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 |
|---|---|---|---|---|---|---|
2018MNRAS.476.5417S__McCray_&_Kafatos_1987_Instance_1 | According to our interpretation, the observed high velocity dispersion region in zone ‘F’ associated with the zone totally empty of gas between the two opposite velocity clouds (that the 3Dbarolo model would instead predict to be filled) resembles an expanding superbubble. Superbubbles are known to be associated with v... | [
"McCray & Kafatos 1987"
] | [
"As the SN explosions start occurring within the cavity formed by the stellar wind bubbles, super-bubbles are created (e.g.",
"), which may eventually reach kiloparsec sizes."
] | [
"Background",
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[
673,
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[
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[
694,
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]
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2018AandA...609A..13K__Mucciarelli_et_al._(2017)_Instance_2 | Gaia 1 is a star cluster that was recently discovered by Koposov et al. (2017) in the first Gaia data release (Gaia Collaboration 2016), alongside with another system of lower mass. Its observation and previous detections were seriously hampered by the nearby bright star Sirius, which emphasized the impressive discover... | [
"Mucciarelli et al. 2017"
] | [
"In particular, it was noted that “the Simpson et al. (2017) stars do not define a red giant branch in the theoretical plane, suggesting that their parameters are not correct” (Fig. 1 of"
] | [
"Compare/Contrast"
] | [
[
1714,
1737
]
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[
1528,
1713
]
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2021MNRAS.503.2108P__Andresen_et_al._2017_Instance_1 | CCSNe are also of interest for GW astronomy as targets in their own right. As the sensitivity of GW detectors increases, they will begin to detect not only binary mergers but also other lower amplitude sources of GWs such as CCSNe. Accurate knowledge of the GW emission from CCSNe will be essential for detection and par... | [
"Andresen et al. 2017"
] | [
"In the non-rotating case, the GW emission from the post-bounce phase has been studied using self-consistent 3D simulations by many groups"
] | [
"Background"
] | [
[
698,
718
]
] | [
[
527,
664
]
] |
2017MNRAS.469.3270V__Chakrabarti,_Jin_&_Arnett_1987_Instance_1 | Observations show that the core temperatures of powerful AGN jets are estimated to be quite high (Moellenbrock et al. 1996). So the jets are hot to start with in this paper too. The advective disc model, as in most disc models, comes with a variety of inner disc temperatures. Simulations of advective discs for high vis... | [
"Chakrabarti, Jin & Arnett 1987"
] | [
"High temperatures in the accretion disc can induce exothermic nucleosynthesis too",
"All these processes taken together in an advective disc will produce very hot jet base."
] | [
"Background",
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1035,
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[
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[
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2022MNRAS.509..314F__Dikpati_et_al._2020_Instance_1 | Magneto-Rossby waves arise due to the inhomogeneity of the Coriolis force depending on latitude on a sphere in rotating astrophysical plasma by analogy with a neutral fluid (Petviashvili & Pokhotelov 1992; Onishchenko et al. 2004; Vallis 2006; Onishchenko, Pokhotelov & Astafieva 2008; Zeitlin 2018). It should be noted ... | [
"Dikpati et al. 2020"
] | [
"Magneto-Rossby waves are basic mechanism in variability of various objects in plasma astrophysics. Magneto-Rossby waves determine the large-scale dynamics of the Sun and stars"
] | [
"Background"
] | [
[
784,
803
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[
555,
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2021AandA...648A...5M__Windhorst_et_al._(1990)_Instance_1 | Another important consistency check regards the angular size distribution of the sources. Figure 6 shows the cumulative size distributions of the final catalogs combined together, in four flux density bins (yellow solid lines). Such distributions can be considered reliable only down to a flux-dependent minimum intrinsi... | [
"Windhorst et al. (1990)"
] | [
"The original function proposed by",
"(Eq. (6) with q = 0.62, see left column) does provide a good approximation of the observed distributions, when assuming the original Θmed − S relation described by Eq. (7), only at flux densities S150 MHz≳10 mJy (see long-dashed lines). This is perhaps not surprising consider... | [
"Differences",
"Differences"
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[
782,
805
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[
748,
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806,
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2021MNRAS.507.1229P__Lyman_et_al._2016_Instance_1 | In this work, we present well-calibrated optical photometric (−0.2 to +413 d), polarimetric (−2 to +31 d) and optical (−5 to +391 d), NIR (−5 to +22 d) spectroscopic studies of SN 2012au, based on data obtained using many observational facilities around the globe. Analysis based on our photometric observations suggests... | [
"Lyman et al. 2016"
] | [
"Similarly, the peak bolometric luminosity of SN 2012au (∼ [6.56 ± 0.70] × 1042 erg s−1) is higher than the mean peak luminosities of SNe Ib and Ic, but still lower than those of SNe Ic-BL"
] | [
"Compare/Contrast"
] | [
[
875,
892
]
] | [
[
686,
873
]
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2022AandA...665A.118F__Carlsson_et_al._2016_Instance_1 | Despite significant advances, the solar wind remains challenging to model (and importantly forecast) due to the large range of scales that need to be incorporated. It is well known that energy is injected into the corona at all scales, from magnetohydrodynamic (MHD) waves (Nutto et al. 2012; Van Doorsselaere et al. 202... | [
"Carlsson et al. 2016"
] | [
"Putting aside large-scale eruptions so as to focus on the quasi-steady input of energy into the corona, it is possible to distinguish three broad magnetic configurations of the solar atmosphere for modelling purposes.",
"active or enhanced regions"
] | [
"Background",
"Background"
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[
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[
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2020ApJ...903L..22T__Vuitton_et_al._2007_Instance_3 | While the Loison et al. (2015) CH3C3N model corroborates the upper atmospheric abundance of C4H3N inferred by Vuitton et al. (2007) from the T5 INMS measurements (a factor of 2 higher than those derived from T40 in Vuitton et al. 2019), a large disparity between the photochemical models (and within the ensemble of mode... | [
"Vuitton et al. 2007"
] | [
"CH3C3N itself may form the protonated species, C4H3NH+, through reactions with the HCNH+ and C2H5+ ions producing HCN and C2H4, respectively"
] | [
"Compare/Contrast"
] | [
[
1673,
1692
]
] | [
[
1531,
1671
]
] |
2020AandA...636A.103H__Xu_&_Borovsky_2015_Instance_1 | Solar wind categorization schemes rely on different solar wind properties to identify the solar wind type and adopt mainly one of the following two approaches: (1) Composition-based schemes exploit the oxygen and carbon charge-state composition of the solar wind (Zhao & Fisk 2010; von Steiger et al. 2000). Based on the... | [
"Xu & Borovsky 2015"
] | [
"Proton plasma properties provide an alternative to determine the solar wind type",
"A clear advantage of this approach is that the required observables are available from more spacecraft."
] | [
"Background",
"Background"
] | [
[
1399,
1417
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[
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2016ApJ...822....7K__Kumar_et_al._2012_Instance_1 | To investigate the particle precipitation or transport sites during the flare, we used HXR 25–50 keV and NoRH 17/34 GHz images. We chose the Pixon algorithm (Metcalf et al. 1996) for the RHESSI image reconstruction. The Pixon method is considered to be the most accurate algorithm (Hurford et al. 2002). The integration ... | [
"Kumar et al. 2012"
] | [
"However, if the kink-unstable filament is heated during magnetic reconnection, it is often observed in the AIA 1600 Å channels (e.g.,"
] | [
"Uses"
] | [
[
1031,
1048
]
] | [
[
897,
1030
]
] |
2015MNRAS.446.1293C__Hauser_&_Dwek_2001_Instance_1 | The contribution to the submm background from LBGs is still poorly constrained; however, our data can finally address this question, since we now have a robust detection of the average 850 μm flux density of LBGs at three epochs, at least those with ultraviolet luminosities of L1700 ≈ 1029 erg s−1 Hz−1, characteristic ... | [
"Hauser & Dwek 2001"
] | [
"By comparison, the total background at 850 μm inferred from COBE-FIRAS is 3.1–4.4 × 104 mJy deg−2",
"Summing these separate surface brightness densities together, we find that the LBGs with L1700 > 1029 erg s−1 Hz−1 in our z ∼ 3, 4, and 5 samples comprise around 6–8 per cent of the submm background at 850 μm (wh... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
659,
677
]
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[
521,
618
],
[
708,
1002
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] |
2022MNRAS.517.2383B__Strat,_Morgenstern_et_al._2009_Instance_1 | The UK Chemistry and Aerosol (UKCA) model (Morgenstern et al. 2009; O’Connor et al. 2014; Archibald et al. 2020) is a framework that we use to describe the global atmospheric chemical composition of our simulated exoplanet. UKCA includes aerosol and gas-phase chemistry and is coupled to the UM dynamics. It uses the UM ... | [
"Strat, Morgenstern et al. 2009"
] | [
"In this study, we use the Stratospheric",
"chemistry schemes."
