The Phoenix galaxy as seen by NuSTAR
The Phoenix galaxy as seen by NuSTAR
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DOI：
10.1051/0004-6361/201629444
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发表时间：
2016-09
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通讯作者：
A. Masini;A. Comastri;S. Puccetti;M. Balokovi'c;P. Gandhi;M. Guainazzi;F. Bauer;S. Boggs;P. Boorman;M. Brightman;F. Christensen;W. Craig;D. Farrah;C. Hailey;F. Harrison;M. Koss;S. LaMassa;C. Ricci;D. Stern;D. Walton;W. Zhang
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作者：
A. Masini;A. Comastri;S. Puccetti;M. Balokovi'c;P. Gandhi;M. Guainazzi;F. Bauer;S. Boggs;P. Boorman;M. Brightman;F. Christensen;W. Craig;D. Farrah;C. Hailey;F. Harrison;M. Koss;S. LaMassa;C. Ricci;D. Stern;D. Walton;W. Zhang
目标。我们研究了著名的Seyfert 2星系Mrk 1210（a.k.a.）的长期变化。UGC 4203，或凤凰星系）。方法.在过去的20年里，许多X射线设备都观察到了这个源。在这里，我们提出了一个努斯塔的观察，并把结果的背景下，以前发表的意见。结果努斯塔在2012年观测到了15.4 k的Mrk 1210。源显示康普顿薄遮蔽类似于钱德拉，朱雀，BeppoSAX和XMM-牛顿在过去二十年中观察到的，但不同于ASCA在1995年的第一次观察，其中活动核被捕获在低通量状态-或被康普顿厚物质遮蔽，具有反射主导的光谱。得益于努斯塔获得的高质量硬X射线光谱，并利用跨越16.9年的长期光谱覆盖范围，我们可以精确地解开透射和反射分量，并对内在的长期变化和隐藏的核情景进行限制。在前一种情况下，反射器和源之间的距离必须至少为~ 2 pc，而在后一种情况下，食云可能被识别为水脉泽发射团。
Aims. We study the long-term variability of the well-known Seyfert 2 galaxy Mrk 1210 (a.k.a. UGC 4203, or the Phoenix galaxy). Methods. The source was observed by many X-ray facilities in the last 20 years. Here we present a NuSTAR observation and put the results in context of previously published observations. Results. NuSTAR observed Mrk 1210 in 2012 for 15.4 ks. The source showed Compton-thin obscuration similar to that observed by Chandra, Suzaku, BeppoSAX and XMM-Newton over the past two decades, but different from the first observation by ASCA in 1995, in which the active nucleus was caught in a low flux state - or obscured by Compton-thick matter, with a reflection-dominated spectrum. Thanks to the high-quality hard X-ray spectrum obtained with NuSTAR and exploiting the long-term spectral coverage spanning 16.9 years, we can precisely disentangle the transmission and reflection components and put constraints on both the intrinsic long-term variability and hidden nucleus scenarios. In the former case, the distance between the reflector and the source must be at least ~ 2 pc, while in the latter one the eclipsing cloud may be identified with a water maser-emitting clump.