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arXiv 2018年

作者： Watts, Anna L. Yu, Wenfei Poutanen, Juri Zhang, Shu Bhattacharyya, Sudip Bogdanov, Slavko Ji, Long Patruno, Alessandro Riley, Thomas E. Bakala, Pavel Baykal, Altan Bernardini, Federico Bombaci, Ignazio Brown, Edward Cavecchi, Yuri Chakrabarty, Deepto Chenevez, Jérôme Degenaar, Nathalie Santo, Melania Del Salvo, Tiziana Di Doroshenko, Victor Falanga, Maurizio Ferdman, Robert D. Feroci, Marco Gambino, Angelo F. Ge, MingYu Greif, Svenja K. Guillot, Sebastien Gungor, Can Hartmann, Dieter H. Hebeler, Kai Heger, Alexander Homan, Jeroen Iaria, Rosario in’t Zand, Jean Kargaltsev, Oleg Kurkela, Aleksi Lai, Xiaoyu Li, Ang Li, XiangDong Li, Zhaosheng Linares, Manuel Lu, FangJun Mahmoodifar, Simin Méndez, Mariano Miller, M. Coleman Morsink, Sharon Nättilä, Joonas Possenti, Andrea Prescod-Weinstein, Chanda Qu, JinLu Riggio, Alessandro Salmi, Tuomo Sanna, Andrea Santangelo, Andrea Schatz, Hendrik Schwenk, Achim Song, LiMing Šrámková, Eva Stappers, Benjamin Stiele, Holger Strohmayer, Tod Tews, Ingo Tolos, Laura Török, Gabriel Tsang, David Urbanec, Martin Vacchi, Andrea Xu, RenXin Xu, Ypeng Zane, Silvia Zhang, Guobao Zhang, ShuangNan Zhang, Wenda Zheng, ShiJie Zhou, Xia Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Shanghai Astronomical Observatory Shanghai200030 China Tuorla Observatory Department of Physics and Astronomy University of Turku Väisäläntie 20 PiikkiöFIN-21500 Finland Nordita KTH Royal Institute of Technology Stockholm University Roslagstullsbacken 23 StockholmSE-10691 Sweden Institute of High Energy Physics CAS Beijing100049 China Tata Institute of Fundamental Research Mumbai400005 India Columbia Astrophysics Laboratory Columbia University 550 West 120th Street New YorkNY10027 United States Institut für Astronomie und Astrophysik Tübingen Universität Tübingen Sand 1 TübingenD-72076 Germany Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands Research Center for Computational Physics and Data Processing Silesian University in Opava Bezrucovo nam. 13 OpavaCZ-74601 Czech Republic Physics Department Middle East Technical University Ankara06531 Turkey INAF Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio CatoneI-00078 Italy New York University Abu Dhabi PO Box 129188 Abu Dhabi United Arab Emirates Dipartimento di Fisica Enrico Fermi University of Pisa PisaI-56127 Italy INFN Italian National Institute for Nuclear Physics Pisa Section Pisa56127 Italy Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Department of Astrophysical Sciences Princeton University Peyton Hall PrincetonNJ08544 United States Mathematical Sciences and STAG Research Centre University of Southampton SouthamptonSO17 1BJ United Kingdom MIT Kavli Institute for Astrophysics and Space Research CambridgeMA02139 United States DTU Space Technical University of Denmark Elektrovej 327-328 Kgs Lyngby2800 Denmark INAF/IASF Palermo via Ugo La Malfa 153 PalermoI-90146 Italy Universita degli Studi di Palermo Dipartimento di Fisica e Chimica via Archira 36 Palermo90123 Italy

In this White Paper we present the potential of the Enhanced X-ray Timing and Polarimetry (eXTP) mission for determining the nature of dense matter;neutron star cores host an extreme density regime which cannot be replicated in a terrestrial laboratory. The tightest statistical constraints on the dense matter equation of state will come from pulse profile modelling of accretion-powered pulsars, burst oscillation sources, and rotation-powered pulsars. Additional constraints will derive from spin measurements, burst spectra, and properties of the accretion flows in the vicinity of the neutron star. Under development by an international Consortium led by the institute of High Energy physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s. Copyright © 2018, The Authors. All rights reserved.

