The X-ray view of optically selected dual AGN
The X-ray view of optically selected dual AGN
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DOI：
10.1093/mnras/stac3664
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发表时间：
2022-12
影响因子：
4.8
通讯作者：
A. De Rosa;C. Vignali;P. Severgnini;S. Bianchi;Tamara Bogdanović;M. Charisi;M. Guainazzi;Z. Haiman;S. Komossa;Z. Paragi;M. Pérez-Torres;E. Piconcelli;L. Ducci;M. Parvatikar;R. Serafinelli
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作者：
A. De Rosa;C. Vignali;P. Severgnini;S. Bianchi;Tamara Bogdanović;M. Charisi;M. Guainazzi;Z. Haiman;S. Komossa;Z. Paragi;M. Pérez-Torres;E. Piconcelli;L. Ducci;M. Parvatikar;R. Serafinelli
我们提出了一个光学选择的双重活动星系核的研究与投影分离的3-97千秒差距。使用多波长（MWL）信息（光学，X射线，中红外），我们的特点是该样品的内在核性质，并将它们与孤立系统的。在124个X射线探测到的活动星系核候选者中，有52个是成对出现的，72个是单个X射线源。通过MWL分析，我们证实了AGN的存在，在一个分数>80%的检测到的目标对（42对52）。X射线光谱分析证实了活动星系核的亮度随着分离度的减小而增加的趋势，这表明合并可能有助于触发更明亮的活动星系核。通过X/中红外比值与X射线颜色，我们估计了一小部分康普顿薄活动星系核（1022 cm−2 1024 cm−2）源。这些部分的遮蔽源大于孤立活动星系核的样本中发现的，证实活动星系核对显示出更高的遮蔽度。通过比较去红[O III]发射与所观察到的X射线光度，进一步证实了这一趋势。然而，在合并的早期阶段，该样品中的康普顿厚源的导出分数低于合并后期的双活动星系核样品的报告。通过比较X射线的NH与窄线区E（B-V）的NH，我们发现吸收物质可能与环面或宽线区有关。我们还探讨了双活动星系核候选者的X射线探测效率，发现当观察正确（在轴上的位置和长时间曝光），X射线数据是一个强大的方式来确认和调查双活动星系核系统。
We present a study of optically selected dual AGN with projected separations of 3–97 kpc. Using multi-wavelength (MWL) information (optical, X-rays, mid-IR), we characterized the intrinsic nuclear properties of this sample and compared them with those of isolated systems. Among the 124 X-ray detected AGN candidates, 52 appear in pairs and 72 as single X-ray sources. Through MWL analysis, we confirmed the presence of the AGN in a fraction >80% of the detected targets in pairs (42 over 52). X-ray spectral analysis confirms the trend of increasing AGN luminosity with decreasing separation, suggesting that mergers may have contributed in triggering more luminous AGN. Through X/mid-IR ratio vs X-ray colors, we estimated a fraction of Compton-thin AGN (with 1022 cm−2 1024 cm−2) sources. These fractions of obscured sources are larger than those found in samples of isolated AGN, confirming that pairs of AGN show higher obscuration. This trend is further confirmed by comparing the de-reddened [O III] emission with the observed X-ray luminosity. However, the derived fraction of Compton-thick sources in this sample at early stage of merging is lower than reported for late-merging dual-AGN samples. Comparing NH from X-rays with that derived from E(B-V) from Narrow Line Regions, we find that the absorbing material is likely associated with the torus or the Broad Line Regions. We also explored the X-ray detection efficiency of dual-AGN candidates, finding that, when observed properly (at on-axis positions and with long exposures), X-ray data represent a powerful way to confirm and investigate dual-AGN systems.