软X射线解缠AGN与恒星形成
Disentangling AGN and Star Formation in Soft X-rays
摘要：
我们探讨了在软X射线（0.5-2千电子伏）在两个样本的Seyfert 2星系（Sy 2s）的恒星形成和活动星系核活动的相互作用。使用低分辨率CCD光谱的组合，从钱德拉和XMM-牛顿，我们建模的软发射的34 Sy 2使用幂律和热模型。对于11个源的高信噪比钱德拉成像的弥漫的宿主星系的发射，我们估计由于恒星形成的光度，通过删除活动星系核，拟合剩余的发射。活动星系核和恒星形成对其余24颗Sy 2软X射线光度（即L $_{x,AGN}$和L $_{x,SF}$）的贡献由幂律和光谱拟合得到的热光度估算。这些光度是根据XSINGS对正常恒星形成星系的分析得出的模板进行缩放的。为了解释光谱拟合产生的光度误差和比例因子的扩展，我们从蒙特卡罗模拟中估计了L $_{x,AGN}$和L $_{x,SF}$。在3σ置信水平内，模拟的光度值与Chandra成像分析的L $_{x,AGN}$和L $_{x,SF}$一致。利用红外[NeII]12.8μm和[OIV]26μm谱线分别作为恒星形成和活动星系核活动的代表，我们独立地解开了这两个过程对软X射线辐射总量的贡献。这种分解一般与3σ水平的L $_{x,SF}$和L $_{x,AGN}$一致。在没有可分辨的核发射，我们的分解方法提供了一个合理的估计，由于在星系中的恒星形成的发射托管2型活动星系核。
英文摘要：
We have explored the interplay of star formation and AGN activity in soft X-rays (0.5-2 keV) in two samples of Seyfert 2 galaxies (Sy2s). Using a combination of low resolution CCD spectra from Chandra and XMM-Newton, we modeled the soft emission of 34 Sy2s using power law and thermal models. For the 11 sources with high signal-to-noise Chandra imaging of the diffuse host galaxy emission, we estimate the luminosity due to star formation by removing the AGN, fitting the residual emission. The AGN and star formation contributions to the soft X-ray luminosity (i.e. L$_{x,AGN}$ and L$_{x,SF}$) for the remaining 24 Sy2s were estimated from the power law and thermal luminosities derived from spectral fitting. These luminosities were scaled based on a template derived from XSINGS analysis of normal star forming galaxies. To account for errors in the luminosities derived from spectral fitting and the spread in the scaling factor, we estimated L$_{x,AGN}$ and L$_{x,SF}$ from Monte Carlo simulations. These simulated luminosities agree with L$_{x,AGN}$ and L$_{x,SF}$ derived from Chandra imaging analysis within a 3σ confidence level. Using the infrared [NeII]12.8μm and [OIV]26μm lines as a proxy of star formation and AGN activity, respectively, we independently disentangle the contributions of these two processes to the total soft X-ray emission. This decomposition generally agrees with L$_{x,SF}$ and L$_{x,AGN}$ at the 3σ level. In the absence of resolvable nuclear emission, our decomposition method provides a reasonable estimate of emission due to star formation in galaxies hosting type 2 AGN.
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