Bolometric luminosities and Eddington ratios of X-ray selected Active Galactic Nuclei in the XMM-COSMOS survey
E. Lusso, A. Comastri, B. D. Simmons, M. Mignoli, G. Zamorani, C. Vignali, M. Brusa, F. Shankar, D. Lutz, J. R. Trump, R. Maiolino, R. Gilli, M. Bolzonella, S. … 展开作者
E. Lusso, A. Comastri, B. D. Simmons, M. Mignoli, G. Zamorani, C. Vignali, M. Brusa, F. Shankar, D. Lutz, J. R. Trump, R. Maiolino, R. Gilli, M. Bolzonella, S. Puccetti, M. Salvato, C. D. Impey, F. Civano, M. Elvis, V. Mainieri, J. D. Silverman, A. M. Koekemoer, A. Bongiorno, A. Merloni, S. Berta, E. Le Floc'h, B. Magnelli, F. Pozzi, L. Riguccini
Bolometric luminosities and Eddington ratios of both X-ray selected broad-line (Type-1) and narrow-line (Type-2) AGN from the XMM-Newton survey in the COSMOS field are presented. The sample is composed by 929 AGN (382 Type-1 AGN and 547 Type-2 AGN) and it covers a wide range of redshifts, X-ray luminosities and absorbing column densities. About 65% of the sources are spectroscopically identified as either Type-1 or Type-2 AGN (83% and 52% respectively), while accurate photometric redshifts are available for the rest of the sample. The study of such a large sample of X-ray selected AGN with a high quality multi-wavelength coverage from the far-infrared (now with the inclusion of Herschel data at 100 micron and 160 micron) to the optical-UV allows us to obtain accurate estimates of bolometric luminosities, bolometric corrections and Eddington ratios. The kbol-Lbol relations derived in the present work are calibrated for the first time against a sizable AGN sample, and rely on observed redshifts, X-ray luminosities and column density distributions. We find that kbol is significantly lower at high Lbol with respect to previous estimates by Marconi et al. (2004) and Hopkins et al. (2007). Black hole masses and Eddington ratios are available for 170 Type-1 AGN, while black hole masses for Type-2 AGN are computed for 481 objects using the black hole mass-stellar mass relation and the morphological information. We confirm a trend between kbol and lambda_Edd, with lower hard X-ray bolometric corrections at lower Eddington ratios for both Type-1 and Type-2 AGN. We find that, on average, Eddington ratio increases with redshift for all Types of AGN at any given Mbh, while no clear evolution with redshift is seen at any given Lbol.
Constraints on cosmological parameters from gamma-ray burst peak photon energy and bolometric fluence measurements and other data
我们使用测量的峰值光子能量和辐射热通量的119伽马射线暴（GRB）的红移范围内的$0.3399 \leq z \leq 8.2$，同时确定宇宙学和Amati关系参数在六个不同的宇宙学模型。由此产生的阿马蒂关系参数是几乎相同的所有六个宇宙学模型，从而验证了使用阿马蒂关系标准化这些伽玛暴。伽玛射线暴数据宇宙学参数的限制是一致的，但显着较少的限制，从联合分析的重子声学振荡和哈勃参数测量。
Bolometric correction for cosmologically redshifted stars with dust: an update to the YBC database
Anhui University（安徽大学）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Universität Potsdam（波茨坦大学）；SISSA（的里雅斯特国际高等研究学院）
Obscured GOODS AGN and Their Host Galaxies at z < 1.25: The Slow Black Hole Growth Phase
我们计算了从GOODS深多波长巡天中选出的红移范围为0.25 < z < 1.25的87个活动星系核的黑洞质量和辐射光度。我们适合的光学图像，并获得宿主星系的形态参数，分离的星系从其中心点源，从而获得一个四波段的光学SED为每个活跃的核。我们计算这些AGN的辐射热光度通过红化一个归一化的平均SED的货物宽线AGN，以匹配所观察到的中心点源SED的每个遮蔽AGN。Lbol的这种估计比对X射线光度的简单测热校正或对观测到的多波长SED的直接积分具有更小的扩展，这表明它是一种更好的测量方法。我们估计中心黑洞质量的隆起光度。黑洞的质量跨度很大，从7 x 10^6 M_sun到6 x 10^9 M_sun;黑洞的质量中值为5 x 10^8 M_sun。这些活动星系核中的大多数具有L/LEdd < 0.01，并且我们没有检测到平均爱丁顿比到z = 1.25的显著演化。这意味着在这些被遮蔽的活动星系核中，大部分黑洞的增长必定发生在z > 1的位置，我们观察到的活动星系核处于缓慢增长或不增长的状态。
The role of the Gamma-Eddington ratio relation on the X-ray Baldwin effect in Active Galactic Nuclei
X射线Baldwin效应是铁K α线窄分量的等效宽度（EW）与活动星系核（AGN）的X射线光度之间的反相关。在Fe K α EW和爱丁顿比（lambda_Edd）之间也观察到类似的趋势。利用Shu等人（2010）的Chandra/HEG结果和测热校正，我们研究了EW和lambda_Edd之间的关系，发现log EW =（-0.13+/-0.03）log（lambda_Edd）+ 1.47。我们探讨了主X射线连续谱的光子指数（Gamma）和lambda_Edd之间的正相关性对X射线Baldwin效应的作用。考虑到反射材料的3种不同几何形状：环形、球-环形和板状，我们模拟了未吸收活动星系核群体发射的铁K α线。我们发现，γ-λ_Edd相关性不能解释整个X射线Baldwin效应，除非假设γ对λ_Edd有很强的依赖性，如Risaliti等人（2009）和Jin等人（2012）最近发现的。EW和Gamma之间没有明显的相关性。我们的结论是，一个很好的理解的斜率的γ-λ_Edd关系是至关重要的，以评估是否在X射线鲍德温效应的趋势起着主导作用，而是一个边缘的作用。
