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 |
|---|---|---|---|---|---|---|
2015ApJ...799..138S__Yuan_&_Kewley_2009_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-... | [
"Yuan & Kewley 2009"
] | [
"At redshifts above z â¼ 1, it is nearly impossible to detect weak auroral lines for directly determining metallicity (but see"
] | [
"Compare/Contrast"
] | [
[
717,
735
]
] | [
[
590,
716
]
] |
2016ApJ...817..152X__Schady_et_al._2007_Instance_1 | The connection between long-duration GRBs (LGRBs) and SNe was predicted theoretically (Colgate 1974; Woosley 1993) and has been verified observationally (e.g., Galama et al. 1998; Hjorth et al. 2003; see a review in Woosley & Bloom 2006). They usually happen in the star formation regions of the galaxies (e.g., Paczyńsk... | [
"Schady et al. 2007"
] | [
"Therefore, GRB afterglows are good probes of burst environment and the interstellar dust and gas in distant, star-forming galaxies"
] | [
"Motivation"
] | [
[
986,
1004
]
] | [
[
726,
856
]
] |
2020ApJ...902...98G__Tacconi_et_al._2020_Instance_1 | On balance, a large abundance of baryon-dominated, dark matter cored galaxies at z ∼ 2, most strongly correlated with baryonic surface density, angular momentum, and central bulge mass, may be most naturally accounted for by the interaction of baryons and dark matter during the formation epoch of massive halos. Massive... | [
"Tacconi et al. 2020"
] | [
"At the same time, gas accretion rates were maximal"
] | [
"Background"
] | [
[
562,
581
]
] | [
[
510,
560
]
] |
2017ApJ...850..197P__Popham_&_Narayan_1991_Instance_1 | It is worth noting that more ECSNe are predicted for systems with a mass ratio close to unity, as the development of contact happens at longer periods for higher-q systems (see Figure 12). As the primary star starts transferring mass to the secondary, the orbit shrinks, until the mass ratio is reversed. This reversal h... | [
"Popham & Narayan 1991"
] | [
"Several mechanisms have been suggested that control the efficiency of mass transfer, mass accretion, and mass loss, including the existence of an accretion disk that regulates the amount of mass and angular momentum that can be accreted"
] | [
"Motivation"
] | [
[
1501,
1522
]
] | [
[
1247,
1483
]
] |
2022MNRAS.509.3488I__Siana_et_al._2008_Instance_1 | In Fig. 11, we present the evolution of the quasar bolometric luminosity function (LF) from $z \sim 3$ down $z \sim 0$. Even though these functions give the number density of accreting black holes in different luminosity bins, they have been a powerful tool to extract information on how MBHs grow with cosmic time, on t... | [
"Siana et al. 2008"
] | [
"In this work, we only focus on the very bright objects, i.e. ${\\gt}10^{45}\\, \\rm erg\\,s^{-1}$, avoiding the comparison with lower luminosity given the current limitations on observational and theoretical models. In particular, from an observational standpoint, the covered area and depth of current surveys pose... | [
"Compare/Contrast"
] | [
[
843,
860
]
] | [
[
445,
841
]
] |
2021MNRAS.508.2743A__Shakura_&_Sunyaev_1973_Instance_1 | The gas particles are distributed such that the initial surface density profile has the power law:
(7)$$\begin{eqnarray*}
\Sigma _\mathrm{g}=\Sigma _{\mathrm{g},0}\left(\frac{R}{R_{\rm in}}\right)^{-p},
\end{eqnarray*}$$where Σg, 0 is a normalization constant. We choose a locally isothermal equation of state with a s... | [
"Shakura & Sunyaev 1973"
] | [
"We use a constant SPH artificial viscosity coefficient αSPH ≈ 0.55 such that the corresponding disc viscosity coefficient",
"is αd = 0.01 at the inner radius."
] | [
"Uses",
"Uses"
] | [
[
681,
703
]
] | [
[
558,
679
],
[
705,
738
]
] |
2022ApJ...926...85S__Brogi_et_al._2016_Instance_1 | A prime example of the unique benefits of the intersection of the 3D nature of (ultra)hot exoplanet atmospheres and high-resolution spectroscopy lies in the ultrahot Jupiter WASP-76b, a gas giant orbiting an F7 star (West et al. 2016) that is well studied at lower resolution (Fu et al. 2017, 2021; Fisher & Heng 2018; T... | [
"Brogi et al. 2016"
] | [
"These speeds far exceed the few km s−1 planet-frame velocities detected on other planets"
] | [
"Compare/Contrast"
] | [
[
952,
969
]
] | [
[
841,
929
]
] |
2018AandA...615A.148D__Sung_et_al._2013_Instance_2 | We study here the Sco OB1 association (Figs. 1 and 2), using this and other techniques. The general properties of this large OB association, which spans almost 5° on the sky, and is surrounded by a ring-shaped HII region called Gum 55, are reviewed by Reipurth (2008). Its central cluster NGC 6231 contains several tens ... | [
"Sung et al. 2013"
] | [
"The currently accepted distance of NGC 6231 is approximately 1580 pc, and its age is between 2and 8 Myr, with a significant intrinsic spread"
] | [
"Background"
] | [
[
732,
748
]
] | [
[
590,
730
]
] |
2018MNRAS.473.1512A__Eichler_et_al._1989_Instance_1 | In an attempt to understand the radio properties of GRBs, Chandra & Frail (2012) conducted a complete investigation of all historical events observed in the radio domain. These included both of the main GRB populations (Kouveliotou et al. 1993): long-duration GRBs (likely produced by massive stellar collapse where the ... | [
"Eichler et al. 1989"
] | [
"These included",
"and short-duration GRBs (likely caused by the coalescence of two neutron stars or a neutron star and black hole, which lasts for less than 2 s;"
] | [
"Background",
"Background"
] | [
[
591,
610
]
] | [
[
171,
185
],
[
422,
565
]
] |
2018AandA...609A.131G__Heithausen_2012_Instance_2 | Moreover, there could also be some contribution to the detected temperature asymmetry from high-latitude gas clouds in our Galaxy along the line of sight toward M 81. In this respect we note that M 81 is at about 40.9° north of the Galactic disk, where contamination from the Milky Way is expected to be low. However, in... | [
"Heithausen 2012"
] | [
"More recently, data from the Spectral and Photometric Imaging Receiver (SPIRE) instrument onboard Herschel ESA space observatory and Multiband Imaging Photometer for Spitzer (MIPS) onboard Spitzer allowed the identification of several dust clouds north of the M 81 galaxy with a total hydrogen column density in the... | [
"Background",
"Compare/Contrast"
] | [
[
2282,
2297
]
] | [
[
1899,
2280
],
[
2300,
2551
]
] |
2021ApJ...919L..23F__Tendulkar_et_al._2021_Instance_1 | Alongside studies of their emission properties, examining the environments of FRBs on subparcsec to kiloparsec scales can be equally informative. Thus far, only a fraction of known extragalactic repeating FRBs have been localized to host galaxies (Chatterjee et al. 2017; Tendulkar et al. 2017; Marcote et al. 2020; Macq... | [
"Tendulkar et al. 2021"
] | [
"several exhibit spiral arm morphologies"
] | [
"Background"
] | [
[
995,
1016
]
] | [
[
909,
948
]
] |
2020AandA...634A..81B__Bleem_et_al._2015_Instance_1 | After checking the results of the U-net in the test area, we applied the same detection method to the full-sky SZ prediction map, with a detection threshold of pmax = 0.1 in order to recover the maximum number of Planck_z clusters. We detected 20 204 sources in the full-sky map with the U-net with pmax = 0.1. We compar... | [
"Bleem et al. 2015"
] | [
"98 clusters are identified by the South Pole Telescope (SPT;",
"but are not included in the Planck PSZ2 catalogue."
] | [
"Uses",
"Differences"
] | [
[
715,
732
]
] | [
[
654,
714
],
[
735,
785
]
] |
2022MNRAS.513.3458B__Robertson,_Massey_&_Eke_2017_Instance_1 | Among the most viable mechanisms of cusp-core transformation that require changes to the assumed cosmogony is one that was proposed specifically as a possible solution to the cusp-core problem. It proposes that the DM is in fact not collisionless but self-interacting (SIDM; Spergel & Steinhardt 2000; Yoshida et al. 200... | [
"Robertson, Massey & Eke 2017"
] | [
"The most stringent and precise constraints on the self-interaction cross-section have been put on the scales of galaxy clusters (e.g.",
"where observations require that $\\sigma _T/m_chi \\lesssim 1\\, {\\rm cm^2g^{-1}}$."
