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The evolutionary history of 2,658 cancers (vol 578, pg 122, 2020)

NATURE 2023年第7948期614卷 E42-E42页

作者： Gerstung, Moritz Jolly, Clemency Leshchiner, Ignaty Dentro, Stefan C. Gonzalez, Santiago Rosebrock, Daniel Mitchell, Thomas J. Rubanova, Yulia Anur, Pavana Yu, Kaixian Tarabichi, Maxime Deshwar, Amit Wintersinger, Jeff Kleinheinz, Kortine Vazquez-Garcia, Ignacio Haase, Kerstin Jerman, Lara Sengupta, Subhajit Macintyre, Geoff Malikic, Salem Donmez, Nilgun Livitz, Dimitri G. Cmero, Marek Demeulemeester, Jonas Schumacher, Steven Fan, Yu Yao, Xiaotong Lee, Juhee Schlesner, Matthias Boutros, Paul C. Bowtell, David D. Zhu, Hongtu Getz, Gad Imielinski, Marcin Beroukhim, Rameen Sahinalp, S. Cenk Ji, Yuan Peifer, Martin Markowetz, Florian Mustonen, Ville Yuan, Ke Wang, Wenyi Morris, Quaid D. Spellman, Paul T. Wedge, David C. Van Loo, Peter European Molecular Biology Laboratory European Bioinformatics Institute (EMBL-EBI) Cambridge UK European Molecular Biology Laboratory Genome Biology Unit Heidelberg Germany Wellcome Sanger Institute Cambridge UK Genome Biology Unit European Molecular Biology Laboratory (EMBL) Heidelberg Germany University of Ljubljana Ljubljana Slovenia The Francis Crick Institute London UK Big Data Institute University of Oxford Oxford UK Wellcome Sanger Institute Wellcome Genome Campus Hinxton UK Big Data Institute Li Ka Shing Centre University of Oxford Oxford UK University of Cambridge Cambridge UK Cambridge University Hospitals NHS Foundation Trust Cambridge UK Department of Applied Mathematics and Theoretical Physics Centre for Mathematical Sciences University of Cambridge Cambridge UK Department of Epidemiology and Biostatistics Memorial Sloan Kettering Cancer Center New York NY USA Department of Statistics Columbia University New York NY USA Department of Haematology University of Cambridge Cambridge UK University of Leuven Leuven Belgium Broad Institute of MIT and Harvard Cambridge MA USA Center for Cancer Research Massachusetts General Hospital Charlestown MA USA Department of Pathology Massachusetts General Hospital Boston MA USA Harvard Medical School Boston MA USA Center for Cancer Research Massachusetts General Hospital Boston MA USA Dana-Farber Cancer Institute Boston MA USA Department of Medical Oncology Dana-Farber Cancer Institute Boston MA USA Department of Cancer Biology Dana-Farber Cancer Institute Boston MA USA Oxford NIHR Biomedical Research Centre Oxford UK Oxford NIHR Biomedical Research Centre University of Oxford Oxford UK University of Toronto Toronto Ontario Canada Vector Institute Toronto Ontario Canada Vector Institute Toronto ON Canada Department of Computer Science University of Toronto Toronto ON Canada Ontario Institute for Cancer Research Toronto Ontario Canada University of California Los Angeles

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Preliminary result of characteristic of convective cloud development observed by x-band meteorological radar in bandung basin

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IOP Conference Series: Earth and Environmental science 2019年第1期303卷

作者： R A Syaraswati N J Trilaksono G A Nugroho Undergraduate Program in Meteorology Faculty of Earth Sciences and Technology Institut Teknologi Bandung ID Weather and Climate Prediction Laboratory Faculty of Earth Sciences and Technology Institut Teknologi Bandung ID Atmospheric Science Research Group Faculty of Earth Sciences and Technology Institut Teknologi Bandung ID Center for Atmospheric Science and Technology Indonesian National Institute of Aeronautics and Space ID

The initial, mature, and dissipation stage changes in a convective cloud development have a short period of time so that the development stage analysis is needed by using data that has a high temporal resolution. The data that used are product CAPPI-V and CAPPI-Z from X-Band meteorological radar and also BBWS Citarum rainfall data from 13 stations that scattered in the area of Bandung basin. The selection of rainfall days is done to take the areas that have a strong convective system, and the result is that Sapan area has higher rainfall than 12 other stations on April 27th, 2017. The precipitation is caused by convective clouds. The initial stage of convective clouds begins with the existence of convergence phenomena in the afternoon and at 10 minutes before the rainfall event. It is also when there are maximum rainfall events on April 27th, 2017 which can indicate the formation of convective clouds. After the formation, the development stage occurs when there is an increase in reflectivity values on the radar and then convective cloud size starts to grow. When convective cloud size is dissipating, there is an identification of a decrease in reflectivity of the previous value in the evening. There is a new convective initiation next to the cloud that is in the dissipation stage and then joins to develops in a short time for about 30 minutes.

