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arXiv 2023年

作者： Blanton, Michael R. Evans, Janet D. Norman, Dara O'Mullane, William Price-Whelan, Adrian Rizzi, Luca Accomazzi, Alberto Ansdell, Megan Bailey, Stephen Barrett, Paul Berukoff, Steven Bolton, Adam Borrill, Julian Cruz, Kelle Dalcanton, Julianne Desai, Vandana Dubois-Felsmann, Gregory P. Economou, Frossie Ferguson, Henry Field, Bryan Foreman-Mackey, Dan Forero-Romero, Jaime Gaffney, Niall Gillies, Kim Graham, Matthew J. Gwyn, Steven Hennawi, Joseph Hughes, Anna L.H. Jaffe, Tess Jagannathan, Preshanth Jenness, Tim Jurić, Mario Kavelaars, J.J. Kee, Kerk Kern, Jeff Kremin, Anthony Labrie, Kathleen Lacy, Mark Law, Casey Martínez-Galarza, Rafael McCully, Curtis McEnery, Julie Miller, Bryan Moriarty, Christopher Muench, August Muna, Demitri Murillo, Angela Narayan, Gautham Neill, James D. Nikutta, Robert Ojha, Roopesh Olsen, Knut O'Meara, John Rusholme, Ben Seaman, Robert Starkman, Nathaniel Still, Martin Stoehr, Felix Swinbank, John D. Teuben, Peter Toledo, Ignacio Tollerud, Erik Turk, Matthew D. Turner, James Vacca, William Vieira, Joaquin Weaver, Benjamin Weiner, Benjamin Weiss, Jason Westfall, Kyle Willman, Beth Zhao, Lily Center for Cosmology & Particle Physics New York University 726 Broadway New York10003 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States NSF's National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Rubin Observatory Project Office 950 N. Cherry Ave. TucsonAZ85719 United States Center for Computational Astrophysics Flatiron Institute 162 Fifth Ave New YorkNY10010 United States National Science Foundation 2415 Eisenhower Avenue AlexandriaVA22314 United States National Aeronautics and Space Administration Goddard Space Flight Center GreenbeltMD United States Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States US Naval Observatory Flagstaff Station 10391 Naval Observatory Road FlagstaffAZ86001 United States City University of New York Hunter College Hunter North Building 695 Park Ave. New YorkNY10065 United States IPAC California Institute of Technology MS 100-22 PasadenaCA91125 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Office of Science U.S. Department of Energy 1000 Independence Ave. SW WashingtonDC20585 United States Universidad de los Andes Cra 1 Num. 18A - 12 Bogotá Colombia Texas Advanced Computing Center The University of Texas Austin United States TMT International Observatory United States Astronomy Department California Institute of Technology 1200 East California Blvd. PasadenaCA91125 United States National Research Council Canada 5071 West Saanich Road Victoria Canada University of California Santa BarbaraCA93106-9530 United States National Solar Observatory 3665 Discovery Drive BoulderCO80303 United States National Radio Astronomy Observstory 520 Edgemont Road CharlottesvilleVA22903 United States Department of Astronomy The DIRAC Institute University of Washington 3910 15th Avenue NE SeattleWA98195 Unite

The astronomical community is grappling with the increasing volume and complexity of data produced by modern telescopes, due to difficulties in reducing, accessing, analyzing, and combining archives of data. To address this challenge, we propose the establishment of a coordinating body, an "entity," with the specific mission of enhancing the interoperability, archiving, distribution, and production of both astronomical data and software. This report is the culmination of a workshop held in February 2023 on the Future of Astronomical data Infrastructure. Attended by 70 scientists and software professionals from ground-based and space-based missions and archives spanning the entire spectrum of astronomical research, the group deliberated on the prevailing state of software and data infrastructure in astronomy, identified pressing issues, and explored potential solutions. In this report, we describe the ecosystem of astronomical data, its existing flaws, and the many gaps, duplication, inconsistencies, barriers to access, drags on productivity, missed opportunities, and risks to the long-term integrity of essential data sets. We also highlight the successes and failures in a set of deep dives into several different illustrative components of the ecosystem, included as an appendix. The report also puts forth a roadmap for the development of the proposed coordination entity, offering four potential structural models for consideration. Alongside, we present preliminary case studies scrutinizing their associated costs, advantages, disadvantages, and risks. We advocate for the establishment of a Steering Committee, bolstered by support from federal funding agencies, to take the lead in defining the entity's scope, requirements, and structural framework. This committee should actively engage with and solicit feedback from the broader astronomical community and the expert cadre specializing in astronomical data, culminating in the formulation of an actionable implementation p

关键词： Ecosystems

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The Spectacular Ultraviolet Flash From the Peculiar Type Ia Supernova 2019yvq

