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arXiv 2020年

作者： Buckley, David A.H. Bagnulo, S. Britto, R.J. Mao, J. Kann, D.A. Cooper, J. Lipunov, V. Hewitt, D.M. Razzaque, S. Kuin, N.P.M. Monageng, I.M. Covino, S. Jakobsson, P. van der Horst, A.J. Wiersema, K. Böttcher, M. Campana, S. D'Elia, V. Gorbovskoy, E.S. Gorbunov, I. Groenewald, D.N. Hartmann, D.H. Kornilov, V.G. Mundell, C.G. Podesta, R. Thomas, J.K. Tyurina, N. Vlasenko, D. van Soelen, B. Xu, D. South African Astronomical Observatory PO Box 9 Observatory Road Observatory Cape Town7935 South Africa Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa Armagh Observatory & Planetarium College Hill ArmaghBT61 9DG United Kingdom Department of Physics University of the Free State PO Box 339 Bloemfontein9300 South Africa Yunnan Observatories Chinese Academy of Sciences Yunnan Province Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Glorieta de la Astronomía s/n Granada18008 Spain M. V. Lomonosov Moscow State University SAI Physics Department 13 Univeristetskij pr-t Moscow119991 Russia M.V.Lomonosov Moscow State University Physics Department Leninskie gory GSP-1 Moscow119991 Russia Department of Physics University of Johannesburg PO Box 524 Auckland Park2006 South Africa Mullard Space Science Laboratory Dept. of Space and Climate Sciences University College London Holmbury St Mary DorkingRH5 6NT United Kingdom I-23807 Italy Centre for Astrophysics and Cosmology Science Institute University of Iceland Dunhagi 5 Reykjavík107 Iceland Department of Physics The George Washington University 725 21st St. NW WashingtonDC20052 United States The George Washington University WashingtonDC20052 United States Department of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Department of Physics and Astronomy University of Leicester LE1 7RH United Kingdom Centre for Space Research North West University Potchefstroom South Africa ASI-Space Science Data Center via del Politecnico snc Rome00133 Italy INAF - Osservatorio Astronomico di Roma via Frascati 33 Monte Porzio Catone00040 Italy Southern African Large Telescope Foundation PO Box 9 Observatory Road Obse

We report on results of spectropolarimetry of the afterglow of the long gamma-ray burst GRB 191221B, obtained with SALT/RSS and VLT/FORS2, as well as photometry from two telescopes in the MASTER Global Robotic network, at the MASTER-SAAO (South Africa) and MASTER-OAFA (Argentina) stations. Prompt optical emission was detected by MASTER-SAAO 38 s after the alert, which dimmed from a magnitude (white-light) of ∼ 10 to 16.2 mag over a period of ∼10 ks, followed by a plateau phase lasting ∼10 ks and then a decline to ∼18 mag after 80 ks. The light curve shows complex structure, with four or five distinct breaks in the power-law decline rate. SALT/RSS linear spectropolarimetry of the afterglow began ∼ 2.9 h after the burst, during the early part of the plateau phase of the light curve. Absorption lines seen at ∼ 6010 Å and 5490 Å are identified with the Mg II 2799 Å line from the host galaxy at z = 1.15 and an intervening system located at z = 0.96. The mean linear polarisation measured over 3400 − 8000 Å was ∼1.5% and the mean equatorial position angle (θ) ∼65◦. VLT/FORS2 spectropolarimetry was obtained ∼ 10 h postburst, during a period of slow decline (α = −0.44), and the polarisation was measured to be p = 1.2% and θ = 60◦. Two observations with the MeerKAT radio telescope, taken 30 and 444 days after the GRB trigger, detected radio emission from the host galaxy only. We interpret the light curve and polarisation of this long GRB in terms of a slow-cooling forward-shock. Copyright © 2020, The Authors. All rights reserved.

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A new, faint population of X-ray transients

