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arXiv 2020年

作者： Ho, Anna Y.Q. Kulkarni, S.R. Perley, Daniel A. Bradley Cenko, S. Corsi, Alessandra Schulze, Steve Lunnan, Ragnhild Sollerman, Jesper Gal-Yam, Avishay Anand, Shreya Barbarino, Cristina Bellm, Eric C. Bruch, Rachel J. Burns, Eric De, Kishalay Dekany, Richard Delacroix, Alexandre Duev, Dmitry A. Fremling, Christoffer Goldstein, Daniel A. Zach Golkhou, V. Graham, Matthew J. Hale, David Kasliwal, Mansi M. Kupfer, Thomas Laher, Russ R. Martikainen, Julia Masci, Frank J. Neill, James D. Rusholme, Ben Shupe, David L. Soumagnac, Maayane T. Strotjohann, Nora L. Taggart, Kirsty Tartaglia, Leonardo Yan, Lin Zolkower, Jeffry Cahill Center for Astrophysics California Institute of Technology MC 249-17 1200 E California Boulevard PasadenaCA91125 United States Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Astrophysics Science Division NASA Goddard Space Flight Center Mail Code 661 GreenbeltMD20771 United States Joint Space-Science Institute University of Maryland College ParkMD20742 United States Department of Physics and Astronomy Texas Tech University Box 1051 LubbockTX79409-1051 United States Department of Particle Physics and Astrophysics Weizmann Institute of Science 234 Herzl St Rehovot76100 Israel The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-106 91 Sweden Division of Physics Mathematics and Astronomy California Institute of Technology PasadenaCA91125 United States DIRAC Institute Department of Astronomy University of Washington 3910 15th Avenue NE SeattleWA98195 United States Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot76100 Israel NASA Postdoctoral Program Fellow Goddard Space Flight Center GreenbeltMD20771 United States Department of Physics & Astronomy Louisiana State University Baton RougeLA70803 United States Caltech Optical Observatories California Institute of Technology PasadenaCA91125 United States eScience Institute University of Washington SeattleWA98195 United States Kavli Institute for Theoretical Physics University of California Santa BarbaraCA93106 United States IPAC California Institute of Technology 1200 E. California Blvd PasadenaCA91125 United States Department of Physics University of Helsinki P.O. box 64 FI-00014 Finland Nordic Optical Telescope Roque de Los Muchachos Observatory Rambla Jos Ana Fernndez Prez 7 Brea Baja La Palma Canarias38711 Spain Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United Sta

We present optical, radio, and X-ray observations of SN 2020bvc (=ASASSN20bs;ZTF20aalxlis), a nearby (z = 0.0252;d = 114 Mpc) broad-lined (BL) Type Ic supernova (SN). Our observations show that SN 2020bvc shares several properties in common with the Ic-BL SN 2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio light curve is on the faint end of LLGRB-SNe (Lradio ≈ 1037 erg s−1): we model our VLA observations (spanning 13-43 d) as synchrotron emission from a mildly relativistic (v & 0.3c) forward shock. Second, with Swift and Chandra we detect X-ray emission (LX ≈ 1041 erg s−1) that is not naturally explained as inverse Compton emission or as part of the same synchrotron spectrum as the radio emission. Third, high-cadence (6×/night) data from the Zwicky Transient Facility (ZTF) shows a double-peaked optical light curve, the first peak from shock-cooling emission from extended low-mass material (mass M −2 M at radius R > 1012 cm) and the second peak from the radioactive decay of 56Ni. SN 2020bvc is the first confirmed double-peaked Ic-BL SN discovered without a GRB trigger, and shows X-ray and radio emission similar to LLGRB-SNe: this is consistent with models in which the same mechanism produces both the LLGRB and the shock-cooling emission. For four of the five other nearby (z. 0.05) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN 2006aj and SN 2020bvc, i.e. that lasts ≈ 1 d and reaches a peak luminosity M ≈ −18. X-ray and radio follow-up observations of future such events will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission. Copyright © 2020, The Authors. All rights reserved.

关键词： Supernovae

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Searching for Gravitational Waves from Cosmological Phase Transitions with the NANOGrav 12.5-Year Dataset

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Physical Review Letters 2021年第25期127卷 251302-251302页

