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 |
|---|---|---|---|---|---|---|
2015MNRAS.446..330W__Milgrom_2009c_Instance_1 | Consider a space–time scale invariance of the equations of motion under the consideration of the transformation in Minkowsky space (Milgrom 2009a; see also Milgrom 2014a,b):
(3)
\begin{equation}
(t,{\boldsymbol r}) \rightarrow (\lambda t,\lambda {\boldsymbol r}),
\end{equation}
where t and ${\boldsymbol r}=(x,y,z)$ a... | [
"Milgrom 2009c"
] | [
"Linking purely gravitational interactions to symmetries such as defined in equation (3) suggests deeper physics and constitutes a motivation for viewing MOND as much more than a mere phenomenological description of galactic dynamics"
] | [
"Compare/Contrast"
] | [
[
1089,
1102
]
] | [
[
855,
1087
]
] |
2021MNRAS.505..515Z__Naul_et_al._2018_Instance_2 | For variable star classification, both convolutional neural networks (CNNs; LeCun, Bengio & Hinton 2015) and recurrent neural networks (RNNs; Hochreiter & Schmidhuber 1997; Cho et al. 2014) have been shown to be competitive to the traditional RF-based methods. Naul et al. (2018) used an RNN autoencoder network to learn... | [
"Naul et al. 2018"
] | [
"Although period-folding improves performance",
"Becker et al. (2020)’s time-space RNN does not require the period to be calculated, and is thus less computationally expensive in terms of preprocessing."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
953,
969
]
] | [
[
907,
951
],
[
972,
1125
]
] |
2021AandA...646A..96C__Brusa_et_al._2018_Instance_2 | AGN-driven outflows. Another possible effect of the AGN activity on the molecular gas is through outflows. This possibility is supported by observations of individual objects: For example, Carniani et al. (2017), Brusa et al. (2018) and Loiacono et al. (2019) find low gas fractions in powerful AGN at cosmic noon hostin... | [
"Brusa et al. 2018"
] | [
"This representative value for our AGN is in line but not as low as previous work targeting extremely powerful sources (e.g., Mgas, mol/M* 0.05 in"
] | [
"Compare/Contrast"
] | [
[
1590,
1607
]
] | [
[
1443,
1589
]
] |
2022MNRAS.512..186K__Datta_et_al._2010_Instance_1 | This work is the second in a series of works aimed at understanding the effect of residual gain errors in different power spectrum estimations in the presence of strong foreground and exploring potential mitigation techniques. In this work, we have not investigated the different possibilities for the presence of residu... | [
"Datta et al. 2010"
] | [
"As a result, when the power spectrum is observed as a function of (k∥, k⊥), the foreground emission remains concentrated near the low k∥, inside the ‘wedge’"
] | [
"Uses"
] | [
[
1601,
1618
]
] | [
[
1443,
1599
]
] |
2021AandA...656A..95P__Houdek_et_al._2017_Instance_1 | Many efforts have thus been devoted to the correction of surface effects, either from theoretical modelling (e.g., Gabriel et al. 1975; Balmforth 1992b; Houdek 1996; Rosenthal et al. 1999; Grigahcène et al. 2005) or through empirical formulae (e.g., Kjeldsen et al. 2008; Christensen-Dalsgaard 2012; Ball & Gizon 2014; S... | [
"Houdek et al. 2017"
] | [
"Another problem is the use of time-dependent mixing-length formalisms",
"to account for modal surface effects (e.g.,"
] | [
"Background",
"Background"
] | [
[
954,
972
]
] | [
[
739,
808
],
[
833,
876
]
] |
2022ApJ...935...49G__Hezaveh_et_al._2016_Instance_1 | Strong gravitational lensing systems are a powerful tool for cosmology. They have been used to study how dark matter is distributed in galaxies and clusters (e.g., Kochanek 1991; Hogg & Blandford 1994; Broadhurst et al. 2000; Koopmans & Treu 2002; Bolton et al. 2006; Koopmans et al. 2006; Bradač et al. 2008; Huang et a... | [
"Hezaveh et al. 2016"
] | [
"Strong gravitational lensing systems are a powerful tool for cosmology. They have been used to study how dark matter is distributed in galaxies and clusters",
"and are uniquely suited to probe the low end of the dark matter mass function and test the prediction of the cold dark matter (CDM) model beyond the loca... | [
"Background",
"Background"
] | [
[
644,
663
]
] | [
[
0,
156
],
[
446,
616
]
] |
2020ApJ...901L..10L__White_et_al._1992_Instance_1 | The 17 GHz polarization reversal during this CRF can be a yet unknown feature inherent to the fan–spine structure, where magnetic polarity around null point (NP) varies so rapidly as to affect the propagation of microwave polarization. A way to possibly explain this polarization change is to view it as a mode-coupling ... | [
"White et al. 1992"
] | [
"A way to possibly explain this polarization change is to view it as a mode-coupling phenomenon, the process by which the rays reverse their original sense of polarization while passing through a quasi-transverse field region along the line of sight from the radiation source to the observer, depending on the degree... | [
"Compare/Contrast"
] | [
[
621,
638
]
] | [
[
236,
574
]
] |
2017MNRAS.464.4495G__Levine_et_al._2006_Instance_1 | To emphasize it again, one may suggest accordingly that several low-m modes of moderately growing collective oscillation with different amplitudes, number of spirals and pitch angles (radial wavelengths), including the most interesting m = 1 mode, may co-exist in the solar neighbourhood. The so-called lopsidedness, or ... | [
"Levine et al. 2006"
] | [
"In addition, we argue that the Galaxy is the azimuthally asymmetric spiral system (cf."
] | [
"Differences"
] | [
[
965,
983
]
] | [
[
878,
964
]
] |
2017MNRAS.469.3252P__Anderson_&_Bedin_2010_Instance_1 | Tol1247 was imaged with the HST (see Fig. 3) in the optical using the Wide Field Ultraviolet-Visible Channel (UVIS) of its Wide Field Camera 3 (WFC3). For UV imaging, the Advanced Camera for Surveys' Solar Blind Channel (ACS/SBC) was used. Seven filters were utilized in total, allowing to apply laxs – the Lyman alpha e... | [
"Anderson & Bedin 2010"
] | [
"The charge transfer inefficiency (CTE) correction for the ACS data was performed by the pipeline, whereas CTE losses in WFC3/UVIS",
"were treated manually using the tools supplied by STScI."