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lenstronomy II: A gravitational lensing software ecosystem

arXiv

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arXiv 2021年

作者： Birrer, Simon Shajib, Anowar J. Gilman, Daniel Galan, Aymeric Aalbers, Jelle Millon, Martin Morgan, Robert Pagano, Giulia Park, Ji Won Teodori, Luca Tessore, Nicolas Ueland, Madison van de Vyvere, Lyne Wagner-Carena, Sebastian Wempe, Ewoud Yang, Lilan Ding, Xuheng Schmidt, Thomas Sluse, Dominique Zhang, Ming Amara, Adam Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States SLAC National Accelerator Laboratory Menlo ParkCA94025 United States Department of Astronomy & Astrophysics University of Chicago ChicagoIL60637 United States Department of Physics and Astronomy University of California Los AngelesCA90095 United States Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada Switzerland Physics Department University of Wisconsin-Madison 1150 University Avenue MadisonWI53706 United States Legacy Survey of Space and Time Corporation Data Science Fellowship Program United States Weizmann Institute 234 Herzl Street Rehovot7610001 Israel Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom STAR Institute Université de Liège Quartier Agora - Allée du six Août 19c LiègeB-4000 Belgium Kapteyn Astronomical Institute University of Groningen PO Box 800 Groningen9700 AV Netherlands School of Physics and Technology Wuhan University Wuhan430072 China UTIAS University of Tokyo Kashiwa Chiba277-8583 Japan Xinjiang Astronomical Observatory Chinese Academy of Sciences 150 Science 1-Street Urumqi831001 China Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom

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Proton emission in ultraperipheral Pb-Pb collisions at sNN=5.02 TeV

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Physical Review C 2025年第5期111卷 054906-054906页

作者： S. Acharya A. Agarwal G. Aglieri Rinella L. Aglietta M. Agnello N. Agrawal Z. Ahammed S. Ahmad S. U. Ahn I. Ahuja A. Akindinov V. Akishina M. Al-Turany D. Aleksandrov B. Alessandro H. M. Alfanda R. Alfaro Molina B. Ali A. Alici N. Alizadehvandchali A. Alkin J. Alme G. Alocco T. Alt A. R. Altamura I. Altsybeev J. R. Alvarado C. O. R. Alvarez M. N. Anaam C. Andrei N. Andreou A. Andronic E. Andronov V. Anguelov F. Antinori P. Antonioli N. Apadula L. Aphecetche H. Appelshäuser C. Arata S. Arcelli R. Arnaldi J. G. M. C. A. Arneiro I. C. Arsene M. Arslandok A. Augustinus R. Averbeck D. Averyanov M. D. Azmi H. Baba A. Badalà J. Bae Y. Bae Y. W. Baek X. Bai R. Bailhache Y. Bailung R. Bala A. Baldisseri B. Balis Z. Banoo V. Barbasova F. Barile L. Barioglio M. Barlou B. Barman G. G. Barnaföldi L. S. Barnby E. Barreau V. Barret L. Barreto C. Bartels K. Barth E. Bartsch N. Bastid S. Basu G. Batigne D. Battistini B. Batyunya D. Bauri J. L. Bazo Alba I. G. Bearden C. Beattie P. Becht D. Behera I. Belikov A. D. C. Bell Hechavarria F. Bellini R. Bellwied S. Belokurova L. G. E. Beltran Y. A. V. Beltran G. Bencedi A. Bensaoula S. Beole Y. Berdnikov A. Berdnikova L. Bergmann M. G. Besoiu L. Betev P. P. Bhaduri A. Bhasin B. Bhattacharjee L. Bianchi J. Bielčík J. Bielčíková A. P. Bigot A. Bilandzic A. Binoy G. Biro S. Biswas N. Bize J. T. Blair D. Blau M. B. Blidaru N. Bluhme C. Blume F. Bock T. Bodova J. Bok L. Boldizsár M. Bombara P. M. Bond G. Bonomi H. Borel A. Borissov A. G. Borquez Carcamo E. Botta Y. E. M. Bouziani D. C. Brandibur L. Bratrud P. Braun-Munzinger M. Bregant M. Broz G. E. Bruno V. D. Buchakchiev M. D. Buckland D. Budnikov H. Buesching S. Bufalino P. Buhler N. Burmasov Z. Buthelezi A. Bylinkin S. A. Bysiak J. C. Cabanillas Noris M. F. T. Cabrera H. Caines A. Caliva E. Calvo Villar J. M. M. Camacho P. Camerini F. D. M. Canedo S. L. Cantway M. Carabas A. A. Carballo F. Carnesecchi R. Caron L. A. D. Carvalho J. Castillo Castellanos M. Castoldi F. Catalano S. Cattaruzzi R. Cerri I. Chakaberia P. Chakraborty S. Chandra Université Clermont Auvergne CNRS/IN2P3 LPC Clermont-Ferrand France Variable Energy Cyclotron Centre Homi Bhabha National Institute Kolkata India European Organization for Nuclear Research (CERN) Geneva Switzerland Dipartimento di Fisica dell'Università and Sezione INFN Turin Italy Dipartimento DISAT del Politecnico and Sezione INFN Turin Italy Dipartimento di Fisica e Astronomia dell'Università and Sezione INFN Bologna Italy Department of Physics Aligarh Muslim University Aligarh India Korea Institute of Science and Technology Information Daejeon Republic of Korea Faculty of Science P.J. Šafárik University Košice Slovak Republic Affiliated with an institute covered by a cooperation agreement with CERN Frankfurt Institute for Advanced Studies Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany Research Division and ExtreMe Matter Institute EMMI GSI Helmholtzzentrum für Schwerionenforschung GmbH Darmstadt Germany INFN Sezione di Torino Turin Italy Central China Normal University Wuhan China Instituto de Física Universidad Nacional Autónoma de México Mexico City Mexico University of Houston Houston Texas USA Sungkyunkwan University Suwon City Republic of Korea Department of Physics and Technology University of Bergen Bergen Norway INFN Sezione di Cagliari Cagliari Italy Institut für Kernphysik Johann Wolfgang Goethe-Universität Frankfurt Frankfurt Germany INFN Sezione di Bari Bari Italy Physik Department Technische Universität München Munich Germany High Energy Physics Group Universidad Autónoma de Puebla Puebla Mexico Horia Hulubei National Institute of Physics and Nuclear Engineering Bucharest Romania University of Derby Derby United Kingdom Universität Münster Institut für Kernphysik Münster Germany Physikalisches Institut Ruprecht-Karls-Universität Heidelberg Heidelberg Germany INFN Sezione di Padova Padova Italy INFN Sezione di Bologna Bologna Italy Lawrence Berkeley National Laboratory Berkeley California USA SUBATECH I

