论文标题
最大的星系中的超大黑孔：$ M _ {\ rm bh} -c $ vers $ m _ {\ rm bh} -r _ {\ rm b} $
Ultramassive black holes in the most massive galaxies: $M_{\rm BH}-σ$ versus $M_{\rm BH}-R_{\rm b}$
论文作者
论文摘要
[删节]我们研究了黑洞（BH）质量（$ M _ {\ rm BH} $）与中央速度分散剂（$σ$）之间的关系的性质，对于Core-Sérsic星系，贫困的Core（$ r _ {\ rm bm b} $）的大小。我们的144个星系的样本具有动态确定的$ M _ {\ rm BH} $包含24个Core-sérsic星系，被认为是气体贫困合并的产物，并根据高分辨率HST成像可靠地识别。对于Core-Sérsic星系 - 即结合普通核（$ r _ {\ rm b} <0.5 $ kpc）和大核星系（$ r _ {\ rm b} \ rm b} \ gtrsim 0.5 $ kpc） $ m _ {\ rm bh} \ propto r _ {\ rm b}^{1.20 \ pm 0.14} $（RMS散布在log $ $ m _ {\ rm bh} $ $Δ_ {\ rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rm rms} \ sim 0.29 $ dex）中，同一范围相同。将样品分为Sérsic，正常和大核星系，我们发现Sérsic和正常核心星系共同定义了单个log-linear $ m _ {\ rm bh} -d $关系$ m _ {\ rm bh} \ rm bh}但是，在高质量端大核星系（四个带有$ m _ {\ rm bh} $）的sim 0.47 $ dex被从这种关系中偏移（$ 2.5-4）\ timesσ_{\ rm s} $，从而将其从这种关系中偏移，并解释了先前报道的$ m _ _ _ {\ rm rm rm mm bh的速度。大核球体具有幅度$ m_ {v} \ le -23.50 $ mag，半光radii re $> $> $ 10 kpc，并且极为巨大的$ m _ {*} \ ge 10^{12} {12} m _ {\ odot} $。此外，这些球体倾向于托管超大BHS（$ m _ {\ rm bh} \ ge 10^{10} m _ {\ odot} $）与他们的$ r _ {\ rm b} $紧密连接。不太流行的$ m _ {\ rm bh} -r _ {\ rm b} $关系与$ m _ {\ rm bh} $ sim $ \ sim $ \ sim $ 62％的散布少62％少于$ 62％的散布。
[Abridged] We investigate the nature of the relations between black hole (BH) mass ($M_{\rm BH}$) and the central velocity dispersion ($σ$) and, for core-Sérsic galaxies, the size of the depleted core ($R_{\rm b}$). Our sample of 144 galaxies with dynamically determined $M_{\rm BH}$ encompasses 24 core-Sérsic galaxies, thought to be products of gas-poor mergers, and reliably identified based on high-resolution HST imaging. For core-Sérsic galaxies -- i.e., combining normal-core ($R_{\rm b} < 0.5 $ kpc) and large-core galaxies ($R_{\rm b} \gtrsim 0.5$ kpc), we find that $M_{\rm BH}$ correlates remarkably well with $R_{\rm b}$ such that $M_{\rm BH} \propto R_{\rm b}^{1.20 \pm 0.14}$ (rms scatter in log $M_{\rm BH}$ of $Δ_{\rm rms} \sim 0.29$ dex), confirming previous works on the same galaxies except three new ones. Separating the sample into Sérsic, normal-core and large-core galaxies, we find that Sérsic and normal-core galaxies jointly define a single log-linear $M_{\rm BH}-σ$ relation $M_{\rm BH} \propto σ^{ 4.88 \pm 0.29}$ with $Δ_{\rm rms} \sim 0.47$ dex, however, at the high-mass end large-core galaxies (four with measured $M_{\rm BH}$) are offset upward from this relation by ($2.5-4) \times σ_{\rm s}$, explaining the previously reported steepening of the $M_{\rm BH}-σ$ relation for massive galaxies. Large-core spheroids have magnitudes $M_{V} \le -23.50$ mag, half-light radii Re $>$ 10 kpc and are extremely massive $M_{*} \ge 10^{12}M_{\odot}$. Furthermore, these spheroids tend to host ultramassive BHs ($M_{\rm BH} \ge 10^{10}M_{\odot}$) tightly connected with their $R_{\rm b}$ rather than $σ$. The less popular $M_{\rm BH}-R_{\rm b}$ relation exhibits $\sim$ 62% less scatter in log $M_{\rm BH}$ than the $M_{\rm BH}- σ$ relations.