] | [
"Uses",
"Uses"
] | [
[
771,
801
]
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[
730,
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[
869,
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2019AandA...623A...1I__Rudick_et_al._(2009)_Instance_1 | From the observational side, the deep FDS data further confirm that the bulk of the gravitational interactions between galaxies happened on the W-NW sub-clump of the cluster. In fact, this is the only region of the cluster, inside the virial radius, where the intra-cluster baryons (diffuse light and GCs) are found, tha... | [
"Rudick et al. (2009)"
] | [
"Compared with simulations by",
"the diffuse form observed for the ICL is consistent with the scenario where this component formed by stripped material from the outskirts of a galaxy in a close passage with the cD"
] | [
"Similarities",
"Similarities"
] | [
[
729,
749
]
] | [
[
700,
728
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[
751,
931
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2022MNRAS.516.1539O__Yang_et_al._2022_Instance_1 | At intermediate energies, Fig. 1 shows that non-thermal bremsstrahlung processes become more important. We find this dominates the keV X-ray emission during the first ∼2 Myr. While OY22 demonstrated this non-thermal emission would likely not be detectable in external galaxies, X-ray observations towards the Galactic Fe... | [
"Yang et al. 2022"
] | [
"Although this may suggest better X-ray detection prospects for external galaxy bubbles than our results would imply, we note that these Galactic observations may include a very significant thermal bremsstrahlung contribution from all the gas in the Milky Way halo, which likely extends to a radius of ∼250 kpc",
"... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1023,
1039
]
] | [
[
525,
834
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[
946,
1021
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[
1069,
1146
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2020ApJ...901...45Z__Gopalswamy_et_al._2004_Instance_1 | In this paper, we are focusing on the association of the acceleration and release of SEPs with different types of CME–CME interaction. In fact, the particle acceleration process is a complex one involving many factors, e.g., (1) the CME (or shock) speeds (Richardson et al. 2015; Papaioannou et al. 2016; Kouloumvakos et... | [
"Gopalswamy et al. 2004"
] | [
"The penultimate point has been widely discussed (e.g.,",
"involving the role of the flare material and the interacting CMEs on seed particles."
] | [
"Background",
"Background"
] | [
[
939,
961
]
] | [
[
884,
938
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[
1007,
1091
]
] |
2016MNRAS.460.3554A__Reville_&_Bell_2014_Instance_1 | We consider that the amplified hotspot magnetic field B is turbulent, and that the large-scale background field downstream of the reverse shock is Bjd, nearly perpendicular to the shock normal because the perpendicular component is compressed and enhanced by a factor of 4 to 7 (i.e. Bjd ∼ rBj). In such a case, to accel... | [
"Reville & Bell 2014"
] | [
"In such a case, to accelerate particles up to an energy Ec via a diffusive mechanism, the mean-free path λc ∼ rg(γc, B)2/s in the shock downstream region, where B is a small-scale field, has to be smaller than Larmor radius in Bjd"
] | [
"Uses"
] | [
[
554,
573
]
] | [
[
296,
526
]
] |
2015MNRAS.446.3631A__Brown,_Bildsten_&_Rutledge_1998_Instance_1 | Note that the evolution scenario in Fig. 2 is qualitatively different from previous expectations that assumed standard viscous damping and a large saturation amplitude, see e.g. Levin (1999). There it was proposed that sources slowly spin-up at low temperatures outside of the instability region (where cooling becomes s... | [
"Brown, Bildsten & Rutledge 1998"
] | [
"These astrophysical observations are furthermore theoretically explained by deep crustal heating due to pycnonuclear reactions"
] | [
"Compare/Contrast"
] | [
[
1074,
1105
]
] | [
[
946,
1072
]
] |
2020MNRAS.492.2528L__Prieto_et_al._2017_Instance_1 | Massive black holes (MBHs) are ubiquitous in the Universe, and inhabit all massive galaxies (e.g. Ferrarese & Merritt 2000). MBHs are typically observed via their accretion-powered radiation as active galactic nuclei (AGNs), whose impact on to the host galaxy is invoked to explain massive galaxy quenching (e.g. Silk & ... | [
"Prieto et al. 2017"
] | [
"In particular, theoretical studies have shown that the MBH–halo occupation fraction can be low in dwarf galaxies",
"and even in systems hosting MBHs, their growth is strongly suppressed because of the typically low gas densities in the host (compared to more massive disc galaxies) and the strong impact of supern... | [
"Background",
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[
1243,
1261
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[
763,
875
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[
951,
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2022MNRAS.511.1439F__Gaensler_et_al._2002_Instance_1 | As discussed before, a fraction of PSRs is bound to emerge from the progenitor SNR before our fiducial final time tend = 105yr, due to the high average kick velocity that characterizes the pulsar population. The typical escape time can be estimated by matching the PSR displacement due to its kick velocity (Vpsr) with t... | [
"Gaensler et al. 2002"
] | [
"These nebulae, whose first examples were detected in Hα",
"more recently have been discovered and observed in X-rays and sometimes in radio"
] | [
"Background",
"Background"
] | [
[
1624,
1644
]
] | [
[
1236,
1291
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[
1542,
1622
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] |
2017MNRAS.464.1065G__Opher_et_al._2015_Instance_1 | Finally in this paper, we restricted ourselves to a very limiting case when the ISM is at rest with respect to the star. This two-jet solution can, in principle, be generalized by adding the interstellar flow. Let us consider an arbitrary plane perpendicular to z-axis. This plane cuts a circle from the astropause. In t... | [
"Opher et al. 2015"
] | [
"However, numerical results (e.g.",
"show some bending of the jets towards the tail. This bending in numerical models (for slow incompressible ISM flows) is connected with the numerical dissipation inherent in the numerical schemes. Numerical viscosity may cause the boundary layer breakage on the surface of the a... | [
"Compare/Contrast",
"Compare/Contrast",
"Future Work"
] | [
[
798,
815
]
] | [
[
765,
797
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[
817,
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[
1457,
1663
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2017AandA...604A..80M__Propris_et_al._(2013)_Instance_3 | Using the whole sample (\hbox{$\bar{z}=0.40$}z̅ = 0.40), we find a decreasing faint end for both datasets with consistent values between HST (α = − 0.76 ± 0.07) and Subaru (α = − 0.78 ± 0.06). Separating between low-redshift (\hbox{$\bar{z}=0.29$}z̅ = 0.29) and high-redshift (\hbox{$\bar{z}=0.51$}z̅ = 0.51) samples,... | [
"De Propris et al. (2013)"
] | [
"In addition,",
"claim that previous estimates of the evolution in the RS GLF",
"were also due to SB effects."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1651,
1675
]
] | [
[
1638,
1650
],
[
1676,
1736
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[
1788,
1816
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] |
2020ApJ...904..185O__Price_et_al._2018_Instance_1 | Recently, rotationally supported disks have been found not only in Class I sources but also in some Class 0 sources (e.g., Murillo et al. 2013; Yen et al. 2013, 2017; Ohashi et al. 2014; Tobin et al. 2015, 2016b, 2016a; Seifried et al. 2016; Aso et al. 2017; Lee et al. 2017; Okoda et al. 2018). In spite of these extens... | [
"Price et al. 2018"
] | [
"Moreover, the disk formation process has been revealed to be much more complicated for binary and multiple cases,",
"and in numerical simulations (e.g.,"
] | [
"Background",
"Background"
] | [
[
905,
922
]
] | [
[
441,
554
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[
748,
783
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2017ApJ...838..132O___2015_Instance_1 | As one of the previous studies on the atomic gas in the Perseus region, Stanimirović et al. (2014) calculated the
optical depth toward 26 extra-Galactic radio continuum sources (such as quasars). They calculated
as a function of velocity toward each radio source by using the method described in Heiles & T... | [
"Fukui et al.",
"2015"
] | [
"We test the results in Stanimirović et al. (2014) and",
"which differ by several factors."
