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| 題名: | Suzaku Wide-band All-sky Monitor measurements of duration distributions of gamma-ray bursts |
| 作者: | 浦田裕次;Ohmori, Norisuke;Yamaoka, Kazutaka;Ohno, Masanori;Sugita, Satoshi;Kinoshita, Ryuuji;Nishioka, Yusuke;Hurley, Kevin;Hanabata, Yoshitaka;Tashiro, Makoto S.;Enomoto, Junichi;Fujinuma, Takeshi;Fukazawa, Yasushi;Iwakiri, Wataru;Kawano, Takafumi;Kokubun, Motohide;Makishima, Kazuo;Matsuoka, Shunsuke;Nagayoshi, Tsutomu;Nakagawa, Yujin E.;Nakaya, Souhei;Nakazawa, Kazuhiro;Takahashi, Tadayuki;Takeda, Sawako;Terada, Yukikatsu;Urata, Yuji;Yabe, Seiya;Yasuda, Tetsuya;Yamauchi, Makoto |
| 貢獻者: | 理學院天文研究所 |
| 日期: | 2016-06-01 |
| 上傳時間: | 2026-04-21 14:53:18 (UTC+8) |
| 出版者: | Oxford University Press;Oxford University Press (OUP) |
| 摘要: | 摘要： AbstractWe report on the T90 and T50 duration distributions and their relations with spectral hardness using 1464 gamma-ray bursts (GRBs), which were observed by the Suzaku Wide-band All-sky Monitor (WAM) from 2005 August 4 to 2010 December 29. The duration distribution is clearly bimodal in three energy ranges (50–120, 120–250, and 250–550 keV), but is unclear in the 550–5000 keV range, probably because of the limited sample size. The WAM durations decrease with energy according to a power-law index of −0.058(−0.034, +0.033). The hardness–duration relation reveals the presence of short–hard and long–soft GRBs. The short:long event ratio tends to be higher with increasing energy. We compared the WAM distribution with ones measured by eight other GRB instruments. The WAM T90 distribution is very similar to those of INTEGRAL/SPI-ACS and Granat/PHEBUS, and least likely to match the Swift/BAT distribution. The WAM short:long event ratio (0.25:0.75) is much different from Swift/BAT (0.08:0.92), but is almost the same as CGRO/BATSE (0.25:0.75). To explain this difference for BAT, we examined three effects: BAT trigger types, energy dependence of the duration, and detection sensitivity differences between BAT and WAM. As a result, we found that the ratio difference could be explained mainly by energy dependence including soft extended emissions for short GRBs and much better sensitivity for BAT which can detect weak/long GRBs. The reason for the same short:long event ratio for BATSE and WAM was confirmed by calculation using the trigger efficiency curve.
出版者： Oxford University Press (OUP)
出版日期： 2016-06-01
出處： Publications of the Astronomical Society of Japan, 2016-06, Vol.68 (SP1), p.S30-
資源來源： Alma/SFX Local Collection
版權： The Author 2016. Published by Oxford University Press on behalf of the Astronomical Society of Japan. All rights reserved. For Permissions, please email: journals.permissionsoup.com 2016
識別號： ISSN: 0004-6264
識別號： ISSN: 2053-051X
識別號： EISSN: 0004-6264
識別號： EISSN: 2053-051X
識別號： DOI: 10.1093/pasj/psw009 |
| 顯示於類別: | [天文研究所] 期刊論文
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