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 |
|---|---|---|---|---|---|---|
2020ApJ...892L..10Y__Macchi_2013_Instance_2 | In this section, we consider the plasma properties under the propagation of strong waves. In strong waves, the motion of electrons in the plasma becomes relativistic. However, different from free electrons that have a relativistic drift velocity in the direction of the incident electromagnetic wave (see Section 3.1), i... | [
"Macchi 2013"
] | [
"The dispersion relation of strong electromagnetic waves is altered due to the effective electron mass increased by the relativistic effect (e.g.,"
] | [
"Uses"
] | [
[
1320,
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[
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2021ApJ...921...20H__Hayasaki_et_al._2013_Instance_1 | It is still debated if and how all the stellar debris efficiently circularizes via the stream–stream collision. Some hydrodynamical simulations show that the TDE disk retains a significantly elliptical shape because the orbital energy is not dissipated efficiently enough to reduce the eccentricity of the entire disk to... | [
"Hayasaki et al. 2013"
] | [
"Nevertheless, the debris that remains bound eventually contributes to the accretion flow around the SMBH. This part of the debris stream will finally be circularized by energy dissipation, leading to the formation of a small, initially ring-like, accretion disk around the black hole"
] | [
"Background"
] | [
[
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[
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2016ApJ...816...41Y__Litvinenko_&_Wheatland_2005_Instance_1 | Some previous observations have shown that surface motions (e.g., shearing motions and converging motions) acting on preexisting coronal fields to form filaments and filament channels always act over a short period of a few days (Gaizauskas et al. 1997; Schmieder et al. 2004; Wang & Muglach 2007; Yan et al. 2015; Yang ... | [
"Litvinenko & Wheatland 2005"
] | [
"It is worth noting that the “head-to-tail” scenario seems to support the idea that the filament is supported by sheared arcades"
] | [
"Compare/Contrast"
] | [
[
951,
978
]
] | [
[
822,
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] |
2020MNRAS.494.4382S___2010_Instance_2 | It has been thought that QPOs originate from the innermost part of an accretion disc, which is associated with strong gravity, so that we might detect general relativistic effects. Miller et al. (1998) proposed beat-frequency models and estimated the parameters of NSs using this model. Stella & Vietri (1999) developed ... | [
"Shi & Li",
"2010"
] | [
"obtained the twin modes of MHD waves in LMXBs (including NS LMXBs and black hole LMXBs), which are considered as the sources of high-frequency QPOs."
] | [
"Background"
] | [
[
679,
687
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2021ApJ...921..179L__Kuznetsov_&_Kolotkov_2021_Instance_1 | Solar flares are powerful eruption events on the Sun associated with a rapid and violent release of magnetic free energy through a reconnection process. A typical flare can radiate at almost all wavelengths constituting the solar spectrum, ranging from radio through optical and ultraviolet (UV) to soft/hard X-ray (SXR/... | [
"Kuznetsov & Kolotkov 2021"
] | [
"The quantitative estimation of the radiated flare energy partition suggested about",
"and 55%–80% in WL for stellar flares (e.g.,"
] | [
"Background",
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] | [
[
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[
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2021AandA...655A..25Z__García-Burillo_et_al._2014_Instance_2 | Outflows are ubiquitous in both luminous AGN and in local Seyfert galaxies, and occur on a wide range of physical scales, from highly ionised semi-relativistic winds and jets in the nuclear region at subparsec scales to galactic scale outflows seen in mildly ionised, molecular, and neutral gas (Morganti et al. 2016; Fi... | [
"García-Burillo et al. 2014"
] | [
"The nuclear semi-relativistic phase and the galaxy-scale molecular phase have been observed simultaneously in less than a dozen sources, with varied results:",
"in other cases data suggest momentum driven flows (e.g."
] | [
"Background",
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] | [
[
2953,
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2020MNRAS.499.4666F__Popping_et_al._2017_Instance_1 | An example of these implications is the so-called ‘dust budget crisis’ introduced in Section 4.4: the dust masses currently estimated at z > 5 are not compatible with standard dust production channels and require an overhaul in our models of the initial mass function for star formation, of supernova production rates, o... | [
"Popping et al. 2017"
] | [
"The growth of dust grains through accretion in the ISM has been proposed as a solution (e.g.",
"but there are doubts on the efficiency of accretion at high z, where high dust temperatures due to the CMB (see Section 3.3) keep the desorption time-scale for accreted materials short"
] | [
"Background",
"Compare/Contrast"
] | [
[
610,
629
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[
478,
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[
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2018ApJ...853..148C__Shibuya_et_al._2014_Instance_1 | LAE galaxies are defined by a high equivalent width (EW > 20 Å) Lyα line and are believed to be composed of extremely large regions of active star formation. Many efforts have been made to detect and characterize LAE galaxies (e.g., Conselice et al. 2003; Conselice 2004; Ravindranath et al. 2006; Shimasaku et al. 2006;... | [
"Shibuya et al. 2014"
] | [
"Efforts have been made in quantifying mass, star formation rates, gas composition, and kinematics, as well as other LAE properties (e.g.,"
] | [
"Background"
] | [
[
1016,
1035
]
] | [
[
789,
926
]
] |
2018AandA...618A.128C__Croft_et_al._2005_Instance_1 | As described in Sect. 1, the galaxy protocluster associated with 7C 1756+6520 is characterized by a high fraction of AGN protocluster members: seven AGN, including the central radio galaxy, have been spectroscopically confirmed in close proximity both spatially and in redshift space of the protocluster. This high AGN f... | [
"Croft et al. 2005"
] | [
"This high AGN fraction detected so far, ~23%, makes the overdensity around 7C 1756+6520 similar to the interesting and well-studied cluster around the radio galaxy PKS 1138−262 from this point of view as well"
] | [
"Motivation"
] | [
[
539,
556
]
] | [
[
305,
513
]
] |
2021MNRAS.500.2336Y__Lin_et_al._2020_Instance_2 | Various surveys of SNRs in our Galaxy and nearby galaxies have been carried out at radio, X-ray, Infrared (IR), and optical wavelengths. The first extragalactic SNR candidates were identified in the LMC by Mathewson & Healey (1964) and later confirmed with a combination of radio and optical techniques by Westerlund & M... | [
"Lin et al. 2020"
] | [
"As a result, optical studies have produced the largest number (∼1200) of new extra-Magellanic SNR candidates. Optical extragalactic searches for SNRs are mainly done by using an emission line ratio criterion of the form [S ii]/H α > 0.4–0.5"
] | [
"Background"
] | [
[
1355,
1370
]
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[
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2022AandA...658A.188S__Kreckel_et_al._2019_Instance_1 | We assumed a screen geometry and used PYNEB3 (Luridiana et al. 2015) to correct line fluxes for dust extinction via the Hα/Hβ ratio, adopting the O’Donnell (1994) reddening law with RV = 3.1 and a theoretical Hα/Hβ = 2.86. The extinction-corrected emission line luminosities of the H II regions were then computed using ... | [
"Kreckel et al. 2019"
] | [
"This calibration is relatively insensitive to changes in gas pressure or ionization parameter, and we adopted it as fiducial approach in this paper (see",
", for a discussion)."
] | [
"Background",
"Background"
] | [
[
1034,
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[
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2016AandA...587A.159G__Tian_et_al._2014_Instance_2 | 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... | [
"Tian et al. 2014"
] | [
"Of course, care has to be taken to avoid combinations of biosignature molecules which can be generated abiotically together (see e.g."
] | [
"Background"
] | [
[
1835,
1851
]
] | [
[
1701,
1834
]
] |
2022ApJ...926...21B__Vida_et_al._2014_Instance_1 | Characterizing the differential rotation (DR) realized at the base and in the convective envelope of solar-type stars is central to the understanding of their magnetic field generation, activity level, and rotation, as it is directly linked to the Ω effect (e.g., stretching of the poloidal magnetic field lines by large... | [
"Vida et al. 2014"
] | [
"short-term Fourier transform",
"are methods to infer DR."