] | [
"Differences",
"Differences"
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[
674,
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698
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620,
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701,
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2020MNRAS.491.1498C__Zhang_&_Wang_2019_Instance_1 | We use the largest sample of FRB 121102, which is observed by GBT at 4–8 GHz (Zhang et al. 2018). This sample contains 21 pulses reported in Gajjar et al. (2018) and 72 pulses identified by machine learning. These pulses were observed within a 6 h observation. They share the same observation conditions and were observe... | [
"Zhang & Wang 2019"
] | [
"Meanwhile, a similar power-law index of energy distribution for non-repeating FRBs is also found"
] | [
"Similarities"
] | [
[
1094,
1111
]
] | [
[
980,
1076
]
] |
2016ApJ...832..183K__Kuiper_1941_Instance_1 | The results presented here are based on the assumptions that the CBPs do not interact with the material ejected from their binary star. However, numerical studies have indicated that this material is neither lost isotropically from the binary during the CE phase, nor does it all become unbound. Instead, 1–10% of the ej... | [
"Kuiper 1941"
] | [
"The results presented here are based on the assumptions that the CBPs do not interact with the material ejected from their binary star. However, numerical studies have indicated that this material is neither lost isotropically from the binary during the CE phase, nor does it all become unbound. Instead, 1–10% of t... | [
"Compare/Contrast"
] | [
[
512,
523
]
] | [
[
0,
511
]
] |
2020MNRAS.493.4950S__Haines_et_al._2015_Instance_2 | In the framework of the hierarchical formation of structures, clusters of galaxies are continuously accreting galaxies. It has been suggested that in this process of falling, galaxies could undergo different physical processes that could affect the star formation even before they reach the cluster. Consequently, to ful... | [
"Haines et al. 2015"
] | [
"In recent years, a deficit of star-forming galaxies in the infalling region of clusters has been reported (e.g."
] | [
"Background"
] | [
[
1186,
1204
]
] | [
[
1054,
1165
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] |
2015ApJ...799..138S__Zaritsky_et_al._1994_Instance_1 | We present these results with one very important caveat. Accurately determining metallicities at different redshifts is of key importance to studying the evolution of the MZR. In the local universe, relationships between strong emission line ratios and metallicity can be calibrated to âdirectâ electron temperature-... | [
"Zaritsky et al. 1994"
] | [
"In the local universe, relationships between strong emission line ratios and metallicity can be calibrated to âdirectâ electron temperature-determined metallicities from",
"or photoionization models of star-forming regions"
] | [
"Background",
"Background"
] | [
[
497,
517
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[
176,
349
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[
446,
495
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2022AandA...658A..77N__Dudzevičiūtė_et_al._(2020)_Instance_1 | Finally, we attempted to estimate the total obscured star formation within the Mpc scale environments of ELAN, which can be achieved by assuming that the excess number of submillimeter sources are all associated with the respective ELAN. To compute the SFR densities we first seek a proper conversion from S850 to SFRs. ... | [
"Dudzevičiūtė et al. 2020",
"Dudzevičiūtė et al. (2020)"
] | [
"We utilized a sample of ALMA-identified SMGs in the UKIDSS-UDS field, which has been studied in detail with proper SED fittings",
"Similarly to our observations, the sample of",
"was drawn from a flux-limited sample produced by the SCUBA-2 Cosmology Legacy Survey"
] | [
"Uses",
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[
449,
473
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[
521,
547
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[
320,
447
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[
476,
520
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[
548,
632
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] |
2015ApJ...810...96S___2010_Instance_1 | Most of our knowledge about reconnection comes from effectively 2D reconnection experiments, and only recently have efforts to understand 3D magnetic reconnection been pursued (Priest 2011; Pontin 2011; Shepherd & Cassak 2012; Janvier et al. 2014), revealing a much wider range of dynamics. Very little is known about th... | [
"Qiu et al.",
"2010"
] | [
"Many authors have studied the global and local reconnection rates and timescales of solar reconnection during solar flares based on analysis of the ribbon motions in the chromosphere"
] | [
"Background"
] | [
[
612,
622
],
[
629,
633
]
] | [
[
404,
586
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] |
2018AandA...618A..62P__Cantalupo_et_al._2010_Instance_1 | The recovery of the sky signal from these huge, noisy time streams, a process called map-making, represents one of the most important steps in CMB data analysis and, if the detector noise properties and scanning strategy are known, map-making becomes a linear inverse problem. The generalized least-squares (GLS) equatio... | [
"Cantalupo et al. 2010"
] | [
"Moreover, if we consider the inverse covariance of the time domain noise as the weights, the GLS estimate is also a minimum variance and a maximum likelihood solution to the problem. However, computation of the solution in such a case may require",
"or an application of some iterative procedure",
"These latte ... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
942,
963
]
] | [
[
468,
714
],
[
823,
868
],
[
966,
1057
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] |
2016MNRAS.461..839K__Galazutdinov,_LoCurto_&_Krelowski_2008b_Instance_1 | Diffuse interstellar bands (DIBs) are absorption features seen in the spectra of many astronomical objects in the visible and infrared wavelength regions. The total number of these features exceeds 400. These bands are observed in absorption in star light crossing translucent clouds and the carriers of only three such ... | [
"Galazutdinov, LoCurto & Krelowski 2008b"
] | [
"Moreover, precisely determined DIB profiles",
"showing a specific substructure pattern each, should facilitate their carrier's identification."
] | [
"Uses",
"Uses"
] | [
[
769,
808
]
] | [
[
724,
767
],
[
811,
906
]
] |
2022ApJ...940...72R__Camilo_et_al._2006_Instance_1 | Several studies have discussed the radio luminosity of GLEAM-X J1627 during its radio outburst in comparison with the limits of its rotational energy (Erkut 2022; Hurley-Walker et al. 2022). In particular, assuming isotropic emission, the radio luminosity of the brightest single peaks (L
radio ∼ 1030–1031 erg s−1; Hurl... | [
"Camilo et al. 2006"
] | [
"For the radio-loud magnetars, given their large variability, we have chosen the brightest radio pulses reported in the literature (data collected from"
] | [
"Uses"
] | [
[
762,
780
]
] | [
[
611,
761
]
] |
2021AandA...654A.132B__Esquej_et_al._(2014)_Instance_1 | A third approach to assessing the central star formation is based on the presence of poly-aromatic hydrocarbons (PAHs), which are known to trace young stars, but over a wider range of ages (∼100 Myr) than the ionised line emission. However, there is a debate about whether the PAHs are excited by stars or by the AGN its... | [
"Esquej et al. (2014)"
] | [
"detected PAHs on subarcsec scales in about half of their sample of 29 nearby Seyfert galaxies.",
"They argued that the high column densities in the torus around the AGN would provide shielding that enables PAHs to survive, and the implied central star formation rate density was much higher than in the circum-nuc... | [
"Background",
"Compare/Contrast",
"Similarities"
] | [
[
764,
784
]
] | [
[
785,
879
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[
880,
1107
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[
1108,
1395
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] |
2021MNRAS.506.1045M__Kotani_et_al._1994_Instance_1 | Discovered in 1977 from its bright H α emission (Stephenson & Sanduleak 1977), SS433’s defining characteristics are undoubtedly the helical motion of highly collimated jets of plasma launched from its innermost regions, and mass-loaded, non-polar outflows (Fabian & Rees 1979; Margon et al. 1979) which together inflate ... | [
"Kotani et al. 1994"
] | [
"Knots in SS433’s jet can be resolved at radio frequencies using very long baseline interferometry (VLBI) and indicate the presence of highly relativistic electrons",
", while the baryon content is revealed by emission lines ranging from H and He lines in the optical through to highly ionized Fe lines in the X-ra... | [
"Background",
"Background"
] | [
[
696,
714
]
] | [
[
359,
522
],
[
546,
694
]
] |
2020MNRAS.494.5110B__Troja_et_al._2018_Instance_1 | Following the short gamma-ray burst (sGRB) associated with this event, GRB 170817A (Abbott et al. 2017a,b; Goldstein et al. 2017), radio emission was anticipated as the associated merger outflow interacted with the circum-merger medium. Monitoring the radio emission could therefore provide crucial information on the en... | [
"Troja et al. 2018"
] | [
"Further monitoring, predominantly at frequencies between 0.6 and 15 GHz, has since taken place (e.g."
] | [
"Background"
] | [
[
928,
945
]
] | [
[
695,
795
]
] |
2020MNRAS.499.1788W__Malhotra_et_al._2001_Instance_1 | Owing to their brightness at rest-frame FIR wavelengths, the ionized and neutral species of Carbon, Nitrogen, and Oxygen are powerful diagnostic lines for tracing the ISM of nearby and distant galaxies. When combined with photodissociation region (PDR) models (Tielens & Hollenbach 1985), measurement of the emission fro... | [
"Malhotra et al. 2001"
] | [
"Multilevel FIR transition lines have now been widely surveyed in local galaxies, originally by ISO (e.g."
