Swift-BAT GUANO Follow-up of Gravitational-wave Triggers in the Third LIGO–Virgo–KAGRA Observing Run

The LIGO Scientific Collaboration, The Virgo Collaboration; The KAGRA Collaboration

doi:10.3847/1538-4357/ad9749

Swift-BAT GUANO Follow-up of Gravitational-wave Triggers in the Third LIGO–Virgo–KAGRA Observing Run

The LIGO Scientific Collaboration, The Virgo Collaboration, The KAGRA Collaboration

Sub Gravitational and Subatomic Physics (GRASP)

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

Abstract

We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO–Virgo–KAGRA network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received with low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wave Transient Catalogs (GWTC-3). Targeted searches were carried out on the entire GW sample using the maximum-likelihood Non-imaging Transient Reconstruction and Temporal Search pipeline on the BAT data made available via the GUANO infrastructure. We do not detect any significant electromagnetic emission that is temporally and spatially coincident with any of the GW candidates. We report flux upper limits in the 15–350 keV band as a function of sky position for all the catalog candidates. For GW candidates where the Swift-BAT false alarm rate is less than 10⁻³ Hz, we compute the GW–BAT joint false alarm rate. Finally, the derived Swift-BAT upper limits are used to infer constraints on the putative electromagnetic emission associated with binary black hole mergers.

Original language	English
Article number	207
Journal	Astrophysical Journal
Volume	980
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ad9749
Publication status	Published - 20 Feb 2025

Bibliographical note

Publisher Copyright:
© 2025. The Author(s). Published by the American Astronomical Society.

Funding

G. Raman, S. Ronchini, and J.A. Kennea acknowledge the support of NASA grants 80NSSC19K0408 and 80NSSC22K1498 awarded as part of the NASA Neil Gehrels Swift Observatory Guest Investigator program. J.A. Kennea and J. Delaunay acknowledge the support of NASA contract NAS5-0136. 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 MaxPlanck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 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 by 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 ALon (AEI), the Spanish Ministerio de Ciencia, Innovaci ALon y Universidades, the European Union NextGenerationEU/PRTR (PRTR-C17.I1), the ICSC -CentroNazionale di Ricerca in High Performance Computing, Big Data and Quantum Computing, funded by the European Union NextGenerationEU, the Comunitat Auton`oma de les Illes Balears through the Direcci ALo General de Recerca, Innovaci ALo i TransformaciALo Digital with funds from the Tourist Stay Tax Law ITS 2017-006, the Conselleria d'Economia, Hisenda i Innovaci AL o, the FEDER Operational Program 2021-2027 of the Balearic Islands, the Conselleria d'Innovaci AL o, Universitats, Ci`encia i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the Polish National Agency for Academic Exchange, the National Science Centre of Poland and the European Union -European Regional Development Fund; the Foundation for Polish Science (FNP), the Polish Ministry of Science and Higher Education, the Swiss National Science Foundation (SNSF), 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 ALees (ARC) and Fonds Wetenschappelijk Onderzoek -Vlaanderen (FWO), Belgium, the Paris Ile-de-France Region, the National Research, Development and Innovation Office of Hungary (NKFIH), the National Research Foundation of Korea, the Natural Science and Engineering Research Council of Canada (NSERC), 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 Israel Science Foundation (ISF), the US-Israel Binational Science Fund (BSF), 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 provision of computational resources. American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Israel Science Foundation (ISF), the US-Israel Binational Science Fund (BSF), 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 provision of computational resources. This work was supported by MEXT, the JSPS Leading-edge Research Infrastructure Program, JSPS Grantin-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 Grants-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, the University of Tokyo, the National Research Foundation (NRF), the Computing Infrastructure Project of 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.