关键词： Pulsars

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accretion in strong field gravity with eXTP

arXiv

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arXiv 2018年

作者： de Rosa, Alessandra Uttley, Phil Gou, Lijun Liu, Yuan Bambi, Cosimo Barret, Didier Belloni, Tomaso Berti, Emanuele Bianchi, Stefano Caiazzo, Ilaria Casella, Piergiorgio Feroci, Marco Ferrari, Valeria Gualtieri, Leonardo Heyl, Jeremy Ingram, Adam Karas, Vladimir Lu, Fangjun Luo, Bin Matt, Giorgio Motta, Sara Neilsen, Joseph Pani, Paolo Santangelo, Andrea Shu, Xinwen Wang, Junfeng Wang, Jian-Min Xue, Yongquan Xu, Yupeng Yuan, Weimin Yuan, Yefei Zhang, Shuang-Nan Zhang, Shu Agudo, Ivan Amati, Lorenzo Andersson, Nils Baglio, Cristina Bakala, Pavel Baykal, Altan Bhattacharyya, Sudip Bombaci, Ignazio Bucciantini, Niccoló Capitanio, Fiamma Ciolfi, Riccardo Cui, Wei K. D’Ammando, Filippo Dauser, Thomas Santo, Melania Del de Marco, Barbara Salvo, Tiziana Di Done, Chris Dovčiak, Michal Fabian, Andrew C. Falanga, Maurizio Gambino, Angelo Francesco Gendre, Bruce Grinberg, Victoria Heger, Alexander Homan, Jeroen Iaria, Rosario Jiang, Jiachen Jin, Chichuan Koerding, Elmar Linares, Manu Liu, Zhu Maccarone, Thomas J. Malzac, Julien Manousakis, Antonios Marin, Frédéric Marinucci, Andrea Mehdipour, Missagh Méndez, Mariano Migliari, Simone Miller, Cole Miniutti, Giovanni Nardini, Emanuele O’Brien, Paul T. Osborne, Julian P. Petrucci, Pierre Olivier Possenti, Andrea Riggio, Alessandro Rodriguez, Jerome Sanna, Andrea Shao, Lijing Sobolewska, Malgosia Sramkova, Eva Stevens, Abigail L. Stiele, Holger Stratta, Giulia Stuchlik, Zdenek Svoboda, Jiri Tamburini, Fabrizio Tauris, Thomas M. Tombesi, Francesco Torok, Gabriel Urbanec, Martin Vincent, Frederic Wu, Qingwen Yuan, Feng in’t Zand, Jean J.M. Zdziarski, Andrzej A. Zhou, Xinlin INAF – Istituto di Astrofisica e Planetologie Spaziali Via Fosso del Cavaliere Rome00133 Italy Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China Institute of High Energy Physics Chinese Academy of Science PO Box 918-3 Beijing100049 China Center for Field Theory and Particle Physics Department of Physics Fudan University 220 Handan Road Shanghai200433 China IRAP Université de Toulouse CNRS UPS CNES Toulouse France INAF – Osservatorio Astronomico di Brera via E. Bianchi 46 Merate23807 Italy Department of Physics and Astronomy University of Mississippi UniversityMS38677 United States Dipartimento di Matematica e Fisica Universitá degli studi Roma Tre Via della Vasca Navale 84 Rome00146 Italy University of British Columbia VancouverBCV6T 1Z1 Canada INAF – Osservatorio Astronomico di Roma Via Frascati 33 Monte Porzio Catone00040 Italy INFN – Roma 2 c/o Dipartimento di Fisica II Universitá di Roma "Tor Vergata" Via della Ricerca Scientifica 1 RomaI-00133 Italy Dipartimento di Fisica Universitá degli Studi di Roma "La Sapienza" Sezione INFN Roma1 Piazzale A. Moro 5 Rome00185 Italy Department of Physics University of Oxford Clarendon Laboratory Parks Road OxfordOX1 3PU United Kingdom Astronomical Institute Academy of Sciences Bovcní II 1401 Prague14131 Czech Republic School of Astronomy and Space Science Nanjing University Nanjing210093 China MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave CambridgeMA02139 United States Department of Physics Anhui Normal University Wuhu Anhui241000 China Department of Astronomy Institute of Theoretical Physics and Astrophysics Xiamen University Xiamen361005 China CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China Glorieta de l

In this paper we describe the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to accretion flows in the strong field gravity regime around both stellar-mass and supermassive black-holes. eXTP has the unique capability of using advanced "spectral-timing-polarimetry" techniques to analyze the rapid variations with three orthogonal diagnostics of the flow and its geometry, yielding unprecedented insight into the inner accreting regions, the effects of strong field gravity on the material within them and the powerful outflows which are driven by the accretion process. Copyright © 2018, The Authors. All rights reserved.

