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3. Fermi and Swift Observations of GRB 190114C: Tracing the Evolution of High-energy Emission from Prompt to Afterglow

Author

M. Ajello, M. Arimoto, M. Axelsson, L. Baldini, G. Barbiellini, D. Bastieri, R. Bellazzini, A. Berretta, E. Bissaldi, R. D. Blandford, R. Bonino, E. Bottacini, J. Bregeon, P. Bruel, R. Buehler, E. Burns, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, S. Chen, G. Chiaro, S. Ciprini, J. Cohen-Tanugi, D. Costantin, S. Cutini, F. D’Ammando, M. DeKlotz, P. de la Torre Luque, F. de Palma, A. Desai, N. Di Lalla, L. Di Venere, F. Fana Dirirsa, S. J. Fegan, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, D. Gasparrini, N. Giglietto, R. Gill, F. Giordano, M. Giroletti, J. Granot, D. Green, I. A. Grenier, M.-H. Grondin, S. Guiriec, E. Hays, D. Horan, G. Jóhannesson, D. Kocevski, M. Kovac’evic’, M. Kuss, S. Larsson, L. Latronico, M. Lemoine-Goumard, J. Li, I. Liodakis, F. Longo, F. Loparco, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, W. Mitthumsiri, T. Mizuno, M. E. Monzani, E. Moretti, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, M. Orienti, E. Orlando, M. Palatiello, V. S. Paliya, D. Paneque, Z. Pei, M. Persic, M. Pesce-Rollins, V. Petrosian, F. Piron, H. Poon, T. A. Porter, G. Principe, J. L. Racusin, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, P. M. Saz Parkinson, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, K. Takagi, M. N. Takahashi, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, E. Troja, J. Valverde, B. Van Klaveren, K. Wood, M. Yassine, G. Zaharijas, B. Mailyan, P. N. Bhat, M. S. Briggs, W. Cleveland, M. Giles, A. Goldstein, M. Hui, Christian Malacaria, R. Preece, O. J. Roberts, P. Veres, C. Wilson-Hodge, A. von Kienlin, S. B. Cenko, P. O’Brien, A. P. Beardmore, A. Lien, J. P. Osborne, A. Tohuvavohu, V. D’Elia, A. D’Aì, M. Perri, J. Gropp, N. Klingler, M. Capalbi, G. Tagliaferri, M. Stamatikos, and M. De Pasquale

Published
2020
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4. Fermi-GBM GRBs with Characteristics Similar to GRB 170817A

Author

Colleen A. Wilson-Hodge, Rachel Hamburg, Bagrat Mailyan, Michael S. Briggs, Christian Malacaria, Péter Veres, Adam Goldstein, C. M. Hui, Dale D. Kocevski, Eric Burns, Oliver J. Roberts, Robert D. Preece, Elisabetta Bissaldi, and A. von Kienlin

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Spectral properties, Gamma-ray burst: general, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, gamma-ray burst: individual (GRB170817A), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Redshift, Neutron star, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Fermi Gamma-ray Space Telescope
Abstract

We present a search for gamma-ray bursts in the Fermi-GBM 10 year catalog that show similar characteristics to GRB 170817A, the first electromagnetic counterpart to a GRB identified as a binary neutron star (BNS) merger via gravitational wave observations. Our search is focused on a non-thermal pulse, followed by a thermal component, as observed for GRB 170817A. We employ search methods based on the measured catalog parameters and Bayesian Block analysis. Our multi-pronged approach, which includes examination of the localization and spectral properties of the thermal component, yields a total of 13 candidates, including GRB 170817A and the previously reported similar burst, GRB 150101B. The similarity of the candidates is likely caused by the same processes that shaped the gamma-ray signal of GRB 170817A, thus providing evidence of a nearby sample of short GRBs resulting from BNS merger events. Some of the newly identfied counterparts were observed by other space telescopes and ground observatories, but none of them have a measured redshift. We present an analysis of this sub-sample, and we discuss two models. From uncovering 13 candidates during a time period of ten years we predict that Fermi-GBM will trigger on-board on about one burst similar to GRB 170817A per year., Comment: 18 pages, 9 figures, 4 tables. Accepted for publication in ApJ