] | [
"Background"
] | [
[
571,
591
]
] | [
[
446,
550
]
] |
2020MNRAS.493.4960T__Young,_Ross_&_Fabian_1998_Instance_1 | The albedo profile is then computed by cloudy after having specified the values of temperature T(r) and density ρ(r) for each radial patch (with r the radial distance). Results for the energy-dependent albedo profile A(Eloc) obtained for different radial patches in the cases of a = 0 (left), 0.9 (centre), and 0.998 (ri... | [
"Young, Ross & Fabian 1998"
] | [
"Here different line features appear, more or less visible depending on the BH spin and radial distance, such as the clear iron absorption edge that occurs at around ∼6–7 keV (see e.g."
] | [
"Uses"
] | [
[
952,
977
]
] | [
[
768,
951
]
] |
2015MNRAS.454.1468K__Winckel_2003_Instance_1 | Owing to their dusty circumstellar environments, a large mid-infrared (mid-IR) excess is a characteristic feature of post-AGB stars and a detection of cold circumstellar material using mid-IR photometry can be used to identify these objects. The first extensive search for these objects was initiated in the mid-80's usi... | [
"Van Winckel 2003"
] | [
"The Galactic sample of post-AGB stars have been found to be a very diverse group of objects"
] | [
"Background"
] | [
[
700,
716
]
] | [
[
607,
698
]
] |
2020MNRAS.499.3792B__Pimbblet_2011_Instance_2 | For consistency, we adopt the translation of this to the absolute velocities of cluster galaxies normalized by their respective galaxy cluster velocity dispersions into the range $0.3 \lt |\Delta \mathrm{V}|/\sigma _{r_{200}} \lt 0.5$ as deduced by Pimbblet (2011). Thus, if the mode of the standardised velocities for a... | [
"Pimbblet 2011"
] | [
"In contrast, a sub-population of backsplash cluster galaxies would be expected to peak significantly at $|\\Delta \\mathrm{V}|/\\sigma _{r_{200}}\\sim 0$ for values at or beyond our definition of the virial radius, with their fraction reaching zero at some upper limit (e.g."
] | [
"Uses"
] | [
[
834,
847
]
] | [
[
544,
814
]
] |
2022ApJ...935..137K__Whittet_et_al._2001_Instance_1 | In Figure 2, the reduced AKARI IRC spectra of all protostars are presented; the absorption features of the H2O, CO2, and CO ices are clearly detected. All of our targets show deep and broad absorption features of H2O ice in the wavelength range 2.7–3.4 μm. In the case of AFGL 7009S, strong extinction toward the source ... | [
"Whittet et al. 2001"
] | [
"At the wavelength around 4.6 μm for Perseus 1 and 3, RNO 91, and AFGL 7009S, there is a hint for another ice component overlapping with the CO absorption feature at 4.67 μm. Many near-infrared observations have revealed the same feature on the blue wing part of the CO absorption feature",
"which was suggested as... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1124,
1143
]
] | [
[
796,
1083
],
[
1195,
1251
]
] |
2015AandA...582A..26G__model,_Young_(2014)_Instance_1 | In addition, if 26Al in the solar system was inherited from a molecular cloud, one would expect the solar system to have a (60Fe/26Al)0 ratio identical to that of the ISM. If the collapse timescales – depending on the amount of turbulence, the intensity of magnetic fields, and other complex parameters (McKee & Ostriker... | [
"Young (2014)"
] | [
"Despite the observational evidence, and to keep alive the inherited model,",
"proposed to decrease the theoretical 60Fe abundance in molecular clouds by assuming that stars more massive than 30 M⊙ do not explode as SNe. These stars would not contribute to the 60Fe inventory, bringing the theoretical ISM 60Fe/26A... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
962,
974
]
] | [
[
887,
961
],
[
975,
1452
]
] |
2018ApJ...867...90N__Hobbs_et_al._2006_Instance_1 | We constructed the gamma-ray folded light curve of 3FGL J2039.6–5618 using the orbital period from J. Strader et al. (2018, in preparation) and the two best periods in our searches using the full data and the data before MJD 57,040. The phase zero is defined to be the epoch of the optical maximum (T0 = 57,603.95787 in ... | [
"Hobbs et al. 2006"
] | [
"The orbital phase is calculated using the TEMPO2 package"
] | [
"Uses"
] | [
[
687,
704
]
] | [
[
629,
685
]
] |
2018AandA...611A..74R__Grady_et_al._2013_Instance_2 | In this context, MWC 758 (HD 36112) offers a unique environment to probe the existence of planetary companions and to explore the connection between disk structures and planet formation. MWC 758 is a young stellar object (3.5 ± 2 Myr, Meeus et al. 2012) at a distance of 151
$^{+9}_{-8}$
151
−9
+8
4
pc (Ga... | [
"Grady et al. 2013"
] | [
"Although a cavity of 55 astronomical units (au) in radius has been inferred from dust millimeter emission",
"infrared polarized intensity observations have found no clear evidence for a cavity in scattered light"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1373,
1390
]
] | [
[
1140,
1245
],
[
1269,
1371
]
] |
2021AandA...653A..36M__Goulding_&_Alexander_(2009)_Instance_5 | 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)"
] | [
"For the other lines in the 10 − 36 μm interval,",
"did not report a detection, and we used the data presented in Bernard-Salas et al. (2009) for a total of 15 objects."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2618,
2645
]
] | [
[
2570,
2617
],
[
2646,
2762
]
] |
2022ApJ...924...56S__Madau_&_Fragos_2017_Instance_1 | The formation and evolution of black holes (BHs) in the universe is one of the major issues to be addressed by the modern research in astrophysics and cosmology. In the mass range m
• ∼ 5–150 M
⊙, BHs are originated from the final, often dramatic stages in the evolution of massive stars (possibly hosted in binary syste... | [
"Madau & Fragos 2017"
] | [
"These compact remnants",
"can inject strong energy inputs in the primeval universe (e.g.,"
] | [
"Background",
"Background"
] | [
[
988,
1007
]
] | [
[
325,
347
],
[
856,
919
]
] |
2018AandA...619A..13V__Saviane_et_al._2012_Instance_2 | The EWs were measured with the methods described in Vásquez et al. (2015). As in Paper I, we used the sum of the EWs of the two strongest CaT lines (λ8542, λ8662) as a metallicity estimator, following the Ca II triplet method of Armandroff & Da Costa (1991). Different functions have been tested in the literature to mea... | [
"Saviane et al. (2012)"
] | [
"Five clusters from the sample of",
"covering a wide metallicity range were re-reduced and analysed with our code to ensure that our EWs measurements are on the same scale as the template clusters used to define the metallicity calibration."
