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 |
|---|---|---|---|---|---|---|
2017ApJ...845..160P__Lyubarsky_2009_Instance_1 | It is a pressing question as to how the radiation that is observed in relativistic jets in active galactic nuclei (AGNs) is generated (e.g., Blandford & Königl 1979; Marscher 1980; Zensus 1997; Laing & Bridle 2002; Honda 2010; Levinson & Rieger 2011; Mościbrodzka et al. 2011; Ito et al. 2013; Mason et al. 2013; Potter ... | [
"Lyubarsky 2009"
] | [
"In the case of collimated relativistic jets, magnetic fields must play an important role"
] | [
"Motivation"
] | [
[
1305,
1319
]
] | [
[
1115,
1203
]
] |
2019ApJ...875L...7D__Saikia_et_al._2018_Instance_1 | The first transit of HD 21749b was identified by both the MIT Quick Look Pipeline (which searches for planet candidates in the 30 minutes Full Frame Images) and the Science Processing Operations Center (SPOC) pipeline based at the NASA Ames Research Center (Jenkins et al. 2016). No other matching transits were found in... | [
"Boro Saikia et al. 2018"
] | [
"A periodogram of these RVs showed a clear signal at 35.57 days, but the TESS photometry and the RHK index",
"indicate a stellar rotation period of around 35 days, calling for caution."
] | [
"Differences",
"Differences"
] | [
[
731,
754
]
] | [
[
624,
729
],
[
756,
830
]
] |
2019MNRAS.487.4473M__Hosokawa_&_Omukai_2009_Instance_1 | The simulation model Run1-hr of Meyer et al. (2018) begins with the gravitational collapse of $100\, \rm M_{\odot }$ of pre-stellar rotating molecular material on to the stellar embryo. At the end of the free-fall collapse phase, the infalling material ends on a centrifugally-balanced disc, from which the gas is subseq... | [
"Hosokawa & Omukai 2009"
] | [
"The accretion rate then reaches the standard value predicted for MYSOs of $10^{-3}\\, \\rm M_{\\odot }\\, \\rm yr^{-1}$",
"up to the onset of the disc formation happening at ${\\approx } 12\\, \\rm kyr$."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1232,
1254
]
] | [
[
1116,
1230
],
[
1256,
1333
]
] |
2019AandA...621A.124B__Leconte_et_al._2010_Instance_1 | A large proportion of systems where one planet or more is orbiting closer to its host star than Mercury to the Sun have been observed. Tidal interactions play a key role in the orbital configuration of these very compact systems since they are likely to circularize orbits, align spins, and synchronize periods (Zahn 197... | [
"Leconte et al. 2010"
] | [
"Since the planet is synchronized within a timescale of a few thousand years, the stellar tide drives the secular orbital evolution"
] | [
"Background"
] | [
[
809,
828
]
] | [
[
637,
767
]
] |
2018ApJ...866L...1S__Pecharromán_et_al._1999_Instance_4 | It was found that the complex dielectric function from Pecharromán et al. (1999) for the sample obtained by heating bayerite at 1273 K, assuming a spheroid with depolarization parameters of (0.35, 0.003), produced an opacity with 11, 20, 28, and 32 μm features, so this component was included in the models. However, wit... | [
"Pecharromán et al. (1999)"
] | [
"This method required",
"to assume an effective medium theory, such that a pellet is a mixture of one of their samples with a matrix of air."
] | [
"Uses",
"Uses"
] | [
[
1067,
1092
]
] | [
[
1046,
1066
],
[
1093,
1208
]
] |
2022MNRAS.517.5541T__Mooley_et_al._2018a_Instance_1 | GRB 170817A, the short GRB directly associated with the first gravitational wave signal GW170817 from a binary neutron star merger, is a great example presenting afterglow spectra with a beautiful single power-law extending from radio to X-ray (Abbott et al. 2017a, b; Goldstein et al. 2017; Savchenko et al. 2017). A su... | [
"Mooley et al. 2018a"
] | [
"The slow rising afterglow light curves also rejected a uniform top-hat jet"
] | [
"Compare/Contrast"
] | [
[
933,
952
]
] | [
[
857,
931
]
] |
2016MNRAS.456.1901H__Yoo_&_Miralda-Escudé_2004_Instance_1 | The growth of supermassive BHs is also altered when considering non-Gaussianities. After deriving the merger history of the most massive haloes at z = 6.5 in both the Gaussian and non-Gaussian simulations, we study the evolution of BHs in massive haloes down to z = 6.5. To investigate the cumulative effect over cosmic ... | [
"Yoo & Miralda-Escudé 2004"
] | [
"We have not included in our models the effects of ‘kicks’ caused by asymmetric emission of gravitational waves, which have been proposed to be possibly responsible for ejecting BHs from haloes with shallow potential wells, thus halting or reducing the growth of high-redshift BHs hosted in small haloes (e.g.",
"T... | [
"Differences",
"Compare/Contrast"
] | [
[
1016,
1041
]
] | [
[
707,
1015
],
[
1089,
1160
]
] |
2016ApJ...827...93N__Neuhauser_et_al._2007_Instance_1 | The results presented in this work answer a number of questions regarding the character of the GG Tau A system, while raising others and leaving others untouched. First among the questions raised by our results are the questions of whether the detailed morphology of features in the circumbinary torus as seen in our sim... | [
"Neuhauser et al. 2007"
] | [
"Whether or not any theoretical mechanism presently exists to explain the formation of giant planets in binary systems, the fact remains that at least a few binary systems, such as γ Cephei",
"do harbor planets. Therefore, some formation mechanism does in fact exist."
] | [
"Uses",
"Uses"
] | [
[
952,
973
]
] | [
[
762,
950
],
[
1038,
1112
]
] |
2018ApJ...855...48Q__Nagy_et_al._2017_Instance_1 | The Orion Bar is probably the best studied PDR in our Galaxy. It is located between the Orion Molecular Cloud 1 and the H ii region excited by the Trapezium cluster, and is exposed to an FUV field a few 104 times the mean interstellar radiation field. Owing to its proximity (417 pc, Menten et al. 2007) and nearly edge-... | [
"Nagy et al. 2017"
] | [
"Owing to its proximity",
"and nearly edge-on orientation, the Bar provides an ideal laboratory for testing PDR models",
"and a primary target for observational studies of physical and chemical structures of PDRs (e.g.,"
] | [
"Background",
"Background",
"Background"
] | [
[
702,
718
]
] | [
[
252,
274
],
[
304,
395
],
[
475,
572
]
] |
2015AandA...584A.103S__Gögelein_&_Müther_2007_Instance_1 | Before leaving this section, in Fig. 8 we display the spatial dependence of the self-consistent neutron and proton density profiles for the optimal solutions in spherical WS cells with average baryon densities nb = 0.0475 fm-3, 0.065 fm-3, and 0.076 fm-3. It is observed that in denser matter the size of the WS cell dec... | [
"Gögelein & Müther 2007"
] | [
"At high nb the density profile inside the WS cell extends towards the edge of the cell, pointing out that the WS approximation may be close to its limits of validity"
] | [
"Background"
] | [
[
837,
859
]
] | [
[
585,
750
]
] |
2020AandA...641A.155V__Ceverino_et_al._2010_Instance_1 | It has also become evident that the normalization of the MS rapidly increases with redshift: distant galaxies form stars at higher paces than in the local Universe, at fixed stellar mass (e.g., Daddi et al. 2007; Elbaz et al. 2007; Whitaker et al. 2012; Speagle et al. 2014; Schreiber et al. 2015). This trend could be e... | [
"Ceverino et al. 2010"
] | [
"Moreover, higher SFRs could be induced by an increased efficiency of star formation due to the enhanced fragmentation in gas-rich, turbulent, and gravitationally unstable high-redshift disks"
] | [
"Background"
] | [
[
876,
896
]
] | [
[
636,
826
]
] |
2016AandA...596A.113B__Perryman_et_al._1997_Instance_1 | The Pleiades open cluster does not only offer us a beautiful spectacle during the fall, it is one of the best-studied stellar associations and one of the cornerstones to understand stellar properties and evolution. In fact, the literature includes more than one thousand refereed papers dealing with the Pleiades, most o... | [
"Perryman et al. 1997"
] | [
"Regarding its distance, there are currently two different methodologies based on parallaxes from Hipparcos",
"and isochrone fitting, respectively."
