SMS4 样品的 Swift X 射线视图。II.17 个明亮射电源的 X 射线特性

Alessandro Maselli, William R. Forman, Christine Jones, Ralph P. Kraft, Matteo Perri
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引用次数: 0

摘要

根据利用 Neil Gehrels Swift 天文台(以下简称 Swift)观测 SMS4 星表中 18 个明亮射电源的提议,我们获得了 17 个目标的 X 射线观测结果(一个目标未观测到)。我们的第一篇论文讨论了 31 个射电源(见 Maselli 等;20 个作为点源探测到的射电源和一个非常扩展的射电源),在这篇论文之后,我们将介绍这 17 个射电源的最终样本的结果,这些射电源以前缺乏专门的尖头窄视场 (FOV) X 射线观测。在这 17 个射电源中,有一个由于曝光时间很短而没有被 Swift 探测到,但却被 eROSITA 探测到,并被列入数据发布 1 (DR1) 目录。其余未被斯威夫特观测到的源在 DR1 中没有发现 1eRASS 源。新的 Swift 观测结果在 0.3-10 keV 波段发现了 11 个 X 射线源,并给出了 6 个上限。我们研究了 X 射线辐射的范围和硬度比,并在统计数据允许的情况下进行了光谱分析。8 个源的 X 射线辐射与点状辐射一致,而 3 个源则显示出明显的范围,每个源都具有奇特的性质。我们利用 X 射线确定的 12 个探测到的光源的位置和不确定性,与 AllWISE 和 GSC 2.4.2 星表中的红外线和光学光源建立了联系。由于需要同时在红外波段和光学波段进行探测,才能为我们的 X 射线探测建立候选对应体,因此我们为所有 12 个源找到了对应体。按照这种基于 X 射线的方法来推算活动核的位置,我们能够确认怀特等人之前为 8 个源提出的红外对应体,并提供了 4 个新的红外候选体。在光学方面,我们确定的对应天体与 Burgess & Hunstead 以前为所有天体提出的候选天体相吻合。我们讨论了 MRC B0344-345 和 PKS B2148-555 的有趣结构,它们是我们在两次 Swift 活动中都探测到的六个扩展 X 射线源中的两个,并建议对它们进行进一步的 X 射线和无线电研究。对于SMS4中的38个源,我们列出了eROSITA DR1星表中可能存在的18个对应天体。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
A Swift X-Ray View of the SMS4 Sample. II. X-Ray Properties of 17 Bright Radio Sources
Based on a proposal to observe 18 bright radio sources from the SMS4 catalog with the Neil Gehrels Swift Observatory (hereafter Swift), we obtained X-ray observations of 17 targets (one target was not observed). Following up our first paper that discussed 31 sources (see Maselli et al.; 20 sources detected as point sources and one very extended source), we present results for this final sample of 17 radio sources that previously lacked dedicated, pointed narrow-field-of-view (FOV) X-ray observations. One of these 17 sources, undetected by Swift due to a very short exposure, was instead detected by eROSITA, and given in the Data Release 1 (DR1) Catalog. No 1eRASS source was found in the DR1 for the remaining source, unobserved by Swift. The new Swift observations led to 11 X-ray source detections in the 0.3–10 keV band and six upper limits. We investigated the extent of the X-ray emission and the hardness ratio, and when statistics allowed, we carried out a spectral analysis. The X-ray emission of eight sources is consistent with pointlike emission, while three sources show clear evidence of extent, each with peculiar properties. We used the X-ray determined positions and uncertainties of the 12 detected sources to establish associations with infrared and optical sources from the AllWISE and the GSC 2.4.2 catalogs. Requiring a detection in both the infrared and the optical bands to establish a candidate counterpart for our X-ray detections, we identify counterparts for all 12 sources. Following this X-ray-based approach to derive the position of the active nucleus, we are able to confirm the same IR counterparts previously proposed by White et al. for eight sources, and provide four new IR candidates. In the optical, we identify counterparts that match the candidates previously given by Burgess & Hunstead for all sources. We discuss the interesting structure of MRC B0344−345 and PKS B2148−555, two of the six extended X-ray sources that we detected in both our Swift campaigns, and suggest they are very promising for further X-ray and radio investigations. For the 38 SMS4 sources that lack pointed, narrow-FOV X-ray telescope observations, after our Swift campaigns, we list 18 likely counterparts from the eROSITA DR1 catalog.
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