adsabs/WIESP2022-NER huggingface dataset:
Paper: 2018MNRAS.478.2599A (fulltext)
et al. 2013 ). Moreover, Cleeves et al. ( 2015 ) show that reduced cosmic ray ionization (a consequence of exclusion by disc winds) produce disc chemistry features in agreement with TW Hya observations. Our population results showing that X-ray ionized models produce populations that better reproduce observational features are in agreement with these results. One key difference in our super Earth populations and the observations is that our model produces fewer close-in super Earths. When comparing the direct population outputs (Fig. 10 ) with the populations that account for observational biases (Fig. 9 ), we see that a portion of the zone 5 planets in our model are filtered out as they have low observation probabilities. Additionally, our model does produce a large number of failed cores, but a significant fraction of these orbit just outside the defined outer observable limit of 2 au, and are situated on orbits out to 5 au. The range of radii between 1 and 5au is the most common region for super Earths to form in our model as this is the region where the ice line, heat transition, and cosmic ray dead zone traps converge to. Thus, our model predicts there to be a significant population of super Earths with orbital radii of 1–5 au. Our planet formation model does not produce low mass super Earths that migrate into short-period orbits. We noted this several times throughout Section 4 and refer to this as a zone of avoidance of our model within zone 5 of the mass-semimajor axis diagram. The lowest mass super Earths formed in our model that populate zone 5 are ∼3 M ⊕ and orbit outside of 1 au. This feature of our populations is tied to the evolution of the traps that evolve from orbital radii outside ∼8 au to within ∼1 au on disc evolution time-scales. This prevents ∼Earth-mass planets from migrating to short period orbits in our model as they evolve with the trap they are forming within. Planets can, however, become liberated from their host planet traps at the onset of type II migration. In this case, planets must exceed their gap opening mass (equation 17 ) of ∼10 M ⊕ to type II migrate separately from their trap. Initially, type II migration takes place on shorter time-scales than trapped type I migration, so these planets can, in some cases, migrate to short period orbits during their slow gas accretion phase before their accretion is terminated at the disc lifetime. Thus, the lowest mass zone 5 planets orbiting between 0.01 and 0.1au formed in our model have masses ≳10 M ⊕ . Hasegawa ( 2016 ) also found that a core accretion model involving trapped type I migration could not form a failed core population consistent with observations. In particular, this model could only form super Earths more massive than ∼4–5 M ⊕ , similar to the results found in this work. Based on the results of our constant dust-to-gas ratio model, one might suggest that formation scenarios in addition to the failed core scenario are necessary to explain the observed
Paper: 2020ApJ...889...68A (acknowledgments)
Members of the CAGE team (Cosmochimie, astrophysique et géophysique expérimentale) at IPGP are thanked for insightful discussions. G.A. acknowledges funding from the Région Ile-de-France through the DIM-ACAV+ program. J.D.G. acknowledges funding from the Science and Technology Facilities Council (STFC) grant No. ST/R000751/1. This study contributes to the IdEx Université de Paris ANR-18-IDEX-0001. This is IPGP contribution #4092.
Paper: 2015A&A...579A..76J (acknowledgments)
This paper has benefitted from discussions in depth with the referee J. Th. van Loon. This work was partially funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070 First Science with the GTC 6 , and through grants AyA2011-24052. This work has been supported by the CoSADIE Coordination Action (FP7, Call INFRA-2012-3.3 Research Infrastructures, project 312559). F.J.E. acknowledges financial support from the ARCHES project (7th Framework of the European Union, No. 313146). Support was also granted by Deutsche Forschungsgemeinschaft through grant EN 176/30.
Paper: 2015MNRAS.446.1716C (acknowledgments)
We acknowledge the insightful discussions and useful comments of A. de Ugarte-Postigo and C. Thöne. We acknowledge the support from the European Research Council (Starting Independent Researcher Grant CAMAP-259276), and the partial support of grants AYA2010-21097-C03-01, CSD2007-00050 and PROMETEO-2009-103. CC-M also acknowledges the support of ACIF/2013/278 fellowship, and the partial support of UV-INV-PREDOC13-110509 fellowship. We thankfully acknowledge the computer resources (‘Lluís Vives’ and ‘Tirant’ supercomputers), technical expertise and assistance provided by the Servei de Informatica at the University of Valencia.