] | [
"Background",
"Background"
] | [
[
1600,
1628
]
] | [
[
1466,
1599
],
[
1704,
1784
]
] |
2017MNRAS.465..383R__Archibald_et_al._2016_Instance_1 | In previous work (Rogers & Safi-Harb 2016, hereafter RSH16), we studied a parametrized phenomenological model for describing magnetic field growth in neutron star (NS) evolution. Assuming that the external dipole field is buried by an intense process of fall-back accretion after the formation of the NS (Muslimov & Page... | [
"Archibald et al. 2016"
] | [
"This process may provide an explanation for the observed braking indices of young pulsars with n ≠ 3",
"in contrast to the prediction of a rotating magnetic dipole in vacuum"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
568,
589
]
] | [
[
451,
551
],
[
592,
661
]
] |
2018ApJ...869...12S__Duc_et_al._2015_Instance_1 | To verify the predictions of CDM, there have been recent attempts to compare the amount of stellar mass observed in the outskirts of galaxies with the mass fraction in accreted stars predicted by simulations (e.g., Font et al. 2008; Pillepich et al. 2014; Merritt et al. 2016; D’Souza & Bell 2018; Elias et al. 2018; Hua... | [
"Duc et al. 2015"
] | [
"Observing stellar halos in integrated light is, in principle, more easily scalable to the sample sizes needed to explore the wide variation in the accreted component that is predicted by simulations (e.g.,"
] | [
"Motivation"
] | [
[
1579,
1594
]
] | [
[
1329,
1534
]
] |
2019MNRAS.484..892R__Wolf_et_al._2009_Instance_1 | In the left-hand panel of Fig. 2, we compare the morphological types assigned by the STAGES collaboration for the galaxies in the whole OMEGA sample and the jellyfish candidates sample. The sample of jellyfish galaxies (JC345) is composed mainly of late-type spirals and irregulars. In the middle panel of Fig. 2, we sho... | [
"Wolf et al. 2009"
] | [
"One reason why we may not detect many dusty reds as jellyfish galaxies might be due to the fact that these galaxies, despite having relatively high SFRs (only four times lower than that in blue spirals at fixed mass,"
] | [
"Uses"
] | [
[
907,
923
]
] | [
[
690,
906
]
] |
2021AandA...655A.111K__Rojas-Arriagada_et_al._(2019)_Instance_2 | 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... | [
"Rojas-Arriagada et al. (2019)"
] | [
"However, this does not explain the discrepancy with",
"who also used magnesium."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2073,
2102
]
] | [
[
2021,
2072
],
[
2104,
2128
]
] |
2020ApJ...898...92C__Occhiogrosso_et_al._2011_Instance_1 | The first interstellar discovery of MF took place in 1975 from the microwave emission spectrum of Sgr B2, which agrees with the rotational constants of the syn isomer (Curl 1959; Brown et al. 1975; Nummelin et al. 2000). Subsequently, it was detected in several other sources such as comet Hale–Bopp, and protostars and ... | [
"Occhiogrosso et al. 2011"
] | [
"The detailed mechanistic route for the interstellar synthesis of MF is a subject of considerable debate"
] | [
"Background"
] | [
[
923,
947
]
] | [
[
729,
832
]
] |
2021ApJ...923...59V__Feruglio_et_al._2015_Instance_1 | We compute the emission line luminosity using the following equation:
1
LCO′=3.25×107SCOΔvDL2(1+z)3νobs2Kkms−1pc2,
where ν
obs is the observed CO transition frequency, D
L
is the luminosity distance, and S
COΔv is the line-integrated flux in units of Jy km s−1. We convert the observed CO transition luminosity int... | [
"Feruglio et al. 2015"
] | [
"These physical conditions are consistent with what is found for Mrk 231"
] | [
"Similarities"
] | [
[
831,
851
]
] | [
[
758,
829
]
] |
2016ApJ...829...53V__Piconcelli_et_al._2005_Instance_1 | Two spectroscopically confirmed X-ray AGNs in the cluster core (#607, 661 in G13) are suitable candidates for ionizing the nebula. The depth of the new Chandra observation, coupled with an optimal on-axis alignment, allowed us to perform a basic X-ray spectral analysis despite the limited photon statistics (34 and 20 n... | [
"Piconcelli et al. 2005"
] | [
"We then included an absorption component and fixed the photon index to 1.8, as expected for the intrinsic AGN emission (e.g.,"
] | [
"Uses"
] | [
[
966,
988
]
] | [
[
840,
965
]
] |
2018AandA...619A..13V__Saviane_et_al._2012_Instance_4 | 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)"
] | [
"For internal consistency, all EWs in this work have been adjusted to the measurement scale of"
] | [
"Uses"
] | [
[
2136,
2157
]
] | [
[
2042,
2135
]
] |
2018ApJ...856...19N__Fischer_et_al._2010_Instance_1 | Models of the ECSN progenitor cores suggest the onset of the electron-capture instability occurs at a unique ONeMg core mass in the mass range of 1.366–1.377 M⊙. (Miyaji et al. 1980; Nomoto 1984, 1987; Podsiadlowski et al. 2005; Takahashi et al. 2013). Electron captures cause the core to contract, and O and Ne burning ... | [
"Fischer et al. 2010"
] | [
"If the core does collapse, the explosion proceeds via delayed explosion on short timescales",
"and 2D simulations suggest the explosion occurs before significant convection has had time to develop",
"and hence a symmetric explosion results."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
900,
919
]
] | [
[
765,
856
],
[
922,
1023
],
[
1045,
1085
]
] |
2018AandA...615A.155H__Chou_et_al._2007_Instance_1 | While the velocity field is very regular, the velocity dispersion looks more complex. Instead of one peak extended along a southeast-northwest axis (Figs. 10, and 11), we find three (Fig. 13). The central one, elongated along the main axis of the galaxy and not perpendicular to it, is accompanied by two additional regi... | [
"Chou et al. 2007"
] | [
"While the velocity field is very regular, the velocity dispersion looks more complex. Instead of one peak extended along a southeast-northwest axis (Figs. 10, and 11), we find three (Fig. 13). The central one, elongated along the main axis of the galaxy and not perpendicular to it, is accompanied by two additional... | [
"Similarities"
] | [
[
535,
551
]
] | [
[
0,
534
]
] |
2021MNRAS.507.4389G__Masters_et_al._2011_Instance_2 | Erwin (2018) showed that, in a sample drawn from the Spitzer Survey of Stellar Structure in Galaxies (S4G), the bar fraction is constant over a range of (g −r) colours and gas fractions. Their bar fraction does not increase, but rather decreases for stellar masses higher than ∼ 109.7M⊙. These results are in contrast to... | [
"Masters et al. 2011"
] | [
"As mentioned before, we conclude that strong bars drive the trends of bar fraction with (g −r) colour, stellar mass, and SFR observed in other studies"
] | [
"Extends"
] | [
[
1041,
1060
]
] | [
[
867,
1017
]
] |
2019ApJ...883..149A__Rodriguez_et_al._2015_Instance_1 | A key question that remains unanswered is how BBHs are formed. Viable formation channels include isolated binary evolution (e.g., Bethe & Brown 1998; Belczynski et al. 2002, 2014, 2016; Dominik et al. 2013; Mennekens & Vanbeveren 2014; Spera et al. 2015; Eldridge & Stanway 2016; Mandel & de Mink 2016; Marchant et al. 2... | [
"Rodriguez et al. 2015"
] | [
"A key question that remains unanswered is how BBHs are formed. Viable formation channels include",
"and dynamical encounters in dense stellar environments, such as globular clusters (e.g.,"
] | [
"Background",
"Background"
] | [
[
653,
674
]
] | [
[
0,
96
],
[
461,
549
]
] |
2015MNRAS.450.2749G__Brinchmann_et_al._2004_Instance_1 | Ideally, however, one would want to go beyond the description of cosmic global history, and trace galaxy evolution on a galaxy-by-galaxy basis to understand the physical processes driving it. In this respect, great progress has been made by surveys at different redshifts that have established the existence of a strong ... | [
"Brinchmann et al. 2004"
] | [
"The existence of relations between SFR and galaxy stellar mass (SFR–Mass) and specific star formation rate and mass (sSFR = SFR/Mass) have been established from z = 0 out to z > 2"
] | [
"Background"
] | [
[
824,
846
]
] | [
[
643,
822
]
] |
2015AandA...584A..75V__Essen_et_al._(2014)_Instance_8 | The data presented here comprise quasi-simultaneous observations during secondary eclipse of WASP-33 b around the V and Y bands. The predicted planet-star flux ratio in the V-band is 0.2 ppt, four times lower than the accuracy of our measurements. Therefore, we can neglect the planet imprint and use this band to measur... | [
"von Essen et al. (2014)"
] | [
"Therefore the amplitudes estimated in",
"listed in Table 1, are used in this work as fixed values."