arXiv

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arXiv 2020年

作者： Miller, Adam A. Magee, M.R. Polin, A. Maguire, K. Zimmerman, E. Yao, Y. Sollerman, J. Schulze, S. Perley, D.A. Kromer, M. Bulla, M. Andreoni, I. Bellm, E.C. De, K. Dekany, R. Delacroix, A. Dhawan, S. Fremling, C. Gal-Yam, A. Goldstein, D.A. Golkhou, V.Z. Goobar, A. Graham, M.J. Irani, I. Kasliwal, M.M. Kaye, S. Kim, Y.-L. Laher, R.R. Mahabal, A.A. Masci, F.J. Nugent, P.E. Ofek, E. Phinney, E.S. Prentice, S.J. Riddle, R. Rigault, M. Rusholme, B. Schweyer, T. Shupe, D.L. Soumagnac, M.T. Walters, R. Yan, L. Zolkower, J. Kulkarni, S.R. Terreran, G. Department of Physics and Astronomy Northwestern University 1800 Sherman Road EvanstonIL60201 United States Adler Planetarium ChicagoIL60605 United States School of Physics Trinity College Dublin University of Dublin Dublin 2 Ireland Departments of Physics and Astronomy University of California Berkeley BerkleyCA94720 United States Department of Particle Physics and Astrophysics Weizmann Institute of Science 234 Herzl St Rehovot76100 Israel Cahill Center for Astrophysics California Institute of Technology 1200 E. California Boulevard PasadenaCA91125 United States Department of Astronomy Oskar Klein Center Stockholm University AlbaNova StockholmSE-10691 Sweden Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Heidelberger Institut für Theoretische Studien Schloss-Wolfsbrunnenweg 35 Heidelberg69118 Germany Nordita KTH Royal Institute of Technology Stockholm University Roslagstullsbacken 23 StockholmSE-106 91 Sweden DIRAC Institute Department of Astronomy University of Washington 3910 15th Avenue NE SeattleWA98195 United States Caltech Optical Observatories California Institute of Technology PasadenaCA91125 United States Oskar Klein Centre Department of Physics Stockholm University AlbaNova StockholmSE-10691 Sweden eScience Institute University of Washington SeattleWA98195 United States Université de Lyon Univ. Claude Bernard Lyon 1 CNRS/IN2P3 IP2I Lyon VilleurbanneF-69622 France IPAC California Institute of Technology 1200 E. California Blvd PasadenaCA91125 United States Center for Data Driven Discovery California Institute of Technology PasadenaCA91125 United States Computational Cosmology Center Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Université Clermont Auvergne CNRS/IN2P3 Laboratoire de Physique de Clermont Clermont-FerrandF-63000 France Lawrence Berkeley National Laborator

Early observations of Type Ia supernovae (SNe Ia) provide essential clues for understanding the progenitor system that gave rise to the terminal thermonuclear explosion. We present exquisite observations of SN 2019yvq, the second observed SN Ia, after iPTF 14atg, to display an early flash of emission in the ultraviolet (UV) and optical. Our analysis finds that SN 2019yvq was unusual, even when ignoring the initial flash, in that it was moderately underluminous for a SN Ia (Mg ≈ −18.5 mag at peak) yet featured very high absorption velocities (v ≈ 15, 000 km s−1 for Si II λ6355 at peak). We find that many of the observational features of SN 2019yvq, aside from the flash, can be explained if the explosive yield of radioactive 56Ni is relatively low (we measure M56Ni = 0.31 ± 0.05 M☉) and it and other iron-group elements are concentrated in the innermost layers of the ejecta. To explain both the UV/optical flash and peak properties of SN 2019yvq we consider four different models: interaction between the SN ejecta and a nondegenerate companion, extended clumps of 56Ni in the outer ejecta, a double-detonation explosion, and the violent merger of two white dwarfs. Each of these models has shortcomings when compared to the observations;it is clear additional tuning is required to better match SN 2019yvq. In closing, we predict that the nebular spectra of SN 2019yvq will feature either H or He emission, if the ejecta collided with a companion, strong [Ca II] emission, if it was a double detonation, or narrow [O I] emission, if it was due to a violent merger. Copyright © 2020, The Authors. All rights reserved.

关键词： Merging

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New limit for neutrinoless double-beta decay of 100Mo from the CUPID-Mo experiment

arXiv

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arXiv 2020年

作者： Armengaud, E. Augier, C. Barabash, A.S. Bellini, F. Benato, G. Benoît, A. Beretta, M. Bergé, L. Billard, J. Borovlev, Y.A. Bourgeois, C. Brudanin, V.B. Camus, P. Cardani, L. Casali, N. Cazes, A. Chapellier, M. Charlieux, F. Chiesa, D. de Combarieu, M. Dafinei, I. Danevich, F.A. de Jesus, M. Dixon, T. Dumoulin, L. Eitel, K. Ferri, F. Fujikawa, B.K. Gascon, J. Gironi, L. Giuliani, Andrea Grigorieva, V.D. Gros, M. Guerard, E. Helis, D.L. Huang, H.Z. Huang, R. Johnston, J. Juillard, A. Khalife, H. Kleifges, M. Kobychev, V.V. Kolomensky, Y.G. Konovalov, S.I. Leder, A. Loaiza, P. Ma, L. Makarov, E.P. de Marcillac, P. Mariam, R. Marini, L. Marnieros, S. Misiak, D. Navick, X.-F. Nones, C. Norman, E.B. Novati, V. Olivieri, E. Ouellet, J.L. Pagnanini, L. Pari, P. Pattavina, L. Paul, B. Pavan, M. Peng, H. Pessina, G. Pirro, S. Poda, D.V. Polischuk, O.G. Pozzi, S. Previtali, E. Redon, T. Rojas, A. Rozov, S. Rusconi, C. Sanglard, V. Scarpaci, J.A. Schäffner, K. Schmidt, B. Shen, Y. Shlegel, V.N. Siebenborn, B. Singh, V. Tomei, C. Tretyak, V.I. Umatov, V.I. Vagneron, L. Velázquez, M. Welliver, B. Winslow, L. Xue, M. Yakushev, E. Zarytskyy, M. Zolotarova, A.S. IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France Univ. Lyon Université Lyon 1 CNRS IN2P3 IP2I-Lyon VilleurbanneF-69622 France National Research Centre Kurchatov Institute Institute of Theoretical and Experimental Physics Moscow117218 Russia Dipartimento di Fisica Sapienza Università di Roma P.le Aldo Moro 2 RomeI-00185 Italy INFN Sezione di Roma P.le Aldo Moro 2 RomeI-00185 Italy I-67100 Italy CNRS-Néel Grenoble Cedex 938042 France University of California BerkeleyCA94720 United States Université Paris-Saclay CNRS IN2P3 IJCLab Orsay91405 France Nikolaev Institute of Inorganic Chemistry Novosibirsk630090 Russia Laboratory of Nuclear Problems JINR Moscow region Dubna141980 Russia Dipartimento di Fisica Università di Milano-Bicocca MilanoI-20126 Italy INFN Sezione di Milano-Bicocca MilanoI-20126 Italy IRAMIS CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France Institute for Nuclear Research of NASU Kyiv03028 Ukraine Karlsruhe Institute of Technology Institute for Astroparticle Physics Karlsruhe76021 Germany Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Fudan University Shanghai200433 China Massachusetts Institute of Technology CambridgeMA02139 United States Karlsruhe Institute of Technology Institute for Data Processing and Electronics Karlsruhe76021 Germany INFN Gran Sasso Science Institute L’AquilaI-67100 Italy Physik Department Technische Universität München GarchingD-85748 Germany Department of Modern Physics University of Science and Technology of China Hefei230027 China LSM Laboratoire Souterrain de Modane Modane73500 France Department of Physics and Astronomy University of South Carolina ColumbiaSC29208 United States Université Grenoble Alpes CNRS Grenoble INP SIMAP Saint Martin d’Héres38402 France