Paper: 2020MNRAS.493.4058B (fulltext)
Lake Meteorite. The first specimen of 131 g was discovered on 2000 September 17. Later investigations on 2006 November identified additional 526 fragments with total mass of 8991 g, i.e. 900 per cent of increase of the total known weight (Verish 2009 ). The distribution of Antarctic ordinary chondrites and elsewhere present similar entropic indices (2.12 and 2.18) what suggests equivalent mechanisms that yield the observed distributions. On the other hand, β q present a variation of the order of 10 times between the distributions. This result confirms the tendency identified by Huss ( 1990 ); the Antarctic meteorites present mean mass smaller than those found in the rest of the Earth. The combined sample is modeled by a q -stretched exponential, most probably due to the influence of the larger mean mass of non-Antarctic meteorites. These results, and the great dispersion of the entropic indices, suggest that the observed distributions, more properly modeled by q -stretched exponential, are more influenced by the ‘gathering bias’. 4.3 Findings/fall location sites Halliday, Blackwell Griffin ( 1989 ) suggested an overall rate of 83 falls of meteorites every 10 6 km 2 /yr. Considering this estimate, it would be expected 85 events per year in Brazil (de Carvalho 2010 ). This amount exceeds the number of meteorites collected in the last two centuries in the country. This suggests the occurrence of a gathering bias on the observed distribution. When meteorites are separated by regions with large territorial areas (Russia, Canada, USA, China, and Brazil), we verified that the distributions are described by q -stretched exponential with a P value ≥0.95 (Fig. 6 ). Figure 6. Inverse cumulative distributions of mass for some types of meteorites found in Brazil (circles), Canada (diamonds), China (squares), Russia (crosses), and USA (plus). The red solid lines represent the fitting of q -stretched exponentials for the meteorites found in Brazil ( q = 1.87, β q = 5.43 × 10 −3 g −1 , N t = 74, and γ = 0.57), Canada ( q = 1.47, β q = 5.08 × 10 −3 g −1 , N t = 65, and γ = 0.61), China ( q = 1.64, β q = 7.48 × 10 −2 g −1 , N t = 359, and γ = 0.39), Russia ( q = 1.91, β q = 4.20 × 10 −3 g −1 , N t = 144, and γ = 0.61), and USA ( q = 1.43, β q = 2.60 × 10 −2 g −1 , N t = 1816, and γ = 0.48). The average γ = 0.53 ± 0.08 overlaps with the value found on sub-Section 4.2. This result may be understood if the fraction of meteorites by mineralogical type is also valid for national (local) samples. This hypothesis is reasonable, since the weight average shape parameter of the total sample of meteorite types modeled by q -stretched exponential is γ = 0.65. The values of β q for China and USA are about 10 times smaller than the other national samples. This implies a smaller number of meteorites of large mass for these two countries. The origin for this may be due to the fraction of iron meteorites in the samples. Iron meteorites are heavier in all national samples, but
Paper: 2016A&A...594A..29B (acknowledgments)
We thank Dr. Jan Robrade of Hamburger Sternwarte for his help in data analysis of the XMM-Newton data. This work was carried out as part of Project A16 funded by the Deutsche Forschungsgemeinschaft (DFG) under SFB 963. AAV acknowledges support from an Ambizione Fellowship of the Swiss National Science Foundation. C.P.F. was supported by the grant ANR 2011 Blanc SIMI5-6 020 01 “Toupies: Towards understanding the spin evolution of stars”. Part of the work was also supported by the COST action MP1104 “Polarisation as a tool to study the Solar-system and beyond”. Finally, we thank the anonymous referee for their detailed and constructive comments.
Paper: 2016MNRAS.461..164I (fulltext)
(SLAC) lenses for a substructure mass function slope α = 0.90 () (Vegetti et al. 2014 ). Thus, as long as baryonic physics does not significantly affect the result, it is reasonable to conclude that CDM substructures are not the entire reason for the flux anomaly problem. On the other hand, our result for line-of-sight lensing significantly differs from the result that was obtained using R cusp and R fold (Xu et al. 2012 ). The difference may come from the typical source redshift z S = 2 assumed in Xu et al. ( 2012 ). In fact, our result indicates that for z S 2, the ratio of the strength of the convergence perturbation from subhaloes to that of the total value is 30 to 40 per cent. For higher source redshifts, however, the ratio becomes much smaller. Moreover, the two lens systems B2045+265 and B1555+375 used in Xu et al. ( 2012 ) (the latter was excluded in our analysis), which have a relatively large R cusp = 0.4–0.5, show another source of anomaly: B2045+265 has a secondary lens (McKean et al. 2007 ) and B1555+375 has an edge-on disc component that can account for the anomaly (Hsueh et al. 2016 ). Excluding these complex lenses would surely weaken the discrepancy with our result. Complex lens environments, such as secondary lenses and disc components and neighbouring groups and clusters, should be taken into account properly. Our result indicates that a secondary lens can reside in the intergalactic space and is not necessarily a companion of the primary lens. Furthermore, the previously claimed subhalo with a mass of (1.9 ± 0.1) × 10 8 M ⊙ discovered from the residual image of an Einstein ring in B1938+666 (Koopmans 2005 ; Vegetti et al. 2012 ) may not be the subhalo of the primary lensing galaxy halo. It may be isolated from any haloes or belong to another distant one. To measure the redshift of a secondary or that of a third lens, we can use the distortion pattern of an extended source and future submillimetre observations would be able to detect such small signals (Inoue Chiba 2005a , b ). Using ALMA, the detection of other anomalous anomalies in lensed quadruple SMGs could be achieved by increasing the number of anomalous targets to ≳10, which would test our findings. In our analysis, we assumed that primary lenses are described by SIEs as indicated by the surface brightness of the lensing galaxies. This assumption may be too simple. We did not take into account the slight smooth distortion of the lens potential, such as low-order multipoles m 3 and m 4, or a deviation from an isothermal profile. As long as these complexities are related with the fluctuations of the first derivatives on scales comparable to or larger than the Einstein radius of the primary lens, we expect that our result would not change significantly. This is because the anomaly in the flux ratios is caused by a perturbation of the second derivatives of the gravitational potential rather than the first derivatives. However, to obtain more accurate results, we do
Paper: 2020ApJ...889....4P (acknowledgments)
M.P. and F.M. acknowledge financial support from the University of Trieste (FRA2016). F.C. acknowledges funding from the INAF PRIN-SKA2017 program 1.05.01.88.04 and from grant PRIN MIUR 2017 - 20173ML3WW_001. The authors thank an anonymous referee for careful reading of the manuscript and useful suggestions.
