adsabs/WIESP2022-NER huggingface dataset:
Paper: 2015A&A...577A..85B (acknowledgments)
The authors would like to thank the anonymous referee for useful comments and their colleagues of the SL2S and SLACS collaborations for many useful discussions as well as stimulating exchanges within the Euclid Strong Lensing Science Working Group. R.G. also acknowledges E. Bertin for valuable discussions about massive model fitting. This work was supported by the Centre National d’Études Spatiales (CNES) and the Programme National Cosmologie et Galaxies (PNCG). This research is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, a joint project of CFHT, Taiwan, Korea, Canada and France, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre.
Paper: 2019ApJS..244...16W (fulltext)
either the use _ f160w or use _ f850lp flags, as noted in each subsequent case. We further compare to the CANDELS GOODS-S photometric catalog released by Guo et al. ( 2013 ), adopting flags equal to zero for non-contaminated sources. The CANDELS GOODS-S catalog presents the multiwavelength (UV to mid-IR) photometry, with source detection performed in the WFC3 H F160W mosaic using a “hot” and “cold” detection methodology. We first present the number counts in Section 3.1 and then cross-match all catalogs within a 05 radius to compare aperture photometry in Section 3.2 . Finally, in Section 3.3 , we show several example SEDs to showcase the high quality of the photometry. 3.1. Number Counts The number densities of galaxies that satisfy the use _ f160w criterion in the GOODS-S field are shown in Figure 13 as a function of the total H F160W magnitude for both HLF (black), 3D- HST (red), and CANDELS (blue). The error bars are Poisson. Though completely independent data reductions, the three data sets are fairly similar in terms of F160W coverage; HLF covers 207 arcmin 2 in H F160W , whereas CANDELS covers 173 arcmin 2 , and 3D- HST covers 171 arcmin 2 . It is therefore not surprising that the number counts are consistent. The deficit of sources with ABmag in CANDELS relative to the two other fields is likely the result of using a deeper multi-band combined detection image. The further excess of objects at the faint end in HLF results from a combination of effects. In part, this population of faint sources will arise due to the more aggressive source detection settings adopted. But in some cases, it is clear that the HLF F160W imaging is deeper than the earlier 3D- HST version (i.e., explaining why both 3D- HST and HLF have more faint number counts), but HLF appears to further reveal an exciting new population of extremely faint sources. Figure 14 shows 15 × 15 postage stamps (, , H F160W ) of 48 ultra-faint sources with magnitudes between 28 and 29 ABmag rank-ordered by S/N that are identified in the HLF photometric catalog but do not have a match within a radius of 04 in the 3D- HST photometric catalog. Figure 13. Number counts of galaxies with Poisson errors in the GOODS-S field as a function H F160W total magnitude, with no correction for incompleteness. The agreement between HLF (black), 3D- HST (red) and CANDELS (blue) is excellent. Figure 14. Example postage stamps (, , H F160W ) of 48 ultra-faint sources between 28 and 29 ABmag identified in HLF but not 3D- HST . The objects are rank-ordered by S/N, with the outline of the segmentation map shown as a white contour for reference. The depths in the HLF GOODS-S mosaic vary significantly within the field (i.e., HUDF, CANDELS deep, wide, ERS, etc.). Such a heterogeneous weight map implies that the single number count histogram shown in Figure 13 is simply the superposition of the histograms at different depths. In order to better understand the improvement, we separate the weight map into four
Paper: 2019MNRAS.486.3517L (fulltext)
