CaltechAUTHORS
Published June 3, 2022 | Version Published + Supplemental Material + Submitted
Journal Article Open

Candidate Tidal Disruption Event AT2019fdr Coincident with a High-Energy Neutrino

Creators

  • 1. ROR icon Deutsches Elektronen-Synchrotron DESY
  • 2. ROR icon Humboldt-Universität zu Berlin
  • 3. ROR icon California Institute of Technology
  • 4. ROR icon Leiden University
  • 5. ROR icon Ruhr University Bochum
  • 6. ROR icon Arizona State University
  • 7. ROR icon Pennsylvania State University
  • 8. ROR icon Kyoto University
  • 9. ROR icon International Centre for Radio Astronomy Research
  • 10. ROR icon Space Research Institute
  • 11. ROR icon Max Planck Institute for Astrophysics
  • 12. ROR icon Aryabhatta Research Institute of Observational Sciences
  • 13. ROR icon University of Maryland, College Park
  • 14. ROR icon Stockholm University
  • 15. ROR icon University of Washington
  • 16. ROR icon University of Würzburg
  • 17. ROR icon University of Minnesota
  • 18. ROR icon Weizmann Institute of Science
  • 19. ROR icon Space Telescope Science Institute
  • 20. ROR icon Tohoku University
  • 21. ROR icon National Tsing Hua University
  • 22. ROR icon Infrared Processing and Analysis Center
  • 23. ROR icon Liverpool John Moores University
  • 24. ROR icon Claude Bernard University Lyon 1
  • 25. ROR icon Goddard Space Flight Center

Abstract

The origins of the high-energy cosmic neutrino flux remain largely unknown. Recently, one high-energy neutrino was associated with a tidal disruption event (TDE). Here we present AT2019fdr, an exceptionally luminous TDE candidate, coincident with another high-energy neutrino. Our observations, including a bright dust echo and soft late-time x-ray emission, further support a TDE origin of this flare. The probability of finding two such bright events by chance is just 0.034%. We evaluate several models for neutrino production and show that AT2019fdr is capable of producing the observed high-energy neutrino, reinforcing the case for TDEs as neutrino sources.

Additional Information

© 2022 American Physical Society. Received 16 December 2021; accepted 9 March 2022; published 3 June 2022. S. R. acknowledges support by the Helmholtz Weizmann Research School on Multimessenger Astronomy, funded through the Initiative and Networking Fund of the Helmholtz Association, DESY, the Weizmann Institute, the Humboldt University of Berlin, and the University of Potsdam. A. F. acknowledges support by the Initiative and Networking Fund of the Helmholtz Association through the Young Investigator Group program (A. F.). C. L. acknowledges support from the National Science Foundation (NSF) with Grant No. PHY-2012195. The work of K. M. is supported by the NSF Grants No. AST-1908689, No. AST-2108466, and No. AST-2108467, and KAKENHI No. 20H01901 and No. 20H05852. M. C. acknowledges support from the National Science Foundation with Grants No. PHY-2010970 and No. OAC-2117997. S. S. acknowledges support from the G.R.E.A.T research environment, funded by Vetenskapsrådet, the Swedish Research Council, Project No. 2016-06012. M. G., P. M., and R. S. acknowledge the partial support of this research by Grant 19-12-00369 from the Russian Science Foundation. S. B. acknowledges financial support by the European Research Council for the ERC Starting grant MessMapp, under Contract No. 949555. The research of A. G.-Y. is supported by the EU via ERC Grant No. 725161, the ISF GW excellence center, an IMOS space infrastructure grant and BSF/Transformative and GIF grants, as well as The Benoziyo Endowment Fund for the Advancement of Science, the Deloro Institute for Advanced Research in Space and Optics, The Veronika A. Rabl Physics Discretionary Fund, Minerva, Yeda-Sela, and the Schwartz/Reisman Collaborative Science Program; A. G.-Y. is the incumbent of the The Arlyn Imberman Professorial Chair. E. C. K. acknowledges support from the G. R. E. A. T research environment funded by Vetenskapsrådet, the Swedish Research Council, under Project No. 2016-06012, and support from The Wenner-Gren Foundations. M. R. has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 Research and Innovation Program (Grant Agreement No. 759194—USNAC). N. L. S. is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) via the Walter Benjamin program—461903330. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 (until 2020 December 1) and No. AST-2034437 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, IN2P3, University of Warwick, Ruhr University Bochum and Northwestern University. Operations are conducted by COO, IPAC, and UW. This work was supported by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation Partnership in International Research and Education program under Grant No. 1545949. GROWTH is a collaborative project between California Institute of Technology (USA), Pomona College (USA), San Diego State University (USA), Los Alamos National Laboratory (USA), University of Maryland College Park (USA), University of Wisconsin Milwaukee (USA), Tokyo Institute of Technology (Japan), National Central University (Taiwan), Indian Institute of Astrophysics (India), Inter-University Center for Astronomy and Astrophysics (India), Weizmann Institute of Science (Israel), The Oskar Klein Centre at Stockholm University (Sweden), Humboldt University (Germany). This work is based on observations with the eROSITA telescope on board the SRG observatory. The SRG observatory was built by Roskosmos in the interests of the Russian Academy of Sciences represented by its Space Research Institute (IKI) in the framework of the Russian Federal Space Program, with the participation of the Deutsches Zentrum für Luft- und Raumfahrt (DLR). The SRG/eROSITA X-ray telescope was built by a consortium of German Institutes led by MPE, and supported by DLR. The SRG spacecraft was designed, built, launched, and is operated by the Lavochkin Association and its subcontractors. The science data are downlinked via the Deep Space Network Antennae in Bear Lakes, Ussurijsk, and Baykonur, funded by Roskosmos. The eROSITA data used in this work were processed using the eSASS software system developed by the German eROSITA consortium and proprietary data reduction and analysis software developed by the Russian eROSITA Consortium. This work was supported by the Australian government through the Australian Research Council's Discovery Projects funding scheme (DP200102471). This work includes data products from the Near-Earth Object Wide-field Infrared Survey Explorer (NEOWISE), which is a project of the Jet Propulsion Laboratory/California Institute of Technology. NEOWISE is funded by the National Aeronautics and Space Administration. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias.