] | [
"Uses",
"Uses"
] | [
[
1147,
1168
]
] | [
[
1016,
1145
],
[
1170,
1226
]
] |
2020ApJ...902...77O__Wuyts_et_al._2012_Instance_1 | Guo et al. (2015) used an automated “blob finder” to identify star-forming regions in the HST/ACS images for 3,239 log M*/M⊙ 10.6 galaxies in CANDELS (GOODS-S and UDS fields) at 0.5 z 3. They defined clumps as blobs which contribute more than 8% of the total UV light of their host galaxies. In contrast to our result... | [
"Wuyts et al. 2012"
] | [
"t is worth pointing out that clumpy galaxy fractions are highly sensitive to methodology and clump definition and vary widely in the literature (e.g.,",
"so we should not expect complete agreement."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
669,
686
]
] | [
[
469,
619
],
[
706,
749
]
] |
2016AandA...588A..48C__Huré_(2013)_Instance_1 | The major difference between the axisymmetric case and the asymmetric approach is that we need to derive the 3D, asymmetric gravitational potential of luminous baryons beforehand. We thus computed the potential in Cartesian coordinates (x,y,z), which enables us to derive both radial and azimuthal forces at any desired ... | [
"Huré (2013)"
] | [
"Here, we use the new formalism presented in",
"who showed that the Newtonian potential is exactly reproduced by using an intermediate scalar function ℋ, namely \\hbox{$\\Phi = \\partial_{xy}^2 {\\cal H}$}Φ=∂xy2ℋ. In 3D, this hyperpotential is written as (12)\\begin{equation} {\\cal H}(x,y,z) = -G \\iiint_{\\Omeg... | [
"Uses",
"Uses"
] | [
[
1078,
1089
]
] | [
[
1034,
1077
],
[
1090,
1512
]
] |
2015ApJ...804..130C___2013_Instance_2 | We have developed the simplest spherical void lens model based on the recently developed embedded lens theory. We have assumed a uniform mass profile for the void, compensated by a thin bounding shell. The infinitesimally thin bounding shell was chosen for convenience (Maeda & Sato 1983a, 1983b). To investigate other v... | [
"Kantowski et al. (2013)"
] | [
"However, the repulsive nature of lensing by a large and deep underdense region (i.e., cosmic voids) as described by the rigorously derived but simply implemented embedded lens formalism did not appear until"
] | [
"Background"
] | [
[
1347,
1370
]
] | [
[
1140,
1346
]
] |
2016AandA...587A.159G__Segura_et_al._2007_Instance_1 | One has to be sure to rule out cases where inorganic chemistry can mimic the presence of life (“false positives”). Potential abiotic ozone production on Venus- and Mars-like planets has been discussed by Schindler & Kasting (2000, and references therein). While this is based on photolysis of e.g., CO2 and H2O and is th... | [
"Segura et al. 2007"
] | [
"Indeed, other studies confirm that abiotic buildup of ozone is possible",
"however, detectable levels are unlikely if liquid water is abundant, as e.g. rainout of oxidized species would keep atmospheric O2 and O3 low",
", unless the CO2 concentration is high and both H2 and CH4 emissions are low"
] | [
"Background",
"Background",
"Background"
] | [
[
829,
847
]
] | [
[
572,
643
],
[
686,
827
],
[
848,
924
]
] |
2022ApJ...931...70B___2022a_Instance_1 | RFs can propagate from the magnetotail to Earth over a long distance more than 10 R
E together with BBFs behind them (Runov et al. 2009; Cao et al. 2010). Studies have suggested that RFs are crucial regions for particle acceleration, pitch-angle evolution, wave–particle interactions, and electromagnetic energy conversi... | [
"Liu et al.",
"2022a"
] | [
"For instance,",
"and RFs are associated with energy conversion from electromagnetic fields to particles"
] | [
"Background",
"Background"
] | [
[
1078,
1088
],
[
1096,
1101
]
] | [
[
359,
372
],
[
925,
1011
]
] |
2016ApJ...817....9K__Chen_et_al._2006_Instance_2 | To perform a statistical analysis of the average quiescent fraction of satellites around our sample of massive galaxies, we use a statistical background subtraction technique (e.g., Kauffmann et al. 2010; Tal et al. 2012; Wang & White 2012; Kawinwanichakij et al. 2014). We detect objects within fixed apertures centered... | [
"Chen et al. 2006"
] | [
"This accounts for the bias due to contaminating galaxies that are physically associated with the centrals but are not satellites (i.e., the 2-halo term of the correlation function; see"
] | [
"Uses"
] | [
[
945,
961
]
] | [
[
760,
944
]
] |
2016ApJ...820...12P__Camenzind_&_Krockenberger_1992_Instance_1 | Variability in observed emission can be considered a defining characteristic of active galactic nuclei (AGNs), and for the roughly 10% of AGNs that are radio-loud (e.g., Jiang et al. 2007) the majority of this variable emission is understood to arise from the relativistic flows of plasma along two oppositely directed j... | [
"Camenzind & Krockenberger 1992"
] | [
"Even modest changes in direction (e.g.,",
"have long been recognized as one way to produce significant changes in the flux and polarization"
] | [
"Background",
"Background"
] | [
[
1529,
1559
]
] | [
[
1489,
1528
],
[
1589,
1685
]
] |
2017MNRAS.465..492M__Taverna_et_al._2015_Instance_2 | Given the quite strong surface magnetic field of the M7, thermal radiation is expected to be polarized, either if emission is from a bare surface or from an atmosphere (see Turolla et al. 2004; Potekhin 2014). The polarization properties are quite different in the two cases, although there are still uncertainties, espe... | [
"Taverna et al. 2015"
] | [
"Vacuum birefringence dramatically increases the linear polarization of the observed radiation, from a level of a few per cent up to even ∼100 per cent, depending on the viewing geometry and the surface emission mechanism"
] | [
"Background"
] | [
[
1309,
1328
]
] | [
[
1042,
1263
]
] |
2016AandA...594A..64P__Judge_(2015)_Instance_1 | There is now renewed interest in the literature concerning these transitions, because some of the O iv and S iv intercombination lines, together with the Si iv resonance lines, are routinely observed with the Interface Region Imaging Spectrograph (IRIS; De Pontieu et al. 2014) at much higher spectral, spatial and tempo... | [
"Judge (2015)"
] | [
"In addition,",
"recalled several issues that should be taken into account when considering the Si iv/O iv density diagnostic. The main ones were: (1) O iv and Si iv ions are formed at quite different temperatures in equilibrium and hence a change in the O iv/Si iv ratio could imply a change in the temperature ra... | [
"Background",
"Background"
] | [
[
1021,
1033
]
] | [
[
1008,
1020
],
[
1034,
1620
]
] |
2016MNRAS.458.3655V__Casella,_Belloni_&_Stella_2005_Instance_1 | Accreting stellar-mass black holes in binary systems regularly display quasi-periodic oscillations (QPOs) in their X-ray flux with frequencies drifting from ∼0.1–10 Hz (e.g. Van der Klis 1989). Three main components can be identified in the spectrum of these sources: disc blackbody emission, power-law emission from the... | [
"Casella, Belloni & Stella 2005"
] | [
"So-called Type-C low-frequency QPOs",
"are believed to originate from the inner accretion flow/corona that is associated with the Comptonized power-law component of the X-ray spectrum, as this component shows a much larger variability amplitude than the blackbody disc component"
] | [
"Background",
"Background"
] | [
[
476,
506
]
] | [
[
439,
474
],
[
508,
747
]
] |
2020ApJ...894..121M__Bruno_&_Carbone_2013_Instance_1 | Current sheet drift is implemented following the approach proposed by Burger (2012) to calculate the drift velocity Vd in Equation (7). The heliospheric current sheet angle is modeled as by Kóta & Jokipii (1983), but now with a time-dependent tilt angle from Equation (8) such that
12
where, after Burger et al. (20... | [
"Bruno & Carbone 2013"
] | [
"This latter assumption does not perfectly reflect spacecraft observations of the same",
", but leads to relatively simple, tractable expressions for the parallel and perpendicular MFPs."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
921,
941
]
] | [
[
780,
865
],
[
942,
1038
]
] |
2022MNRAS.515L..39Z__Weiss_et_al._2008_Instance_1 | Rocky planets are the only harbour for life form in the Solar system, so unravelling their origin and history is fundamental for understanding the habitability of planets other than Earth (Lineweaver & Chopra 2012; Cockell et al. 2016). For example, mantle–crust differentiation on Earth has set boundary conditions thro... | [
"Weiss et al. 2008"
] | [
"Non-chondrite meteorites (including achondrites) also originate from differentiated asteroids and planets, e.g. from Moon, Mars, and Vesta, and the angrite and ureilite parent bodies"
] | [
"Background"
] | [
[
965,
982
]
] | [
[
763,
945
]
] |
2018AandA...613A..35K__Anderson_et_al._2010_Instance_1 | As shown in Fig. 3, the differences in metallicity between different SN subclasses are not significant. This is in contradiction with what is expected from single-star evolution theory, where metallicity-driven winds are crucial: type Ic SNe, which are the most highly stripped, would show the highest metallicity, follo... | [
"Anderson et al. 2010"
] | [
"This result strengthens the notion that metallicity may not play an important role in deciding theresulting SN type, in agreement with other works based on SN environments"
] | [
"Similarities"
] | [
[
717,
737
]
] | [
[
544,
715
]
] |