] | [
"Uses",
"Uses"
] | [
[
2148,
2171
]
] | [
[
2110,
2147
],
[
2173,
2230
]
] |
2016AandA...588A..44Y__Jones_et_al._2014_Instance_1 | The second issue concerns the fact that inside a given region, coreshine is not detected in all the dense clouds observed by Paladini (2014) and Lefèvre et al. (2014) and that the proportion of clouds exhibiting coreshine varies from one region to another. For instance, 75% of the dense clouds detected in Taurus exhibi... | [
"Jones et al. 2014"
] | [
"A second explanation is related to the stability of H-rich carbon in the ISM, which depends strongly on the radiation field intensity to local density ratio"
] | [
"Background"
] | [
[
1569,
1586
]
] | [
[
1391,
1547
]
] |
2017AandA...600A.138C__Wakeford_et_al._(2016)_Instance_1 | Gibson (2014) proposed that marginalization over many systematics is more robust than simple model selection, and that the BIC-based model selection could be the worst criterion in their experiments. To assess the impact of BIC-based model selection choices (hereafter Method 1) on our derived transmission spectrum, we ... | [
"Wakeford et al. (2016)"
] | [
"We followed the implication of this approach described in",
"and refer the reader to that work for more details."
] | [
"Uses",
"Uses"
] | [
[
520,
542
]
] | [
[
462,
519
],
[
544,
595
]
] |
2019ApJ...872...52C__Ranjan_et_al._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... | [
"Ranjan et al. 2017"
] | [
"As for Earth, modeling of exoplanet atmospheres requires as fundamental input the spectral energy distribution of the hosting star, especially UV and shorter wavelengths (e.g.,"
] | [
"Background"
] | [
[
899,
917
]
] | [
[
704,
880
]
] |
2019ApJ...876L..28D__Lamb_et_al._2018_Instance_1 | In Figures 1 and 2 we show that the X-ray (1.7 keV5
5
This value corresponds to the geometric mean of the XRT energy band, at which the error of the estimated flux can be reasonably suppressed.
), optical (R-band), and radio (6 GHz) fluxes varied with the time of observation applied to the proper corrections if observ... | [
"Lamb et al. 2018"
] | [
"The radio to X-ray spectrum of the forward shock afterglow emission of GW170817/GRB 170817A is fν ∝ ν−0.6, which yields a p = 2.2 in the slow-cooling synchrotron radiation scenario"
] | [
"Uses"
] | [
[
1177,
1193
]
] | [
[
995,
1175
]
] |
2021MNRAS.504.2168G__Steiner_et_al._2011_Instance_2 | Finally, we attempt to characterize the reflection component using the full 2–35 keV spectra with a sophisticated model [M4: ${\tt{\rm constant}}$*${\tt{\rm TBabs}}$*(${\tt{\rm simplr}}$*${\tt {\rm kerrbb2}}$+${\tt{\rm kerrconv}}$*(${\tt{\rm ireflect}}$*${\tt{\rm simplc}}$)), to evaluate the impact on the spin measurem... | [
"Steiner et al. 2011"
] | [
"while a portion of the Compton component will escape to reach an observer, the remains (refer as ${\\tt{\\rm simplc}}$,",
"will strike back to the disc to generate the reflected component."
] | [
"Uses",
"Uses"
] | [
[
864,
883
]
] | [
[
746,
863
],
[
885,
950
]
] |
2015ApJ...807..148G__Rees_&_Mészáros_1994_Instance_2 | The fireball model remains the most popular scenario for the gamma-ray burst (GRB) phenomenon (Cavallo & Rees 1978; Goodman 1986; Paczynski 1986; Shemi & Piran 1990; Rees & Mészáros 1992, 1994; Mészáros & Rees 1993). In this model, the GRB central engine is a stellar-mass black hole or a rapidly spinning and highly mag... | [
"Rees & Mészáros 1994"
] | [
"When the fastest layers catch up with the slowest, the charged particles contained in the layers are accelerated through mildly relativistic collisionless shocks (internal shocks;"
] | [
"Background"
] | [
[
1038,
1058
]
] | [
[
858,
1037
]
] |
2021AandA...655A..12T__Tang_et_al._2017b_Instance_6 | 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"
] | [
"Previous observations show that para-H2CO (3–2) is sensitive to gas temperature at density 105 cm−3"
] | [
"Uses"
] | [
[
1953,
1970
]
] | [
[
1811,
1910
]
] |
2021MNRAS.500.3083C__Lupi_&_Bovino_2020_Instance_2 | Previous theorethical studies have outlined that the [C ii] emission originates from the cold (with temperatures of a few 100 K) neutral medium and from photo-dissociation regions (PDR, Vallini et al. 2013). This seems to suggest that its presence closely traces star formation sites, resulting in a linear relation, as ... | [
"Lupi & Bovino 2020"
] | [
"The main conclusion in all these studies is that a [C ii] deficit exists at high redshift, most likely due to the starbursting nature of these galaxies rather than their metallicity, since most of these systems are close to solar (see, e.g."
] | [
"Compare/Contrast"
] | [
[
1503,
1521
]
] | [
[
1241,
1481
]
] |
2020MNRAS.494.6012W__Middleton_et_al._2015a_Instance_1 | Walton et al. (2017) suggested that the broad-band spectral variability seen in Holmberg IX X-1, similar to that reported here for NGC 1313 X-1, could potentially be related to the presence of the expected funnel-like geometry for the inner accretion flow. In such a scenario, the funnel is expected to geometrically col... | [
"Middleton et al. 2015a"
] | [
"In principle, an increase in accretion rate would be expected to result in an increase in the scale height of the funnel (e.g.",
"However, while this must happen over some range of $\\dot{M}$ in order for the disc structure to transition from the thin disc expected for standard sub-Eddington accretion to the fun... | [
"Motivation",
"Motivation"
] | [
[
1097,
1119
]
] | [
[
959,
1085
],
[
1122,
1586
]
] |
2021MNRAS.507.2115M__Hoyle_2016_Instance_1 | In astrophysics, the number of studies that apply ML techniques has risen substantially in the last years. Unsupervised learning algorithms have been used to identify different kinematic components of simulated galaxies (Obreja et al. 2018, 2019), to compare stellar spectra (Traven et al. 2017), to classify pulsars (Le... | [
"Hoyle 2016"
] | [
"Supervised learning has been used to",
"and to determine the redshift of galaxies"
] | [
"Background",
"Background"
] | [
[
619,
629
]
] | [
[
404,
440
],
[
557,
598
]
] |
2020AandA...641A.126B__Lyutikov_et_al._2005_Instance_1 | Many low-luminosity active galactic nuclei (LLAGN) display prominent jets and compact cores that are sources of highly nonthermal continuum radio emission (see, e.g., Heeschen 1970; Wrobel & Heeschen 1991). The observational signatures of the compact cores have been reproduced using models that produce self-absorbed sy... | [
"Lyutikov et al. 2005"
] | [
"In the optically thin limit, the emission is significantly polarized",
", an effect that has been observed in higher-luminosity AGN sources"
] | [
"Background",
"Background"
] | [
[
864,
884
]
] | [
[
658,
726
],
[
748,
815
]
] |
2019ApJ...873...32M__Deming_et_al._2007_Instance_1 | Inspired by these works, we investigated the possibility of introducing a color diagram for the characterization of irradiated planets using their effective temperature instead of their absolute magnitude. The effective temperature can be used as a proxy for the luminosity/absolute magnitude because the reference radiu... | [
"Deming et al. 2007"
] | [
"To take an even more practical approach, we chose a normalized color parameter based on the Spitzer Infrared Array Camera",
"as a commonly used photometer for the observation of exoplanets (see, e.g.,"
] | [
"Uses",
"Uses"
] | [
[
632,
650
]
] | [
[
364,
485
],
[
531,
606
]
] |
2022ApJ...938...92B__Favier_et_al._2010_Instance_1 | Flows with
Rem≪1
and
N∼(1)
have the distinct property that the induced magnetic field is quickly diffused away, yet the Lorentz force is not negligible. This limit is referred to as the quasi-static approximation to MHD (which we call “QMHD” henceforth; Moffatt 1967; Sommeria & Moreau 1982; Davidson 1995; ... | [
"Favier et al. 2010"
] | [