] | [
"Background",
"Background"
] | [
[
696,
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]
] | [
[
666,
694
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[
714,
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2019ApJ...886...15T__Gruendl_&_Chu_2009_Instance_1 | ALMA is capable of resolving internal structures of molecular clouds even in external galaxies. In particular, the Large Magellanic Cloud (LMC) is an ideal laboratory to investigate high-mass star formation thanks to its nearly face-on view (Balbinot et al. 2015) and the close distance, ∼50 kpc (Schaefer 2008; de Grijs... | [
"Gruendl & Chu 2009"
] | [
"It is also a great advantage to directly compare the distributions of molecular gas observed by ALMA and positions of massive YSOs identified by Spitzer and Herschel (e.g.,",
"without any serious contamination in the line of sight."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
508,
526
]
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[
335,
507
],
[
565,
620
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] |
2019AandA...627A..53H__Sutherland_&_Bicknell_2007_Instance_1 | A spatial coincidence of the radio jet morphology and velocity dispersion of the ionised gas has already been reported for spatially-resolved spectroscopy of more luminous radio-quiet AGN (e.g. Husemann et al. 2013; Villar-Martín et al. 2017) and powerful compact radio sources (e.g. Roche et al. 2016), but it has been ... | [
"Sutherland & Bicknell 2007"
] | [
"Hence, we think that the radio jet is transferring its energy and momentum to the ambient medium through an extended shock front, which creates turbulence in a dense clumpy ISM. Such a great impact of the radio jet has been observationally shown in many cases",
"and theoretically supported through detailed hydro... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1269,
1295
]
] | [
[
703,
962
],
[
1168,
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2018AandA...616A..11G__Quinn_et_al._1993_Instance_1 | In addition to secular evolutionary processes, a disc galaxy like ours is expected to have experienced several accretion events in its recent and early past (Bullock & Johnston 2005; De Lucia & Helmi 2008; Stewart et al. 2008; Cooper et al. 2010; Font et al. 2011; Brook et al. 2012; Martig et al. 2012; Pillepich et al.... | [
"Quinn et al. 1993"
] | [
"Events that took place in the far past are expected to have induced a thickening of the early Galactic disc, first by increasing the in-plane and vertical velocity dispersion of stars"
] | [
"Background"
] | [
[
931,
948
]
] | [
[
746,
929
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2017ApJ...834...20A__Temi_et_al._2007a_Instance_2 | Lenticular galaxies seems to have a wider range of properties compared to ellipticals that resemble more the old definition of ETGs. However, even in ellipticals, large differences prevail. Recent observations of elliptical galaxies with Spitzer and Herschel (Temi et al. 2005, 2007a, 2007b, 2009; Smith et al. 2012; Agi... | [
"Temi et al. 2007a"
] | [
"The 70 μm band luminosities (from",
"is a good example of such a huge scatter in the FIR luminosity of elliptical galaxies."
] | [
"Background",
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] | [
[
534,
551
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] | [
[
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[
560,
646
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2021MNRAS.501.4148L__Buchhave_et_al._2012_Instance_1 | We derived the photospheric stellar parameters using three different techniques: the curve-of-growth approach, spectral synthesis match, and empirical calibration. The first method minimizes the trend of iron abundances (obtained from the equivalent width, EW, of each line) with respect to excitation potential and redu... | [
"Buchhave et al. 2012"
] | [
"The spectral synthesis match was performed using the Stellar Parameters Classification tool (SPC,",
"It determines effective temperature, surface gravity, metallicity, and line broadening by performing a cross-correlation of the observed spectra with a library of synthetic spectra, and interpolating the correlat... | [
"Uses",
"Uses"
] | [
[
1238,
1258
]
] | [
[
1140,
1237
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[
1267,
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2022MNRAS.514.1961R__Prochaska_&_Zheng_2019_Instance_1 | Along with the time-domain detections, we identified J173438.35-504550.4 as a potential host galaxy for FRB 20201123A using robust statistical treatment given the relatively small localization error region. At face value, the low redshift of J173438.35-504550.4 appears at odds with the large dispersion measure for FRB ... | [
"Prochaska & Zheng 2019"
] | [
"Our Galaxy, however, contributes",
"from its interstellar medium and a presumed ${\\rm DM}_{\\rm Halo}\\sim 50 \\, {\\rm pc \\, cm^{-3}}$ from its halo"
] | [
"Uses",
"Uses"
] | [
[
670,
692
]
] | [
[
388,
420
],
[
559,
668
]
] |
2017ApJ...850...20G__Vidaña_2016_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... | [
"Vidaña 2016"
] | [
"On the one hand, it is more energetically favorable for the system to populate new degrees of freedom, such as hyperons"
] | [
"Motivation"
] | [
[
933,
944
]
] | [
[
542,
661
]
] |
2015ApJ...804..130C__Bertschinger_1985_Instance_1 | We have rigorously developed the embedded gravitational lensing theory for point mass lenses in a series of recent papers (Chen et al. 2010, 2011, 2015; Kantowski et al. 2010, 2012, 2013) including the embedded lens equation, time delays, lensing magnifications, shears, etc. We successfully extended the lowest-order em... | [
"Bertschinger 1985"
] | [
"For a cosmic void, embedding requires the underdense interior to be “compensated” by an overdense bounding ridge, i.e., a compensated void"
] | [
"Background"
] | [
[
1365,
1382
]
] | [
[
1206,
1344
]
] |
2019MNRAS.488.2825F__Hamers_et_al._2015_Instance_1 | On the other hand, the distribution of the orbital inclination of the third companion with respect to the inner binary in the triple i3 (bottom panel) is found to peak at ∼100°, but with non-negligible tails. For comparison, isolated triples that merge due to the KL mechanism show a very pronounced peak at ∼90°, with o... | [
"Hamers et al. 2015"
] | [
"Secondly, there are three different KL mechanisms competing, thus the eccentricity of the inner binary of the CO triple can be pumped up by the torque either of the SMBH or the third companion in the CO triple, for which the KL time-scale is shorter (e.g."
] | [
"Uses"
] | [
[
863,
881
]
] | [
[
607,
862
]
] |
2019AandA...629A..54U__Evans_et_al._2007_Instance_2 | 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... | [
"Evans et al. 2007"
] | [
"A soft excess below 1.5 keV is also present"
] | [
"Background"
] | [
[
766,
783
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] | [
[
721,
764
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2018ApJ...860...24P__Warmuth_2015_Instance_3 | Figure 13 shows the temporal evolution of the density, ρ, plasma flow velocity, vx, position of the wave crest, PosA, phase speed, vw, and magnetic field component in the z-direction, Bz, for the primary waves in every different case of initial amplitude, ρIA. In Figure 13(a), we observe that the amplitude of the densi... | [
"Warmuth 2015"
] | [
"In all four cases of different initial amplitude, ρIA, the phase speed decreases slighty (consistent with observations; see"
] | [
"Similarities"
] | [
[
2131,
2143
]
] | [
[
1983,
2106
]
] |
2015AandA...580L...2Z__Fender_et_al._2000_Instance_1 | Synchrotron radiation emitted from one relativistic electron population with density Nrel gyrating along a magnetic field B produces a power-law radio spectrum (S ∝ να) with spectral slope αthin 0 above a critical frequency νbreak that depends on B and Nrel. Below this critical frequency self-absorption effects become ... | [
"Fender et al. 2000"
] | [
"In the microquasar Cygnus X-1, radio emission has been measured with a flat spectrum, i.e. α = −0.06 ± 0.05 and α = 0.07 ± 0.04"
] | [
"Similarities"
] | [
[
1294,
1312
]
] | [
[
1165,
1292
]
] |
2016AandA...591A..30L__Fall_et_al._(2010)_Instance_1 | The catalog reported by Lada & Lada (2003) for embedded clusters is consistent with the mass-size relation R ~ M1/3 − M1/2 for low-mass clusters as pointed out by Murray (2009), where R and M are the gas radius and mass, respectively. While the stellar mass of an embedded cluster is not directly observable and is obtai... | [
"Fall et al. (2010)"
] | [
"Larger data sets of star-forming clumps, identified as gaseous protoclusters, also exhibit a mass-size relation.",
"compiled the observations of Shirley et al. (2003), Faúndez et al. (2004), and Fontani et al. (2005) in their Fig. 1, and found via least-squares regression the relation R ∝ M0.38.",
"Meanwhile, ... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1133,
1151
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] | [
[
1020,
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[
1727,