Published
2019
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5. OBSERVATIONS OF THE SHELL-TYPE SUPERNOVA REMNANT CASSIOPEIA A AT TeV ENERGIES WITH VERITAS

Author

R. G. Wagner, Gernot Maier, Stephanie Wissel, C. M. Hui, M. J. Lang, S. P. Wakely, T. B. Humensky, Daniel Gall, B. R. Smith, Geza Gyuk, Y. Butt, D. Boltuch, J. E. Ward, A. Cesarini, John L. Quinn, R. Dickherber, A. J.R. Weinstein, M. Bautista, S. Thibadeau, S. McArthur, V. A. Acciari, D. S. Hanna, David Kieda, J. P. Finley, R. A. Ong, Thomas Weisgarber, N. Karlsson, Jamie Holder, A. McCann, Martin Pohl, Wystan Benbow, T. C. Weekes, M. Beilicke, D. Steele, R. Guenette, V. Bugaev, S. LeBohec, F. Krennrich, E. Roache, P. Fortin, H. J. Rose, J. Grube, A. Furniss, S. P. Swordy, J. Millis, K. Byrum, Matthew J.A. Wood, Tulun Ergin, P. Moriarty, Nicola Galante, J. S. Perkins, M. Kertzman, S. J. Fegan, S. Vincent, M. Schroedter, G. H. Sembroski, P. T. Reynolds, Lucy Fortson, A. Varlotta, Wei Cui, D. Huang, M. Theiling, P. Cogan, T. Aune, Y. C. Chow, V. V. Vassiliev, P. Kaaret, G. Finnegan, A. W. Smith, C. Duke, J. H. Buckley, A. Konopelko, G. H. Gillanders, T. Arlen, L. Ciupik, E. Aliu, H. Krawczynski, K. Ragan, S. M. Bradbury, A. Cannon, D. Pandel, and M. McCutcheon

Subjects
Photon, Astrophysics::High Energy Astrophysical Phenomena, cosmic-rays, Shell (structure), Flux, Astrophysics, 01 natural sciences, Power law, cosmic rays, 0103 physical sciences, air cerenkov telescopes, crab-nebula, Supernova remnant, ism: individual objects (cassiopeia a), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Cherenkov radiation, acceleration of particles, Physics, magnetic-fields, electron acceleration, particle-acceleration, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy and Astrophysics, gamma-ray emission, Cassiopeia A, gamma rays: ism, rx j1713.7-3946, 13. Climate action, Space and Planetary Science, ism: supernova remnants, a supernova, magic telescope
Abstract

We report on observations of very high energy gamma rays from the shell-type supernova remnant (SNR) Cassiopeia A with the Very Energetic Radiation Imaging Telescope Array System stereoscopic array of four imaging atmospheric Cherenkov telescopes in Arizona. The total exposure time for these observations is 22 hr, accumulated between September and November of 2007. The gamma-ray source associated with the SNR Cassiopeia A was detected above 200 GeV with a statistical significance of 8.3 sigma. The estimated integral flux for this gamma-ray source is about 3% of the Crab-Nebula flux. The photon spectrum is compatible with a power law dN/dE proportional to E(-Gamma) with an index Gamma = 2.61 +/- 0.24(stat) +/- 0.2(sys). The data are consistent with a point-like source. We provide a detailed description of the analysis results and discuss physical mechanisms that may be responsible for the observed gamma-ray emission.

