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 |
|---|---|---|---|---|---|---|
2021AandA...651A.111P__Herrera-Camus_et_al._2018_Instance_1 | Irrespective of its origin, the [C II] emission is linked to the presence of stellar far-ultraviolet (FUV) photons (E 13.6 eV). As FUV photons are tied to the presence of massive O and B stars that have short lifetimes, the [C II] 158 μm line is also astar formation rate (SFR) indicator. Indeed, ISO, Herschel and SOFIA... | [
"Herrera-Camus et al. 2018"
] | [
"With ALMA and NOEMA, ground-based observations of the [C II] 158 μm line in high redshift galaxies have come into reach and such data are routinely used to infer SFRs",
"based upon validations of this relationship in the nearby Universe"
] | [
"Background",
"Background"
] | [
[
957,
982
]
] | [
[
606,
772
],
[
889,
955
]
] |
2018ApJ...853..131L__Renzini_2009_Instance_1 | Classifying galaxies into different star formation regimes at high redshift is facilitated by the fact that star formation rate (SFR) and stellar mass (M*) of star-forming galaxies (SFGs) are strongly correlated out to at least
(Daddi et al. 2007; Noeske et al. 2007; Pannella et al. 2009, 2015; Elbaz et al. 2011... | [
"Renzini 2009"
] | [
"A common interpretation of the MS is that the location of galaxies relative to the MS follows a different time evolution of SFR"
] | [
"Background"
] | [
[
641,
653
]
] | [
[
512,
639
]
] |
2017MNRAS.464.2120S__Diego_et_al._2015_Instance_1 | Hu, Holz & Vale (2007b) proposed the idea of using the ratio of CMB convergence to galaxy lensing convergence as a way to measure the distance ratio (distance to surface of last scattering relative to the distance to the source galaxy sample used to estimate the galaxy lensing) and hence constrain the geometry, Ωk and ... | [
"Diego et al. 2015"
] | [
"Several studies have already measured the distance ratios (e.g.",
"though they are afflicted by several systematics such as, uncertainties in modelling cluster profiles and cosmic variance in the case of multiple strong lens systems, and photometric redshift uncertainties as well as imaging systematics that caus... | [
"Background",
"Differences"
] | [
[
931,
948
]
] | [
[
847,
910
],
[
1018,
1333
]
] |
2021AandA...645A..96P__Marcantonio_et_al._(2018)_Instance_1 | The ESPRESSO DFS concept (Di Marcantonio et al. 2018) was conceived during its preliminary design phases with the goal of maximizing operational efficiency, flexibility, and scientific output while complying with the standard Paranal Observatory operational scheme. The main challenge derives from the requirement to ope... | [
"Di Marcantonio et al. 2018"
] | [
"The ESPRESSO DFS concept",
"was conceived during its preliminary design phases with the goal of maximizing operational efficiency, flexibility, and scientific output while complying with the standard Paranal Observatory operational scheme."