"This limit is referred to as the quasi-static approximation to MHD",
"although recent numerical studies on its turbulent properties and anisotropy have been done as well"
] | [
"Background",
"Background"
] | [
[
748,
766
]
] | [
[
166,
232
],
[
602,
701
]
] |
2019MNRAS.484.4083H__Pytte,_Mcpherron_&_Kokubun_1976_Instance_1 | According to the Dst index reconstructed by Love, Hayakawa & Cliver (2019), the interval of the telegraphic glitches taking place between ∼13:35 ut and ∼17:20 ut corresponds to the storm main phase (Dst ∼ −320 nT to ∼ −570 nT). This interval also corresponds to that of the low-latitude aurorae witnessed at many points ... | [
"Pytte, Mcpherron & Kokubun 1976"
] | [
"Downward field-aligned current is connected to the dawnside ionosphere, and upward field-aligned current is connected to the duskside ionosphere. The pair of field-aligned currents causes magnetic disturbances at mid- and low- latitudes"
] | [
"Uses"
] | [
[
1085,
1116
]
] | [
[
847,
1083
]
] |
2018AandA...609A..13K__Mucciarelli_et_al._(2017)_Instance_3 | 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)"
] | [
"Combined with the red clump sample of",
"stars in different evolutionary states in Gaia 1 are progressively being sampled."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
2283,
2308
]
] | [
[
2245,
2282
],
[
2372,
2453
]
] |
2016AandA...595A..72M__Vergani_et_al._2015_Instance_2 | On the other hand, the Australia Telescope Compact Array (ATCA) 21 cm line survey of GRB host galaxies revealed high levels of atomic hydrogen (H i), suggesting that the connection between atomic gas and star formation is stronger than previously thought (Michałowski et al. 2015). Star formation may be directly fuelled... | [
"Vergani et al. 2015"
] | [
"This provides a natural route for forming GRBs in low-metallicity environments, as found for most GRB hosts"
] | [
"Compare/Contrast"
] | [
[
1418,
1437
]
] | [
[
1184,
1291
]
] |
2019ApJ...872..143B__Seckel_et_al._1991_Instance_1 | The gamma-ray emission from the solar disk due to CR cascades in the solar atmosphere is denoted as a disk component. This secondary gamma-ray produced by the hadronic interaction of cosmic ray with the solar surface was first proposed by Dolan & Fazio (1965). While only upper limits were obtained by early measurements... | [
"Seckel et al. (1991)"
] | [
"A detailed theoretical model for gamma-rays from the collision of cosmic ray with the solar atmosphere was presented by",
"The predicted gamma-ray flux at energies from 10 MeV to 10 GeV has a large uncertainty, being sensitive to the assumptions about the cosmic-ray transport in the magnetic field near the Sun."... | [
"Background",
"Background"
] | [
[
494,
514
]
] | [
[
374,
493
],
[
516,
705
]
] |
2017ApJ...850...18H__Murase_et_al._2015_Instance_2 | The heating due to the reprocessing of non-thermal photons produced in the nebula can be efficient even at late times. Here, we treat these processes in a simple way as follows. At early times, electromagnetic cascades proceed in the saturation regime, leading to a flat energy spectrum up to ∼1 MeV (Metzger et al. 2014... | [
"Murase et al. 2015"
] | [
"Here, τγ, ν is the optical depth of the ejecta to γ-rays and Kγ, ν is the photon inelasticity at a given frequency, where the Klein–Nishina cross section and the cross section for the Bethe–Heitler pair production in the field of a carbon nucleus are taken into account"
] | [
"Uses"
] | [
[
1845,
1863
]
] | [
[
1549,
1818
]
] |
2020ApJ...898...92C__Harrison_&_Tsang_1976_Instance_1 | We recorded the IRPD spectra of mass-selected H+MF and H+MF-Ln≤2 clusters (L = Ar/N2) in the 2950–3650 cm−1 spectral range in a tandem quadrupole mass spectrometer interfaced with an electron ionization source (Dopfer 2003, 2005), a setup used previously to record IR spectra of a variety of hydrocarbon cations and thei... | [
"Harrison & Tsang 1976"
] | [
"One possible reaction pathway begins with electron ionization of H2, followed by exothermic proton transfer reactions to form H+MF and subsequent three-body association to generate H+MF-Ln clusters"
] | [
"Compare/Contrast"
] | [
[
1053,
1074
]
] | [
[
854,
1051
]
] |
2022AandA...658A.194P__Khata_et_al._2020_Instance_1 | 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"
] | [
"These methods include:",
"empirical relations to derive stellar mass in the form of mass-luminosity relations"
] | [
"Background",
"Background"
] | [
[
933,
950
]
] | [
[
467,
489
],
[
830,
913
]
] |
2015ApJ...813...47M__Morley_et_al._2012_Instance_1 | The consequences of a potential rainout for a planetary atmosphere can be manyfold. First of all the rainout removes metals from the atmosphere, relocating them to deeper layers. Hence the corresponding grain or droplet opacity will be missing from higher atmospheric layers. Because we do not include cloud opacities in... | [
"Morley et al. 2012"
] | [
"It has been found that alkali atoms are present in cool brown dwarf atmospheres, indicating that silicate rainout may occur in these objects"
] | [
"Motivation"
] | [
[
1427,
1445
]
] | [
[
1265,
1405
]
] |
2019MNRAS.485.3185C__Orienti_et_al._2015_Instance_1 | We detected radio emission for six sources, but while the morphology of radio emission in four over six cases is compact on $\le \,$arcseconds scales, predominantly unresolved, for NGC 3185 and NGC 3941 we find a more complex morphology. The estimated radio luminosities at this frequency are L$\, \sim \, 5\, \times \, ... | [
"Orienti et al. 2015"
] | [
"There is evidence for radio emission spread over the host galaxy scale for a number of Seyferts when observed with adequate angular resolution and sensitivity"
] | [
"Background"
] | [
[
960,
979
]
] | [
[
800,
958
]
] |
2017ApJ...845...92R__Mosqueira_&_Estrada_2003a_Instance_1 | Concerning case (1), the first explanation that has been proposed is an increasing relative velocity among the building blocks with decreasing distance from the planet leading to substantial water loss in the case of the most energetic impacts (Estrada & Mosqueira 2006), which occurred closer to Jupiter. Nonetheless, t... | [
"Mosqueira & Estrada 2003a"
] | [
"In this case, bodies that formed inward of the snowline (Io) accreted from essentially water-poor building blocks, whereas bodies that formed outward of the snowline (Ganymede, Callisto) formed from a primordial mixture of water ice and silicates (e.g.,",
"Within this scenario, the low water content of Europa is... | [
"Background",
"Differences"
] | [
[
1095,
1120
]
] | [
[
822,
1075
],
[
1153,
1219
]
] |
2021AandA...646A..21C__Polyansky_et_al._(2018)_Instance_1 | (1a) Work is underway for an updated ExoMol line list for SiO which will extend into the ultraviolet. The current line list only considers vibration-rotation transitions and so the current maximum wavenumber was set at 6049 cm−1. (1b) The HITEMP line list for NO includes data from the ExoMol NOname line list (Wong et a... | [
"Polyansky et al. (2018)"
] | [
"whereas the more accurate ExoMol POKAZATEL line list",
"is complete up to 4000 K."
] | [
"Background",
"Background"
] | [
[
683,
706
]
] | [
[
630,
682
],
[
707,
732
]
] |
2022ApJ...935..148M__Shamasundar_et_al._2011_Instance_1 | Using the high-level ab initio calculations implemented in the MOLPRO 2015 software package (Werner et al. 2015, 2020), the electronic structures of CO have been determined. In our calculations, the molecular orbitals (MOs) and ground-state energies are computed by the HF method. Then, the CASSCF method (Knowles & Wern... | [
"Shamasundar et al. 2011"
] | [
"Finally, based on the CASSCF wave functions, the internally contracted multi-reference configuration interaction method with the Davidson correction (icMRCI+Q)",
"is performed to consider the dynamic correlation and size-consistency error."