Funders	Funder number
NASA	80NSSC19K0408, 80NSSC22K1498, NAS5-0136
NSF's LIGO Laboratory - National Science Foundation
Science and Technology Facilities Council (STFC) of the United Kingdom
MaxPlanck-Society (MPS)
State of Niedersachsen/Germany
Australian Research Council
Italian Istituto Nazionale di Fisica Nucleare (INFN)
French Centre National de la Recherche Scientifique (CNRS)
Netherlands Organization for Scientific Research (NWO)
EGO consortium
Council of Scientific and Industrial Research of India
Department of Science and Technology, India
Science & Engineering Research Board (SERB), India
Ministry of Human Resource Development, India
Spanish Ministerio de Ciencia, Innovaci ALon y Universidades	PRTR-C17
European Union NextGenerationEU
Comunitat Auton`oma de les Illes Balears through the Direcci ALo General de Recerca
Tourist Stay Tax Law ITS
Conselleria d'Economia, Hisenda i Innovaci AL	2021-2027
Conselleria d'Innovaci AL o, Universitats, Ci`encia i Societat Digital de la Generalitat Valenciana
CERCA Programme Generalitat de Catalunya, Spain
Polish National Agency for Academic Exchange
National Science Centre of Poland
European Union -European Regional Development Fund
Foundation for Polish Science (FNP)
Polish Ministry of Science and Higher Education
Swiss National Science Foundation (SNSF)
Russian Science Foundation
European Commission
European Social Funds (ESF)
European Regional Development Funds (ERDF)
Royal Society
Scottish Funding Council
Scottish Universities Physics Alliance
Hungarian Scientific Research Fund (OTKA)
French Lyon Institute of Origins (LIO)
Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concert ALees (ARC)
Fonds Wetenschappelijk Onderzoek -Vlaanderen (FWO), Belgium
Paris Ile-de-France Region
National Research, Development and Innovation Office of Hungary (NKFIH)
National Research Foundation of Korea
Natural Science and Engineering Research Council of Canada (NSERC)
Canadian Foundation for Innovation (CFI)
Brazilian Ministry of Science, Technology
Research Grants Council of Hong Kong
National Natural Science Foundation of China (NSFC)
Israel Science Foundation (ISF)
US-Israel Binational Science Fund (BSF)
Leverhulme Trust
National Science and Technology Council (NSTC), Taiwan
Kavli Foundation
NSF
STFC
CNRS
American Institute for Fundamental Research (ICTP-SAIFR)
Research Corporation
United States Department of Energy
MEXT
JSPS Leading-edge Research Infrastructure Program
JSPS	20A203: JP20H05854
JSPS Core-to-Core Program A, Advanced Research Networks, JSPS	17H06133, 20H05639
University of Tokyo
National Research Foundation (NRF)
Computing Infrastructure Project of Global Science experimental Data hub Center (GSDC) at KISTI
Ministry of Science and ICT (MSIT) in Korea
AS Grid Center (ASGC)
National Science and Technology Council (NSTC) in Taiwan
Rising Star Program and Science Vanguard Research Program
Advanced Technology Center (ATC) of NAOJ

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Raman_2025_ApJ_980_207Final published version, 9.62 MBLicence: CC BY

Cite this

@article{cc9e1b4af8034eda868262f4e809b28f,

title = "Swift-BAT GUANO Follow-up of Gravitational-wave Triggers in the Third LIGO–Virgo–KAGRA Observing Run",

abstract = "We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO–Virgo–KAGRA network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received with low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wave Transient Catalogs (GWTC-3). Targeted searches were carried out on the entire GW sample using the maximum-likelihood Non-imaging Transient Reconstruction and Temporal Search pipeline on the BAT data made available via the GUANO infrastructure. We do not detect any significant electromagnetic emission that is temporally and spatially coincident with any of the GW candidates. We report flux upper limits in the 15–350 keV band as a function of sky position for all the catalog candidates. For GW candidates where the Swift-BAT false alarm rate is less than 10−3 Hz, we compute the GW–BAT joint false alarm rate. Finally, the derived Swift-BAT upper limits are used to infer constraints on the putative electromagnetic emission associated with binary black hole mergers.",

author = "{The LIGO Scientific Collaboration, The Virgo Collaboration} and {The KAGRA Collaboration} and Gayathri Raman and Samuele Ronchini and James Delaunay and Aaron Tohuvavohu and Kennea, {Jamie A.} and Tyler Parsotan and Elena Ambrosi and Bernardini, {Maria Grazia} and Sergio Campana and Giancarlo Cusumano and Antonino D'A{\`i} and Paolo D'Avanzo and Valerio D'Elia and {De Pasquale}, Massimiliano and Simone Dichiara and Phil Evans and Dieter Hartmann and Paul Kuin and Andrea Melandri and Paul O{\textquoteright}Brien and Osborne, {Julian P.} and Kim Page and Palmer, {David M.} and Boris Sbarufatti and Gianpiero Tagliaferri and Eleonora Troja and Abac, {A. G.} and R. Abbott and H. Abe and I. Abouelfettouh and F. Acernese and K. Ackley and C. Adamcewicz and S. Adhicary and N. Adhikari and Adhikari, {R. X.} and Adkins, {V. K.} and Adya, {V. B.} and C. Affeldt and D. Agarwal and S. Caudill and T. Dietrich and P. Gupta and Hannuksela, {O. A.} and P. Kuijer and Pang, {P. T.H.} and Phukon, {K. S.} and A. Puecher and Y. Setyawati and {Van Den Broeck}, C.",

note = "Publisher Copyright: {\textcopyright} 2025. The Author(s). Published by the American Astronomical Society.",

year = "2025",

month = feb,

day = "20",

doi = "10.3847/1538-4357/ad9749",

language = "English",

volume = "980",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

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TY - JOUR

T1 - Swift-BAT GUANO Follow-up of Gravitational-wave Triggers in the Third LIGO–Virgo–KAGRA Observing Run