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2021MNRAS.500..291B__Longinotti_et_al._2015_Instance_1 | We have presented the analysis of the current X-ray observations of the disc wind in MCG-03-58-007. Here, multiple and variable wind components with velocities ranging from $\sim \! -0.08\, c$ to $\sim \! - 0.2\, c$ (and potentially up to $0.35\, c$) are seen at different times. Multi-epoch observations of disc winds, ... | [
"Longinotti et al. 2015"
] | [
"Other examples of AGN with at least two variable phases of the X-ray winds are",
"IRAS 17020+4544"
] | [
"Background",
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] | [
[
1362,
1384
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[
1099,
1177
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1345,
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2016ApJ...827...31F__Das_&_Chakrabarti_2007_Instance_1 | Accretion physics has been extensively studied for decades, particularly in terms of the theoretical aspects including semi-analytic investigations as well as global numerical simulations, in an effort to further understand its physical nature and observational consequences. Many of the works on BH accretion have, in g... | [
"Das & Chakrabarti 2007"
] | [
"Previous studies include",
"and magnetohydrodynamic (MHD) shocks"
] | [
"Background",
"Background"
] | [
[
1088,
1110
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] | [
[
886,
910
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[
1019,
1055
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2016ApJ...817...12P__Sur_et_al._2007_Instance_2 | Large-scale magnetic fields with strength of the order of 1–10 μG have been observed in disk galaxies (e.g., Beck et al. 1996; Fletcher 2010; Beck 2012; Beck & Wielebinski 2013; Van Eck et al. 2015). The origin of these fields can be explained through mean-field dynamo theory (Ruzmaikin et al. 1988; Beck et al. 1996; B... | [
"Sur et al. 2007"
] | [
"magnetic helicity flux from anisotropy of the turbulence produced by differential rotation"
] | [
"Background"
] | [
[
1358,
1373
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] | [
[
1207,
1297
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] |
2022AandA...663A.105P__Brunetti_et_al._2008_Instance_1 | Regardless of the cluster orientation, the spectral index observed for the halo at all available frequencies suggests that it is a USSRH. Despite the number of detected USSRH is still low, radio halos with steep indices are being discovered more and more frequently in the last years thanks to the improved observational... | [
"Brunetti et al. 2008"
] | [
"USSRH are a prediction of turbulent re-acceleration models"
] | [
"Background"
] | [
[
769,
789
]
] | [
[
688,
746
]
] |
2017MNRAS.470.2517H__D'Angelo_&_Lubow_2010_Instance_1 | We carry out analysis of the orbital properties of our clumps only using the sample as detected by the DDS, as this method is sensitive to most clump masses and semimajor axes. The total semimajor axis evolution of all clumps is shown in the left-hand panel of Fig. 3, which we have already discussed, and refer the read... | [
"D'Angelo & Lubow 2010"
] | [
"However, about half of our most massive clumps migrate radially outwards.",
"but requires either large torques or steep surface density gradients"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1001,
1022
]
] | [
[
787,
860
],
[
931,
999
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] |
2016ApJ...824..138Y__Frail_et_al._2013_Instance_1 | The above qualitative theoretical reasoning raises the question about why would Swift J1834.9−0846 be the only magnetar so far powering a wind nebula, given that previous searches around individual magnetars have returned no sign of extended emission attributable to wind nebulae (e.g., Viganò et al. 2014). With only on... | [
"Frail et al. 2013"
] | [
"Nevertheless, Swift J1834.9−0846 has some interesting characteristics that are not shared with the entire magnetar population. First, the environment of Swift J1834.9−0846 is extremely crowded, with a Fermi GeV source, an H.E.S.S. TeV source, an SNR, a GMC, and an OH maser in its vicinity"
] | [
"Compare/Contrast"
] | [
[
676,
693
]
] | [
[
385,
674
]
] |
2021MNRAS.503..594S__Tremaine,_Ostriker_&_Spitzer_1975_Instance_1 | Nuclear star clusters (NSCs) are dense and massive clusters observed with high frequency ($\gt 80{{\ \rm per\ cent}}$) at the centre of galaxies with stellar masses 109–1011 M⊙ (e.g. Böker et al. 2002, 2004; Côté et al. 2006; Turner et al. 2012; Baldassare et al. 2014; den Brok et al. 2014; Georgiev & Böker 2014; Sánch... | [
"Tremaine, Ostriker & Spitzer 1975"
] | [
"There are two main formation channels that are thought to compete in NSC formation:",
"or via orbital segregation and merger of massive star clusters that migrate towards the galactic centre via dynamical friction"
] | [
"Background",
"Background"
] | [
[
968,
1001
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] | [
[
641,
724
],
[
840,
966
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2022AandA...659A..41E__Sarbadhicary_et_al._2017_Instance_1 | The age of a neutron star is difficult to measure, as for many other astronomical sources. The most robust way to do it is by identifying the birth supernova of the neutron star. However, this can be done precisely only for a very small number of objects, as 5–10 supernovae have historically been observed in our galaxy... | [
"Sarbadhicary et al. 2017"
] | [
"The explosions, however, leave imprints in the interstellar medium that can remain visible at radio wavelengths for 10 − 100 kyr",
"thereby allowing the association of pulsars with supernova remnants (SNRs)."
] | [
"Background",
"Background"
] | [
[
582,
606
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] | [
[
452,
580
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[
609,
684
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2021MNRAS.505.5427N__Buen-Abad_et_al._2018_Instance_1 | While the status of the S8 discrepancy is perhaps somewhat less clear than that of the H0 tension, it is beyond question that there overall is some disagreement between high- and low-redshift probes of the amplitude of matter fluctuations (see, for instance, Di Valentino et al. 2020c, for a concise review of the proble... | [
"Buen-Abad et al. 2018"
] | [
"It is thus worthwhile to investigate whether new physics might solve or at least alleviate the S8 discrepancy, a possibility that has been investigated in several works.",
"Models that have been contemplated in this sense include for example",
"extended or exotic DM and/or dark energy (DE) models and interacti... | [
"Motivation",
"Background",
"Background"
] | [
[
1170,
1191
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] | [
[
324,
493
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[
494,
562
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[
971,
1040
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] |
2021ApJ...917L..38K__Mushtukov_et_al._2015a_Instance_1 | With the increase in precision of CRSF measurements, the dependence of CRSFs on luminosity and spin phase has become obvious and is one of the important areas of current X-ray pulsar research, as it potentially allows probing of emission region geometry and properties (Staubert et al. 2019). Of particular interest is t... | [
"Mushtukov et al. 2015a"
] | [
"As a result, two main accretion regimes, super- and subcritical accretion, are expected depending on whether the source luminosity is higher or lower than a “critical luminosity” Lcrit, which strongly depends on the magnetic field of the NS"
] | [
"Background"
] | [
[
889,
911
]
] | [
[
605,
845
]
] |
2018AandA...609A.131G__Heithausen_2012_Instance_1 | 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"
] | [
"Unfortunately, in the case of the M 81 Group, this technique appears hardly applicable since the radial velocities of extragalactic and Galactic clouds share a similar LSR (local standard of rest) velocity range"
] | [
"Compare/Contrast"
] | [
[
1609,
1624
]
] | [
[
1396,
1607
]
] |
2022MNRAS.511.1750J__Zirker_1977_Instance_1 | Table 1 depicts the heliolatitudes of the solar offset points on different experiment days and the corresponding heliocentric distances. It is to be noted that owing to the trajectory constraints of the spacecraft along the ecliptic plane, a pure latitudinal dependence (at a constant heliocentric distance) of the spect... | [
"Zirker 1977"
] | [
"The fast solar winds emanate from coronal holes at higher heliolatitudes"
] | [
"Uses"
] | [
[
882,
893
]
] | [
[
808,
880
]
] |
2021MNRAS.503.3065S__Silverman_1986_Instance_1 | In this work, the difference between G and NG clusters plays a major role. In a first step, we focus our attention on characterizing the structure and distribution of galaxy member properties in each class. In Fig. 1, we show the distributions of: (a) logarithmic virial mass ($\rm log(\mathit{ M}_{200}/M_{\odot })$); (... | [
"Silverman 1986"
] | [
"Aside from the histograms, we add a kernel smoothed curve, shown as shaded area, which is derived directly from the data set using an Epanechnikov Kernel Density estimator",
"with a bandwidth equal to 1.5 times the bin size."
