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Gemini近红外光谱仪-遥远类星体巡天：校准高红移类星体中超大质量黑洞质量的基于紫外估计的规范

Gemini Near Infrared Spectrograph - Distant Quasar Survey: Prescriptions for Calibrating UV-Based Estimates of Supermassive Black Hole Masses in High-Redshift Quasars

Cooper Dix, Brandon Matthews, Ohad Shemmer, Michael S. Brotherton, Adam D. Myers, I. Andruchow, W. N. Brandt, Gabriel A. Ferrero, Richard Green, Paulina Lira, R… 展开作者

Cooper Dix, Brandon Matthews, Ohad Shemmer, Michael S. Brotherton, Adam D. Myers, I. Andruchow, W. N. Brandt, Gabriel A. Ferrero, Richard Green, Paulina Lira, Richard M. Plotkin, Gordon T. Richards, Donald P. Schneider

备注：
19 pages (AASTeX 6.3.1), 9 figures, accepted for publication in ApJ
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AI总结：

本研究通过引入C IV等值宽度改进进基于Mg II和C IV的黑洞质量估计，使其规范在利用双线时可使散布减少约15%，为高红移类星体的超大黑洞质量估计提供更精确的方法。

摘要：

类星体中最可靠的单历元超大质量黑洞质量（$M_{\rm BH}$）估计是通过使用低电离发射线的速度宽度获得的，通常是H$β$ $\lambda4861$线。遗憾的是，这条线在$z\approx1$时红移出光学波段，使得$M_{\rm BH}$$估计依赖于代理静止参考系紫外（UV））发射线，如C IV $\lambda1549$或Mg II $\lambda2800$，这些在测量时存在内在挑战，导致$M_{\rm BH}$估计不确定。在这项工作中，我们旨在基于从H$β$发射线得出的估计，校正从C IV和Mg II发射线得出的$M_{\rm BH}$估计。我们发现，在基于Mg II和C IV推导出$M_{\rm BH}$估计时采用C IV的等值宽度，能提供最接近从H$β$获得的值我们还提供了当仅可测量C IV、仅可测量Mg II、以及两者均可测量时估计$M_{\rm BH}$值的的规范。我们发现，在可用情况下利用两条发射线，与先前研究相比，将\rm BH}$估计的散布减少约$\sim15\\%$。最后，我们讨论了我们的规范在给定一个更大的类星体样本（$3.20 \lesssim z \lesssim 3.50$））时提供更准确和精确的$M_{\rm BH}$$估计的的潜力，在该样本中，Mg II和H$β$可在同一近红外光谱中测量。

英文摘要：

The most reliable single-epoch supermassive black hole mass ($M_{\rm BH}$) estimates in quasars are obtained by using the velocity widths of low-ionization emission lines, typically the H$β$ $\lambda4861$ line. Unfortunately, this line is redshifted out of the optical band at $z\approx1$, leaving $M_{\rm BH}$ estimates to rely on proxy rest-frame ultraviolet (UV) emission lines, such as C IV $\lambda1549$ or Mg II $\lambda2800$, which contain intrinsic challenges when measuring, resulting in uncertain $M_{\rm BH}$ estimates. In this work, we aim at correcting $M_{\rm BH}$ estimates derived from the C IV and Mg II emission lines based on estimates derived from the H$β$ emission line. We find that employing the equivalent width of C IV in deriving $M_{\rm BH}$ estimates based on Mg II and C IV provides values that are closest to those obtained from H$β$. We also provide prescriptions to estimate $M_{\rm BH}$ values when only C IV, only Mg II, and both C IV and Mg II are measurable. We find that utilizing both emission lines, where available, reduces the scatter of UV-based $M_{\rm BH}$ estimates by $\sim15\%$ when compared to previous studies. Lastly, we discuss the potential of our prescriptions to provide more accurate and precise estimates of $M_{\rm BH}$ given a much larger sample of quasars at $3.20 \lesssim z \lesssim 3.50$, where both Mg II and H$β$ can be measured in the same near-infrared spectrum.

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