论文标题
超大的黑洞具有微弱的宽窄发射线
Hyper-massive Black Holes have Faint Broad and Narrow Emission Lines
论文作者
论文摘要
EUV提供了大部分电离，从而产生高等效宽度（EW）宽和狭窄的排放线（BELS，NELS）。超大型Schwarzschild黑洞的光谱（HMBHS，$ M_ {BH} \ GEQ 10^{10} M _ {\ odot} $）具有$α$ -DISCS，在EUV中迅速下降，表明EUV较低。质量$ 10^{6} -10^{12} m _ {\ odot} $的模型光谱$ 10^{6} -10^{\ odot} $ $ 0.03 \ leq l_ {bol}/l_ {bol}/l_ {edd} \ leq leq 1.0 $是对云的照相代码输入的。 bels从$ m_ {bh} \ sim 10^8 m _ {\ odot} $ to $ m_ {\ m_ {bh} \ sim 10^{10} m _ {\ odot} $弱从$ m_ {bh} \ sim 10^8 m _ {\ odot} $弱于$ \ sim $ 100倍。高电离bels（O VI 1034 $ \ Overset {\ Circ} {\ Mathrm {a}} $，C IV 1549 $ \ overset {\ circ} {\ mathrm {a}} $ （$ m_ {bh} \ geq 10^6 m _ {\ odot} $，重现baldwin效果，但以$ m_ {bh} \ geq 10^{10} {10} m _ {\ odot} $重新恢复EW。低电离线（MGII 2798 $ \ OUTSET {\ CRIC} {\ MATHRM {a}} $，H $β$ 4861 $ \ overset {\ circ} {\ Mathrm {a a}}} $ 虚弱的。最大旋转HMBH的线的行为也类似。 BELS的线比图表明，较高的OVI/H $β$和Low CIV/H $α$可能会挑选HMBH，尽管OVI通常很难观察到。在NEL BPT图中，HMBHS位于星形区域之间，除了高度旋转，高积聚率HMBHS。总之，使用当前的光学设施很难检测到HMBHS的BEL。从100到$ 10^{12} m _ {\ odot} $，用于检测AGN的发射线仅在$ 10^6-6-10^9 m _ {\ odot} $ window中，在其中找到了大多数AGN。这种选择效果可能会使报告的$ M_ {BH} $的分布变形。
The EUV provides most of the ionization that creates the high equivalent width (EW) broad and narrow emission lines (BELs, NELs) of quasars. Spectra of Hypermassive Schwarzschild black holes (HMBHs, $M_{BH} \geq 10^{10} M_{\odot}$) with $α$-discs, decline rapidly in the EUV suggesting much lower EWs. Model spectra for black holes of mass $10^{6}-10^{12} M_{\odot}$ and accretion rates $0.03 \leq L_{bol}/L_{edd} \leq 1.0$ were input to the CLOUDY photoionization code. BELs become $\sim$100 times weaker in EW from $M_{BH} \sim 10^8 M_{\odot}$ to $M_{BH} \sim 10^{10} M_{\odot}$. The high ionization BELs (O VI 1034 $\overset{\circ}{\mathrm {A}}$, C IV 1549 $\overset{\circ}{\mathrm {A}}$, He II 1640 $\overset{\circ}{\mathrm {A}}$) decline in EW from ($M_{BH} \geq 10^6 M_{\odot}$, reproducing the Baldwin effect, but regain EW for $M_{BH} \geq 10^{10} M_{\odot}$). The low ionization lines (MgII 2798 $\overset{\circ}{\mathrm {A}}$, H$β$ 4861 $\overset{\circ}{\mathrm {A}}$ and H$α$ 6563 $\overset{\circ}{\mathrm {A}}$) remain weak. Lines for maximally spinning HMBHs behave similarly. Line ratio diagrams for the BELs show that high OVI/H$β$ and low CIV/H$α$ may pick out HMBH, although OVI is often hard to observe. In NEL BPT diagrams HMBHs lie among star-forming regions, except for highly spinning, high accretion rate HMBHs. In summary, the BELs expected from HMBHs would be hard to detect using the current optical facilities. From 100 to $10^{12} M_{\odot}$, the emission lines used to detect AGN only have high EW in the $10^6 - 10^9 M_{\odot}$ window, where most AGN are found. This selection effect may be distorting reported distributions of $M_{BH}$.
