IC 2497附近的Hanny Voorwerp的软X射线对应物
The soft X-ray counterpart of Hanny's Voorwerp near IC 2497
摘要：
我们报告在钱德拉ACIS档案数据中探测到一个细长的软（<3 keV）X射线特征TP南部的康普顿厚活动星系核（CT AGN）星系IC 2497，与发射特征称为汉尼的Voorwerp（HV）。这些数据与X射线、光发射线和在附近被遮蔽的活动星系核中探测到的射电特征（例如，ESO 428-G014）。软特征的X射线亮度（0.3-3.0 keV）约为1.2 × 10^40 erg/s。我们推断[OIII]/软X射线比值在~200的范围内，与NGC 4151的一些云中测量的最高值一致。总体而言，考虑到不确定性，汉尼的Voorwerp似乎是一个功能与附近活动星系核的电离锥发射一致。我们估计X射线复合时间为2 × 10^7年，比[OIII]复合时间（约8000年）长。这表明，扩展软X射线组件可能是整体长期活动的更好诊断，而[OIII] HV的检测将指向限时活动爆发。
英文摘要：
We report the detection in Chandra ACIS archival data of an elongated soft (<3 keV) X-ray feature tp the south of the Compton Thick Active Galactic Nucleus (CT AGN) galaxy IC 2497, coincident with the emission feature known as Hanny's Voorwerp (HV). The data are consistent with the spatial correspondence between X-ray, optical emission line, and radio features detected in nearby obscured AGNs (e.g., ESO 428-G014). The X-ray luminosity of the (0.3-3.0 keV) soft feature is ~1.2x10^40 erg/s. We infer an [OIII]/Soft-X-ray ratio in the range of ~200, consistent with the highest values measured in some of the clouds of NGC 4151. Overall, given the uncertainties, Hanny's Voorwerp appears to be a feature consistent with the ionization cone emission of nearby AGNs. We estimate an X-ray recombination time of 2x10^7 yr, longer than the [OIII] recombination time (~8000 yr). This suggests that extended soft X-ray components may be a better diagnostic of overall long-term activity, while detection of an [OIII] HV would point to a time-limited activity burst.
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