] | [
"Uses",
"Uses"
] | [
[
1210,
1231
]
] | [
[
1177,
1209
],
[
1232,
1435
]
] |
2015ApJ...815....7V__Davila_1987_Instance_1 | There are also simplified problems, less complex than fully developed turbulence, in which one finds the formation of small scales in the direction perpendicular to an applied magnetic field
It is well known that this effect appears in the context of MHD when imposed parallel-propagating waves interact with an i... | [
"Davila 1987"
] | [
"These processes have been studied both by investigating normal modes of the inhomogeneous structure"
] | [
"Background"
] | [
[
1294,
1305
]
] | [
[
1128,
1227
]
] |
2018MNRAS.480.1174H__Jehin_et_al._2009_Instance_1 | The origin of nitrogen in the Solar system is still an open question. More specifically, the main repository of nitrogen in the protosolar nebula (PSN) is still unclear, although there is some consensus that it may be atomic, N, or molecular, ${\rm N_2}$ (Schwarz & Bergin 2014). Furthermore, the large variations of the... | [
"Jehin et al. 2009"
] | [
"One striking problem is the ${\\rm ^{14}N}/{\\rm ^{15}N}$ isotopic ratio of nitrogen in comets. Its average value, 144 ± 3",
", is three times lower than the bulk ratio of 441 ± 6 in the protosun as inferred from solar wind measurements",
"The reasons for these different ratios remain elusive, casting doubts o... | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
664,
681
]
] | [
[
542,
662
],
[
757,
867
],
[
889,
1088
]
] |
2019AandA...630A..37S__Behar_et_al._2017_Instance_3 | Solar wind velocity distribution moments are described in Behar et al. (2017). The ion density nsw is the moment of order 0, and the ion bulk velocity usw (a vector) appears in the moment of order 1, the flux density
$n_{\mathrm{sw}} \ \underline{\mathbf{u}_{\mathrm{sw}}}$
n
sw
u
sw
_
. The bulk speed ... | [
"Behar et al. 2017"
] | [
"Over the entire mission, the deceleration of the solar wind using the mean speed of the particles is much more limited than the deceleration shown by the norm of the bulk velocity",
": there is more kinetic energy in the solar wind than the bulk velocity vector would let us think."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1659,
1676
]
] | [
[
1478,
1657
],
[
1677,
1775
]
] |
2015ApJ...814...84D__Ellison_et_al._2008_Instance_1 | We first need to discuss that the environmental dependence of the metallicity of star-forming galaxies may depend on the scale at which the environment is defined. At small scales (a few tens of kpc), there is substantial evidence from observations and simulations for a decrement of metallicity and an enhancement of st... | [
"Ellison et al. 2008"
] | [
"At small scales (a few tens of kpc), there is substantial evidence from observations and simulations for a decrement of metallicity and an enhancement of star-formation activity in galaxy close pairs, merging, and interacting systems compared to isolated, field galaxies, mostly attributed to the interaction-induce... | [
"Compare/Contrast"
] | [
[
688,
707
]
] | [
[
164,
642
]
] |
2021AandA...654A..88W__Cai_et_al._2017_Instance_1 | This paper focuses on the population of high-redshift radio galaxies (HzRGs; L500 MHz > 1026 W Hz−1Miley & De Breuck 2008), which are some of the most massive galaxies known at any redshift (with a narrow range in stellar masses of (1 − 6)×1011 M⊙ for 1 z 5.2; De Breuck et al. 2010). Their energetic radio jets are un... | [
"Cai et al. 2017"
] | [
"The quasar-level AGN activity",
"at the center is blocked by the thick dusty torus acting as the “coronograph”",
"this makes HzRGs true obscured type-2 quasars, allowing us to probe their host galaxies and CGM without strong AGN contamination (e.g.",
"for radio-quite type-2 sources, see"
] | [
"Motivation",
"Motivation",
"Motivation",
"Motivation"
] | [
[
1092,
1107
]
] | [
[
703,
732
],
[
758,
835
],
[
858,
992
],
[
1056,
1091
]
] |
2018ApJ...854..120M__Baxter_et_al._2016_Instance_1 | The main purpose of this paper is to calibrate the mass–observable relation from a joint measurement of the abundance (number counts) and the stacked cluster weak lensing profiles. We develop and apply our method to the Sloan Digital Sky Survey (SDSS) red-sequence Matched-filter Probabilistic Percolation (redMaPPer) cl... | [
"Baxter et al. 2016"
] | [
"This is in contrast with previous studies",
"where the backward modeling approach is employed to constrain the probability of mass for a given richness,"
] | [
"Differences",
"Differences"
] | [
[
991,
1009
]
] | [
[
948,
989
],
[
1073,
1180
]
] |
2022AandA...659A.180G__Kutsenko_et_al._2018_Instance_1 | In the last few decades, the dynamic properties of the quiet Sun have been thoroughly investigated using a range of substantially different techniques, allowing us to elaborate a consistent picture of the photospheric dynamics by approaching the problem from different points of view. Particularly interesting and promis... | [
"Kutsenko et al. 2018"
] | [
"These studies are based on the hypothesis that magnetic fields are passively transported by the plasma flow and provide a characterisation of advection and diffusion processes in the quiet photosphere from granular to supergranular scales (see, e.g",
"These studies reveal an anomalous scaling of magnetic field t... | [
"Background",
"Background"
] | [
[
1274,
1294
]
] | [
[
645,
893
],
[
1349,
1550
]
] |
2022ApJ...926...21B__Viviani_et_al._2018_Instance_1 | Some studies have used the 2.5D mean-field dynamo approach to do so, extending solar mean-field dynamo models to other stellar spectral types (Chabrier & Küker 2006; Jouve et al. 2010; Küker et al. 2011; Kitchatinov et al. 2018, and references therein). While these studies are very helpful, most of them lack the full n... | [
"Viviani et al. 2018"
] | [
"These studies pointed out the large magnetic temporal variability and the critical effect of stellar rotation and mass on magnetic field generation through dynamo mechanism, leading in some parameter regimes to configurations with cyclic activity"
] | [
"Background"
] | [
[
1489,
1508
]
] | [
[
1001,
1247
]
] |
2018ApJ...869..143P__Wills_&_Browne_1986_Instance_1 | In order to understand this discrepancy, we consider the BL Lac object nature of NGC 1275 (Veron 1978). The BL Lac object properties of 3C 84 have been noted in connection with the synchrotron optical emission that hides the accretion generated continuum. The BL Lac object aspect can be very pronounced with optical pol... | [
"Wills & Browne 1986"
] | [
"The Hβ BEL is considered to be rotating gas in a flat “pancake-like” region in which the normal to the BEL disk is parallel to the jet axis",
"Thus, the FWHM that appears in Equation (4) depends on the LOS."
] | [
"Uses",
"Uses"
] | [
[
1170,
1189
]
] | [
[
1029,
1168
],
[
1192,
1255
]
] |
2021ApJ...908...95H__Harrington_et_al._2016_Instance_1 | Strong gravitational lensing of high-z star-forming galaxies offers a unique way to examine highly magnified molecular gas. The method for selecting strongly lensed dusty galaxy candidates, at z > 1, is primarily based on unusually bright (sub)millimeter fluxes compared to the expected steep drop-off in (sub)millimeter... | [
"Harrington et al. 2016"
] | [
"This method has since identified a large number across the extragalactic sky, i.e., more than 100 lensed candidates at z > 1"
] | [
"Background"
] | [
[
632,
654
]
] | [
[
371,
495
]
] |
2019ApJ...880...92J__Yang_et_al._2013_Instance_1 | Studies of molecules play a prominent role in explaining the physical, chemical, and kinematic properties of the interstellar medium (ISM) in galaxies (Omont 2007; Tielens 2013). One such molecule is H2O, the third most abundant molecule in the warm dense ISM after H2 and CO (Neufeld et al. 1995). As an asymmetric roto... | [
"Yang et al. 2013"
] | [
"Observations from local galaxies",
"have shown H2O emission to be ubiquitous with intensities as bright as CO lines."
] | [
"Background",
"Background"
] | [
[
632,
648
]
] | [
[
532,
564
],
[
805,
885
]
] |
2016ApJ...821...74J__Tokovinin_et_al._2013_Instance_1 | Recent theoretical work has suggested that the presence, or lack thereof, of long-period giant planets could affect the formation of such systems. Batygin & Laughlin (2015) argued that the migration of Jupiter within our own solar system might have disrupted a massive primordial inner protoplanetary disk that could hav... | [
"Tokovinin et al. 2013"
] | [
"Such high-precision RV surveys include those being undertaken currently with",
"and CHIRON"
] | [
"Background",
"Background"
] | [
[
1155,
1176
]
] | [
[
995,
1071
],
[
1143,
1153
]
] |
2018AandA...612A..77M__Gromadzki_&_Mikołajewska_(2009)_Instance_1 | “Wiggling” outflows are often observed among young stellar jets and protostellar molecular outflows (Eisloffel et al. 1996; Terquem et al. 1999). Terquem et al. (1999) investigated such binary systems where the accretion disk, from which the jet originates, is inclined to the binary orbital plane. They concluded that t... | [
"Gromadzki & Mikołajewska (2009)"
] | [
"We estimated the precession period using the theory from Terquem et al. (1999) and the binary parameters taken from",
"– Mh = 0.8M⊙ (the mass of the hot WD companion), Mp∕Mh = 1.65 (where Mp is the mass of the primary companion), D = 15.5 AU (the mean semi-major axis of the system), and e = 0.25 (eccentricity)."... | [
"Uses",
"Uses"
] | [
[
961,
992
]
] | [
[
845,
960
],
[
993,
1186
]
] |
2018MNRAS.479.3438G___2005_Instance_1 | For instance, due to its dissipative nature, gas can be very efficient in absorbing and transporting outwards the angular momentum of the pair, likely leading to a rapid evolution and eventual coalescence. From observations, as well as numerical simulations, it has been established that in gas-rich galaxy mergers there... | [
"Escala et al.",
"2005"
] | [
"Driven by dynamical friction and global torques from this disc, the pair of MBHs decays very efficiently down to separations of the order of ∼1–0.1 pc, where it forms a gravitationally bound binary"
] | [
"Background"
] | [
[
727,
740
],
[
747,
751
]
] | [
[
528,
725
]
] |
2021AandA...654A.124W__Tanvir_et_al._2017_Instance_1 | The first multi-messenger GW event was discovered on 17 August, 2017. About 1.7 s after the GW170817 signal detected by LIGO and Virgo (Abbott et al. 2017a), the Fermi Gamma-ray Burst Monitor was successfully triggered by GRB 170817A (Abbott et al. 2017b; Goldstein et al. 2017; Zhang et al. 2018) and subsequently a lar... | [
"Tanvir et al. 2017"
] | [
"and the kilonova AT 2017gfo in the ultraviolet–optical–infrared band"
] | [
"Background"
] | [
[
992,
1010
]
] | [
[
621,
689
]
] |
2022AandA...658A.194P__Khata_et_al._2020_Instance_2 | 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"
] | [
"as well as the combination of the H2O-K2 index with pEWs to derive [Fe/H]"
] | [
"Background"
] | [
[
1788,
1805
]
] | [
[
1688,
1761
]
] |
2022AandA...659A..44S__Gandolfi_et_al._2010_Instance_1 | Discovery of exoplanetary systems has presented a rather more complex picture of planetary architectures. Transiting exoplanets, those that cross the visible disk of their host stars from our vantage point, permit the measurement of the spin-orbit misalignment between the planetary orbital plane and the stellar equator... | [
"Gandolfi et al. 2010"
] | [
"These have revealed a surprising diversity in the orbital alignments (for example",
"which is in contrast to the Laplacian ideals of planets forming inside a flat disk, coplanar with the stellar equator and staying there"
] | [
"Background",
"Compare/Contrast"
] | [
[
1510,
1530
]
] | [
[
1358,
1439
],
[
1612,
1747
]
] |
2018AandA...619A..13V__Saviane_et_al._2012_Instance_1 | The EWs were measured with the methods described in Vásquez et al. (2015). As in Paper I, we used the sum of the EWs of the two strongest CaT lines (λ8542, λ8662) as a metallicity estimator, following the Ca II triplet method of Armandroff & Da Costa (1991). Different functions have been tested in the literature to mea... | [
"Saviane et al. 2012"
] | [
"Following our previous work",
"we have adopted here a G+L profile fit."
