A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run

Research output: Contribution to journal › Article › Research › peer review

Authors

  • Collaboration
  • the KAGRA Collaboration
  • Fermi Gamma-Ray Burst Monitor Team
  • The LIGO Scientific Collaboration

External Research Organisations

  • Australian National University
  • Inter-University Centre for Astronomy and Astrophysics India
  • Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
  • University of Adelaide
  • University of Western Australia
  • California Institute of Caltech (Caltech)
  • National Tsing Hua University
  • Cardiff University
  • University of Florida
  • National Institute for Subatomic Physics (Nikhef)
  • Maastricht University
  • University of Utah
  • Indian Institute of Technology Bombay (IITB)
  • National Science Foundation (NSF)
  • Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav)
  • Monash University
  • Universität Hamburg
  • University of Glasgow
  • University of Cambridge
  • Massachusetts Institute of Technology
  • University of Texas at Austin
  • Seoul National University
  • Inje University
  • Northwestern University
  • Wuhan University
  • The Chinese University of Hong Kong
  • University of Wisconsin Milwaukee
  • Texas A and M University
  • Utrecht University
  • Marquette University
  • University of Birmingham
  • University of Michigan
  • University of Toyama
  • National Taiwan Normal University
  • CAS - Innovation Academy for Precision Measurement Science and Technology (APM)
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Details

Original languageEnglish
Article number149
JournalAstrophysical Journal
Volume964
Issue number2
Publication statusPublished - 1 Apr 2024
Externally publishedYes

Abstract

We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift- BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers.

ASJC Scopus subject areas

Cite this

A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run. / Collaboration; the KAGRA Collaboration; Fermi Gamma-Ray Burst Monitor Team et al.
In: Astrophysical Journal, Vol. 964, No. 2, 149, 01.04.2024.