] | [
"Background",
"Background"
] | [
[
1049,
1069
]
] | [
[
941,
1047
],
[
1071,
1107
]
] |
2018AandA...614A..48B__Keselman_&_Nusser_2012_Instance_1 | The driving mechanisms and chronology of the buildup of bulges in late-type galaxies (LTGs) is an issue of key relevance to our understanding of galaxy evolution. According to our current knowledge on bulge demographics in the local universe, a large fraction of LTGs host pseudo-bulges (PBs; e.g., Gadotti 2009; Fisher ... | [
"Keselman & Nusser 2012"
] | [
"Traditionally, bulges were thought to invariably form early-on via",
"or mergers",
"with the disk gradually building up around them.",
"Whereas this inside-out galaxy formation scenario appears consistent with important integral characteristics of CBs (e.g., their red colors), it does not offer a plausible e... | [
"Background",
"Background",
"Background",
"Compare/Contrast"
] | [
[
1391,
1413
]
] | [
[
1219,
1285
],
[
1338,
1348
],
[
1475,
1523
],
[
1524,
1752
]
] |
2019AandA...630A..26M__Wozniakiewicz_et_al._(2012)_Instance_2 | The majority of the particles collected by Stardust are olivine and pyroxene silicates with solar isotopic compositions, which suggests an origin in our solar system rather than an interstellar provenance. These polymineralic particles dominate those made of a single mineral even down to sizes smaller than 100 nm, indi... | [
"Wozniakiewicz et al. (2012)"
] | [
"No fits of these sizedistributions are available, but the figures in",
"and Price et al. (2010) indicate that the differential sizes may follow a log-normal distribution."
] | [
"Uses",
"Uses"
] | [
[
1772,
1799
]
] | [
[
1703,
1771
],
[
1800,
1898
]
] |
2021MNRAS.507..524M__Steidel_et_al._2016_Instance_1 | In particular, stellar wind P-Cygni profiles and photospheric absorption lines are detected with high significance (green and yellow dashed lines in Fig. 2). The detection of photospheric lines in J0121+0025 indicates unambiguously that the UV luminosity is dominated by stellar emission, rather than an AGN. We identify... | [
"Steidel et al. 2016"
] | [
"These stellar absorption lines are intrinsically weak in star-forming galaxies, with EW0 typically well bellow 1 Å (e.g."
] | [
"Background"
] | [
[
832,
851
]
] | [
[
690,
810
]
] |
2018ApJ...863..162M__Liu_et_al._2013_Instance_1 | 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 general morphologies and the locations of the high-twist fields are also in agreement with many previous studies"
] | [
"Similarities"
] | [
[
739,
754
]
] | [
[
538,
654
]
] |
2022AandA...663L...4L___2020_Instance_1 | While previous studies mainly focused on the optical-UV properties of a MAD in RLAGNs, for the first time we try to investigate their X-ray properties in this work. The origin of X-ray emission in RLAGNs is still under debate, which may come from a corona, jet, or both. In observations, there is a big difference betwee... | [
"Gupta et al.",
"2020"
] | [
"Second,",
"discovered that the distributions of X-ray photon spectral indices between RLAGNs and their radio-quiet counterpart are very similar"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1305,
1317
],
[
1325,
1329
]
] | [
[
1297,
1304
],
[
1331,
1463
]
] |
2016MNRAS.462.3945A__Ebbets_&_Savage_1982_Instance_1 | A comparison of the He and O abundances in RWT 152 with evolutionary models of stellar yields by Marigo (2001) suggests a progenitor star with an initial mass of ∼1.3 M⊙ and very low metallicity Z = 0.004. The stellar mass is compatible with that expected for sdOs (Heber 2009) and the low metallicity indicates that the... | [
"Ebbets & Savage 1982"
] | [
"The location of the star (Teff ≃ 45 000 K, log g ≃ 4.5;",
"is consistent with a current mass of M∼0.55 M⊙ which implies an initial mass in the main sequence of ∼1 M⊙."
] | [
"Similarities",
"Similarities"
] | [
[
1114,
1134
]
] | [
[
1058,
1113
],
[
1136,
1243
]
] |
2021AandA...653A.111R__Jones_et_al._(2021)_Instance_1 | As done by Le Fèvre et al. (2020), we visually inspect the ancillary data, the intensity maps, the velocity and velocity dispersion fields presented in Sect. 3.1 to search for the presence of multiple components or disturbed morphology near the position of the targets. The channel maps, the spectra and the PVDs are che... | [
"Jones et al. (2021)"
] | [
"By taking into account the results of the initial qualitative classification by Le Fèvre et al. (2020) and of the more recent quantitative analysis of a subsample of the ALPINE targets by",
"we proceed with a more in-depth characterization of the [CII]-detected galaxies aimed at obtaining a robust merger fractio... | [
"Extends",
"Extends"
] | [
[
566,
585
]
] | [
[
378,
565
],
[
587,
720
]
] |
2017AandA...605A..88L__Cordiner_et_al._2015_Instance_1 | Altogether, the approximately thirty molecules recently detected have confirmed the chemical complexity in the nebula, and generated our interest for the present study. Of these species, we will focus our attention on the seventeen species listed by molecular families in Table 1. As can be seen in this table, the WHISP... | [
"Cordiner et al. 2015"
] | [
"Because they are detected in a wide variety of interstellar sources",
"and even in comets",
"it is of prime importance to understand well how these precursor molecules form."
] | [
"Background",
"Motivation",
"Motivation"
] | [
[
932,
952
]
] | [
[
642,
709
],
[
889,
907
],
[
956,
1036
]
] |
2018MNRAS.473.1512A__Granot_&_Sari_2002_Instance_1 | The duration of the manually scheduled follow-up observations were also increased to improve the likelihood of a radio detection. The recent investigation of the entire sample of radio-detected GRBs before 2011 April by Chandra & Frail (2012) demonstrated that the majority of GRBs detected in the radio band at 8.5 GHz ... | [
"Granot & Sari 2002"
] | [
"However, it is worth noting that since GRB relativistic blast waves generate synchrotron radiation as they expand into the circumstellar (wind generated) medium",
"we expect the forward-shock of the afterglow to peak more brightly at 15.7 GHz and at earlier times than the peaks recorded by Chandra & Frail (2012)... | [
"Uses",
"Compare/Contrast",
"Uses"
] | [
[
750,
768
]
] | [
[
588,
748
],
[
771,
921
],
[
922,
1040
]
] |
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 location of the flare ribbons"
] | [
"Similarities",
"Similarities"
] | [
[
1612,
1627
]
] | [
[
1434,
1495
],
[
1558,
1591
]
] |
2021AandA...645A..96P__Marcantonio_et_al._(2018)_Instance_2 | The ESPRESSO DFS concept (Di Marcantonio et al. 2018) was conceived during its preliminary design phases with the goal of maximizing operational efficiency, flexibility, and scientific output while complying with the standard Paranal Observatory operational scheme. The main challenge derives from the requirement to ope... | [
"Di Marcantonio et al. (2018)"
] | [
"The flexibility in ESPRESSO’s operations has been tackled by adopting a new DFS deployment plan described in",
"that is exceptional under various aspects because it has to cope with various telescope and instrument configurations while remaining operationally simple."