arXiv

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arXiv 2017年

作者： Bauer, Franz E. Treister, Ezequiel Schawinski, Kevin Schulze, Steve Luo, Bin Alexander, David M. Brandt, William N. Comastri, Andrea Forster, Francisco Gilli, Roberto Kann, David Alexander Maeda, Keiichi Nomoto, Kenichi Paolillo, Maurizio Ranalli, Piero Schneider, Donald P. Shemmer, Ohad Tanaka, Masaomi Tolstov, Alexey Tominaga, Nozomu Tozzi, Paolo Vignali, Cristian Wang, Junxian Xue, Yongquan Yang, Guang Instituto de Astrofísica Facultad de Física Pontificia Universidad Católica de Chile 306 Santiago 22 Chile Nuncio Monseñor Sótero Sanz 100 Providencia Santiago Chile Space Science Institute 4750 Walnut Street Suite 205 BoulderCO80301 United States EMBIGGEN Anillo Concepción Chile Departamento de Astronomía Universidad de Concepción Casilla 160-C Concepción Chile Institute for Astronomy Department of Physics ETH Zurich Wolfgang-Pauli-Strasse 27 ZurichCH-8093 Switzerland School of Astronomy and Space Science Nanjing University Nanjing210093 China Ministry of Education Nanjing210093 China Department of Physics Durham University DurhamDH1 3LE United Kingdom Department of Astronomy and Astrophysics Pennsylvania State University 525 Davey Lab University ParkPA16802 United States Institute for Gravitation and the Cosmos Pennsylvania State University University ParkPA16802 United States Department of Physics 104 Davey Laboratory Pennsylvania State University University ParkPA16802 United States INAF-Osservatorio Astronomico di Bologna via Ranzani 1 Bologna40127 Italy Centro de Modelamiento Matemático Universidad de Chile Av. Blanco Encalada 2120 Piso 7 Santiago Chile Thüringer Landessternwarte Tautenburg Sternwarte 5 Tautenburg07778 Germany Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan University of Tokyo KashiwaChiba277-8583 Japan Hamamatsu Department of Physics University Federico II via Cintia 9 Naples80126 Italy INFN - Sezione di Napoli via Cinthia 9 Naples80126 Italy Agenzia Spaziale Italiana Science Data Center via del Politecnico snc Roma00133 Italy Lund Observatory Department of Astronomy and Theoretical Physics Lund University Box 43 Lund22100 Sweden Department of Physics University of North Texas DentonTX76203 National Astronomical Observatory of Japan Mitaka Tokyo181-8588 Japan Department of Physics Faculty of Science and Engineering Konan University 8-

We report on the detection of a remarkable new fast high-energy transient found in the Chandra Deep Field-South, robustly associated with a faint (mR = 27.5 mag, zph∼2.2) host in the CANDELS survey. The X-ray event is comprised of 115+−1211 net 0.3–7.0 keV counts, with a light curve characterised by a ≈100 s rise time, a peak 0.3–10 keV flux of ≈5×10−12 erg s−1 cm−2, and a power-law decay time slope of −1.53 ± 0.27. The average spectral slope is Γ = 1.43+−00..2313, with no clear spectral variations. The X-ray and multi-wavelength properties effectively rule out the vast majority of previously observed high-energy transients. A few theoretical possibilities remain: an "orphan" X-ray afterglow from an off-axis short-duration Gamma-ray Burst (GRB) with weak optical emission;a low-luminosity GRB at high redshift with no prompt emission below ∼20 keV rest-frame;or a highly beamed Tidal Disruption Event (TDE) involving an intermediate-mass black hole and a white dwarf with little variability. However, none of the above scenarios can completely explain all observed properties. Although large uncertainties exist, the implied rate of such events is comparable to those of orphan and low-luminosity GRBs as well as rare TDEs, implying the discovery of an untapped regime for a known transient class, or a new type of variable phenomena whose nature remains to be determined. Copyright © 2017, The Authors. All rights reserved.

关键词： Luminance

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A global overview of marine heatwaves in a changing climate (vol 5, 701, 2024)

COMMUNICATIONS EARTH & ENVIRONMENT

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COMMUNICATIONS EARTH & ENVIRONMENT 2024年第1期5卷 701页

作者： Capotondi, Antonietta Rodrigues, Regina R. Sen Gupta, Alex Benthuysen, Jessica A. Deser, Clara Froelicher, Thomas L. Lovenduski, Nicole S. Amaya, Dillon J. Le Grix, Natacha Xu, Tongtong Hermes, Juliet Holbrook, Neil J. Martinez-Villalobos, Cristian Masina, Simona Roxy, Mathew Koll Schaeffer, Amandine Schlegel, Robert W. Smith, Kathryn E. Wang, Chunzai University of Colorado Boulder Cooperative Institute for Research in Environmental Sciences Boulder USA (GRID:grid.266190.a) (ISNI:***) NOAA/Physical Sciences Laboratory Boulder USA (GRID:grid.511342.0) Federal University of Santa Catarina Florianópolis Brazil (GRID:grid.411237.2) (ISNI:0000 0001 2188 7235) University of New South Wales Climate Change Research Centre and Centre for Marine Science and Innovation Sydney Australia (GRID:grid.1005.4) (ISNI:0000 0004 4902 0432) University of New South Wales Australian Research Council Centre of Excellence for Climate Extremes Sydney Australia (GRID:grid.1005.4) (ISNI:0000 0004 4902 0432) Australian Institute of Marine Science Crawley Australia (GRID:grid.1046.3) (ISNI:0000 0001 0328 1619) National Center for Atmospheric Research Climate and Global Dynamics Laboratory Boulder USA (GRID:grid.57828.30) (ISNI:0000 0004 0637 9680) University of Bern Climate and Environmental Physics Physics Institute Bern Switzerland (GRID:grid.5734.5) (ISNI:0000 0001 0726 5157) University of Bern Oeschger Centre for Climate Change Research Bern Switzerland (GRID:grid.5734.5) (ISNI:0000 0001 0726 5157) University of Colorado Boulder Department of Atmospheric and Oceanic Sciences and Institute of Arctic and Alpine Research Boulder USA (GRID:grid.266190.a) (ISNI:***) NOAA/Physical Sciences Laboratory Boulder USA (GRID:grid.511342.0) South African Environmental Observation Network Cape Town South Africa (GRID:grid.507758.8) (ISNI:0000 0004 0499 441X) University of Tasmania Institute for Marine and Antarctic Studies Hobart Australia (GRID:grid.1009.8) (ISNI:0000 0004 1936 826X) University of Tasmania ARC Centre of Excellence for Climate Extremes Hobart Australia (GRID:grid.1009.8) (ISNI:0000 0004 1936 826X) Universidad Adolfo Ibáñez Faculty of Engineering and Science Santiago Chile (GRID:grid.440617.0) (ISNI:0000 0001 2162 5606) ANID Technology Center No. DO210001 Data Observatory Foundation Santiago Chile (GRID:grid.440617.0) CMCC Foundation—Euro-M

