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arXiv 0906.2773astro-ph.HE
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Swift J1753 .5-0127的回波标测

Echo-Mapping of Swift J1753.5-0127

R. I. Hynes, K. O'Brien, F. Mullally, T. Ashcraft

备注：
7 pages, accepted for publication in Monthly Notices of the Royal Astronomical Society
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摘要：

我们提出了两个时期的协调X射线光学定时观测的黑洞候选人斯威夫特J1753.5-0127在其2005年爆发。7月第一次出现在爆发高峰期。连续两个晚上使用麦克唐纳天文台Argos相机和罗西X射线定时探测器进行的观测表明，与即时响应和持续约5秒的延长尾巴一致。这种变化和相关性的性质与吸积盘中的热后处理是一致的。滞后时间短表明轨道周期短，与最近声称的一致。8月的第二个纪元再次使用VLT FORS 2 HIT模式与RXTE结合使用。在两个独立的数据子集之间再次看到可重复的相关性。然而，在这种情况下，交叉关联函数具有不寻常的结构，其包括一个谷，随后是一个双峰。我们认为这可能相当于Kanbach等人（2001年）在XTE J1118+480中观察到的下降加单峰结构，并将其归因于同步辐射; Durant等人（2008年）在Swift J1753.5-0127的后期活动中观察到类似的结构。

英文摘要：

We present two epochs of coordinated X-ray-optical timing observations of the black hole candidate Swift J1753.5-0127 during its 2005 outburst. The first epoch in July occurred at outburst peak. Two consecutive nights of observations using the McDonald Observatory Argos camera with the Rossi X-ray Timing Explorer show a consistent correlation with an immediate response and an extended tail lasting ~5s. The properties of the variability and the correlation are consistent with thermal reprocessing in an accretion disk. The shortness of the lag suggests a short orbital period consistent with that recently claimed. The second epoch in August used the VLT FORS2 HIT mode again in conjunction with RXTE. Again a repeatable correlation is seen between two independent subsets of the data. In this case, though, the cross-correlation function has an unusual structure comprising a dip followed by a double-peak. We suggest that this may be equivalent to the dip plus single peak structure seen by Kanbach et al. (2001) in XTE J1118+480 and attributed there to synchrotron emission; a similar structure was seen during later activity of Swift J1753.5-0127 by Durant et al. (2008).

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