] | [
"Background",
"Background"
] | [
[
605,
633
]
] | [
[
496,
604
],
[
634,
789
]
] |
2022MNRAS.513.2349C__Bradač_et_al._2002_Instance_1 | Eigenbrod et al. (2006) first modelled this system with HST imaging and suspected that the second set of bluer arcs in F814W band (see Fig. 1) inside and outside the area delimited by the red arcs in F160W band could be either a second source at a different redshift or a star-forming region in the source galaxy. We exa... | [
"Bradač et al. 2002"
] | [
"Many studies (e.g.",
"have shown that the macro model cannot explain the flux ratios in this lens, which suggested the presence of microlensing or dark matter substructures. Thus, to avoid possible biases caused by flux ratios, we only use the lensed quasar positions and the extended arc to constrain the mass mo... | [
"Uses",
"Uses"
] | [
[
1173,
1191
]
] | [
[
1132,
1150
],
[
1300,
1873
]
] |
2021ApJ...913..115A__Linden_et_al._2012_Instance_1 | The origin of the GC VHE emission remains undetermined, due in part to source confusion and the limitations of current instruments. The source of VER J1745–290 may be Sgr A* (Atoyan & Dermer 2004; Aharonian & Neronov 2005; Ballantyne et al. 2011; Chernyakova et al. 2011; Fatuzzo & Melia 2012; Kusunose & Takahara 2012; ... | [
"Linden et al. 2012"
] | [
"The mechanism of gamma-ray emission may be predominantly due to hadronic processes, where relativistic protons interact with gas and subsequently produce gamma rays through neutral pion decay"
] | [
"Background"
] | [
[
1119,
1137
]
] | [
[
829,
1020
]
] |
2015MNRAS.451.2174T__Yoshida_et_al._2006_Instance_1 | In the last two decades, it has been demonstrated that massive galaxies harbour supermassive black holes (SMBHs) in the centres of their bulge components (Kormendy & Ho 2013, and references therein). Also, at redshifts higher than 6, quasars are found that possess SMBHs with the mass higher than 109 M⊙ (Fan et al. 2001... | [
"Yoshida et al. 2006"
] | [
"The initial mass function of first stars is thought to be more or less top-heavy"
] | [
"Background"
] | [
[
1008,
1027
]
] | [
[
846,
926
]
] |
2018ApJ...864..158L__Zank_&_Matthaeus_1992_Instance_1 | So far, the discussion has emphasized particle energization by local plasma regions of contracting and fast reconnecting (merging) small-scale flux ropes generated in the vicinity of large-scale primary current sheets through turbulent current sheet reconnection. However, one can also approach this topic from the persp... | [
"Zank & Matthaeus 1992"
] | [
"Theoretical considerations and simulations of MHD turbulence in the presence of a significant background/guide magnetic field suggest that solar wind turbulence can to lowest order be modeled in terms of a combination of a dominant quasi-2D turbulence component of coherent structures (small-scale magnetic islands)... | [
"Background",
"Similarities",
"Similarities"
] | [
[
852,
873
]
] | [
[
403,
828
],
[
921,
987
],
[
1032,
1143
]
] |
2019ApJ...874..166C__Dyks_et_al._2004_Instance_1 | The realistic structures of the pulsar magnetosphere still remain uncertain. Knowledge about the pulsar magnetosphere structures can be used to identify the potential sites of particle acceleration and gamma-ray emission. A vacuum dipole field is generally adopted in the early study of pulsar emission, because it has a... | [
"Dyks et al. 2004"
] | [
"Due to different emission zone locations, standard pulsar radiation models include the",
"the slot-gap (SG) (e.g.,",
"models."
] | [
"Background",
"Background",
"Background"
] | [
[
1003,
1019
]
] | [
[
796,
882
],
[
959,
983
],
[
1146,
1153
]
] |
2018AandA...620A.122S__Švanda_et_al._(2014)_Instance_1 | Simon & Leighton (1964) described supergranulation as a system of atmospheric currents in the photosphere. The currents form a cellular network, which is visible in Doppler maps after the reduction of other larger scale flows (e.g. differential rotation and convective blueshift). Inside the cells, the flow is radially ... | [
"Švanda et al. (2014)"
] | [
"By averaging over 222 976 supergranular cells and applying time-distant helioseismic inversions,",
"found a symmetrical flow in supergranules, which is directed radially away from the centre of the cells to its periphery, with horizontal velocities in the range of 0.3–0.6 km s−1. Their velocity profile is found ... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1107,
1127
]
] | [
[
1010,
1106
],
[
1128,
1492
]
] |
2020AandA...639A..46B__Štverák_et_al._(2009)_Instance_4 | The linear relationship that we observe between breakpoint energy and core temperature is in line with previous measurements (e.g. McComas et al. 1992; Štverák et al. 2009), for both the halo and strahl. According to Scudder & Olbert (1979), a linear trend in the halo relation also follows under the assumption that bin... | [
"Štverák et al. (2009)"
] | [
"Scudder & Olbert (1979) also predict that the halo Ebp/kBTc ratio remains constant with heliocentric distance, whereas",
"find that the halo Ebp/kBTc ratio decreases with heliocentric distance."
] | [
"Differences",
"Differences"
] | [
[
1376,
1397
]
] | [
[
1257,
1375
],
[
1398,
1469
]
] |
2021ApJ...916...64T__Lundstedt_et_al._2002_Instance_1 | The above results, when considered as relating to different aspects of the same physical process, suggest the probable existence of correlations between periods of significant Alfvénic turbulence, higher time-integrated AE and HILDCAA periods, and longer storm recovery phases. However, a statistical demonstration of th... | [
"Lundstedt et al. 2002"
] | [
"This is crucial since, although space weather forecasting often focuses on estimating the onset and intensity of geomagnetic storms"
] | [
"Background"
] | [
[
1650,
1671
]
] | [
[
1503,
1634
]
] |
2021AandA...655A..99D__Bensby_&_Feltzing_2006_Instance_1 | In Fig. 6, we plot the [C/O] ratios dependence on [O/H] for the different stellar populations. This figure serves to evaluate the balance between the two different elements directly with the evolution of one of them, which in this case has a well-known, single production site. Here, we chose to only show the ratios wit... | [
"Bensby & Feltzing 2006"
] | [
"Previous works in the literature have shown an increase of [C/O] ratios as [O/H] increases (e.g.",
"but our ratios present a quite large dispersion that together with the shorter range in [O/H] prevents us from seeing a clear behaviour."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
676,
698
]
] | [
[
579,
675
],
[
741,
877
]
] |
2016MNRAS.461.1719C__Fu_et_al._2012_Instance_2 | HATLAS12-00 had already been identified as a candidate gravitationally lensed galaxy as a result of its high submm flux (i.e. F500 > 100 mJy), red Herschel colours and the lack of a bright optical or radio counterpart (see e.g. Negrello et al. 2010 for a discussion of the selection of lens candidates in H-ATLAS and oth... | [
"Fu et al. (2012)"
] | [
"Additional followup observations in the optical, near-IR, submm and other wavelengths were targeted at the lensed z = 3.26 source and the foreground objects responsible for the lensing, resulting in detailed analyses of this lensing system by",
"and Bussmann et al. (2013)."