Marine heatwaves have profoundly impacted marine ecosystems over large areas of the world oceans, calling for improved understanding of their dynamics and predictability. Here, we critically review the recent substantial advances in this active area of research, including the exploration of the three-dimensional structure and evolution of these extremes, their drivers, their connection with other extremes in the ocean and over land, future projections, and assessment of their predictability and current prediction skill. To make progress on predicting and projecting marine heatwaves and their impacts, a more complete mechanistic understanding of these extremes over the full ocean depth and at the relevant spatial and temporal scales is needed, together with models that can realistically capture the leading mechanisms at those scales. Sustained observing systems, as well as measuring platforms that can be rapidly deployed, are essential to achieve comprehensive event characterizations while also chronicling the evolving nature of these extremes and their impacts in our changing *** understanding of marine heatwave predictability and impacts requires analysis of these extremes at full ocean depth, using models and observations capturing their key drivers at the relevant scales, according to a broad literature review.

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The fraction of ionizing radiation from massive stars that escapes to the intergalactic medium

arXiv

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arXiv 2018年

作者： Tanvir, N.R. Fynbo, J.P.U. de Ugarte Postigo, A. Japelj, J. Wiersema, K. Malesani, D. Perley, D.A. Levan, A.J. Selsing, J. Cenko, S.B. Kann, D.A. Milvang-Jensen, B. Berger, E. Cano, Z. Chornock, R. Covino, S. Cucchiara, A. D'Elia, V. Goldoni, P. Gomboc, A. Heintz, K.E. Hjorth, J. Izzo, L. Jakobsson, P. Kaper, L. Krühler, T. Laskar, T. Myers, M. Piranomonte, S. Pugliese, G. Sánchez-Ramírez, R. Schulze, S. Sparre, M. Stanway, E.R. Tagliaferri, G. Thöne, C.C. Vergani, S. Vreeswijk, P.M. Wijers, R.A.M.J. Watson, D. Xu, D. University of Leicester Department of Physics & Astronomy Leicester Institute of Space & Earth Observation University Road LeicesterLE1 7RH United Kingdom Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Maries Vej 30 Copenhagen Ø2100 Denmark Glorieta de la Astronomía s/n GranadaE-18008 Spain Astronomical Institute Anton Pannekoek University of Amsterdam PO Box 94249 Amsterdam1090 GE Netherlands Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Department of Physics University of Warwick CoventryCV4 7AL United Kingdom Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States NASA's Goddard Space Flight Center GreenbeltMD20771 United States Joint Space-Science Institute University of Maryland College ParkMD20742 United States Astrophysical Institute Department of Physics and Astronomy Ohio University AthensOH45701 United States INAF Osservatorio Astronomico di Brera Via Bianchi 46 Merate23807 Italy University of the Virgin Islands College of Science and Mathematics USVI #2 Brewers Bay Road Charlotte Amalie00802 I-00040 00078 Italy ASI-Science Data Centre Via del Politecnico snc RomeI-00133 Italy APC Astroparticule et Cosmologie Université Paris Diderot CNRS IN2P3 CEA Irfu Observatoire de Paris Sorbonne Paris Cité 10 Rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France Centre for Astrophysics and Cosmology University of Nova Gorica Vipavska 11c Ajdovščina5270 Slovenia Centre for Astrophysics and Cosmology Science Institute University of Iceland Dunhagi 5 Reykjavík107 Iceland Max-Planck-Institut für Extraterrestrische Physik Giessenbachstrasse Garching85748 Germany National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Department of Astronomy University of California 501 Campbell Hall BerkeleyCA94720-3411 United Stat

The part played by stars in the ionization of the intergalactic medium (IGM) remains an open question. A key issue is the proportion of the stellar ionizing radiation that escapes the galaxies in which it is produced. Spectroscopy of gamma-ray burst (GRB) afterglows can be used to determine the neutral hydrogen column-density, NH i, in their host galaxies and hence the opacity to extreme ultra-violet (EUV) radiation along the lines-of-sight to the bursts. Thus, making the reasonable assumption that long-duration GRB locations are representative of the sites of massive stars that dominate EUV production, one can calculate an average escape fraction of ionizing radiation in a way that is independent of galaxy size, luminosity or underlying spectrum. Here we present a sample of NH i measures for 138 GRBs in the range 1.6 esci ≈ 0.005, with a 98% confidence upper limit of h fesci ≈ 0.015. This analysis suggests that stars provide a small contribution to the ionizing radiation budget of the IGM at z 5, firm conclusions are limited by the small size of the GRB sample (7/138), but any decline in average H i column-density seems to be modest. We also find no indication of a significant correlation of NH i with galaxy UV luminosity or host stellar mass, for the subset of events for which these are available. We discuss in some detail a number of selection effects and potential biases. Drawing on a range of evidence we argue that such effects, while not negligible, are unlikely to produce systematic errors (in either direction) of more than a factor ∼ 2 in fesc, and so would not affect the primary conclusions. Given that many GRB hosts are low metallicity, high specific star-formation rate, dwarf galaxies, these results present a particular problem for the hypothesis that such galaxies dominated the reionization of the universe. Copyright © 2018, The Authors. All rights reserved.

