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FERMI GBM OBSERVATIONS OF LIGO GRAVITATIONAL-WAVE EVENT GW150914

V. ConnaughtonUniversities Space Research Association, 320 Sparkman Drive, Huntsville, AL 35806, USA; [email protected]Eric BurnsPhysics Department, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USAA. GoldsteinAstrophysics Office, ZP12, NASA/Marshall Space Flight Center, Huntsville, AL 35812, USALindy BlackburnHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAM. S. BriggsCSPAR, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USABin‐Bin ZhangCSPAR, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USAJ. B. CampNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAN. ChristensenPhysics and Astronomy, Carleton College, MN 55057, USAC. M. HuiAstrophysics Office, ZP12, NASA/Marshall Space Flight Center, Huntsville, AL 35812, USAPeter JenkeCSPAR, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USAT. B. LittenbergUniversities Space Research Association, 320 Sparkman Drive, Huntsville, AL 35806, USA; [email protected]J. E. McEneryNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAJ. L. RacusinNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAP. ShawhanDepartment of Physics, University of Maryland, College Park, MD 20742, USAL. P. SingerNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAJ. VeitchUniversity of Birmingham, Birmingham B15 2TT, UKC. Wilson‐HodgeAstrophysics Office, ZP12, NASA/Marshall Space Flight Center, Huntsville, AL 35812, USAP. N. BhatCSPAR, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USAC. MeeganDipartimento di Fisica, Politecnico di Bari, I-70125, Bari, ItalyW. H. ClevelandUniversities Space Research Association, 320 Sparkman Drive, Huntsville, AL 35806, USA; [email protected]G. FitzpatrickCSPAR, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USAM. M. GilesJacobs Technology, Inc., Huntsville, AL, USAM. H. GibbyJacobs Technology, Inc., Huntsville, AL, USAA. von KienlinMax-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching, GermanyR. M. KippenLos Alamos National Laboratory, NM 87545, USAS. McBreenSchool of Physics, University College Dublin, Belfield, Stillorgan Road, Dublin 4, IrelandB. MailyanCSPAR, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USAW. S. PačiesasUniversities Space Research Association, 320 Sparkman Drive, Huntsville, AL 35806, USA; [email protected]R. D. PreeceDepartment of Space Science, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USAO. J. RobertsSchool of Physics, University College Dublin, Belfield, Stillorgan Road, Dublin 4, IrelandL. SparkeM. StanbroDepartment of Space Science, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USAK. ToelgeDipartimento di Fisica, Politecnico di Bari, I-70125, Bari, ItalyP. VerešCSPAR, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USA

2016en

ABI

Annotatsiya

ABSTRACT With an instantaneous view of 70% of the sky, the Fermi Gamma-ray Burst Monitor (GBM) is an excellent partner in the search for electromagnetic counterparts to gravitational-wave (GW) events. GBM observations at the time of the Laser Interferometer Gravitational-wave Observatory (LIGO) event GW150914 reveal the presence of a weak transient above 50 keV, 0.4 s after the GW event, with a false-alarm probability of 0.0022 (2.9 σ ). This weak transient lasting 1 s was not detected by any other instrument and does not appear to be connected with other previously known astrophysical, solar, terrestrial, or magnetospheric activity. Its localization is ill-constrained but consistent with the direction of GW150914. The duration and spectrum of the transient event are consistent with a weak short gamma-ray burst (GRB) arriving at a large angle to the direction in which Fermi was pointing where the GBM detector response is not optimal. If the GBM transient is associated with GW150914, then this electromagnetic signal from a stellar mass black hole binary merger is unexpected. We calculate a luminosity in hard X-ray emission between 1 keV and 10 MeV of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>1.8</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>1.5</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>49</mml:mn> </mml:mrow> </mml:msup> </mml:math> erg s −1 . Future joint observations of GW events by LIGO/Virgo and Fermi GBM could reveal whether the weak transient reported here is a plausible counterpart to GW150914 or a chance coincidence, and will further probe the connection between compact binary mergers and short GRBs.

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DOI: 10.3847/2041-8205/826/1/l6

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