] | [
"Uses",
"Uses"
] | [
[
729,
752
]
] | [
[
502,
661
],
[
754,
830
]
] |
2019MNRAS.487.3702O__Owen_et_al._2011b_Instance_1 | The photoevaporation model successfully explains the ‘two-time-scale’ nature of protoplanetary disc evolution, where the inner regions of protoplanetary discs appear to evolve slowly on Myr time-scales, before dispersing on a much more rapid time-scale (e.g. Kenyon & Hartmann 1995; Ercolano, Clarke & Hall 2011; Koepfer... | [
"Owen et al. 2011b"
] | [
"This final long-lived stage of disc dispersal gives rise to transition discs which have lifetimes between 105 and 106 yr, but remain optically thick – ‘relic discs’"
] | [
"Background"
] | [
[
1764,
1781
]
] | [
[
1598,
1762
]
] |
2020ApJ...898...49N__Sowmya_et_al._2014_Instance_1 | In the line cores of Q/I and U/I profiles, we see depolarization and rotation for fields in the range
G. These are due to the Hanle effect. For
G, we see the signatures of level-crossings in the line cores of (Q/I, U/I) profiles, namely they tend toward the non-magnetic value (see Figures 1(b) and 2(b)). ... | [
"Sowmya et al. 2014"
] | [
"We recall that, traditionally the loops in the polarization diagram (namely, a plot of Q/I versus U/I for a given wavelength and for a range of magnetic field strength or orientation values) are identified to be due to the level-crossings in the incomplete PBE regime",
"see also"
] | [
"Background",
"Background"
] | [
[
661,
679
]
] | [
[
320,
587
],
[
652,
660
]
] |
2020ApJ...888..126Z__Warren_et_al._2006_Instance_1 | Achondritic meteorites are fragments of differentiated asteroids or planetary bodies of the solar system. Ureilites are coarse-grained ultramafic (olivine–pyroxene) achondrites. They include accessory minerals of metal and sulfide associated with high abundances of carbon phases (on average 3 vol% and up to ∼7 vol%; Go... | [
"Warren et al. 2006"
] | [
"The main group ureilites represent the mantle residues after the extraction of",
"and a sulfur-rich iron melt"
] | [
"Background",
"Background"
] | [
[
884,
902
]
] | [
[
671,
749
],
[
833,
860
]
] |
2018AandA...618A..38K__Kirchschlager_&_Wolf_2013_Instance_1 | In Fig. 1, we investigate the dust grain size distributions at the periastron and apastron of debris disks a belt eccentricity of eb = 0.4 (with dynamical excitation Δeb = 0.1) for different material strengths. Since the radiation pressure has a strong influence on the cutoff in the grain size distribution at smallest ... | [
"Kirchschlager & Wolf 2013"
] | [
"We note that the blowout size can be increased with particle porosity and increasing stellar temperature"
] | [
"Uses"
] | [
[
542,
567
]
] | [
[
417,
521
]
] |
2021ApJ...910...84E__Rappazzo_&_Velli_2011_Instance_1 | Based on these results, a series of 3D numerical simulations solving the simplified reduced magnetohydrodynamic (RMHD) equations, introduced by Strauss (1976), in Cartesian geometry were performed. The goal of these simulations was twofold: (1) to determine how a coronal loop responds to different photospheric velocity... | [
"Rappazzo & Velli 2011"
] | [
"The goal of these simulations was twofold: (1) to determine how a coronal loop responds to different photospheric velocity patterns, and (2) to investigate how the electric current sheets are formed, as well as the details of the heating that occurs through the dissipation of magnetic energy"
] | [
"Motivation"
] | [
[
526,
547
]
] | [
[
198,
490
]
] |
2022AandA...665A.115C__Clark_&_Steele_(2000)_Instance_2 | While different studies devoted to the near-IR spectra of Be stars show low-resolution data, many of them are restricted to a small sample, and some others analyse reduced spectral ranges. For instance, there are only a few studies done in the J band, and they focus mainly on a particular object or a specific spectral ... | [
"Clark & Steele (2000)"
] | [
"related the infrared characteristics to the underlying properties of the stars: objects that present He i features in emission or absorption are B3 or earlier; if the star presents Mg ii in emission but no He i, it is between B2 and b4; objects with Brγ emission but no evidence of He i or Mg ii are B5 or later."
] | [
"Background"
] | [
[
1749,
1770
]
] | [
[
1771,
2083
]
] |
2022MNRAS.511.1819S__Bengaly_et_al._2019_Instance_1 | A sky survey at multiple frequencies, carried out with the Square Kilometre Array (SKA) could be used for an independent investigation of the controversial dipole anisotropy with a much superior sensitivity and thereby settle the question of the CP, hopefully, in a more decisive manner. In fact it was argued by Crawfor... | [
"Bengaly et al. 2019"
] | [
"Although SKA might provide number counts at sub-µJy levels",
"however, one may need to be wary of possible caveats in using radio source number counts at these flux-density levels as one might start seeing at sub-mJy levels, in addition to the powerful distant radio sources, a substantially increasing fraction o... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1167,
1186
]
] | [
[
1086,
1144
],
[
1189,
1561
]
] |
2021ApJ...909..175Y__Buzzicotti_et_al._2018_Instance_3 | The filtered MHD equations read
11
12
where we sum over repeated indices, and
13
14
15
16
denote the inertial (I), Maxwell (M), advective (A), and dynamo (D) subfilter-scale stresses, respectively. Despite their common origin through the electric field in the induction equation, we... | [
"Buzzicotti et al. 2018"
] | [
"However, the energy balance equations can be expressed in an alternative way by including terms that vanish under spatial averaging and ensure Galilean invariance of all terms"
] | [
"Uses"
] | [
[
1468,
1490
]
] | [
[
1291,
1466
]
] |
2015AandA...580A..71L__Sutton_et_al._(2013)_Instance_2 | The simplest two component model (power law + disk) is a phenomenological model often used to describe the spectra of ULXs as an empirical description of a disk plus corona geometry. In the presence of a cool (kT ~ 0.1−0.4 keV) and luminous (L ~ 1039−1040 erg/s) disk, it allows inferring the presence of intermediate-ma... | [
"Sutton et al. (2013)"
] | [
"Our result is consistent with that found by",
"using XMM-Newton data,",
"and, according to their classification, it identifies M33 X-8 as a broadened disk source, or in other words, as a source whose spectrum is dominated by emission from a hot disk (see Table 2) and where the additional soft component may be ... | [
"Similarities",
"Similarities",
"Uses"
] | [
[
1412,
1432
]
] | [
[
1368,
1411
],
[
1433,
1455
],
[
1456,
1776
]
] |
2021AandA...648A..73B__Marois_et_al._2008_Instance_1 | We present the photometry of the companion in Fig. 4 in a color-magnitude diagram. The corresponding numerical values are reported in Table 2. YSES 2b is consistent with a late L to early T spectral type when comparing it to colors of field brown dwarfs from the NIRSPEC Brown Dwarf Spectroscopic Survey (McLean et al. 2... | [
"Marois et al. 2008"
] | [
"In color-magnitude space, YSES 2b is very close to the innermost three planets of the HR 8799 multi-planetary system"
] | [
"Compare/Contrast"
] | [
[
1133,
1151
]
] | [
[
1015,
1131
]
] |
2019AandA...622A.180L__Cappellari_et_al._2011_Instance_1 | Large spectroscopic and photometric surveys, such as the Sloan Digital Sky Survey (SDSS, York et al. 2000), have revolutionized astrophysics in many fields, but can only deliver a limited view of the star formation activity in the local universe, given that instruments have a small field of view (FoV) in the case of sp... | [
"Cappellari et al. 2011"
] | [
"In recent years, integral field spectroscopic (IFS) surveys",
"have overcome these problems with the use of instruments with larger FoVs and a fully spectral coverage (e.g",
"ATLAS3D,"
] | [
"Background",
"Background",
"Background"
] | [
[
729,
751
]
] | [
[
404,
463
],
[
584,
692
],
[
720,
728
]
] |
2022ApJ...934...73A__Ryan_et_al._2011_Instance_1 | In contrast, deep narrow-field surveys can reach more distant UCD populations, enabling measurement of disk structure and a greater proportion of halo and thick disk sources. The majority of deep surveys for UCDs (Table 1) have been undertaken with the Hubble Space Telescope (HST), as these objects often comprise a for... | [
"Ryan et al. 2011"
] | [
"subsequently identified 17 candidate late-M, L, and T dwarfs in 232 arcmin2 of HST/Wide Field Camera 3 (WFC3) imaging of the Great Observatories Origins Deep Survey",
"using optical and near-infrared color selection, and determined a thin disk vertical scaleheight for these sources of 290 ± 40 pc."