关键词： Stars

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26th Annual Computational Neuroscience Meeting (CNS*2017): Part 3 Antwerp, Belgium. 15-20 July 2017 Abstracts

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BMC NEUROscience 2017年第Sup1期18卷 95-176页

作者： [Anonymous] Department of Neuroscience Yale University New Haven CT 06520 USA Department Physiology & Pharmacology SUNY Downstate Brooklyn NY 11203 USA NYU School of Engineering 6 MetroTech Center Brooklyn NY 11201 USA Kings County Hospital Center Brooklyn NY 11203 USA Departament de Matemàtica Aplicada Universitat Politècnica de Catalunya Barcelona 08028 Spain Institut de Neurobiologie de la Méditerrannée (INMED) INSERM UMR901 Aix-Marseille Univ Marseille France Center of Neural Science New York University New York NY USA Aix-Marseille Univ INSERM INS Inst Neurosci Syst Marseille France Laboratoire de Physique Théorique et Modélisation CNRS UMR 8089 Université de Cergy-Pontoise 95300 Cergy-Pontoise Cedex France Department of Mathematics and Computer Science ENSAT Abdelmalek Essaadi’s University Tangier Morocco Laboratory of Natural Computation Department of Information and Electrical Engineering and Applied Mathematics University of Salerno 84084 Fisciano SA Italy Department of Medicine University of Salerno 84083 Lancusi SA Italy Dipartimento di Fisica Università degli Studi Aldo Moro Bari and INFN Sezione Di Bari Italy Data Analysis Department Ghent University Ghent Belgium Coma Science Group University of Liège Liège Belgium Cruces Hospital and Ikerbasque Research Center Bilbao Spain BIOtech Department of Industrial Engineering University of Trento and IRCS-PAT FBK 38010 Trento Italy Department of Data Analysis Ghent University Ghent 9000 Belgium The Wellcome Trust Centre for Neuroimaging University College London London WC1N 3BG UK Department of Electronic Engineering NED University of Engineering and Technology Karachi Pakistan Blue Brain Project École Polytechnique Fédérale de Lausanne Lausanne Switzerland Departement of Mathematics Swansea University Swansea Wales UK Laboratory for Topology and Neuroscience at the Brain Mind Institute École polytechnique fédérale de Lausanne Lausanne Switzerland Institute of Mathematics

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Evidence of jet activity from the secondary black hole in the OJ287 binary system

arXiv

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arXiv 2024年

作者： Valtonen, Mauri J. Zola, Staszek Gupta, Alok C. Kishore, Shubham Gopakumar, Achamveedu Jorstad, Svetlana G. Wiita, Paul J. Gu, Minfeng Nilsson, Kari Marscher, Alan P. Zhang, Zhongli Hudec, Rene Matsumoto, Katsura Drozdz, Marek Ogloza, Waldemar Berdyugin, Andrei V. Reichart, Daniel E. Mugrauer, Markus Dey, Lankeswar Pursimo, Tapio Lehto, Harry J. Ciprini, Stefano Nakaoka, T. Uemura, M. Imazawa, Ryo Zejmo, Michal Kouprianov, Vladimir V. Davidson, James W. Sadun, Alberto Štrobl, Jan Weaver, Z.R. Jelínek, Martin FINCA University of Turku TurkuFI-20014 Finland Tuorla Observatory Department of Physics and Astronomy University of Turku TurkuFI-20014 Finland Astronomical Observatory Jagiellonian University ul. Orla 171 Krakow30-244 Poland Manora Peak Nainital263001 India Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Department of Astronomy and Astrophysics Tata Institute of Fundamental Research Mumbai400005 India Institute for Astrophysical Research Boston University 725 Commonwealth Avenue BostonMA02215 United States Department of Physics The College of New Jersey 2000 Pennington Rd. EwingNJ08628-0718 United States Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Key Laboratory of Radio Astronomy and Technology Chinese Academy of Sciences A20 Datun Road Chaoyang District Beijing100101 China Faculty of Electrical Engineering Czech Technical University Prague166 36 Czech Republic Astronomical Institute ASU CAS Ondřejov251 65 Czech Republic Astronomical Institute Osaka Kyoiku University 4-698 Asahigaoka Kashiwara Osaka582-8582 Japan Mt. Suhora Astronomical Observatory University of the National Education Commission ul.Podchorazych 2 Krakow30-084 Poland Department of Physics and Astronomy University of North Carolina at Chapel Hill Chapel HillNC27599 United States Astrophysical Institute University Observatory Schillergässchen 2 JenaD-07745 Germany Department of Physics and Astronomy West Virginia University PO Box 135 Willey Street MorgantownWV26506 United States Nordic Optical Telescope Apartado 474 Santa Cruz de La PalmaE-38700 Spain Istituto Nazionale di Fisica Nucleare Sezione di Roma "Tor Vergata" RomaI-00133 Italy Space Science Data Center - Agenzia Spaziale Italiana Via del Politecnico snc RomaI-00133 Italy Hiroshima Astrophysical Science Center Hiroshima University 1-3-1 Kagamiyam