] | [
"Uses",
"Uses"
] | [
[
1134,
1148
]
] | [
[
961,
1132
],
[
1150,
1199
]
] |
2022ApJ...927..106C__Motte_et_al._2007_Instance_1 | To identify the fibers seen in the PPV space, we apply the agglomerative clustering implementation in the scikit-learn package
7
7
https://scikit-learn.org/stable/
(Pedregosa et al. 2011) to the PPV points for each transition. The agglomerative clustering algorithm groups points in N-dimensional space via recursive... | [
"Motte et al. 2007"
] | [
"Among the fibers, f1 is clearly tracing the central-densest part of the dust ridge well known from previous dust-continuum observations"
] | [
"Uses"
] | [
[
1790,
1807
]
] | [
[
1653,
1788
]
] |
2022MNRAS.509..212D__Farris_et_al._2015_Instance_1 | On the other hand, at separations ≲ 0.01 pc, smaller than those characteristics of spectroscopic binary candidates, many theoretical studies have predicted a significant variability in the observed nuclear light curve due to different physical processes. For example, in studies of the evolution of MBHBs in circumnuclea... | [
"Farris et al. 2015"
] | [
"For example, in studies of the evolution of MBHBs in circumnuclear discs, a modulated gas inflow from the outer gas distribution periodically fuels the accretion discs within the Hill radii of the individual MBHs (that, being smaller than the surrounding circumbinary disc, are commonly referred to as ‘mini-discs’ ... | [
"Background",
"Background"
] | [
[
762,
780
]
] | [
[
255,
588
],
[
903,
987
]
] |
2018MNRAS.478..126G___2018b_Instance_1 | It may be appropriate to single out at this point the recent and interesting works by Lin & Ishak (2017a,b) in which the authors run a so-called (dis)cordance test based on using a proposed index of inconsistency (IOI) tailored at finding possible inconsistencies/tensions between two or more data sets in a systematic a... | [
"Riess et al",
"2018b"
] | [
"For instance, it is well known that there is a persistent discrepancy between the Planck CMB measurements of H0 and the local measurements based on distance ladder"
] | [
"Motivation"
] | [
[
503,
514
],
[
522,
527
]
] | [
[
338,
501
]
] |
2021AandA...655A..12T__Tang_et_al._2017b_Instance_1 | Using the RADEX3 non local thermodynamic equilibrium (LTE) modeling program (van der Tak et al. 2007) with collisional rate coefficients from Wiesenfeld & Faure (2013), we modeled the relation between the gas kinetic temperature and the measured average of para-H2CO 0.5 × [(322–221 + 321–220)/303–202] ratios, adopting ... | [
"Tang et al. 2017b"
] | [
"The values of the para-H2CO column density were obtained with APEX data (beam size ~30″;"
] | [
"Uses"
] | [
[
626,
643
]
] | [
[
537,
625
]
] |
2018MNRAS.480.1796S__Morić_et_al._2010_Instance_1 | To distinguish the emission from AGNs and star formation we use the fact that star-forming galaxies (SFGs) are known to exhibit radio–IR correlation across a wide range of luminosities and redshifts (see Condon 1992; Appleton et al. 2004; Basu et al. 2015). The correlation between 1.4 GHz luminosity and IR luminosity (... | [
"Morić et al. 2010"
] | [
"AGNs with predominant radio emission from jet deviate from radio–IR correlation by showing radio-excess",
"Therefore, we examine if our NLS1s show radio-excess in the radio–IR correlation."
] | [
"Uses",
"Uses"
] | [
[
644,
661
]
] | [
[
539,
642
],
[
686,
767
]
] |
2018AandA...609A...2M__Titov_&_Démoulin_(1999)_Instance_1 | The equilibrium between the MFR and the two magnetic charges can lead to an infinite twist on the surface of the MFR because no toroidal field exists outside the MFR. The magnetic field of the line current I0 is included to decrease this to reasonable values, typically less than 4π, suggested by many observations (Liu ... | [
"Titov & Démoulin (1999)"
] | [
"For an analytical expression of the poloidal magnetic field, we follow the practice of",
"in which poloidal field is given in terms of the vector potential as in (8)\\begin{equation} B_{p}=-\\frac{\\partial A_{t}}{\\partial x}\\frac{\\vec{r}_{\\perp}}{r_{\\perp}}+\\left(\\frac{\\partial A_t}{\\partial r_{\\perp}... | [
"Uses",
"Uses"
] | [
[
921,
944
]
] | [
[
834,
920
],
[
946,
1236
]
] |
2020AandA...633A.147B__Miville-Deschênes_et_al._2017_Instance_1 | Another possible indication of the different nature of the smallest clouds with respect to the largest ones is shown by their behaviour in the velocity dispersion vs. radius relation. This relation, known as the first Larson relation (Larson 1981), is expected to be of the form σv ∝ Rβ. The observed non-thermal motions... | [
"Miville-Deschênes et al. 2017"
] | [
"Various values of β in MCs have been derived by several authors, ranging from β ∼ 0.38",
"to β = 0.6 ± 0.3"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
686,
715
]
] | [
[
567,
653
],
[
668,
684
]
] |
2020MNRAS.496.4468S__Chang_et_al._2018_Instance_1 | More interestingly, there are hints suggesting that the impacts of projection effects extend beyond richness misidentification. First, when Miyatake et al. (2016) reported a possible detection of assembly bias for subsamples of clusters divided based on the concentration of member galaxies, the signal appeared too larg... | [
"Chang et al. 2018"
] | [
"More interestingly, there are hints suggesting that the impacts of projection effects extend beyond richness misidentification.",
"Secondly, when More et al. (2016) reported a detection of the so-called ‘splashback’ radius, a physically motivated boundary of cluster haloes, for redMaPPer clusters, the location o... | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
840,
857
]
] | [
[
0,
127
],
[
570,
839
],
[
859,
884
]
] |
2022ApJ...927...89W__Stetson_1987_Instance_1 | IRIS always takes short exposure (with the shortest possible exposure time of 2.2 s) and long exposure with specified exposure time (14.5 s) one by one. In order to estimate and subtract the sky background, each field was observed in 10 dithered positions. Raw exposures were sky-subtracted and flat-fielded using standa... | [
"Stetson 1987"
] | [
"Aperture photometry was performed with the DAOPHOT",
"package"
] | [
"Uses",
"Uses"
] | [
[
693,
705
]
] | [
[
641,
691
],
[
707,
714
]
] |
2020ApJ...897...38D__Gough_1990_Instance_1 | The problem of imaging global magnetic fields through helioseismology has been relatively underexplored, as studies have mainly focused on the solar rotational profile and other global and local flow fields (Lavely & Ritzwoller 1992; Basu et al. 1999; Giles 2000; Zhao & Kosovichev 2004; Hanasoge et al. 2012b, 2017). So... | [
"Gough 1990"
] | [
"Nevertheless, early attempts (e.g.,",
"that were made to study the impact of global magnetic fields (Lorentz-stress perturbations) on the eigenfrequencies and eigenfunctions of the standard solar model (model S in Christensen-Dalsgaard et al. 1996) focused on the details of the forward problem of frequency shift... | [
"Background",
"Background"
] | [
[
667,
677
]
] | [
[
631,
666
],
[
679,
1032
]
] |
2018MNRAS.474.3162T__Gavazzi_et_al._2004_Instance_1 | We then used the fxcor task to determine the redshifts of selected objects in the field. This task allows to calculate the radial velocity through Fourier cross-correlation between the spectrum of the object under analysis and a reference (template) spectrum (Tonry & Davis 1979). Both spectra are continuum subtracted a... | [
"Gavazzi et al. 2004"
] | [
"For this work, we used two reference spectra:",
"and the spectrum of NGC 4387",
"an elliptical galaxy showing strong absorptions."