we only observe in the vertical direction, meteor ablation height generally correlates very well with the vector velocity of a meteor. The average ablation height for the three groups of meteors is 105, 103, and 99 km, respectively. Meteors observed on the back-side of the Earth are largely prograde meteors with a heliocentric velocity larger than 30 km s −1 . Their detection rate is very low because of small atmospheric entry velocity. 6 DISCUSSION AND CONCLUSION The most important aspect of the current report is the conclusion that the majority of the meteors observed by the Arecibo radar are in nearly circular orbits. This points to the importance of Poynting–Robertson and solar wind drags. The nature of the two drags is similar, with the latter being about 30 per cent of the former (Gustafson 1994 ). In order for the drag forces to be effective, meteoroid mass is typically smaller than 10 −11 kg. On the other hand, when β, the ratio of radiation pressure to solar gravitation force, is larger than 0.5, a particle will be blown out of the solar system. β = 0.5 corresponds to a particle size of 1 μm (Dermott et al. 2001 ) and a mass of 10 −14 kg, which is the lower boundary of the meteors observed at Arecibo as discussed above. Thus, Arecibo meteors appear to have the ‘Goldilocks’ size, small enough for the drags to force them into nearly circular orbits and being pulled inward to the Sun but large enough not to be blown away by the radiation pressure. The simulations by Borin et al ( 2017 ) show that it takes several million years to reduce the semimajor axis from 3.4 to 1 au for a 10 μm in radius particle. The evolution time for the smaller Arecibo particles is expected to be much shorter. As the Earth lies relatively close to the Sun, the majority of the meteoroids have their initial orbits outside that of the Earth whether they are of asteroidal or cometary origin. For meteoroids whose size is right for drag forces to be important, their orbits will evolve into nearly circular ones at 1 au if not rejected by gravitational scattering by outer planets. Meteoroids with a diameter of 1–9 μm originating from as far as the Kuiper belt have a 20 per cent chance of reaching 1 au and once a meteoroid's orbit reaches within that of Jupiter, it will largely spiral onto the Sun (Liou, Zook Dermott 1996 ). As all meteoroids in the mass range of 10 −14 –10 −11 kg generated outside Earth's orbit have a good chance to be on nearly circular orbits when they reach the inner solar system, their population is thus expected to be uncharacteristically large at 1 au. Further, meteoroids in the ecliptic plane have a higher probability ejected by outer planets than those on inclined planes. Although the distribution shown in Fig. 4 is a convolution of instrument aspect sensitivity and the true distribution, it indicates at least that a large number of meteoroids exist in inclined orbits. The ‘inclined’ population discussed by Divine ( 1993 ) has low
Paper: 2020ApJ...900...67K (fulltext)
respectively (Kouveliotou et al. 1993 ; Mészáros 2006 ). While long GRBs are most likely associated with the collapse of massive stellar objects (Woosley 1993 ; MacFadyen Woosley 1999 ), the short ones are usually attributed to the merger of two neutron stars (Eichler et al. 1989 ; Paczynski 1990 ), or one neutron star with one black hole (Lattimer Schramm 1976 ; Lee Ramirez-Ruiz 2007 ). They are also potential sources responsible for the emission of ultrahigh-energy cosmic rays (Milgrom Usov 1995 ; Waxman 1995a , 1995b ; Dermer Humi 2001 ; Chakraborti et al. 2011 ), high-energy neutrinos (Waxman Bahcall 1997 ; Waxman 2000 ; Abbasi et al. 2012 ; Murase et al. 2013 ), and gravitational waves (Kobayashi Mészáros 2003 ; Corsi Mészáros 2009 ; Chen Holz 2013 ; Lasky Glampedakis 2016 ; Abbott et al. 2017 ). The study of GRBs has been prolific over the past decades (Zhang Meszaros 2004 ; Nakar 2007 ; Kouveliotou et al. 2012 ; D’Avanzo 2015 ). GRBs have opened a unique window into connecting the fields of stellar, interstellar, and intergalactic astronomy as well as cosmology. With the new generation of space-borne experiments, such as the Swift and Fermi observatories, high-energy observations of GRBs have entered a new era in the study of extragalactic background light (EBL; Ackermann et al. 2012 ; Desai et al. 2017 ) and the search for Lorentz invariance violation (LIV; Ellis et al. 2019 ; Lang