] | [
"Background",
"Background"
] | [
[
985,
1001
]
] | [
[
742,
984
],
[
1002,
1029
]
] |
2022MNRAS.517.1313M__Meidt_et_al._2018_Instance_1 | Star formation is an inefficient process, as evidenced by observed gas depletion times,1 which are two orders of magnitude above the dynamical time, both in galaxies (e.g. Leroy et al. 2017; Utomo et al. 2018), and in individual giant molecular clouds (GMCs) (e.g. Krumholz & Tan 2007; Evans, Heiderman & Vutisalchavakul... | [
"Meidt et al. 2018"
] | [
"Theoretical models explain this inefficiency through a combination of mechanisms that provide support against gravitational collapse, including turbulence, magnetic fields, stellar feedback, and dynamical stabilization"
] | [
"Background"
] | [
[
782,
799
]
] | [
[
384,
602
]
] |
2015ApJ...799..149J___2014_Instance_1 | With our joint analysis of stellar mass fraction and source size, we find a larger stellar mass fraction than earlier statistical studies. In Figure 2, we compare our determination of the stellar surface density fraction to a simple theoretical model and to the best fit of a sample of lens galaxies by Oguri et al. (2... | [
"Oguri et al. (2014)"
] | [
"In Figure 2, we compare our determination of the stellar surface density fraction to a simple theoretical model and to the best fit of a sample of lens galaxies by"
] | [
"Uses"
] | [
[
304,
324
]
] | [
[
139,
303
]
] |
2020MNRAS.499.2575E__Madau,_Shen_&_Governato_2014_Instance_1 | We note in passing that recent studies address improved satellite modellimg that ameliorates many of these issues, including the core–cusp issue via non-sphericity of the stellar velocity distribution (Hayashi, Chiba & Ishiyama 2020) and the detectability of MWG satellites (Nadler et al. 2020). Other proposed solutions... | [
"Madau, Shen & Governato 2014"
] | [
"Other proposed solutions include those",
"or through dynamical feedback driven by starbursts or active galactic nuclei (AGNs;"
] | [
"Background",
"Background"
] | [
[
1050,
1078
]
] | [
[
296,
334
],
[
720,
803
]
] |
2019ApJ...887..185S__Pushkarev_et_al._2010_Instance_1 | The radio versus optical DCF peaks at non-zero lags (τdelay) with the optical emissions leading the radio emissions, implying that the radio and optical emission regions are not cospatial with the optical/IR emission region being closer to the base of the jet. This is consistent with the observation that optical emissi... | [
"Pushkarev et al. 2010"
] | [
"The linear separation of the V and 37 GHz emission region can be estimated using the relation"
] | [
"Uses"
] | [
[
997,
1018
]
] | [
[
902,
995
]
] |
2015MNRAS.448..666S__Steidel_et_al._2014_Instance_1 | In local galaxies, the ISM conditions are often described by some physical quantities such as ionization parameter (q), gaseous metallicity (Z) and electron density (ne). At high redshift, the ionization parameter is raised by a large flux of ionizing photons in ISM originated from hot O, B stars due to intensive star ... | [
"Steidel et al. 2014"
] | [
"Secondly, the chemical abundance of SF galaxies at z ∼ 2 is lower by 0.1–0.3 dex for a given stellar mass compared to those at low-z"
] | [
"Background"
] | [
[
730,
749
]
] | [
[
557,
689
]
] |
2022MNRAS.512.3243S__Mason_&_Gronke_2020_Instance_1 | A more equitable view of the catalogue is given by considering the distributions of band values across all haloes. In Fig. 14, we quantify the relative probability for a given integrated ($\mathcal {T}_\rm{IGM}^\rm{\,int}$, bottom panels) and maximum ($\mathcal {T}_\rm{IGM}^\rm{\,max}$, top panels) band transmission at... | [
"Mason & Gronke 2020"
] | [
"When also considering the central band in rare cases it is plausible to witness multiple-peaked or otherwise complex spectral line profiles (e.g. see the discussions by",
"This also stresses the need for systemic tracers beyond Lyα to distinguish IGM signatures and pinpoint the origins of various spectral featu... | [
"Background",
"Motivation"
] | [
[
841,
860
]
] | [
[
650,
818
],
[
901,
1046
]
] |
2015AandA...584A.103S__Potekhin_et_al._2013_Instance_1 | 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"
] | [
"More recently, unified EoSs for NS have been derived by the Brussels-Montreal group"
] | [
"Background"
] | [
[
580,
600
]
] | [
[
433,
516
]
] |
2016AandA...594A..64P__Judge_(2015)_Instance_2 | 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)"
] | [
"has also mentioned the well known problem of the “anomalous ions”, that is, the observed high intensities of the Li- and Na-like (as Si iv) ions"
] | [
"Background"
] | [
[
1621,
1633
]
] | [
[
1634,
1778
]
] |
2018MNRAS.478.2576M__Marleau_et_al._2017_Instance_1 | The search for low-mass BHs (MBH ≲ 106 M⊙) in dwarf galaxies is mostly based on the detection of X-ray emission (e.g. Greene & Ho 2007a; Desroches, Greene & Ho 2009; Reines et al. 2011; Dong et al. 2012; Schramm et al. 2013; Baldassare et al. 2015, 2017; Lemons et al. 2015; Secrest et al. 2015; Pardo et al. 2016; Chen ... | [
"Marleau et al. 2017"
] | [
"Additional searches in the infrared (IR) regime have yielded a few more candidates (e.g."
] | [
"Background"
] | [
[
890,
909
]
] | [
[
740,
828
]
] |
2021ApJ...923..126S__Samsing_&_Ilan_2018_Instance_1 | The question is, which of these proposed merger channels dominate the merger rate? Are several channels operating with a possible dependence on redshift? Or are the majority of GW sources formed through a still unknown mechanism? Several studies show that one can distinguish at least classes of channels, such as isolat... | [
"Samsing & Ilan 2018"
] | [
"Several studies show that one can distinguish at least classes of channels, such as isolated binaries and dynamically induced mergers,",
"as well as the orbital eccentricity at some reference GW frequency"
] | [
"Background",
"Background"
] | [
[
665,
684
]
] | [
[
230,
364
],
[
525,
591
]
] |
2021ApJ...916...68B__Chakrabarti_1989_Instance_1 | In this paper, we presented our analysis of the spectral and timing behavior of GRS 1915+105 using the TCAF paradigm. For this purpose, the θ class data of the source as obtained by the LAXPC instrument of AstroSat satellite were used. To the best of our knowledge, this is the first time that the θ class data of AstroS... | [
"Chakrabarti 1989"
] | [
"In the sub-Keplerian flow, shocks are formed when the Rankine–Hugoniot conditions are satisfied"
] | [
"Background"
] | [
[
763,
779
]
] | [
[
666,
761
]
] |
2015ApJ...806..152S__Ransom_et_al._2005_Instance_3 | 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"
] | [
"This is the most intense emission detected so far from a Galactic GC, again suggesting the presence of a large number of MSPs. However, no direct radio detection of these objects has been obtained so far in this system"
] | [
"Motivation"
] | [
[
1645,
1663
]
] | [
[
1425,
1643
]
] |
2021AandA...647A..49S__Murphy_et_al._2015_Instance_1 | The λ Boötis stars are a group of chemically peculiar objects on the upper main-sequence, showing underabundances (~1–2 dex) of iron-peak elements and near-solar abundances of C, N, O, and S (e.g., Kamp et al. 2001; Heiter 2002; Andrievsky et al. 2002). The class was discovered by Morgan et al. (1943) and named followi... | [
"Murphy et al. 2015"
] | [
"Unlike common chemical peculiarities seen in Am and Ap stars, λ Boötis stars are not constrained to slow rotation"
] | [
"Compare/Contrast"
] | [
[
948,
966
]
] | [
[
813,
926
]
] |
2018ApJ...864..154D__Liu_et_al._2016_Instance_1 | Feedback from massive stars plays a critical role in the star formation process and evolution of molecular clouds. In particular, expanding H ii regions may have a positive effect on star formation, i.e., they can trigger a new generation of star formation in molecular clouds either by sweeping ambient clouds into dens... | [
"Liu et al. 2016"
] | [
"Since the PG108.3 cloud consists of three evolved H ii regions, one can thus speculate that the formation of young sources in the region might have been triggered by the expanding bubble. However, our observations largely do not favor such a process because in such a scenario one would expect the distribution of y... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
958,
973
]
] | [
[
503,
898
],
[
995,
1181
]
] |
2021MNRAS.503.2108P__Andresen_et_al._2017_Instance_2 | CCSNe are also of interest for GW astronomy as targets in their own right. As the sensitivity of GW detectors increases, they will begin to detect not only binary mergers but also other lower amplitude sources of GWs such as CCSNe. Accurate knowledge of the GW emission from CCSNe will be essential for detection and par... | [
"Andresen et al. 2017"
] | [
"In addition, some models",
"exhibit low-frequency GW emission due to the standing accretion shock instability (SASI"
] | [
"Background",
"Background"
] | [
[
1369,
1389
]
] | [
[
1317,
1341
],
[
1437,
1524
]
] |