Research output: Contribution to journal › Article › Research › peer review

Collaboration, the KAGRA Collaboration, Fermi Gamma-Ray Burst Monitor Team & The LIGO Scientific Collaboration 2024, 'A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run', Astrophysical Journal, vol. 964, no. 2, 149. https://doi.org/10.3847/1538-4357/ad1eed
Collaboration, the KAGRA Collaboration, Fermi Gamma-Ray Burst Monitor Team, & The LIGO Scientific Collaboration (2024). A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run. Astrophysical Journal, 964(2), Article 149. https://doi.org/10.3847/1538-4357/ad1eed
Collaboration, the KAGRA Collaboration, Fermi Gamma-Ray Burst Monitor Team, The LIGO Scientific Collaboration. A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run. Astrophysical Journal. 2024 Apr 1;964(2):149. doi: 10.3847/1538-4357/ad1eed
Collaboration ; the KAGRA Collaboration ; Fermi Gamma-Ray Burst Monitor Team et al. / A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run. In: Astrophysical Journal. 2024 ; Vol. 964, No. 2.
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@article{f8c4a76b348244989ba2103292c74be4,
title = "A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run",
abstract = "We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift- BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers.",
author = "Collaboration and {the KAGRA Collaboration} and {Fermi Gamma-Ray Burst Monitor Team} and {The LIGO Scientific Collaboration} and Adya, {V. B.} and S. Bose and M. Brinkmann and Brown, {D. D.} and M. Carlassara and C. Chatterjee and X. Chen and Chen, {Y. B.} and Chen, {Y. B.} and Z. Chen and H. Cheng and Choudhary, {R. K.} and S. Danilishin and K. Danzmann and Guo, {H. K.} and Gupta, {S. K.} and H. Hansen and A. Heidt and J. Hennig and M. Heurs and A. Hreibi and H{\"u}bner, {M. T.} and K. Isleif and R. Jones and J. Junker and T. Klinger and N. Knust and Lang, {R. N.} and J. Lange and Lee, {H. M.} and Lee, {H. M.} and J. Lehmann and B. Li and J. Li and P. Li and Li, {T. G.F.} and X. Li and X. Liu and H. Luck and M. Matiushechkina and A. More and T. Nguyen and H. Pham and L. Richardson and Rose, {C. A.} and S. Roy and Sanders, {J. R.} and P. Schmidt and S. Schmidt and Schulte, {B. W.} and L. Sun and Wang, {J. Z.} and Wang, {J. Z.} and D. Wilken and B. Willke and Wu, {D. S.} and H. Wu and K. Yamamoto and H. Zhang and J. Zhang and L. Zhang and R. Zhang and Y. Zhang and Z. Zhou and Zhu, {X. J.}",
note = "Funding Information: This material is based upon work supported by NSF's LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for supporting the construction of Advanced LIGO and the construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Netherlands Organization for Scientific Research (NWO) for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as from the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigaci\u00F3n (AEI), the Spanish Ministerio de Ciencia e Innovaci\u00F3n and Ministerio de Universidades, the Conselleria de Fons Europeus, Universitat i Cultura and the Direcci\u00F3 General de Pol\u00EDtica Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d\u2019Innovaci\u00F3 Universitats, Ci\u00E8ncia i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the European Union\u2014European Regional Development Fund; the Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Social Funds (ESF), the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concert\u00E9es (ARC) and Fonds Wetenschappelijk Onderzoek\u2014Vlaanderen (FWO), Belgium, the Paris \u00CEle-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, the Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the National Science and Technology Council (NSTC), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN, and CNRS for the provision of computational resources. Funding Information: This work was supported by MEXT, the JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-in-Aid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361, and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant-in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, the National Research Foundation (NRF), the Computing Infrastructure Project of the Global Science experimental Data hub Center (GSDC) at KISTI, the Korea Astronomy and Space Science Institute (KASI), the Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), the AS Grid Center (ASGC) and the National Science and Technology Council (NSTC) in Taiwan under grants including the Rising Star Program and Science Vanguard Research Program, the Advanced Technology Center (ATC) of NAOJ, and the Mechanical Engineering Center of KEK. Funding Information: The USRA coauthors gratefully acknowledge NASA funding through contract 80MSFC17M0022. R.H. acknowledges funding from the European Union's Horizon 2020 research and innovation program under the Marie Sk\u0142odowska-Curie grant agreement No. 945298-ParisRegionFP. The UAH coauthors gratefully acknowledge NASA funding from co-operative agreement 80MSFC22M0004. The NASA authors gratefully acknowledge NASA funding through the Fermi-GBM project. This research also made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. , , ); NumPy (Harris et al. ); SciPy (Virtanen et al. ), and matplotlib, a Python library for publication-quality graphics (Hunter ). Funding Information: The Swift authors acknowledge the use of public data from the Swift data archive. M.C. acknowledges support from NASA under award number 80GSFC21M0002 and from Vetenskapsr\u00E5det through project number 31004019. J.D. acknowledges support by the NSF under award numbers PHY-1913607 and PHY-2209445.",
year = "2024",
month = apr,
day = "1",
doi = "10.3847/1538-4357/ad1eed",
language = "English",
volume = "964",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

Download

TY - JOUR

T1 - A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run

AU - Collaboration

AU - the KAGRA Collaboration

AU - Fermi Gamma-Ray Burst Monitor Team

AU - The LIGO Scientific Collaboration

AU - Adya, V. B.

AU - Bose, S.

AU - Brinkmann, M.

AU - Brown, D. D.

AU - Carlassara, M.

AU - Chatterjee, C.

AU - Chen, X.

AU - Chen, Y. B.

AU - Chen, Y. B.

AU - Chen, Z.

AU - Cheng, H.

AU - Choudhary, R. K.

AU - Danilishin, S.

AU - Danzmann, K.

AU - Guo, H. K.

AU - Gupta, S. K.

AU - Hansen, H.

AU - Heidt, A.

AU - Hennig, J.

AU - Heurs, M.

AU - Hreibi, A.

AU - Hübner, M. T.

AU - Isleif, K.

AU - Jones, R.

AU - Junker, J.

AU - Klinger, T.

AU - Knust, N.

AU - Lang, R. N.

AU - Lange, J.

AU - Lee, H. M.

AU - Lee, H. M.

AU - Lehmann, J.

AU - Li, B.

AU - Li, J.

AU - Li, P.

AU - Li, T. G.F.

AU - Li, X.

AU - Liu, X.

AU - Luck, H.

AU - Matiushechkina, M.

AU - More, A.

AU - Nguyen, T.

AU - Pham, H.

AU - Richardson, L.

