Mrk573的高分辨X射线能谱和成像
High resolution X-ray spectroscopy and imaging of Mrk573
摘要：
本文详细分析了Seyfert 2星系Mrk 573的XMM-Newton RGS高分辨率X射线谱。这项分析是由钱德拉图像的研究，并比较光学（HST）和无线电（VLA）数据的补充。软X射线发射主要是由于气体光电离的活动星系核，从OVII和OVIII的辐射复合连续的检测，以及由OVII禁戒线的突出表明。这一结果证实了与自洽云光电离模型获得的最佳拟合。然而，为了再现FeXVII线，也需要碰撞激发的分量，约占15-26 A带总光度的1/3。一旦在Chandra ACIS数据中采用相同的模型，则需要另一个具有更高电离参数的光电离组分来考虑来自更高Z金属的发射。宽带ACIS光谱也证实了源的康普顿厚度性质。成像分析显示软X射线和[OIII]发射之间的密切形态对应。无线电发射看起来更紧凑，虽然明显与窄线区域对齐。软X射线发射的碰撞阶段可能是由于星暴，需要$\simeq5-9$ M $_\odot$ yr $^{-1}$的恒星形成率，但没有来自其他波长的这种活动的明确证据。另一方面，它可能与无线电喷射物有关，负责加热与流出物相互作用的等离子体，但热气体的估计压力远大于无线电喷流的压力，假设均分和合理的物理参数。
英文摘要：
We present a detailed analysis of the XMM-Newton RGS high resolution X-ray spectra of the Seyfert 2 galaxy, Mrk573. This analysis is complemented by the study of the Chandra image, and its comparison to optical (HST) and radio (VLA) data. The soft X-ray emission is mainly due to gas photoionised by the central AGN, as indicated by the detection of radiative recombination continua from OVII and OVIII, as well as by the prominence of the OVII forbidden line. This result is confirmed by the best fit obtained with a self-consistent CLOUDY photoionisation model. However, a collisionally excited component is also required, in order to reproduce the FeXVII lines, accounting for about 1/3 of the total luminosity in the 15-26 A band. Once adopted the same model in the Chandra ACIS data, another photoionised component, with higher ionisation parameter, is needed to take into account emission from higher Z metals. The broadband ACIS spectrum also confirms the Compton-thick nature of the source. The imaging analysis shows the close morphological correspondence between the soft X-ray and the [OIII] emission. The radio emission appears much more compact, although clearly aligned with the narrow line region. The collisional phase of the soft X-ray emission may be due to starburst, requiring a star formation rate of $\simeq5-9$ M$_\odot$ yr$^{-1}$, but there is no clear evidence of this kind of activity from other wavelengths. On the other hand, it may be related to the radio ejecta, responsible for the heating of the plasma interacting with the outflow, but the estimated pressure of the hot gas is much larger than the pressure of the radio jets, assuming equipartition and under reasonable physical parameters.
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