2021MNRAS.503..354G__Griv_et_al._2020_Instance_1 | The Lindblad–Oort idea of a rotation of the Galaxy around the Galactic Centre (GC) proposes that for any type of Galactic object there is at each point in the plane a mean circular, differential motion (Oort 1927a,b). In the conventional lowest order approach to the determination of the rotation parameters of the syste... | [
"Griv et al. 2020"
] | [
"Here, $\\widetilde{v}_r$ and $\\widetilde{v}_\\varphi$ are the amplitudes of the radial and tangential wave motions that depend weakly on the Galactocentric distance r, and ϕ is the phase of the wave",
", annexure B therein"
] | [
"Uses",
"Uses"
] | [
[
921,
937
]
] | [
[
682,
878
],
[
937,
957
]
] |
2015ApJ...806..152S__Ransom_et_al._2005_Instance_2 | One of the most astonishing characteristics of Liller 1 is the extremely large value of the collision rate parameter. Verbunt & Hut (1987) showed that Liller 1 has the second-highest value of stellar encounter rate (after Terzan 5; see also Lanzoni et al. 2010) among all star clusters in the Galaxy, thus suggesting tha... | [
"Ransom et al. 2005"
] | [
"Indeed, Terzan 5 hosts the largest population of MSPs among all Galactic GCs"
] | [
"Motivation"
] | [
[
1034,
1052
]
] | [
[
956,
1032
]
] |
2021ApJ...910...52C__Kleihaus_et_al._2004_Instance_1 | Half a century ago, a series of theorems laid the ground for the Kerr hypothesis (Israel 1967; Carter 1971; Robinson 1975); according to these no-hair theorems, the only stationary, axisymmetric, asymptotically flat, regular outside of the horizon solution to four-dimensional GR when the matter fields feature the same ... | [
"Kleihaus et al. 2004"
] | [
"Still, in four dimensions, hairy BHs have been described in different theories of gravity, such as Einstein–Yang–Mills"
] | [
"Background"
] | [
[
724,
744
]
] | [
[
484,
602
]
] |
2018MNRAS.476.1889T__Kulkarni,_Hut_&_McMillan_1993_Instance_1 | The high interaction rates in globular clusters, especially at their centres, lead to the efficient formation of exotic binaries like accreting compact objects – cataclysmic variables (white dwarfs) and X-ray binaries (neutron stars and black holes; Clark, Markert & Li 1975). Soon after the first X-ray missions, it was... | [
"Kulkarni, Hut & McMillan 1993"
] | [
"Originally it was proposed that due to mutual gravitational interactions that all black holes would have been ejected from globular clusters"
] | [
"Background"
] | [
[
835,
864
]
] | [
[
693,
833
]
] |
2020AandA...644A..97C__Leroy_et_al._2013_Instance_4 | Major nearby galaxy cold gas mapping surveys (Regan et al. 2001; Wilson et al. 2009; Rahman et al. 2011; Leroy et al. 2009; Donovan Meyer et al. 2013; Bolatto et al. 2017; Sorai et al. 2019; Sun et al. 2018) have focused on observations of the molecular gas (through CO lines). Despite a few notable exceptions (e.g. Ala... | [
"Leroy et al. 2013"
] | [
"These differences",
"do not seem to be related to unaccounted variation in the CO-to-H2 conversion factor"
] | [
"Background",
"Background"
] | [
[
2074,
2091
]
] | [
[
1852,
1869
],
[
1988,
2072
]
] |
2020AandA...637A..59A__Massalkhi_et_al._2019_Instance_3 | 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"
] | [
"but has been interpreted as evidence that SiO disappears from the gas phase at high densities to be incorporated into dust grains"
] | [
"Compare/Contrast"
] | [
[
1114,
1135
]
] | [
[
910,
1039
]
] |
2021ApJ...916...70Z__Liu_et_al._2020_Instance_1 | At this juncture in cosmology, independent and complementary probes with considerable precision are very helpful for providing clues about the origin of the abovementioned crises. Strong-lensing systems are one of the most promising probes for investigating these issues. The time delay between images of strongly lensed... | [
"Liu et al. 2020"
] | [
"This method has been intensively implemented with updated observations"
] | [
"Background"
] | [
[
1148,
1163
]
] | [
[
1042,
1112
]
] |
2015AandA...579A..56B__Lebrun_et_al._2003_Instance_1 | Swift J1734.5-3027 was detected by INTEGRAL for the first time during the observations performed toward the Galactic bulge in the satellite revolution 1329, i.e., about half a day before the BAT discovery (from 56 535.85950 MJD to 56 536.01338 MJD; see Table 1). It remained within the field of view (FoV) of the instrum... | [
"Lebrun et al. 2003"
] | [
"To limit the ISGRI calibration uncertainties"
] | [
"Uses"
] | [
[
808,
826
]
] | [
[
762,
806
]
] |
2020AandA...641A..85S__Orienti_&_Dallacasa_2008_Instance_2 | To derive the equipartition magnetic field of J1146+4037, we predict the rest-frame 8.4 GHz (redshifted to 1.4 GHz at z = 5.0059) flux density from our spectral model. However, there is no source size measurement at 1.4 GHz. We make use of the full width at half maximum (FWHM) source size of 0.74 ± 0.01 mas derived by ... | [
"Orienti & Dallacasa 2008"
] | [
"This is within the range of the equipartition magnetic fields of 17 HFP radio sources",
"and 5 HFPs at 0.084 z 1.887 (18–160 mG"
] | [
"Similarities",
"Similarities"
] | [
[
877,
901
]
] | [
[
670,
755
],
[
833,
875
]
] |
2021AandA...654A..89P__Vincentelli_et_al._2021_Instance_1 | The spectral analysis above 3 keV allows us to characterise the hot corona and the relativistic reflection emission properties. The deep January 2017 NuSTAR observation was also included in the simultaneous fit (Ezhikode et al. 2020; Panagiotou & Walter 2020). From the RELXILL reflection model, and assuming a primary e... | [
"Vincentelli et al. 2021"
] | [
"These values are in very good agreement with those measured from the average long-term Swift/BAT (Burst Alert Telescope) spectrum"
] | [
"Similarities"
] | [
[
588,
611
]
] | [
[
457,
586
]
] |
2020AandA...639A.104S__Kitaura_et_al._2006_Instance_1 | Today, at least three known populations of gap transients are recognized in the luminoisty gap. These include classical luminous blue variable (LBV) outbursts, intermediate-luminosity red transients (ILRTs), and luminous red novae (LRNe). LBVs are thought to be related to eruptions of massive luminous stars (see Smith ... | [
"Kitaura et al. 2006"
] | [
"As shown in greater detail in Stritzinger et al. (2020, hereafter Paper I), the ILRT subtype is well represented by NGC 300-2008-OT and SN 2008S, and has been linked to asymptotic giant branch (S-AGB) stars",
"that die as electron-capture supernovae"
] | [
"Background",
"Background"
] | [
[
788,
807
]
] | [
[
334,
540
],
[
669,
708
]
] |
2021ApJ...911...89M__Mozer_et_al._2020a_Instance_2 | Time domain structures (TDSs; electrostatic or electromagnetic electron holes, ion holes, solitary waves, double layers, nonlinear whistlers, etc.) are ∼1 ms pulses having significant electric fields parallel to the background magnetic field (Mozer et al. 2015). They are abundant through space, occurring along auroral ... | [
"Mozer et al. 2020a"
] | [
"In this paper, the data from DC to 2 MHz are discussed. These measurements are obtained from the potentials of the four antennas, V1 through V4, that are located in the plane perpendicular to the Sun–satellite line. They produce E12 = (V1−V2)/3.5 and E34 = (V3−V4)/3.5, which are then rotated into the spacecraft co... | [
"Uses"
] | [
[
2184,
2202
]
] | [
[
1517,
2182
]
] |
2019AandA...629A..54U__Marinucci_et_al._2015_Instance_1 | NGC 2110. NGC 2110 is another nearby (z = 0.00779, Gallimore et al. 1999), X-ray bright Seyfert galaxy. Diniz et al. (2015) report a black hole mass of
2
.
7
−
2.1
+
3.5
×
10
8
M
⊙
$ 2.7^{+ 3.5}_{- 2.1} \times 10^{8}\,{{M}_{\odot}} $
, from the relation with the stellar velocity dispersion. From Bepp... | [
"Marinucci et al. 2015"
] | [
"No Compton reflection hump has been detected with",
"or NuSTAR",
"despite the presence of a complex Fe Kα line."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
966,
987
]
] | [
[
877,
926
],
[
955,
964
],
[
990,
1035
]
] |
2021AandA...651L...8D__Just_et_al._2007_Instance_2 | As the most luminous persistent sources in the Universe, quasars are bright enough to be detected up to redshifts z > 7 (Mortlock et al. 2011; Banados et al. 2018; Wang et al. 2018; Yang et al. 2020). According to the currently accepted model, quasars are extremely luminous active galactic nuclei (AGNs), where the obse... | [
"Just et al. 2007"
] | [
"The initial dispersion of the LUV − LX relation is relatively large (δ ∼ 0.35−0.4,",
"but after a detailed study, Lusso & Risaliti (2016) suggest that most of the observed dispersion is not intrinsic, but it is rather due to observational effects."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1639,
1655
]
] | [
[
1556,
1638
],
[
1677,
1838
]
] |
2017AandA...599A..55B__Shakura_1972_Instance_2 | When the characteristic time of variability of the mass flux along the accretion disk is longer than the relaxation time of the local disk equilibrium, it is possible to use the approximation of local equilibrium Shakura (1972), see also Bisnovatyi-Kogan (2011), to calculate the transient disk structure. The equilibriu... | [
"Shakura 1972"
] | [
"We use an α approximation for the turbulent viscosity",
"when the (rφ) component of the stress tensor trφ is written as (5)\\begin{equation} t_{r\\phi}=\\alpha\\, P, \\label{trphi} \\end{equation}trφ=α P,where the phenomenological non-dimensional parameter α ≤ 1."