] | [
"Uses",
"Uses"
] | [
[
792,
811
]
] | [
[
738,
765
],
[
813,
852
]
] |
2015AandA...578A.124N__Jansen_et_al._(1995)_Instance_1 | The Orion Bar is an ideal source for probing the excitation and chemistry of molecules in PDRs, thanks to its close distance of 414 pc (Menten et al. 2007) and its well-known structure and geometry. The Orion Bar is located between the Orion molecular cloud and an Hii region illuminated by the Trapezium cluster. The FU... | [
"Jansen et al. (1995)"
] | [
"The tilt angle compared to a completely edge-on orientation was suggested to be 3° in the model of Hogerheijde et al. (1995) and",
"A tilt angle of 3° is equivalent to an enhancement factor of 20 for the measured column densities."
] | [
"Uses",
"Uses"
] | [
[
955,
975
]
] | [
[
826,
954
],
[
977,
1075
]
] |
2022AandA...663A.105P__Bonafede_et_al._2012_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... | [
"Bonafede et al. 2012"
] | [
"The Largest Linear Sizes (LLS) and radio powers of relics are correlated, as well as the integrated spectral index and the radio power"
] | [
"Background"
] | [
[
775,
795
]
] | [
[
614,
748
]
] |
2019MNRAS.484.2605M__Umeda_et_al._2016_Instance_1 | Remnant BHs of Population III stars with ${\sim }10^{2}\, \mathrm{M}_{\odot }$ are one of the candidates for such seeds (e.g. Madau & Rees 2001). They can grow SMBHs in the available time if either with continuous accretion at the Eddington limit or with short episode of super-Eddington growth. In reality, however, the... | [
"Umeda et al. 2016"
] | [
"An alternative and attractive pathway for seed BH formation is via the so-called direct collapse",
"where a supermassive star (SMS) with ${\\sim } 10^{5}\\, \\mathrm{M}_{\\odot }$ collapses into a BH with a similar mass by general relativistic instability"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
777,
794
]
] | [
[
501,
597
],
[
624,
775
]
] |
2020AandA...640A..56R__Hosseinzadeh_et_al._2017_Instance_1 | SN2006jc, PS15dpn and other narrow-line SNe. Two out of the three SNe we considered above are super-luminous, however the final collapse of a PPI+CC progenitor or PISNe does not need to be superluminous (Woosley 2017). The PPI is just one possible mechanism to create CSM, which can produce extreme luminosities by gener... | [
"Hosseinzadeh et al. 2017"
] | [
"Both kinds of event are too common to be entirely explained with PPI+CC progenitors, and it is likely that both classes contain events with a diversity of physical mechanisms (e.g.,"
] | [
"Compare/Contrast"
] | [
[
853,
877
]
] | [
[
635,
816
]
] |
2018MNRAS.476..184A__Rocha-Pinto_et_al._2000_Instance_1 | The task of estimating stellar ages has been addressed by several authors and lots of different methods are found in the literature. For instance, there are (i) empirical methods, which use a deterministic relation between a given parameter and the age of a star (first proposed by Skumanich 1972). This is the case of g... | [
"Rocha-Pinto et al. 2000"
] | [
"The task of estimating stellar ages has been addressed by several authors and lots of different methods are found in the literature. For instance, there are (i) empirical methods, which use a deterministic relation between a given parameter and the age of a star (first proposed by Skumanich 1972). This is the case... | [
"Background",
"Background"
] | [
[
516,
539
]
] | [
[
0,
318
],
[
417,
448
]
] |
2015MNRAS.450.3458C__Cichowolski_et_al._2001_Instance_1 | The kinetic energy stored in the CO shell can be estimated as $E_{\rm kin} = 0.5\, M_{\rm shell}\, V^2_{\rm exp}$, where Vexp is the expansion velocity of the shell and Mshell is the total (molecular, atomic, and ionized) shell mass. Adopting an expansion velocity equal to half the velocity interval where the structure... | [
"Cichowolski et al. (2001)"
] | [
"Adopting an expansion velocity equal to half the velocity interval where the structure is observed, Vexp = 7.0 ± 1.3 km s− 1 , the molecular mass given in Table 1 and the atomic and ionized masses estimated by",
"1450 and 3000 M⊙, respectively, we obtain Ekin = (2.5 ± 1.0) × 1049 erg, assuming a 40 per cent erro... | [
"Uses",
"Uses"
] | [
[
444,
469
]
] | [
[
234,
443
],
[
471,
588
]
] |
2020AandA...641A.139D__Dvorak_et_al._(2015)_Instance_1 | The use of N-body simulations that include fragmentation allows us to perform a more detailed study of the final composition of the planets formed. In particular, we can study the water loss and/or accretion of the final planets more realistically than in the classic models of accretion. Marcus et al. (2010) presented ... | [
"Dvorak et al. (2015)"
] | [
"performed SPH (smoothed particle hydrodynamics) simulations and studied water loss in planetary embryos and water retained in significant fragments after a collision. They concluded that the impact velocity and the impact angle play a key role in the water loss of a planetary embryo after a collision."