] | [
"Background",
"Background"
] | [
[
26,
52
]
] | [
[
0,
24
],
[
54,
265
]
] |
2019MNRAS.490.3588M__Burgio_et_al._2018_Instance_1 | In the era of gravitational wave and multimessenger astronomy of binary neutron stars accurate numerical modelling of neutron-star mergers and their remnants on long time-scales $\simeq 1\, \rm s$ has never been more important. The coincident detection of a gravitational-wave signal from a neutron-star merger (The LIGO... | [
"Burgio et al. 2018"
] | [
"A neutron-star merger consists of several stages starting from the late inspiral, where accurate numerical waveforms are needed to calibrate analytical models for waveforms, through merger",
"which requires sophisticated microphysics in terms of finite-temperature equations of state (EOS) satisfying recent obser... | [
"Motivation",
"Motivation"
] | [
[
1177,
1195
]
] | [
[
711,
899
],
[
966,
1107
]
] |
2022AandA...659A..21P__Khadka_et_al._2021_Instance_1 | Using Eq. (16), we derive the probability density in the parameter space (σDRW, RBLR) for a given set of parameters ⟨M⟩, fBLR, ve, and R0. By marginalising on ve and R0 we obtain the measurement of RBLR shown in Fig. 10. One could argue that we obtain a bi-modal distribution in the posterior probability for RBLR. This ... | [
"Khadka et al. 2021"
] | [
"Indeed, the Hβ",
"and Mg II lines seem to arise from the same part of the BLR in various quasars (e.g.,",
"and should both yield similar sizes; whereas the Fe II line is thought to arise from a larger part of the BLR",
"Therefore, the combination of the two signals modelled as a single BLR emission could bro... | [
"Uses",
"Uses",
"Uses",
"Uses"
] | [
[
659,
677
]
] | [
[
501,
515
],
[
551,
636
],
[
679,
788
],
[
867,
1011
]
] |
2018ApJ...854..137S__Zank_&_Matthaeus_1993_Instance_1 | Modulation in steady-state has been well studied by previous works (Potgieter 2013; Potgieter et al. 2014; Zhao et al. 2014). Potgieter et al. (2014) studied the modulation of proton spectra with the PAMELA data from 2006 to 2009 July, and they concluded that the recent solar minimum was “diffusion dominated.” In the w... | [
"Zank & Matthaeus 1993"
] | [
"In the solar wind, the evaluation of turbulence is well described by magnetohydrodynamic (MHD) theory",
"and the turbulence transport throughout the heliosphere has been studied over the years (e.g.,"
] | [
"Background",
"Background"
] | [
[
1416,
1437
]
] | [
[
1176,
1277
],
[
1321,
1415
]
] |
2018AandA...614A...9J__in_2017_Instance_1 | During our monitoring period V2492 Cyg remained always undetected at our sensitivity, therefore the light curve depicted in Fig. 1 displays only upper limit values at different levels, as explained in Sect. 3. As a consequence, no fading or outbursting event can be detected, nevertheless some useful information can be ... | [
"Giannini et al. (2018)"
] | [
"As mentioned above, after its discovery in 2010, V2492 underwent a long-lasting period of strong activity with intermittent burst and fading events",
"and reached its maximum recorded brightness in 2017"
] | [
"Background",
"Background"
] | [
[
575,
597
]
] | [
[
329,
476
],
[
523,
574
]
] |
2018ApJ...861....2T__Poisson_1999_Instance_1 | However, one can reduce the order of the LD equation using the method proposed in Landau & Lifshitz (1975), i.e., by rewriting the self-force in terms of the external force and the four-velocity of a particle. Substituting the higher-order terms in Equation (3) with the derivatives of the Lorentz force, we get the equa... | [
"Poisson 1999"
] | [
"This equation, usually referred to as the Landau–Lifshitz (LL) equation, has important consequences: it is of the second order, does not violate the principle of inertia, and the self-force vanishes in the absence of the external (Lorentz) force"
] | [
"Background"
] | [
[
617,
629
]
] | [
[
355,
600
]
] |
2020ApJ...904...11F__Zamirri_et_al._2019a_Instance_1 | BE values can also be obtained by means of computational approaches that, in some situations, can overcome the experimental limitations. Many computational works have so far focused on a few important astrochemical species like H, H2, N, O, CO, and CO2, in which BEs are calculated on periodic/cluster models of crystall... | [
"Zamirri et al. 2019a"
] | [
"Many computational works have so far focused on a few important astrochemical species like H, H2, N, O, CO, and CO2, in which BEs are calculated on periodic/cluster models of crystalline/amorphous structural states using different computational techniques (e.g.,"
] | [
"Background"
] | [
[
559,
579
]
] | [
[
137,
399
]
] |
2019ApJ...876...85R__Shappee_et_al._2014_Instance_1 | Next, we applied a correction for the expected difference between the magnitude of each Cepheid at the observed phase and the magnitude at the epoch of mean intensity of its light curve. These phase corrections are derived from ground-based light curves of each Cepheid in filters with wavelengths best corresponding to ... | [
"Shappee et al. 2014"
] | [
"For some Cepheids (OGL0434, OGL0501, OGL0510, OGL0512, OGL0528, OGL0545, OGL0590, OGL0712, OGL0757, OGL0966, and OGL0992), we also included V-band light curves from the",
"and/or ASAS-SN survey",
"to increase the baseline coverage."