Paper: 2017A&A...598A..96L (acknowledgments)
Guang-Xing Li received support for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne and is currently supported by the Priority Program 1573 ISM-SPP from the DFG (Deutsche Forschungsgemeinschaft). Guang-Xing Li would like to thank ISIMA (International Summer Institute for Modelling in Astrophysics, now Kavli Summer Program in Astrophysics) for facilitating collaborations, and would like to thank Nicolas Peretto and Patrick Hennebelle for discussions. Lee Hartman is acknowledged for giving a nice lecture in ISIMA, which motivates the thinking of gravity, and Di Li is acknowledged for providing references on angular momentum. Guang-Xing Li thanks Alexei Kritsuk for discussions and for his final push towards the publication of the results. Guang-Xing Li thanks Manuel Behrendt for discussions of gravitational instabilities and clumps in disk galaxies. This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of Boston University and Five College Radio Astronomy Observatory, funded by the National Science Foundation under grants AST-9800334, AST-0098562, and AST-0100793. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We also would like to thank Thomas Robitaille for making his code publicly available. The research made use of the astropy package. The referee has to be acknowledged, whose comments have lead to very significant improvements in our paper.
Paper: 2016A&A...587A..98W (fulltext)
the measured Ly profiles in Fig. 4 feature a more or less pronounced inwards upturn around a radius of 1, suggesting either a superposition of a compact emission component on top of a more extended one, or alternatively a more complicated radial law. Modelling such curved profiles as single exponentials would yield spurious values for the scale lengths that strongly depended on the chosen radial range for the fitting. We adopted a two-component model as the functional form fitted to the Ly SB distributions of each object, decomposing it into two distinct components. The first was taken to resemble that of the compact UV continuum; we call it the “continuum-like” component and assume that its shape parameters are precisely known from our GALFIT modelling of the HST images (i.e. as elongated exponential discs or as point sources), except for a single flux scaling factor related to the Ly EW of this component. The Ly halo, on the other hand, was again parametrised as a single exponential. Since in this paper we only aim at obtaining robust estimates of the azimuthally averaged halo sizes, we enforced the halo model to be circularly symmetric; we also assumed both components to be concentric (see Sect. 4.4 for a brief discussion of the fitting results when these restrictions were relaxed). There were thus 3 free parameters to be optimised in each fit: The integrated fluxes and of both Ly components, and the exponential scale length of the halo. We present the results from these fits in the next subsection. Our two-component model can be seen as a minimalistic extension of the conventional single exponential profile, but it may also represent a physically meaningful hypothesis: If some fraction of the Ly luminosity produced within the star-forming regions escapes (more or less) directly – possibly suffering from dust attentuation but without large-scale spatial redistribution – then this Ly emission will roughly follow our continuum-like component. The halo component, on the other hand, describes the Ly emission more extended than the continuum, irrespective of whether it has its origin inside the galaxy and then got scattered outwards, or whether it is produced by mechanisms other than recombination in H ii regions. An alternative approach to model the Ly SB distribution would be to replace the separation into two components by a more flexible single SB law for the Ly profile such as a Sersic function. Note that a circular Sersic profile has again 3 free parameters to be fitted (total flux, half-ligh radius and Sersic index). We explored such fits as well and briefly report about the outcome below. Fig. 7 Decomposition of the observed Ly surface brightness distributions into a compact (continuum-like) and an extended exponential component (halo), as described in the text. Only the objects with detected haloes () are shown. The datapoints are the same as in Fig. 4 , but now plotted against linear radii. The green curves show the profiles of the
Paper: 2017A&A...598A.105P (acknowledgments)
V.P. and S.M. acknowledge funding by the European Research Council through ERC grant SPIRE 647383. The authors acknowledge funding by SpaceInn, PNPS (CNRS/INSU), and CNES CoRoT/ Kepler and PLATO grants at SAp and IRAP. The authors thank the anonymous referee for helping to improve the quality of the paper.