] | [
"Uses",
"Uses",
"Uses"
] | [
[
607,
626
]
] | [
[
443,
488
],
[
577,
605
],
[
629,
677
]
] |
2018MNRAS.477..392L__Izotov_&_Thuan_1998_Instance_1 | Here, we present new Very Large Telescope (VLT) VIMOS (Le Févre et al. 2003) observations of two star-forming dwarf galaxies using the integral field unit (IFU) spectroscopy mode (hereafter VIMOS-IFU). UM 461 (the upper panel in Fig. 1) is a well-studied H ii/BCD galaxy (e.g. Taylor et al. 1995; van Zee, Skillman & Sal... | [
"Izotov & Thuan 1998"
] | [
"It has been classified as having a cometary-like morphology with an integrated subsolar metallicity of 12 + log(O/H) = 7.73–7.78"
] | [
"Background"
] | [
[
784,
803
]
] | [
[
615,
743
]
] |
2016AandA...587A.133G__Wise_et_al._2014_Instance_1 | Theoretically, the production, propagation, and escape of LyC photons are related to the physical properties of the galaxies. Firstly, the production of LyC radiation implies the presence of young, massive stars, and therefore of on-going star formation. Because of the fast recombination timescale of the HI atoms, prev... | [
"Wise et al. 2014"
] | [
"Secondly, the propagation of LyC photons within the ISM is favoured by a negligible amount of dust and low column density of HI (N(HI) ≤ 1018 cm-2) in a 10-pc scale region around the emitting star clusters. This could be the case for galaxies embedded in dark-matter halos with masses less than 108 M⊙"
] | [
"Background"
] | [
[
804,
820
]
] | [
[
481,
782
]
] |
2018AandA...609A..13K__Mucciarelli_et_al._(2017)_Instance_1 | 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)"
] | [
"Subsequently,",
"measured chemical abundances of six stars in Gaia 1, suggesting an equally high metallicity, but based on their abundance study, the suggestion of an extragalactic origin was revoked.",
"While a more metal-rich nature found by the latter authors conformed with the results by Simpson et al. (20... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1088,
1113
]
] | [
[
1074,
1087
],
[
1114,
1297
],
[
1298,
1527
]
] |
2018AandA...615A.148D__Sung_et_al._2013_Instance_1 | 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"
] | [
"On the other hand, many fewer studies, all recent, were devoted to the full mass spectrum, using optical photometry"
] | [
"Background"
] | [
[
487,
498
],
[
505,
509
]
] | [
[
370,
485
]
] |
2016ApJ...832..195N__Jin_et_al._2012_Instance_1 | We ignore the density stratification effect in Case I, II, and IIa, because the width of the horizontal current sheet in our simulations is much shorter than the length. The simulation domain extends from x = 0 to x = L0 in the x-direction, and from
y
=
−
0.5
L
0
to
y
=
0.5
L
0
in the y-dire... | [
"Jin et al.",
"2012"
] | [
"The magnetic fields in the low solar atmosphere could be very strong"
] | [
"Uses"
] | [
[
1392,
1402
],
[
1409,
1413
]
] | [
[
1322,
1390
]
] |
2015AandA...580A.135D__Cormier_et_al._2015_Instance_1 | How does the propagation of radiation and the ISM composition affect ISM observables in low-metallicity galaxies? Addressing this question is important to understand the evolution of low-metallicity galaxies, which undergo more bursty star formation than normal galaxies. Nearby star-forming dwarf galaxies present disti... | [
"Cormier et al. 2015"
] | [
"Mid-IR (MIR) and far-IR (FIR) observations have revealed bright atomic lines from H ii regions ([S iii], [Ne iii], [Ne ii], [O iii], etc.) and PDRs ([C ii], [O i]) (e.g.,"
] | [
"Background"
] | [
[
808,
827
]
] | [
[
563,
733
]
] |
2021MNRAS.501.2112S__Rubin_et_al._2012_Instance_1 | This work improves the efficiency of component by component modelling that has been successful in recovering the physical conditions for various individual absorbers (e.g. Churchill & Charlton 1999; Charlton et al. 2000, 2003; Ding et al. 2003a, 2003b; Zonak et al. 2004; Ding, Charlton & Churchill 2005; Masiero et al. ... | [
"Rubin et al. 2012"
] | [
"It is important to do so because different processes, e.g.",
"pristine accretion",
"are surely contributing to the same system"
] | [
"Motivation",
"Motivation",
"Motivation"
] | [
[
1139,
1156
]
] | [
[
944,
1002
],
[
1099,
1117
],
[
1294,
1336
]
] |
2017ApJ...838...32Y__Somov_et_al._1981_Instance_1 | The question whether electrons are able to penetrate into deep and dense layers of the solar atmosphere is currently under scrutiny. Calculations by Emslie (1978) showed that for electrons and/or protons to reach the
level, their energy has to be of the order of a few MeV, while electron energy in the strongest ... | [
"Somov et al. 1981"
] | [
"Works by other authors seem to support the idea that power-law beam electrons may precipitate throughout the entire flaring atmosphere down to the photosphere",
", causing its heating via inelastic collisions with the ambient plasma via a hydrodynamic response"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1073,
1090
]
] | [
[
773,
931
],
[
973,
1071
]
] |
2015AandA...584A.103S__Potekhin_et_al._2013_Instance_4 | Douchin & Haensel (2001; DH) formulated a unified EoS for NS on the basis of the SLy4 Skyrme nuclear effective force (Chabanat et al. 1998), where some parameters of the Skyrme interaction were adjusted to reproduce the Wiringa et al. calculation of neutron matter (Wiringa et al. 1988) above saturation density. Hence, ... | [
"Potekhin et al. 2013"
] | [
"and a comparison with the other EoSs of the BSk family",
"shall be left for future study."
] | [
"Future Work",
"Future Work"
] | [
[
2025,
2045
]
] | [
[
1907,
1961
],
[
2088,
2119
]
] |
2021MNRAS.500.3527B__Bernet_et_al._2008_Instance_1 | The origin of kiloparsec scale magnetic fields observed in the nearby galaxies through the polarized radio synchrotron emission (e.g. Fletcher 2010; Beck 2012, etc.) is attributed to the large-scale dynamo operating in the interstellar medium (ISM). This is driven mainly via the helical turbulent motions in the interst... | [
"Bernet et al. 2008"
] | [
"This is perhaps a much too slow to account for the strong equipartition strength magnetic fields observed in the high-redshift galaxies with z > 1 (e.g.",
"or even for that in the slowly rotating nearby galaxies. This discrepancy leads one to invoke some additional mechanism such as cosmic rays (CRs) boosting th... | [
"Motivation",
"Motivation"
] | [
[
1022,
1040
]
] | [
[
869,
1021
],
[
1042,
1223
]
] |
2016AandA...592A..19C__Maraston_et_al._(2009)_Instance_1 | Since the star-formation histories of galaxies (ETGs included, e.g. De Lucia et al. 2006; Maraston et al. 2009) can be stochastic and include multiple bursts, we also verify the full-spectrum fitting capabilities to retrieve more complex SFHs. In particular, we take an 11 Gyr old composite stellar population with an ex... | [
"Maraston et al. 2009"
] | [
"Since the star-formation histories of galaxies (ETGs included, e.g.",
"can be stochastic and include multiple bursts, we also verify the full-spectrum fitting capabilities to retrieve more complex SFHs."