] | [
"Uses",
"Uses"
] | [
[
1435,
1447
]
] | [
[
1380,
1433
],
[
1449,
1649
]
] |
2022MNRAS.516.5618P__Muzahid_et_al._2020_Instance_1 | Recent technological advances related to 3D Integral Field Spectroscopy (IFS), which produces data cubes where each pixel on the image has a spectrum, have opened a new window for examining the CGM gas. This approach combines the information gathered in absorption against background sources (whose lines of sight pass t... | [
"Muzahid et al. 2020"
] | [
"Early on, the MUSE Guaranteed Time Observations (GTO) team established surveys including MUSE-QuBES",
"to relate gas traced by absorbers to galaxies."
] | [
"Background",
"Background"
] | [
[
1096,
1115
]
] | [
[
995,
1094
],
[
1217,
1263
]
] |
2021MNRAS.507.1421M__Novikov,_Schmalzing_&_Mukhanov_2000_Instance_1 | Topological estimators such as the Minkowski functionals (MFs) are also important diagnostics in this direction as they carry information at all orders. The MFs have been extensively developed as a statistical tool in a cosmological setting for both two-dimensional (2D; projected) and 3D (redshift) surveys. The MFs hav... | [
"Novikov, Schmalzing & Mukhanov 2000"
] | [
"Topological estimators such as the Minkowski functionals (MFs) are also important diagnostics in this direction as they carry information at all orders. The MFs have been extensively developed as a statistical tool in a cosmological setting for both two-dimensional (2D; projected) and 3D (redshift) surveys. The MF... | [
"Background"
] | [
[
500,
535
]
] | [
[
0,
472
]
] |
2015ApJ...799..149J___2013_Instance_1 | We use the microlensing magnification estimates for 27 quasar image pairs in 19 lens systems from MED09. In order to have the largest possible sample, but with a similar range of observed rest wavelengths, we include all of the objects from MED09 with magnifications measured in the wavelength range between Lyα (1216â... | [
"Guerras et al. 2013"
] | [
"These microlensing magnification estimates are calculated after subtracting the emission line flux ratios, which are little affected by microlensing (see, e.g.,",
"from the continuum flux ratios, and are therefore virtually free from extinction, substructure, and macro model effects (as these affect the line and... | [
"Uses",
"Uses"
] | [
[
783,
803
]
] | [
[
622,
782
],
[
806,
987
]
] |
2015MNRAS.448.2260G__Debes_et_al._2011_Instance_1 | Furthermore, well-defined large samples of white dwarfs are an extremely useful starting point for identifying rare white dwarf types like magnetic white dwarfs (Gänsicke, Euchner & Jordan 2002; Schmidt et al. 2003; Külebi et al. 2009; Kepler et al. 2013), pulsating white dwarfs (Castanheira et al. 2004; Greiss et al. ... | [
"Debes et al. 2011"
] | [
"Furthermore, well-defined large samples of white dwarfs are an extremely useful starting point for identifying rare white dwarf types like",
"or white dwarfs with dusty or gaseous planetary debris discs"
] | [
"Motivation",
"Motivation"
] | [
[
985,
1002
]
] | [
[
0,
138
],
[
870,
930
]
] |
2015ApJ...813..103M__Koss_et_al._2012_Instance_1 | The stochastic accretion of gas and galaxy merger-driven gas inflows are both known triggers of supermassive black hole (SMBH) growth and nuclear activity, but the relative contributions of each is still unclear. Simulations of galaxy mergers show that they drive gas to the centers of merger-remnant galaxies (e.g., Spr... | [
"Koss et al. 2012"
] | [
"Observations have shown that the AGN fraction does increase with decreasing distance between two merging galaxies",
"but this has not been well tested at the very centers of merger-remnant galaxies because of the observational difficulty of detecting and resolving two AGNs with separations 10 kpc."
] | [
"Background",
"Motivation"
] | [
[
616,
632
]
] | [
[
480,
593
],
[
656,
837
]
] |
2019AandA...625A.147A__Chantzos_et_al._2018_Instance_1 | Hydrocarbons also show a variety of deuterated molecules in L483. We detected C4D, with an isotopic ratio of 1.9 ± 0.6%, which is slightly above that found in TMC-1 (0.43; Turner 1989) and similar to that derived in L1527 (1.8; Sakai et al. 2009b). We also detected the singly and doubly deuterated forms of c-C3H2, with... | [
"Chantzos et al. 2018"
] | [
"Moreover, c-C3HD and c-C3D2 have been surveyed in a sample of low-mass prestellar and protostellar cores",
"finding that the corresponding isotopic ratios are relatively uniform, within a factor of a few, and similar to those in L1544 and L483."
] | [
"Background",
"Background"
] | [
[
612,
632
]
] | [
[
506,
610
],
[
635,
771
]
] |
2021AandA...656A..94G__Gronow_et_al._2021_Instance_2 | Major differences between our approach and a full re-calculation of the hydrodynamics were not expected since the changes in the 14N and 22Ne abundances at the different metallicities do not alter the energy release in the hydrodynamic simulations significantly. The situation is different for deflagrations where the bu... | [
"Gronow et al. 2021"
] | [
"However, differences in the yields produced in the He detonation can in part be attributed to the slightly different setups of Model M2a (and therefore Model M2a_pp) and Model M10_05_1 at the beginning of the relaxation simulation, with the differences in the total and shell masses being less than 1% (see",
"for... | [
"Differences",
"Differences"
] | [
[
1816,
1834
]
] | [
[
1509,
1815
],
[
1835,
1873
]
] |
2021AandA...649A..84H__Geers_et_al._2007_Instance_1 | The objective of this article is to study the spatial distribution and possible changes in the properties of carbon nano-dust in protoplanetary disks (PPDs). Carbon nanodust, detected under more or less organised structures and different ionisation states, constitutes a major component of dust in the interstellar and c... | [
"Geers et al. 2007"
] | [
"This results in different spatial distributions in which tiny grains are present at the disk surfaces",
"and in the cavity or gaps from which the pebbles are missing (e.g."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1005,
1022
]
] | [
[
771,
872
],
[
938,
1004
]
] |
2021MNRAS.504....1C__Ripepi_et_al._2014_Instance_1 | Our first attempt to derive the $PL_{K_\mathrm{s}}$ relation has revealed a number of RRLs brighter than the main relation. We investigated their spatial distribution and found that they are mainly located in the central part of the LMC. This is shown in Fig. 5 which presents in the bottom panel the spatial distributio... | [
"Ripepi et al. 2014"
] | [
"We expect the centroid of a blended source to be determined with poor accuracy (see e.g.",
"For this reason as a further test we plotted the distribution of distances in arcsec of the VMC sources cross-matched with the OGLE IV RRLs."
] | [
"Uses",
"Uses"
] | [
[
1272,
1290
]
] | [
[
1183,
1271
],
[
1299,
1439
]
] |
2021MNRAS.506.1715D__Jones_et_al._2003_Instance_1 | In direct relation to the interplay between the structure of the dark matter distribution and the baryon physics, galaxies are found in a wide range of structural hierarchies, from low-density regions to groups and clusters (see e.g. Tully 1987; Berlind et al. 2006; Yang et al. 2007), and during their lifetime they exp... | [
"Jones et al. 2003"
] | [
"In some cases, the mergers eventually devoid their entire neighbourhood, leaving behind a single elliptical galaxy of group-scale mass, called a fossil group galaxy"
] | [
"Background"
] | [
[
568,
585
]
] | [
[
382,
546
]
] |
2016AandA...596A.116S__Bochanski_et_al._2010_Instance_1 | At present, however, kinematical studies of the nearby late-type stars have become somewhat foreshadowed with the advent of deep, wide-field SDSS (York et al. 2000), SDSS/SEGUE (Yanny et al. 2009) and RAVE (Steinmetz et al. 2006) surveys which have made it possible to study K–M dwarfs to much greater distances from the... | [
"Bochanski et al. 2010"
] | [
"Using their spectroscopic catalog with radial velocities measured with an external accuracy of 7–10 km s-1 and applying photometric parallax relations, the SDSS teams have traced K–M dwarfs in the distance range up to ~2 kpc, thus providing valuable information on the spatial, velocity, and metallicity distributio... | [
"Background",
"Background"
] | [
[
959,
980
]
] | [
[
326,
701
],
[
851,
938
]
] |
2019ApJ...874..154D__Stanway_et_al._2016_Instance_1 | There are several reasons to suspect that the (galaxy-sourced) ionizing background during reionization may have been somewhat harder than the estimates given here. First, our calculations neglect the filtering effects of optically thick H i in the ISM of the host galaxy, and within the cosmic web. Absorption by this ga... | [
"Stanway et al. 2016"
] | [
"Second, our calculations neglect the effects of binary star systems. Mass transfers and mergers between binary companions can extend the period over which ionizing photons are produced by the stellar population, which would harden the time-integrated spectrum"
] | [
"Compare/Contrast"
] | [
[
949,
968
]
] | [
[
663,
922
]
] |
2021MNRAS.505..523R__Mościbrodzka_et_al._2017_Instance_1 | Recently, the EHT Collaboration completed an analysis of the linear polarization of M87*, providing novel insights into its magnetic field structure in particular (Event Horizon Telescope Collaboration 2021a,b; Goddi et al. 2021). Synchrotron emission, which dominates the millimetre image, is initially generated perpen... | [
"Mościbrodzka et al. 2017"
] | [
"Then, as this polarization propagates, it is further modified by Faraday effects, important for depolarizing accretion flows down to observed levels and generating the observed rotation measure"
] | [
"Background"
] | [
[
693,
717
]
] | [
[
465,
658
]
] |
2019MNRAS.486.4671M__Schwenn_2006_Instance_1 | CMEs are known for large-scale expulsion of magnetized plasma structures from closed magnetic field regions on the Sun. They were first detected in the coronagraphic images taken in 1971 by NASA’s OSO-7 spacecraft (Tousey 1973). However, some definite inferences for the solar wind (Eddington 1910; Birkeland 1916; Bierm... | [
"Schwenn 2006"
] | [
"Following OSO-7, a series of spacecraft (Skylab, Helios, P78-1 Solwind, SOHO, Coriolis, and STEREO, etc.) have observed thousands of CMEs leading to a vast literature"
] | [
"Background"
] | [
[
706,
718
]
] | [
[
444,
610
]
] |
2021AandA...645A.137A__Gopal-Krishna_et_al._(2011)_Instance_1 | The first INM of PG 1553+113 to our knowledge was reported by Stalin et al. (2005) – they applied the C-test to the R-band LCs (total duration of about 10 h) and found the source to be variable in one night out of two. Another two nights of INM about 13 h long were presented by Osterman et al. (2006). They found no sig... | [
"Gopal-Krishna et al. (2011)"
] | [
"detected INV during three nights out of three using C- and F-tests (a total monitoring duration of 16 h in the R-band)."