2015MNRAS.452.1112E__Illarionov_&_Sunyaev_1975_Instance_1 | The X-ray luminosity of CG X-1 is variable by a factor of ≈10 (Bianchi et al. 2002; Weisskopf et al. 2004). The highest flux reported in the literature (5.2 × 10−12 erg cm−2 s−1 for a power-law fit or 5 × 10−12 erg cm−2 s−1 for an MCD fit, in the 0.5–8 keV band; Weisskopf et al. 2004) would imply, for a distance of 4.2... | [
"Illarionov & Sunyaev 1975"
] | [
"This condition corresponds for CG X-1 to the requirement MBH ≳ 1.5 vw, 10004δ2 M⊙, where MBH is the BH mass, vw, 1000 is the wind velocity in units of 1000 km s−1, and δ ≈ 1 is a dimensionless parameter",
"see also"
] | [
"Uses",
"Uses"
] | [
[
888,
913
]
] | [
[
640,
842
],
[
879,
887
]
] |
2022ApJ...928....3A__Rappazzo_et_al._2019_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) ... | [
"Rappazzo et al. 2019"
] | [
"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"
] | [
[
1044,
1064
]
] | [
[
837,
1016
]
] |
2021MNRAS.503.5367B__Lu,_Kumar_&_Zhang_2020_Instance_2 | Since the discovery of the radio burst, there have been extensive follow-up observations of SGR J1935+2154 across the electromagnetic spectrum. The lack of another radio pulse coincident with an X-ray flare puts interesting constraints on the emission mechanism and begs the question of whether we should be able to see ... | [
"Lu, Kumar & Zhang 2020"
] | [
"Hence, if we assume that FRBs produced by magnetars are created in the magnetosphere close to the polar cap, we can expect them to be significantly beamed"
] | [
"Compare/Contrast"
] | [
[
1320,
1342
]
] | [
[
1164,
1318
]
] |
2019MNRAS.485.5652D__Yamanaka_et_al._2009_Instance_1 | Einstein’s theory has been tested successfully mainly in the regime of weak gravity through Solar system tests and laboratory experiments. But the validity of this highly accepted theory still faces stringent constraint in the regime of strong gravity, viz., the region near to a black hole, ultradense compact stars, an... | [
"Yamanaka et al. 2009"
] | [
"The recent discovery of peculiar highly overluminous SNeIa,",
"indicates a huge Ni-mass and confirms the highly super-Chandrasekhar white dwarfs, having mass 2.1–2.8 M⊙, as a suitable progenitors"
] | [
"Background",
"Background"
] | [
[
667,
687
]
] | [
[
342,
401
],
[
494,
626
]
] |
2017ApJ...850...81P__Muñoz-Jaramillo_et_al._2012_Instance_1 | Solar cycle predictions are needed to plan long-term space missions and are of high importance for space weather applications. Currently, precursor methods are the most favored models for the prediction of solar cycle strength (Conway 1998; Svalgaard et al. 2005; Kane 2008; Hathaway 2009). These precursor techniques of... | [
"Muñoz-Jaramillo et al. 2012"
] | [
"Predicting the amplitude of a solar cycle can be done using solar polar magnetic fields from the previous cycle as “precursors” of the next cycle"
] | [
"Background"
] | [
[
725,
752
]
] | [
[
496,
641
]
] |
2020AandA...641A.123H__Mikal-Evans_et_al._(2019)_Instance_4 | To confirm the importance of VO, water and an inversion layer (Evans et al. 2018; Mikal-Evans et al. 2019, 2020) obtained repeated HST observations of the transmission spectrum and the secondary eclipse using the STIS and WFC 3 instruments. The optical transmission spectrum displays rich variation, with multiple featur... | [
"Mikal-Evans et al. (2019)"
] | [
"Although the chemical retrievals follow different strategies (equilibriumversus free-chemistry), both indicate that a depletion of TiO relative to VO is needed to explain the observed emission spectrum, supporting the earlier findings by"
] | [
"Similarities"
] | [
[
2047,
2072
]
] | [
[
1809,
2046
]
] |
2021MNRAS.504.4626K__Kraljic_et_al._2020b_Instance_3 | Galaxies seem to retain a memory of their spin orientation with respect to the cosmic web filaments and walls, as suggested by the results from large-scale cosmological hydrodynamical simulations (Dubois et al. 2014; Codis et al. 2018; Wang et al. 2018; Ganeshaiah Veena et al. 2019; Kraljic, Davé & Pichon 2020b). The m... | [
"Kraljic et al. 2020b"
] | [
"Further support for this interpretation was provided by the findings of stronger impact of large-scale tides on the galaxy spin orientation in denser filaments",
"using filament density as a proxy for the thickness of filaments"
] | [
"Similarities",
"Background"
] | [
[
1504,
1524
]
] | [
[
1343,
1502
],
[
1526,
1590
]
] |
2017ApJ...835..151A__Gaisser_et_al._2014_Instance_1 | In the southern sky, the large background of atmospheric muons reduces the efficiency to select through-going tracks induced by neutrinos below the PeV regime. A very large fraction of the aforementioned background can be rejected by imposing an active veto at the detector boundary, as, for example, used in Aartsen et ... | [
"Gaisser et al. 2014"
] | [
"Furthermore, the more clearly an event is identified as a starting track, the more probable it is to be an astrophysical rather than atmospheric background. Down-going atmospheric neutrino events at high energy are likely to be accompanied by muons produced in the same cosmic-ray shower that triggers the veto and ... | [
"Background"
] | [
[
839,
858
]
] | [
[
457,
815
]
] |
2020ApJ...899L...6L__Margalit_et_al._2019_Instance_2 | 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"
] | [
"However, if this fraction is very low, as required if GW170817 leaves behind a black hole",
"the fast magnetar model may fail to explain the small fraction of LGRB/SLSN-like hosts in FRB samples."
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1236,
1256
]
] | [
[
1145,
1234
],
[
1259,
1361
]
] |
2018ApJ...863..162M__Liu_et_al._2013_Instance_1 | 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 general morphologies and the locations of the high-twist fields are also in agreement with many previous studies"
] | [
"Similarities"
] | [
[
739,
754
]
] | [
[
538,
654
]
] |
2021MNRAS.502..772L__Cowley_et_al._2015_Instance_1 | A number of semi-analytic models (SAMs) have attempted to reproduce submm number counts (e.g. Granato et al. 2000; Fontanot et al. 2007; Somerville et al. 2012). One such model is the galform (SAM), which has been tuned to successfully reproduce the number counts of 850 μm and $\mathrm{1.1 \, mm}$ selected galaxies.1 H... | [
"Cowley et al. 2015"
] | [
"Later versions of the model used a more moderately top-heavy IMF in starbursts, triggered by disc instabilities rather than mergers, and found similarly good agreement with the number counts"
] | [
"Background"
] | [
[
859,
877
]
] | [
[
667,
857
]
] |
2016AandA...588A..74C__Böhm-Vitense_1958_Instance_1 | The pulsational analysis presented in this work makes use of full stellar evolution models of pre-WDs generated with the LPCODE stellar evolution code. LPCODE computes in detail the complete evolutionary stages leading to WD formation, allowing the WD and pre-WD evolution to be studied in a consistent way based on the ... | [
"Böhm-Vitense 1958"
] | [
"In particular, we have also used the ML1 (α = 1,a = 1 / 8,b = 1 / 2,c = 24,"
] | [
"Uses"
] | [
[
1271,
1288
]
] | [
[
1195,
1270
]
] |
2015AandA...574A..70F__Padova_1994_Instance_1 | We used the stellar population synthesis code STARLIGHT (Cid Fernandes et al. 2004) to describe the age distributions and metallicities of the stellar populations that fit the integrated light spectrum of object I. For object H it is not possible to perform the stellar population synthesis because of the low signal-to-... | [
"Padova 1994"
] | [
"We used the",
"tracks, as recommended by Bruzual & Charlot (2003)"
] | [
"Uses",
"Uses"
] | [
[
1144,
1155
]
] | [
[
1132,
1143
],
[
1156,
1206
]
] |
2022AandA...667A.131B__Izumi_et_al._(2016)_Instance_3 | Molecular line ratio diagnostics are often used to investigate the physics and chemistry of the ISM in all of these environments. For example, as the gas chemistry located in the central, nuclear regions of galaxies is believed to be dominated by X-rays produced by the AGN, in so-called X-ray dominated regions (XDRs), ... | [
"Izumi et al. (2016)"
] | [
"propose a scenario where it is the high temperature that is responsible for the HCN enhancement, whereby neutral-neutral reactions with high reaction barriers are enhanced",
"thus leading to the possible enhancement of HCN and the depletion of HCO+ via newly available formation and destruction paths, respectivel... | [
"Background",
"Background",
"Motivation",
"Motivation",
"Motivation"
] | [
[
1429,
1448
]
] | [
[
1449,
1620
],
[
1643,
1783
],
[
1784,
2197
],
[
2223,
2658
],
[
2684,
2844
]
] |
2017ApJ...849...63R__Pascucci_et_al._2016_Instance_1 | The (sub)mm wavelength range is of particular interest for various reasons: at sufficiently long wavelengths, disks become optically thin, and an estimate of their dust mass can be directly obtained (via some assumptions) by simply measuring their flux (e.g., Beckwith et al. 1990). Although the bulk of the disk mass in... | [
"Pascucci et al. 2016"