AU - Rose, C. A.

AU - Roy, S.

AU - Sanders, J. R.

AU - Schmidt, P.

AU - Schmidt, S.

AU - Schulte, B. W.

AU - Sun, L.

AU - Wang, J. Z.

AU - Wang, J. Z.

AU - Wilken, D.

AU - Willke, B.

AU - Wu, D. S.

AU - Wu, H.

AU - Yamamoto, K.

AU - Zhang, H.

AU - Zhang, J.

AU - Zhang, L.

AU - Zhang, R.

AU - Zhang, Y.

AU - Zhou, Z.

AU - Zhu, X. J.

N1 - Funding Information: This material is based upon work supported by NSF's LIGO Laboratory, which is a major facility fully funded by the National Science Foundation. The authors also gratefully acknowledge the support of the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for supporting the construction of Advanced LIGO and the construction and operation of the GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS), and the Netherlands Organization for Scientific Research (NWO) for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as from the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigaci\u00F3n (AEI), the Spanish Ministerio de Ciencia e Innovaci\u00F3n and Ministerio de Universidades, the Conselleria de Fons Europeus, Universitat i Cultura and the Direcci\u00F3 General de Pol\u00EDtica Universitaria i Recerca del Govern de les Illes Balears, the Conselleria d\u2019Innovaci\u00F3 Universitats, Ci\u00E8ncia i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland and the European Union\u2014European Regional Development Fund; the Foundation for Polish Science (FNP), the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Social Funds (ESF), the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concert\u00E9es (ARC) and Fonds Wetenschappelijk Onderzoek\u2014Vlaanderen (FWO), Belgium, the Paris \u00CEle-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council Canada, the Canadian Foundation for Innovation (CFI), the Brazilian Ministry of Science, Technology, and Innovations, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the National Science and Technology Council (NSTC), Taiwan, the United States Department of Energy, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, INFN, and CNRS for the provision of computational resources. Funding Information: This work was supported by MEXT, the JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, JSPS Grant-in-Aid for Scientific Research on Innovative Areas 2905: JP17H06358, JP17H06361, and JP17H06364, JSPS Core-to-Core Program A. Advanced Research Networks, JSPS Grant-in-Aid for Scientific Research (S) 17H06133 and 20H05639, JSPS Grant-in-Aid for Transformative Research Areas (A) 20A203: JP20H05854, the joint research program of the Institute for Cosmic Ray Research, University of Tokyo, the National Research Foundation (NRF), the Computing Infrastructure Project of the Global Science experimental Data hub Center (GSDC) at KISTI, the Korea Astronomy and Space Science Institute (KASI), the Ministry of Science and ICT (MSIT) in Korea, Academia Sinica (AS), the AS Grid Center (ASGC) and the National Science and Technology Council (NSTC) in Taiwan under grants including the Rising Star Program and Science Vanguard Research Program, the Advanced Technology Center (ATC) of NAOJ, and the Mechanical Engineering Center of KEK. Funding Information: The USRA coauthors gratefully acknowledge NASA funding through contract 80MSFC17M0022. R.H. acknowledges funding from the European Union's Horizon 2020 research and innovation program under the Marie Sk\u0142odowska-Curie grant agreement No. 945298-ParisRegionFP. The UAH coauthors gratefully acknowledge NASA funding from co-operative agreement 80MSFC22M0004. The NASA authors gratefully acknowledge NASA funding through the Fermi-GBM project. This research also made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. , , ); NumPy (Harris et al. ); SciPy (Virtanen et al. ), and matplotlib, a Python library for publication-quality graphics (Hunter ). Funding Information: The Swift authors acknowledge the use of public data from the Swift data archive. M.C. acknowledges support from NASA under award number 80GSFC21M0002 and from Vetenskapsr\u00E5det through project number 31004019. J.D. acknowledges support by the NSF under award numbers PHY-1913607 and PHY-2209445.

PY - 2024/4/1

Y1 - 2024/4/1

N2 - We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift- BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers.

AB - We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift- BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers.

UR - http://www.scopus.com/inward/record.url?scp=85189472922&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ad1eed

DO - 10.3847/1538-4357/ad1eed

M3 - Article

AN - SCOPUS:85189472922

VL - 964

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 149

ER -

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