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arxiv: 1107.4216 · v1 · pith:22LRMHPJnew · submitted 2011-07-21 · 🌌 astro-ph.HE

MAXI GSC monitoring of the Crab nebula and pulsar during the GeV gamma-ray flare in September 2010

Mikio Morii , Mutsumi Sugizaki , Nobuyuki Kawai , Motoko Serino , Takayuki Yamamoto , Ryuichi Usui , Arata Daikyuji , Ken Ebisawa
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Satoshi Eguchi Kazuo Hiroi Masaki Ishikawa Naoki Isobe Kazuyoshi Kawasaki Masashi Kimura Hiroki Kitayama Mitsuhiro Kohama Takanori Matsumura Masaru Matsuoka Tatehiro Mihara Yujin E. Nakagawa Satoshi Nakahira Motoki Nakajima Hitoshi Negoro Hiroshi Ozawa Megumi Shidatsu Tetsuya Sootome Kousuke Sugimori Fumitoshi Suwa Hiroshi Tomida Yohko Tsuboi Hiroshi Tsunemi Yoshihiro Ueda Shiro Ueno Akiko Uzawa Kazutaka Yamaoka Kyohei Yamazaki Atsumasa Yoshida
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classification 🌌 astro-ph.HE
keywords gamma-rayduringflareperiodpulsarpulsepulsedvariations
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We report on the MAXI GSC X-ray monitoring of the Crab nebula and pulsar during the GeV gamma-ray flare for the period of 2010 September 18-24 (MJD 55457-55463) detected by AGILE and Fermi-LAT. There were no significant variations on the pulse phase averaged and pulsed fluxes during the gamma-ray flare on time scales from 0.5 to 5 days. The pulse profile also showed no significant change during this period. The upper limits on the variations of the pulse phase averaged and pulsed fluxes for the period MJD 55457.5-55462.5 in the 4-10 keV band are derived to be 1 and 19%, respectively, at the 90% confidence limit of the statistical uncertainty. The lack of variations in the pulsed component over the multi-wavelength range (radio, X-ray, hard X-ray, and gamma-ray) supports not the pulsar but the nebular origin for the gamma-ray flare.

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