作者： Zaven Arzoumanian Paul T. Baker Harsha Blumer Bence Bécsy Adam Brazier Paul R. Brook Sarah Burke-Spolaor Maria Charisi Shami Chatterjee Siyuan Chen James M. Cordes Neil J. Cornish Fronefield Crawford H. Thankful Cromartie Megan E. DeCesar Paul B. Demorest Timothy Dolch Justin A. Ellis Elizabeth C. Ferrara William Fiore Emmanuel Fonseca Nathan Garver-Daniels Peter A. Gentile Deborah C. Good Jeffrey S. Hazboun A. Miguel Holgado Kristina Islo Ross J. Jennings Megan L. Jones Andrew R. Kaiser David L. Kaplan Luke Zoltan Kelley Joey Shapiro Key Nima Laal Michael T. Lam T. Joseph W. Lazio Vincent S. H. Lee Duncan R. Lorimer Jing Luo Ryan S. Lynch Dustin R. Madison Maura A. McLaughlin Chiara M. F. Mingarelli Andrea Mitridate Cherry Ng David J. Nice Timothy T. Pennucci Nihan S. Pol Scott M. Ransom Paul S. Ray Brent J. Shapiro-Albert Xavier Siemens Joseph Simon Renée Spiewak Ingrid H. Stairs Daniel R. Stinebring Kevin Stovall Jerry P. Sun Joseph K. Swiggum Stephen R. Taylor Jacob E. Turner Michele Vallisneri Sarah J. Vigeland Caitlin A. Witt Kathryn M. Zurek X-Ray Astrophysics Laboratory NASA Goddard Space Flight Center Code 662 Greenbelt Maryland 20771 USA Department of Physics and Astronomy Widener University One University Place Chester Pennsylvania 19013 USA Department of Physics and Astronomy West Virginia University P.O. Box 6315 Morgantown West Virginia 26506 USA Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building Morgantown West Virginia 26505 USA Department of Physics Montana State University Bozeman Montana 59717 USA Cornell Center for Astrophysics and Planetary Science and Department of Astronomy Cornell University Ithaca New York 14853 USA Cornell Center for Advanced Computing Cornell University Ithaca New York 14853 USA CIFAR Azrieli Global Scholars program CIFAR Toronto Canada Department of Physics and Astronomy Vanderbilt University 2301 Vanderbilt Place Nashville Tennessee 37235 USA Station de Radioastronomie de Nancay Observatoire de Paris Universite PSL CNRS Universite d’Orleans 18330 Nancay France FEMTO-ST Institut de recherche Department of Time and Frequency UBFC and CNRS ENSMM 25030 Besancon France Laboratoire de Physique et Chimie de l’Environment et de l’Espace LPC2E UMR7328 Universite d’Orleans CNRS 45071 Orleans France Department of Physics and Astronomy Franklin & Marshall College P.O. Box 3003 Lancaster Pennsylvania 17604 USA Department of Physics Lafayette College Easton Pennsylvania 18042 USA George Mason University Fairfax Virginia 22030 USA National Radio Astronomy Observatory 1003 Lopezville Road Socorro New Mexico 87801 USA Department of Physics Hillsdale College 33 E. College Street Hillsdale Michigan 49242 USA Eureka Scientific Inc. 2452 Delmer Street Suite 100 Oakland California 94602-3017 Infinia ML 202 Rigsbee Avenue Durham North Carolina 27701 USA Department of Astronomy University of Maryland College Park Maryland 20742 USA Center for Research and Exploration in Space Science and Technolog

We search for a first-order phase transition gravitational wave signal in 45 pulsars from the NANOGrav 12.5-year dataset. We find that the data can be modeled in terms of a strong first order phase transition taking place at temperatures below the electroweak scale. However, we do not observe any strong preference for a phase-transition interpretation of the signal over the standard astrophysical interpretation in terms of supermassive black hole mergers; but we expect to gain additional discriminating power with future datasets, improving the signal to noise ratio and extending the sensitivity window to lower frequencies. An interesting open question is how well gravitational wave observatories could separate such signals.

关键词： First order phase transitions Gravitational wave detection Gravitational wave sources Gravitational waves

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The Birth of a Relativistic Jet Following the Disruption of a Star by a Cosmological Black Hole

arXiv

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arXiv 2022年

作者： Pasham, Dheeraj R. Lucchini, Matteo Laskar, Tanmoy Gompertz, Benjamin P. Srivastav, Shubham Nicholl, Matt Smartt, Stephen J. Miller-Jones, James C.A. Alexander, Kate D. Fender, Rob Smith, Graham P. Fulton, Michael D. Dewangan, Gulab Gendreau, Keith Coughlin, Eric R. Rhodes, Lauren Horesh, Assaf van Velzen, Sjoert Sfaradi, Itai Guolo, Muryel Segura, N. Castro Aamer, Aysha Anderson, Joseph P. Arcavi, Iair Brennan, Seán J. Chambers, Kenneth Charalampopoulos, Panos Chen, Ting-Wan Clocchiatti, A. de Boer, Thomas Dennefeld, Michel Ferrara, Elizabeth Galbany, Lluís Gao, Hua Gillanders, James H. Goodwin, Adelle Gromadzki, Mariusz Huber, M. Jonker, Peter G. Joshi, Manasvita Kara, Erin Killestein, Thomas L. Kosec, Peter Kocevski, Daniel Leloudas, Giorgos Lin, Chien-Cheng Margutti, Raffaella Mattila, Seppo Moore, Thomas Müller-Bravo, Tomás Ngeow, Chow-Choong Oates, Samantha Onori, Francesca Pan, Yen-Chen Pérez-Torres, Miguel Rani, Priyanka Remillard, Ronald Ridley, Evan J. Schulze, Steve Sheng, Xinyue Shingles, Luke Smith, Ken W. Steiner, James Wainscoat, Richard Wevers, Thomas Yang, Sheng Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology CambridgeMA United States Department of Astrophysics IMAPP Radboud University PO Box 9010 6500 GL Netherlands Institute of Gravitational Wave Astronomy University of Birmingham B15 2TT United Kingdom School of Physics and Astronomy University of Birmingham B15 2TT United Kingdom Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast Belfast BT7 1NN United Kingdom International Centre for Radio Astronomy Research Curtin University GPO Box U1987 PerthWA6845 Australia Department of Physics and Astronomy Northwestern University 1800 Sherman Ave EvanstonIL60201 United States Astrophysics Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Inter-University Centre for Astronomy and Astrophysics Pune India NASA Goddard Space Flight Center GreenbeltMD United States Department of Physics Syracuse University SyracuseNY United States Racah Institute of Physics The Hebrew University of Jerusalem Jerusalem91904 Israel Leiden Observatory Leiden University Postbus 9513 Leiden2300 RA Netherlands Department of Physics and Astronomy Johns Hopkins University 3400 N. Charles St. BaltimoreMD21218 United States Department of Physics & Astronomy University of Southampton SouthamptonSO17 1BJ United Kingdom European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel CIFAR Azrieli Global Scholars program CIFAR Toronto Canada School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Institute for Astronomy University of Hawaii United States DTU Space National Space Institute Technical University of Denmark Elektrovej 327 Kgs. Lyngby2800 Denmark The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden Institut

A black hole can launch a powerful relativistic jet after it tidally disrupts a star. If this jet fortuitously aligns with our line of sight, the overall brightness is Doppler boosted by several orders of magnitude. Consequently, such on-axis relativistic tidal disruption events (TDEs) have the potential to unveil cosmological (redshift z >1) quiescent black holes and are ideal test beds to understand the radiative mechanisms operating in super-Eddington jets. Here, we present multi-wavelength (X-ray, UV, optical, and radio) observations of the optically discovered transient AT 2022cmc at z = 1.193. Its unusual X-ray properties, including a peak observed luminosity of ≿1048 erg s−1, systematic variability on timescales as short as 1000 seconds, and overall duration lasting more than 30 days in the rest-frame are traits associated with relativistic TDEs. The X-ray to radio spectral energy distributions spanning 5-50 days after discovery can be explained as synchrotron emission from a relativistic jet (radio), synchrotron self-Compton (X-rays), and thermal emission similar to that seen in low-redshift TDEs (UV/optical). Our modeling implies a beamed, highly relativistic jet akin to blazars but requires extreme matter-domination, i.e, high ratio of electron-to-magnetic field energy densities in the jet, and challenges our theoretical understanding of jets. © 2022, CC BY.