] | [
"Uses",
"Uses",
"Uses"
] | [
[
1271,
1290
]
] | [
[
1050,
1218
],
[
1248,
1269
],
[
1314,
1348
]
] |
2021AandA...654A.141L__Li_2019_Instance_1 | The situation seems to be more complicated in luminous AGNs, which can be divided into radio-quiet (RQ) and radio-loud (RL) AGNs according to their radio loudness R (R = f5 GHz/f4400 Å, where f5 GHz and f4400 Å are the radio flux at 5 GHz and optical flux at 4400 Å, respectively, Kellermann et al. 1989). The accretion ... | [
"Li 2019",
"Li 2019"
] | [
"This model can naturally fit the observational positive relationships between αOX and λO as well as Γ and λO in RQAGNs",
"In observations, RLAGNs appear to have different properties than RQAGNs, for instance the positive relationships listed above in RQAGNs have not been found in RLAGNs"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
852,
859
],
[
1382,
1389
]
] | [
[
645,
763
],
[
1215,
1380
]
] |
2018ApJ...857...79J__Fadda_et_al._1996_Instance_1 | Finally, in order to measure the ICL fraction once we have a background-free ICL map, we created an image of the cluster removing the CHEF models of the foreground and background galaxies. As described in Jiménez-Teja & Benítez (2012), the cluster membership is determined in a two-step process, the PEAK+GAP algorithm (... | [
"Fadda et al. 1996"
] | [
"This crude selection of cluster member candidates is obviously prone to contamination by interlopers. So, we further refine it using the shifting gapper method",
"which uses velocity and spatial information on the candidates simultaneously. The shifting gapper method spatially distributes the candidates accordin... | [
"Uses",
"Background"
] | [
[
969,
986
]
] | [
[
808,
967
],
[
1050,
1875
]
] |
2017ApJ...850..195E__Lacy_et_al._1982_Instance_1 | RCW 57A (also known as NGC 3576, G291.27–0.70, or IRAS 11097–6102) is a H ii region associated with a filament and bipolar bubble, and is located at a distance of 2.4–2.8 kpc (Persi et al. 1994; de Pree et al. 1999). We adopt 2.4 kpc, which is within uncertainties of both the kinematic and spectroscopic determinations ... | [
"Lacy et al. 1982"
] | [
"The observed ratios of the infrared fine-structure ionic lines (Ne ii, Ar iii, and S iv;",
"indicate that at least eight O7.5V stars are necessary to account for the ionization of the region."
