..168X__Bai_2014_Instance_1 | MRI is considered to be the most promising mechanism driving angular-momentum transport in protoplanetary disks (Balbus & Hawley 1991; Brandenburg et al. 1995; Hawley et al. 1995; Balbus et al. 1996; Balbus & Hawley 1998). However, protoplanetary disks are cold, dense, and, therefore, poorly ionized. The low level of i... | [
"Bai 2014"
] | [
"Ohmic dissipation operates in high-density regions with weak field, AD dominates in highly ionized and low-density regions, and the Hall effect lies in between"
] | [
"Background"
] | [
[
1016,
1024
]
] | [
[
815,
974
]
] |
2020AandA...643A.149S__Nilsson_et_al._2011_Instance_1 | An increasing number of recent works focus on the study of high-redshift Lyman-α emitters (LAEs), objects showing prominent rest-frame Lyα emission within a spectrum (usually) devoid of other line features (e.g. Cassata et al. 2011; Nakajima et al. 2018). The spectral properties of LAEs are usually interpreted as comin... | [
"Nilsson et al. 2011"
] | [
"The spectral properties of LAEs are usually interpreted as coming from young (≲50 Myr) and low-mass (M* 1010 M⊙) galaxies",
"which are actively star forming (SFR ∼ 1 − 100 M⊙ yr−1) and dust poor (dust attenuation AV 0.2, see e.g."
] | [
"Background",
"Background"
] | [
[
866,
885
]
] | [
[
256,
381
],
[
708,
818
]
] |
2019AandA...631A.109W__Rivera_et_al._(2017)_Instance_1 | With the advent of the LOw Frequency ARray (LOFAR; Röttgering et al. 2011; van Haarlem et al. 2013) which combines a large field of view with high sensitivity on both small and large angular scales, we can now study the FIRC at lower frequencies where the contribution from thermal free-free emission is even less import... | [
"Calistro Rivera et al. (2017)"
] | [
"Using deep LOFAR 150 MHz observations in the 7 deg2 Boötes field",
"studied the FIRC at 150 MHz from z ∼ 0.05 out to z ∼ 2.5. They found fairly mild redshift evolution in the logarithmic IR to radio luminosity ratio in the form of qIR ∼ (1 + z)−0.22 ± 0.05.",
"However, if the FIRC is non-linear (i.e. the logar... | [
"Background",
"Background",
"Compare/Contrast"
] | [
[
558,
587
]
] | [
[
469,
533
],
[
588,
777
],
[
778,
931
]
] |
2019AandA...632A.129W__Shodhan_et_al._2000_Instance_1 | Coronal mass ejections (CMEs) are intense solar explosive eruptions during which large amounts of plasma and magnetic field from the solar atmosphere are ejected into interplanetary space. The interplanetary manifestations of CMEs (ICMEs; Kilpua et al. 2017) can be measured by a spacecraft at about 1 AU and exhibit the... | [
"Shodhan et al. 2000"
] | [
"The interplanetary manifestations of CMEs",
"can be measured by a spacecraft at about 1 AU and exhibit the following characteristics:",
"counterstreaming suprathermal electron (CSE) strahls and declining speed"
] | [
"Background",
"Background",
"Background"
] | [
[
838,
857
]
] | [
[
189,
230
],
[
259,
347
],
[
723,
795
]
] |
2019ApJ...878..108L___1991_Instance_1 | A charged particle moving in the electromagnetic field can feel Landau–Lifshitz radiation reaction force due to synchrotron radiation, thus modifying the motion of the charged particle significantly when taking into account the radiation reaction force. Recent observations have demonstrated that there is strong evidenc... | [
"Punsly",
"1991"
] | [
"In particular, if the field line angular velocity is set much less than the horizon angular velocity by distant plasma and a very tenuous plasma exists in the event horizon magnetosphere, then radiation resistance will determine the flow dynamics of accretion as well as the rotational energy extraction by a putati... | [
"Background"
] | [
[
2169,
2175
],
[
2182,
2186
]
] | [
[
1846,
2167
]
] |
2020MNRAS.496.4127V__Homan_et_al._2010_Instance_1 | The recent report by Buisson et al. (2020b) of the detection of Type-I bursts in Sw J1858 shows the presence of a neutron star primary. Therefore, here, we first consider whether Eddington-limited accretion in such a neutron star LMXB might explain the observed radio behaviour in Sw J1858. The neutron star LMXBs with t... | [
"Homan et al. 2010",
"Homan et al. 2010"
] | [
"Therefore, here, we first consider whether Eddington-limited accretion in such a neutron star LMXB might explain the observed radio behaviour in Sw J1858. The neutron star LMXBs with the highest mass accretion rates are the Z-sources, which are thought to accrete near or at the Eddington luminosity, tracing out Z-... | [
"Uses",
"Compare/Contrast"
] | [
[
534,
551
],
[
2023,
2040
]
] | [
[
136,
502
],
[
1794,
2021
]
] |
2017MNRAS.465..383R__Tong_et_al._2013_Instance_1 | In general, the Hall time-scale for magnetic field evolution depends on the strength of the magnetic field, as seen in equation (4). For young NSs with fields below 1014 G, this time-scale may be longer than the observed SNR age. Therefore, magnetic field growth does not have a dramatic effect on these young NSs. Howev... | [