关键词： Luminance

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Open Data from the Third Observing Run of LIGO, Virgo, KAGRA, and GEO

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Astrophysical Journal, Supplement Series 2023年第2期267卷 29-29页

作者： Abbott, R. Abe, H. Acernese, F. Ackley, K. Adhicary, S. Adhikari, N. Adhikari, R.X. Adkins, V.K. Adya, V.B. Affeldt, C. Agarwal, D. Agathos, M. Aguiar, O.D. Aiello, L. Ain, A. Ajith, P. Akutsu, T. Albanesi, S. Alfaidi, R.A. Al-Jodah, A. Alléné, C. Allocca, A. Almualla, M. Altin, P.A. Amato, A. Amez-Droz, L. Amorosi, A. Anand, S. Ananyeva, A. Andersen, R. Anderson, S.B. Anderson, W.G. Andia, M. Ando, M. Andrade, T. Andres, N. Andrés-Carcasona, M. Andrić, T. Ansoldi, S. Antelis, J.M. Antier, S. Aoumi, M. Apostolatos, T. Appavuravther, E.Z. Appert, S. Apple, S.K. Arai, K. Araya, A. Araya, M.C. Areeda, J.S. Arène, M. Aritomi, N. Arnaud, N. Arogeti, M. Aronson, S.M. Arun, K.G. Asada, H. Ashton, G. Aso, Y. Assiduo, M. Assis de Souza Melo, S. Aston, S.M. Astone, P. Aubin, F. AultONeal, K. Babak, S. Badalyan, A. Badaracco, F. Badger, C. Bae, S. Bagnasco, S. Bai, Y. Baier, J.G. Baiotti, L. Baird, J. Bajpai, R. Baka, T. Ball, M. Ballardin, G. Ballmer, S.W. Baltus, G. Banagiri, S. Banerjee, B. Bankar, D. Baral, P. Barayoga, J.C. Barber, J. Barish, B.C. Barker, D. Barneo, P. Barone, F. Barr, B. Barsotti, L. Barsuglia, M. Barta, D. Barthelmy, S.D. Barton, M.A. Bartos, I. Basak, S. Basalaev, A. Bassiri, R. Basti, A. Bawaj, M. Bayley, J.C. Baylor, A.C. Bazzan, M. Bécsy, B. Bedakihale, V.M. Beirnaert, F. Bejger, M. Bell, A.S. Benedetto, V. Beniwal, D. Benoit, W. Bentley, J.D. Ben Yaala, M. Bera, S. Berbel, M. Bergamin, F. Berger, B.K. Bernuzzi, S. Beroiz, M. Berry, C.P.L. Bersanetti, D. Bertolini, A. Betzwieser, J. Beveridge, D. Bevins, N. Bhandare, R. Bhandari, A.V. Bhardwaj, U. Bhatt, R. Bhattacharjee, D. Bhaumik, S. Bianchi, A. Bilenko, I.A. Bilicki, M. Billingsley, G. Bini, S. Birnholtz, O. Biscans, S. Bischi, M. Biscoveanu, S. Bisht, A. Biswas, B. Bitossi, M. Bizouard, M.-A. Blackburn, J.K. Blair, C.D. Blair, D.G. Blair, R.M. Bobba, F. Bode, N. Boër, M. Bogaert, G. Boileau, G. Boldrini, M. Bolingbroke, G.N. Bonavena, L.D. Bondarescu, R. Bondu, F. Bonilla, E. Bonilla, G.S. Bonnand, R. Booker, P. Bork, R. Boschi, V. Bose, N. LIGO Laboratory California Institute of Technology Pasadena 91125 CA United States Graduate School of Science Tokyo Institute of Technology 2-12-1 Ookayama Meguro-ku Tokyo 152-8551 Japan Dipartimento di Farmacia Università di Salerno Salerno Fisciano I-84084 Italy INFN Sezione di Napoli Napoli I-80126 Italy OzGrav School of Physics & Astronomy Monash University Clayton 3800 VIC Australia The Pennsylvania State University University Park 16802 PA United States University of Wisconsin-Milwaukee Milwaukee 53201 WI United States Louisiana State University Baton Rouge 70803 LA United States OzGrav Australian National University Canberra 0200 ACT Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) Hannover D-30167 Germany Leibniz Universität Hannover Hannover D-30167 Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Instituto Nacional de Pesquisas Espaciais São Paulo São José dos Campos 12227-010 Brazil Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa Pisa I-56127 Italy International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India Gravitational Wave Science Project National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka City Tokyo 181-8588 Japan Dipartimento di Fisica Università degli Studi di Torino Torino I-10125 Italy INFN Sezione di Torino Torino I-10125 Italy SUPA University of Glasgow Glasgow G12 8QQ United Kingdom OzGrav University of Western Australia Crawley 6009 WA Australia Univ. Savoie Mont Blanc CNRS Laboratoire d'Annecy de Physique des Particules - IN2P3 Annecy F-74000 France Università di Napoli “Federico II” Napoli I-80126 Italy University of Minnesota Minneapolis 55455 MN United States M

The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open science Center at https://***. The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages. © 2023. The Author(s). Published by the American Astronomical Society.