The CUPID-Mo experiment at the Laboratoire Souterrain de Modane (France) is a demonstrator for CUPID, the next-generation ton-scale bolometric 0νββ experiment. It consists of a 4.2 kg array of 20 enriched Li2100MoO4 scintillating bolometers to search for the lepton number violating process of 0νββ decay in 100Mo. With more than one year of operation (100Mo exposure of 1.17 kg×yr for physics data), no event in the region of interest and hence no evidence for 0νββ is observed. We report a new limit on the half-life of 0νββ decay in 100Mo of T1/2 > 1.5 × 1024 yr at 90% C.I. The limit corresponds to an effective Majorana neutrino mass hmββi © 2020, CC BY.

关键词： Neutrons

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The INTEGRAL view of the pulsating hard X-ray sky: From accreting and transitional millisecond pulsars to rotation-powered pulsars and magnetars

arXiv

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arXiv 2020年

作者： Papitto, A. Falanga, M. Hermsen, W. Mereghetti, S. Kuiper, L. Poutanen, J. Bozzo, E. Ambrosino, F. Coti Zelati, F. de Falco, V. de Martino, D. Di Salvo, T. Esposito, P. Ferrigno, C. Forot, M. Götz, D. Gouiffes, C. Iaria, R. Laurent, P. Li, J. Li, Z. Mineo, T. Moran, P. Neronov, A. Paizis, A. Rea, N. Riggio, A. Sanna, A. Savchenko, V. Slowikowska, A. Shearer, A. Tiengo, A. Torres, D.F. INAF-Osservatorio Astronomico di Roma via Frascati 33 Monte Porzio CatoneI-00078 Italy Hallerstrasse 6 BernCH-3012 Switzerland SRON Netherlands Institute for Space Research Sorbonnelaan 2 UtrechtNL-3584 CA Netherlands Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 AmsterdamNL-1098 XH Netherlands INAF Istituto di Astrofisica Spaziale e Fisica Cosmica Via A. Corti 12 MilanoI-20133 Italy Tuorla Observatory Department of Physics and Astronomy 20014 University of Turku Finland Space Research Institute of Russian Academy of Sciences Profsoyuznaya str. 84/32 Moscow117997 Russia Nordita KTH Royal Institute of Technology Stockholm University Roslagstullsbacken 23 Stockholm10691 Sweden ISDC Department of Astronomy University of Geneva Chemin d’Ecogia 16 Versoix1290 Switzerland Via del Fosso del Cavaliere 100 RomeI-00133 Italy Campus UAB Carrer de Can Magrans BarcelonaE-08193 Spain Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo namesti 13 OpavaCZ-746 01 Czech Republic INAF Osservatorio Astronomico di Capodimonte Salita Moiariello 16 NapoliI-80131 Italy Università degli Studi di Palermo Dipartimento di Fisica e Chimica - Emilio Segré via Archirafi 36 PalermoI-90123 Italy Scuola Universitaria Superiore IUSS Pavia piazza della Vittoria 15 Pavia27100 Italy CEA IRFU Service d’Astrophysique Orme des Merisiers Gif-sur-Yvette91191 France CEA Saclay Bt. 709 Gif-sur-Yvette CedexF-91191 France Deutsches Elektronen Synchrotron DESY ZeuthenD-15738 Germany Department of Physics Xiangtan University Xiangtan411105 China INAF Istituto di Astrofisica Spaziale e Fisica Cosmica Palermo Via U. La Malfa 153 PalermoI-90146 Italy Centre for Astronomy School of Physics National University of Ireland Galway University Road Galway Ireland Astronomy Department University of Geneva Ch. d’Ecogia 16 Versoix1290 Switzerland Dipartime