] | [
"Uses",
"Uses"
] | [
[
90,
110
]
] | [
[
0,
67
],
[
112,
243
]
] |
2022MNRAS.509.6091H__Tremmel_et_al._2017_Instance_1 | Galactic winds have been ubiquitously observed in galaxies at both low and high redshifts, and they are critical to galaxy formation and evolution. Simulations calibrated to match these observations predict that a large amount of galactic material is ejected as a wind before reaccreting to either form stars or be eject... | [
"Tremmel et al. 2017"
] | [
"Current cosmological hydrodynamic simulations of galaxy formation employ a variety of subgrid models (e.g.",
"that artificially launch galactic winds, but the results are sensitive to numerical resolution and the exact subgrid model employed"
] | [
"Background",
"Background"
] | [
[
669,
688
]
] | [
[
389,
495
],
[
751,
882
]
] |
2022MNRAS.512.4893Z__Toft_et_al._2014_Instance_1 | Submillimetre galaxies (SMGs) are ultraluminous dusty star-forming galaxies (SFGs) with the vast majority of radiation energy in the far-infrared (FIR) and submillimetre bands (Smail, Ivison & Blain 1997; Barger et al. 1998; Hughes et al. 1998; Michałowski et al. 2012; Casey, Narayanan & Cooray 2014). They are extreme ... | [
"Toft et al. 2014"
] | [
"The physical properties of SMGs derived from detailed studies of individual sources and large sky area submillimetre surveys suggest that SMGs represent an early evolutionary phase of all local ellipticals"
] | [
"Background"
] | [
[
958,
974
]
] | [
[
694,
899
]
] |
2018ApJ...863..162M__Liu_et_al._2013_Instance_3 | NLFFF extrapolation provides the reconstructed coronal magnetic field for AR 11158 from 2011 February 13 − 2011 February 15 (Figures 1(d)–(f)). The field lines (yellow lines) within the core of the AR have arcade-like structure with a relatively strong twist mainly near the PIL. These figures show that the magnetic fie... | [
"Liu et al. 2013"
] | [
"The high-twist region in our result is also in agreement with the",
"and the location of the flare ribbons"
] | [
"Similarities",
"Similarities"
] | [
[
1612,
1627
]
] | [
[
1434,
1499
],
[
1554,
1591
]
] |
2021ApJ...915...86A__Owen_&_Sathyaprakash_1999_Instance_1 | This analysis searches for a GW signal compatible with the inspiral of a BNS or NSBH binary—collectively NS binaries—within 6 s of data associated with an observed short GRB. This stretch of data is the on-source window and runs from −5 s to +1 s around the start of the GRB emission (i.e., the GRB trigger time). The su... | [
"Owen & Sathyaprakash 1999"
] | [
"We scan each trial of data and the on-source window in the 30–1000 Hz frequency band using a predefined bank of waveform templates"
] | [
"Uses"
] | [
[
1128,
1153
]
] | [
[
996,
1126
]
] |
2016ApJ...826L..14W__Goudfrooij_et_al._2015_Instance_1 | Figure 1 shows the NGC 419 CMD after field-star decontamination. The cluster has an eMSTO at 20 ≤ V ≤ 22 mag. We adopted the Padova stellar evolution models (PARSEC CMD 2.7, v. 1.2S; Bressan et al. 2012),8
8
http://stev.oapd.inaf.it/cgi-bin/cmd_2.7
for Z = 0.004 (Glatt et al. 2008; Girardi et al. 2009), and fitted ... | [
"Goudfrooij et al. 2015"
] | [
"Previous studies of intermediate-age star clusters with eMSTOs usually showed tight SGBs throughout",
"but see"
] | [
"Differences",
"Differences"
] | [
[
1036,
1058
]
] | [
[
853,
952
],
[
1028,
1035
]
] |
2022ApJ...926...21B__Käpylä_et_al._2011_Instance_1 | Some studies have used the 2.5D mean-field dynamo approach to do so, extending solar mean-field dynamo models to other stellar spectral types (Chabrier & Küker 2006; Jouve et al. 2010; Küker et al. 2011; Kitchatinov et al. 2018, and references therein). While these studies are very helpful, most of them lack the full n... | [
"Käpylä et al. 2011"
] | [
"Nevertheless, with the arrival of more powerful supercomputers, other authors have used instead global 3D MHD simulations to model DR and stellar magnetism in the convection zone of solar-like stars"
] | [
"Background"
] | [
[
911,
929
]
] | [
[
589,
787
]
] |
2022MNRAS.513.5377F__Blum_et_al._2017_Instance_1 | At each heliocentric distance rh, the activity model (Fulle et al. 2020b) is defined by five analytical equations fixing (i) the gas pressure P(s) depending on the depth s from the nucleus surface (Fig. 1 for the CO2 case), (ii) the gas flux Q from the nucleus surface, (iii) the temperature gradient ∇T at depths of a f... | [
"Blum et al. 2017"
] | [
"where P0, T0, and Λ values are listed in Table 1, s is the depth from the nucleus surface, $f(s) = 1 - (1 - {s \\over R})^4$ for s ≤ R, f(s) = 1 elsewhere, r ≈ 50 nm and R ≈ 5 mm are the radii of the grains of which cometary dust consists",
"and of the pebbles of which cometary nuclei"
] | [
"Uses",
"Uses"
] | [
[
1434,
1450
]
] | [
[
1070,
1307
],
[
1381,
1424
]
] |
2016ApJ...826..168X__Bai_2014_Instance_2 | MRI is considered to be the most promising mechanism driving angular-momentum transport in protoplanetary disks (Balbus & Hawley 1991; Brandenburg et al. 1995; Hawley et al. 1995; Balbus et al. 1996; Balbus & Hawley 1998). However, protoplanetary disks are cold, dense, and, therefore, poorly ionized. The low level of i... | [
"Bai 2014"
] | [
"Three-dimensional simulations that include all three non-ideal MHD effects are also performed"
] | [
"Background"
] | [
[
1859,
1867
]
] | [
[
1764,
1857
]
] |
2021AandA...653A..36M__Goulding_&_Alexander_(2009)_Instance_1 | 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)"
] | [
"To also cover lower luminosity galaxies, as the GOALS sample only includes luminous IR galaxies (LIRGs) and ultra-luminous IR galaxies (ULIRGs), we included 38 galaxies from Bernard-Salas et al. (2009) and",
"to reach the total sample of 196 galaxies with IR line fluxes in the 5.5 − 35 μm interval in which an AG... | [
"Uses",
"Uses"
] | [
[
933,
960
]
] | [
[
727,
932
],
[
962,
1094
]
] |
2020MNRAS.492..686L__Shiokawa_et_al._2015_Instance_1 | After the disruption phase, the star is tidally stretched into a very long thin stream and the evolution of the stream structure in the transverse and longitudinal directions are decoupled (Kochanek 1994). Thus, the system enters the free-fall phase where each stream segment follows its own geodesic like a test particl... | [
"Shiokawa et al. 2015"
] | [
"It has been shown that shocks at the self-intersection point is the main cause of orbital energy dissipation and the subsequent formation of an accretion disc"
] | [
"Background"
] | [
[
961,
981
]
] | [
[
704,
862
]
] |
2018ApJ...854..141D__Vegetti_et_al._2014_Instance_1 | Our approach shares its transdimensional nature with that of Brewer et al. (2015), which implemented an independent transdimensional framework to infer substructure in strong lens systems. However, in addition to differences concerning substructure modeling and the sampling method used, our code and analysis were devel... | [
"Vegetti et al. 2014"
] | [
"While both codes are public, we understand that this approach is not yet ubiquitous in the field of galaxy-scale strong lensing (for instance, it has been difficult thus far to reproduce/check the results of",
"and Hezaveh et al. 2016), but we hope that our work can help make substructure lensing more reproducib... | [
"Differences",
"Differences"
] | [
[
782,
801
]
] | [
[
574,
781
],
[
802,
907
]
] |
2016AandA...586A..80O__Fornasier_et_al._2015_Instance_1 | Figure 1 shows that in the regions where activity was detected visually, i.e., Hapi, Seth, and Ma’at pits have lower (8–13%/100 nm) spectral slopes than the rest of the comet surface (13–22%/100 nm). In addition to those places, Seth alcoves, the wall of the large Anuket alcove, around the circular features, both clust... | [
"Fornasier et al. 2015"
] | [
"In the regions we investigated, the Hapi region displays the lowest spectral slopes 8–11%/100 nm (see also",
"together with the isolated bright features (IBFs) and the clustered bright features in the Imhotep region."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
848,
869
]
] | [
[
741,
847
],
[
871,
977
]
] |
2021ApJ...906...57S__Mishra-Sharma_et_al._2017_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... | [
"Mishra-Sharma et al. 2017"
] | [
"We introduce a method to search for signatures of DM annihilation from a Galactic subhalo population using the non-Poissonian template fitting (NPTF) framework"
] | [
"Uses"
] | [
[
945,
970
]
] | [
[
739,
898
]
] |
2020AandA...635A.121M__Matter_et_al._(2016)_Instance_1 | Our model consists of four zones; an inner disk (zone 1, as in Matter et al. 2016), and three zones into which the outer disk is divided (zones 2–4) in order to produce the azimuthal asymmetries seen in our SPHERE observations. The radial extent of these zones were constrained from our images: zone 2 corresponds to the... | [
"Matter et al. 2016"
] | [
"Our model consists of four zones; an inner disk (zone 1, as in"
] | [
"Uses"
] | [
[
63,
81
]
] | [
[
0,
62
]
] |
2017AandA...601A.134M__Fung_&_Dong_(2015)_Instance_1 | Several predictions for planet(s) shaping the disk of SAO 206462 have been proposed (Muto et al. 2012; Garufi et al. 2013; Fung & Dong 2015; Bae et al. 2016; van der Marel et al. 2016a. Using linear equations from the spiral density wave theory, Muto et al. (2012) suggested two planets with separations beyond ~50 au by... | [
"Fung & Dong 2015"
] | [
"Several predictions for planet(s) shaping the disk of SAO 206462 have been proposed"
] | [
"Background"
] | [
[
123,
139
]
] | [
[
0,
83
]
] |
2021AandA...650A.205V__Jones_et_al._2021_Instance_2 | The question of the evolution of exoplanet systems after the main sequence of their host is generally addressed by studying exoplanets around subgiants, RGB stars, and normal HB (RC) stars (hereafter the ’classical’ evolved stars). These classical evolved stars are typically very large stars, with radii ranging from ~ ... | [
"Jones et al. 2021"
] | [
"The lack of close-in giant planets may also be explained by the intrinsically different planetary formation for these intermediate-mass stars (see the discussion in"
] | [
"Compare/Contrast"
] | [
[
1690,
1707
]
] | [
[
1525,
1689
]
] |
2022ApJ...939L..19I__Petigura_et_al._2017_Instance_1 | Kepler transit observations have shown that planets with sizes between those of Earth (1 R
⊕) and Neptune (∼4 R
⊕) are extremely common (Lissauer et al. 2011; Batalha et al. 2013; Fressin et al. 2013; Howard 2013; Fabrycky et al. 2014; Marcy et al. 2014). Demographics analysis suggests that at least 30%–55% of the Sun-... | [
"Petigura et al. 2017"
] | [
"Uncertainties in stellar radius estimates from photometric Kepler observations prevented a detailed assessment of the intrinsic planet size distribution"
] | [
"Background"
] | [
[
758,
778
]
] | [
[
584,
736
]
] |
2015AandA...584A.103S__Lattimer_&_Swesty_1991_Instance_2 | The energy in the inner crust is largely influenced by the properties of the neutron gas and, therefore, the EoS of neutron matter of the different calculations plays an essential role. The NV calculation (Negele & Vautherin 1973) is based on a local energy density functional that closely reproduces the Siemens-Pandhar... | [
"Lattimer & Swesty 1991"
] | [
"The calculations of LS",
"are the two EoS tables in more widespread use for astrophysical simulations."