] | [
"Background",
"Background"
] | [
[
1194,
1210
]
] | [
[
1212,
1376
],
[
1402,
1532
]
] |
2018AandA...613A...3Q__Kelly_et_al._2017_Instance_2 | As a prototypical Seyfert 2 galaxy with starburst at a distance of 14.4 Mpc (1″ = 72 pc, Bland-Hawthorn et al. 1997), NGC 1068 was observed at radio (Greenhill et al. 1996), millimeter (Schinnerer et al. 2000), infrared (Jaffe et al. 2004), optical (Antonucci & Miller 1985), UV (Antonucci et al. 1994), and X-ray (Kinkh... | [
"Kelly et al. 2017"
] | [
"The spatially resolved observations showed that the CND region was a complex dynamical system. For instance, the east and west dots were dominated by a fast shock and a slower shock"
] | [
"Background"
] | [
[
2225,
2242
]
] | [
[
2042,
2223
]
] |
2022MNRAS.512..439C__Johnson,_Sangwan_&_Shankaranarayanan_2022_Instance_1 | It is still unclear whether this incompatibility is evidence against the spatially flat ΛCDM model or is caused by unidentified systematic errors in one of the established cosmological probes or by evolution of the parameters themselves with the redshift (Dainotti et al. 2021b, 2022). Newer, alternate cosmological prob... | [
"Johnson, Sangwan & Shankaranarayanan 2022"
] | [
"Newer, alternate cosmological probes could help alleviate this issue.",
"Recent examples of such probes include",
"H ii starburst galaxy measurements that reach to z ∼ 2.4"
] | [
"Motivation",
"Background",
"Background"
] | [
[
736,
777
]
] | [
[
286,
355
],
[
356,
394
],
[
555,
611
]
] |
2015AandA...573A.102B__Fernández_et_al._1999_Instance_1 | The cumulative total absolute magnitude distribution of the comets obeys N( HT) ∝ 10− αTHT. Since we have imposed that the total brightness of the comets scales as BT ∝ fD2, it is easy to show that the slope of the total absolute magnitude distribution, αT, is equal to the slope of the nuclear absolute magnitude distr... | [
"Fernández et al. 1999"
] | [
"Even though there is a lot of scatter in the D − HT diagram caused by variation in f from one comet to the next"
] | [
"Uses"
] | [
[
543,
564
]
] | [
[
430,
541
]
] |
2017MNRAS.471.4286F__Colpi_2014_Instance_1 | Following the first detection by ROSAT (Komossa & Bade 1999; Bade, Komossa & Dahlem 2016), about 50 TDEs have been observed (Komossa 2015) in hard X-ray (Bloom et al. 2011; Burrows et al. 2011; Cenko et al. 2012; Pasham et al. 2015), soft X-ray (Komossa & Bade 1999; Donley et al. 2002; Esquej et al. 2008; Maksym et al.... | [
"Colpi 2014"
] | [
"This candidate appears to have one of the most compact orbits among the known SMBH binaries and has overcome the ‘final parsec problem’"
] | [
"Compare/Contrast"
] | [
[
1049,
1059
]
] | [
[
912,
1047
]
] |
2022MNRAS.517.4529B__Zaroubi,_Hoffman_&_Dekel_1999_Instance_1 | The other criteria that we can use to categorize the reconstruction methods is whether the reconstruction is performed using forward-modelling or uses a direct inversion from the data. Inverting non-linear problems from partial, noisy, observations is an ill-posed inverse problem, which makes forward-modelled Bayesian ... | [
"Zaroubi, Hoffman & Dekel 1999"
] | [
"The simplest of such methods uses a Wiener filtering technique",
"This approach assumes that the density/velocity field is described as a Gaussian random field and the Wiener filtered reconstruction is the maximum-a-posteriori (MAP) solution for the problem."
] | [
"Background",
"Background"
] | [
[
975,
1004
]
] | [
[
911,
973
],
[
1007,
1199
]
] |
2020AandA...641A.155V__Elmegreen_et_al._2007_Instance_1 | It has also become evident that the normalization of the MS rapidly increases with redshift: distant galaxies form stars at higher paces than in the local Universe, at fixed stellar mass (e.g., Daddi et al. 2007; Elbaz et al. 2007; Whitaker et al. 2012; Speagle et al. 2014; Schreiber et al. 2015). This trend could be e... | [
"Elmegreen et al. 2007"
] | [
"Moreover, higher SFRs could be induced by an increased efficiency of star formation due to the enhanced fragmentation in gas-rich, turbulent, and gravitationally unstable high-redshift disks",
"reflected on their clumpy morphologies"
] | [
"Background",
"Background"
] | [
[
961,
982
]
] | [
[
636,
826
],
[
921,
959
]
] |
2016ApJ...820..113J__Malanushenko_et_al._2009_Instance_1 | There have been previous studies that utilized coronal extreme ultraviolet (EUV) images in combination with models to try to more accurately determine the magnetic field. Conlon and Gallagher (Conlon & Gallagher 2010) used Extreme Ultraviolet Imager (EUVI) images to choose the best value of the parameter α in an LFFF m... | [
"Malanushenko et al. 2009"
] | [
"Malanushenko and co-authors",
"have presented a method for deriving an NLFFF model from sparsely distributed EUV loop observations.",
"These studies have focused on modeling the field in active regions, where the high density results in bright EUV emission and the limited size of the region allows for a reason... | [
"Background",
"Background",
"Compare/Contrast"
] | [
[
748,
772
]
] | [
[
719,
746
],
[
780,
880
],
[
881,
1497
]
] |
2015AandA...584A..75V__Essen_et_al._(2014)_Instance_7 | The data presented here comprise quasi-simultaneous observations during secondary eclipse of WASP-33 b around the V and Y bands. The predicted planet-star flux ratio in the V-band is 0.2 ppt, four times lower than the accuracy of our measurements. Therefore, we can neglect the planet imprint and use this band to measur... | [
"von Essen et al. (2014)"
] | [
"and we restricted them to the limiting cases derived in Sect. 3.5 of",
"rather than allowing them to take arbitrary values."
] | [
"Uses",
"Uses"
] | [
[
1830,
1853
]
] | [
[
1761,
1829
],
[
1855,
1906
]
] |
2021MNRAS.503..354G__Hou_&_Han_2014_Instance_2 | The spatial distribution of OB stars and associations, young long-period Cepheids and open clusters, star-forming regions, H ii regions, interstellar dust, and giant molecular and neutral gas clouds in the solar vicinity that have been in existence generally τ ≲ 108 yr is known to correlate with the location of the inn... | [
"Hou & Han 2014"
] | [
"The radial distance between the centres of the Orion and Sagittarius arms near the Sun is λrad ≈ 2 kpc (cf."
] | [
"Background"
] | [
[
1883,
1897
]
] | [
[
1775,
1882
]
] |
2019ApJ...871...82G__Tarr_et_al._2014_Instance_1 | By considering the UV emission at several wavelengths, we have been able to reconstruct the evolution of the EFR at different layers using radiance maps. The optically thin view provided by the O i λ1355.6 line (Lin & Carlsson 2015) images the AFS that formed above the EFR. AFSs are typically observed in absorption in ... | [
"Tarr et al. 2014"
] | [
"They also can reconnect with the ambient field (e.g.,"
] | [
"Background"
] | [
[
584,
600
]
] | [
[
506,
559
]
] |
2017AandA...603A.107A__Leconte_et_al._(2015)_Instance_1 | The second equation of our system is the conservation of mass, (12)\begin{equation} \dfrac{\partial \rho}{\partial t} + \boldsymbol{\nabla}. \left( \rho {\vec V} \right) = 0, \end{equation}∂ρ∂t+∇.ρV=0,which, in spherical coordinates, writes (13)\begin{equation} \dfrac{\partial \delta \rho}{\partial t } + \frac{1}{r^2} ... | [
"Leconte et al. (2015)"
] | [
"However, recent numerical simulations of thermal tides in optically thick atmospheres by",
"show behaviour of the flow that is in good agreement with a model that uses radiative cooling.",
"Therefore, in this work we assumeNewtonian cooling as a first model of the action of radiation on atmospheric tides."