In the last 25 years, a new generation of X-ray satellites imparted a significant leap forward in our knowledge of X-ray pulsars. The discovery of accreting and transitional millisecond pulsars proved that disk accretion can spin up a neutron star to a very high rotation speed. The detection of MeV-GeV pulsed emission from a few hundreds of rotation-powered pulsars probed particle acceleration in the outer magnetosphere, or even beyond. Also, a population of two dozens of magnetars has emerged. INTEGRAL played a central role to achieve these results by providing instruments with high temporal resolution up to the hard X-ray/soft γ-ray band and a large field of view imager with good angular resolution to spot hard X-ray transients. In this article, we review the main contributions by INTEGRAL to our understanding of the pulsating hard X-ray sky, such as the discovery and characterization of several accreting and transitional millisecond pulsars, the generation of the first catalog of hard X-ray/soft γ-ray rotation-powered pulsars, the detection of polarization in the hard X-ray emission from the Crab pulsar, and the discovery of persistent hard X-ray emission from several magnetars. Copyright © 2020, The Authors. All rights reserved.

关键词： Pulsars

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SARS-CoV-2 evolution during treatment of chronic infection (vol 592, pg 277, 2021)

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NATURE 2022年第7922期608卷 E23-E23页

作者： Kemp, Steven A. Collier, Dami A. Datir, Rawlings P. Ferreira, Isabella A. T. M. Gayed, Salma Jahun, Aminu Hosmillo, Myra Rees-Spear, Chloe Mlcochova, Petra Lumb, Ines Ushiro Roberts, David J. Chandra, Anita Temperton, Nigel Sharrocks, Katherine Blane, Elizabeth Modis, Yorgo Leigh, Kendra E. Briggs, John A. G. van Gils, Marit J. Smith, Kenneth G. C. Bradley, John R. Smith, Chris Doffinger, Rainer Ceron-Gutierrez, Lourdes Barcenas-Morales, Gabriela Pollock, David D. Goldstein, Richard A. Smielewska, Anna Skittrall, Jordan P. Gouliouris, Theodore Goodfellow, Ian G. Gkrania-Klotsas, Effrossyni Illingworth, Christopher J. R. Mccoy, Laura E. Gupta, Ravindra K. Division of Infection and Immunity University College London London UK Cambridge Institute of Therapeutic Immunology & Infectious Disease (CITIID) Cambridge UK Department of Medicine University of Cambridge Cambridge UK Wellcome Sanger Centre Hinxton UK Department of Biomedicine University and University Hospital Basel Basel Switzerland Botnar Research Centre for Child Health (BRCCH) University Basel & ETH Zurich Basel Switzerland MRC Toxicology Unit School of Biological Sciences University of Cambridge Cambridge UK Medical Research Council Laboratory of Molecular Biology Cambridge UK Africa Health Research Institute Durban South Africa Cambridge Clinical Research Centre NIHR Clinical Research Facility Cambridge University Hospitals NHS Foundation Trust Addenbrooke’s Hospital Cambridge UK Heart and Lung Research Institute Cambridge UK Royal Papworth Hospital NHS Foundation Trust Cambridge UK Department of Applied Mathematics and Theoretical Physics University of Cambridge Cambridge UK Department of Haematology University of Cambridge Cambridge UK Department of Infectious Diseases Cambridge University Hospitals NHS Foundation Trust Cambridge UK Department of Microbiology Cambridge University Hospitals NHS Foundation Trust Cambridge UK NIHR Cambridge Bioresource Cambridge UK Department of Infectious Diseases Cambridge University NHS Hospitals Foundation Trust Cambridge UK Clinical Microbiology and Public Health Laboratory Addenbrooke’s Hospital Cambridge UK Department of Pathology University of Cambridge Cambridge UK Division of Virology Department of Pathology University of Cambridge Cambridge UK Department of Virology Cambridge University NHS Hospitals Foundation Trust Cambridge UK NHS Blood and Transplant Oxford and BRC Haematology Theme University of Oxford Oxford UK Viral Pseudotype Unit Medway School of Pharmacy University of Kent Canterbury UK Department of Medical Microbiology Academic Medical Center University of Amsterdam Amsterdam

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Searching for low-redshift faint galaxies with MMT/Hectospec

arXiv

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arXiv 2021年

作者： Cheng, Cheng Huang, Jia-Sheng Willmer, Christopher N.A. Zhang, Hong-Xin Ashby, Matthew L.N. Xu, Hai Sawicki, Marcin Arnouts, Stephane Gwyn, Stephen Desprez, Guillaume Coupon, Jean Golob, Anneya Liang, Piaoran Cao, Tianwen Shi, Yaru Jin, Gaoxiang He, Chuan Wu, Shumei Li, Zijian Sophia Dai, Y. Kevin Xu, C. Shao, Xu Musin, Marat Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China CAS Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Steward Observatory University of Arizona 933 N. Cherry Avenue TucsonAZ85721 United States CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Anhui Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Hefei230026 China Center for Astrophysics Harvard and Smithsonian 60 Garden St CambridgeMA02138 United States Institute for Computational Astrophysics Department of Astronomy and Physics Saint Mary's University 923 Robie Street HalifaxNSB3H 3C3 Canada Aix Marseille Université CNRS Laboratoire d'Astrophysique de Marseille UMR 7326 MarseilleF-13388 France Canadian Astronomy Data Centre NRC-Herzberg 5071 West Saanich Road VictoriaBCV9E 2E7 Canada Department of Astronomy University of Geneva ch. d'Écogia 16 Versoix CH-1290 Switzerland

We present redshifts for 2753 low-redshift galaxies between 0.03 zspec 0.5 with 18 ≤ r ≤ 22 obtained with Hectospec at the Multi-Mirror Telescope (MMT). The observations targeted the XMMLSS, ELAIS-N1 and DEEP2-3 fields, each of which covers ∼ 1 deg2. These fields are also part of the recently completed CFHT Large Area U-band Deep Survey (CLAUDS) and on-going Hyper Suprime-Cam deep fields surveys. The efficiency of our technique for selecting low-redshift galaxies is confirmed by the redshift distribution of our sources. In addition to redshifts, these high S/N spectra are used to measure ages, metallicities, and nuclear activity levels. In combination with the photometric catalogue in u, g, r, i, z, y down to 27 AB mag, we are able to study the galaxy population down to stellar masses of ∼ 108Mo. This paper presents the observational strategy, the reduction procedure and properties of the galaxy sample. © 2021, CC BY.