关键词： Polarimeters

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SciPy 1.0—Fundamental algorithms for scientific computing in python

arXiv

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arXiv 2019年

作者： Virtanen, Pauli Gommers, Ralf Oliphant, Travis E. Haberland, Matt Reddy, Tyler Cournapeau, David Burovski, Evgeni Peterson, Pearu Weckesser, Warren Bright, Jonathan van der Walt, Stéfan J. Brett, Matthew Wilson, Joshua Millman, K. Jarrod Mayorov, Nikolay Nelson, Andrew R.J. Jones, Eric Kern, Robert Larson, Eric Carey, C.J. Polat, Ilhan Feng, Yu Moore, Eric W. VanderPlas, Jake Laxalde, Denis Perktold, Josef Cimrman, Robert Henriksen, Ian Quintero, E.A. Harris, Charles R. Archibald, Anne M. Ribeiro, Antônio H. Pedregosa, Fabian van Mulbregt, Paul University of Jyväskylä University of Jyväskylä FI-40014 Finland Quansight LLC AustinTX United States Ultrasound Imaging Mayo Clinic RochesterMN55902 United States Electrical Engineering Brigham Young University ProvoUT84604 United States Enthought Inc. AustinTX78701 United States Anaconda Inc AustinTX78701 United States BioResource and Agricultural Engineering Department California Polytechnic State University San Luis ObispoCA93407 United States Department of Mathematics University of California Los AngelesCA90025 United States Los Alamos National Laboratory Los AlamosNM87544 United States Independent Researcher Higher School of Economics Myasnitskaya 20 Moscow101000 Russia Independent Researcher Saue Estonia Department of Mechanics and Applied Mathematics Institute of Cybernetics Tallinn Technical University Akadeemia Rd 21 Tallinn Estonia Independent Researcher NY United States Berkeley Institute for Data Science University of California BerkeleyCA94720 United States School of Psychology University of Birmingham Edgbaston BirmighamB15 2TT United Kingdom Division of Biostatistics University of California BerkeleyCA94720 United States WayRay LLC Skolkovo Innovation Center Moscow143026 Russia Australian Nuclear Science and Technology Organisation Locked Bag 2001 Kirrawee DCNSW2232 Australia Institute for Learning and Brain Sciences University of Washington SeattleWA98195 United States College of Information and Computing Sciences University of Massachusetts Amherst AmherstMA01002 United States Berkeley Center for Cosmological Physics University of California BerkeleyCA94720 United States Bruker Biospin Corp. 15 Fortune Drive BillericaMA01821 United States University of Washington SeattleWA98195 United States New Technologies - Research Centre University of West Bohemia Univerzitní 8 Plzeň306 14 Czech Republic Oden Institute for Computational Engineering and Sciences University of Texas at Austin AustinTX7

SciPy is an open source scientific computing library for the Python programming language. SciPy 1.0 was released in late 2017, about 16 years after the original version 0.1 release. SciPy has become a de facto standard for leveraging scientific algorithms in the Python programming language, with more than 600 unique code contributors, thousands of dependent packages, over 100,000 dependent repositories, and millions of downloads per year. This includes usage of SciPy in almost half of all machine learning projects on GitHub, and usage by high profile projects including LIGO gravitational wave analysis and creation of the first-ever image of a black hole (M87). The library includes functionality spanning clustering, Fourier transforms, integration, interpolation, file I/O, linear algebra, image processing, orthogonal distance regression, minimization algorithms, signal processing, sparse matrix handling, computational geometry, and statistics. In this work, we provide an overview of the capabilities and development practices of the SciPy library and highlight some recent technical developments. Copyright © 2019, The Authors. All rights reserved.

关键词： Open source software

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Pixel-level APS Sensor Integration and Sensitivity Scaling for Vision Based Speed Measurement

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Procedia Engineering 2016年 168卷 1321-1324页

作者： M. Németh Á. Zarándy P. Földesy Computational Optical Sensing and Processing Laboratory Computer and Research Automation Institute Hungarian Academy of Sciences MTA-SZTAKI Budapest Hungary Faculty of Information Technology Péter Pázmány Catholic University PPKE-ITK Budapest Hungary Institute of Technical Physics and Materials Science Centre for Energy Research – HAS Budapest Hungary

A dual-pixel APS sensor architecture is proposed in this paper, for vision based speed measurement applications, based on a novel double exposure method. The sensor integrates two type of imaging elements on pixel level, and is designed to generate two spatially and temporally coherent images. The primary sensor generates a good quality image for vehicle identification, while the output of the secondary sensor is used to calculate speed estimates, based on the intra-frame displacement of the vehicle's headlight. A scaling process has also been developed for the sensitivity of the secondary sensor, based on photodiode parasitic capacitor discharge time.