] | [
"Compare/Contrast"
] | [
[
1053,
1080
]
] | [
[
1081,
1200
]
] |
2016MNRAS.462S.376B__Bowell_et_al._1989_Instance_1 | In order to assess the impact of the brightness enhancement due to the phase function effects in the light scattering of the coma dust, we apply different phase function corrections to the measured coma brightness of 67P for the 10 000 km aperture radius. In general, the phase function reduces the reflected coma magnit... | [
"Bowell et al. 1989"
] | [
"Fornasier et al. (2015) obtained results for the 67P nucleus surface reflectivity applying a HG-type phase function",
"with a best-fitting G of −0.13. Fig. 5 shows the phase angle-corrected afρ values of 67P for the various phase function solutions."
] | [
"Uses",
"Uses"
] | [
[
928,
946
]
] | [
[
811,
926
],
[
948,
1078
]
] |
2015ApJ...805..134M__Yoo_et_al._2014_Instance_1 | The physics of asymmetric inflow reconnection has been investigated in detail for fully ionized plasmas. One of the principal applications of this work has been Earth's dayside magnetopause. Asymmetric inflow reconnection has also been investigated in the context of Earth's magnetotail and elsewhere in the magnetospher... | [
"Yoo et al. 2014"
] | [
"Asymmetric inflow reconnection has also been investigated in",
"laboratory experiments"
] | [
"Background",
"Background"
] | [
[
536,
551
]
] | [
[
191,
251
],
[
476,
498
]
] |
2021ApJ...910...18C__Rubele_et_al._2018_Instance_1 | The LMC is known to have brought a large population of star clusters as it has been accreted onto the Milky Way (Bica et al. 2008); thus, it is possible that DELVE 2 may share a similar history to the thousands of known star clusters in the Magellanic system. The LMC star cluster formation history is believed to be thr... | [
"Rubele et al. 2018"
] | [
"The LMC star cluster formation history is believed to be three-staged, including a period of rapid cluster star formation in the early universe (τ ≳ 10 Gyr), followed by a long quiescent period between ∼10 and ∼2–4 Gyr ago and then by a period of rapid star cluster formation extending to the present day, potential... | [
"Background"
] | [
[
669,
687
]
] | [
[
260,
624
]
] |
2017ApJ...834L..21A__Larsen_&_Lane_1994_Instance_1 | The experiment was carried out using the VULCAN laser facility at the Rutherford Appleton Laboratory (Danson et al. 1998), using the setup shown in Figure 1(a). A laser pulse of duration ∼1 ns and energy ∼ 70 J, was focused onto a 50 μm thick gold foil, at an incidence angle of
∼
45
°
to a peak intensity of ∼10... | [
"Larsen & Lane 1994"
] | [
"Hydrodynamic simulations using the code HYADES"
] | [
"Uses"
] | [
[
965,
983
]
] | [
[
916,
962
]
] |
2015AandA...580A..71L__Sutton_et_al._(2013)_Instance_1 | 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)"
] | [
"developed a classification scheme based on a disk+power law fit, to be applied to ULX spectra, according to which the spectral state of an ULX source can be defined by the disk temperature, the power-law slope, and the ratio between the flux contribution of the two spectral components in the 0.3−1 keV band."
] | [
"Background"
] | [
[
1038,
1058
]
] | [
[
1059,
1367
]
] |
2022ApJ...924...97W__Zhang_&_Mészáros_2001_Instance_1 | Using all GRBs showing X-ray plateau phases, Dainotti et al. (2008) discovered a tight correlation between L0 and tb (the Dainotti relation). Subsequently, the Dainotti relation has been used to measure cosmological parameters (Cardone et al. 2009, 2010; Dainotti et al. 2013; Postnikov et al. 2014). Cardone et al. (201... | [
"Zhang & Mészáros 2001"
] | [
"The X-ray luminosity of GRBs is given by the energy input from the electromagnetic and gravitational waves into the surrounding medium",
"Therefore, in order to standardize GRBs as standard candles through the Dainotti relation, it is recommended that X-ray plateaus caused by the same physical mechanism are used... | [
"Uses",
"Uses"
] | [
[
1051,
1072
]
] | [
[
900,
1034
],
[
1096,
1330
]
] |
2021AandA...653A..85S__However,_Genovali_et_al._(2014)_Instance_2 | Figure 6 shows the orbital eccentricities as a function of [M/H] for the metal-rich disc sample. The solid lines correspond to the required eccentricity (see Eq. (2)) for different values of ISM radial metallicity gradients: −0.10 dex kpc−1 (black), −0.07 dex kpc−1 (our measured gradient for young stars in Table 1; see... | [
"Genovali et al. (2014)"
] | [
"For the three first cases, we assumed ISM[M/H](R⊙) = 0.0 to estimate Rbirth from the stellar metallicity. However,",
"have their own zero point, defined as: [Fe/H] = −0.06 * Rg + 0.57, with a clear shift in the relation compared to the other ones assumed in this work."
] | [
"Differences",
"Differences"
] | [
[
568,
590
]
] | [
[
453,
567
],
[
591,
741
]
] |
2015ApJ...799...55G__Klassen_et_al._2000_Instance_2 | While the angular extent of IP shocks can be directly investigated using multi-point in situ measurements, the size of coronal shocks can only be indirectly inferred via remote-sensing observations of the electromagnetic emissions associated with them. According to Nelson & Robinson (1975), the average angle subtended ... | [
"Klassen et al. 2000"
] | [
"Single-case studies reported some EIT waves covering a whole solar hemisphere"
] | [
"Background"
] | [
[
1468,
1487
]
] | [
[
1389,
1466
]
] |
2021AandA...653A..36M__Goulding_&_Alexander_(2009)_Instance_2 | 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 Bernard-Salas et al. (2009),",
"and the GOALS samples, we excluded all the composite starburst-AGN objects identified as those with a detection of [NeV] either at 14.3 or 24.3 μm."