Paper: 2018MNRAS.477.4131J (acknowledgments)
ACKNOWLEDGEMENTS We thank U. Gorti for sharing her FUV models, as well as I. Pascucci and R. Alexander for the useful and constructive discussions. JJ thanks D. Henderson for his remarks. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. BE, JJ and GR acknowledge the support of the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG Cluster of Excellence ‘Origin and Structure of the Universe.’ BE is supported by the Deutsche Forschungsgemeinschaft - Ref no. DFG ER 685/8-1 FOR 2634/1. This work has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC-2013-ADG.
Paper: 2019MNRAS.489.2669M (acknowledgments)
ACKNOWLEDGEMENTS The authors thank Charlie Conroy for useful discussions and for providing comments on a draft of this paper. We thank Steve Finkelstein, Fred Davies, and Brad Greig for useful discussions and for providing: the model from Finkelstein et al. ( 2019 ), and posteriors from Davies et al. ( 2018 ) and Greig et al. ( 2019 ), respectively. We thank Austin Hoag for sharing the posterior from Hoag et al. ( 2019 ). CAM acknowledges support by NASA Headquarters through the NASA Hubble Fellowship grant HST-HF2-51413.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. RPN gratefully acknowledges an Ashford Fellowship and Peirce Fellowship granted by Harvard University. ST is supported by the Smithsonian Astrophysical Observatory through the CfA Fellowship. JL is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1701487. Software : ipython (Pérez Granger 2007 ), matplotlib (Hunter 2007 ), numpy (Van Der Walt, Colbert Varoquaux 2011 ), scipy (Oliphant 2007 ), astropy (Robitaille et al. 2013 ), dynesty (Speagle 2019 ).
Paper: 2017MNRAS.466.3088W (fulltext)
u g as well, the sample increases to 114. We also see that as we impose even stricter cuts, we can decrease the number of SDSS objects by an order of magnitude, while keeping nearly all of the known lenses. We do not use the stricter cuts in this implementation, but they could be used in the future with larger data sets to keep things more tractable. 3.2.4 Choosing features We build our features from combinations of magnitudes in different bands. Fig. 1 shows the distribution of our training set data in various colour and magnitude spaces. As can be seen, different kinds of objects occupy specific locations in feature space. By choosing features that best distinguish between types of objects and combining them into one high-dimensional space, our model can more easily separate the different populations of objects. Figure 1. Colourcolour plots showing the locations of our training sets in feature space. The red, green, blue and orange points represent the point-like QSOs, extended QSOs, simulated lensed quasars and blue cloud galaxies, respectively. The black stars are known lensed quasars that lie in the SDSS footprint. The dashed lines show the colour cuts listed in equation ( 6 ). Dotted lines represent either cuts that are within or statements or other cuts often used to eliminate contaminants. The black stars represent 128 known lenses that lie in SDSS, found by various selection techniques. Many have similar colours to point-like quasars, indicative of the colour selection step described by Oguri etal. ( 2006 ). Others have redder colours, corresponding to either Type-II AGN sources or bright lensing galaxies. We are mainly concerned with finding blended, small-separation lenses, since the large separation counterparts are more likely to have been found already. Therefore, we are less interested in the objects that fall on the point-like QSO locus. The dashed lines in the plot show the typical cuts that we use when selecting objects. In order to include lenses that have larger contributions from the lensing galaxy, we use relatively loose cuts in u g and W 1 W 2. However, known lenses do not lie predominantly at low W 1 W 2 or high u g . Additional metrics, such as those using the K band, can be useful for trimming contaminants in these regimes, as is done by Ostrovski etal. ( 2017 ), but this introduces two issues for our purposes. First, many of the simulated lenses are particularly bright in K . This is because the lenses are constructed via sparse interpolation over 2MASS magnitudes that suffer from Malmquist bias. Secondly, we are introduced with a depth-versus-footprint trade-off that must be addressed. Surveys such as the Two Micron All-Sky Survey (2MASS) cover the whole sky, but are not always deep enough for our purposes. In fact, only 16percent of our SDSS training set objects have valid K magnitudes in 2MASS. Deeper surveys such as the UKIRT Infrared Deep Sky Survey (UKIDSS) and the VISTA Hemisphere Survey (VHS), on the other