et al. 2019 ; Wei 2019 ). As one example, GRB 130427A (Ackermann et al. 2014 ) was able to produce photons of up to 94 GeV in observations (126 GeV at the source after redshift correction, which accounts for the attenuation due to EBL). It is unknown up to what energy the spectrum extends, as present-day observations are limited by effective area in the case of space-based instruments. Ground-based detectors may prove to be an important compensator for GRB observation when γ -ray energy is above tens of GeV (Grupen Buvat 2011 ; Abeysekara et al. 2012 ; de Angelis 2016 ). Two types of experimental techniques are available for this purpose: imaging air Cerenkov telescopes (IACTs) and extended air shower (EAS) array. IACTs have better observational sensitivity to stable point sources due to their higher angular resolution and better background rejection power (Poggiani 2017 ). However, IACTs have a limited field of view, which makes them useful for follow-up observations. Moreover, the requirement of a safe slew time makes follow-up of real-time alerts difficult. Even when slew time is not an issue, a small field of view requires accurate pointing in the GRB direction. However, the error boxes provided by wide-field-of-view GRB monitors are usually large at alert time. Another disadvantage is that IACTs operate in good weather on moonless nights, which makes the duty cycle of IACTs only 10%–15% (Hinton 2009 ; Bigongiari 2016 ). A small field of view and low duty cycle make IACTs an inconvenient and inefficient instrument for GRB observation. While EAS arrays
Paper: 2018ApJ...861...76P (acknowledgments)
We are thankful to Zhoujian Zhang for providing us the results of his paper. This paper makes use of data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The material is based upon work supported by NASA under award Nos. NNX15AV64G, NNX16AE55G, and NNX16AJ22G. P.K.G.W. and E.B. acknowledge support for this work from the National Science Foundation through grant AST-1614770. Some/all of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non- HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This publication makes use of data from the Sloan Digital Sky Survey. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High Performance Computing at the University of Utah. The SDSS website is http://www.sdss.org . SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, which can be found at http://www.sdss.org/collaboration/affiliations/ . This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work made use of the http://gaia-kepler.fun cross-match database created by Megan Bedell. Software : Astropy Collaboration et al. ( 2013 ), Matplotlib (Hunter 2007 ), Numpy (Oliphant 2015 ). Facility: Kepler .
Paper: 2017MNRAS.469.2441L (acknowledgments)
Acknowledgments This research was partially supported by an iCore grant and an ISF grant. We thank Scott Tremaine, Kenta Hotokezaka and Sivan Ginzburg for useful discussions.
Paper: 2019MNRAS.485.4091M (acknowledgments)
ACKNOWLEDGEMENTS We thank Andrei Beloborodov, Yuri Lyubarsky, Illya Plotnikov, and Indrek Vurm for helpful information and conversations. We thank the reviewer, Jonathan Katz, for helpful comments. BDM and LS acknowledge funding from the National Science Foundation (grant number 80NSSCK1104). BM is supported by NASA through the NASA Hubble Fellowship grant #HST-HF2-51412.001-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.
Paper: 2019ApJ...876...89V (acknowledgments)
Support for the German contribution to GBM was provided by the Bundesministerium für Bildung und Forschung (BMBF) via the Deutsches Zentrum für Luft und Raumfahrt (DLR) under grant No. 50 QV 0301. The USRA coauthors gratefully acknowledge NASA funding through contract NNM13AA43C. The UAH coauthors gratefully acknowledge NASA funding from cooperative agreement NNM11AA01A. E.B. and C.M. are supported by an appointment to the NASA Postdoctoral Program, administered by the Universities Space Research Association under contract with NASA. D.K., C.A.W.H., and C.M.H. gratefully acknowledge NASA funding through the Fermi -GBM project.