] | [
"Background"
] | [
[
763,
783
]
] | [
[
784,
1086
]
] |
2022MNRAS.515...22J__Newman_et_al._2013_Instance_2 | In Fig. 5, we consider how the velocity dispersion profile scales with radius. Specifically, we plot the power-law index (η) versus the central velocity dispersion (σ0). The vast majority of the galaxies with σ0 ≲ 2.45 are BGGs and these have negative η values. This includes most of the Romulus galaxies (red filled and... | [
"Newman et al. 2013"
] | [
"We leave a more detailed investigation of this change to future work. Here, we simply mention two possible explanations: The change in slope may be a reflection of the differences in the dynamical state (e.g. mass-to-light ratio; M/L) at the outskirts of BCGs"
] | [
"Future Work"
] | [
[
1663,
1681
]
] | [
[
1270,
1529
]
] |
2018AandA...610A..38F__Bisterzo_et_al._2017_Instance_1 | 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"
] | [
"Among the four s-process elements mentioned above, GES provides the abundances of Y II (the first s-process peak element) and Ba II (the second s-process peak element) for all our sample stars. Their abundances behave differently in the Galactic thick and thin discs"
] | [
"Compare/Contrast"
] | [
[
830,
850
]
] | [
[
513,
779
]
] |
2021ApJ...923..106Z__Gabici_et_al._2009_Instance_1 | Diffusive shock acceleration (DSA) operating at expanding shock waves of supernova remnants (SNRs) is widely believed to be the mechanism converting the kinetic energy released by supernova explosions into the energy of cosmic rays (CRs) (e.g., Malkov & Drury 2001). In the DSA theory, CRs being accelerated at shocks mu... | [
"Gabici et al. 2009"
] | [
"In the presence of molecular clouds surrounding the SNR, escaping CRs can illuminate the clouds through pp interactions, producing gamma-ray emission with a flux depending on the amount of nuclear CRs released by an SNR and the diffusion coefficient in the interstellar medium (ISM;"
] | [
"Background"
] | [
[
988,
1006
]
] | [
[
626,
908
]
] |
2019AandA...622A.106M__Maddox_et_al._2018_Instance_1 | The standard single-frequency detection methods for point sources in the CMB and far IR are based on wavelet techniques (Vielva et al. 2003; Barnard et al. 2004; González-Nuevo et al. 2006) or on the matched filter (or MF hereafter, Tegmark & de Oliveira-Costa 1998; Herranz et al. 2002; Barreiro et al. 2003; López-Cani... | [
"Maddox et al. 2018"
] | [
"By default, these techniques are applicable only to single-frequency sky images: even for multiwavelength observatories such as the Herschel Space Observatory",
"or Planck",
"the standard detection pipelines have produced individual source catalogs for each frequency band (see e.g.,",
"The next logical step ... | [
"Background",
"Background",
"Background",
"Motivation"
] | [
[
1223,
1241
]
] | [
[
803,
961
],
[
985,
994
],
[
1017,
1125
],
[
1244,
1400
]
] |
2018ApJ...858...91Y__Leroy_et_al._2008_Instance_1 | Our spectroscopic coverage includes the damped Lyα absorption (DLA) feature from neutral hydrogen. Analysis of this feature is complicated by blending between the host and the companion, as well as uncertainties in the continuum modeling, and it is difficult to constrain the individual contributions of the two componen... | [
"Leroy et al. 2008"
] | [
"The derived N(H i) is an order of magnitude less than a typical value through a disk of a spiral galaxy with stellar mass >1010 M⊙, measured by The H i Nearby Galaxy Survey (THINGS"
] | [
"Compare/Contrast"
] | [
[
966,
983
]
] | [
[
764,
944
]
] |
2021MNRAS.503.3279S__Magrini_et_al._2017_Instance_1 | Among the several features, the distribution of chemical elements across the Galactic disc historically constitutes the most important constraint to chemo-dynamical models of our Milky Way. A number of studies (e.g. Tosi 1988; Hayden et al. 2014, 2015; Anders et al. 2017) have shown the spatial distributions of chemica... | [
"Magrini et al. 2017"
] | [
"Open clusters are a valuable alternative, being on average younger",
"and therefore a better tracer of the gradients in the disc out of which the most recent stars formed."
] | [
"Background",
"Background"
] | [
[
716,
735
]
] | [
[
648,
714
],
[
738,
839
]
] |
2020ApJ...895..128M__Zaldarriaga_et_al._2018_Instance_2 | 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"
] | [
"While tides on the progenitor of the second-born black hole can spin up the progenitor star",
"this effect can be counteracted by mass loss in stellar winds, and more detailed simulations find only low or moderate spin increases due to tides"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1124,
1147
]
] | [
[
1031,
1122
],
[
1150,
1296
]
] |
2015MNRAS.450..630S__Chung_et_al._2010_Instance_1 | Many studies often have environmental classes simply divided into (relaxed) ‘clusters’ or ‘fields’. However, in a Λ cold dark matter (ΛCDM) Universe, most clusters are expected to be the result of group/smaller cluster mergers – some of which can be extremely violent. Little is known about the role of cluster and group... | [
"Chung et al. 2010"
] | [
"It is particularly important to understand if cluster mergers",
"or, alternatively, if they have no direct effect (e.g."
] | [
"Motivation",
"Motivation"
] | [
[
787,
804
]
] | [
[
489,
550
],
[
732,
786
]
] |
2015ApJ...799...42D__Roberge_et_al._2012_Instance_1 | The possible presence of dust in the habitable zones of nearby main-sequence stars is considered a major threat for the direct imaging and characterization of Earth-like extrasolar planets (exo-Earths) with future dedicated space-based telescopes. Several independent studies have addressed this issue and concluded that... | [
"Roberge et al. 2012"
] | [
"The possible presence of dust in the habitable zones of nearby main-sequence stars is considered a major threat for the direct imaging and characterization of Earth-like extrasolar planets (exo-Earths) with future dedicated space-based telescopes. Several independent studies have addressed this issue and concluded... | [
"Background"
] | [
[
582,
601
]
] | [
[
0,
537
]
] |
2016MNRAS.455.2959D__Church_et_al._2014_Instance_1 | Here, we invoke an extend accretion disc corona (ADC) model to explain the long-term time lags detected in NS-LMXBs, including the long-term time lags of GX 349+2 that we derive in this work. Analysing the dip and non-dip spectra of NS-LMXBs, Church & Bałucińska-Church (1993, 1995) proposed a Birmingham model which con... | [
"Church et al. 2014"
] | [
"This model was successfully applied to",
"as well as atoll sources",
"so it could be a universal model for NS-LMXBs."
] | [
"Background",
"Background",
"Background"
] | [
[
1566,
1584
]
] | [
[
1302,
1340
],
[
1540,
1564
],
[
1587,
1633
]
] |
2021MNRAS.500.2577K__Mathys_2017_Instance_1 | The binary characteristics of early-type magnetic stars may provide crucial clues, allowing one to test alternative fossil field hypotheses. The non-magnetic chemically peculiar stars of Am (A-type stars with enhanced lines of Fe-peak elements) and HgMn (late-B stars identified by strong lines of Hg and/or Mn) types ar... | [
"Mathys 2017"
] | [
"The overall incidence rate of magnetic upper main sequence stars in close binaries is less than 2 per cent",
"although this fraction is significantly higher if one includes wide long-period systems"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
905,
916
]
] | [
[
686,
792
],
[
816,
903
]
] |
2021MNRAS.506.5836R__Lyne_&_Manchester_1988_Instance_1 | Below, we describe a simple emission model that can explain most of the key emission features of the pulsars presented in this paper. It draws significantly from the model proposed in Timokhin (2010) that explains nulling and mode changing in pulsars by shrinking and expanding the magnetosphere of the neutron star. The... | [
"Lyne & Manchester 1988"
] | [
"The patchy beam scenario is one of the common beam models that has been used to explain the emission properties of pulsars (see"
] | [
"Background"
] | [
[
839,
861
]
] | [
[
711,
838
]
] |
2020MNRAS.497...52H__Sereno_&_Umetsu_2011_Instance_1 | In Fig. 11, we compared the WL-derived masses (MWL) with those derived from the dynamical analysis (Mdyn) and listed in Table 1. The dynamical masses were computed under the assumption of the singular isothermal model and velocity dispersions (Haines et al. 2018). We obtained the WL masses for the four massive clusters... | [
"Sereno & Umetsu 2011"
] | [
"Previous studies showed that WL masses obtained from the tangential shear fitting were biased low up to 10 per cent with a scatter of ∼25 per cent",
"The main source of the bias are due to substructures and triaxiality. When a cluster whose major axis is perpendicular to the line of sight, i.e elongated in the s... | [
"Background",
"Background"
] | [
[
1199,
1219
]
] | [
[
1032,
1178
],
[
1244,
1492
]
] |
2020AandA...637A..59A__Massalkhi_et_al._2019_Instance_1 | Silicon monoxide (SiO) is predicted to be the most abundant Si-bearing molecule in the entire 1–10 R* range in the atmospheres of M stars. In S-type atmospheres, the calculated abundance of SiO decreases by two orders of magnitude in the 1–5 R* but retains a very high abundance beyond, and the same occurs in C-rich atm... | [
"Massalkhi et al. 2019"
] | [
"Observations indicate that the abundance of SiO does not differ significantly between envelopes around M-, S-, and C-type stars, although in all them the SiO abundance decreases with increasing mass-loss rate"
] | [
"Compare/Contrast"
] | [
[
743,
764
]
] | [
[
460,
668
]
] |
2021AandA...656A.148R__Wiel_et_al._2019_Instance_1 | After the gravitational collapse and if the total mass of the individual cloud is approximately the mass of the Sun (2 × 1030 Kg; (van Dishoeck 2014), a new astrophysical system forms that is dominated gravitationally by a low-mass protostar known as a young stellar object (YSO). The protostar is in the center of the s... | [
"van der Wiel et al. 2019"
] | [
"IRAS 16293-2422 (hereafter IRAS 16293) was chosen for this work as the quintessential example of such an object. IRAS 16293 is adequate for this role because formaldehyde has previously been detected with notable variations in abundances in three differentiated regions of its protodisk"
] | [
"Motivation"
] | [
[
1476,
1500
]
] | [
[
1122,
1408
]
] |
2021MNRAS.500.5009M__Criscienzo_et_al._2006_Instance_1 | RR Lyrae are old low-mass stars that, during the central helium-burning phase, show mainly radial pulsation while crossing the classical instability strip in the colour–magnitude diagram. From the observational point of view, they represent the most numerous class of pulsating stars in the Milky Way and, being associat... | [
"Di Criscienzo et al. 2006"
] | [
"Being associated with old stellar populations, they represent the basis of an alternative Population II distance scale",
"more suitable to calibrate secondary distance indicators that are not specifically associated with spiral galaxies (e.g. the globular cluster luminosity function, see",
"and references ther... | [
"Background",
"Background",
"Background"
] | [
[
1596,
1621
]
] | [
[
1230,
1348
],
[
1429,
1595
],
[
1623,
1647
]
] |
2016MNRAS.461..248S__Munari_et_al._2013_Instance_3 | In Sifón et al. (2013), we used the σ–M200 scaling relation of Evrard et al. (2008) to estimate dynamical masses. As discussed in Section 1, the scaling relation of Evrard et al. (2008) was calibrated from a suite of N-body simulations using DM particles to estimate velocity dispersions. However, the galaxies, from whi... | [
"Munari et al. (2013)",
"Munari et al. (2013)"
] | [
"The difference between the Saro et al. (2013) and",
"galaxy scaling relations depends on the details of the semi-analytic and hydrodynamical implementations used in Saro et al. (2013) and",
"respectively."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2266,
2286
],
[
2422,
2442
]
] | [
[
2216,
2265
],
[
2287,
2421
],
[
2444,
2457
]
] |
2017MNRAS.469.2859S__Ramella_et_al._2002_Instance_1 | The difficulty resides in the definition of ‘group’ itself. If on the simulation side, groups are well defined thanks to an access to the entire three-dimensional information, on the observational side, calling an ensemble of galaxies a group constitutes a great challenge because of a restricted access to the informati... | [
"Ramella et al. 2002"
] | [
"Still several schemes have been developed to define groups within galaxy catalogues. They mainly invoke Friends of Friends (FoF) like algorithms based on projected separation, radial velocities and even luminosities to identify what are called ‘groups’ of galaxies (e.g."
