Mrk 509上的多波长活动。V. Chandra-LETGS对电离吸收体的观测
Multiwavelength campaign on Mrk 509. V. Chandra-LETGS observation of the ionized absorber
摘要：
在这里，我们提出了一个180 KS的Chandra-LETGS观测的一部分，一个大型的多波长运动Mrk 509的结果。我们研究了Mrk 509中的暖吸收体，并使用同时进行的HST-COS观测数据，以评估负责紫外线和X射线吸收的气体是否相同。我们使用dac拟合软件包分析了Mrk 509的LETGS X射线光谱。我们检测到几个吸收功能起源于电离吸收源，随着解决发射线和辐射复合连续。吸收特征属于具有至少三个不同电离度的离子。最低的电离分量有轻微的红移（v = +73 km/s），并且与其他分量的压力不平衡，因此它不太可能是外流的一部分，可能属于宿主星系的星际介质。其他组分分别以-196和-455 km/s的速度流出。该源与HST-COS同时观测，发现了13个紫外线运动学分量。其中至少有三个可以与观察到的X射线分量运动学相关。基于HST-COS的结果和FUSE的观测，我们发现了紫外吸收气体可能与X射线吸收气体共位且属于同一结构的证据。
英文摘要：
We present here the results of a 180 ks Chandra-LETGS observation as part of a large multi-wavelength campaign on Mrk 509. We study the warm absorber in Mrk 509 and use the data from a simultaneous HST-COS observation in order to assess whether the gas responsible for the UV and X-ray absorption are the same. We analyzed the LETGS X-ray spectrum of Mrk 509 using the SPEX fitting package. We detect several absorption features originating in the ionized absorber of the source, along with resolved emission lines and radiative recombination continua. The absorption features belong to ions with, at least, three distinct ionization degrees. The lowest ionized component is slightly redshifted (v = +73 km/s) and is not in pressure equilibrium with the others, and therefore it is not likely part of the outflow, possibly belonging to the interstellar medium of the host galaxy. The other components are outflowing at velocities of -196 and -455 km/s, respectively. The source was observed simultaneously with HST-COS, finding 13 UV kinematic components. At least three of them can be kinematically associated with the observed X-ray components. Based on the HST-COS results and a previous FUSE observation, we find evidence that the UV absorbing gas might be co-located with the X-ray absorbing gas and belong to the same structure.
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