] | [
"Similarities",
"Similarities",
"Uses"
] | [
[
2251,
2272
]
] | [
[
2162,
2250
],
[
2273,
2367
],
[
2368,
2484
]
] |
2019AandA...629A..63J__XIX_2015_Instance_1 | Our knowledge of magnetic fields in molecular clouds is based mainly on light polarisation, the optical and near-infrared (NIR) observations of background stars (Goodman et al. 1995; Whittet et al. 2001; Pereyra & Magalhães 2004; Alves et al. 2008; Chapman et al. 2011; Cox et al. 2016; Neha et al. 2018; Kandori et al. ... | [
"Planck Collaboration Int. XIX 2015"
] | [
"The Planck survey provides a large amount of data for polarisation studies at cloud scales"
] | [
"Background"
] | [
[
656,
690
]
] | [
[
529,
619
]
] |
2017AandA...604A.118T__Pilkington_et_al._(2012)_Instance_1 | A large effort has been invested in understanding the chemical patterns of galaxies using analytical and numerical chemical modelling (e.g. Brook et al. 2007; Calura et al. 2012; Mollá et al. 2015). In particular, hydrodynamical simulations provide the chemical enrichment of baryons as galaxies are assembled in a cosmo... | [
"Pilkington et al. (2012)"
] | [
"carried out a comparison of the metallicity gradients in the ISM (traced by young SPs) obtained by different numerical and analytical models"
] | [
"Background"
] | [
[
530,
554
]
] | [
[
555,
695
]
] |
2017AandA...600A..67P__Nakariakov_et_al._2003_Instance_1 | Many theoretical models have been proposed to explain the generation of QPPs. The most elaborated model of QPPs considers MHD oscillations, which affect almost all aspects of the flare emission generation. Indeed, QPPs are involved in triggering the magnetic reconnection, modulating the reconnection rate, accelerating ... | [
"Nakariakov et al. 2003"
] | [
"Different MHD oscillation modes have been identified to be responsible for QPPs in a single flaring loop"
] | [
"Background"
] | [
[
812,
834
]
] | [
[
706,
810
]
] |
2017MNRAS.472..205S__Becerra_et_al._2015_Instance_1 | Throughout the initial collapse the halo structure is well approximated by ellipsoidal collapse models. We therefore explore radial profiles of various physical quantities to extract information about the galactic environment. The density is illustrated in Fig. 2, which is reasonably approximated by a broken power law ... | [
"Becerra et al. 2015"
] | [
"If the evolution proceeds under self-similar, isothermal collapse then the break in the profile will shift to smaller scales, eventually reaching the radius of the protostar"
] | [
"Uses"
] | [
[
845,
864
]
] | [
[
643,
816
]
] |
2021ApJ...910..120K__Schlafly_et_al._2018_Instance_1 | Many of these objects have been confirmed as DNe through an identification spectrum or a measurement of the superhump period, but we find that 27 sources were not confirmed through any method. Quiescent multiband photometry of these remaining candidates can provide insights into the distance and ultimately constrain th... | [
"Schlafly et al. 2018"
] | [
"As described in Section 2.4, we find quiescent counterparts in Pan-STARRS and also add in coverage of southerly declinations by using the DeCAPS catalog (",
"; cross-matching for both catalogs is as explained in Appendix A.3)."
] | [
"Uses",
"Uses"
] | [
[
1011,
1031
]
] | [
[
857,
1011
],
[
1031,
1099
]
] |
2022AandA...666A..95H__Hartman_et_al._2022_Instance_1 | Scaling relations for the core radii rc, core densities δc, and core masses Mc as functions of the total halo mass M200 were fitted to the simulated halo populations, which largely agree with hydrostatic considerations of the halo cores where rc is nearly constant, as well as velocity dispersion tracing in the halo env... | [
"Hartman et al. 2022"
] | [
"However, these trends do not agree with those obtained by fitting the Burkert profile to nearby galaxies in the SPARC dataset and the classical Milky Way dSphs. This poses an issue for SIBEC-DM with Rc ≳ 1 kpc and a largely CDM-like matter power spectrum at late times",
"as was used in our simulations, although ... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
789,
808
]
] | [
[
392,
660
],
[
811,
891
]
] |
2021ApJ...919..140S__Bartos_et_al._2017_Instance_1 | Resonant dynamical friction may have applications beyond the relaxation of IMBHs examined in this paper. It may affect all objects in stellar clusters much more massive than the individual constituents of the disk, if present, including massive stars, stellar mass black holes (BHs), or the center of mass of massive bin... | [
"Bartos et al. 2017"
] | [
"Previously, it has been argued that stars and BHs crossing the disk on low-inclination orbits get captured by Chandrasekhar dynamical friction into the disk"
] | [
"Background"
] | [
[
639,
657
]
] | [
[
481,
637
]
] |
2022MNRAS.516.4833J__Munday_et_al._2020_Instance_1 | Bond & Ciardullo (2018) identify a periodicity of 2.06 d in their data, with a similar period clearly evident in the newly acquired data. However, no single period and time of first minima could be found that fits all the data (perhaps not unexpected given that the variability is clearly not constant, see Section 2.3 f... | [
"Munday et al. 2020"
] | [
"Given the nature of the variability, we measure the period via the reduced χ2 of a sinusoidal fit as a function of frequency (ideally suited to sinusoidal variability, e.g."
] | [
"Uses"
] | [
[
750,
768
]
] | [
[
550,
722
]
] |
2022MNRAS.516.3175B__Law_et_al._2015_Instance_1 | We use the final version of the MaNGA data (Abdurro’uf et al. 2022). MaNGA is the survey project in SDSS-IV (Sloan Digital Sky Survey) using IFU observations of galaxies to produce spatially resolved spectroscopic data (Gunn et al. 2006; Bundy et al. 2015; Drory et al. 2015; Blanton et al. 2017; Aguado et al. 2019; Abd... | [
"Law et al. 2015"
] | [
"MaNGA observed approximately 10 000 galaxies, selected as an unbiased sample in terms of stellar mass (${\\it M}_{\\star } \\gt 10^{9}\\, {\\rm M}_{\\odot }$) and environments"
] | [
"Background"
] | [
[
513,
528
]
] | [
[
342,
511
]
] |
2020MNRAS.492.5247S__Sasaki_et_al._2018_Instance_1 | A lognormal mass function:
(7)$$\begin{eqnarray}
\psi (M;\mu ,\sigma)=\frac{1}{M\sqrt{2\pi \sigma ^2}}\exp {\left(- \frac{\ln ^2(M/\mu)}{2\sigma ^2}\right)},
\end{eqnarray}$$where μ > 0 and σ > 0. The mean PBH mass in the assumption of a lognormal mass function is $\bar{M}=\mu \exp \left(-\sigma ^2/2\right)$. Such ma... | [
"Sasaki et al. 2018"
] | [
"The (μ, σ) pairs allowed in the window relevant for the operational gravitational wave detectors",
"are mainly constrained by (i) the results from searches for microlensing events on stars in our Galactic neighbourhood and (ii) the effect PBH gas accretion would have on the CMB temperature and ionization history... | [
"Uses",
"Uses"
] | [
[
914,
932
]
] | [
[
506,
602
],
[
681,
894
]
] |
2021MNRAS.507.5882S__Mackereth_et_al._2018_Instance_3 | Cosmological hydro dynamical N-body simulations offer another possibility to investigate the origin of the bimodality in the ([Fe/H], [α/Fe]) plane. Earlier simulations, e.g. full N-body simulations by Loebman et al. (2011), Brook et al. (2012) or hybrid simulations in which a semi-analytic chemical evolution was added... | [
"Mackereth et al. (2018)"
] | [
"attribute the bimodality to unusually rapid gas accretion at earlier times, which is also characterized by a short time-scale to convert gas to stars."