We report the study of a huge optical intraday flare on November 12, 2021, at 2 am UT, in the blazar OJ 287. In the binary black hole model it is associated with an impact of the secondary black hole on the accretion disk of the primary. Our multifrequency observing campaign was set up to search for such a signature of the impact, based on a prediction made eight years earlier. The first I-band results of the flare have already been reported by Kishore et al. (2024). Here we combine these data with our monitoring in the R-band. There is a big change in the R-I spectral index by 1.0 ± 0.1 between the normal background and the flare, suggesting a new component of radiation. The polarization variation during the rise of the flare suggests the same. The limits on the source size place it most reasonably in the jet of the secondary black hole. We then ask why we have not seen this phenomenon before. We show that OJ 287 was never before observed with sufficient sensitivity on the night when the flare should have happened according to the binary model. We also study the probability that this flare is just an oversized example of intraday variability, using the Krakow-dataset of intense monitoring between 2015 and 2023. We find that the occurrence of a flare of this size and rapidity is unlikely. In the Appendix, we give the full orbit-linked historical light curve of OJ 287 as well as the dense monitoring sample of Krakow. Copyright © 2024, The Authors. All rights reserved.

关键词： Active Galactic Nuclei

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GRB190114C in the nuclear region of an interacting galaxy? A detailed host analysis using ALMA, HST and VLT

arXiv

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arXiv 2019年

作者： Postigo, A. De Ugarte Thöne, C.C. Martín, S. Japelj, J. Levan, A.J. Micha³owski, M.J. Selsing, J. Kann, D.A. Schulze, S. Palmerio, J.T. Vergani, S.D. Tanvir, N.R. Bensch, K. Covino, S. D'Elia, V. Pasquale, M. De Fruchter, A.S. Fynbo, J.P.U. Hartmann, D. Heintz, K.E. Horst, A. J. Vander Izzo, L. Jakobsson, P. Ng, K.C.Y. Perley, D.A. Rossi, A. Sbarufatti, B. Salvaterra, R. Sánchez-Ramírez, R. Watson, D. Xu, D. Instituto de Astrofisica de Andalucia Glorieta de la Astronomia s/n Granada18008 Spain DARK Niels Bohr Institute University of Copenhagen Lyngbyvej 2 CopenhagenDK-2100 Denmark European Southern Alonso de Cordova 3107 Vitacura Santiago763-0355 Joint ALMA Observatory Alonso de Cordova 3107 Vitacura Santiag763-0355 Chile Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 Amsterdam1098 Netherlands Department of Astrophysics IMAPP Radboud University Nijmegen Netherlands Department of Physics University OfWarwick CoventryCV47AL United Kingdom Astronomical Observatory Institute Faculty of Physics Adam Mickiewicz University ul. S.oneczna 36 Pozna-Ln60-286 Cosmic Dawn Center Niels Bohr Institute University of Copenhagen Lyngbyvej 2 CopenhagenDK-2100 Denmark Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot7610001 Israel GEPI Observatoire de Paris PSL University CNRS 5 Place Jules Janssen MeudonF-92190 Institut D-fAstrophysique de Paris Sorbonne Universite CNRS ParisF-75014 France Department of Physics and Astronomy University of Leicester LE17RH United Kingdom INAF-Osservatorio Astronomico di Brera via E. Bianchi 46 MerateI-23807 Italy ASI-Space Science Data Centre Via del Politecnico snc RomeI-00133 Italy INAF-Osservatorio Astronomico di Roma Via Frascati 33 Monte Porzio CatoneI-00040 Italy Department of Astronomy and Space Sciences Istanbul University Beyazt Istanbul34119 Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Physics and Astronomy Clemson University ClemsonSC29634 United States Centre for Astrophysics and Cosmology Science Institute University of Iceland Dunhagi 5 Reykjavik107 Department of Physics George Washington University 725 21st Street NW WashingtonDC20052 United States Department of Astronomy Physics Statistics Institute of Sciences George Washington University WashingtonDC20052 Uni