] | [
"Uses",
"Uses"
] | [
[
1132,
1159
]
] | [
[
1095,
1131
],
[
1161,
1308
]
] |
2018AandA...613A..50C__Reiners_et_al._2013_Instance_1 | As previously mentioned, the small amplitude of the RV modulation in the NIR as measured by GIANO contemporaneously with REM photometry is intriguing. Assuming that the depth of the spectral lines relative to their adjacent continuum is constant and considering a spot with a contrast Cs at latitude ϕ with a filling fac... | [
"Reiners et al. 2013"
] | [
"A cool spot at a higher latitude would reduce the amplitude of the NIR wide-band flux modulations; a quenching of the convective shifts or the Zeeman effect also do not appear to be viable explanations because they increase the effect of a cool spot on the RV at NIR wavelengths"
] | [
"Uses"
] | [
[
814,
833
]
] | [
[
534,
812
]
] |
2021MNRAS.506.5015H__Page_et_al._2004_Instance_1 | Due to their high core temperatures at birth, neutron stars cool pre-dominantly by neutrino emission at ages ≲ 106 yr (Potekhin, Pons & Page 2015). The most rapid changes of surface temperature occur early, first when the temperature of the outer layers achieves equilibrium with the rapidly cooling core at an age of ≲ ... | [
"Page et al. 2004"
] | [
"The most rapid changes of surface temperature occur early,",
"and then when the temperature drops below the critical temperature for core neutrons to become superfluid, which activates the efficient neutrino emission process of Cooper pair formation and breaking"
] | [
"Background",
"Background"
] | [
[
639,
655
]
] | [
[
148,
206
],
[
416,
616
]
] |
2020AandA...637A..59A__Ziurys_et_al._(2018)_Instance_1 | Several molecules show a large discrepancy between the abundances derived from observations and calculated by chemical equilibrium, although it is not as severe as for the molecules discussed above. We refer to PN in O-rich stars and H2S in C-rich stars, which are indicated by hatched rectangles in Fig. 2. For PN in O-... | [
"Ziurys et al. 2018"
] | [
"For PN in O-rich AGB atmospheres, the disagreement between the observed abundances, (1–2) × 10−8",
"and the calculated maximum chemical equilibrium abundance is almost three orders of magnitude."
] | [
"Differences",
"Differences"
] | [
[
406,
424
]
] | [
[
308,
404
],
[
427,
521
]
] |
2018ApJ...864...90M__Shields_1992_Instance_1 | The LLAGN interpretation of LINERs was initially motivated by their significant X-ray emission (Ferland & Netzer 1983; Halpern & Steiner 1983). Although LLAGNs are found via radio and X-ray observations in the majority of LINERs (Dudik et al. 2005, 2009; Nagar et al. 2005; Filho et al. 2006; Flohic et al. 2006; Gonzále... | [
"Shields 1992"
] | [
"Compact starbursts containing hot O stars offer an alternative explanation for the relative intensities of LINER emission lines",
", but have difficulty explaining the broad Balmer emission wings often seen in LINER spectra",
", since this would require long-lived supernova remnants."
] | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1676,
1688
]
] | [
[
1518,
1645
],
[
1689,
1781
],
[
1799,
1856
]
] |
2016ApJ...830...15J__Rice_et_al._2011_Instance_1 | T Tauri stars in general are known to flare (e.g., Gahm 1990; Guenther & Ball 1999). A potentially better analog of the type of variable Hα emission expected from chromospheric emission and flaring on PTFO 8-8695 is the WTTS V410 Tau, with v sin i = 77.7 km s−1 (e.g., Carroll et al. 2012) compared to the measured v sin... | [
"Rice et al. 2011"
] | [
"The Hα line of V410 Tau can grow much stronger and broader during a flare, and also show asymmetries; however, the observed asymmetries seen during flares do not show excess emission with apparent peaks shifted out to greater than ±200 km s−1",
"as seen here in PTFO 8-8695."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1277,
1293
]
] | [
[
1020,
1262
],
[
1295,
1323
]
] |
2017AandA...605A...5S__Dokkum_2001_Instance_1 | The Hα imaging for the galaxies discussed in this paper was generated from two different sources: NGC 3628 was observed on May 8, 1991 using the ESO New Technology Telescope (NTT, red arm of the ESO Multi-Mode Instrument (EMMI)) for 900 s in Hα and 300 s in R as part of ESO program 047.01-003. The detector was a Ford 2... | [
"van Dokkum 2001"
] | [
"L.A. Cosmic",
"was used to clear the image of cosmic rays to produce the final Hα and final R image."
] | [
"Uses",
"Uses"
] | [
[
617,
632
]
] | [
[
604,
615
],
[
634,
719
]
] |
2021MNRAS.503.6155C__Lovisari_et_al._2017_Instance_1 | Galaxy clusters are the traces of the formation of the largest structures in the Universe and so reliable tools to investigate structures formation and evolution. In principle, this is possible only if and when we have full knowledge of the properties of these objects. The total mass (i.e. the total amount of the dark ... | [
"Lovisari et al. 2017"
] | [
"Several attempts have been made to infer clusters dynamical state, using both observational data and simulations, by analysing the images of the emission in optical",
"and in the X-ray band (see e.g."
] | [
"Background",
"Background"
] | [
[
2022,
2042
]
] | [
[
1735,
1899
],
[
1957,
1988
]
] |
2018MNRAS.475.4704R__Smith_et_al._2010_Instance_1 | Understanding the influence of environment is contingent on being able to identify and quantify galaxy environments. Common environmental measures include the projected number density of galaxies out to the Nth nearest neighbour, the halo mass of a host group or cluster, or the projected separation from the centre of a... | [
"Smith et al. 2010"
] | [
"A relaxed, dynamically old group or cluster should be characterized by a central galaxy which is the brightest (most massive) member by a significant margin (e.g."
] | [
"Background"
] | [
[
1147,
1164
]
] | [
[
929,
1091
]
] |
2021AandA...655A..12T__Tang_et_al._2017b_Instance_2 | 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"
] | [
"Different column densities of para-H2CO only weakly affect derived kinetic temperatures (see Fig. 3 in",
"as long as all lines are optically thin."
] | [
"Uses",
"Uses"
] | [
[
778,
795
]
] | [
[
675,
777
],
[
914,
954
]
] |
2019AandA...626A.130T__Imanishi_et_al._(2007)_Instance_1 | We detect a deep (τsil ∼ 2.3) absorption feature due to silicate grains at around 10 μm. We compared the optical depth of the silicate feature in LEDA 1712304 with those in other AGNs in a wide range of IR luminosities (1010 L⊙ LIR 1013 L⊙). The spectra of the AGNs to be compared are taken from those of the IR ga... | [
"Imanishi et al. 2007"
] | [
"The spectra of the AGNs to be compared are taken from those of the IR galaxies observed by Spitzer/IRS"
] | [
"Uses"
] | [
[
375,
395
]
] | [
[
248,
350
]
] |
2020AandA...641A..29G__Kotera_et_al._(2015)_Instance_1 | Our case studies focus on several regions of the parameter space of explosive transients that may be related to specific source categories. From Sect. 3, different types of transient emissions from highly magnetized pulsars (also magnetars) can be affected by secondary acceleration. As mentioned previously, magnetars h... | [
"Kotera et al. (2015)"
] | [
"As mentioned previously, magnetars have been identified in many studies as promising candidates for the acceleration of cosmic rays and the production of secondary high-energy neutrinos, for instance Blasi et al. (2000), Fang et al. (2012, 2013), Lemoine et al. (2015),"
] | [
"Motivation"
] | [
[
554,
574
]
] | [
[
284,
553
]
] |
2019AandA...626A.130T__Imanishi_et_al._(2007)_Instance_2 | We detect a deep (τsil ∼ 2.3) absorption feature due to silicate grains at around 10 μm. We compared the optical depth of the silicate feature in LEDA 1712304 with those in other AGNs in a wide range of IR luminosities (1010 L⊙ LIR 1013 L⊙). The spectra of the AGNs to be compared are taken from those of the IR ga... | [
"Imanishi et al. (2007)"
] | [
"We estimated the optical depths of the AGNs of Stierwalt et al. (2013), Wu et al. (2010), and Roussel et al. (2006) by ourselves in the same manner as was performed for LEDA 1712304 with the method defined by"
] | [
"Uses"
] | [
[
988,
1010
]
] | [
[
779,
987
]
] |
2021MNRAS.507.6012Z__Kendrick,_Hazra_&_Balakrishnan_2015_Instance_1 | The interaction of H2 and HD with atomic hydrogen is among the most widely investigated and important processes in elementary chemical reactions. The H + H2, H + D2, and H + HD reactions serve as benchmarks for experimental and theoretical investigations of bimolecular processes (Marinero, Rettner & Zare 1984; Zhang & ... | [