] | [
"Compare/Contrast"
] | [
[
2232,
2255
]
] | [
[
2256,
2406
]
] |
2021AandA...648A.109G__Talon_&_Charbonnel_2005_Instance_1 | The transport of angular momentum (AM) and chemical elements in stars strongly affects their evolution, from pre-main sequence (PMS) to evolved stages. These processes are particularly crucial in the stellar radiative zones, but their modelling remains an open question. In standard evolution models, these stably strati... | [
"Talon & Charbonnel 2005"
] | [
"The importance of additional processes such as internal waves (e.g.,"
] | [
"Background"
] | [
[
839,
862
]
] | [
[
770,
838
]
] |
2020MNRAS.492.5247S__Sasaki_et_al._2018_Instance_2 | A lognormal mass function:
(7)$$\begin{eqnarray}
\psi (M;\mu ,\sigma)=\frac{1}{M\sqrt{2\pi \sigma ^2}}\exp {\left(- \frac{\ln ^2(M/\mu)}{2\sigma ^2}\right)},
\end{eqnarray}$$where μ > 0 and σ > 0. The mean PBH mass in the assumption of a lognormal mass function is $\bar{M}=\mu \exp \left(-\sigma ^2/2\right)$. Such ma... | [
"Sasaki et al. 2018"
] | [
"Additionally, wide binaries are in principle hard to detect, yielding some uncertainty in identifying them and consequently in drawing any conclusion on the PBH abundance"
] | [
"Uses"
] | [
[
2042,
2060
]
] | [
[
1870,
2040
]
] |
2019AandA...632A.129W__Feng_&_Wang_2015_Instance_2 | In this study, the 272 eV suprathermal electron pitch-angle distributions (PADs) measured by ACE are used. The electron PADs are obtained from the Solar Wind Electron Proton Alpha Monitor (SWEPAM) with angular and time resolutions of 9° and 64 s respectively (McComas et al. 1998). Here we examined 16 s average magnetic... | [
"Feng & Wang 2015"
] | [
"The high Fe charge states (⟨Fe⟩ ≥ 12) and abnormally high O7+/O6+ ratio (≥1) are the result of flare-related heating in the corona",
"and therefore they are independently reliable ICME indicators"
] | [
"Uses",
"Uses"
] | [
[
1189,
1205
]
] | [
[
955,
1085
],
[
1126,
1187
]
] |
2021ApJ...906...57S__Lee_et_al._2016_Instance_1 | Complementary to studies using the integrated emission and angular power spectrum of DM annihilation from a population of Galactic subhalos, in this paper we present a novel strategy using one-point photon statistics to search for the annihilation signature. Our technique takes advantage of the information in the entir... | [
"Lee et al.",
"2016",
"Lee et al. 2016"
] | [
"We introduce a method to search for signatures of DM annihilation from a Galactic subhalo population using the non-Poissonian template fitting (NPTF) framework",
"which has previously been applied to characterize unresolved point sources in the inner Galaxy"
] | [
"Uses",
"Motivation"
] | [
[
922,
932
],
[
939,
943
],
[
1069,
1084
]
] | [
[
739,
898
],
[
973,
1067
]
] |
2018ApJ...868..139W__Schlickeiser_&_Jenko_2010_Instance_2 | By radio continuum surveys of interstellar space and direct in situ measurements in the solar system, it is well established that for many scenarios the background magnetic fields are spatially varying. However, the above research about parallel and perpendicular diffusion only explored the uniform mean magnetic field.... | [
"Schlickeiser & Jenko 2010"
] | [
"By using the truncating method to neglect the higher-order derivative terms, the approximate correction formulas of parallel or perpendicular diffusion coefficients were obtained (see, e.g.,"
] | [
"Background"
] | [
[
1783,
1808
]
] | [
[
1563,
1753
]
] |
2019AandA...630A..37S__Behar_et_al._2017_Instance_2 | 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"
] | [
"For instance, partial ring distributions were frequently observed for solar wind protons at intermediate heliocentric distances, when the spacecraft approached the SWIC"
] | [
"Background"
] | [
[
892,
909
]
] | [
[
722,
890
]
] |
2020ApJ...895...82V__Fryer_et_al._2018_Instance_2 | The shock is then revived by adding an energy injection following the parameterized method of Fryer et al. (2018). In this model, roughly
was deposited into the inner
in the first
. Some of this energy is lost through neutrino emission and the total explosion energy at late times for this model is
... | [
"Fryer et al. 2018"
] | [
"We note that our 1D methods employed for modeling the collapse, core bounce, and initial explosion do not capture the full physics of the central engine (for a discussion, see",
"and this is a source of uncertainty in our yield calculations."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
737,
754
]
] | [
[
561,
736
],
[
757,
819
]
] |
2019AandA...627A.130D__Broadhurst_et_al._2019_Instance_1 | Gravitational-wave astronomy has recently become a reality with the first detection of gravitational waves (GW hereafter) by the Laser Interferometer Gravitational-Wave Observatory (LIGO) and Virgo ground-based interferemeters. To date, eleven events have been reported by the LIGO and Virgo detectors (Abbott 2018), and... | [
"Broadhurst et al. 2019"
] | [
"Some of these events may correspond to gravitationally lensed events with magnification factors ranging from a few tens to a few hundreds"
] | [
"Background"
] | [
[
605,
627
]
] | [
[
394,
531
]
] |
2019MNRAS.484.1946G__Biesiadzinski_et_al._2012_Instance_1 | Secondly, we focus on galaxies to discuss some remaining solutions. The miscentring (e.g. A1986, A1961) decreases the X-ray luminosity/SZ signal, as some flux moves outside of the aperture. Sehgal et al. (2013) demonstrated the effect of miscentring on decreasing SZ signal. They also proposed that the miscentring effec... | [
"Biesiadzinski et al. 2012"
] | [
"Moreover, most miscentred clusters are merging or disturbed clusters with lower X-ray or SZ surface brightness, which makes them more difficult to be detected. The discrepancy of SZ signal is at a level of 10 per cent in our richness range"
] | [
"Compare/Contrast"
] | [
[
846,
871
]
] | [
[
605,
844
]
] |
2021MNRAS.503.5385Z__Barnes_et_al._2001_Instance_1 | ‘Blind’ searches through H i surveys performed by large aperture single-dish telescopes provide chances to uncover more H i absorption systems. Although such surveys usually utilize the non-tracking, drift scan observing strategy, with integration time for each individual source is limited, the collecting areas of the ... | [
"Barnes et al. 2001"
] | [
"Allison, Sadler & Meekin (2014) identified four H i absorbers, including one previously unknown source, with the archival data of the H i Parkes All-Sky Survey (H i PASS; see"
] | [
"Background"
] | [
[
566,
584
]
] | [
[
391,
565
]
] |
2022AandA...666A.134S__Snyder_et_al._2005_Instance_1 | Observation of amino acids and their most essential isomers and potential precursors in the interstellar medium (ISM) should be crucial for revealing the chemistry that may have led to life's origin (Ehrenfreund et al. 2001). In particular, the central question of whether glycine (CH2(NH2)C(O)OH) exists or not in the I... | [
"Snyder et al. 2005"
] | [
"In particular, the central question of whether glycine (CH2(NH2)C(O)OH) exists or not in the ISM is one of the most pursued targets in astrochemistry.",
"its detection has never been confirmed"
] | [
"Motivation",
"Motivation"
] | [
[
579,
597
]
] | [
[
226,
376
],
[
539,
577
]
] |
2015AandA...577A.118M__Swift_et_al._2011_Instance_1 | On the other hand, meteoroid rates on the Moon can be related to rates on Earth by taking into account the different gravitational focusing effect between both bodies. The gravitational focusing factor Φ is given by (6)\begin{equation} \Phi=1+\frac{V^{2}_{\rm esc}}{V^{2}}, \end{equation}Φ=1+Vesc2V2,where Vesc is the es... | [
"Swift et al. 2011"
] | [
"However, the masses corresponding to impact flashes recorded on the Moon are several orders of magnitudes larger than mo",
"This means that the minimum kinetic energy Emin to produce a detectable impact flash on the Moon is much higher than the kinetic energy of a portion of the meteoroids included in the comput... | [
"Differences",
"Uses"
] | [
[
4365,
4382
]
] | [
[
4189,
4309
],
[
4385,
4878
]
] |
2022ApJ...929....7V__Caprioli_&_Spitkovsky_2014a_Instance_1 | Diffusive shock acceleration (DSA), a process entering the category of first-order Fermi acceleration, is the process by which astrophysical shocks accelerate charged particles to relativistic speeds. DSA requires the magnetic field near the shock front to reflect the particle, leading to repeated shock-crossings with ... | [
"Caprioli & Spitkovsky 2014a"
] | [
"Simulations of this type seem to indicate that although this process is effective in the case of (quasi-)parallel shocks where the magnetic field is aligned with the direction of motion, it becomes ineffective once the angle between the magnetic field and the shock exceeds approximately 50°"
] | [
"Compare/Contrast"
] | [
[
1128,
1155
]
] | [
[
835,
1126
]
] |
2016AandA...593A..95C__Smith_1963_Instance_1 | Galactic fountains or infall are the possible origins for the ECs in this sample. Both scenarios present possible explanations and restrictions. The accretion of low metallicity gas from the intergalactic medium may occur through filamentary structures with the gas cooling into clouds (Fernández et al. 2012). Subsequen... | [
"Smith 1963"
] | [
"Star formation can be triggered by these interactions, within clouds that reach sufficient density (Figs. 9 and 10). However, there is evidence that star formation is possible only within dark-matter encapsulated HVCs such as the Smith Cloud"
] | [
"Compare/Contrast"
] | [
[
726,
736
]
] | [
[
483,
724
]
] |
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