CIV和Fe K α Baldwin效应的起源探讨
Probing the Origins of the CIV and Fe Kalpha Baldwin Effect
摘要：
利用对272个射电宁静的1型活动星系核和类星体的紫外、光学和X射线观测资料，研究了CIV Baldwin效应（BEff）。紫外/光学光谱来自哈勃太空望远镜，国际紫外线探测器和斯隆数字巡天档案。X射线光谱来自Chandra和XMM-Newton档案。我们应用相关和偏相关分析的等效宽度，连续单色光度，和alpha_ox，它的相对X射线紫外亮度的特点。CIV 1549发射线的等效宽度与α_ox和亮度都相关。我们发现用EW（CIV）和alpha_ox回归l_UV比只用EW（CIV）回归l_UV能得到更紧密的相关性。相关和回归分析表明，lUV不是控制EW（CIV）变化的唯一因素，α ox（或软X射线发射）在CIV的形成和变化中起着重要作用。变异性对EW（CIV）-l_UV关系的分散性的贡献至少为60%，对EW（CIV）-alpha_ox关系的分散性的贡献至少为75%。在我们的样品中，窄Fe Ka 6.4 keV的发射线中检测到50个对象。虽然窄Fe K α具有与CIV相似的BEff，但其等效宽度几乎不依赖于α_ox或EW（CIV）。这表明大部分窄Fe K α发射不太可能在宽发射线区域产生。我们确实发现CIV和Fe Ka的发射线光度之间存在暗示性的相关性，这可能被潜在地用于估计类星体的Fe Ka线从静止帧UV光谱观测的可探测性。
英文摘要：
We use UV/optical and X-ray observations of 272 radio-quiet Type 1 AGNs and quasars to investigate the CIV Baldwin Effect (BEff). The UV/optical spectra are drawn from the Hubble Space Telescope, International Ultraviolet Explorer and Sloan Digital Sky Survey archives. The X-ray spectra are from the Chandra and XMM-Newton archives. We apply correlation and partial-correlation analyses to the equivalent widths, continuum monochromatic luminosities, and alpha_ox, which characterizes the relative X-ray to UV brightness. The equivalent width of the CIV 1549 emission line is correlated with both alpha_ox and luminosity. We find that by regressing l_UV with EW(CIV) and alpha_ox, we can obtain tighter correlations than by regressing l_UV with only EW(CIV). Both correlation and regression analyses imply that l_UV is not the only factor controlling the changes of EW(CIV); alpha_ox (or, equivalently, the soft X-ray emission) plays a fundamental role in the formation and variation of CIV. Variability contributes at least 60% of the scatter of the EW(CIV)-l_UV relation and at least 75% of the scatter of the of the EW(CIV)-alpha_ox relation. In our sample, narrow Fe Kalpha 6.4 keV emission lines are detected in 50 objects. Although narrow Fe Kalpha exhibits a BEff similar to that of CIV, its equivalent width has almost no dependence on either alpha_ox or EW(CIV). This suggests that the majority of narrow Fe Kalpha emission is unlikely to be produced in the broad emission-line region. We do find suggestive correlations between the emission-line luminosities of CIV and Fe Kalpha, which could be potentially used to estimate the detectability of the Fe Kalpha line of quasars from rest-frame UV spectroscopic observations.
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。