"Kendrick, Hazra & Balakrishnan 2015"
] | [
"and continue to attract much attention in the quest for unraveling quantum effects such as the geometric phase (GP) in chemical reactions"
] | [
"Background"
] | [
[
689,
724
]
] | [
[
550,
687
]
] |
2022MNRAS.516..731B__Wang,_Hammer_&_Yang_2022_Instance_1 | Now with the recent availability of high quality full 6D phase-space information for large numbers of sources, much effort has been made to decrease the uncertainties in the Milky Way mass estimate. Recent works using a tracer mass estimator with 6D phase-space information include Sohn et al. (2018, globular clusters),... | [
"Wang, Hammer & Yang 2022"
] | [
"Using Bayesian analysis to fit a distribution function to full 6D phase-space data (globular clusters, satellites, and halo stars) has been a recent popular choice among many works"
] | [
"Background"
] | [
[
1049,
1073
]
] | [
[
720,
900
]
] |
2018MNRAS.475.1646F__Ji_et_al._2003_Instance_1 | Solar filaments, or prominences as they are called when observed above the solar limb, can be observed in a stable state for many days or weeks. Sometimes, they suddenly start to ascend as a whole (full eruptions) (Joshi & Srivastava 2011; Holman & Foord 2015) or within limited sections of their length (partial eruptio... | [
"Ji et al. 2003"
] | [
"The ascending of a filament can go on high into the corona (successful eruptions) and gives rise to a coronal mass ejection (CME) or can stop at some greater height in the corona (confined or failed eruptions)"
] | [
"Background"
] | [
[
575,
589
]
] | [
[
364,
573
]
] |
2018ApJ...864..165W__Golub_et_al._1974_Instance_1 | In configuration 1S, the field close to the separatrix was sheared, producing steady interchange reconnection modulated by quasi-periodic reconnection bursts. We can roughly estimate the free energy release rate of the steady component from the energy injected before the onset of reconnection in the first 200 time unit... | [
"Golub et al. 1974"
] | [
"Accounting for the ramp up of the driver and scaling the values, this corresponds to an energy injection rate of ≈5.6 × 1023 erg s−1 at the maximum driving speed. During the quasi-steady phase, this injection is balanced by losses to numerical diffusion and equates to roughly the free energy available for heating ... | [
"Similarities"
] | [
[
955,
972
]
] | [
[
446,
953
]
] |
2020ApJ...899L...6L__Margalit_et_al._2019_Instance_1 | The leading FRB source model invokes magnetars as the power source to produce repeating bursts. There are two versions of this model. One version invokes rapidly spinning young magnetars that are produced in extreme stellar transients such as GRBs and SLSNe. The main motivation is that the host galaxy of FRB 121102 res... | [
"Margalit et al. 2019"
] | [
"A possible fix of this proposal is to introduce rapidly spinning magnetars born from binary neutron star (BNS) mergers"
] | [
"Background"
] | [
[
670,
690
]
] | [
[
550,
668
]
] |
2021MNRAS.503.3629D__Kelley,_Blecha_&_Hernquist_2017a_Instance_1 | Having found evidence that galaxies show morphological signatures of a recent galaxy merger over time-scales on the order of 300–500 Myr, we now consider the typical BH merger time-scales and the impact that may have on our results. Within the Illustris simulation (and indeed many similar simulations), a pair of BHs me... | [
"Kelley, Blecha & Hernquist 2017a"
] | [
"Recently, several works have attempted to estimate the expected coalescence time for binary BHs by post-processing cosmological simulations, finding time-scales on the order of 100s of Myr to Gyr for the binary coalescence time (e.g."
] | [
"Background"
] | [
[
734,
766
]
] | [
[
459,
692
]
] |
2016ApJ...821..107G__Gloeckler_&_Fisk_2015_Instance_2 | We repeated the plasma pressure calculation presented by Schwadron et al. (2011) and Fuselier et al. (2012) for the new ENA energy spectrum. The results for the downwind hemisphere and for the Voyager 1 region are summarized in Table 3. The measured intensity
j
ENA
of neutralized hydrogen at a given energ... | [
"Gloeckler & Fisk 2015"
] | [
"For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed"
] | [
"Uses"
] | [
[
1174,
1195
]
] | [
[
1053,
1149
]
] |
2018ApJ...853...34Z__Giebels_et_al._2007_Instance_1 | Several well-studied TeV blazars show rich spectral behavior in X-rays, which may represent the general behavior of the synchrotron peak of all AGN jets. The X-ray spectra are usually curved (Massaro et al. 2004) and can only locally be fitted by a power law. The spectral variation with flux can be complex (Zhang et al... | [
"Giebels et al. 2007"
] | [
"Generally, the spectrum hardens when the flux increases",
"but photon indices can saturate at higher fluxes"
] | [
"Background",
"Background"
] | [
[
530,
549
]
] | [
[
339,
394
],
[
464,
512
]
] |
2022AandA...665A..46M__Côté_et_al._2019_Instance_1 | Several nucleosynthesis processes have been proposed as production sites of these light neutron-capture elements, including r-process in neutron star mergers (Wanajo et al. 2014; Watson et al. 2019), in magneto-rotational supernovae (Winteler et al. 2012), or in collapsars (Siegel et al. 2019), s-process in low- to int... | [
"Côté et al. 2019"
] | [
"It is not yet clear which process is the dominant source of the elements in the early Universe (see discussions by, e.g.,"
] | [
"Motivation"
] | [
[
661,
677
]
] | [
[
539,
660
]
] |
2022MNRAS.513.1459M__Conselice,_Yang_&_Bluck_2009_Instance_1 | Hierarchical structure formation scenarios (e.g. Fall & Efstathiou 1980; van den Bosch et al. 2002; Agertz, Teyssier & Moore 2011) predict that massive galaxies acquire much of their stellar mass through a combination of continuous cold gas accretion and mergers with smaller objects (e.g. Press & Schechter 1974; Moster... | [
"Conselice, Yang & Bluck 2009"
] | [
"As a consequence, mergers are also expected to play a significant role in driving the evolution of galaxy properties, for example,",
"star formation in the host galaxy or by driving its morphological evolution (e.g."
] | [
"Background",
"Background"
] | [
[
946,
974
]
] | [
[
454,
584
],
[
851,
932
]
] |
2019MNRAS.486....2M__Yamamoto_et_al._2014_Instance_1 | The discovery of ultraluminous pulsars (ULPs or PULXs; Bachetti et al. 2014; Fürst et al. 2016; Israel et al. 2017a,b; Carpano et al. 2018) has revolutionised the field of ultraluminous X-ray sources (ULXs; see the review of Kaaret, Feng & Roberts 2017). Whilst ULXs were long considered to be possible candidates for ho... | [
"Yamamoto et al. 2014"
] | [
"At the centre of the debate is the strength of the surface dipole field and any multipolar component. Should the dipole field strength be similar to that of Galactic HMXBs (1012 G – e.g.",
"then it is quite plausible that the flow will be supercritical ($\\dot{m}/\\dot{m}_{\\rm Edd} \\gt $ 1 where $\\dot{m}_{\\r... | [
"Motivation",
"Motivation"
] | [
[
1226,
1246
]
] | [
[
978,
1164
],
[
1248,
1470
]
] |
2016AandA...593A..22R__Shibuya_et_al._2015_Instance_2 | Although it is a simple concept, obtaining galaxy sizes is not an easy task and is subject to a number of assumptions. The most common way to derive galaxy sizes is by performing light-profile fitting assuming a given shape of the surface brightness profile using a χ2 minimization (e.g. Simard et al. 1999; Peng et al. ... | [
"Shibuya et al. 2015"
] | [
"We have now access to the size evolution up to z ~ 10 from the deepest HST imaging data"
] | [
"Background"
] | [
[
1614,
1633
]
] | [
[
1420,
1507
]
] |
2021ApJ...922..131T__Kumari_et_al._2019_Instance_1 | DIG contributes with a fraction of 20% to 90% of the total Hα flux in galaxy disks, with a mean fraction around 50%–60% (Hoopes & Walterbos 2003; Oey et al. 2007; Sanders et al. 2017; Tomičić et al. 2017; Poetrodjojo et al. 2019; Della Bruna et al. 2020; Tomičić et al. 2021). This large contribution may cause star form... | [
"Kumari et al. 2019"
] | [
"There is a debate about the extent to which DIG affects measurements of gas-phase metallicity and its radial slope",
"as some observations indicate lower metallicity (up to 1 dex) in DIG compared to nearby H ii regions."
