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arXiv · 1406.3912

MAXI observations of GRBs

Motoko Serino·Takanori Sakamoto·Nobuyuki Kawai·Atsumasa Yoshida·Masanori Ohno·Yuji Ogawa·Yasunori Nishimura·Kosuke Fukushima·Masaya Higa·Kazuto Ishikawa·Masaki Ishikawa·Taiki Kawamuro·Masashi Kimura·Masaru Matsuoka·Tatehiro Mihara·Mikio Morii·Yujin E. Nakagawa·Satoshi Nakahira·Motoki Nakajima·Yuki Nakano·Hitoshi Negoro·Takuya Onodera·Masayuki Sasaki·Megumi Shidatsu·Juri Sugimoto·Mutsumi Sugizaki·Fumitoshi Suwa·Kazuhiko Suzuki·Yutaro Tachibana·Toshihiro Takagi·Takahiro Toizumi·Hiroshi Tomida·Yohko Tsuboi·Hiroshi Tsunemi·Yoshihiro Ueda·Shiro Ueno·Ryuichi Usui·Hisaki Yamada·Takayuki Yamamoto·Kazutaka Yamaoka·Makoto Yamauchi·Koshiro Yoshidome·Taketoshi Yoshii
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Abstract

Monitor of all-sky image (MAXI) Gas Slit Camera (GSC) detects gamma-ray bursts (GRBs) including the bursts with soft spectra, such as X-ray flashes (XRFs). MAXI/GSC is sensitive to the energy range from 2 to 30 keV. This energy range is lower than other currently operating instruments which is capable of detecting GRBs. Since the beginning of the MAXI operation on August 15, 2009, GSC observed 35 GRBs up to the middle of 2013. One third of them are also observed by other satellites. The rest of them show a trend to have soft spectra and low fluxes. Because of the contribution of those XRFs, the MAXI GRB rate is about three times higher than those expected from the BATSE log N - log P distribution. When we compare it to the observational results of the Wide-field X-ray Monitor on the High Energy Transient Explorer 2, which covers the the same energy range to that of MAXI/GSC, we find a possibility that many of MAXI bursts are XRFs with Epeak lower than 20 keV. We discuss the source of soft GRBs observed only by MAXI. The MAXI log N - log S distribution suggests that the MAXI XRFs distribute in closer distance than hard GRBs. Since the distributions of the hardness of galactic stellar flares and X-ray bursts overlap with those of MAXI GRBs, we discuss a possibility of a confusion of those galactic transients with the MAXI GRB samples.

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Motoko Serino, Takanori Sakamoto, Nobuyuki Kawai, Atsumasa Yoshida, Masanori Ohno, Yuji Ogawa, Yasunori Nishimura, Kosuke Fukushima, Masaya Higa, Kazuto Ishikawa, Masaki Ishikawa, Taiki Kawamuro, Masashi Kimura, Masaru Matsuoka, Tatehiro Mihara, Mikio Morii, Yujin E. Nakagawa, Satoshi Nakahira, Motoki Nakajima, Yuki Nakano, Hitoshi Negoro, Takuya Onodera, Masayuki Sasaki, Megumi Shidatsu, Juri Sugimoto, Mutsumi Sugizaki, Fumitoshi Suwa, Kazuhiko Suzuki, Yutaro Tachibana, Toshihiro Takagi, Takahiro Toizumi, Hiroshi Tomida, Yohko Tsuboi, Hiroshi Tsunemi, Yoshihiro Ueda, Shiro Ueno, Ryuichi Usui, Hisaki Yamada, Takayuki Yamamoto, Kazutaka Yamaoka, Makoto Yamauchi, Koshiro Yoshidome, Taketoshi Yoshii. 2014-06-16. MAXI observations of GRBs. https://doi.org/10.1093/pasj%2Fpsu063

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