Published
2010
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6. OBSERVATION OF EXTENDED VERY HIGH ENERGY EMISSION FROM THE SUPERNOVA REMNANT IC 443 WITH VERITAS

Author

R. A. Ong, Thomas Weisgarber, S. LeBohec, S. M. Bradbury, A. Cannon, D. Pandel, D. Horan, P. Cogan, J. Grube, David Kieda, L. Ciupik, P. T. Reynolds, A. McCann, Lucy Fortson, M. Kertzman, M. K. Daniel, E. Aliu, H. Krawczynski, A. Varlotta, Gernot Maier, S. P. Swordy, V. V. Vassiliev, Martin Pohl, S. P. Wakely, Daniel Gall, K. Ragan, M. Wood, M. Beilicke, G. Finnegan, T. B. Humensky, A. W. Smith, B. Zitzer, A. Konopelko, R. G. Wagner, C. Duke, M. Schroedter, L. Valcarcel, Vikram V. Dwarkadas, P. Moriarty, Geza Gyuk, A. Weinstein, T. Arlen, P. Colin, A. N. Otte, A. Furniss, J. H. Buckley, P. Kaaret, Tulun Ergin, F. Krennrich, P. Fortin, S. Vincent, D. S. Hanna, Wystan Benbow, M. Theiling, C. M. Hui, Y. Butt, J. P. Finley, V. Bugaev, G. H. Sembroski, J. A. Toner, T. C. Weekes, R. Dickherber, A. Imran, E. Hays, J. S. Perkins, John Kildea, D. A. Williams, R. Guenette, J. Millis, O. Celik, K. Byrum, Wei Cui, Stephanie Wissel, T. Aune, Y. C. K. Chow, S. J. Fegan, D. Steele, V. A. Acciari, M. J. Lang, H. J. Rose, N. Karlsson, A. Cesarini, John L. Quinn, M. Bautista, K. G. Gibbs, Jamie Holder, L. C. Reyes, E. Roache, J. E. Ward, G. H. Gillanders, S. Godambe, M. McCutcheon, and OpenMETU

Subjects
Physics, nebula, 010308 nuclear & particles physics, ic-443, Molecular cloud, cosmic-rays, Flux, Astronomy and Astrophysics, Context (language use), xmm-newton observations, molecular clouds, Astrophysics, gamma-ray emission, 01 natural sciences, Pulsar wind nebula, ism: individual (ic 443=ver j0616.9+2230, = magic j0616+225), radiation, Space and Planetary Science, 0103 physical sciences, Supernova remnant, 010303 astronomy & astrophysics, gamma rays: observations, magic telescope, discovery, pulsar
Abstract

We present evidence that the very high energy (VHE, E > 100 GeV) gamma-ray emission coincident with the supernova remnant IC 443 is extended. IC 443 contains one of the best studied sites of supernova remnant/molecular cloud interaction and the pulsar wind nebula CXOU J061705.3+222127, both of which are important targets for VHE observations. VERITAS observed IC 443 for 37.9 hr during 2007 and detected emission above 300 GeV with an excess of 247 events, resulting in a significance of 8.3 standard deviations (sigma) before trials and 7.5 sigma after trials in a point-source search. The emission is centered at 6(h)16(m)51(s)+22 degrees 30'11 '' (J2000)+/- 0 degrees.03(stat)+/- 0 degrees.08(sys), with an intrinsic extension of 0 degrees.16 +/- 0 degrees.03(stat)+/- 0 degrees.04(sys). The VHE spectrum is well fit by a power law (dN/dE = N(0) x(E/TeV)(-Gamma)) with a photon index of 2.99 +/- 0.38(stat)+/- 0.3(sys) and an integral flux above 300 GeV of (4.63 +/- 0.90(stat)+/- 0.93(sys)) x 10(-12) cm(-2) s(-1). These results are discussed in the context of existing models for gamma-ray production in IC 443.