关键词： Surveys

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Overview of the Medium and High Frequency Telescopes of the LiteBIRD satellite mission

arXiv

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arXiv 2021年

作者： Montier, L. Mot, B. de Bernardis, P. Maffei, B. Pisano, G. Columbro, F. Gudmundsson, J.E. Henrot-Versillé, S. Lamagna, L. Montgomery, J. Prouvé, T. Russell, M. Savini, G. Stever, S. Thompson, K.L. Tsujimoto, M. Tucker, C. Westbrook, B. Ade, P.A.R. Adler, A. Allys, E. Arnold, K. Auguste, D. Aumont, J. Aurlien, R. Austermann, J. Baccigalupi, C. Banday, A.J. Banerji, R. Barreiro, R.B. Basak, S. Beall, J. Beck, D. Beckman, S. Bermejo, J. Bersanelli, M. Bonis, J. Borrill, J. Boulanger, F. Bounissou, S. Brilenkov, M. Brown, M. Bucher, M. Calabrese, E. Campeti, P. Carones, A. Casas, F.J. Challinor, A. Chan, V. Cheung, K. Chinone, Y. Cliche, J.F. Colombo, L. Cubas, J. Cukierman, A. Curtis, D. D’Alessandro, G. Dachlythra, N. de Petris, M. Dickinson, C. Diego-Palazuelos, P. Dobbs, M. Dotani, T. Duband, L. Duff, S. Duval, J.M. Ebisawa, K. Elleflot, T. Eriksen, H.K. Errard, J. Essinger-Hileman, T. Finelli, F. Flauger, R. Franceschet, C. Fuskeland, U. Galloway, M. Ganga, K. Gao, J.R. Genova-Santos, R. Gerbino, M. Gervasi, M. Ghigna, T. Gjerløw, E. Gradziel, M.L. Grain, J. Grupp, F. Gruppuso, A. de Haan, T. Halverson, N.W. Hargrave, P. Hasebe, T. Hasegawa, M. Hattori, M. Hazumi, M. Herman, D. Herranz, D. Hill, C.A. Hilton, G. Hirota, Y. Hivon, E. Hlozek, R.A. Hoshino, Y. de la Hoz, E. Hubmayr, J. Ichiki, K. Iida, T. Imada, H. Ishimura, K. Ishino, H. Jaehnig, G. Kaga, T. Kashima, S. Katayama, N. Kato, A. Kawasaki, T. Keskitalo, R. Kisner, T. Kobayashi, Y. Kogiso, N. Kogut, A. Kohri, K. Komatsu, E. Komatsu, K. Konishi, K. Krachmalnicoff, N. Kreykenbohm, I. Kuo, C.L. Kushino, A. Lanen, J.V. Lattanzi, M. Lee, A.T. Leloup, C. Levrier, F. Linder, E. Louis, T. Luzzi, G. Maciaszek, T. Maino, D. Maki, M. Mandelli, S. Martinez-Gonzalez, E. Masi, S. Matsumura, T. Mennella, A. Migliaccio, M. Minami, Y. Mitsuda, K. Morgante, G. Murata, Y. Murphy, J.A. Nagai, M. Nagano, Y. Nagasaki, T. Nagata, R. Nakamura, S. Namikawa, T. IRAP Université de Toulouse CNRS CNES UPS Toulouse France Dipartimento di Fisica Università La Sapienza INFN Roma P. le A. Moro 2 Roma Italy CNRS UMR 8617 Université Paris-Sud 11 Bâtiment 121 Orsay91405 France Cardiff University School of Physics and Astronomy CardiffCF10 3XQ United Kingdom Stockholm University Sweden Université Paris-Saclay CNRS/IN2P3 IJCLab Orsay91405 France McGill University Physics Department MontrealQCH3A 0G4 Canada Univ. Grenoble Alpes CEA IRIG-DSBT Grenoble38000 France University of California San Diego Department of Physics San DiegoCA92093-0424 United States United Kingdom Okayama University Department of Physics Okayama700-8530 Japan UTIAS University of Tokyo KashiwaChiba277-8583 Japan Menlo ParkCA94025 United States Stanford University Department of Physics CA94305-4060 United States Sagamihara Kanagawa252-5210 Japan University of California Berkeley Department of Physics BerkeleyCA94720 United States Stockholm University Sweden Laboratoire de Physique de l’École Normale Supérieure ENS Université PSL CNRS Sorbonne Université Université de Paris Paris75005 France University of Oslo Institute of Theoretical Astrophysics OsloNO-0315 Norway BoulderCO80305 United States Via Bonomea 265 Trieste34136 Italy Avenida los Castros SN Santander39005 Spain School of Physics Indian Institute of Science Education and Research Thiruvananthapuram Maruthamala PO Vithura ThiruvananthapuramKerala695551 India Plaza Cardenal Cisneros 3 Madrid28040 Spain Dipartimento di Fisica Università degli Studi di Milano INAF-IASF Milano Sezione INFN Milano Italy Computational Cosmology Center BerkeleyCA94720 United States University of California Berkeley Space Science Laboratory BerkeleyCA94720 United States University of Manchester ManchesterM13 9PL United Kingdom - University Paris Diderot CNRS/IN2P3 CEA/Irfu Obs de Paris Sorbonne Paris Cité France Dipartimento di Fisica Univ

LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium- and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89–224 GHz) and the High-Frequency Telescope (166–448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD. © 2021, CC BY.