关键词： CMOS sensor Quantum efficiency Multi exposure Speed estimation Dual-pixel

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Euclid: On the reduced shear approximation and magnification bias for Stage IV cosmic shear experiments

arXiv

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arXiv 2019年

作者： Deshpande, Anurag C. Kitching, T.D. Cardone, V.F. Taylor, P.L. Casas, S. Camera, S. Carbone, C. Kilbinger, M. Pettorino, V. Sakr, Z. Sapone, D. Tutusaus, I. Auricchio, N. Bodendorf, C. Bonino, D. Brescia, M. Capobianco, V. Carretero, J. Castellano, M. Cavuoti, S. Cledassou, R. Congedo, G. Conversi, L. Corcione, L. Dubath, F. Dusini, S. Fabbian, G. Fumana, M. Garilli, B. Grupp, F. Hoekstra, H. Hormuth, F. Israel, H. Jahnke, K. Kermiche, S. Kubik, B. Kunz, M. Ligori, S. Lilje, P.B. Lloro, I. Maiorano, E. Marggraf, O. Massey, R. Mei, S. Meneghetti, M. Meylan, G. Moscardini, L. Padilla, C. Paltani, S. Pasian, F. Pires, S. Polenta, G. Poncet, M. Raison, F. Rhodes, J. Roncarelli, M. Saglia, R. Schneider, P. Secroun, A. Serrano, S. Sirri, G. Starck, J.L. Sureau, F. Taylor, A.N. Tereno, I. Toledo-Moreo, R. Valenziano, L. Wang, Y. Zoubian, J. Mullard Space Science Laboratory University College London Holmbury St Mary Dorking SurreyRH5 6NT United Kingdom I.N.F.N.-Sezione di Roma Piazzale Aldo Moro 2 - c/o Dipartimento di Fisica Edificio G. Marconi RomaI-00185 Italy INAF-Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio CatoneI-00078 Italy Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States AIM CEA CNRS Université Paris-Saclay Université Paris Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France INFN-Sezione di Torino Via P. Giuria 1 TorinoI-10125 Italy Dipartimento di Fisica Universitá degli Studi di Torino Via P. Giuria 1 TorinoI-10125 Italy I-10025 Italy INFN-Sezione di Milano Via Celoria 16 MilanoI-20133 Italy INAF-IASF Milano Via Alfonso Corti 12 MilanoI-20133 Italy Institut d’Astrophysique de Paris 98bis Boulevard Arago ParisF-75014 France Université St Joseph UR EGFEM Faculty of Sciences Beirut Lebanon Université de Toulouse CNRS UPS CNES 14 Av. Edouard Belin ToulouseF-31400 France Departamento de Física FCFM Universidad de Chile Blanco Encalada 2008 Santiago Chile Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Barcelona08034 Spain INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Piero Gobetti 93/3 BolognaI-40129 Italy Max Planck Institute for Extraterrestrial Physics Giessenbachstr. 1 GarchingD-85748 Germany INAF-Osservatorio Astronomico di Capodimonte Via Moiariello 16 NapoliI-80131 Italy Institut de Física d’Altes Energies IFAE 08193 Bellaterra Barcelona Spain Department of Physics "E. Pancini" University Federico II Via Cinthia 6 NapoliI-80126 Italy INFN section of Naples Via Cinthia 6 NapoliI-80126 Italy Centre National d’Etudes Spatiales Toulouse France Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom ESAC ESA Camino Bajo del Castillo s/n. Urb. Villafranca

Context. Stage IV weak lensing experiments will offer more than an order of magnitude leap in precision. We must therefore ensure that our analyses remain accurate in this new era. Accordingly, previously ignored systematic effects must be addressed. Aims. In this work, we evaluate the impact of the reduced shear approximation and magnification bias, on the information obtained from the angular power spectrum. To first-order, the statistics of reduced shear, a combination of shear and convergence, are taken to be equal to those of shear. However, this approximation can induce a bias in the cosmological parameters that can no longer be neglected. A separate bias arises from the statistics of shear being altered by the preferential selection of galaxies and the dilution of their surface densities, in high-magnification regions. Methods. The corrections for these systematic effects take similar forms, allowing them to be treated together. We calculate the impact of neglecting these effects on the cosmological parameters that would be determined from Euclid, using cosmic shear tomography. We also demonstrate how the reduced shear correction can be calculated using a lognormal field forward modelling approach. Results. These effects cause significant biases in Ωm, ns, σ8, ΩDE, w0, and wa of −0.51σ, −0.36σ, 0.37σ, 1.36σ, −0.66σ, and 1.21σ, respectively. We then show that these lensing biases interact with another systematic: the intrinsic alignment of galaxies. Accordingly, we develop the formalism for an intrinsic alignment-enhanced lensing bias correction. Applying this to Euclid, we find that the additional terms introduced by this correction are sub-dominant. Copyright © 2019, The Authors. All rights reserved.

