CALET UPPER LIMITS on X-RAY and GAMMA-RAY COUNTERPARTS of GW151226

ADRIANI, O.; AKAIKE, Y.; ASANO, K.; ASAOKA, Y.; BAGLIESI, M.G.; BIGONGIARI, G.; BINNS, W.R.; BONECHI, S.; BONGI, M.; BROGI, P.; BUCKLEY, J.H.; CANNADY, N.; CASTELLINI, G.; CHECCHIA, C.; CHERRY, M.L.; COLLAZUOL, G.; FELICE, V. DI; EBISAWA, K.; FUKE, H.; GUZIK, T.G.; HAMS, T.; HAREYAMA, M.; HASEBE, N.; HIBINO, K.; ICHIMURA, M.; IOKA, K.; ISHIZAKI, W.; ISRAEL, M.H.; JAVAID, A.; KASAHARA, K.; KATAOKA, J.; KATAOKA, R.; KATAYOSE, Y.; KATO, C.; KAWANAKA, N.; KAWAKUBO, Y.; KITAMURA, H.; KRAWCZYNSKI, H.S.; KRIZMANIC, J.F.; KURAMATA, S.; LOMTADZE, T.; MAESTRO, P.; MARROCCHESI, P.S.; MESSINEO, A.M.; MITCHELL, J.W.; MIYAKE, S.; MIZUTANI, K.; MOISEEV, A.A.; MORI, K.; MORI, M.; MORI, N.; MOTZ, H.M.; MUNAKATA, K.; MURAKAMI, H.; NAKAGAWA, Y.E.; NAKAHIRA, S.; NISHIMURA, J.; OKUNO, S.; ORMES, J.F.; OZAWA, S.; PACINI, L.; PALMA, F.; PAPINI, P.; PENACCHIONI, A.V.; RAUCH, B.F.; RICCIARINI, S.; SAKAI, K.; SAKAMOTO, T.; SASAKI, M.; SHIMIZU, Y.; SHIOMI, A.; SPARVOLI, R.; SPILLANTINI, P.; STOLZI, F.; TAKAHASHI, I.; TAKAYANAGI, M.; TA

Astrophysical Journal Letters

Institute of Physics Publishing

Año: 2016 vol. 829

2041-8205

We present upper limits in the hard X-ray and gamma-ray bands at the time of the Laser Interferometer Gravitational-wave Observatory (LIGO) gravitational-wave event GW151226 derived from the CALorimetric Electron Telescope (CALET) observation. The main instrument of CALET, CALorimeter (CAL), observes gamma-rays from ∼1 GeV up to 10 TeV with a field of view of ∼2 sr. The CALET gamma-ray burst monitor (CGBM) views ∼3 sr and ∼2π sr of the sky in the 7 keV-1 MeV and the 40 keV-20 MeV bands, respectively, by using two different scintillator-based instruments. The CGBM covered 32.5% and 49.1% of the GW151226 sky localization probability in the 7 keV-1 MeV and 40 keV-20 MeV bands respectively. We place a 90% upper limit of 2 ×10-7 erg cm-2 s-1 in the 1-100 GeV band where CAL reaches 15% of the integrated LIGO probability (∼1.1 sr). The CGBM 7σ upper limits are 1.0 ×10-6 erg cm-2 s-1 (7-500 keV) and 1.8 ×10-6 erg cm-2 s-1 (50-1000 keV) for a 1 s exposure. Those upper limits correspond to the luminosity of 3-5 ×1049 erg s-1, which is significantly lower than typical short GRBs.