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Intensive monitoring survey of nearby galaxies (IMSNG)

arXiv

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arXiv 2019年

作者： Im, Myungshin Choi, Changsu Hwang, Sungyong Lim, Gu Kim, Joonho Kim, Sophia Paek, Gregory S.H. Lee, Sang-Yun Yoon, Sung-Chul Jung, Hyunjin Sung, Hyun-Il Jeon, Yeong-beom Ehgamberdiev, Shuhrat Burhonov, Otabek Milzaqulov, Davron Parmonov, Omon Lee, Sang Gak Kang, Wonseok Kim, Taewoo Kwon, Sun-gill Pak, Soojong Ji, Tae-Geun Lee, Hye-In Park, Woojin Ahn, Hojae Byeon, Seoyeon Han, Jimin Gibson, Coyne Wheeler, J. Craig Kuehne, John Johns-Krull, Chris Marshall, Jennifer Hyun, Minhee Lee, Seong-Kook J. Kim, Yongjung Yoon, Yongmin Paek, Insu Shin, Suhyun Taak, Yoon Chan Kang, Juhyung Choi, Seoyeon Jeong, Mankeun Jung, Moo-Keon Kim, Hwara Kim, Jisu Lee, Dayae Park, Bomi Park, Keunwoo Seong, A.O. Center for the Exploration of the Origin of the Universe Department of Physics and Astronomy Seoul National University Gwanak-gu Seoul08826 Korea Republic of Astronomy Program Department of Physics and Astronomy Seoul National University Gwanak-gu Seoul151-742 Korea Republic of Department of Physics Pohang University of Science and Technology 77 Cheongam-Ro Nam-Gu Pohang Gyeongbuk37673 Korea Republic of Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Ulugh Beg Astronomical Institute Uzbek Academy of Sciences 33 Astronomical Street Tashkent700052 Uzbekistan National Youth Space Center Goheung Jeollanam-do59567 Korea Republic of Department of Astronomy and Space Science Chungbuk National University Cheongju-City28644 Korea Republic of School of Space Research Kyung Hee University 1732 Deogyeong-daero Giheung-gu Yongin-si Gyeonggi-do17104 Korea Republic of Department of Astronomy and Space Science Kyung Hee University 1732 Deogyeong-daero Giheung-gu Yongin-si Gyeonggi-do17104 Korea Republic of McDonald Observatory University of Texas at Austin 3640 Dark Sky Drive Fort DavisTX79734 United States Department of Astronomy University of Texas at Austin 2515 Speedway AustinTX78712 United States Department of Physics & Astronomy Rice University 6100 Main St. MS-108 HoustonTX77005 United States Mitchell Institute for Fundamental Physics and Astronomy Department of Physics and Astronomy Texas A&M University College StationTX77843-4242 United States Phillips Academy 180 Main St AndoverMA01810 United States Department of Earth Science Education Seoul National University Gwanak-gu Seoul151-742 Korea Republic of Department of Astronomy Yonsei University 50 Yonsei-ro Seodaemun-gu Seoul03722 Korea Republic of Department of Astronomy and Space Science Sejong University 209 Neungdong-ro Kwangjin-gu Seoul05006 Korea Republic of

Intensive Monitoring Survey of Nearby Galaxies (IMSNG) is a high cadence observation program monitoring nearby galaxies with high probabilities of hosting supernovae (SNe). IMSNG aims to constrain the SN explosion mechanism by inferring sizes of SN progenitor systems through the detection of the shock-heated emission that lasts less than a few days after the SN explosion. To catch the signal, IMSNG utilizes a network of 0.5-m to 1-m class telescopes around the world and monitors the images of 60 nearby galaxies at distances D NUV −1 per galaxy). With this strategy, we expect to detect the early light curves of 3.4 SNe per year to a depth of R ∼ 19.5 mag, enabling us to detect the shock-heated emission from a progenitor star with a radius as small as 0.1 R∙. The accumulated data will be also useful for studying faint features around the target galaxies and other science projects. So far, 18 SNe have occurred in our target fields (16 in IMSNG galaxies) over 5 years, confirming our SN rate estimate of 0.06 SN yr−1 per galaxy. Copyright © 2019, The Authors. All rights reserved.

关键词： Galaxies

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Millimeter light curves of Sagittarius A∗ observed during the 2017 Event Horizon Telescope campaign