关键词： Galaxies

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Illuminating Gravitational Waves: A Concordant Picture of Photons from a Neutron Star Merger

arXiv

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arXiv 2017年

作者： Kasliwal, M.M. Nakar, E. Singer, L.P. Kaplan, D.L. Cook, D.O. van Sistine, A. Lau, R.M. Fremling, C. Gottlieb, O. Jencson, J.E. Adams, S.M. Feindt, U. Hotokezaka, K. Ghosh, S. Perley, D.A. Yu, P.-C. Piran, T. Allison, J.R. Anupama, G.C. Balasubramanian, A. Bannister, K.W. Bally, J. Barnes, J. Barway, S. Bellm, E. Bhalerao, V. Bhattacharya, D. Blagorodnova, N. Bloom, J.S. Brady, P.R. Cannella, C. Chatterjee, D. Cenko, S.B. Cobb, B.E. Copperwheat, C. Corsi, A. De, K. Dobie, D. Emery, S.W.K. Evans, P.A. Fox, O.D. Frail, D.A. Frohmaier, C. Goobar, A. Hallinan, G. Harrison, F. Helou, G. Hinderer, T. Ho, A.Y.Q. Horesh, A. Ip, W.-H. Itoh, R. Kasen, D. Kim, H. Kuin, N.P.M. Kupfer, T. Lynch, C. Madsen, K. Mazzali, P.A. Miller, A.A. Mooley, K. Murphy, T. Ngeow, C.-C. Nichols, D. Nissanke, S. Nugent, P. Ofek, E.O. Qi, H. Quimby, R.M. Rosswog, S. Rusu, F. Sadler, E.M. Schmidt, P. Sollerman, J. Steele, I. Williamson, A.R. Xu, Y. Yan, L. Yatsu, Y. Zhang, C. Zhao, W. Division of Physics Math and Astronomy California Institute of Technology 1200 East California Boulevard PasadenaCA91125 United States Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Astroparticle Physics Laboratory NASA Goddard Space Flight Center Joint Space-Science Institute University of Maryland College ParkMD20742 United States Department of Physics University of Wisconsin MilwaukeeWI53201 United States The Oskar Klein Centre Department of Physics Stockholm University AlbaNova StockholmSE-106 91 Sweden Center for Computational Astrophysics Simons Foundation Flatiron Institute 162 5th Ave New YorkNY10010 United States Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Browlow Hill LiverpoolL3 5RF United Kingdom Graduate Institute of Astronomy National Central University No. 300 Zhongda Rd. Zhongli Dist. Taoyuan City32001 Taiwan Racah Institute of Physics The Hebrew University of Jerusalem Jerusalem91904 Israel Sydney Institute for Astronomy School of Physics A28 University of Sydney NSW2006 Australia Indian Institute of Astrophysics II Block Koramangala Bangalore560034 India Indian Institute of Science Education and Research Dr. Homi Bhabha Road Pashan Pune411008 India Australia Telescope National Facility Commonwealth Scientific and Industrial Research Organisation Astronomy and Space Science PO Box 76 EppingNSW1710 Australia University of Colorado Boulder United States Columbia Astrophysics Laboratory Columbia University New YorkNY10027 United States P.O. Box 9 Observatory Cape Town7935 South Africa Department of Astronomy University of Washington SeattleWA98195 United States Department of Physics Indian Institute of Technology Bombay Mumbai400076 India Inter-University Centre for Astronomy and Astrophysics P O Ba 4 Ganeskhind Pune411007 India Department of Astronomy University of California BerkeleyCA94720-

Merging neutron stars offer an exquisite laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart (EM170817) to gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic dataset, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma-rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultra-relativistic jets. Instead, we suggest that breakout of a wide-angle, mildly-relativistic cocoon engulfing the jet elegantly explains the low-luminosity gamma-rays, the high-luminosity ultraviolet-optical-infrared and the delayed radio/X-ray emission. We posit that all merging neutron stars may lead to a wide-angle cocoon breakout;sometimes accompanied by a successful jet and sometimes a choked jet. Copyright © 2017, The Authors. All rights reserved.

关键词： Merging

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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SUPPL 1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 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 University of Aberdeen Aberdeen Scotland UK Department of Integrativ

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Planck 2018 results. I. Overview, and the cosmological legacy of Planck