] | [
"Motivation",
"Motivation"
] | [
[
721,
739
]
] | [
[
426,
540
],
[
766,
867
]
] |
2022AandA...667A..90M__Priestley_&_Whitworth_2022_Instance_1 | The line mass (mass per unit length) of G1.75-0.08 is Mline = 1011 ± 146 M⊙ pc−1. The dynamical state of the filament can be addressed by comparing its line mass with the virial or critical line mass (e.g. Fiege & Pudritz 2000, Eq. (12) therein). To calculate the latter quantity, we used the total (thermal+non-thermal)... | [
"Priestley & Whitworth 2022"
] | [
"For example, if G1.75-0.08 follows the line width–size relation in the central molecular zone, or CMZ, which for HCN is found to be σ ∝ R0.62",
", the aforementioned HCN(1 – 0) line width would be expected to be only ~2.5 km s−1 on the ~0.1 pc scale, which is a typical inner width (FWHM) of filamentary molecular... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1595,
1621
]
] | [
[
1209,
1350
],
[
1388,
1563
]
] |
2022ApJ...937...97C__Bottrell_et_al._2019_Instance_1 | Recently, machine learning (ML) has been applied to derive various physical parameters of galaxies (e.g., Masters et al. 2015; Krakowski et al. 2016; D’Isanto & Polsterer 2018; Bonjean et al. 2019; Davidzon et al. 2019; Hemmati et al. 2019; Chang et al. 2021) and improves on linear combinations through nonlinear activa... | [
"Bottrell et al. 2019"
] | [
"In particular, classification by ML (e.g.,",
"can avoid time-consuming visual inspections and will be helpful for the visual classification of galaxy−galaxy interactions from the forthcoming large surveys."
] | [
"Future Work",
"Future Work"
] | [
[
589,
609
]
] | [
[
465,
507
],
[
671,
830
]
] |
2018ApJ...864...31A__Smith_2007_Instance_1 | The FORCAST images of HD 168625 are shown in Figure 4. The nebula is clearly resolved, with a partially complete ring structure that has two peaks almost symmetric around the star. We concur with Meixner et al. (1999) and O’Hara et al. (2003) in their interpretation of these two peaks as limb-brightened peaks of a toru... | [
"Smith 2007"
] | [
"We stress that our SOFIA/FORCAST images do not detect the outer polar rings seen in Spitzer IRAC images"
] | [
"Differences"
] | [
[
621,
631
]
] | [
[
516,
619
]
] |
2018AandA...620L...8H__Gundlach_&_Blum_2013_Instance_1 | We adopted the model developed by Ďapek et al. (2005), in which 1D thermal conduction below each of the surface facets is solved numerically with the nonlinear Robin boundary condition at the surface, and the assumption of an isothermal core at a sufficient depth is made. A temperature-dependence of the thermal conduct... | [
"Gundlach & Blum 2013"
] | [
"For the sake of simplicity, the specific heat capacity c was assumed constant, c = 560 J kg−1 K−1, and the regolith grain density obtained for C-type meteorites was used, ρ = 3.11 g cm−3 (both from"
] | [
"Uses"
] | [
[
552,
572
]
] | [
[
354,
551
]
] |
2022MNRAS.517.4202X__Lister_et_al._2018_Instance_1 | Cavagnolo et al. (2010) suggested that the jet kinetic power is able to inflate the X-ray cavities or bubbles in different systems, including giant elliptical galaxies and cD galaxies (Type cD galaxy, a subtype of type-D giant elliptical galaxy), and proposed to evaluate the kinetic power Pkin = Pcav. However, this met... | [
"Lister et al. 2018"
] | [
"We collect the total radio flux density from literature"
] | [
"Uses"
] | [
[
1070,
1088
]
] | [
[
947,
1002
]
] |
2015MNRAS.453.3414A__the_1999_Instance_2 | Filippenko & Chornock (2001) first presented the dynamical estimate of mass of the source to be around 7.4 ± 1.1 M⊙. Recently, Radhika & Nandi (2014) claimed that the mass of XTE J1859+226 is perhaps in between 6.58 and 8.84 M⊙ which is similar to the prediction of Shaposhnikov & Titarchuk (2009), although the lower ma... | [
"Radhika & Nandi 2014"
] | [
"We estimate the fluxes Fx (see Table 1) of LHS and HIMS of the 1999 outburst of the source"
] | [
"Uses"
] | [
[
839,
859
]
] | [
[
747,
837
]
] |
2017MNRAS.472..940K__Malu_et_al._2010_Instance_1 | Cluster mergers can stir the intra-cluster medium (ICM) and lead to complex distributions of density and temperatures. The X-ray surface brightness traces regions of high electron densities ($\propto n_e^{2}$) and the SZ is sensitive to the pressure (∝neT) along the line of sight. An offset in the peaks of these signal... | [
"Malu et al. 2010"
] | [
"There are examples of merging clusters that show presence of X-ray–SZ offsets, such as",
"and Bullet cluster"
] | [
"Background",
"Background"
] | [
[
563,
579
]
] | [
[
416,
502
],
[
543,
561
]
] |
2016ApJ...821..107G__Schwadron_et_al._2011_Instance_3 | We repeated the plasma pressure calculation presented by Schwadron et al. (2011) and Fuselier et al. (2012) for the new ENA energy spectrum. The results for the downwind hemisphere and for the Voyager 1 region are summarized in Table 3. The measured intensity
j
ENA
of neutralized hydrogen at a given energ... | [
"Schwadron et al. 2011"
] | [
"For the density of neutral hydrogen in the inner heliosheath a constant nH = 0.1 cm−3 is assumed"
] | [
"Uses"
] | [
[
1151,
1172
]
] | [
[
1053,
1149
]
] |
2021MNRAS.500.5614A__Adrián-Martínez_et_al._2013_Instance_1 | Using ANTARES data from the end of 2007–2017, a search for upward-going muon neutrinos and antineutrinos in spatial and temporal coincidence with 784 GRBs has been performed. The numerical model NeuCosmA was used to estimate the expected neutrino flux from each burst individually, in the context of one-zone internal sh... | [
"Adrián-Martínez et al. 2013",
"Adrián-Martínez et al. 2013"
] | [
"A novel aspect of the search here presented is the inclusion in the data analysis chain of the uncertainty that possible unknown parameters, related to the characteristic activity of the central engine, can introduce in the neutrino flux evaluation. This is crucial in order to correctly interpret the validity of m... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
756,
783
],
[
1864,
1891
]
] | [
[
331,
754
],
[
1822,
1862
],
[
1920,
2084
]
] |
2019MNRAS.487.5902K__Behroozi,_Wechsler_&_Conroy_2013_Instance_1 | In the 50 Myr after a star particle is formed, it can undergo supernova (SN) explosions. These are randomly drawn from a delay-time distribution (Kimm et al. 2015). We employ the mechanical feedback model described in Kimm et al. (2015, 2017) and Rosdahl et al. (2018) and the amount of momentum injected into the gas de... | [
"Behroozi, Wechsler & Conroy 2013"
] | [
"Following Rosdahl et al. (2018), we have calibrated the SN feedback in order to reproduce the high-redshift stellar mass–halo mass relation from abundance matching"
] | [
"Uses"
] | [
[
961,
993
]
] | [
[
796,
959
]
] |
2017ApJ...850L..40A__Yang_et_al._2017_Instance_2 | Aided by the tight localization constraints of the three-detector network and the proximity of the GW source, multiple independent surveys across the EM spectrum were launched in search of a counterpart beyond the sGRB (Abbott et al. 2017c). Such a counterpart, SSS17a (later IAU-designated AT 2017gfo), was first discov... | [
"Yang et al. 2017"
] | [
"The same source was followed up and consistently localized at other wavelengths (e.g.,"
] | [
"Background"
] | [
[
1343,
1359
]
] | [
[
824,
910
]
] |
2017ApJ...850...20G__Lonardoni_et_al._2015_Instance_1 | The observation of massive neutron stars Demorest et al. (2010), Antoniadis et al. (2013) indicates that the EoS of nuclear matter must be very stiff in the regime of high densities and low temperatures. The degree of stiffness in the nuclear matter EoS is directly related to the repulsive interaction among particles a... | [
"Lonardoni et al. 2015"
] | [
"On the one hand, it is more energetically favorable for the system to populate new degrees of freedom, such as hyperons",
"in order to lower its Fermi energy (starting at about two times the saturation density)."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
814,
835
]
] | [
[
542,
661
],
[
1345,
1433
]
] |
2019MNRAS.484.4083H__Kappenman_2006_Instance_1 | The primary impact of the 1859 storm was on telegraphy (e.g. Boteler 2006). Today the principal ‘space weather’ threat is to the electric power grid (Baker et al. 2008; Hapgood, 2011, 2012; Oughton et al. 2016; Dyer et al. 2018). Because of this threat, several studies have been carried out to estimate how frequently s... | [
"Kappenman 2006"
] | [
"Such studies are dependent on the observations of a handful of storms that have approached or rivalled the Carrington geomagnetic storm in observed/inferred intensity and/or auroral extent. These include great storms in",
"May 1921"
] | [
"Background",
"Background"
] | [
[
868,
882
]
] | [
[
458,
677
],
[
833,
841
]
] |
2020MNRAS.499.3792B__Pimbblet_2011_Instance_1 | 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)"
] | [
"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"
] | [
"Uses"
] | [
[
249,
264
]
] | [
[
0,
248
]
] |
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