arXiv

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arXiv 2022年

作者： Wielgus, Maciek Marchili, Nicola Martí-Vidal, Iván Keating, Garrett K. Ramakrishnan, Venkatessh Tiede, Paul Fomalont, Ed Issaoun, Sara Neilsen, Joey Nowak, Michael A. Blackburn, Lindy Gammie, Charles F. Goddi, Ciriaco Haggard, Daryl Lee, Daeyoung Moscibrodzka, Monika Tetarenko, Alexandra J. Bower, Geoffrey C. Chan, Chi-Kwan Chatterjee, Koushik Chesler, Paul M. Dexter, Jason Doeleman, Sheperd S. Georgiev, Boris Gurwell, Mark Johnson, Michael D. Marrone, Daniel P. Mus, Alejandro Psaltis, Dimitrios Ripperda, Bart Witzel, Gunther Akiyama, Kazunori Alberdi, Antxon Alef, Walter Algaba, Juan Carlos Anantua, Richard Asada, Keiichi Azulay, Rebecca Bach, Uwe Baczko, Anne-Kathrin Ball, David Baloković, Mislav Barrett, John Bauböck, Michi Benson, Bradford A. Bintley, Dan Blundell, Raymond Boland, Wilfred Bouman, Katherine L. Boyce, Hope Bremer, Michael Brinkerink, Christiaan D. Brissenden, Roger Britzen, Silke Broderick, Avery E. Broguiere, Dominique Bronzwaer, Thomas Bustamante, Sandra Byun, Do-Young Carlstrom, John E. Ceccobello, Chiara Chael, Andrew Chatterjee, Shami Chen, Ming-Tang Chen, Yongjun Cho, Ilje Christian, Pierre Conroy, Nicholas S. Conway, John E. Cordes, James M. Crawford, Thomas M. Crew, Geoffrey B. Cruz-Osorio, Alejandro Cui, Yuzhu Davelaar, Jordy de Laurentis, Mariafelicia Deane, Roger Dempsey, Jessica Desvignes, Gregory Dhruv, Vedant Dzib, Sergio A. Eatough, Ralph P. Emami, Razieh Falcke, Heino Farah, Joseph Fish, Vincent L. Alyson Ford, H. Fraga-Encinas, Raquel Freeman, William T. Friberg, Per Fromm, Christian M. Fuentes, Antonio Galison, Peter García, Roberto Gentaz, Olivier Gold, Roman Gómez-Ruiz, Arturo I. Gómez, José L. Gu, Minfeng Hada, Kazuhiro Haworth, Kari Hecht, Michael H. Hesper, Ronald Ho, Luis C. Ho, Paul Honma, Mareki Huang, Chih-Wei L. Huang, Lei Hughes, David H. Ikeda, Shiro Violette Impellizzeri, C.M. Inoue, Makoto James, David J. Jannuzi, Buell T. Janssen, Michael Jeter, Britton Jiang, Wu Jiménez-Rosales, Alejandra Jorstad, Svetlana Joshi, Abhishek V. Jung, Taehyun Karami, Mansour Karupp Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Italian ALMA Regional Centre INAF-Istituto di Radioastronomia Via P. Gobetti 101 BolognaI-40129 Italy Departament d’Astronomia i Astrofísica Universitat de València C. Dr. Moliner 50 Burjassot ValènciaE-46100 Spain Observatori Astronòmic Universitat de València C. Catedrático José Beltrán 2 Paterna ValenciaE-46980 Spain Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Astronomy Department Universidad de Concepción Casilla 160-C Concepción Chile Finnish Centre for Astronomy with ESO University of Turku FI-20014 Finland Aalto University Metsähovi Radio Observatory Metsähovintie 114 KylmäläFI-02540 Finland Harvard University 20 Garden Street CambridgeMA02138 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States NASA Hubble Fellowship Program Einstein Fellow United States Villanova University Mendel Science Center Rm. 263B 800 E Lancaster Ave VillanovaPA19085 United States Physics Department Washington University CB 1105 St LouisMO63130 United States Department of Physics University of Illinois 1110 West Green Street UrbanaIL61801 United States Department of Astronomy University of Illinois at Urbana-Champaign 1002 West Green Street UrbanaIL61801 United States Dipartimento di Fisica Università degli Studi di Cagliari SP Monserrato-Sestu km 0.7 MonserratoI-09042 Italy INAF - Osservatorio Astronomico di Cagliari Via della Scienza 5 CA Selargius09047 Italy Department of Physics McGill University 3600 rue University MontréalQCH3A 2T8 Canada McGill Space Institute McGill University 3550 rue University MontréalQCH3A 2A7 Canada Radboud University P.O. Box 9010 Nijmegen6500 GL Netherlands Department of Physics and Astronomy Texas Tech University LubbockTX79409-1051 United States Institute of Astronomy and Astrophysics Academia Sinica 645 N. A’oho

The Event Horizon Telescope (EHT) observed the compact radio source, Sagittarius A∗ (Sgr A∗), in the Galactic Center on 2017 April 5-11 in the 1.3 millimeter wavelength band. At the same time, interferometric array data from the Atacama Large Millimeter/submillimeter Array and the Submillimeter Array were collected, providing Sgr A∗ light curves simultaneous with the EHT observations. These data sets, complementing the EHT very-long-baseline interferometry, are characterized by a cadence and signal-to-noise ratio previously unattainable for Sgr A∗ at millimeter wavelengths, and they allow for the investigation of source variability on timescales as short as a minute. While most of the light curves correspond to a low variability state of Sgr A∗, the April 11 observations follow an X-ray flare, and exhibit strongly enhanced variability. All of the light curves are consistent with a red noise process, with a power spectral density (PSD) slope measured to be between -2 and -3 on timescales between 1 min and several hours. Our results indicate a steepening of the PSD slope for timescales shorter than 0.3 h. The spectral energy distribution is flat at 220 GHz and there are no time-lags between the 213 and 229 GHz frequency bands, suggesting low optical depth for the event horizon scale source. We characterize Sgr A∗’s variability, highlighting the different behavior observed just after the X-ray flare, and use Gaussian process modeling to extract a decorrelation timescale and a PSD slope. We also investigate the systematic calibration uncertainties by analyzing data from independent data reduction pipelines. © 2022, CC BY.

关键词： Signal to noise ratio

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Correction to: Simultaneous multicolour transit photometry of hot Jupiters HAT-P-19b, HAT-P-51b, HAT-P-55b, and HAT-P-65b

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Monthly Notices of the Royal Astronomical Society 2024年第4期531卷 4929-4929页