Attached Files

Published - PhysRevLett.128.221101.pdf

Submitted - 2111.09390.pdf

Supplemental Material - SM.pdf

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Additional details

Identifiers

Eprint ID
112118
Resolver ID
CaltechAUTHORS:20211130-215810453

Related works

Describes
https://arxiv.org/abs/2111.09390 (URL)

Funding

Helmholtz Weizmann Research School on Multimessenger Astronomy
Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF)
Deutsches Elektronen-Synchrotron (DESY)
Weizmann Institute of Science
Humboldt University
University of Potsdam
NSF
PHY-2012195
NSF
AST-1908689
NSF
AST-2108466
NSF
AST-2108467
NSF
PHY-2010970
NSF
OAC-2117997
Swedish Research Council
2016-06012
Russian Science Foundation
19-12-00369
European Research Council (ERC)
949555
European Research Council (ERC)
725161
Israel Science Foundation
Ministry of Science (Israel)
Binational Science Foundation (USA-Israel)
German-Israeli Foundation for Research and Development
Benoziyo Endowment Fund for the Advancement of Science
Deloro Institute for Advanced Research in Space and Optics
Veronika A. Rabl Physics Discretionary Fund
MINERVA (Israel)
Yeda-Sela
Schwartz/Reisman Collaborative Science Program
Arlyn Imberman Professorial Chair
Wenner-Gren Foundation
European Research Council (ERC)
759194
Deutsche Forschungsgemeinschaft (DFG)
461903330
NSF
AST-1440341
NSF
AST-2034437
ZTF partner institutions
NSF
OISE-1545949
Roskosmos
Deutsches Zentrum für Luft- und Raumfahrt (DLR)
Australian Research Council
DP200102471
NASA/JPL/Caltech
Japan Society for the Promotion of Science (JSPS)
20H01901
Japan Society for the Promotion of Science (JSPS)
20H05852

Dates

Created
2021-11-30
Created from EPrint's datestamp field
Updated
2022-06-08
Created from EPrint's last_modified field

Caltech Custom Metadata

Caltech groups
Astronomy Department, Infrared Processing and Analysis Center (IPAC), Zwicky Transient Facility