关键词： Cosmology

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Concept design of low frequency telescope for CMB B-mode polarization satellite liteBIRD

arXiv

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arXiv 2021年

作者： Sekimoto, Yutaro Ade, P.A.R. Adler, A. Allys, E. Arnold, K. Auguste, D. Aumont, J. Aurlien, R. Austermann, J. Baccigalupi, C. Banday, A.J. Banerji, R. Barreiro, R.B. Basak, S. Beall, J. Beck, D. Beckman, S. Bermejo, J. de Bernardis, P. Bersanelli, M. Bonis, J. Borrill, J. Boulanger, F. Bounissou, S. Brilenkov, M. Brown, M. Bucher, M. Calabrese, E. Campeti, P. Carones, A. Casas, F.J. Challinor, A. Chan, V. Cheung, K. Chinone, Y. Cliche, J.F. Colombo, L. Columbro, F. Cubas, J. Cukierman, A. Curtis, D. D’Alessandro, G. Dachlythra, N. de Petris, M. Dickinson, C. Diego-Palazuelos, P. Dobbs, M. Dotani, T. Duband, L. Duff, S. Duval, J.M. Ebisawa, K. Elleflot, T. Eriksen, H.K. Errard, J. Essinger-Hileman, T. Finelli, F. Flauger, R. Franceschet, C. Fuskeland, U. Galloway, M. Ganga, K. Gao, J.R. Genova-Santos, R. Gerbino, M. Gervasi, M. Ghigna, T. Gjerløw, E. Gradziel, M.L. Grain, J. Grupp, F. Gruppuso, A. Gudmundsson, J.E. de Haan, T. Halverson, N.W. Hargrave, P. Hasebe, T. Hasegawa, M. Hattori, M. Hazumi, M. Henrot-Versillé, S. Herman, D. Herranz, D. Hill, C.A. Hilton, G. Hirota, Y. Hivon, E. Hlozek, R.A. Hoshino, Y. de la Hoz, E. Hubmayr, J. Ichiki, K. Iida, T. Imada, H. Ishimura, K. Ishino, H. Jaehnig, G. Kaga, T. Kashima, S. Katayama, N. Kato, A. Kawasaki, T. Keskitalo, R. Kisner, T. Kobayashi, Y. Kogiso, N. Kogut, A. Kohri, K. Komatsu, E. Komatsu, K. Konishi, K. Krachmalnicoff, N. Kreykenbohm, I. Kuo, C.L. Kushino, A. Lamagna, L. Lanen, J.V. Lattanzi, M. Lee, A.T. Leloup, C. Levrier, F. Linder, E. Louis, T. Luzzi, G. Maciaszek, T. Maffei, B. Maino, D. Maki, M. Mandelli, S. Martinez-Gonzalez, E. Masi, S. Matsumura, T. Mennella, A. Migliaccio, M. Minami, Y. Mitsuda, K. Montgomery, J. Montier, L. Morgante, G. Mot, B. Murata, Y. Murphy, J.A. Nagai, M. Nagano, Y. Nagasaki, T. Nagata, R. Nakamura, S. Namikawa, T. Natoli, P. Nerval, S. Nishibori, T. Nishino, H. O’Sullivan, C. Ogawa, H. Ogawa, H. Oguri, S. Ohsaki, H. SagamiharaKanagawa252-5210 Japan The University of Tokyo Department of Astronomy Tokyo113-0033 Japan TsukubaIbaraki305-0801 Japan Cardiff University School of Physics and Astronomy CardiffCF10 3XQ United Kingdom Stockholm University Sweden Laboratoire de Physique de l’École Normale Supérieure ENS Université PSL CNRS Sorbonne Université Université de Paris Paris75005 France University of California San Diego Department of Physics San DiegoCA92093-0424 United States Université Paris-Saclay CNRS/IN2P3 IJCLab Orsay91405 France IRAP Université de Toulouse CNRS CNES UPS Toulouse France University of Oslo Institute of Theoretical Astrophysics OsloNO-0315 Norway BoulderCO80305 United States Via Bonomea 265 Trieste34136 Italy Avenida los Castros SN Santander39005 Spain School of Physics Indian Institute of Science Education and Research Thiruvananthapuram Maruthamala PO Vithura ThiruvananthapuramKerala695551 India Stanford University Department of Physics CA94305-4060 United States University of California Berkeley Department of Physics BerkeleyCA94720 United States Plaza Cardenal Cisneros 3 Madrid28040 Spain Dipartimento di Fisica Università La Sapienza INFN Roma P. le A. Moro 2 Roma Italy Dipartimento di Fisica Università degli Studi di Milano INAF-IASF Milano Sezione INFN Milano Italy Computational Cosmology Center BerkeleyCA94720 United States University of California Berkeley Space Science Laboratory BerkeleyCA94720 United States CNRS UMR 8617 Université Paris-Sud 11 Bâtiment 121 Orsay91405 France University of Manchester ManchesterM13 9PL United Kingdom University Paris Diderot CNRS/IN2P3 CEA/Irfu Obs de Paris Sorbonne Paris Cité France Dipartimento di Fisica Università di Roma"Tor Vergata" Sezione INFN Roma2 Italy DAMTP Centre for Mathematical Sciences Wilberforce Road CambridgeCB3 0WA United Kingdom Institute of Astronomy Madingley Road CambridgeCB3 0HA United Kingdom Kavli Instit

LiteBIRD has been selected as JAXA’s strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) B-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of −56 dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT: 34–161 GHz), one of LiteBIRD’s onboard telescopes. It has a wide field-of-view (18◦ × 9◦) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90◦ are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at 5 K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented. © 2021, CC BY.