] | [
"Using this method, surveys of star-forming regions with (sub)mm facilities such as SMA and ALMA have determined that protoplanetary disks have typical masses of 0.1%–0.5% of that of their host star (e.g.,"
] | [
"Background"
] | [
[
844,
864
]
] | [
[
593,
797
]
] |
2015MNRAS.454.1644L__Kotze_&_Charles_2012_Instance_1 | The period candidates of other three ULXs may range from ∼100 to ∼600 d. Apart from noise and artefacts, all the candidate periods are only significant in a specific epoch. This suggests that they are not associated with any stable mechanism such as orbital motion. Instead, such long-term (> 100 d) X-ray quasi-periodic... | [
"Kotze & Charles 2012"
] | [
"Alternatively, mass transfer rate-related events such as X-ray state changes and disc instability can also cause long-term modulations"
] | [
"Compare/Contrast"
] | [
[
679,
699
]
] | [
[
543,
677
]
] |
2021AandA...653A..99T__Pallé_et_al._2004_Instance_1 | To minimize the undesired effects caused by observing different lunar locations, we conducted observations according to the following procedure. On each observing night, we first pointed the Nayuta telescope toward the crater Grimaldi (selenographic coordinate: 68.6°W, 5.2°S) in the waxing phase and the crater Neper (8... | [
"Pallé et al. 2004"
] | [
"Our target locations are not on a major maria and near sites repeatedly observed in previous Earthshine photometry because they were expected to have roughly comparable albedos"
] | [
"Motivation"
] | [
[
886,
903
]
] | [
[
691,
867
]
] |
2022ApJ...940...86K__Cohen_et_al._1997_Instance_1 | Currently, about 20 Be stars are known to have stripped companions, most of which were confirmed with far-UV (FUV) spectroscopy, as it is in the FUV where the flux ratios are most favorable (Wang et al. 2021; Klement et al. 2022, and references therein). All of the spectroscopic FUV detections were found to be compatib... | [
"Cohen et al. 1997"
] | [
"The WD companions to Be stars proved unexpectedly elusive"
] | [
"Background"
] | [
[
1149,
1166
]
] | [
[
1071,
1128
]
] |
2022MNRAS.517.3881L__GRB_2004_Instance_1 | During a GF, a huge amount of the magnetic energy E > 1046 erg is subsequently released at the surface of the magnetar within the first 1 s, leading to the formation of a hot fireball similar to the case of classic GRBs (Mészáros & Rees 2000), which might be rich in electron–positron pairs (Thompson & Duncan 1995; Ferm... | [
"Chand et al. (2021)"
] | [
"suggest that a baryon-poor outflow can explain the high-energy afterglow emission of GRB 200415A, while a baryon-rich outflow is also viable if the dissipation happens below the photosphere via internal shocks. Therefore, in this paper, we calculate two situations that the ejecta is dominated by electron–positron ... | [
"Motivation"
] | [
[
899,
918
]
] | [
[
919,
1265
]
] |
2016AandA...587A..30M__Mihalas_&_Binney_1981_Instance_1 | For a star that moves with respect to its surrounding medium, the stellar motion adds an asymmetry to the wind velocity profile, since different parts of the wind face the ISM with different relative velocities. If the motion is supersonic, a bow shock arises at the interface where the ram pressure of the ISM and the s... | [
"Mihalas & Binney 1981"
] | [
"The density can be expressed in number density of hydrogen atoms (mH = 1.6727 × 10-27 kg), which follows roughly (2)\\begin{equation} \\label{density} n_{\\rm H} = 2.0 \\; {\\rm e}^{-\\frac{|z|}{100\\,{\\rm pc}}}, \\end{equation}nH=2.0e−|z|100 pc,where z is the galactic height",
"and nH is given in atoms per cm3... | [
"Uses",
"Uses"
] | [
[
1002,
1023
]
] | [
[
732,
1000
],
[
1025,
1058
]
] |
2021MNRAS.508.1020D__Schuhmann_et_al._2019_Instance_1 | A few possibilities are explored for XCl: (1) The most straightforward explanation is that the Cl radical itself is present in the coma. Although it seems unlikely due to its reactivity, the CN radical was discovered in the coma of 67P (Hänni et al. 2020); therefore, the Cl radical cannot be excluded as a possible cand... | [
"Schuhmann et al. 2019"
] | [
"However, as all results show that EII product ion fractions decrease as the complexity of the molecules increases"
] | [
"Motivation"
] | [
[
677,
698
]
] | [
[
562,
675
]
] |
2016ApJ...832....1R__Plekan_et_al._2011_Instance_1 | When dipolar species, such as CO, are allowed to deposit in the laboratory on a cold surface under vacuum to form a layer of approximately 4–5 monolayers (ML), the molecules may spontaneously orient throughout the layer such that their positive or negative ends protrude from the surface, creating a polarization potenti... | [
"Plekan et al. 2011"
] | [
"The analysis, described in detail in Field et al. (2013), is remarkably successful in describing important characteristics of spontelectrics, such as the deposition temperature dependence of the surface polarization charge, including the counterintuitive behavior of solid methyl formate"
] | [
"Compare/Contrast"
] | [
[
993,
1011
]
] | [
[
704,
991
]
] |
2021ApJ...912...20J__Murray_et_al._1995_Instance_1 | Dramatic changes in the optical broad emission lines (BELs) of CLQs can also probe the physical origin of the lines themselves. Optical spectra of AGN are characterized primarily by a power-law continuum, BELs, and narrow emission lines (e.g., Vanden Berk et al. 2001). BELs are emitted from the broad-line region (BLR),... | [
"Murray et al. 1995"
] | [
"The disk-wind model suggests that the BLR gas comes from winds produced by the accretion disk"
] | [
"Background"
] | [
[
1041,
1059
]
] | [
[
924,
1017
]
] |
2019AandA...623A.145M__Lofthouse_et_al._2017_Instance_1 | Low redshift (z ≲ 3) LyC emitters have proven difficult to find (e.g., Leitherer et al. 1995; Bergvall et al. 2006; Siana et al. 2007, 2015; Vanzella et al. 2010; Leitet et al. 2011, 2013) due to the attenuation of LyC photons by the intergalactic medium (IGM). For decades, the only confirmed, directly detected LyC esc... | [
"Lofthouse et al. 2017"
] | [
"Pioneering work with integral field unit (IFU) observations of four GPs",
"reveals that two are rotationally supported, with seemingly undisturbed morphology, and two are dispersion-dominated, leading the authors to conclude that mergers may not be a necessary driver of their star formation properties, and by ex... | [
"Background",
"Background"
] | [
[
1487,
1508
]
] | [
[
1414,
1485
],
[
1510,
1780
]
] |
2015AandA...584A...4D__Schneider_et_al._2015_Instance_1 | The density structure and infall kinematics discussed here are probably dominated by the most massive object clearly identified in Fig. 2b. The envelope profile defined above (see Sect. 3.5) and their corresponding values given in Table 3 have been used in Eq. (A.2) to estimate a mass of ~3500 M⊙ in a 2.5 pc radius for... | [
"Schneider et al. 2015"
] | [
"This region exhibits a steeper density gradient in its outer envelope, with qout ≃ −2.5, also illustrated by the cloud structure studied with probability density function"
] | [
"Similarities"
] | [
[
520,
541
]
] | [
[
348,
518
]
] |
2017MNRAS.472.1052B__Bruno_&_Telloni_2015_Instance_1 | Typical corotating high-speed streams (HSS), i.e. those streams coming from the equatorial extension of polar coronal holes, are characterized by different regions. Within these regions, extending on daily scales, field and plasma parameters assume different average values and fluctuations have a different character. T... | [
"Bruno & Telloni 2015"
] | [
"Interesting enough, these two portions of the stream are separated by a very narrow region across which Alfvénicity changes abruptly, from high to low"
] | [
"Background"
] | [
[
1126,
1146
]
] | [
[
974,
1124
]
] |
2018ApJ...869...69M__Künzel_1960_Instance_1 | The AR NOAA 12673 was highly flare productive.5
5
https://www.swpc.noaa.gov/products/solar-region-summary
It appeared in the eastern limb of the Sun on August 28 as a simple α-type AR and gradually evolved into complex βγ-type on September 4. It became an even more complex βγδ-type on September 5 and remained so un... | [
"Künzel 1960"
] | [
"During the occurrence of X-class flares, the complex AR had shown δ-sunspots, which are identified with a complex distribution of sunspot groups in which the umbrae of positive and negative polarities share a common penumbra"
] | [
"Background"
] | [
[
933,
944
]
] | [
[
707,
931
]
] |
2020MNRAS.493..559B__Kulow_et_al._2014_Instance_1 | Nearly half of the known exoplanets orbit within 0.1 au from their star. At such close distances, the nature and evolution of these planets is shaped by interactions with their host star (irradiation, tidal effects, and magnetic fields). In particular, the deposition of stellar X-ray and extreme ultraviolet radiation (... | [
"Kulow et al. 2014"
] | [
"This scenario is strengthened by the recent observations of warm Neptunes at the border of the desert, on the verge of",
"considerable mass-loss."
