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arXiv 0803.1113astro-ph
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瞬态X射线双星IGR J01583 +6713的多波长研究

Multiwavelength study of the transient X-ray binary IGR J01583+6713

Ramanpreet Kaur, Biswajit Paul, Brijesh Kumar, Ram Sagar

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22 pages, 8 figures, accepted for publication in MNRAS
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摘要：

我们研究了瞬态X射线双星IGR J 01583 +6713的H $α$谱线轮廓的多波段光度变化和稳定性。在3个月的时间尺度内，我们将{ \it V}波段的光度变化上限设定为0.05 mag。发现H $α$线由非高斯分布组成，并且在2个月的持续时间内相当稳定。我们已经确定伴星的光谱类型为B2 IV e，而到源的距离估计为$\sim$ 4.0 kpc。除了光学观测，我们还对该源的三次短观测的X射线数据进行了分析，两次是用{ \it Swift}-XRT，一次是用{ \it RXTE}-PCA。我们已经检测到吸收柱密度的变化，从爆发后即刻的22.0 $\times$ 10 $^{22}$ cm $^{-2}$下降到4个月后的2.6 $\times$ 10 $^{22}$ cm $^{-2}$。在静止状态下，X射线吸收与E（B-V）= 1.46 mag.的光学红化测量一致。从{ \it Swift}的一次观测中，在此期间X射线强度较高，我们有可能检测到周期为469.2 s的脉冲。对于Be X射线双星，这表明该双星系统的轨道周期在216- 561天之间。

英文摘要：

We have investigated multiband optical photometric variability and stability of the H$α$ line profile of the transient X-ray binary IGR J01583+6713. We set an upper limit of 0.05 mag on photometric variations in the {\it V} band over a time scale of 3 months. The H$α$ line is found to consist of non-Gaussian profile and quite stable for a duration of 2 months. We have identified the spectral type of the companion star to be B2 IVe while distance to the source is estimated to be $\sim$ 4.0 kpc. Along with the optical observations, we have also carried out analysis of X-ray data from three short observations of the source, two with the {\it Swift}--XRT and one with the {\it RXTE}--PCA. We have detected a variation in the absorption column density, from a value of 22.0 $\times$ 10$^{22}$ cm$^{-2}$ immediately after the outburst down to 2.6 $\times$ 10$^{22}$ cm$^{-2}$ four months afterwards. In the quiescent state, the X-ray absorption is consistent with the optical reddening measurement of E(B - V) = 1.46 mag. From one of the {\it Swift} observations, during which the X-ray intensity was higher, we have a possible pulse detection with a period of 469.2 s. For a Be X-ray binary, this indicates an orbital period in the range of 216--561 days for this binary system.

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