关键词： Millimeter waves

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Developments and applications of the OPTIMADE API for materials discovery, design, and data exchange

arXiv

引用

arXiv 2024年

作者： Evans, Matthew L. Bergsma, Johan Merkys, Andrius Andersen, Casper W. Andersson, Oskar B. Beltrán, Daniel Blokhin, Evgeny Boland, Tara M. Balderas, Rubén Castañeda Choudhary, Kamal Díaz, Alberto Díaz García, Rodrigo Domínguez Eckert, Hagen Eimre, Kristjan Montero, María Elena Fuentes Krajewski, Adam M. Mortensen, Jens Jørgen Duarte, José Manuel Nápoles Pietryga, Jacob Qi, Ji de Jesús Trejo Carrillo, Felipe Vaitkus, Antanas Yu, Jusong Zettel, Adam de Castro, Pedro Baptista Carlsson, Johan Cerqueira, Tiago F.T. Divilov, Simon Hajiyani, Hamidreza Hanke, Felix Jose, Kevin Oses, Corey Riebesell, Janosh Schmidt, Jonathan Winston, Donald Xie, Christen Yang, Xiaoyu Bonella, Sara Botti, Silvana Curtarolo, Stefano Draxl, Claudia Cobas, Luis Edmundo Fuentes Hospital, Adam Liu, Zi-Kui Marques, Miguel A.L. Marzari, Nicola Morris, Andrew J. Ong, Shyue Ping Orozco, Modesto Persson, Kristin A. Thygesen, Kristian S. Wolverton, Chris Scheidgen, Markus Toher, Cormac Conduit, Gareth J. Pizzi, Giovanni Gražulis, Saulius Rignanese, Gian-Marco Armiento, Rickard Chemin des Étoiles 8 Louvain-la-Neuve1348 Belgium Matgenix SRL 185 Rue Armand Bury Gozée6534 Belgium École Polytechnique Fédérale de Lausanne Avenue de Forel 3 Lausanne1015 Switzerland Institute of Biotechnology Life Sciences Center Vilnius University Sauletekio av. 7 VilniusLT-10257 Lithuania SINTEF P.O. Box 4760 Torgarden TrondheimNO-7465 Norway Materials Design and Informatics unit Department of Physics Chemistry and Biology Linköping University Sweden Baldiri i Reixac 10-12 Barcelona08028 Spain Tilde Materials Informatics Straßmannstraße 25 Berlin10249 Germany Materials Platform for Data Science Sepapaja 6 Tallinn15551 Estonia Computational Atomic-Scale Materials Design Technical University of Denmark Kgs. Lyngby Denmark Av. Miguel de Cervantes 120 Complejo Industrial Chihuahua Chihuahua Chih. 31136 Mexico Material Measurement Laboratory National Institute of Standards and Technology GaithersburgMD20899 United States Department of Mechanical Engineering and Materials Science Duke University DurhamNC27708 United States Center for Extreme Materials Duke University DurhamNC27708 United States École Polytechnique Fédérale de Lausanne Lausanne1015 Switzerland Universidad Autónoma de Chihuahua Facultad de Ciencias Quimicas Chihuahua31125 Mexico Department of Materials Science and Engineering The Pennsylvania State University University ParkPA16802 United States Department of Materials Science and Engineering Northwestern University EvanstonIL60208 United States Department of NanoEngineering University of California 9500 Gilman Drive La Jolla San DiegoCA92093-0448 United States National Institute for Materials Science 1-2-1 Sengen Ibaraki Tsukuba305-0047 Japan Dassault Systèmes Germany GmbH Am Kabellager 11-13 Cologne51063 Germany CFisUC Department of Physics University of Coimbra Rua Larga Coimbra3004-516 Portugal Dassault Systèmes 22 Science Park CB4 0FJ United Kingdom Theory of Condensed Matter Cavendis

The Open databases Integration for Materials Design (OPTIMADE) application programming interface (API) empowers users with holistic access to a growing federation of databases, enhancing the accessibility and discoverability of materials and chemical data. Since the first release of the OPTIMADE specification (v1.0), the API has undergone significant development, leading to the v1.2 release, and has underpinned multiple scientific studies. In this work, we highlight the latest features of the API format, accompanying software tools, and provide an update on the implementation of OPTIMADE in contributing materials databases. We end by providing several use cases that demonstrate the utility of the OPTIMADE API in materials research that continue to drive its ongoing development. © 2024, CC BY.