AU - The LIGO Scientific Collaboration, The Virgo Collaboration

AU - The KAGRA Collaboration

AU - Raman, Gayathri

AU - Ronchini, Samuele

AU - Delaunay, James

AU - Tohuvavohu, Aaron

AU - Kennea, Jamie A.

AU - Parsotan, Tyler

AU - Ambrosi, Elena

AU - Bernardini, Maria Grazia

AU - Campana, Sergio

AU - Cusumano, Giancarlo

AU - D'Aì, Antonino

AU - D'Avanzo, Paolo

AU - D'Elia, Valerio

AU - De Pasquale, Massimiliano

AU - Dichiara, Simone

AU - Evans, Phil

AU - Hartmann, Dieter

AU - Kuin, Paul

AU - Melandri, Andrea

AU - O’Brien, Paul

AU - Osborne, Julian P.

AU - Page, Kim

AU - Palmer, David M.

AU - Sbarufatti, Boris

AU - Tagliaferri, Gianpiero

AU - Troja, Eleonora

AU - Abac, A. G.

AU - Abbott, R.

AU - Abe, H.

AU - Abouelfettouh, I.

AU - Acernese, F.

AU - Ackley, K.

AU - Adamcewicz, C.

AU - Adhicary, S.

AU - Adhikari, N.

AU - Adhikari, R. X.

AU - Adkins, V. K.

AU - Adya, V. B.

AU - Affeldt, C.

AU - Agarwal, D.

AU - Caudill, S.

AU - Dietrich, T.

AU - Gupta, P.

AU - Hannuksela, O. A.

AU - Kuijer, P.

AU - Pang, P. T.H.

AU - Phukon, K. S.

AU - Puecher, A.

AU - Setyawati, Y.

AU - Van Den Broeck, C.

PY - 2025/2/20

Y1 - 2025/2/20

N2 - We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO–Virgo–KAGRA network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received with low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wave Transient Catalogs (GWTC-3). Targeted searches were carried out on the entire GW sample using the maximum-likelihood Non-imaging Transient Reconstruction and Temporal Search pipeline on the BAT data made available via the GUANO infrastructure. We do not detect any significant electromagnetic emission that is temporally and spatially coincident with any of the GW candidates. We report flux upper limits in the 15–350 keV band as a function of sky position for all the catalog candidates. For GW candidates where the Swift-BAT false alarm rate is less than 10−3 Hz, we compute the GW–BAT joint false alarm rate. Finally, the derived Swift-BAT upper limits are used to infer constraints on the putative electromagnetic emission associated with binary black hole mergers.

AB - We present results from a search for X-ray/gamma-ray counterparts of gravitational-wave (GW) candidates from the third observing run (O3) of the LIGO–Virgo–KAGRA network using the Swift Burst Alert Telescope (Swift-BAT). The search includes 636 GW candidates received with low latency, 86 of which have been confirmed by the offline analysis and included in the third cumulative Gravitational-Wave Transient Catalogs (GWTC-3). Targeted searches were carried out on the entire GW sample using the maximum-likelihood Non-imaging Transient Reconstruction and Temporal Search pipeline on the BAT data made available via the GUANO infrastructure. We do not detect any significant electromagnetic emission that is temporally and spatially coincident with any of the GW candidates. We report flux upper limits in the 15–350 keV band as a function of sky position for all the catalog candidates. For GW candidates where the Swift-BAT false alarm rate is less than 10−3 Hz, we compute the GW–BAT joint false alarm rate. Finally, the derived Swift-BAT upper limits are used to infer constraints on the putative electromagnetic emission associated with binary black hole mergers.

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U2 - 10.3847/1538-4357/ad9749

DO - 10.3847/1538-4357/ad9749

M3 - Article

AN - SCOPUS:85219630308

SN - 0004-637X

VL - 980

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 207

ER -

Swift-BAT GUANO Follow-up of Gravitational-wave Triggers in the Third LIGO–Virgo–KAGRA Observing Run

Abstract

Bibliographical note

Funding

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