] | [
"Similarities",
"Similarities"
] | [
[
1589,
1606
]
] | [
[
1469,
1587
],
[
1762,
1785
]
] |
2017AandA...607A.107W__Michałowski_et_al._2015_Instance_1 | A likely scenario for the geometry of the entire system is presented in Fig. 15. The locations of systems A–C are fairly well constrained by their metal absorption. System D is harder to place, as there is little to be learned from its negligibly low metal content. It is highly improbable that it is an outflow similar ... | [
"Michałowski et al. 2015"
] | [
"Instead we believe it to trace the metal-poor gas that acts as a replenishment mechanism of galaxies throughout the universe. It has indeed been suggested that GRB hosts in general are fuelled by recent metal-poor gas inflow"
] | [
"Compare/Contrast"
] | [
[
638,
661
]
] | [
[
412,
636
]
] |
2021MNRAS.506.3511M__Foucart_et_al._2012_Instance_1 | In this work, we study the merger and post-merger evolution of near equal-mass BH–NS binaries. Before turning to the properties of the accretion discs formed in such mergers, we first provide a very brief overview of their formation. We do this by considering the fiducial system TNT.chit.0.35. In order to illustrate th... | [
"Foucart et al. 2012"
] | [
"The general dynamics of this process have been studied extensively in purely hydrodynamical simulations"
] | [
"Background"
] | [
[
912,
931
]
] | [
[
765,
868
]
] |
2015MNRAS.454.1644L__Kotze_&_Charles_2012_Instance_3 | The period candidates of other three ULXs may range from ∼100 to ∼600 d. Apart from noise and artefacts, all the candidate periods are only significant in a specific epoch. This suggests that they are not associated with any stable mechanism such as orbital motion. Instead, such long-term (> 100 d) X-ray quasi-periodic... | [
"Kotze & Charles 2012"
] | [
"For a warped disc, the binary separation and the mass ratio suggest that M81 X-6 lies in the intermediate instability zone for radiation-driven warping in X-ray binaries (see fig. 1 of"
] | [
"Compare/Contrast"
] | [
[
2057,
2077
]
] | [
[
1872,
2056
]
] |
2022AandA...666A.112L__Cormier_et_al._2015_Instance_1 | Local dwarf galaxies were the focus of large Herschel and Spitzer surveys (e.g., The Dwarf Galaxy Survey, DGS; Madden et al. 2006). Studies on both resolved and integrated-galaxy scales have highlighted some distinctively unique observational signatures of star-forming low-metallicity dwarf galaxies. A non-linear relat... | [
"Cormier et al. 2015"
] | [
"Furthermore, the hard radiation fields in star-forming dwarf galaxies, along with their lower dust abundance, result in extended ionized gas regions prominent on global galaxy scales"
] | [
"Compare/Contrast"
] | [
[
796,
815
]
] | [
[
592,
774
]
] |
2022AandA...663A.105P__Bonafede_et_al._2012_Instance_2 | Cluster radio relics are usually found in the outskirts of merging galaxy clusters. They exhibit elongated morphologies and high degrees of polarisation above 1 GHz (up to 70%, Ensslin et al. 1998; Bonafede et al. 2014; Loi et al. 2019; de Gasperin et al. 2022). The resolved spectral index in radio relics shows a gradi... | [
"Bonafede et al. 2012"
] | [
"In some cases, double relics have been detected on opposite sides of the cluster centre (e.g.,",
"In these clusters it is possible to constrain the merger history, providing important information about the formation processes of relics."
] | [
"Background",
"Background"
] | [
[
2022,
2042
]
] | [
[
1872,
1966
],
[
2071,
2209
]
] |
2021MNRAS.501.3781R__Nisini_et_al._2005_Instance_2 | While spatially extended optical jets and bipolar CO molecular outflows have been observed in numerous Class 0/I protostars (e.g. Reipurth & Bally 2001; Bally 2016, and references therein), near-infrared high-resolution spectroscopy and spectroimaging observations in the past two decades have made it possible to study ... | [
"Nisini et al. 2005"
] | [
"The mass accretion and loss rates for Class 0/I low-mass protostars span the range of 10−6–10−8 M⊙ yr−1, and the derived jet efficiencies (ratio between mass ejection and accretion rates) range between ∼1 per cent and 10 per cent (e.g."
] | [
"Background"
] | [
[
1810,
1828
]
] | [
[
1543,
1778
]
] |
2022ApJ...932...98S__hand,_FRB_2018_Instance_1 | The band-limited nature of repeaters makes it essential to have high-resolution simultaneous observations with a large bandwidth that can help detect variations in the spectrotemporal and even polarimetric structures of the bursts at different frequencies. The study of these contemporaneous frequency-dependent variatio... | [
"Pleunis et al. 2021"
] | [
"On the other hand, FRB 20180916B has a nominal RM and has shown a gradual variation in RM value over the two year timescale"
] | [
"Differences"
] | [
[
1048,
1067
]
] | [
[
923,
1046
]
] |
2021ApJ...908...40M__Muschietti_&_Lembège_2017_Instance_1 | These signatures are inconsistent with ultra-low frequency waves, which have circular polarization and a period similar to the upstream ion gyroperiod. The waves are also inconsistent with ion Weibel instability, which generates linearly polarized waves. Interaction of reflected ions with incoming solar wind electrons ... | [
"Muschietti & Lembège 2017"
] | [
"Modified Two Stream Instability (MTSI) due to relative drift between reflected ions and incoming solar wind electrons (fast drift), and incoming solar wind ions and electrons (slow drift) has been frequently considered"
] | [
"Compare/Contrast"
] | [
[
733,
758
]
] | [
[
404,
622
]
] |
2016ApJ...821..107G__Gloeckler_&_Fisk_2015_Instance_4 | 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"
] | [
"At low energies they assumed the ENA energy spectra provided by Fuselier et al. (2012). They derived a total pressure of 2.5 pdyn cm−2 in all three plasma regions in the nose of the heliotail",
"Pressure contributions from the slowed solar wind, magnetic pressure, and the pressure exerted from pickup ions and an... | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
3133,
3154
]
] | [
[
2940,
3131
],
[
3157,
3358
]
] |
2016ApJ...824..138Y__yanin_2011_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... | [
"Istomin and Sob’yanin 2011"
] | [
"However, it is tempting to speculate that environmental effects from such a rich field could be playing a role in the production of this wind nebula (e.g., triggering of pair cascade by external gamma rays from a nearby source"
] | [
"Motivation"
] | [
[
1044,
1070
]
] | [
[
787,
1013
]
] |
2016MNRAS.457.3084M__Storm_et_al._2005_Instance_1 | The populous blue LMC cluster NGC 1866 is already known to host an exceptionally rich sample of more than 20 Cepheids (Musella et al. 2006; Welch & Stetson 1993). One of these was identified by Musella et al. (2006) in a preliminary analysis of the proprietary BVI Very Large Telescope (VLT) data. It is unquestionable t... | [
"Storm et al. 2005"
] | [
"It is unquestionable that such a unique sample of Cepheids – likely all members of the cluster and at the same distance, chemical composition and age – would constitute a milestone in our understanding of the Cepheid pulsational scenario. Indeed, it offers an unprecedented opportunity to investigate both empirical... | [
"Motivation",
"Motivation"
] | [
[
908,
925
]
] | [
[
298,
807
],
[
946,
1076
]
] |
2020MNRAS.494.2465B__Hornik_1991_Instance_1 | Here we demonstrate that, over a fixed time interval, the planar three-body problem can be solved by means of a multilayered deep artificial neural network (ANN; e.g. see LeCun, Bengio & Hinto 2015). These networks are designed for high-quality pattern recognition by mirroring the function of our brains (McCulloch & Pi... | [
"Hornik 1991"
] | [
"The abundance of real-world applications of ANNs is largely a consequence of two properties: (i) an ANN is capable of closely approximating any continuous function that describes the relationship between an outcome and a set of covariates, known as the universal approximation theorem"