Paper: 2015A&A...583A..30F (acknowledgments)
OSIRIS was built by a consortium of the Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany, CISAS–University of Padova, Italy, the Laboratoire d’Astrophysique de Marseille, France, the Instituto de Astrofísica de Andalucia, CSIC, Granada, Spain, the Research and Scientific Support Department of the European Space Agency, Noordwijk, The Netherlands, the Instituto Nacional de Técnica Aeroespacial, Madrid, Spain, the Universidad Politéchnica de Madrid, Spain, the Department of Physics and Astronomy of Uppsala University, Sweden, and the Institut für Datentechnik und Kommunikationsnetze der Technischen Universität Braunschweig, Germany. The support of the national funding agencies of Germany (DLR), France (CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical Directorate is gratefully acknowledged. We thank the referee, J.-Y. Li, for his comments and suggestions that helped to improve this manuscript.
Paper: 2015ApJ...809...90B (acknowledgments)
This work is supported in China by NSFC (No. 11375052, No. 10975046, No. 10120130794, No. 11165013), the Chinese Ministry of Science and Technology, the Chinese Academy of Sciences, and the Key Laboratory of Particle Astrophysics, CAS, and in Italy by the Istituto Nazionale di Fisica Nucleare (INFN). We also acknowledge essential support from W.Y. Chen, G. Yang, X. F. Yuan, C. Y. Zhao, R. Assiro, B. Biondo, S. Bricola, F. Budano, A. Corvaglia, B. D’Aquino, R. Esposito, A. Innocente, A. Mangano, E. Pastori, C. Pinto, E. Reali, F. Taurino, and A. Zerbini in the installation, debugging, and maintenance of the detector.
Paper: 2018A&A...616A..77B (acknowledgments)
We thank the referee for his or her comments that improved the manuscript, and the Kepler /K2 science teams for providing such excellent data. Funding for the Kepler /K2 mission is provided by NASA’s Science Mission Directorate. The K2 data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. The research leading to these results has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement N o 670519: MAMSIE). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France; the SAO/NASA Astrophysics Data System; and the VizieR catalogue access tool, CDS, Strasbourg, France.
Paper: 2019MNRAS.483.4766P (acknowledgments)
ACKNOWLEDGEMENTS We thank the referee for the thorough reading of the manuscript and timely suggestions to improve it. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. We also thank support from the IdP II 2015 0002 64 grant of the Polish Ministry of Science and Higher Education.
Paper: 2015ApJ...807...48S (acknowledgments)
We thank the anonymous referee for a careful review that improved this paper. This work was supported by the National Aeronautics and Space Administration (NASA) through Chandra Award Numbers (GO3-14120 A, GO3-14120B) issued by the Chandra X-ray Observatory Center (CXC), which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under contract NAS8-03060. Support for program number 13116 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. The MOJAVE program is supported under NASA-Fermi grant NNX12A087G. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Facilities: VLA, HST (WFC3), CXO (ACIS).
