VIRIAL BLACK HOLE MASS ESTIMATES FOR 280,000 AGNs FROM THE SDSS BROADBAND PHOTOMETRY AND SINGLE-EPOCH SPECTRA
VIRIAL BLACK HOLE MASS ESTIMATES FOR 280,000 AGNs FROM THE SDSS BROADBAND PHOTOMETRY AND SINGLE-EPOCH SPECTRA
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DOI：
10.3847/1538-4365/228/1/9
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发表时间：
2016-09
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通讯作者：
S. Kozłowski
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作者：
S. Kozłowski
我们使用包含近 300,000 个活动星系核 (AGN) 的斯隆数字巡天 (SDSS) 类星体数据第 12 版 (DR12Q) 来计算从宽带消光校正的 SDSS 星等得出的 5100、3000 和 1350 Å 处的单色光度。将这些源与 SDSS Quasar Data Release 7 (DR7Q) 中的对应源进行匹配后，我们发现我们的光度和基于 DR7Q 光谱的光度之间具有非常高的相关性，在 2.5 dex 的光度范围内，平均偏移量 (∼0.01 dex) 和差异色散分别为 0.11、0.10 和 0.12 dex。然后，我们使用宽线区域半径-圆盘光度关系以及 Mg ii 和 C iv 发射线的 FWHM 来估计 AGN 的黑洞 (BH) 质量，以提供 283,033 个维里 BH 质量估计值的目录（Mg ii 为 132,451，C iv 为 213,071，两者均为 62,489）以及辐射热测量值的估计值0.1 < z < 5.5 以及大约四分之一的天空被 SDSS 覆盖的情况下的光度和爱丁顿比。 Mg ii 的 BH 质量估计值与 DR7Q 的 BH 质量估计值非常匹配，在约 2 dex 的 BH 质量范围内差异分散为 0.34 dex。我们发现与 DR7Q 相比，从 DR12Q 导出的 C iv FWHM 存在偏差，我们根据经验进行了纠正。应谨慎使用 C iv BH 质量估计，因为已知 C iv 线会导致从单历元光谱估计 BH 质量时出现问题。最后，在 FWHM 校正后，C iv 的 AGN BH 质量估计值与 DR7Q 的估计值非常匹配（离散度为 0.28 dex），更重要的是，Mg ii 和 C iv BH 质量在内部一致，平均偏移量为 0.07 dex，离散度为 0.39 dex。
We use the Sloan Digital Sky Survey (SDSS) Quasar Data Release 12 (DR12Q), containing nearly 300,000 active galactic nuclei (AGNs), to calculate the monochromatic luminosities at 5100, 3000, and 1350 Å, derived from the broadband extinction-corrected SDSS magnitudes. After matching these sources to their counterparts from the SDSS Quasar Data Release 7 (DR7Q), we find very high correlations between our luminosities and DR7Q spectra-based luminosities with minute mean offsets (∼0.01 dex) and dispersions of differences of 0.11, 0.10, and 0.12 dex, respectively, across a luminosity range of 2.5 dex. We then estimate the black hole (BH) masses of the AGNs using the broad line region radius–disk luminosity relations and the FWHM of the Mg ii and C iv emission lines, to provide a catalog of 283,033 virial BH mass estimates (132,451 for Mg ii, 213,071 for C iv, and 62,489 for both) along with the estimates of the bolometric luminosity and Eddington ratio for 0.1 < z < 5.5 and for roughly a quarter of the sky covered by SDSS. The BH mass estimates from Mg ii turned out to be closely matched to the ones from DR7Q with a dispersion of differences of 0.34 dex across a BH mass range of ∼2 dex. We uncovered a bias in the derived C iv FWHMs from DR12Q as compared to DR7Q, which we correct empirically. The C iv BH mass estimates should be used with caution because the C iv line is known to cause problems in the estimation of BH mass from single-epoch spectra. Finally, after the FWHM correction, the AGN BH mass estimates from C iv closely match the DR7Q ones (with a dispersion of 0.28 dex), and more importantly the Mg ii and C iv BH masses agree internally with a mean offset of 0.07 dex and a dispersion of 0.39 dex.