Context. GRB190114C is the first GRB for which the detection of very-high energy emission up to the TeV range has been reported. It is still unclear whether environmental properties might have contributed to the production of these very high-energy photons, or if it is solely related to the released GRB emission. Aims. The relatively low redshift of the GRB (z = 0:425) allows us to study the host galaxy of this event in detail, and to potentially identify idiosyncrasies that could point to progenitor characteristics or environmental properties responsible for such a unique event. Methods. We use ultraviolet, optical, infrared and submillimetre imaging and spectroscopy obtained with HST, VLT and ALMA to obtain an extensive dataset on which the analysis of the host galaxy is based. Results. The host system is composed of a close pair of interacting galaxies (Δv=50 km s-1), both of which are well-detected by ALMA in CO(3-2). The GRB occurred within the nuclear region (-170 pc from the centre) of the less massive but more starforming galaxy of the pair. The host is more massive (log(M/Mo)=9.3) than average GRB hosts at that redshift and the location of the GRB is rather unique. The enhanced star-formation rate was probably triggered by tidal interactions between the two galaxies. Our ALMA observations indicate that both host galaxy and companion have a high molecular gas fraction, as has been observed before in interacting galaxy pairs. Conclusions. The location of the GRB within the core of an interacting galaxy with an extinguished line-of-sight is indicative of a denser environment than typically observed for GRBs and could have been crucial for the generation of the very-high-energy photons that were observed. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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Research and development of the back-end electronics for the two-dimensional improved resistive plate chambers in CMS upgrade

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Radiation Detection technology and Methods 2021年第2期5卷 181-191页

作者： P.Cao Z-A.Liu J.Zhao H.Kou J.Tao J.Song W.Gong N.Wang A.Samalan M.Tytgat N.Zaganidis G.A.Alves F.Marujo F.Torres.Da.S.ilva.De.Araujo E.M.Da Costa D.De Jesus Damiao H.Nogima A.Santoro S.Fonseca De Souza A.Aleksandrov R.Hadjiiska P.Iaydjiev M.Rodozov M.Shopova G.Sultanov M.Bonchev A.Dimitrov L.Litov B.Pavlov P.Petkov A.Petrov S.J.Qian C.Bernal A.Cabrera J.Fraga A.Sarkar S.Elsayed Y.Assran M.El Sawy M.A.Mahmoud Y.Mohammed X.Chen C.Combaret M.Gouzevitch G.Grenier I.Laktineh L.Mirabito K.Shchablo I.Bagaturia D.Lomidze I.Lomidze V.Bhatnagar R.Gupta P.Kumari J.Singh V.Amoozegar B.Boghrati M.Ebraimi R.Ghasemi M.Mohammadi Najafabadi E.Zareian M.Abbrescia R.Aly W.Elmetenawee N.De Filippis A.Gelmi G.Iaselli S.Leszki F.Loddo I.Margjeka G.Pugliese D.Ramos L.Benussi S.Bianco D.Piccolo S.Buontempo A.Di Crescenzo F.Fienga G.De Lellis L.Lista S.Meola P.Paolucci A.Braghieri P.Salvini P.Montagna C.Riccardi P.Vitulo B.Francois T.J.Kim J.Park S.Y.Choi B.Hong K.S.Lee J.Goh H.Lee J.Eysermans C.Uribe Estrada I.Pedraza H.castilla-Valdez A.Sanchez-Hernandez C.A.Mondragon Herrera D.A.Perez Navarro G.A.Ayala Sanchez S.Carrillo E.Vazquez A.Radi A.Ahmad I.Asghar H.Hoorani S.Muhammad M.A.Shah I.Crotty Department of Physics and Astronomy Ghent UniversityProeftuinstraat 869000 GhentBelgium Centro Brasileiro Pesquisas Fisicas R.Dr.Xavier Sigaud150-UrcaRio de JaneiroRJ 22290-180Brazil Dep.de Fisica Nuclear e Altas Energias Instituto de FisicaUniversidade do Estado do Rio de JaneiroRua Sao Francisco Xavier524BR-Rio de Janeiro 20559-900RJBrazil Bulgarian Academy of Sciences Inst.for Nucl.Res.and Nucl.EnergyTzarigradsko shaussee Boulevard 721784 SofiaBulgaria Faculty of Physics University of Sofia5 James Bourchier Boulevard1164 SofiaBulgaria School of Physics Peking UniversityBeijing 100871China Institute of High Energy Physics UCAS/CAS19(B)Yuquan RoadShijingshan DistrictBeijing 100049China Universidad de Los Andes Apartado Aereo 4976Carrera 1Eno.18A 10BogotaCOColombia Egyptian Network for High Energy Physics Academy of Scientific Research and Technology101 Kasr El-Einy St.CairoEgypt The British University in Egypt(BUE) P.O.Box 43Elsherouk CitySuez Desert RoadCairo 11837Egypt Suez University Elsalam CitySuez-Cairo RoadSuez 43522Egypt Department of Physics Faculty of ScienceBeni-Suef UniversityBeni-SuefEgypt Center for High Energy Physics Faculty of ScienceFayoum UniversityEl-Fayoum 63514Egypt Univ Lyon Univ Claude Bernard Lyon 1CNRS/IN2P3IP2I LyonUMR 582269622 VilleurbanneFrance Georgian Technical University 77 Kostava Str.Tbilisi 0175Georgia Department of Physics Panjab UniversityChandigarh 160014India School of Particles and Accelerators Institute for Research in Fundamental Sciences(IPM)P.O.Box 19395-5531TehranIran School of Engineering Damghan UniversityDamghan ***Iran INFN Sezione di BariVia Orabona 470126 BariItaly INFN Laboratori Nazionali di Frascati(LNF)Via Enrico Fermi 4000044 FrascatiItaly INFN Sezione di NapoliComplesso Univ.Monte S.AngeloVia Cintia80126 NaplesItaly INFN Sezione di PaviaVia Bassi 6PaviaItaly INFN Sezione di Pavia and University of PaviaVia Bassi 6PaviaItaly Hanyang University 222 Wangsimni-roSageun-dongSeongdong