The first measurements of proton emission accompanied by neutron emission in the electromagnetic dissociation (EMD) of Pb208 nuclei in the ALICE experiment at the Large Hadron Collider are presented. The EMD protons and neutrons emitted at very forward rapidities are detected by the proton and neutron zero degree calorimeters of the ALICE experiment. The emission cross sections of zero, one, two, and three protons accompanied by at least one neutron were measured in ultraperipheral Pb208−Pb208 collisions at a center-of-mass energy per nucleon pair sNN=5.02TeV. The 0p and 3p cross sections are described by the RELDIS model within their measurement uncertainties, while the 1p and 2p cross sections are underestimated by the model by 17–25%. According to this model, these 0p, 1p, 2p, and 3p cross sections are associated, respectively, with the production of various isotopes of Pb, Tl, Hg, and Au in the EMD of Pb208. The cross sections of the emission of a single proton accompanied by the emission of one, two, or three neutrons in EMD were also measured. The data are significantly overestimated by the RELDIS model, which predicts that the (1p,1n), (1p,2n), and (1p,3n) cross sections are very similar to the cross sections for the production of the thallium isotopes Tl206,205,204.

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PTF11rka: an interacting supernova at the crossroads of stripped-envelope and h-poor super-luminous stellar core collapses

arXiv

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arXiv 2020年

作者： Pian, Elena Mazzali, Paolo A. Moriya, Takashi J. Rubin, Adam Gal-Yam, Avishay Arcavi, Iair Ben-Ami, Sagi Blagorodnova, Nadia Bufano, Milena F. Filippenko, Alex V. Kasliwal, Mansi Kulkarni, Shri R. Lunnan, Ragnhild Manulis, Ilan Matheson, Tom Nugent, Peter E. Ofek, Eran Perley, Dan A. Prentice, Simon J. Yaron, Ofer INAF Astrophysics and Space Science Observatory via P. Gobetti 101 Bologna40129 Italy Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany National Astronomical Observatory of Japan National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan School of Physics and Astronomy Faculty of Science Monash University ClaytonVIC3800 Australia European Southern Observatory Karl-Schwarzschild-Strasse 2 Garching bei München85748 Germany Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot76100 Israel School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel CIFAR Azrieli Global Scholars program CIFAR Toronto Canada Harvard Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Department of Astrophysics IMAPP Radboud University Nijmegen Netherlands INAF-Osservatorio Astrofisico di Catania Via Santa Sofia 78 CataniaI-95123 Italy Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Cahill Center for Astrophysics California Institute of Technology 1200 E. California Blvd PasadenaCA91125 United States Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-106 91 Sweden NSF’s National Optical-Infrared Astronomy Research Laboratory TucsonAZ United States Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States School of Physics Trinity College Dublin University of Dublin Dublin 2 Ireland

The hydrogen-poor supernova PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 Dec. 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the RPTF filter band, and maximum in this band was reached ∼ 30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a ∼10 M carbon-oxygen core evolved from a progenitor of main-sequence mass 25–40 M, that liberated a kinetic energy Ek≈ 4 × 1051 erg, expelled ∼ 8 M of ejecta, and synthesised ∼ 0.5 M of 56Ni. The photospheric spectra of PTF11rka are characterised by narrow absorption lines that point to suppression of the highest ejecta velocities (>∼ 15, 000 km s−1). This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (∼ 5 × 1050 erg), less than 2% of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst supernovae (GRB-SNe) in luminosity, although it has a lower energy and a lower Ek/Mej ratio. Copyright © 2020, The Authors. All rights reserved.