] | [
"Background"
] | [
[
809,
820
]
] | [
[
509,
793
]
] |
2016ApJ...817...12P__Sur_et_al._2007_Instance_1 | 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"
] | [
"Mechanisms suggested to produce these small-scale magnetic helicity fluxes are: advection of magnetic fields by an outflow from the disk through the galactic fountain or wind"
] | [
"Background"
] | [
[
1167,
1182
]
] | [
[
969,
1143
]
] |
2022AandA...667A...5R__Bakx_et_al._2020_Instance_1 | The characterization of the dynamics of galaxies just after (4 ≲ z ≲ 6) and within the Epoch of Reionization (z ≳ 6) is still in its infancy as spatially resolved observations targeting emission lines are available only for about ten of sub-mm sources (e.g., Rizzo et al. 2020; Lelli et al. 2021; Rizzo et al. 2021) and ... | [
"Bakx et al. 2020"
] | [
"Similar results are obtained in studies of individual galaxies at z ∼ 6–8",
"However, given the low angular resolution of these data, they can not rule out the possibility that one or more merging [C II]-bright satellites are mimicking the smooth gradient observed in the velocity maps"
] | [
"Similarities",
"Compare/Contrast"
] | [
[
1032,
1048
]
] | [
[
957,
1030
],
[
1073,
1281
]
] |
2015MNRAS.450.4364N__Wu_et_al._2004_Instance_2 | Low- and intermediate-mass stars are formed by the gravitational collapse of the parental giant molecular cloud (GMC), followed by the accretion process (Palla 1996). During the accretion phase, material is ejected as well via collimated bipolar jets. However, when a YSO reaches 8 M⊙, the radiative flux becomes so inte... | [
"Wu et al. 2004"
] | [
"Massive YSO outflows mapped in high-velocity CO lines have collimation factors R = length/width ∼2.05 ± 0.96 as compared to R ∼ 2.81 ± 2.16 for low-mass stars",
"indicating a weak tendency that outflows associated with massive stars are less collimated than those from low-mass stars as previously thought"
] | [
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1643,
1657
]
] | [
[
1483,
1641
],
[
1660,
1803
]
] |
2021AandA...645A..95H__Boese_2000_Instance_1 | Next we chose an optimum cut-off radius for the detector FOV. The PSPC has a circular FOV with a radius 57′. The PSPC entrance window has a rib support structure with an inner ring at a radius corresponding to 20′ (Pfeffermann et al. 1987; Hasinger & Zamorani 2000). Both the ROSAT telescope angular resolution and its v... | [
"Boese (2000)"
] | [
"The combined detector and telescope PSFs are described in detail in"
] | [
"Background"
] | [
[
513,
525
]
] | [
[
445,
512
]
] |
2018AandA...613A..76J__Kennedy_&_Kenyon_2008_Instance_2 | One of the most intriguing results from RV surveys is the observed scarcity of relatively close-in (a ≲ 0.5 AU) planets around post-MS stars. This observational trend has been attributed to the strong tidal torque exerted by the star as its radius grows during the giant phase. As a result, planets are expected to lose ... | [
"Kennedy & Kenyon 2008"
] | [
"In addition,",
"and the snow line is located at a greater distance from the central star",
"As a consequence, these planets are most likely formed at greater orbital distances and, due to the shorter disk timescale, inward migration is halted; they thus reach their final position at a relatively large distance... | [
"Compare/Contrast",
"Compare/Contrast",
"Compare/Contrast"
] | [
[
1419,
1440
]
] | [
[
1162,
1174
],
[
1345,
1417
],
[
1443,
1684
]
] |
2017ApJ...850...97B__Haynes_et_al._2011_Instance_1 | The H i mass fraction of every gas particle in the baryonic runs is calculated based on the particle’s temperature and density and the cosmic UV background radiation flux while including a prescription for self-shielding of H2 and dust shielding in both H i and H2 (Christensen et al. 2012). This allows for the straight... | [
"Haynes et al. 2011"
] | [
"Specifically, we create mock data cubes that mimic ALFALFA observations"
] | [
"Uses"
] | [
[
534,
552
]
] | [
[
461,
532
]
] |
2021MNRAS.505.2561C__Hunt_et_al._2018_Instance_1 | Several mechanisms have been suggested to explain the formation of moving groups. A common explanation is that these velocity structures are the remnants of open clusters, or formed by interactions with a bar (Eggen 1965; Dehnen 2000). One problem with the cluster formation idea is that stars in moving groups can have ... | [
"Hunt et al. 2018"
] | [
"Recent work also finds that transient spiral structure",
"may lead to the formation of moving groups,"
] | [
"Background",
"Background"
] | [
[
826,
842
]
] | [
[
770,
824
],
[
844,
887
]
] |
2019AandA...632A..37B__Desidera_et_al._2015_Instance_1 | Of the almost 4000 exoplanets known today, more than 3700 were discovered via the radial-velocity (RV) or transit methods1. According to the database, only three of them (V830 Tau b, Donati et al. 2016; K2-33 b, David et al. 2016, and TAP 26 b, Yu et al. 2017) are younger than 100 Myr. The main reason for this is the s... | [
"Desidera et al. 2015"
] | [
"Thus, in order to discover all planets in a system, one either needs to image old stars – which seems currently impossible given the already low detection rate around young stars probed by large DI surveys (e.g.,",
"– or try to minimize the impact of the stellar activity of young stars."
] | [
"Background",
"Background"
] | [
[
1106,
1126
]
] | [
[
893,
1105
],
[
1181,
1252
]
] |
2020MNRAS.493.4868L__Stephens_et_al._2019_Instance_1 | Recently, polarized (sub)millimetre emission has been detected in an increasing number of discs by Atacama Large Millimeter/submillimeter Array (ALMA) with its high sensitivity and angular resolution. However, the origin of disc polarization remains uncertain, since grains do not have to be aligned with just the magnet... | [
"Stephens et al. 2019"
] | [
"Furthermore, even spherical grains can produce polarized emission by self-scattering of large grains in an anisotropic radiation field"
] | [
"Compare/Contrast"
] | [
[
794,
814
]
] | [
[
613,
747
]
] |
2022ApJ...939..117Z__Malkan_&_Moore_1986_Instance_1 | Blazars are a subclass of active galactic nuclei (AGNs) with relativistic jets of high-energy particles pointing near our line of sight (e.g., Urry & Padovani 1995). Their nonthermal emission is generally detected across the entire electromagnetic spectrum from radio to γ-ray bands. Blazars are subclassified into flat-... | [
"Malkan & Moore 1986"
] | [
"FSRQs have high luminosity and a thin and radiatively efficient black hole accretion disk"
] | [
"Background"
] | [
[
755,
774
]
] | [
[
664,
753
]
] |
2022AandA...663A...4S__Jönsson_et_al._2020_Instance_1 | The pioneer of spectroscopic surveys, the Radial Velocity Experiment (RAVE), produced its first data release (DR) 15 years ago (Steinmetz et al. 2006) and its final one, DR6, last year (Steinmetz et al. 2020a,b). In the meantime, other surveys have been operated, and survey designers have developed new methodologies, l... | [
"Jönsson et al. 2020"
] | [
"Besides RAVE, other surveys have published successive DRs that are available for public use. At the time of writing, there is open access to the DR16 of the Apache Point Observatory Galactic Evolution Experiment (APOGEE;"
] | [
"Background"
] | [
[
792,
811
]
] | [
[
571,
791
]
] |
2020AandA...639A..20K___2015_Instance_1 | where
D
ϵ
Dt
$ \frac{D \epsilon}{Dt} $
is the advective derivative of the energy density,
κ
=
κ
0
T
5
/
2
b
̂
$ {\boldsymbol{\kappa}} = \kappa_0 T^{5/2} \hat{{\boldsymbol{b}}} $
is the Spitzer conductivity along magnetic field lines, Qheat and Qcool are heating and radiative cooling ra... | [
"Fang et al.",
"2015"
] | [
"The user defined heating is therefore highly stratified, spatially smooth and steady (e.g."
] | [
"Compare/Contrast"
] | [
[
859,
870
],
[
877,
881
]
] | [
[
748,
838
]
] |
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