Published
2009
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7. EVIDENCE FOR LONG-TERM GAMMA-RAY AND X-RAY VARIABILITY FROM THE UNIDENTIFIED TeV SOURCE HESS J0632+057

Author

V. A. Acciari, E. Aliu, T. Arlen, M. Beilicke, W. Benbow, D. Boltuch, S. M. Bradbury, J. H. Buckley, V. Bugaev, K. Byrum, A. Cannon, A. Cesarini, Y. C. Chow, L. Ciupik, P. Cogan, R. Dickherber, C. Duke, T. Ergin, A. Falcone, S. J. Fegan, J. P. Finley, G. Finnegan, P. Fortin, L. Fortson, A. Furniss, K. Gibbs, G. H. Gillanders, J. Grube, R. Guenette, G. Gyuk, D. Hanna, J. Holder, D. Horan, C. M. Hui, T. B. Humensky, A. Imran, P. Kaaret, N. Karlsson, M. Kertzman, D. Kieda, J. Kildea, A. Konopelko, H. Krawczynski, F. Krennrich, M. J. Lang, S. LeBohec, G. Maier, A. McCann, M. McCutcheon, J. Millis, P. Moriarty, R. Mukherjee, R. A. Ong, A. N. Otte, D. Pandel, J. S. Perkins, D. Petry, M. Pohl, J. Quinn, K. Ragan, L. C. Reyes, P. T. Reynolds, H. J. Rose, M. Schroedter, G. H. Sembroski, A. W. Smith, D. Steele, S. Swordy, M. Theiling, J. A. Toner, A. Varlotta, V. V. Vassiliev, S. Vincent, R. G. Wagner, S. P. Wakely, J. E. Ward, T. C. Weekes, A. Weinstein, T. Weisgarber, D. A. Williams, S. Wissel, and M. Wood

Subjects
stars, catalog, Be star, Astrophysics::High Energy Astrophysical Phenomena, binary, FOS: Physical sciences, Astrophysics, telescope, 01 natural sciences, emission, 0103 physical sciences, 010303 astronomy & astrophysics, acceleration of particles, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, stars: individual (hess j0632+057, mwc 148), Gamma ray, X-ray, Astronomy and Astrophysics, Crab Nebula, binaries: general, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, gamma rays: observations, discovery
Abstract

HESS J0632+057 is one of only two unidentified very-high-energy gamma-ray sources which appear to be point-like within experimental resolution. It is possibly associated with the massive Be star MWC 148 and has been suggested to resemble known TeV binary systems like LS I +61 303 or LS 5039. HESS J0632+057 was observed by VERITAS for 31 hours in 2006, 2008 and 2009. During these observations, no significant signal in gamma rays with energies above 1 TeV was detected from the direction of HESS J0632+057. A flux upper limit corresponding to 1.1% of the flux of the Crab Nebula has been derived from the VERITAS data. The non-detection by VERITAS excludes with a probability of 99.993% that HESS J0632+057 is a steady gamma-ray emitter. Contemporaneous X-ray observations with Swift XRT reveal a factor of 1.8+-0.4 higher flux in the 1-10 keV range than earlier X-ray observations of HESS J0632+057. The variability in the gamma-ray and X-ray fluxes supports interpretation of the ob ject as a gamma-ray emitting binary., Comment: 8 pages, 3 figures, Accepted for publication in The Astrophysical Journal

Published
2009
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8. The HAWC Real-time Flare Monitor for Rapid Detection of Transient Events