作者： Kang, H Chen, G Pallé, E Murgas, F García, N Abreu de Leon, J Enoc, G Esparza-Borges, E Fukuda, I Fukui, A Galán, D Hayashi, Y Isogai, K Kagetani, T Kawauchi, K Korth, J Livingston, J H Luque, R Ma, Y Madrigal-Aguado, A Meni, P Rodriguez, P Montañes Mori, M Torres, S Muñoz Narita, N Orell-Miquel, J Parviainen, H Peláez-Torres, A Stangret, M Tamura, M Watanabe, N CAS Key Laboratory of planetary sciences Purple Mountain Observatory Chinese Academy of Sciences Nanjing 210023 China School of Astronomy and Space Science University of Science and Technology of China Hefei 230026 China CAS Center for Excellence in Comparative Planetology Hefei 230026 China Instituto de Astrofísica de Canarias Vía Láctea s/n E-38205 La Laguna Tenerife Spain Departamento de Astrofísica Universidad de La Laguna C/ Padre Herrera E-38206 La Laguna Spain Department of Multi-Disciplinary Sciences Graduate School of Arts and Sciences The University of Tokyo 3-8-1 Komaba Meguro Tokyo 153-8902 Japan Komaba Institute for Science The University of Tokyo 3-8-1 Komaba Meguro Tokyo 153-8902 Japan Okayama Observatory Kyoto University 3037-5 Honjo Kamogatacho Asakuchi Okayama 719-0232 Japan Department of Physical Sciences Ritsumeikan University Kusatsu Shiga 525-8577 Japan Lund Observatory Division of Astrophysics Department of Physics Lund University Box 43 22100 Lund Sweden Astrobiology Center 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Astronomical Science Program Graduate University for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo 181-8588 Japan Department of Astronomy & Astrophysics University of Chicago Chicago IL 60637 USA School of Architecture Universidad Europea de Canarias C/ Inocencio Garcia 1 E-38300 La Orotava Tenerife Spain INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 I-35122 Padova Italy Department of Astronomy University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo 113-0033 Japan

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Simultaneous Millimeter-wave, Gamma-ray, and Optical Monitoring of the Blazar PKS 2326-502 During a Flaring State

arXiv

引用

arXiv 2023年

作者： Hood, J.C. Simpson, A. McDaniel, A. Foster, A. Ade, P.A.R. Ajello, M. Anderson, A.J. Austermann, J.E. Beall, J.A. Bender, A.N. Benson, B.A. Bianchini, F. Bleem, L.E. Carlstrom, J.E. Chang, C.L. Chaubal, P. Chiang, H.C. Chou, T.-L. Citron, R. Corbett Moran, C. Crawford, T.M. Crites, A.T. De Haan, T. Dobbs, M.A. Everett, W. Gallicchio, J. George, E.M. Gupta, N. Halverson, N.W. Hilton, G.C. Holder, G.P. Holzapfel, W.L. Hrubes, J.D. Huang, N. Hubmayr, J. Irwin, K.D. Knox, L. Lee, A.T. Li, D. Lowitz, A. Madejski, G. Malkan, M. McMahon, J.J. Meyer, S.S. Montgomery, J. Natoli, T. Nibarger, J.P. Noble, G. Novosad, V. Omori, Y. Padin, S. Patil, S. Pryke, C. Reichardt, C.L. Ruhl, J.E. Saliwanchik, B.R. Schaffer, K.K. Sievers, C. Smecher, G. Stark, A.A. Tucker, C. Veach, T. Vieira, J.D. Wang, G. Whitehorn, N. Wu, W.L.K. Yefremenko, V. Zebrowski, J.A. Zhang, L. Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics and Astronomy Vanderbilt University NashvilleTN37235 United States Department of Physics Rensselaer Polytechnic Institute TroyNY12180 United States Department of Physics and Astronomy Clemson University ClemsonSC29631 United States Department of Physics Case Western Reserve University ClevelandOH44106 United States Cardiff University CardiffCF10 3XQ United Kingdom Fermi National Accelerator Laboratory MS209 P.O. Box 500 BataviaIL60510 United States Nist Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Physics University of Colorado BoulderCO80309 United States High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue ArgonneIL60439 United States School of Physics University of Melbourne VIC Parkville3010 Australia Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics McGill University 3600 Rue University QC MontrealH3A 2T8 Canada School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban South Africa University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Tapir Walter Burke Institute for Theoretical Physics California Institute of Technology 1200 E California Blvd PasadenaCA91125 United States Dunlap Institute for Astronomy & Astrophysics University of Toronto 50 St George St ON TorontoM5S 3H4 Canada Department of Astronomy & Astrophysics University of Toronto 50 St George St ON TorontoM5S 3H4 Canada Ibaraki Tsukuba305-0801 Japan Ibaraki Tsukuba305-0801 Japan Canadian Institute f

Including millimeter-wave (mm-wave) data in multi-wavelength studies of the variability of active galactic nuclei (AGN) can provide insights into AGN physics that are not easily accessible at other wavelengths. We demonstrate in this work the potential of cosmic microwave background (CMB) telescopes to provide long-term, high-cadence mm-wave AGN monitoring over large fractions of sky. We report on a pilot study using data from the SPTpol instrument on the South Pole Telescope (SPT), which was designed to observe the CMB at arcminute and larger angular scales. Between 2013 and 2016, SPTpol was used primarily to observe a single 500 deg2field, covering the entire field several times per day with detectors sensitive to radiation in bands centered at 95 and 150 GHz. We use SPT 150 GHz observations to create AGN light curves, and we compare these mm-wave light curves to those at other wavelengths, in particular γ-ray and optical. In this Letter, we focus on a single source, PKS 2326-502, which has extensive, day-timescale monitoring data in gamma-ray, optical, and now mm-wave between 2013 and 2016. We find PKS 2326-502 to be in a flaring state in the first two years of this monitoring, and we present a search for evidence of correlated variability between mm-wave, optical R band, and γ-ray observations. This pilot study is paving the way for AGN monitoring with current and upcoming CMB experiments such as SPT-3G, Simons Observatory, and CMB-S4, including multi-wavelength studies with facilities such as VRO-LSST. © 2023, CC BY.