] | [
"Background"
] | [
[
736,
755
]
] | [
[
421,
691
]
] |
2022MNRAS.511.1714T__Quataert,_Jiang_&_Thompson_2022_Instance_1 | Outflows present similarly confounding puzzles, e.g. the existence and survival of cool and low-ionization gas moving at high speeds in observed outflows (e.g. Veilleux, Cecil & Bland-Hawthorn 2005; Tremonti, Moustakas & Diamond-Stanic 2007; Zhang et al. 2017; Cashman et al. 2021) and high-velocity clouds (HVCs; e.g. P... | [
"Quataert, Jiang & Thompson 2022"
] | [
"Possibly the material is accelerated by radiation pressure",
"or cosmic rays (CRs; e.g.",
"but alternatively the high-speed cool gas may be due rapid radiative cooling in some situations."
] | [
"Background",
"Background",
"Background"
] | [
[
790,
821
]
] | [
[
538,
596
],
[
702,
727
],
[
824,
920
]
] |
2015MNRAS.447.3832D__Gandhi_et_al._2008_Instance_1 | GX 339-4 is a recurrent X-ray transient and the system is a confirmed black hole X-ray binary with a low-mass companion star. Although the black hole mass, the system inclination angle and distance are still unknown, they range between 5.8 and 10 M⊙ (Hynes et al. 2003; Muñoz-Darias, Casares & Martínez-Pais 2008; Shidat... | [
"Gandhi et al. 2008"
] | [
"In addition, it also shows evidence of relativistic jets"
] | [
"Background"
] | [
[
857,
875
]
] | [
[
738,
794
]
] |
2017ApJ...839...72A__Emsellem_et_al._1994_Instance_2 | We fit the radial dispersion profiles of each UCD to dynamical models using the Jeans Anisotropic Models (JAM) method with the corresponding code discussed in detail in Cappellari (2008). To briefly summarize, the dynamical models are made in a series of steps making two general assumptions: (1) the velocity ellipsoid ... | [
"Emsellem et al. 1994"
] | [
"Although a supermassive BH can be modeled by adding a Keplerian potential, it is much simpler to model the BH as this small Gaussian"
] | [
"Uses"
] | [
[
1822,
1842
]
] | [
[
1688,
1820
]
] |
2022ApJ...925..203J__Combes_et_al._2019_Instance_1 | The ALMA results mentioned earlier (Alonso-Herrero et al. 2020; García-Burillo et al. 2021) add yet another scale given that the KDC contains both an r ∼ 150–200 pc molecular gas ring and an inner r 50 pc torus-like structure. This smaller nuclear disk/ring may correspond to the structure predicted by a radiation-driv... | [
"Combes et al. 2019"
] | [
"This mechanism would lead to tori that are a few tens of parsec wide and are dynamic, evolving structures as proposed to interpret several recent observational studies and compilations (e.g.,"
] | [
"Compare/Contrast"
] | [
[
671,
689
]
] | [
[
451,
642
]
] |
2020ApJ...890...89G__Bieler_et_al._2015_Instance_1 | Consequently, the neutral gas measured in situ in the coma of comet 67P by the ROSINA experiment (and also MIRO, VIRITS, and Alice) on board Rosetta likely originated several tens of meters beneath the primordial surface of the comet. ROSINA observations provided evidence that this comet is formed from pristine materia... | [
"Bieler et al. 2015"
] | [
"ROSINA observations provided evidence that this comet is formed from pristine material that has not been significantly altered after its formation in the first Myr of the solar nebula stage. The high abundance of",
"of molecular oxygen",
"all indicate that comet 67P formed at low temperature and did not experi... | [
"Background",
"Background",
"Background"
] | [
[
613,
631
]
] | [
[
235,
447
],
[
592,
611
],
[
1025,
1159
]
] |
2022MNRAS.512.3137Z__Katz_et_al._1999_Instance_1 | However, it is not straightforward to explain H2 formation in astronomical sources even when the catalytic roles of dust grains are introduced into models. Interstellar species are believed to be formed on cold grain surfaces via the so called Langmuir–Hinshelwood mechanism (Watson & Salpeter 1972; Pickles & Williams 1... | [
"Katz et al. 1999"
] | [
"However, laboratory and theorectical studies showed that quantum tunnelling does not contribute much to the mobility of H atoms on silicate, carbonaceous or solid amorphous water (ASW) surfaces"
] | [
"Compare/Contrast"
] | [
[
808,
824
]
] | [
[
583,
776
]
] |
2016ApJ...822L..10I__Imanishi_&_Dudley_2000_Instance_1 | We measured the total continuum flux in the SW star-forming region (rectangular with a width of 07 in the east–west × a width of 21 in the north–south) (02h42m4059–4064, −00°00′4789–5000)J2000 to be ∼10 mJy. If this is solely due to the thermal free–free emission inside star-forming H ii-regions, then the corresponding... | [
"Imanishi & Dudley 2000"
] | [
"Previous infrared spectroscopy failed to clearly detect the signatures of ongoing active star formation at the central few arcsec region of the NGC 1068 nucleus due to the lack of polycyclic aromatic hydrocarbon (PAH) emission features",
"which are a good probe of star formation activity"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
991,
1013
]
] | [
[
642,
877
],
[
925,
974
]
] |
2020ApJ...898...25T__Spera_et_al._2019_Instance_1 | Recent detections of gravitational waves (GWs) have shown evidence for a high rate of black hole (BH)–BH and neutron star (NS)–NS mergers in the universe (Abbott et al. 2016a, 2016b, 2017a, 2017b, 2017c, 2019a; Zackay et al. 2019, 2020; Venumadhav et al. 2020). However, the proposed astrophysical pathways to mergers re... | [
"Spera et al. 2019"
] | [
"However, the proposed astrophysical pathways to mergers remain highly debated. Possible compact-object merger pathways include isolated binary evolution"
] | [
"Background"
] | [
[
552,
569
]
] | [
[
262,
414
]
] |
2021ApJ...923L..22A__Rosado_et_al._2015_Instance_2 | 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... | [
"Rosado et al. 2015"
] | [
"individual periodic signals or continuous waves (CWs"
] | [
"Background"
] | [
[
1032,
1050
]
] | [
[
865,
917
]
] |
2022AandA...659A.124H__Liu_et_al._(2013b)_Instance_1 | 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"
] | [
"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 = 0.25 ± 0.02",
"are reported in the literature."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
308,
324
]
] | [
[
0,
252
],
[
291,
306
],
[
437,
468
]
] |
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