关键词： Electronic data interchange

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Constraints on black-hole charges with the 2017 EHT observations of M87*

引用

Physical Review D 2021年第10期103卷 104047-104047页

作者： Prashant Kocherlakota Luciano Rezzolla Heino Falcke Christian M. Fromm Michael Kramer Yosuke Mizuno Antonios Nathanail Héctor Olivares Ziri Younsi Kazunori Akiyama Antxon Alberdi Walter Alef Juan Carlos Algaba Richard Anantua Keiichi Asada Rebecca Azulay Anne-Kathrin Baczko David Ball Mislav Baloković John Barrett Bradford A. Benson Dan Bintley Lindy Blackburn Raymond Blundell Wilfred Boland Katherine L. Bouman Geoffrey C. Bower Hope Boyce Michael Bremer Christiaan D. Brinkerink Roger Brissenden Silke Britzen Avery E. Broderick Dominique Broguiere Thomas Bronzwaer Do-Young Byun John E. Carlstrom Andrew Chael Chi-kwan Chan Shami Chatterjee Koushik Chatterjee Ming-Tang Chen Yongjun Chen (陈永军) Paul M. Chesler Ilje Cho Pierre Christian John E. Conway James M. Cordes Thomas M. Crawford Geoffrey B. Crew Alejandro Cruz-Osorio Yuzhu Cui Jordy Davelaar Mariafelicia De Laurentis Roger Deane Jessica Dempsey Gregory Desvignes Sheperd S. Doeleman Ralph P. Eatough Joseph Farah Vincent L. Fish Ed Fomalont Raquel Fraga-Encinas Per Friberg H. Alyson Ford Antonio Fuentes Peter Galison Charles F. Gammie Roberto García Olivier Gentaz Boris Georgiev Ciriaco Goddi Roman Gold José L. Gómez Arturo I. Gómez-Ruiz Minfeng Gu (顾敏峰) Mark Gurwell Kazuhiro Hada Daryl Haggard Michael H. Hecht Ronald Hesper Luis C. Ho (何子山) Paul Ho Mareki Honma Chih-Wei L. Huang Lei Huang (黄磊) David H. Hughes Shiro Ikeda Makoto Inoue Sara Issaoun David J. James Buell T. Jannuzi Michael Janssen Britton Jeter Wu Jiang (江悟) Alejandra Jimenez-Rosales Michael D. Johnson Svetlana Jorstad Taehyun Jung Mansour Karami Ramesh Karuppusamy Tomohisa Kawashima Garrett K. Keating Mark Kettenis Dong-Jin Kim Jae-Young Kim Jongsoo Kim Junhan Kim Motoki Kino Jun Yi Koay Yutaro Kofuji Patrick M. Koch Shoko Koyama Carsten Kramer Thomas P. Krichbaum Cheng-Yu Kuo Tod R. Lauer Sang-Sung Lee Aviad Levis Yan-Rong Li (李彦荣) Zhiyuan Li (李志远) Michael Lindqvist Rocco Lico Greg Lindahl Jun Liu (刘俊) Kuo Liu Elisabetta Liuzzo Wen-Ping Lo Andrei P. Lobanov Laurent Loinard Colin Lonsdale Ru-Sen Lu Institut für Theoretische Physik Goethe-Universität Max-von-Laue-Strasse 1 60438 Frankfurt Germany Frankfurt Institute for Advanced Studies Ruth-Moufang-Strasse 1 60438 Frankfurt Germany School of Mathematics Trinity College Dublin 2 Ireland Department of Astrophysics Institute for Mathematics Astrophysics and Particle Physics (IMAPP) Radboud University P.O. Box 9010 6500 GL Nijmegen Netherlands Black Hole Initiative at Harvard University 20 Garden Street Cambridge Massachusetts 02138 USA Center for Astrophysics—Harvard & Smithsonian 60 Garden Street Cambridge Massachusetts 02138 USA Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 D-53121 Bonn Germany Tsung-Dao Lee Institute and School of Physics and Astronomy Shanghai Jiao Tong University Shanghai 200240 China Institut für Theoretische Physik Goethe-Universität Frankfurt Max-von-Laue-Straße 1 D-60438 Frankfurt am Main Germany Department of Physics National and Kapodistrian University of Athens Panepistimiopolis GR 15783 Zografos Greece Mullard Space Science Laboratory University College London Holmbury St. Mary Dorking Surrey RH5 6NT United Kingdom Massachusetts Institute of Technology Haystack Observatory 99 Millstone Road Westford Massachusetts 01886 USA National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n E-18008 Granada Spain Department of Physics Faculty of Science University of Malaya 50603 Kuala Lumpur Malaysia Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New York New York 10010 USA Institute of Astronomy and Astrophysics Academia Sinica 11F of Astronomy-Mathematics Building AS/NTU No. 1 Sec. 4 Roosevelt Rd Taipei 10617 Taiwan R.O.C. Departament d’Astronomia i Astrofísica Universitat de València C. Dr. Moliner 50 E-46100 Burjassot València Spain Observatori Astronòmic Universitat de València C. Catedrático José Beltrán 2 E-46980 Paterna

Our understanding of strong gravity near supermassive compact objects has recently improved thanks to the measurements made by the Event Horizon Telescope (EHT). We use here the M87* shadow size to infer constraints on the physical charges of a large variety of nonrotating or rotating black holes. For example, we show that the quality of the measurements is already sufficient to rule out that M87* is a highly charged dilaton black hole. Similarly, when considering black holes with two physical and independent charges, we are able to exclude considerable regions of the space of parameters for the doubly-charged dilaton and the Sen black holes.

关键词： Alternative gravity theories Experimental studies of gravity General relativity Radio, microwave, & sub-mm astronomy Accretion disk & black-hole plasma Classical black holes Galaxies Electromagnetic radiation astronomy

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