Author

Humberto Ibarguen Salazar, O. Martinez, Karen S. Caballero-Mora, Mehr Nisa, J. Braun, S. Coutiño de León, H. A. Ayala Solares, Ignacio Taboada, J. P. Harding, M. Newbold, Daniel Rosa-Gonzalez, Brenda Dingus, J. Martínez-Castro, J. Pretz, E. Moreno, J.C. Arteaga-Velázquez, N. Fraija, R. Arceo, P. W. Younk, Abel Bernal, Chad Brisbois, D. W. Fiorino, M. J. F. Rosenberg, J. T. Linnemann, Dirk Lennarz, R. W. Springer, Chang Dong Rho, E. G. Pérez-Pérez, Giacomo Vianello, Michael DuVernois, S. Hernandez, U. Cotti, Michael Schneider, I. G. Wisher, R. Luna-Garcia, C. Alvarez, David Kieda, Fernando Garfias, A. Becerril, A. J. Smith, I. Torres, A. González Muñoz, Ruben Lopez-Coto, A. Iriarte, Thomas Weisgarber, Edna Ruiz-Velasco, I. Martinez-Castellanos, M. Mostafá, T. Capistrán, Anna Lia Longinotti, F. Salesa Greus, M. Castillo, Pooja Surajbali, C. De León, A. Sandoval, H. León Vargas, Kristi Engel, Maria Magdalena González, R. J. Lauer, Sarah Kaufmann, K. Malone, Juan Carlos Diaz-Velez, Kirsten Tollefson, H. Martínez-Huerta, Armelle Jardin-Blicq, Z. Ren, T. Yapici, Harm Schoorlemmer, G. Luis Raya, A. Zepeda, R. Noriega-Papaqui, Sabrina Casanova, C. Rivière, V. Joshi, E. De la Fuente, Z. Hampel-Arias, D. Avila Rojas, T. N. Ukwatta, S. S. Marinelli, M. Gerhardt, J. D. Álvarez, J. A. Goodman, Jose Andres Garcia-Gonzalez, Diego Lopez-Camara, J. Becerra González, Ernesto Belmont-Moreno, P. Hüntemeyer, W. H. Lee, J. Cotzomi, Rodrigo Pelayo, S. Westerhoff, Binita Hona, G. Sinnis, Joshua A. Wood, A. Hernandez-Almada, A. Carraminana, A. S. Barber, Anushka Udara Abeysekara, R. W. Ellsworth, O. Tibolla, N. Bautista-Elivar, Pedro Miranda-Romagnoli, C. M. Hui, Lukas Nellen, Segev BenZvi, Hao Zhou, R. Alfaro, and J. A. Matthews

Subjects
HAWC - Abteilung Hinton, High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Rapid detection, law.invention, Space and Planetary Science, law, 0103 physical sciences, Transient (oscillation), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Flare
Abstract

We present the development of a real-time flare monitor for the High Altitude Water Cherenkov (HAWC) observatory. The flare monitor has been fully operational since 2017 January and is designed to detect very high energy (VHE; $E\gtrsim100$ GeV) transient events from blazars on time scales lasting from 2 minutes to 10 hours in order to facilitate multiwavelength and multimessenger studies. These flares provide information for investigations into the mechanisms that power the blazars' relativistic jets and accelerate particles within them, and they may also serve as probes of the populations of particles and fields in intergalactic space. To date, the detection of blazar flares in the VHE range has relied primarily on pointed observations by imaging atmospheric Cherenkov telescopes. The recently completed HAWC observatory offers the opportunity to study VHE flares in survey mode, scanning 2/3 of the entire sky every day with a field of view of $\sim$1.8 steradians. In this work, we report on the sensitivity of the HAWC real-time flare monitor and demonstrate its capabilities via the detection of three high-confidence VHE events in the blazars Markarian 421 and Markarian 501., Comment: 19 pages, 14 figures, revised version submitted to The Astrophysical Journal on 1 June 2017

Published
2017
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9. FERMIGBM OBSERVATIONS OF V404 CYG DURING ITS 2015 OUTBURST

Author

Valerie Connaughton, Mark H. Finger, Péter Veres, Jeroen Homan, M. Hui, Colleen A. Wilson-Hodge, Eric Burns, Michael S. Briggs, and Peter Jenke

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Compton scattering, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Electron, 01 natural sciences, Spectral line, Luminosity, Black hole, Space and Planetary Science, 0103 physical sciences, Electron temperature, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract

V404 Cygni was discovered in 1989 by the $Ginga$ X-ray satellite during its only previously observed X-ray outburst and soon after confirmed as a black hole binary. On June 15, 2015, the Gamma Ray Burst Monitor (GBM) triggered on a new outburst of V404 Cygni. We present 13 days of GBM observations of this outburst including Earth occultation flux measurements, spectral and temporal analysis. The Earth occultation fluxes reached 30 Crab with detected emission to 100 keV and determined, via hardness ratios, that the source was in a hard state. At high luminosity, spectral analysis between 8 and 300 keV showed that the electron temperature decreased with increasing luminosity. This is expected if the protons and electrons are in thermal equilibrium during an outburst with the electrons cooled by the Compton scattering of softer seed photons from the disk. However, the implied seed photon temperatures are unusually high, suggesting a contribution from another source, such as the jet. No evidence of state transitions is seen during this time period. The temporal analysis reveals power spectra that can be modeled with two or three strong, broad Lorentzians, similar to the power spectra of black hole binaries in their hard state.

Published
2016
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10. FERMI GBM OBSERVATIONS OF LIGO GRAVITATIONAL-WAVE EVENT GW150914

Author

Judith Racusin, Melissa Gibby, Péter Veres, K. Toelge, Gerard Fitzpatrick, P. N. Bhat, Valerie Connaughton, M. Stanbro, J. B. Camp, Adam Goldstein, P. Shawhan, Nelson Christensen, Robert D. Preece, Bin-Bin Zhang, Eric Burns, Peter Jenke, W. H. Cleveland, William S. Paciesas, Tyson Littenberg, R. M. Kippen, Leo Singer, Elisabetta Bissaldi, Colleen A. Wilson-Hodge, Misty Giles, Bagrat Mailyan, Charles A. Meegan, C. M. Hui, Oliver J. Roberts, Sheila McBreen, Michael S. Briggs, A. von Kienlin, Linda S. Sparke, J. McEnery, John Veitch, and Lindy Blackburn

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Stellar mass, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, LIGO, Luminosity, Black hole, gravitational waves, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Transient (oscillation), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Event (particle physics), Fermi Gamma-ray Space Telescope
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$\sigma$). This weak transient lasting 1 s was not detected by any other instrument and does not appear 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 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, 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 $1.8^{+1.5}_{-1.0} \times 10^{49}$~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 Gamma-Ray Bursts., Comment: Accepted for publication in ApJL

Published
2016
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11. A Fermi Gamma-Ray Burst Monitor Search for Electromagnetic Signals Coincident with Gravitational-wave Candidates in Advanced LIGO's First Observing Run