Purpose To complement and ensure redundancy in the endcap muon system of the Compact Muon Solenoid(CMS)detector and to extend the Resistive Plate Chamber(RPC)system coverage,improved RPCs(iRPCs)with either orthogonal layer strips with one-end electronics or single layer strips with two-end electronics providing more precise time measurement will be installed in the very forward pseudorapidity region of|η|<*** iRPC readout system needs to support twodimensional(2D)or two-end *** addition,it must combine detector data with Timing,Trigger and fast Control(TTC)and Slow Control(SC)into one data stream over a bi-directional optical link with a line rate of 4.8 Gb/s between the Front-End Electronics(FEE)and the Back-End Electronics(BEE).To fulfill these requirements,a prototype BEE for the iRPC 2D chamber has been researched and *** A Micro-Telecommunication and Computing Architecture(μTCA)-based processing card was designed in this study to establish a prototype system together with aμTCA *** Giga-Bit Transceiver(GBT)protocol is integrated to provide bi-directional communication between the FEE and BEE.A server is connected with the BEE by a Gigabit Ethernet(GbE)link for SC and a 10-GbE link for data AcQuisition(DAQ).Results The Bit Error Rate(BER)test of the back-end board and a joint test with the iRPC 2D prototype chamber were *** less than 1.331×10−16 was *** timemeasurement with a resolution of 3.05 nswas successfully realized,and detector efficiencies of 97.7%for longitudinal strips and 96.0%for orthogonal strips were *** results demonstrate the correctness and reliability of the prototype *** The BEE prototype satisfies the requirements for the iRPC 2D chamber,and it worked stably and reliably during a long-term joint test run.

关键词： CMS iRPC TTC SC BEE μTCA GBT DAQ

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The Prime Focus Spectrograph Galaxy Evolution Survey

arXiv

引用

arXiv 2022年

作者： Greene, Jenny E. Bezanson, Rachel Ouchi, Masami Silverman, John Arnouts, Stéphane Goulding, Andy D. Gu, Meng Gunn, James E. Harikane, Yuichi Heckman, Timothy Horowitz, Benjamin Johnson, Sean D. Kashino, Daichi Lee, Khee-Gan Leja, Joel Lin, Yen-Ting Marchesini, Danilo Matsuoka, Yoshiki Nagamine, Kentaro Ono, Yoshiaki Pearl, Alan Shibuya, Takatoshi Strauss, Michael A. Strom, Allison L. Sugahara, Yuma Tresse, Laurence Yabe, Kiyoto Yamashita, Takuji Akiyama, Masayuki Ata, Metin Azevedo, Gabriel M. Chen, Chian-Chou Chies-Santos, Ana L. Ellis, Richard S. Hahn, Changhoon Roier, Gabriel Roberto Hauschild Ichikawa, Kohei Ito, Kei Jiang, Linhua Jing, Y.P. Kawamuro, Taiki Kobayashi, Chiaki Kraljic, Katarina Le Brun, Vincent Liu, Xin Melchior, Peter Mendes De Oliveira, Claudia L. Monteiro-Oliveira, Rogério Nagao, Tohru Onodera, Masato Overzier, Roderik A. Schiminovich, David Schramm, Malte Shimakawa, Rhythm Sodré, Laerte Storchi-Bergmann, Thaisa Suzuki, Tomoko L. Tanaka, Masayuki Toba, Yoshiki Umehata, Hideki Wang, Jiaqi Welker, Charlotte Whitaker, Katherine Xu, Kun Xue, Yongquan Yang, Xiaohu Zu, Ying Department of Astrophysical Sciences Princeton University Princeton NJ08544 United States Department of Physics and Astronomy University of Pittsburgh PittsburghPA15260 United States Institute for Cosmic Ray Research The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8582 Japan The University of Tokyo 5-1-5 Kashiwanoha Chiba Kashiwa277-8583 Japan Department of Astronomy School of Science The University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Aix Marseille University CNRS CNES LAM Marseille France Johns Hopkins University United States University of Michigan United States Institute for Advanced Research Nagoya University Nagoya464-8601 Japan Division of Particle and Astrophysical Science Graduate School of Science Nagoya University Nagoya464-8602 Japan Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Institute of Astronomy and Astrophysics Academia Sinica Taiwan Tufts University United States Research Center for Space and Cosmic Evolution Ehime University Japan Theoretical Astrophysics Department of Earth & Space Science Graduate School of Science Osaka University 1-1 Machikaneyama Osaka Toyonaka560-0043 Japan Department of Physics & Astronomy University of Nevada Las Vegas 4505 S. Maryland Pkwy Las VegasNV89154-4002 United States Kitami Institute of Technology 165 Koen-cho Hokkaido Kitami090-8507 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan Astronomical Institute Tohoku University Japan Av. Bento Gonçalves RS Porto Alegre9500