关键词： Active Galactic Nuclei

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Constraints on VHE gamma-ray emission of Flat Spectrum Radio Quasars with the MAGIC telescopes

arXiv

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arXiv 2024年

作者： Abe, S. Abhir, J. Abhishek, A. Acciari, V.A. Aguasca-Cabot, A. Agudo, I. Aniello, T. Ansoldi, S. Antonelli, L.A. Engels, A. Arbet Arcaro, C. Artero, M. Asano, K. Babić, A. Baquero, A. de Almeida, U. Barres Barrio, J.A. Batković, I. Bautista, A. Baxter, J. González, J. Becerra Bednarek, W. Bernardini, E. Bernete, J. Berti, A. Bigongiari, C. Biland, A. Blanch, O. Bonnoli, G. Bošnjak, Ž. Bronzini, E. Burelli, I. Busetto, G. Buson, S. Campoy-Ordaz, A. Carosi, A. Carosi, R. Carretero-Castrillo, M. Castro-Tirado, A.J. Cerasole, D. Ceribella, G. Chai, Y. Cifuentes, A. Ciprini, S. Colombo, E. Contreras, J.L. Cortina, J. Covino, S. D’Amico, G. D’Ammando, F. D’Elia, V. Da Vela, P. Dazzi, F. De Angelis, A. De Lotto, B. de Menezes, R. Del Popolo, A. Delfino, M. Delgado, J. Mendez, C. Delgado Di Pierro, F. Di Tria, R. Di Venere, L. Donini, A. Dorner, D. Doro, M. Elsaesser, D. Escudero, J. Fariña, L. Fattorini, A. Foffano, L. Font, L. Fröse, S. Fukami, S. Fukazawa, Y. López, R.J. García Garczarczyk, M. Gasparyan, S. Gaug, M. Paiva, J.G. Giesbrecht Giglietto, N. Giordano, F. Gliwny, P. Gradetzke, T. Grau, R. Green, D. Green, J.G. Günther, P. Hadasch, D. Hahn, A. Hassan, T. Heckmann, L. Herrera, J. Hrupec, D. Hütten, M. Imazawa, R. Ishio, K. Martínez, I. Jiménez Jormanainen, J. Kayanoki, T. Kerszberg, D. Kobayashi, Y. Kouch, P.M. Kubo, H. Kushida, J. Láinez, M. Lamastra, A. Leone, F. Lindfors, E. Linhoff, L. Lombardi, S. Longo, F. López-Coto, R. López-Moya, M. López-Oramas, A. Loporchio, S. Lorini, A. Lyard, E. de Oliveira Fraga, B. Machado Majumdar, P. Makariev, M. Maneva, G. Mang, N. Manganaro, M. Mangano, S. Mannheim, K. Mariotti, M. Martínez, M. Martínez-Chicharro, M. Mas-Aguilar, A. Mazin, D. Menchiari, S. Mender, S. Miceli, D. Miener, T. Miranda, J.M. Mirzoyan, R. González, M. Molero Molina, E. Mondal, H.A. Moralejo, A. Morcuende, D. Nakamori, T. Nanci, C. Neustroev, V. Nickel, L. Rosillo, M. Nievas Nigro, C. Nikolić, L. Nilsson, K. Nishijima, K. The University of Tokyo Chiba Kashiwa277-8582 Japan ETH Zürich ZürichCH-8093 Switzerland Università di Siena INFN Pisa SienaI-53100 Italy Bellaterra BarcelonaE-08193 Spain Universitat de Barcelona ICCUB IEEC-UB BarcelonaE-08028 Spain Instituto de Astrofísica de Andalucía-CSIC Glorieta de la Astronomía s/n Granada18008 Spain RomeI-00136 Italy Università di Udine INFN Trieste UdineI-33100 Italy Max-Planck-Institut für Physik GarchingD-85748 Germany Università di Padova INFN PadovaI-35131 Italy Zagreb10000 Croatia IPARCOS Institute EMFTEL Department Universidad Complutense de Madrid MadridE-28040 Spain URCA RJ Rio de Janeiro22290-180 Brazil Instituto de Astrofísica de Canarias Dpto. de Astrofísica Universidad de La Laguna Tenerife La LagunaE-38200 Spain University of Lodz Faculty of Physics and Applied Informatics Department of Astrophysics Lodz90-236 Poland Centro de Investigaciones Energéticas Medioambientales y Tecnológicas MadridE-28040 Spain Departament de Física CERES-IEEC Universitat Autònoma de Barcelona BellaterraE-08193 Spain Università di Pisa INFN Pisa PisaI-56126 Italy INFN MAGIC Group INFN Sezione di Bari Dipartimento Interateneo di Fisica dell’Università e del Politecnico di Bari BariI-70125 Italy Department for Physics and Technology University of Bergen Norway INFN MAGIC Group INFN Sezione di Torino Università degli Studi di Torino TorinoI-10125 Italy Universität Würzburg WürzburgD-97074 Germany Technische Universität Dortmund DortmundD-44221 Germany Japanese MAGIC Group: Physics Program Graduate School of Advanced Science and Engineering Hiroshima University Hiroshima739-8526 Japan ZeuthenD-15738 Germany Armenian MAGIC Group: ICRANet-Armenia Yerevan0019 Armenia Croatian MAGIC Group Josip Juraj Strossmayer University of Osijek Department of Physics Osijek31000 Croatia Finnish MAGIC Group Finnish Centre for Astronomy with ESO Department of Physics and Astronomy University of Turku T

Flat spectrum radio quasars (FSRQs) constitute a class of jetted active galaxies characterized by a very luminous accretion disk, prominent and rapidly moving line-emitting cloud structures (Broad Line Region, BLR), and a surrounding dense dust structure known as dusty torus. The intense radiation field of the accretion disk strongly determines the observational properties of FSRQs. While hundreds of such sources have been detected at GeV energies, only a handful of them exhibit emission in the very-high-energy (VHE, E 100 GeV) range. This study presents the results and interpretation derived from a cumulative observation period of 174 hours dedicated to nine FSRQs conducted with the MAGIC telescopes from 2008 to 2020. Our findings indicate no statistically significant (≥ 5 σ) signal for any of the studied sources, resulting in upper limits on the emission within the VHE energy range. In two of the sources, we derived quite stringent constraints on the γ-ray emission in the form of upper limits. Our analysis focuses on modeling the VHE emission of these two sources in search for hints of absorption signatures within the broad line region (BLR) radiation field. For these particular sources, constraints on the distance between the emission region and the central black hole are derived using a phenomenological model. Subsequently, these constraints are tested using a framework based on a leptonic model. Copyright © 2024, The Authors. All rights reserved.