arXiv

引用

arXiv 2018年

作者： Akrami, Y. Arroja, F. Ashdown, M. Aumont, J. Baccigalupi, C. Ballardini, M. Banday, A.J. Barreiro, R.B. Bartolo, N. Basak, S. Battye, R. Benabed, K. Bernard, J.-P. Bersanelli, M. Bielewicz, P. Bock, J.J. Bond, J.R. Borrill, J. Bouchet, F.R. Boulanger, F. Bucher, M. Burigana, C. Butler, R.C. Calabrese, E. Cardoso, J.-F. Carron, J. Casaponsa, B. Challinor, A. Chiang, H.C. Colombo, L.P.L. Combet, C. Contreras, D. Crill, B.P. Cuttaia, F. de Bernardis, P. de Zotti, G. Delabrouille, J. Delouis, J.-M. Désert, F.-X. Di Valentino, E. Dickinson, C. Diego, J.M. Donzelli, S. Doré, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Enßlin, T.A. Eriksen, H.K. Falgarone, E. Fantaye, Y. Fergusson, J. Fernandez-Cobos, R. Finelli, F. Forastieri, F. Frailis, M. Franceschi, E. Frolov, A. Galeotta, S. Galli, S. Ganga, K. Génova-Santos, R.T. Gerbino, M. Ghosh, T. González-Nuevo, J. Górski, K.M. Gratton, S. Gruppuso, A. Gudmundsson, J.E. Hamann, J. Handley, W. Hansen, F.K. Helou, G. Herranz, D. Hivon, E. Huang, Z. Jaffe, A.H. Jones, W.C. Karakci, A. Keihänen, E. Keskitalo, R. Kiiveri, K. Kim, J. Kisner, T.S. Knox, L. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J.-M. Langer, M. Lasenby, A. Lattanzi, M. Lawrence, C.R. Le Jeune, M. Leahy, J.P. Lesgourgues, J. Levrier, F. Lewis, A. Liguori, M. Lilje, P.B. Lilley, M. Lindholm, V. López-Caniego, M. Lubin, P.M. Ma, Y.-Z. Macías-Pérez, J.F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Marcos-Caballero, A. Maris, M. Martin, P.G. Martínez-González, E. Matarrese, S. Mauri, N. McEwen, J.D. Meerburg, P.D. Meinhold, P.R. Melchiorri, A. Mennella, A. Migliaccio, M. Millea, M. Mitra, S. Miville-Deschênes, M.-A. Molinari, D. Moneti, A. Montier, L. Morgante, G. Moss, A. Mottet, S. Münchmeyer, M. Natoli, P. Nørgaard-Nielsen, H.U. Oxborrow, C.A. Pagano, L. Paoletti, D. Partridge, B. Patanchon, G. Pearson, T.J. Peel, M. Peiris, H.V. AIM CEA CNRS Université Paris-Saclay Gif sur YvetteF-91191 France AIM Université Paris Diderot Sorbonne Paris Cité Gif sur YvetteF-91191 France APC AstroParticule et Cosmologie Université Paris Diderot CNRS IN2P3 CEA Lrfu Observatoire de Paris Sorbonne Paris Cité 10 rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France African Institute for Mathematical Sciences 6-8 Melrose Road Muizenberg Cape Town South Africa Aix Marseille Univ CNRS CNES LAM Marseille France Astrophysics Group Cavendish Laboratory University of Cambridge J J Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Private Bag X54001 Durban4000 South Africa CITA University of Toronto 60 St. George St. TorontoONM5S 3H8 Canada CNRS IRAP 9 Av. colonel Roche BP 44346 Toulouse Cedex 4F-31028 France Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91125 United States California Institute of Technology PasadenaCA United States Centre for Theoretical Cosmology DAMTP University of Cambridge Wilberforce Road CambridgeCB3 0WA United Kingdom Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA United States DTU Space National Space Institute Technical University of Denmark Elektrovej 327 Kgs. LyngbyDK-2800 Denmark Département de Physique Théorique Université de Genève 24 Quai E. Ansermet Genève 41211 Switzerland La Laguna TenerifeE-38206 Spain Departamento de Física Universidad de Oviedo C/ Federico García Lorca 18 Oviedo Spain Departamento de Física Matematica Instituto de Física Universidade de São Paulo Rua do Matão 1371 São Paulo Brazil Department of Astrophysics IMAPP Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of General Education National Institute of Technology Kagawa College 355 Chokushi-cho Takamatsu Kagawa76

The European Space Agency's Planck satellite, which was dedicated to studying the early Universe and its subsequent evolution, was launched on 14 May 2009. It scanned the microwave and submillimetre sky continuously between 12 August 2009 and 23 October 2013, producing deep, high-resolution, all-sky maps in nine frequency bands from 30 to 857 GHz. This paper presents the cosmological legacy of Planck, which currently provides our strongest constraints on the parameters of the standard cosmological model and some of the tightest limits available on deviations from that model. The 6-parameter ΛCDM model continues to provide an excellent fit to the cosmic microwave background data at high and low redshift, describing the cosmological information in over a billion map pixels with just six parameters. With 18 peaks in the temperature and polarization angular power spectra constrained well, Planck measures five of the six parameters to better than 1 % (simultaneously), with the best-determined parameter (θ∗) now known to 0.03 %. We describe the multi-component sky as seen by Planck, the success of the ΛCDM model, and the connection to lower-redshift probes of structure formation. We also give a comprehensive summary of the major changes introduced in this 2018 release. The Planck data, alone and in combination with other probes, provide stringent constraints on our models of the early Universe and the large-scale structure within which all astrophysical objects form and evolve. We discuss some lessons learned from the Planck mission, and highlight areas ripe for further experimental advances. Copyright © 2018, The Authors. All rights reserved.