Paper: 2018ApJ...852....6O (fulltext)
quality factors. A selection of these factors from the original sources is summarized below. 4.1. Selected Galaxy Information When measuring rotation curve data, there are many systematic issues that affect the accuracy of the information. In Oh et al. ( 2015 ), the authors gave a comprehensive discussion of each of the galaxies in the entire sample. Although both CG and MOND capture the essence of the rotation curves across the sample well, there are occurrences where it is useful to have the relevant information about the galaxy to understand why a fit may not be as precise. We have compiled some of the relevant information below for convenience. CVN (UGCA 292) is a gas rich dwarf galaxy in the Canes Venatici constellation. This galaxy has been shown to have a high gas mass fraction and low metallicity suggesting that it is highly unevolved with an extremely LSB (van Zee 2000 ). From a fitting point of view, this galaxy is unique with its extremely low rotational measured velocities. The models shown, however, provide a sufficient fit despite this property. DDO 133 (UGC 7698) is a large, faint galaxy in the Canes Venatici cloud whose extremely LSB shows high stellar evolution (Zhang et al. 2012 ). Due to its lack of tidal motions, this galaxy is assumed to be an isolated system, which is typically beneficial for obtaining a rotation curve. However, this rotation curve was studied by one of us in the past, and can be shown to have a lower than quoted inclination (O’Brien 2012 ). Hence, we use the inclination that was previously studied and published to alleviate any discrepancies. DDO 154 (UGC 8024) is an asymmetrical dwarf galaxy and is a member of the Coma Benenices star constellation. It has been proposed that it is a physical companion of the M64 group. The galaxy is very dim, presenting a low star formation rate and contains a very large amount of atomic hydrogen (Drexler 2006 ). The galaxy is also hypothesized to have a large dark matter to baryon ratio and hence is extremely important to this work. This galaxy has been studied in CG (Mannheim O’Brien 2012 ) after the initial THINGS survey was completed by Walter et al. ( 2008 ). It can be seen in this most recent survey that the alternative gravity models can circumvent the need for the quoted high dark matter to baryon ratio. DDO 168 (UGC 8320) is a galaxy in the Canes Venatici group and is a probable pair with UGC 8308 and sometimes included in the M51 group (Karachentsev et al. 2003 ). The galaxy has a large number of dispersed H ii regions, resulting in an unusual shape to the rotation curve. The essence of the rotation curve is captured in the fits, but due to the overall structure, one cannot expect a high-resolution fit. DDO 210 is located in the Aquarius star constellation. It was one of the original galaxies discovered by van den Bergh ( 1959 ) of the David Dunlap Observatory catalog (DDO) survey. This aquarius dwarf is extremely faint, and has a very LSB, though it contains
Paper: 2015ApJ...813...71S (acknowledgments)
We thank University of Memphis students, Peter Matheny and Adam Chastain, for help with data analysis. This work was inspired and motivated by discussions at the series of Coronal Loops Workshops. The Atmospheric Imaging Assembly on the Solar Dynamics Observatory is part of NASA’s Living with a Star program. CHIANTI is a collaborative project involving the NRL (USA), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). Solar physics research at the University of Memphis is supported by a Hinode subcontract from NASA/SAO.
Paper: 2018ApJ...869...17L (acknowledgments)
We thank the anonymous referee for useful comments. F.L. thanks Sean Andrews for discussions on comparing ALMA fluxes to past interferometer fluxes, and Zhaohuan Zhu, Kaitlin Kratter, and Andrew Youdin for insightful discussions. F.L. and G.J.H. thank Subo Dong for discussions of planet mass functions and radial distributions. F.L. and G.J.H. are supported by general grants 11473005 and 11773002 awarded by the National Science Foundation of China. P.P. acknowledges support by NASA through Hubble Fellowship grant HST-HF2-51380.001-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 NAS 5-26555. G.D. acknowledges financial support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement no. 681601). D.H. is supported by European Union A-ERC grant 291141 CHEMPLAN, NWO, and by a KNAW professor prize awarded to E. van Dishoeck. C.F.M. acknowledges support through the ESO Fellowship. M.T. has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC-2013-ADG. F.M., G.v.d.P., and Y.B. acknowledge funding from ANR of France under contract no. ANR-16-CE31-0013 (Planet-Forming-Disks). D.J. is supported by NRC Canada and by an NSERC Discovery Grant. B.N. and G.L. thank the support by the project PRIN-INAF 2016 The Cradle of Life—GENESIS-SKA (General Conditions in Early Planetary Systems for the rise of life with SKA). Y.L. acknowledges support by the Natural Science Foundation of Jiangsu Province of China (grant no. BK20181513) and by the Natural Science Foundation of China (grant no. 11503087). This paper makes use of the following ALMA data: 2016.1.01164.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Software: Galario (Tazzari et al. 2018 ), emcee (Foreman-Mackey et al. 2013 ), RADMC-3D (Dullemond et al. 2012 ), CASA (v5.1.1; McMullin et al. 2007 ).