关键词： Supernovae

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SPT Clusters with DES and HST Weak Lensing. II. Cosmological Constraints from the Abundance of Massive Halos

arXiv

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arXiv 2024年

作者： Bocquet, S. Grandis, S. Bleem, L.E. Klein, M. Mohr, J.J. Schrabback, T. Abbott, T.M.C. Ade, P.A.R. Aguena, M. Alarcon, A. Allam, S. Allen, S.W. Alves, O. Amon, A. Anderson, A.J. Annis, J. Ansarinejad, B. Austermann, J.E. Avila, S. Bacon, D. Bayliss, M. Beall, J.A. Bechtol, K. Becker, M.R. Bender, A.N. Benson, B.A. Bernstein, G.M. Bhargava, S. Bianchini, F. Brodwin, M. Brooks, D. Bryant, L. Campos, A. Canning, R.E.A. Carlstrom, J.E. Rosell, A. Carnero Kind, M. Carrasco Carretero, J. Castander, F.J. Cawthon, R. Chang, C.L. Chang, C. Chaubal, P. Chen, R. Chiang, H.C. Choi, A. Chou, T.-L. Citron, R. Moran, C. Corbett Cordero, J. Costanzi, M. Crawford, T.M. Crites, A.T. da Costa, L.N. Pereira, M.E.S. Davis, C. Davis, T.M. DeRose, J. Desai, S. de Haan, T. Diehl, H.T. Dobbs, M.A. Dodelson, S. Doux, C. Drlica-Wagner, A. Eckert, K. Elvin-Poole, J. Everett, S. Everett, W. Ferrero, I. Ferté, A. Flores, A.M. Frieman, J. Gallicchio, J. García-Bellido, J. Gatti, M. George, E.M. Giannini, G. Gladders, M.D. Gruen, D. Gruendl, R.A. Gupta, N. Gutierrez, G. Halverson, N.W. Harrison, I. Hartley, W.G. Herner, K. Hinton, S.R. Holder, G.P. Hollowood, D.L. Holzapfel, W.L. Honscheid, K. Hrubes, J.D. Huang, N. Hubmayr, J. Huff, E.M. Huterer, D. Irwin, K.D. James, D.J. Jarvis, M. Khullar, G. Kim, K. Knox, L. Kraft, R. Krause, E. Kuehn, K. Kuropatkin, N. Kéruzoré, F. Lahav, O. Lee, A.T. Leget, P.-F. Li, D. Lin, H. Lowitz, A. MacCrann, N. Mahler, G. Mantz, A. Marshall, J.L. McCullough, J. McDonald, M. McMahon, J.J. Mena-Fernández, J. Menanteau, F. Meyer, S.S. Miquel, R. Montgomery, J. Myles, J. Natoli, T. Navarro-Alsina, A. Nibarger, J.P. Noble, G.I. Novosad, V. Ogando, R.L.C. Omori, Y. Padin, S. Pandey, S. Paschos, P. Patil, S. Pieres, A. Malagón, A.A. Plazas Porredon, A. Prat, J. Pryke, C. Raveri, M. Reichardt, C.L. Roberson, J. Rollins, R.P. Romero, C. Roodman, A. Ruhl, J.E. Rykoff, E.S. Saliwanchik, B.R. University Observatory Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 Munich81679 Germany Universität Innsbruck Institut für Astro- und Teilchenphysik Technikerstr. 25/8 Innsbruck6020 Austria High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue LemontIL60439 United States Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Max Planck Institute for Extraterrestrial Physics Gießenbachstr. 1 Garching85748 Germany Argelander-Institut für Astronomie Auf dem Hügel 71 Bonn53121 Germany Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile School of Physics and Astronomy Cardiff University CardiffCF24 3YB United Kingdom Laboratório Interinstitucional de e-Astronomia - LIneA Rua Gal. José Cristino 77 RJ Rio de Janeiro20921-400 Brazil Fermi National Accelerator Laboratory P. O. Box 500 BataviaIL60510 United States Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall StanfordCA94305 United States Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo ParkCA94025 United States Department of Physics University of Michigan Ann ArborMI48109 United States Institute of Astronomy University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom School of Physics University of Melbourne ParkvilleVIC3010 Australia NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of Colorado BoulderCO80309 United States The Barcelona Institute of Science and Technology Campus UAB Bellaterra Barcelona08193 Spain Institute of Cosmology and Gravitation Universit