We present the Prime Focus Spectrograph (PFS) Galaxy Evolution pillar of the 360-night PFS Subaru Strategic Program. This 130-night program will capitalize on the wide wavelength coverage and massive multiplexing capabilities of PFS to study the evolution of typical galaxies from cosmic dawn to the present. From Lyman α emitters at z ∼ 7 to probe reionization, drop-outs at z ∼ 3 to map the inter-galactic medium in absorption, and a continuum-selected sample at z ∼ 1.5, we will chart the physics of galaxy evolution within the evolving cosmic web. This article is dedicated to the memory of Olivier Le Fevre, who was an early advocate for the construction of PFS, and a key early member of the Galaxy Evolution Working Group. © 2022, CC BY.

关键词： Spectrographs

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The XMM-SERVS survey: XMM-Newton point-source catalogs for the W-CDF-S and ELAIS-S1 fields

arXiv

引用

arXiv 2021年

作者： Ni, Qingling Brandt, W.N. Chen, Chien-Ting Luo, Bin Nyland, Kristina Yang, Guang Zou, Fan Aird, James Alexander, David M. Bauer, Franz Erik Lacy, Mark Lehmer, Bret D. Mallick, Labani Salvato, Mara Schneider, Donald P. Tozzi, Paolo Traulsen, Iris Vaccari, Mattia Vignali, Cristian Vito, Fabio Xue, Yongquan Banerji, Manda Chow, Kate Comastri, Andrea Moro, Agnese Del Gilli, Roberto Mullaney, James Paolillo, Maurizio Schwope, Axel Shemmer, Ohad Sun, Mouyuan Timlin, John D. Trump, Jonathan R. Department of Astronomy and Astrophysics 525 Davey Lab The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Physics 104 Davey Laboratory The Pennsylvania State University University ParkPA16802 United States Marshall Space Flight Center HuntsvilleAL35811 United States School of Astronomy and Space Science Nanjing University Jiangsu Nanjing210093 China Key Laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education Jiangsu Nanjing210093 China National Research Council The U.S. Naval Research Laboratory 4555 Overlook Ave. SW WashingtonDC20375 United States Department of Physics and Astronomy Texas A&M University College StationTX77843-4242 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University College StationTX77843-4242 United States Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom Centre for Extragalactic Astronomy Department of Physics Durham University DurhamDH1 3LE United Kingdom Instituto de Astrofísica and Centro de Astroingeniería Facultad de Física Pontificia Universidad Católica de Chile Casilla 306 Santiago 22 Chile Millennium Institute of Astrophysics Nuncio Monseñor Sótero Sanz 100 of 104 Providencia Santiago Chile Space Science Institute 4750 Walnut Street Suite 205 BoulderCO80301 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Department of Physics University of Arkansas 226 Physics Building 825 West Dickson Street FayettevilleAR72701 United States Indian Institute of Astrophysics Block II Koramangala Bangalore560034 India MPE Giessenbachstrasse 1 Garching85748 Germany INAF Osservatorio Astrofisico di Firenze Largo Enrico Fermi 5 FirenzeI-50125 Italy An der Ster

We present the X-ray point-source catalogs in two of the XMM-Spitzer Extragalactic Representative Volume Survey (XMM-SERVS) fields, W-CDF-S (4.6 deg2) and ELAIS-S1 (3.2 deg2), aiming to fill the gap between deep pencil-beam X-ray surveys and shallow X-ray surveys over large areas. The W-CDF-S and ELAIS-S1 regions were targeted with 2.3 Ms and 1.0 Ms of XMM-Newton observations, respectively;1.8 Ms and 0.9 Ms exposures remain after flare filtering. The survey in W-CDF-S has a flux limit of 1.0 × 10−14 erg cm−2 s−1 over 90% of its area in the 0.5-10 keV band;4053 sources are detected in total. The survey in ELAIS-S1 has a flux limit of 1.3 × 10−14 erg cm−2 s−1 over 90% of its area in the 0.5-10 keV band;2630 sources are detected in total. Reliable optical-to-IR multiwavelength counterpart candidates are identified for ≈ 89% of the sources in W-CDF-S and ≈ 87% of the sources in ELAIS-S1. 3186 sources in W-CDF-S and 1985 sources in ELAIS-S1 are classified as AGNs. We also provide photometric redshifts for X-ray sources;≈ 84% of the 3319/2001 sources in W-CDF-S/ELAIS-S1 with optical-to-NIR forced photometry available have either spectroscopic redshifts or high-quality photometric redshifts. The completion of the XMM-Newton observations in the W-CDF-S and ELAIS-S1 fields marks the end of the XMM-SERVS survey data gathering. The ≈ 12,000 point-like X-ray sources detected in the whole ≈ 13 deg2 XMM-SERVS survey will benefit future large-sample AGN studies. Copyright © 2021, The Authors. All rights reserved.

关键词： Surveys

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