"Tong et al. 2013"
] | [
"A possible explanation for these low braking indices may be through the emission of a relativistic particle wind"
] | [
"Background"
] | [
[
602,
618
]
] | [
[
428,
540
]
] |
2017MNRAS.470.2959K___2013_Instance_1 | At large distances, the proper motions of the halo stars are either unreliable or generally unavailable, which hinders a direct measurement of their velocity dispersions. However, our off-centric location in the Galaxy means that the galactocentric radial (r) and heliocentric radial (s) directions are not the same. Thi... | [
"Kafle et al. (2013)"
] | [
"For example, Sirko et al. (2004), Kafle et al. (2012),",
"Kafle et al. (2014) and King et al. (2015) fit an ellipsoidal distribution of velocities"
] | [
"Background",
"Background"
] | [
[
1263,
1282
]
] | [
[
1208,
1262
],
[
1284,
1372
]
] |
2021AandA...645A..95H__Boese_2000_Instance_2 | Next we chose an optimum cut-off radius for the detector FOV. The PSPC has a circular FOV with a radius 57′. The PSPC entrance window has a rib support structure with an inner ring at a radius corresponding to 20′ (Pfeffermann et al. 1987; Hasinger & Zamorani 2000). Both the ROSAT telescope angular resolution and its v... | [
"Boese 2000"
] | [
"Taking into account all these effects, the HPR of the overall RASS PSF is 84″"
] | [
"Background"
] | [
[
937,
947
]
] | [
[
858,
935
]
] |
2021MNRAS.506.3313G__Gao_&_Ho_2017_Instance_1 | The B/T ratio of galaxies has been traditionally measured by modelling their surface brightness profile. Such modelling allows one to find the light-profiles of individual photometric components of galaxies and then measure their properties such as luminosity, shape, size etc. The earliest such works aimed at photometr... | [
"Gao & Ho 2017"
] | [
"However, this method leads to systematic errors as creation of 1D light profile by either averaging over the galaxy image or by taking a single cut along the major axis do not properly take into account non-axisymmetric features like a bar or isophotal twist (for more details see"
] | [
"Background"
] | [
[
719,
732
]
] | [
[
438,
718
]
] |
2021MNRAS.500.1772N__Shibata,_Kiuchi_&_Sekiguchi_2017_Instance_1 | While these early studies demonstrated the viability of neutron star mergers as a major r-process site, they identified only one ejection channel: ‘dynamical ejecta’ that are tidally flung out by gravitational torques. Since they are never substantially heated, these ejecta carry their original β −equilibrium electron ... | [
"Shibata, Kiuchi & Sekiguchi 2017"
] | [
"As of today, many more mass ejection channels have been discussed:",
"and by viscous effects"
] | [
"Background",
"Background"
] | [
[
1289,
1321
]
] | [
[
869,
935
],
[
1265,
1287
]
] |
2019AandA...623A..75V__Tetarenko_et_al._2018a_Instance_1 | The X-ray transient MAXI J1820+070 was first detected on 2018 March 11 (Kawamuro et al. 2018) by the Monitor of All-sky X-ray Image (MAXI, Matsuoka et al. 2009) and was associated with the optical transient ASASSN-18ey (Denisenko 2018; Tucker et al. 2018). In the X-rays, the source flux exceeded 3 Crabs (Bozzo et al. 2... | [
"Tetarenko et al. 2018a"
] | [
"The course of the outburst was monitored in",
"sub-millimeter"
] | [
"Background",
"Background"
] | [
[
913,
935
]
] | [
[
799,
842
],
[
897,
911
]
] |
2019MNRAS.490.5739X__Zahn_et_al._2011_Instance_1 | It is generally believed that reionization started first in high-density regions, where the first luminous objects formed first. In the ‘bubble model’ of reionization (Furlanetto, Zaldarriaga & Hernquist 2004), the amount of star formation and the resulting ionizing photons are estimated using the excursion set model. ... | [
"Zahn et al. 2011"
] | [
"It has been demonstrated that the statistical predictions of the ‘bubble model’ and the 21cmFAST agree fairly well with radiative–hydrodynamic simulations",
"at least when recombination, feedback, etc. are ignored."
] | [
"Similarities",
"Compare/Contrast"
] | [
[
1021,
1037
]
] | [
[
825,
979
],
[
1040,
1096
]
] |
2021AandA...655A.111K__Bovy_et_al._2012_Instance_1 | Over the last decade, the radial and vertical dependences of the metallicity-alpha-element distribution have been studied in more and more detail with increasingly larger samples (e.g., Bensby et al. 2011; Anders et al. 2014; Nidever et al. 2014; Hayden et al. 2015; Queiroz et al. 2020). Figure 6 is mostly consistent w... | [
"Bovy et al. 2012",
"Bovy et al. 2012"
] | [
"Because of their scale height",
"these two sequences are associated with the thick disc (high-alpha) and thin disc (low-alpha), respectively.",
"This is in agreement with the finding that the thick disc has a shorter scale length than the thin disc"
] | [
"Uses",
"Uses",
"Similarities"
] | [
[
767,
783
],
[
2337,
2353
]
] | [
[
736,
765
],
[
861,
969
],
[
2193,
2296
]
] |
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