] | [
"Background",
"Background"
] | [
[
1546,
1568
]
] | [
[
1522,
1544
],
[
1639,
1715
]
] |
2019ApJ...885..168O__Thomas_et_al._2004_Instance_2 | Tidal heating of Io has been shown to be responsible for its widespread volcanism. The tidal heating rate of Jupiter’s tidally locked moon,
, driven by forced eccentricities, e, locked by Europa and Ganymede’s Laplace resonance with Io, is the dominant interior heating source. Similarly, the tidal heating of an e... | [
"Thomas et al. 2004"
] | [
"varying within an order of magnitude over decades of observations"
] | [
"Background"
] | [
[
1443,
1461
]
] | [
[
1336,
1401
]
] |
2019ApJ...887...40W__Willott_et_al._2017_Instance_1 | In recent years, the Atacama Large Millimeter/submillimeter Array (ALMA) has carried out comprehensive surveys of the [C II] 158 μm fine structure line in high-z quasars. For example, Decarli et al. (2018) detected [C II] in 85% of 27 optically selected quasars at z > 5.94. This line is an important coolant that traces... | [
"Willott et al. 2017"
] | [
"The [C II]–FIR luminosity ratios of these quasar hosts range from 10−4 to a few ×10−3",
"following the trend of decreasing [C II]–FIR ratio with increasing FIR luminosities found with the IR luminous star-forming systems"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
744,
763
]
] | [
[
617,
702
],
[
787,
918
]
] |
2021AandA...650A.172J__Mangum_&_Shirley_2015_Instance_1 | In the second, complimentary method, the line profiles were fitted using the least-squares method with the SCIPY routine CURVE_FIT. Toward B335, the fit was allowed to include up to four Gaussian line profiles, one for each potential transition in the blended emission feature. Bounds on the fits were estimated from the... | [
"Mangum & Shirley 2015"
] | [
"The column density is estimated from the fitted line profile by assuming local thermodynamic equilibrium (LTE)"
] | [
"Uses"
] | [
[
854,
875
]
] | [
[
742,
852
]
] |
2016ApJ...821..107G__Schwadron_et_al._2011_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... | [
"Schwadron et al. 2011"
] | [
"In Equation (3), ΔE denotes the width of the respective energy bin; for the typical radial velocity of solar wind in the flanks and the downwind hemisphere of the inner heliosheath, we assumed uR = 140 km s−1 as measured by Voyager 2, whereas uR = 40 km s−1 for the heliosheath in the Voyager 1 direction"
] | [
"Uses"
] | [
[
1006,
1027
]
] | [
[
700,
1004
]
] |
2016AandA...588A..44Y__Jones_et_al._2014_Instance_2 | 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"
] | [
"In low-density regions (according to",
"\\hbox{$A_{V} \\leqslant 0.7$}AV⩽ 0.7 for the standard ISRF), UV photons are responsible for causing the photo-dissociation of CH bonds, a-C:H → a-C."
] | [
"Background",
"Background"
] | [
[
1626,
1643
]
] | [
[
1589,
1625
],
[
1645,
1792
]
] |
2021AandA...654A..80S__Leclercq_et_al._2017_Instance_1 | For this comparison we rely on HST broad-band magnitudes, Lyα line fluxes, Lyα EW0 estimates, spectral UV slopes β, continuum magnitudes, and Lyα FWHM from the catalog that will be presented by Kerutt et al. (2021). This LAE study is based on the same data and source identification (see Sect. 3) as the current study, b... | [
"Leclercq et al. 2017"
] | [
"However, Lyα emission is known to be extended beyond the continuum",
"and fluxes based on the TDOSE spectra would therefore be biased."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
969,
989
]
] | [
[
832,
898
],
[
997,
1061
]
] |
2022AandA...661A.129S__Rodríguez-Almeida_et_al._2021_Instance_1 | Radio astronomy is recognized as one of the most effective techniques to search for interstellar molecules. By comparing the spectra of candidate molecules in the laboratory with the spectra observed in astronomical surveys, we can determine whether these molecules exist in interstellar space. Therefore, it is necessar... | [
"Rodríguez-Almeida et al. 2021"
] | [
"Methanethiol (or methyl mercaptan, CH3SH) was detected in the Sagittarius B2 (Sgr B2) region of the center of our Galaxy"
] | [
"Background"
] | [
[
729,
758
]
] | [
[
550,
670
]
] |
2022ApJ...928....3A__Wedemeyer_&_Steiner_2014_Instance_1 | Solar vortex tubes can be spontaneously generated by turbulent convection. In simulations of quiet Sun regions, vortices are found along intergranular lanes (Shelyag et al. 2011a; Kitiashvili et al. 2012; Moll et al. 2012; Silva et al. 2020). These structures have an average lifetime of around 80 s (Silva et al. 2021) ... | [
"Wedemeyer & Steiner 2014"
] | [
"In some cases, twisted magnetic flux tubes appear close enough to flow vortices, leading to magnetic and kinetic vortex structures closely coexisting in regions with high plasma-β"
] | [
"Background"
] | [
[
1018,
1042
]
] | [
[
837,
1016
]
] |
2021AandA...649A..58L__Bemporad_et_al._(2018)_Instance_2 | The leading edges of the transients normally leave bright traces in the images of visible light, inspiring many methods that were developed to derive their locations and velocities, such as the icecream cone model (Fisher & Munro 1984), the graduated cylindrical shell (GCS) model (Thernisien 2011), geometric triangulat... | [
"Bemporad et al. (2018)"
] | [
"In the FS (BS), the 2D velocity map between the current and the previous (next) frame is constructed with almost the same method as"
] | [
"Uses"
] | [
[
1764,
1786
]
] | [
[
1632,
1763
]
] |
2021ApJ...909..172Z__Read_&_Lebonnois_2018_Instance_1 | Atmospheric superrotation is characterized by eastward wind at the equator, which means the atmosphere there has a higher angular momentum than the solid surface. Atmospheric superrotation is a common phenomenon across the universe. In the solar system, superrotation exists in the atmospheres of Venus, Titan, Saturn, a... | [
"Read & Lebonnois 2018"
] | [
"In the solar system, superrotation exists in the atmospheres of Venus, Titan, Saturn, and Jupiter, as well as the stratospheric atmosphere of Earth during the westerly phase of the quasi-biennial oscillation (e.g.,"
] | [
"Background"
] | [
[
510,
531
]
] | [
[
233,
447
]
] |
2019ApJ...885...81S__Dekel_et_al._2009b_Instance_1 | This scenario could also explain the reason why star-forming galaxies with a relatively thin disk appeared around z ∼ 1, because the hot-mode accretion is expected not to dominate even in massive halos at z ≳ 2 owing to gas supply through the cold gas stream (e.g., Dekel et al. 2009a; Kereš et al. 2009). Some of the ga... | [
"Dekel et al. 2009b"
] | [
"Some of the gas accreting onto a dark matter halo is expected to penetrate surrounding hot gas in a form of filaments of dense and cold infalling gas and directly accrete onto the central galaxy at such high redshift, where the mass accretion rate and matter density tend to be high. Such direct gas supply through ... | [
"Compare/Contrast"
] | [
[
831,
849
]
] | [
[
306,
830
]
] |
2022MNRAS.514.2974M__the_2003_Instance_1 | NGC 2992 has been observed at different flux levels (e.g. Fig. 14) and in Marinucci et al. (2018) a detailed analysis of XMM–Newton exposures of this object is presented. In order to provide an holistic view of the spectral properties of the central engine in NGC 2992, we tested our 2019 best-fitting model (model 1 pre... | [
"Nandra et al. 1997"
] | [
"Moreover, to account for the broad emission line found required by the 2003 data, we added a Gaussian component whose width was kept fixed to σ = 400 eV, in accordance with what literature papers (e.g."
