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arXiv 1301.3522astro-ph.HE
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宇宙伽马射线暴费米GBM星表的行星际网络补充

The Interplanetary Network Supplement to the Fermi GBM Catalog of Cosmic Gamma-Ray Bursts

K. Hurley, V. D. Pal'shin, R. L. Aptekar, S. V. Golenetskii, D. D. Frederiks, E. P. Mazets, D. S. Svinkin, M. S. Briggs, V. Connaughton, C. Meegan, J. Goldsten,… 展开作者

K. Hurley, V. D. Pal'shin, R. L. Aptekar, S. V. Golenetskii, D. D. Frederiks, E. P. Mazets, D. S. Svinkin, M. S. Briggs, V. Connaughton, C. Meegan, J. Goldsten, W. Boynton, C. Fellows, K. Harshman, I. G. Mitrofanov, D. V. Golovin, A. S. Kozyrev, M. L. Litvak, A. B. Sanin, A. Rau, A. von Kienlin, X. Zhang, K. Yamaoka, Y. Fukazawa, Y. Hanabata, M. Ohno, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, S. Barthelmy, T. Cline, N. Gehrels, J. Cummings, H. A. Krimm, D. M. Smith, E. Del Monte, M. Feroci, M. Marisaldi

备注：
52 pages, 12 figures, 4 tables. Revised version, resubmitted to the Astrophysical Journal Supplement Series following refereeing. Figures of the localizations in Table 3 may be found on the IPN website, at ssl.berkeley.edu/ipn3/YYMMDD, where YY, MM, and DD are the year, month, and day of the burst, sometimes with suffixes A or B
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摘要：

本文介绍了第一个费米伽马射线暴监测器（GBM）星表中伽马射线暴的行星际网络（IPN）数据。在该目录中的491个爆发中，涵盖2008年7月12日至2010年7月11日，其中427个被9艘航天器IPN中的至少一个其他仪器观测到。在427个中，149个的定位可以通过到达时间分析（或三角测量）来改进。对于GBM和另一个遥远的航天器观测到的任何给定的爆发，三角测量给出了一个可能到达方向的环形，其半宽度在0.4'和32度之间变化，这取决于爆发的强度，时间历史和到达方向，以及航天器之间的距离。我们发现，IPN本地化相交的1西格玛GBM误差圆的情况下，只有52%，如果没有系统的不确定性是假设后者。如果假设6度系统不确定性并以正交方式添加，则两个定位样本在约87%的时间内一致，如预期的那样。如果我们将所得误差半径乘以3，则两个样本在略高于98%的情况下一致，从而提供了对GBM 3 sigma误差半径的良好估计。IPN 3 sigma误差框具有约1平方角分和110平方度之间的面积，并且平均比相应的GBM局部化小180倍。我们确定两个突发的IPN/GBM样品中没有出现在GBM目录。在一种情况下，GBM触发了地面伽马闪光，而在另一种情况下，其起源是不确定的。我们还讨论了IPN的灵敏度和校准。

英文摘要：

We present Interplanetary Network (IPN) data for the gamma-ray bursts in the first Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 491 bursts in that catalog, covering 2008 July 12 to 2010 July 11, 427 were observed by at least one other instrument in the 9-spacecraft IPN. Of the 427, the localizations of 149 could be improved by arrival time analysis (or triangulation). For any given burst observed by the GBM and one other distant spacecraft, triangulation gives an annulus of possible arrival directions whose half-width varies between about 0.4' and 32 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. We find that the IPN localizations intersect the 1 sigma GBM error circles in only 52% of the cases, if no systematic uncertainty is assumed for the latter. If a 6 degree systematic uncertainty is assumed and added in quadrature, the two localization samples agree about 87% of the time, as would be expected. If we then multiply the resulting error radii by a factor of 3, the two samples agree in slightly over 98% of the cases, providing a good estimate of the GBM 3 sigma error radius. The IPN 3 sigma error boxes have areas between about 1 square arcminute and 110 square degrees, and are, on the average, a factor of 180 smaller than the corresponding GBM localizations. We identify two bursts in the IPN/GBM sample that did not appear in the GBM catalog. In one case, the GBM triggered on a terrestrial gamma flash, and in the other, its origin was given as uncertain. We also discuss the sensitivity and calibration of the IPN.

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