XMM-牛顿广角巡天（XWAS）：1型AGN的X射线谱
The XMM-Newton Wide Angle Survey (XWAS): the X-ray spectrum of type-1 AGN
摘要：
我们讨论的宽频带X射线属性的X射线选择1型活动星系核迄今为止（487个对象），从XMM-牛顿广角巡天绘制的最大样本之一。这些天体的亮度范围为2-10 keV，范围为~10^{42}-10 ^<$45} erg s^{-1}，并且被探测到的红移高达~4。我们约束的宽带连续谱，软过剩和X射线吸收的整体性能，以及它们对X射线亮度和红移的依赖关系，我们讨论了活动星系核发射模型的影响。我们将宽带X射线连续谱的平均谱指数限制为<Gamma>=1.96+-0.02，本征色散σ =0.27 - 0.02 ^{+0.01}。在微弱的流量和更高的红移和光度下，连续谱变得更难。伽马与通量的相关性可能是由于未检测到的吸收，而不是光谱变化。我们发现物体的检测效率对光谱形状有很强的依赖性，这会对不同红移和光度下源的测量平均连续谱形状产生很大影响。我们在大约3%的物体中检测到了过量吸收，柱密度大约为几× 10 ^{22} cm^{-2}。这些天体的光学分类和X射线性质之间的明显不匹配对标准活动星系核统一模型是一个挑战。我们发现，检测到软过剩的对象的分数是~ 36%。使用热模型，我们约束的软过剩平均温度和本征色散<kT>~100 eV和σ ~34 eV。根据探测到的温度和测量温度与X射线光度之间缺乏相关性（删节），排除了软过剩的起源是来自吸积盘的热发射或康普顿散射盘发射。
英文摘要：
We discuss the broad band X-ray properties of one of the largest samples of X-ray selected type-1 AGN to date (487 objects in total), drawn from the XMM-Newton Wide Angle Survey. The objects cover 2-10 keV luminosities from ~10^{42}-10^{45} erg s^{-1} and are detected up to redshift ~4. We constrain the overall properties of the broad band continuum, soft excess and X-ray absorption, along with their dependence on the X-ray luminosity and redshift and we discuss the implications for models of AGN emission. We constrained the mean spectral index of the broad band X-ray continuum to <Gamma>=1.96+-0.02 with intrinsic dispersion sigma=0.27_{-0.02}^{+0.01}. The continuum becomes harder at faint fluxes and at higher redshifts and luminosities. The dependence of Gamma with flux is likely due to undetected absorption rather than to spectral variation. We found a strong dependence of the detection efficiency of objects on the spectral shape which can have a strong impact on the measured mean continuum shapes of sources at different redshifts and luminosities. We detected excess absorption in ~3% of our objects, with column densities ~a few x10^{22} cm^{-2}. The apparent mismatch between the optical classification and X-ray properties of these objects is a challenge for the standard AGN unification model. We found that the fraction of objects with detected soft excess is ~36%. Using a thermal model, we constrained the soft excess mean temperature and intrinsic dispersion to <kT>~100 eV and sigma~34 eV. The origin of the soft excess as thermal emission from the accretion disk or Compton scattered disk emission is ruled out on the basis of the temperatures detected and the lack of correlation of the measured temperature with the X-ray luminosity (abridged).
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