关键词： Germanium alloys

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All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run

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Physical Review D 2021年第10期104卷 102001-102001页

作者： R. Abbott T. D. Abbott F. Acernese K. Ackley C. Adams N. Adhikari R. X. Adhikari V. B. Adya C. Affeldt D. Agarwal M. Agathos K. Agatsuma N. Aggarwal O. D. Aguiar L. Aiello A. Ain P. Ajith T. Akutsu S. Albanesi A. Allocca P. A. Altin A. Amato C. Anand S. Anand A. Ananyeva S. B. Anderson W. G. Anderson M. Ando T. Andrade N. Andres T. Andrić S. V. Angelova S. Ansoldi J. M. Antelis S. Antier S. Appert Koji Arai Koya Arai Y. Arai S. Araki A. Araya M. C. Araya J. S. Areeda M. Arène N. Aritomi N. Arnaud S. M. Aronson K. G. Arun H. Asada Y. Asali G. Ashton Y. Aso M. Assiduo S. M. Aston P. Astone F. Aubin C. Austin S. Babak F. Badaracco M. K. M. Bader C. Badger S. Bae Y. Bae A. M. Baer S. Bagnasco Y. Bai L. Baiotti J. Baird R. Bajpai M. Ball G. Ballardin S. W. Ballmer A. Balsamo G. Baltus S. Banagiri D. Bankar J. C. Barayoga C. Barbieri B. C. Barish D. Barker P. Barneo F. Barone B. Barr L. Barsotti M. Barsuglia D. Barta J. Bartlett M. A. Barton I. Bartos R. Bassiri A. Basti M. Bawaj J. C. Bayley A. C. Baylor M. Bazzan B. Bécsy V. M. Bedakihale M. Bejger I. Belahcene V. Benedetto D. Beniwal T. F. Bennett J. D. Bentley M. BenYaala F. Bergamin B. K. Berger S. Bernuzzi D. Bersanetti A. Bertolini J. Betzwieser D. Beveridge R. Bhandare U. Bhardwaj D. Bhattacharjee S. Bhaumik I. A. Bilenko G. Billingsley S. Bini R. Birney O. Birnholtz S. Biscans M. Bischi S. Biscoveanu A. Bisht B. Biswas M. Bitossi M.-A. Bizouard J. K. Blackburn C. D. Blair D. G. Blair R. M. Blair F. Bobba N. Bode M. Boer G. Bogaert M. Boldrini L. D. Bonavena F. Bondu E. Bonilla R. Bonnand P. Booker B. A. Boom R. Bork V. Boschi N. Bose S. Bose V. Bossilkov V. Boudart Y. Bouffanais A. Bozzi C. Bradaschia P. R. Brady A. Bramley A. Branch M. Branchesi J. E. Brau M. Breschi T. Briant J. H. Briggs A. Brillet M. Brinkmann P. Brockill A. F. Brooks J. Brooks D. D. Brown S. Brunett G. Bruno R. Bruntz J. Bryant T. Bulik H. J. Bulten A. Buonanno R. Buscicchio D. Buskulic C. Buy R. L. Byer L. Cadonati G. Cagnoli C. Cahillane J. Calderón Bustillo J. D. Callaghan T. A. Callis LIGO Laboratory California Institute of Technology Pasadena California 91125 USA Louisiana State University Baton Rouge Louisiana 70803 USA Dipartimento di Farmacia Università di Salerno I-84084 Fisciano Salerno Italy INFN Sezione di Napoli Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy OzGrav School of Physics and Astronomy Monash University Clayton 3800 Victoria Australia LIGO Livingston Observatory Livingston Louisiana 70754 USA University of Wisconsin-Milwaukee Milwaukee Wisconsin 53201 USA OzGrav Australian National University Canberra Australian Capital Territory 0200 Australia Max Planck Institute for Gravitational Physics (Albert Einstein Institute) D-30167 Hannover Germany Leibniz Universität Hannover D-30167 Hannover Germany Inter-University Centre for Astronomy and Astrophysics Pune 411007 India University of Cambridge Cambridge CB2 1TN United Kingdom Theoretisch-Physikalisches Institut Friedrich-Schiller-Universität Jena D-07743 Jena Germany University of Birmingham Birmingham B15 2TT United Kingdom Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA) Northwestern University Evanston Illinois 60208 USA Instituto Nacional de Pesquisas Espaciais 12227-010 São José dos Campos São Paulo Brazil Gravity Exploration Institute Cardiff University Cardiff CF24 3AA United Kingdom INFN Sezione di Pisa I-56127 Pisa Italy International Centre for Theoretical Sciences Tata Institute of Fundamental Research Bengaluru 560089 India Gravitational Wave Science Project National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan Advanced Technology Center National Astronomical Observatory of Japan (NAOJ) Mitaka City Tokyo 181-8588 Japan INFN Sezione di Torino I-10125 Torino Italy Università di Napoli “Federico II ” Complesso Universitario di Monte S. Angelo I-80126 Napoli Italy Université de Lyon Université Claude Bernard Lyon 1 CNRS Institut Lumière Matière F-69622 Villeurbanne France

After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into “short” ≲1 s and “long” ≳1 s duration signals, these signals are expected from a variety of astrophysical processes, including non-axisymmetric deformations in magnetars or eccentric binary black hole coalescences. In this work, we present a search for long-duration gravitational-wave transients from Advanced LIGO and Advanced Virgo’s third observing run from April 2019 to March 2020. For this search, we use minimal assumptions for the sky location, event time, waveform morphology, and duration of the source. The search covers the range of 2–500 s in duration and a frequency band of 24–2048 Hz. We find no significant triggers within this parameter space; we report sensitivity limits on the signal strength of gravitational waves characterized by the root-sum-square amplitude hrss as a function of waveform morphology. These hrss limits improve upon the results from the second observing run by an average factor of 1.8.

关键词： Astrophysical studies of gravity Gravitational wave detection Gravitational wave sources Gravitational waves

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