论文标题
Wissh Quasars项目XI。最具发光的类星体的平均光谱能分布和降压校正
The WISSH quasars project XI. The mean Spectral Energy Distribution and Bolometric Corrections of the most luminous quasars
论文作者
论文摘要
高透光的准星对象（QSO）代表了研究主动银河核（AGN）反馈机制的理想实验室，因为它们的强大能量释放在所有尺度上都会引起强大的风，因此预期最大反馈。 我们旨在得出85个明智的SDSS样品的平均光谱能量分布（SED）。由于SED提供了研究AGN结构的直接方法，因此我们的目标是了解与大部分人群相比，光度函数的明亮末端是否具有独特的特性。在校正粉尘灭绝，吸收和发射线以及半层次培养基吸收后，我们建立了平均内在的SED。我们还得出了降压测量值，IR频带和单色光度，并在lambda = 5100 A和3微米处进行降压校正。我们定义了3微米辐射校正的新关系。我们发现，高光WISSH QSO的平均SED与较不发光的来源不同，即相对较低的X射线发射和近乎IR的过量量，可以假设较大的灰尘贡献来解释。 Wissh QSO的温暖和非常热的灰尘具有更强的发射，后者是将AGN SED的典型倾角从1.3转移到1.1微米的原因。我们还根据存在宽的吸收线和CIV线的等效宽度而得出了两个子样本的平均SED。我们确认BALS X射线较弱，并且它们具有变红的紫外线连续体。我们还发现，从热灰尘成分中，香脂往往会更强。该分析表明，与较不发光的物体相比，高光QSO具有特殊的SED。因此，在处理特别发光的源时，使用专门从非常明亮的类星体样品构建的SED模板至关重要。
Hyper-luminous Quasi-Stellar Objects (QSOs) represent the ideal laboratory to investigate Active Galactic Nuclei (AGN) feedback mechanism since their formidable energy release causes powerful winds at all scales and thus the maximum feedback is expected. We aim at deriving the mean Spectral Energy Distribution (SED) of a sample of 85 WISE-SDSS Selected Hyper-luminous (WISSH) quasars. Since the SED provides a direct way to investigate the AGN structure, our goal is to understand if quasars at the bright end of the luminosity function have peculiar properties compared to the bulk of the population. We built a mean intrinsic SED after correcting for the dust extinction, absorption and emission lines and intergalactic medium absorption. We also derived bolometric, IR band and monochromatic luminosities together with bolometric corrections at lambda = 5100 A and 3 micron. We define a new relation for the 3 micron bolometric correction. We find that the mean SED of hyper-luminous WISSH QSOs is different from that of less luminous sources, i.e. a relatively lower X-ray emission and a near and mid IR excess which can be explained assuming a larger dust contribution. WISSH QSOs have stronger emission from both warm and very hot dust, the latter being responsible for shifting the typical dip of the AGN SED from 1.3 to 1.1 micron. We also derived the mean SEDs of two sub-samples created according to the presence of Broad Absorption Lines and equivalent width of CIV line. We confirm that BALs are X-ray weak and that they have a reddened UV-optical continuum. We also find that BALs tend to have stronger emission from the hot dust component. This analysis suggests that hyper-luminous QSOs have a peculiar SED compared to less luminous objects. It is therefore critical to use SED templates constructed exclusively from very bright quasars samples when dealing with particularly luminous sources.