Author

E. Burns, A. Goldstein, C. M. Hui, L. Blackburn, M. S. Briggs, V. Connaughton, R. Hamburg, D. Kocevski, P. Veres, C. A. Wilson-Hodge, E. Bissaldi, W. H. Cleveland, M. M. Giles, B. Mailyan, C. A. Meegan, W. A. Paciesas, S. Poolakkil, R. D. Preece, J. L. Racusin, O. J. Roberts, A. von Kienlin, Gamma-Ray Burst Monitor, B. P. Abbott, R. Abbott, T. D. Abbott, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso, R. X. Adhikari, V. B. Adya, C. Affeldt, B. Agarwal, M. Agathos, K. Agatsuma, N. Aggarwal, O. D. Aguiar, L. Aiello, A. Ain, P. Ajith, B. Allen, G. Allen, A. Allocca, M. A. Aloy, P. A. Altin, A. Amato, A. Ananyeva, S. B. Anderson, W. G. Anderson, S. V. Angelova, S. Antier, S. Appert, K. Arai, M. C. Araya, J. S. Areeda, M. Arène, N. Arnaud, K. G. Arun, S. Ascenzi, G. Ashton, M. Ast, S. M. Aston, P. Astone, D. V. Atallah, F. Aubin, P. Aufmuth, C. Aulbert, K. AultONeal, C. Austin, A. Avila-Alvarez, S. Babak, P. Bacon, F. Badaracco, M. K. M. Bader, S. Bae, P. T. Baker, F. Baldaccini, G. Ballardin, S. W. Ballmer, S. Banagiri, J. C. Barayoga, S. E. Barclay, B. C. Barish, D. Barker, K. Barkett, S. Barnum, F. Barone, B. Barr, L. Barsotti, M. Barsuglia, D. Barta, J. Bartlett, I. Bartos, R. Bassiri, A. Basti, J. C. Batch, M. Bawaj, J. C. Bayley, M. Bazzan, B. Bécsy, C. Beer, M. Bejger, I. Belahcene, A. S. Bell, D. Beniwal, M. Bensch, B. K. Berger, G. Bergmann, S. Bernuzzi, J. J. Bero, C. P. L. Berry, D. Bersanetti, A. Bertolini, J. Betzwieser, R. Bhandare, I. A. Bilenko, S. A. Bilgili, G. Billingsley, C. R. Billman, J. Birch, I. A. Birney, O. Birnholtz, S. Biscans, S. Biscoveanu, A. Bisht, M. Bitossi, M. A. Bizouard, J. K. Blackburn, J. Blackman, C. D. Blair, D. G. Blair, R. M. Blair, S. Bloemen, O. Bock, N. Bode, M. Boer, Y. Boetzel, G. Bogaert, A. Bohe, F. Bondu, E. Bonilla, R. Bonnand, P. Booker, B. A. Boom, C. D. Booth, R. Bork, V. Boschi, S. Bose, K. Bossie, V. Bossilkov, J. Bosveld, Y. Bouffanais, A. Bozzi, C. Bradaschia, P. R. Brady, A. Bramley, M. 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Wallace, S. Walsh, G. Wang, H. Wang, J. Z. Wang, W. H. Wang, Y. F. Wang, R. L. Ward, J. Warner, M. Was, J. Watchi, B. Weaver, L.-W. Wei, M. Weinert, A. J. Weinstein, R. Weiss, F. Wellmann, L. Wen, E. K. Wessel, P. Weßels, J. Westerweck, K. Wette, J. T. Whelan, B. F. Whiting, C. Whittle, D. Wilken, D. Williams, R. D. Williams, A. R. Williamson, J. L. Willis, B. Willke, M. H. Wimmer, W. Winkler, C. C. Wipf, H. Wittel, G. Woan, J. Woehler, J. K. Wofford, W. K. Wong, J. Worden, J. L. Wright, D. S. Wu, D. M. Wysocki, S. Xiao, W. Yam, H. Yamamoto, C. C. Yancey, L. Yang, M. J. Yap, M. Yazback, Hang Yu, Haocun Yu, M. Yvert, A. Zadrożny, M. Zanolin, T. Zelenova, J.-P. Zendri, M. Zevin, J. Zhang, L. Zhang, M. Zhang, T. Zhang, Y.-H. Zhang, C. Zhao, M. Zhou, Z. Zhou, S. J. Zhu, X. J. Zhu, M. E. Zucker, J. Zweizig, and The LIGO Scientific Collaboration and the Virgo Collaboration

Subjects
gamma-ray burst: general, gravitational waves, Astrophysics, QB460-466
Abstract

We present a search for prompt gamma-ray counterparts to compact binary coalescence gravitational wave (GW) candidates from Advanced LIGO’s first observing run (O1). As demonstrated by the multimessenger observations of GW170817/GRB 170817A, electromagnetic and GW observations provide complementary information about the astrophysical source, and in the case of weaker candidates, may strengthen the case for an astrophysical origin. Here we investigate low-significance GW candidates from the O1 compact binary coalescence searches using the Fermi Gamma-Ray Burst Monitor (GBM), leveraging its all sky and broad energy coverage. Candidates are ranked and compared to background to measure the significance. Those with false alarm rates (FARs) of less than 10 ^−5 Hz (about one per day, yielding a total of 81 candidates) are used as the search sample for gamma-ray follow-up. No GW candidates were found to be coincident with gamma-ray transients independently identified by blind searches of the GBM data. In addition, GW candidate event times were followed up by a separate targeted search of GBM data. Among the resulting GBM events, the two with the lowest FARs were the gamma-ray transient GW150914-GBM presented in Connaughton et al. and a solar flare in chance coincidence with a GW candidate.

Published
2019
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