] | [
"Uses",
"Uses"
] | [
[
955,
971
]
] | [
[
866,
954
],
[
973,
1072
]
] |
2020ApJ...889...42B__Ricker_et_al._2014_Instance_1 | The characterization of the interior of observed exoplanets is one of the main goals in current exoplanetary science. With the large number of newly discovered exoplanets expected in the next 10 years by ground-based surveys such as the Wide Angle Search for Planets (WASP; Pollacco et al. 2006), the Next-Generation Tra... | [
"Ricker et al. 2014"
] | [
"With the large number of newly discovered exoplanets expected in the next 10 years by ground-based surveys such as",
"as well as the ongoing Transiting Exoplanet Survey Satellite (TESS) space survey",
"a rapid characterization scheme of the interior structure of these planets will become increasingly necessary... | [
"Background",
"Background",
"Motivation"
] | [
[
593,
611
]
] | [
[
118,
232
],
[
511,
591
],
[
703,
867
]
] |
2020MNRAS.497..687S__Dere_et_al._1997_Instance_1 | The object J004415.00 required our special consideration. We notice large variations of spectra at the hydrogen series limits. We designate the limits of the Balmer, Paschen, Brackett and Pfund series in Fig. 4 for J004415.00 with vertical arrows. A jump at the Brackett series limit in the IR spectrum can be clearly se... | [
"Dere et al. 1997"
] | [
"To take the contribution of f–f and f–b radiations into account and estimate the corresponding spectra, we used the chianti package"
] | [
"Uses"
] | [
[
868,
884
]
] | [
[
735,
866
]
] |
2022AandA...663A.105P__Weeren_et_al._2009b_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... | [
"van Weeren et al. 2009b"
] | [
"The Largest Linear Sizes (LLS) and radio powers of relics are correlated, as well as the integrated spectral index and the radio power"
] | [
"Background"
] | [
[
750,
773
]
] | [
[
614,
748
]
] |
2019AandA...627A.172R__Rozitis_&_Green_(2013)_Instance_2 | For comparisons with the light curve YORP constraints, the YORP effect acting on Cuyo could be predicted by computing the total recoil forces and torques from reflected and thermally emitted photons from the asteroid surface using the ATPM. These calculations were made for both a smooth and rough surface, and were aver... | [
"Rozitis & Green 2013"
] | [
"Since the light curve inversion produced convex shape models only, then shadowing and self-heating effects inside global-scale concavities (see",
") were not possible to model."
] | [
"Differences",
"Differences"
] | [
[
872,
892
]
] | [
[
728,
871
],
[
892,
921
]
] |
2016ApJ...832..128C___1983a_Instance_1 | The understanding of proton acceleration at the Sun in large solar energetic particle (SEP) events has oscillated between flare and shock pictures (Cliver 2009b; Reames 2015). The earliest picture following the discovery of ground-level events (GLEs; major SEP events requiring >500 MeV protons) by Forbush (1946) was th... | [
"Cliver et al.",
"1983a"
] | [
"Through the work of Švestka & Fritzová-Švestková (1974), Kahler et al. (1978, 1984)",
"(1982",
"1983b), Cane & Stone (1984), Klecker et al. (1984), Mason et al. (1984, 1986), Meyer (1985), Reames et al. (1985, 1994, 1996), Cane et al. (1986, 1988), Luhn et al. (1987), Reames (1990, 1999), Kahler (1992, 1994), ... | [
"Background",
"Background",
"Background"
] | [
[
847,
860
],
[
868,
873
]
] | [
[
762,
845
],
[
861,
866
],
[
875,
1456
]
] |
2018ApJ...865...60V__Baym_et_al._1969_Instance_1 | The core of a neutron star is composed primarily of neutrons, with ∼5%–10% of the mass in protons; for the electrically neutral medium, the number density of electrons is equal to that of the protons. At the supranuclear densities of the outer core, the Fermi energy for protons and neutrons is well above the typical te... | [
"Baym et al. 1969"
] | [
"At the supranuclear densities of the outer core, the Fermi energy for protons and neutrons is well above the typical temperature of a mature neutron star, and both the neutrons and protons are expected to condense into Bardeen–Cooper–Schrieffer superfluids, with 3PF2 and 1S0 Cooper pairing, respectively"
] | [
"Uses"
] | [
[
520,
536
]
] | [
[
201,
505
]
] |
2022ApJ...937L..34K__Narayan_et_al._2012_Instance_1 | We consider a radio galaxy of SMBH mass M = 109
M
9
M
⊙ with a mass accretion rate of
Ṁ=ṁLEdd/c2≃1.4×1022M9ṁ−4gcm−2
, where c is the speed of light and L
Edd is the Eddington luminosity. The gravitational radius of the BH is r
g
= GM/c
2 ≃ 1.5 × 1014
M
9 cm. We consider that the accretion flow is in the MAD s... | [
"Narayan et al. 2012"
] | [
"where Φmad ≈ 50Φmad,1.7 is the saturated magnetic flux"
] | [
"Uses"
] | [
[
568,
587
]
] | [
[
486,
540
]
] |
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