关键词： Cosmology

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Planck 2018 results. XII. Galactic astrophysics using polarized dust emission

arXiv

引用

arXiv 2018年

作者： Aghanim, N. Akrami, Y. Alves, M.I.R. Ashdown, M. Aumont, J. Baccigalupi, C. Ballardini, M. Banday, A.J. Barreiro, R.B. Bartolo, N. Basak, S. Benabed, K. Bernard, J.-P. Bersanelli, M. Bielewicz, P. Bock, J.J. Bond, J.R. Borrill, J. Bouchet, F.R. Boulanger, F. Bracco, A. Bucher, M. Burigana, C. Calabrese, E. Cardoso, J.-F. Carron, J. Chary, R.-R. Chiang, H.C. Colombo, L.P.L. Combet, C. Crill, B.P. Cuttaia, F. de Bernardis, P. de Zotti, G. Delabrouille, J. Delouis, J.-M. Di Valentino, E. Dickinson, C. Diego, J.M. Doré, O. Douspis, M. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Enßlin, T.A. Eriksen, H.K. Falgarone, E. Fantaye, Y. Fernandez-Cobos, R. Ferrière, K. Finelli, F. Forastieri, F. Frailis, M. Fraisse, A.A. Franceschi, E. Frolov, A. Galeotta, S. Galli, S. Ganga, K. Génova-Santos, R.T. Gerbino, M. Ghosh, T. González-Nuevo, J. Górski, K.M. Gratton, S. Green, G. Gruppuso, A. Gudmundsson, J.E. Guillet, V. Handley, W. Hansen, F.K. Helou, G. Herranz, D. Hivon, E. Huang, Z. Jaffe, A.H. Jones, W.C. Keihänen, E. Keskitalo, R. Kiiveri, K. Kim, J. Krachmalnicoff, N. Kunz, M. Kurki-Suonio, H. Lagache, G. Lamarre, J.-M. Lasenby, A. Lattanzi, M. Lawrence, C.R. Le Jeune, M. Levrier, F. Liguori, M. Lilje, P.B. Lindholm, V. López-Caniego, M. Lubin, P.M. Ma, Y.-Z. Macías-Pérez, J.F. Maggio, G. Maino, D. Mandolesi, N. Mangilli, A. Marcos-Caballero, A. Maris, M. Martin, P.G. Martínez-González, E. Matarrese, S. Mauri, N. McEwen, J.D. Melchiorri, A. Mennella, A. Migliaccio, M. Miville-Deschênes, M.-A. Molinari, D. Moneti, A. Montier, L. Morgante, G. Moss, A. Natoli, P. Pagano, L. Paoletti, D. Patanchon, G. Perrotta, F. Pettorino, V. Piacentini, F. Polastri, L. Polenta, G. Puget, J.-L. Rachen, J.P. Reinecke, M. Remazeilles, M. Renzi, A. Ristorcelli, I. Rocha, G. Rosset, C. Roudier, G. Rubiño-Martín, J.A. Ruiz-Granados, B. Salvati, L. Sandri, M. Savelainen, M. Scott, D. Sirignano, C. AIM CEA CNRS Université Paris-Saclay Université Paris-Diderot Sorbonne Paris Cité Gif-sur-YvetteF-91191 France APC AstroParticule et Cosmologie Université Paris Diderot CNRS IN2P3 CEA Lrfu Observatoire de Paris Sorbonne Paris Cité 10 rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France African Institute for Mathematical Sciences 6-8 Melrose Road Muizenberg Cape Town South Africa Aix Marseille Univ CNRS CNES LAM Marseille France Astrophysics Group Cavendish Laboratory University of Cambridge J J Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics & Cosmology Research Unit School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Westville Campus Private Bag X54001 Durban4000 South Africa CITA University of Toronto 60 St. George St. TorontoONM5S 3H8 Canada CNRS IRAP 9 Av. colonel Roche BP 44346 Toulouse Cedex 4F-31028 France Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91125 United States California Institute of Technology PasadenaCA United States Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA United States Département de Physique Théorique Université de Genève 24 Quai E. Ansermet Genève 41211 Switzerland Département de Physique École Normale Supérieure PSL Research University CNRS 24 rue Lhomond Paris75005 France La Laguna TenerifeE-38206 Spain Departamento de Física Universidad de Oviedo C/ Federico García Lorca 18 Oviedo Spain Department of Astrophysics IMAPP Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of Mathematics University of Stellenbosch Stellenbosch7602 South Africa Department of Physics & Astronomy University of British Columbia 6224 Agricultural Road VancouverBC Canada Department of Physics & Astronomy University of the Western Cape Cape Town7535 South Africa Department of Physics and Astronomy University of Sussex BrightonBN1 9QH United Kingdom Depar

Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle ψ, and dispersion function of polarization angles S. The joint distribution (one-point statistics) of p and NH confirms that the mean and maximum polarization fractions decrease with increasing NH. The uncertainty on the maximum observed polarization fraction, pmax = 22.0+−31..54 % at 353 GHz and 800 resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and S found earlier is seen to be present at high latitudes. This follows the S ∝ p−1 relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, ψ, and S for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map S × p, looking for residual trends. While the polarization fraction p decreases by a factor of 3-4 between NH = 1020 cm−2 and NH = 2 × 1022 cm−2, out of the Galactic plane, this product S × p only decreases by about 25 %. Because S is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with NH is determined mostly by the magnetic-field stru

关键词： Polarization

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Supernovae 2016bdu and 2005gl, and their link with SN 2009ip-like transients: another piece of the puzzle

arXiv

引用

arXiv 2017年

作者： Pastorello, A. Kochanek, C.S. Fraser, M. Dong, S. Elias-Rosa, N. Benetti, S. Cappellaro, E. Tomasella, L. Drake, A.J. Hermanen, J. Reynolds, T. Shappee, B.J. Smartt, S.J. Chambers, K.C. Huber, M.E. Smith, K. Stanek, K.Z. Filippenko, A.V. Christensen, E.J. Denneau, L. Djorgovski, S.G. Flewelling, H. Gall, C. Gal-Yam, A. Geier, S. Heinze, A. Holoien, T.W.-S. Isern, J. Kangas, T. Kankare, E. Koff, R.A. Llapasset, J.-M. Lowe, T.B. Lundqvist, P. Magnier, E.A. Mattila, S. Morales-Garoffolo, A. Mutel, R. Nicolas, J. Ochner, P. Ofek, E.O. Prosperi, E. Rest, A. Sano, Y. Stalder, B. Stritzinger, M.D. Taddia, F. Terreran, G. Tonry, J.L. Wainscoat, R.J. Waters, C. Weiland, H. Willman, M. Young, D.R. Zheng, W. INAF-Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Department of Astronomy Ohio State University 140 West 18th Avenue ColumbusOH43210 United States Ohio State University 191 W. Woodruff Ave. ColumbusOH43210 United States School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Royal Society – Science Foundation Ireland University Research Fellow Kavli Institute for Astronomy and Astrophysics Peking University Yi He Yuan Road 5 Hai Dian District Beijing100871 China Astronomy Department California Institute of Technology PasadenaCA91125 United States Tuorla Observatory Department of Physics and Astronomy University of Turku Väisäläntie 20 PiikkiöFI-21500 Finland Nordic Optical Telescope Apartado 474 Santa Cruz de La PalmaE-38700 Spain Carnegie Observatories 813 Santa Barbara Street PasadenaCA91101 United States Hubble Fellow and Carnegie-Princeton Fellow Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast BelfastBT7 1NN United Kingdom Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Lunar and Planetary Lab Department of Planetary Sciences University of Arizona TucsonAZ85721 United States Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Maries Vej 30 Copenhagen2100 Denmark Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Department of Particle Physics and Astrophysics Faculty of Physics Weizmann Institute of Science Rehovot76100 Israel Cuesta de San José s/n Breña Baja La PalmaE-38712 Spain Instituto de Astrofísica de Canarias Vía Láctea s/n La Laguna TenerifeE-38200 Spain US Department of Energy Computatio

Supernova (SN) 2016bdu is an unusual transient resembling SN 2009ip. SN 2009ip-like events are characterized by a long-lasting phase of erratic variability which ends with two luminous outbursts a few weeks apart. The second outburst is significantly more luminous (about 3 mag) than the first. In the case of SN 2016bdu, the first outburst (Event A) reached an absolute magnitude Mr ≈ −15.3 mag, while the second one (Event B) occurred over one month later and reached Mr ≈ −18 mag. By inspecting archival data, a faint source at the position of SN 2016bdu is detectable several times in the past few years. We interpret these detections as signatures of a phase of erratic variability, similar to that experienced by SN 2009ip between 2008 and mid-2012, and resembling the currently observed variability of the luminous blue variable SN 2000ch in NGC 3432. Spectroscopic monitoring of SN 2016bdu during the second peak initially shows features typical of a SN IIn. One month after the Event B maximum, the spectra develop broad Balmer lines with P Cygni profiles and broad metal features. At these late phases, the spectra resemble those of a typical Type II SN. All members of this SN 2009ip-like group are remarkably similar to the Type IIn SN 2005gl. For this object, the claim of a terminal SN explosion is supported by the disappearance of the progenitor star. The similarity with SN 2005gl suggests that all members of this family may finally explode as genuine SNe, although the unequivocal detection of nucleosynthesised elements in their nebular spectra is still missing. Copyright © 2017, The Authors. All rights reserved.

关键词： Supernovae

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