论文标题
使用低到高光度的活性银核校准基于MG II的黑洞质量估计器
Calibrating Mg II-based black-hole mass estimators using Low-to-High-Luminosity Active Galactic Nuclei
论文作者
论文摘要
我们提出基于其余框架紫外线（UV）\ MGII \2798Å和光学\ Hb \4861Å发射线的单期黑孔质量（\ MBH）估计器。为了扩大活性银河核（AGN）的光度范围，我们将31个回响映射的AGN与Bahk等人的亮度相对较低。 2019年，Woo等人的47个中度亮度AGN。 2018年，来自斯隆数字天空调查（SDSS）的425个高光度AGN。组合样品的单色光度为5100Å$ \ mathrm {\logλl_{5100} \ sim 41.3-46.5} $ \ ergs，超过5.5 $ <$ <$ <$ <$ \ $ \ $ \ log $ \ $ \ mbh \ $ \ $ <$ <$ <$ 9.5。基于\ hb \ \ hb \的全宽度最大（FWHM）的基准质量，与5100Å处的连续亮度配对，我们使用\ mgii \ line校准了黑洞质量估计器中最佳拟合参数。我们发现，\ mgii \和\ hb \之间的线轮廓上的差异对校准UV \ MBH \估计量具有重大影响。通过探索UV和光学\ MBH \估计器之间的系统差异，我们建议添加校正项$Δ$ m = -1.14 $ \ rm \ log（fwhm_ {mgii}/nm_ {mgii}/σ_{mgii} $ 0.33 + 0.33 In uv MasseTor exator exoration exoration。我们还发现$ \ sim $ 0.1 DEX偏置在\ MBH \估计中，由于光谱斜率在2800-5200Å范围内的差异。取决于基于线色散或FWHM的\ MBH \估计量以及连续性或线发光度，衍生的UV质量估计器相对于基于基于\ Hb \ MBH的基准\ Hb \ MBH显示> 〜0.1 DEX固有散射。
We present single-epoch black-hole mass (\mbh) estimators based on the rest-frame ultraviolet (UV) \MgII\ 2798Å and optical \Hb\ 4861Å emission lines. To enlarge the luminosity range of active galactic nuclei (AGNs), we combine the 31 reverberation-mapped AGNs with relatively low luminosities from Bahk et al. 2019, 47 moderate-luminosity AGNs from Woo et al. 2018, and 425 high-luminosity AGNs from the Sloan Digital Sky Survey (SDSS). The combined sample has the monochromatic luminosity at 5100Å ranging $\mathrm{\log λL_{5100} \sim 41.3-46.5}$ \ergs, over the range of 5.5 $<$ $\log$\mbh\ $<$ 9.5. Based on the fiducial mass from the line dispersion or full width half maximum (FWHM) of \Hb\ paired with continuum luminosity at 5100Å, we calibrate the best-fit parameters in the black hole mass estimators using the \MgII\ line. We find that the differences in the line profiles between \MgII\ and \Hb\ have significant effects on calibrating the UV \mbh\ estimators. By exploring the systematic discrepancy between the UV and optical \mbh\ estimators as a function of AGN properties, we suggest to add correction term $Δ$M = -1.14 $\rm \log(FWHM_{MgII}/σ_{MgII}$) + 0.33 in the UV mass estimator equation. We also find a $\sim$0.1 dex bias in the \mbh\ estimation due to the difference of the spectral slope in the 2800-5200 Å range. Depending on the selection of \mbh\ estimator based on either line dispersion or FWHM and either continuum or line luminosity, the derived UV mass estimators show >~0.1 dex intrinsic scatter with respect to the fiducial \Hb\ based \mbh.