We present cosmological constraints from the abundance of galaxy clusters selected via the thermal Sunyaev-Zel’dovich (SZ) effect in South Pole Telescope (SPT) data with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble space Telescope (HST). The cluster sample is constructed from the combined SPT-SZ, SPTpol ECS, and SPTpol 500d surveys, and comprises 1,005 confirmed clusters in the redshift range 0.25 − 1.78 over a total sky area of 5,200 deg2. We use DES Year 3 weak-lensing data for 688 clusters with redshifts z m = 0.286 ± 0.032, σ8 = 0.817 ± 0.026, and the parameter combination σ8 (Ωm/0.3)0.25 = 0.805 ± 0.016. Our measurement of S8 ≡ σ8 √Ωm/0.3 = 0.795 ± 0.029 and the constraint from Planck CMB anisotropies (2018 TT,TE,EE+lowE) differ by 1.1σ. In combination with that Planck dataset, we place a 95% upper limit on the sum of neutrino masses ∑ mν +0.22−0.15, or a 2.2σ difference with a cosmological constant. We use the cluster abundance to measure σ8 in five redshift bins between 0.25 and 1.8, and we find the results to be consistent with structure growth as predicted by the ΛCDM model fit to Planck primary CMB data. Copyright © 2024, The Authors. All rights reserved.

关键词： Cosmology

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Event horizon telescope observations of the jet launching and collimation in centaurus A

arXiv

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arXiv 2021年

作者： Janssen, Michael Falcke, Heino Kadler, Matthias Ros, Eduardo Wielgus, Maciek Akiyama, Kazunori Baloković, Mislav Blackburn, Lindy Bouman, Katherine L. Chael, Andrew Chan, Chi-Kwan Chatterjee, Koushik Davelaar, Jordy Edwards, Philip G. Fromm, Christian M. Gómez, José L. Goddi, Ciriaco Issaoun, Sara Johnson, Michael D. Kim, Junhan Koay, Jun Yi Krichbaum, Thomas P. Liu, Jun Liuzzo, Elisabetta Markoff, Sera Markowitz, Alex Marrone, Daniel P. Mizuno, Yosuke Müller, Cornelia Ni, Chunchong Pesce, Dominic W. Ramakrishnan, Venkatessh Roelofs, Freek Rygl, Kazi L.J. van Bemmel, Ilse Alberdi, Antxon Alef, Walter Algaba, Juan Carlos Anantua, Richard Asada, Keiichi Azulay, Rebecca Baczko, Anne-Kathrin Ball, David Barrett, John Benson, Bradford A. Bintley, Dan Blundell, Raymond Boland, Wilfred Bower, Geoffrey C. Boyce, Hope Bremer, Michael Brinkerink, Christiaan D. Brissenden, Roger Britzen, Silke Broderick, Avery E. Broguiere, Dominique Bronzwaer, Thomas Byun, Do-Young Carlstrom, John E. Chatterjee, Shami Chen, Ming-Tang Chen, Yongjun Chesler, Paul M. Cho, Ilje Christian, Pierre Conway, John E. Cordes, James M. Crawford, Thomas M. Crew, Geoffrey B. Cruz-Osorio, Alejandro Cui, Yuzhu de Laurentis, Mariafelicia Deane, Roger Dempsey, Jessica Desvignes, Gregory Dexter, Jason Doeleman, Sheperd S. Eatough, Ralph P. Farah, Joseph Fish, Vincent L. Fomalont, Ed Ford, H. Alyson Fraga-Encinas, Raquel Friberg, Per Fuentes, Antonio Galison, Peter Gammie, Charles F. García, Roberto Gelles, Zachary Gentaz, Olivier Georgiev, Boris Gold, Roman Gómez-Ruiz, Arturo I. Gu, Minfeng Gurwell, Mark Hada, Kazuhiro Haggard, Daryl Hecht, Michael H. Hesper, Ronald Himwich, Elizabeth Ho, Luis C. Ho, Paul Honma, Mareki Huang, Chih-Wei L. Huang, Lei Hughes, David H. Ikeda, Shiro Inoue, Makoto James, David J. Jannuzi, Buell T. Jeter, Britton Jiang, Wu Jimenez-Rosales, Alejandra Jorstad, Svetlana Jung, Taehyun Karami, Mansour Karuppusamy, Ramesh Kawashima, Tomohisa Keating, Garrett K. Kettenis, Mark Kim, Dong-Jin Kim, Jae-Young Kim, Jongsoo Kino, Motoki Kofuji, Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Lehrstuhl für Astronomie Universität Würzburg Emil-Fischer Str. 31 Würzburg97074 Germany Black Hole Initiative at Harvard University 20 Garden Street CambridgeMA02138 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Massachusetts Institute of Technology Haystack Observatory 99 Millstone Road WestfordMA01886 United States National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Yale Center for Astronomy & Astrophysics 52 Hillhouse Avenue New HavenCT06511 United States Department of Physics Yale University P.O. Box 2018120 New HavenCT06520 United States California Institute of Technology 1200 East California Boulevard PasadenaCA91125 United States Princeton Center for Theoretical Science Jadwin Hall Princeton University PrincetonNJ08544 United States NASA Hubble Fellowship Program Einstein Fellow Steward Observatory and Department of Astronomy University of Arizona 933 N. Cherry Ave. TucsonAZ85721 United States Data Science Institute University of Arizona 1230 N. Cherry Ave. TucsonAZ85721 United States Anton Pannekoek Institute for Astronomy University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Department of Astronomy and Columbia Astrophysics Laboratory Columbia University 550 W 120th Street New YorkNY10027 United States Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States Australia Telescope National Facility CSIRO Astronomy and Space Science EppingNSW1710 Australia Institut für Theoretische Physik Goethe-Universität Frankfurt Max-von-Laue-Straße 1 Frankfurt am MainD-60438 Germany Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n GranadaE-18008 Spain Leiden Observatory—Allegro Leiden University P.O. Box

