论文标题
螺旋星系中的球状簇系统与超质量黑洞之间的关系III。 $ m_ \ bullet-m_ \ ast $相关的链接
The relation between globular cluster systems and supermassive black holes in spiral galaxies III. The link to the $M_\bullet-M_\ast$ correlation
论文作者
论文摘要
我们继续探索球形群集总数，$ n _ {\ rm gc} $与中央黑洞质量（$ m_ \ bullet $）之间的关系。我们在这里介绍了SAB Galaxies NGC 3368，NGC 4736（M 94）和NGC 4826（M 64）和SM Galaxy NGC 4395的结果。球形集群（GC）候选候选者的选择是基于（$ u^*$ u^*$ i^$ i^\ pirm $ i^$ i^\ k_ $ i^\ k_ $ i^\ k_ $ i^\ k_ $ i^\ k_ $ i^\ k_ $ i^\ prime $ -band形状参数。我们确定$ m_ \ bullet $ vess $ n _ {\ rm gc} $相关性，以及NGC 4258，NGC 253，M 104，M 104，M 81，M 31，以及银河系。我们还重新确定了Harris，Poole和Harris（2014）中椭圆样样品的相关性，并从Sahu等人那里进行了更新的星系类型。 2019b。此外，我们从与$ n _ {\ rm gc} $（Hudson，Harris，＆Harris 2014）和Fit $ m_ \ bulterus $ vers $ versus $ m_ \ ast $ for spiper and for spiper and for spiper和enlipticals $ n _ {\ rm gc} $中得出了总恒星星系质量，$ m_ \ ast $。 We obtain log $M_\bullet \propto$ (1.01 $\pm$ 0.13) log $N_{\rm GC}$ for ellipticals, and log $M_\bullet \propto$ (1.64 $\pm$ 0.24) log $N_{\rm GC}$ for late type galaxies (LTG).线性$ m_ \ bullet $ vess $ n _ {\ rm gc} $相关性可能是由于通过合并通过统计收敛而引起的，而不是LTG的陡峭相关性。但是，在$ m_ \ bullet $与总恒星质量（$ m_ \ ast $）参数空间中，$ m_ \ ast $从与$ n _ {\ rm gc} $，$ m_ \ bulet \ bullet \ propto $（1.48 $ \ pm $ 0.18 $ $ m_ $ $ apirt $ asticy ast y yst AST $ stiration $ stiration $ stiration $ ast $ ast $ ast $ ast AST AST AST AST AST $ compers $ m。 （1.21 $ \ pm $ 0.16）log $ m_ \ ast $ for LTG。在此参数空间中，观察到的椭圆形和LTG之间的一致性可能暗示黑洞和星系通过“平静”增强，AGN反馈和其他世俗过程共同发展。
We continue to explore the relationship between globular cluster total number, $N_{\rm GC}$, and central black hole mass, $M_\bullet$, in spiral galaxies. We present here results for the Sab galaxies NGC 3368, NGC 4736 (M 94) and NGC 4826 (M 64), and the Sm galaxy NGC 4395. The globular cluster (GC) candidate selection is based on the ($u^*$ - $i^\prime$) versus ($i^\prime$ - $K_s$) color-color diagram, and $i^\prime$-band shape parameters. We determine the $M_\bullet$ versus $N_{\rm GC}$ correlation for these spirals, plus NGC 4258, NGC 253, M 104, M 81, M 31, and the Milky Way. We also redetermine the correlation for the elliptical sample in Harris, Poole, & Harris (2014), with updated galaxy types from Sahu et al. 2019b. Additionally, we derive total stellar galaxy mass, $M_\ast$, from its two-slope correlation with $N_{\rm GC}$ (Hudson, Harris, & Harris 2014), and fit $M_\bullet$ versus $M_\ast$ for both spirals and ellipticals. We obtain log $M_\bullet \propto$ (1.01 $\pm$ 0.13) log $N_{\rm GC}$ for ellipticals, and log $M_\bullet \propto$ (1.64 $\pm$ 0.24) log $N_{\rm GC}$ for late type galaxies (LTG). The linear $M_\bullet$ versus $N_{\rm GC}$ correlation in ellipticals could be due to statistical convergence through mergers, but not the much steeper correlation for LTG. However, in the $M_\bullet$ versus total stellar mass ($M_\ast$) parameter space, with $M_\ast$ derived from its correlation with $N_{\rm GC}$, $M_\bullet \propto$ (1.48 $\pm$ 0.18) log $M_\ast$ for ellipticals, and $M_\bullet \propto$ (1.21 $\pm$ 0.16) log $M_\ast$ for LTG. The observed agreement between ellipticals and LTG in this parameter space may imply that black holes and galaxies co-evolve through "calm" accretion, AGN feedback, and other secular processes.