] | [
"Uses"
] | [
[
1175,
1193
]
] | [
[
973,
1174
]
] |
2019MNRAS.484.3356G__Häring-Neumayer_et_al._2006_Instance_1 | Optical-NIR Spectral Energy Distribution (SED) modelling of diffuse light (e.g. Carson et al. 2015; Dale et al. 2016) at high spatial resolution can provide a map of the spatial variation and composition of the main stellar population components of the NSC, as well as their host galaxy. Such analysis can also unveil (a... | [
"Häring-Neumayer et al. 2006"
] | [
"To understand NSC formation, it is therefore critical to be able to disentangle such degeneracies. For example, follow-up spectroscopic observations aiming at decomposing the main stellar populations and the dynamical imprint of a MBH rely on a good mass model to predict the stellar population velocity profile (e.... | [
"Motivation"
] | [
[
820,
847
]
] | [
[
502,
819
]
] |
2021MNRAS.508.3111M__Garton,_Gallagher_&_Murray_2018_Instance_1 | The initially used automated methods for detection of solar activity in the solar images are based on the predefined rules inferred from the appearance and usual characteristics of the structures in the solar atmosphere (Henney & Harvey 2005; Krista & Gallagher 2009; Pérez-Suárez et al. 2011). However, it is not possib... | [
"Garton, Gallagher & Murray 2018"
] | [
"Therefore, methods with more advanced mathematical algorithms were introduced.",
"Coronal Hole Identification via Multi-thermal Emission Recognition Algorithm (CHIMERA)",
"have been found to be very effective and are widely used in online solar data visualization tools1$^,$ .2"
] | [
"Background",
"Background",
"Background"
] | [
[
664,
695
]
] | [
[
397,
475
],
[
576,
662
],
[
697,
802
]
] |
2021MNRAS.506.5129B__Momose_et_al._2014_Instance_1 | More recently, Lyman α haloes (LAHs) have been discovered around star-forming galaxies that show Ly α emission far beyond the galaxies’ optical bodies, tracing the circumgalactic rather than interstellar gas (e.g. Hayes et al. 2013). While LAHs are fainter and smaller than LABs in their Ly α extent, they might be a gen... | [
"Momose et al. 2014"
] | [
"Narrow-band imaging can efficiently detect LAHs at targeted redshifts through stacking",
"and narrow-band surveys enable ultradeep, blind samples of LAHs around distant galaxies"
] | [
"Background",
"Background"
] | [
[
630,
648
]
] | [
[
364,
450
],
[
541,
628
]
] |
2021MNRAS.508.3499V__Takahashi,_Witti_&_Janka_1994_Instance_1 | The astrophysical environments of r-process events in the cosmos usually involve explosive physical conditions, because very high neutron densities are required. The neutron-rich isotopes produced along the r-process path have a very short half-life, causing the neutron-rich nuclei to β-decay over time-scales of the or... | [
"Takahashi, Witti & Janka 1994"
] | [
"Examples of r-process sites that have been proposed and investigated by theoretical studies include (i) neutrino-driven winds from proto-neutron stars (NSs;"
] | [
"Background"
] | [
[
553,
582
]
] | [
[
396,
552
]
] |
2018ApJ...861...77M__Pillai_2017_Instance_1 | Previous Herschel studies confirmed numerical calculations (e.g., Nagai et al. 1998) showing that a parallel orientation between filaments and the local magnetic field is to be expected for filaments having low column densities (e.g., Peretto et al. 2012; Busquet et al. 2013; Palmeirim et al. 2013; André et al. 2014; C... | [
"Pillai 2017"
] | [
"In fact, a variety of orientations have previously been observed, and the alignment of filaments and apparent field direction appear to vary between regions and for different gas densities (cf.,",
"for a review)"
] | [
"Background",
"Background"
] | [
[
556,
567
]
] | [
[
361,
555
],
[
569,
582
]
] |
2022ApJ...927...61K__SN_2011f_Instance_1 | Statistical investigations of a large sample of photometric data are useful in exploring the bulk properties of various types of events. Nevertheless, such studies are generally limited to LCs in selected passbands, and also the follow-up covers a short duration of the SN evolution. Further, the spectroscopic follow-up... | [
"Kumar et al. 2013"
] | [
"During the past two decades, several Type IIb SNe with such interesting features have been monitored and studied well, e.g.,",
"SN 2011fu"
] | [
"Background",
"Background"
] | [
[
1381,
1398
]
] | [
[
1157,
1281
],
[
1370,
1379
]
] |
2017MNRAS.465..213B__David_et_al._1993_Instance_1 | As a baseline for understanding how the scaling relations evolve as a function of mass and redshift, we adopt the following self-similar scalings:
(2)
\begin{equation}
M_{\rm {gas},\Delta }\propto M_{\Delta },
\end{equation}
(3)
\begin{equation}
T_{\Delta }\propto M^{2/3}_{\Delta }E^{2/3}(z),
\end{equation}
(4)
... | [
"David et al. 1993"
] | [
"Although shown to be too simplistic by the first X-ray studies of clusters",
"the self-similar relations allow us to investigate if astrophysical processes are less significant in more massive clusters or at higher redshift."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1036,
1053
]
] | [
[
923,
997
],
[
1056,
1202
]
] |
2019MNRAS.487...24G__Rogers_2015_Instance_1 | NASA’s Kepler mission has unveiled a wealth of new planetary systems (e.g. Borucki et al. 2010). These systems offer new insights into the process of planet formation and evolution. One of Kepler’s key findings is that the most common planets in our Galaxy, observed to date, are between 1 and 4 R⊕, i.e. larger than Ear... | [
"Rogers 2015"
] | [
"Further observations revealed a transition in average densities at planet sizes ∼1.5 R⊕",
"with smaller planets having densities consistent with rocky compositions while larger planets having lower densities indicating significant H/He envelopes."
] | [
"Background",
"Background"
] | [
[
510,
521
]
] | [
[
402,
489
],
[
524,
679
]
] |
2022MNRAS.515.5121B__Spiniello_et_al._2018_Instance_1 | There are multiple sources of spurious detections in strong lensing analysis, and some of them are just image artefacts. None the less, others are images that might look like a lens, as in the case of edge-on galaxies and some spiral galaxies. One popular approach to reduce this issue is to use colours and look for red... | [
"Spiniello et al. 2018"
] | [
"The colour information is considered an important feature to find lenses (see e.g.",
"The use of colour queries is considered at least an interesting way to make a pre-selection and improve the final deep learning result purity."
] | [
"Uses",
"Uses"
] | [
[
462,
483
]
] | [
[
356,
438
],
[
486,
628
]
] |
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