Very-long-baseline interferometry (VLBI) observations of active galactic nuclei at millimeter wavelengths have the power to reveal the launching and initial collimation region of extragalactic radio jets, down to 10 – 100 gravitational radii (rg ≡ GM/c2) scales in nearby sources 1. Centaurus A is the closest radio-loud source to Earth 2. It bridges the gap in mass and accretion rate between the supermassive black holes (SMBHs) in Messier 87 and our galactic center. A large southern declination of −43° has however prevented VLBI imaging of Centaurus A below λ 1 cm thus far. Here, we show the millimeter VLBI image of the source, which we obtained with the Event Horizon Telescope at 228 GHz. Compared to previous observations 3, we image Centaurus A’s jet at a tenfold higher frequency and sixteen times sharper resolution and thereby probe sub-lightday structures. We reveal a highly-collimated, asymmetrically edge-brightened jet as well as the fainter counterjet. We find that Centaurus A’s source structure resembles the jet in Messier 87 on ∼ 500 rg scales remarkably well. Furthermore, we identify the location of Centaurus A’s SMBH with respect to its resolved jet core at λ 1.3 mm and conclude that the source’s event horizon shadow 4 should be visible at THz frequencies. This location further supports the universal scale invariance of black holes over a wide range of masses 5,6 © 2021, CC BY.

关键词： Radio astronomy

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Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck. III. Combined cosmological constraints

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Physical Review D 2023年第2期107卷 023531-023531页

作者： T. M. C. Abbott M. Aguena A. Alarcon O. Alves A. Amon F. Andrade-Oliveira J. Annis B. Ansarinejad S. Avila D. Bacon E. J. Baxter K. Bechtol M. R. Becker B. A. Benson G. M. Bernstein E. Bertin J. Blazek L. E. Bleem S. Bocquet D. Brooks E. Buckley-Geer D. L. Burke H. Camacho A. Campos J. E. Carlstrom A. Carnero Rosell M. Carrasco Kind J. Carretero R. Cawthon C. Chang C. L. Chang R. Chen A. Choi R. Chown C. Conselice J. Cordero M. Costanzi T. Crawford A. T. Crites M. Crocce L. N. da Costa C. Davis T. M. Davis T. de Haan J. De Vicente J. DeRose S. Desai H. T. Diehl M. A. Dobbs S. Dodelson P. Doel C. Doux A. Drlica-Wagner K. Eckert T. F. Eifler F. Elsner J. Elvin-Poole S. Everett W. Everett X. Fang I. Ferrero A. Ferté B. Flaugher P. Fosalba O. Friedrich J. Frieman J. García-Bellido M. Gatti E. M. George T. Giannantonio G. Giannini D. Gruen R. A. Gruendl J. Gschwend G. Gutierrez N. W. Halverson I. Harrison K. Herner S. R. Hinton G. P. Holder D. L. Hollowood W. L. Holzapfel K. Honscheid J. D. Hrubes H. Huang E. M. Huff D. Huterer B. Jain D. J. James M. Jarvis T. Jeltema S. Kent L. Knox A. Kovacs E. Krause K. Kuehn N. Kuropatkin O. Lahav A. T. Lee P.-F. Leget P. Lemos A. R. Liddle C. Lidman D. Luong-Van J. J. McMahon N. MacCrann M. March J. L. Marshall P. Martini J. McCullough P. Melchior F. Menanteau S. S. Meyer R. Miquel L. Mocanu J. J. Mohr R. Morgan J. Muir J. Myles T. Natoli A. Navarro-Alsina R. C. Nichol Y. Omori S. Padin S. Pandey Y. Park F. Paz-Chinchón M. E. S. Pereira A. Pieres A. A. Plazas Malagón A. Porredon J. Prat C. Pryke M. Raveri C. L. Reichardt R. P. Rollins A. K. Romer A. Roodman R. Rosenfeld A. J. Ross J. E. Ruhl E. S. Rykoff C. Sánchez E. Sanchez J. Sanchez K. K. Schaffer L. F. Secco I. Sevilla-Noarbe E. Sheldon T. Shin E. Shirokoff M. Smith Z. Staniszewski A. A. Stark E. Suchyta M. E. C. Swanson G. Tarle C. To M. A. Troxel I. Tutusaus T. N. Varga J. D. Vieira N. Weaverdyck R. H. Wechsler J. Weller R. Williamson W. L. K. Wu B. Yanny B. Yin Y. Zhang J. Zuntz Cerro Tololo Inter-American Observatory NSF’s National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Laboratório Interinstitucional de e-Astronomia–LIneA Rua Gal. José Cristino 77 Rio de Janeiro RJ–20921-400 Brazil Argonne National Laboratory 9700 South Cass Avenue Lemont Illinois 60439 USA Department of Physics University of Michigan Ann Arbor Michigan 48109 USA Institute of Astronomy University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road Cambridge CB3 0HA United Kingdom Fermi National Accelerator Laboratory P. O. Box 500 Batavia Illinois 60510 USA School of Physics University of Melbourne Parkville VIC 3010 Australia Instituto de Fisica Teorica UAM/CSIC Universidad Autonoma de Madrid 28049 Madrid Spain Institute of Cosmology and Gravitation University of Portsmouth Portsmouth PO1 3FX United Kingdom Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive Honolulu Hawaii 96822 USA Physics Department 2320 Chamberlin Hall University of Wisconsin-Madison 1150 University Avenue Madison Wisconsin 53706-1390 USA Department of Astronomy and Astrophysics University of Chicago Chicago Illinois 60637 USA Kavli Institute for Cosmological Physics University of Chicago Chicago Illinois 60637 USA Department of Physics and Astronomy University of Pennsylvania Philadelphia Pennsylvania 19104 USA CNRS UMR 7095 Institut d’Astrophysique de Paris F-75014 Paris France Sorbonne Universités UPMC Univ Paris 06 UMR 7095 Institut d’Astrophysique de Paris F-75014 Paris France Department of Physics Northeastern University Boston Massachusetts 02115 USA High-Energy Physics Division Argonne National Laboratory 9700 South Cass Avenue Argonne Illinois 60439 USA University Observatory Faculty of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 81679 Munich Germany Department of Physics and Astronomy University College London Gower Stre

