对17个性质不确定或未知的INTEGRAL来源进行迅速的后续观察
Swift follow-up observations of 17 INTEGRAL sources of uncertain or unknown nature
摘要：
我们分析了雨燕卫星对17个积分源的观测数据。我们将硬X射线源的位置精确到几个弧秒。然后我们浏览了在线目录（例如，NED、SIMBAD、2 MASS、2 MASX、USNO）来搜索其它波长处的对应物。我们还利用X射线光谱参数试图确定这些来源的性质。我们提供的X射线的位置与arcsec的精度，确定可能的红外和光学同行（当发现），在这些波段，并在光学和紫外线看到的斯威夫特/UVOT望远镜观测时，给出的幅度。我们确认了先前建议的IGR J 03532 -6829、J 05346 -5759、J10101-5654、J13000+2529、J13020-6359、J15479-4529、J18214-1318和J23206+6431的关联和源类型。我们首次确认IGR J 09025 -6814为活动星系核，并认为它可能是Seyfert 2。我们认为IGR J 05319 -6601、J16287-5021、J17353-3539和J17476-2253是X射线双星，其中J 05319 -6601位于大麦哲伦星系，另外三个可能是银河系中的HMXB。对于IGR J15161-3827和J20286+2544，我们在IBIS误差区域中找到了几个可能的X射线对应物，并且我们讨论了哪些（如果有的话）是可能的对应物。两者都可能是活动星系核，尽管后者可能是两个活动星系核的混合体。对于IGR J 03184 -0014和J19267+1325，我们发现X射线源略微超出IBIS误差圆。在前者中，我们不赞成将Swift和INTEGRAL源代码联系在一起，而IGR J19267+1325和Swift源代码很可能是相同的。
英文摘要：
(abridged) We analysed data from observations of 17 INTEGRAL sources made with the Swift satellite. We refine the position of the hard X-ray sources to an accuracy of a few arcsec. We then browsed the online catalogs (e.g., NED, SIMBAD, 2MASS, 2MASX, USNO) to search for counterparts at other wavelengths. We also made use of the X-ray spectral parameters to try to identify the nature of those sources. We provide the X-ray position with arcsec accuracy, identify possible infrared and optical counterparts (when found), give the magnitudes in those bands and in the optical and UV as seen with the Swift/UVOT telescope when observations are available. We confirm the previously suggested associations and source types for IGR J03532-6829, J05346-5759, J10101-5654, J13000+2529, J13020-6359, J15479-4529, J18214-1318, and J23206+6431. We identify IGR J09025-6814 as an AGN for the first time, and we suggest that it may be a Seyfert 2. We suggest that IGR J05319-6601, J16287-5021, J17353-3539 and J17476-2253 are X-ray binaries, with J05319-6601 being located in the LMC and the other three possibly being HMXBs in our Galaxy. For IGR J15161-3827 and J20286+2544, we find several possible X-ray counterparts in the IBIS error region, and we discuss which, if any, are the likely counterparts. Both are likely AGNs, although the latter could be a blend of two AGNs. For IGR J03184-0014 and J19267+1325, we find X-ray sources slightly outside the IBIS error circle. In the former, we do not favour an association of the Swift and INTEGRAL source, while it is very likely that IGR J19267+1325 and the Swift source are the same.
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