We present cosmological constraints from the analysis of two-point correlation functions between galaxy positions and galaxy lensing measured in Dark Energy Survey (DES) Year 3 data and measurements of cosmic microwave background (CMB) lensing from the South Pole Telescope (SPT) and Planck. When jointly analyzing the DES-only two-point functions and the DES cross-correlations with SPT+Planck CMB lensing, we find Ωm=0.344±0.030 and S8≡σ8(Ωm/0.3)0.5=0.773±0.016, assuming ΛCDM. When additionally combining with measurements of the CMB lensing autospectrum, we find Ωm=0.306−0.021+0.018 and S8=0.792±0.012. The high signal-to-noise of the CMB lensing cross-correlations enables several powerful consistency tests of these results, including comparisons with constraints derived from cross-correlations only, and comparisons designed to test the robustness of the galaxy lensing and clustering measurements from DES. Applying these tests to our measurements, we find no evidence of significant biases in the baseline cosmological constraints from the DES-only analyses or from the joint analyses with CMB lensing cross-correlations. However, the CMB lensing cross-correlations suggest possible problems with the correlation function measurements using alternative lens galaxy samples, in particular the redmagic galaxies and high-redshift maglim galaxies, consistent with the findings of previous studies. We use the CMB lensing cross-correlations to identify directions for further investigating these problems.

关键词： Cosmic microwave background Cosmological constant Cosmological parameters Dark energy Dark matter Evolution of the Universe Large scale structure of the Universe Optical, UV, & IR astronomy Normal galaxies

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Analysis of Mesoscale Convective Complex during Madden Julian Oscillation Phase 4 (Case Study: Heavy rain in Cilacap on Sept 16-17, 2016)

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IOP Conference Series: Earth and Environmental science 2019年第1期303卷

作者： L F Aiqiu A Zakir Trismidianto Undergraduate program of Meteorology State College of Meteorology Climatology and GeophysicsJakarta Indonesia Lecturer Department of Meteorology State College of Meteorology Climatology and GeophysicsJakarta Indonesia Center for Atmospheric Science and Technology National Institute of Aeronautics and SpaceBandung Indonesia

This research aims to analyze the heavy rain which accompanied by severe winds, caused floods and landslides in several of sub-districts in Cilacap, Central Java on 16-17 September 2016 that coincides with the phase 4 of Madden Jullian Oscillation (MJO) event. In the same time, also found a Mesoscale Convective Complex (MCC) in the around Central Java. MCCs were identified by infrared satellite imagery from Himawari 8 using an algorithm that combines criteria of cloud coverage, eccentricity, and cloud lifetime. The data used is a combination of observation data, satellite data and reanalysis data. This study results that there is an increase in vertical velocity accompanied by strong negative vorticity since the development of MCC until it reached its mature phase, then the vertical velocity decreases as the cloud systems disseminated. These results indicate there is the evolution of MCC convective cells from growth until dissipation. Throughout its lifetime the MCC system moves south-east into the Indian Ocean and is decapitated there. Based on GSMaP rainfall data it was observed that in Central Java area especially Cilacap area has extreme rainfall which caused by MCC activity. The influence of MCC on significant rainfall is also supported by the existence of MJO phase 4. The significant increase in rainfall when phase 4 active MJO is followed by the MCC. The value of rainfall intensity when MJO followed by the presence of MCC is greater than in the absence of MCC.

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The DESI Survey Validation: Results from Visual Inspection of Bright Galaxies, Luminous Red Galaxies, and Emission Line Galaxies

arXiv

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arXiv 2022年

作者： Lan, Ting-Wen Tojeiro, R. Armengaud, E. Prochaska, J. Xavier Davis, T.M. Alexander, David M. Raichoor, A. Zhou, Rongpu Yèche, Christophe Balland, C. BenZvi, S. Berti, A. Canning, R. Carr, A. Chittenden, H. Cole, S. Cousinou, M.-C. Dawson, K. Dey, Biprateep Douglass, K. Edge, A. Escoffier, S. Glanville, A. Gontcho, S.A. Gontcho Guy, J. Hahn, C. Howlett, C. Hwang, Ho Seong Jiang, L. Kovács, A. Mezcua, M. Moore, S. Nadathur, S. Oh, M. Parkinson, D. Rocher, A. Ross, A.J. Ruhlmann-Kleider, V. Sabiu, C.G. Said, K. Saulder, C. Sierra-Porta, D. Weiner, B. Yu, J. Zarrouk, P. Zhang, Y. Zou, H. Ahlen, S. Bailey, S. Brooks, D. Cooper, A.P. de la Macorra, A. Dey, A. Dhungana, G. Doel, P. Eftekharzadeh, S. Fanning, K. Font-Ribera, A. Garrison, L. Gaztañaga, E. Kehoe, R. Kisner, T. Kremin, A. Landriau, M. Le Guillou, L. Levi, Michael E. Magneville, C. Meisner, Aaron M. Miquel, R. Moustakas, J. Myers, Adam D. Newman, Jeffrey A. Nie, J.D. Palanque-Delabrouille, N. Percival, W.J. Poppett, C. Prada, F. Schubnell, M. Tarlé, Gregory Weaver, B.A. Zhang, K. Zhou, Zhimin Graduate Institute of Astrophysics Department of Physics National Taiwan University No. 1 Sec. 4 Roosevelt Rd. Taipei10617 Taiwan Department of Astronomy and Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA95065 United States SUPA School of Physics and Astronomy University of St Andrews St AndrewsKY16 9SS United Kingdom IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France The University of Tokyo Chiba Kashiwa Kashiwa277-8583 Japan School of Mathematics and Physics University of Queensland 4072 Australia Centre for Extragalactic Astronomy Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States ParisFR-75005 France Department of Physics & Astronomy University of Rochester 206 Bausch and Lomb Hall P.O. Box 270171 RochesterNY14627-0171 United States Department of Physics and Astronomy The University of Utah 115 South 1400 East Salt Lake CityUT84112 United States Institute of Cosmology & Gravitation University of Portsmouth Dennis Sciama Building PortsmouthPO1 3FX United Kingdom Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Aix Marseille Univ CNRS IN2P3 CPPM Marseille France University of Pittsburgh 3941 O’Hara Street PittsburghPA15260 United States Department of Astrophysical Sciences Princeton University Peyton Hall PrincetonNJ08544 United States Lawrence Berkeley National Laboratory One Cyclotron Road BerkeleyCA94720 United States Astronomy Program Department of Physics and Astronomy Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of SNU Astronomy Research Center Seoul National University 1 Gwanak-ro Gwanak-gu Seoul08826 Korea Republic of 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Kavli Institute for Astronomy and Astrophysics Peking Unive

The Dark Energy Spectroscopic Instrument (DESI) Survey has obtained a set of spectroscopic measurements of galaxies to validate the final survey design and target selections. To assist in these tasks, we visually inspect (VI) DESI spectra of approximately 2,500 bright galaxies, 3,500 luminous red galaxies (LRGs), and 10,000 emission line galaxies (ELGs), to obtain robust redshift identifications. We then utilize the VI redshift information to characterize the performance of the DESI operation. Based on the VI catalogs, our results show that the final survey design yields samples of bright galaxies, LRGs, and ELGs with purity greater than 99%. Moreover, we demonstrate that the precision of the redshift measurements is approximately 10 km/s for bright galaxies and ELGs and approximately 40 km/s for LRGs. The average redshift accuracy is within 10 km/s for the three types of galaxies. The VI process also helps improve the quality of the DESI data by identifying spurious spectral features introduced by the pipeline. Finally, we show examples of unexpected real astronomical objects, such as Lyα emitters and strong lensing candidates, identified by VI. These results demonstrate the importance and utility of visually inspecting data from incoming and upcoming surveys, especially during their early operation phases. © 2022, CC BY.

关键词： Galaxies

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