Henize 2-10核的扩展结构和命运
Extended Structure and Fate of the Nucleus in Henize 2-10
摘要：
我们研究了Henize 2 -10星系的黑洞结构和核区域。使用Magellan/Megacam $g$ -和$r$ -波段图像分析表面亮度（SB）分布。排除中心星爆，我们找到了一个最佳拟合的两个组成部分Sérsic配置文件与$n_{\rm in} \sim 0.6$，$r_{\text{eff,in}} \sim$ 260~pc，和$n_{\rm out}\sim 1.8$，$r_{\text{eff, out}}\sim$ 1 kpc。积分到我们最外面的数据点（100弧秒$\sim$ 4.3 kpc），我们计算$M_g=-19.2$和$M_r=-19.8$。相应的封闭恒星质量是$M_{\star}\sim(10\pm3)\times10^9$ M $_\odot$，$\sim3\times$比以前的估计大。除了中央的$\lesssim$ 500 pc，蓝色和不规则的形态，该星系似乎是一个早期类型的系统。外部颜色相当红，$(g-r)_0=0.75$，表明一个占主导地位的老年人口。我们使用档案双子座/NIFS $K$波段自适应光学光谱学和{ \it哈勃太空望远镜}成像来研究星系的核区域。我们把一个上限的BH质量的$\sim10^7M_{\odot}$从NIFS数据，从$M_{\rm BH}$ -无线电X射线基本平面一致。没有看到日冕线，但Br $γ$源位于BH的位置，亮度与X射线发射一致。Henize 2-10中心的星暴导致了几个超级星团的形成，它们位于BH的$\sim$ 100 pc范围内。我们研究的命运的核估计的动态质量和动态摩擦的时间尺度的集群。最大质量的星团（$\sim 10^6 M_\odot$）有$τ_{\rm dyn} \lesssim 200$ Myr，因此Henize 2-10可能代表了一个罕见的围绕着一个已经存在的大质量BH的核星团形成的快照。
英文摘要：
We investigate the structure and nuclear region of the black hole (BH) hosting galaxy Henize2-10. Surface brightness (SB) profiles are analyzed using Magellan/Megacam $g$- and $r$-band images. Excluding the central starburst, we find a best-fit two component Sérsic profile with $n_{\rm in} \sim 0.6$, $r_{\text{eff,in}} \sim$ 260~pc, and $n_{\rm out}\sim 1.8$, $r_{\text{eff, out}}\sim$ 1 kpc. Integrating out to our outer most data point (100 arc sec $\sim$ 4.3 kpc), we calculate $M_g=-19.2$ and $M_r=-19.8$. The corresponding enclosed stellar mass is $M_{\star}\sim(10\pm3)\times10^9$ M$_\odot$, $\sim3\times$ larger than previous estimates. Apart from the central $\lesssim$500 pc, with blue colors and an irregular morphology, the galaxy appears to be an early-type system. The outer color is quite red, $(g-r)_0=0.75$, suggesting a dominant old population. We study the nuclear region of the galaxy using archival Gemini/NIFS $K$-band adaptive optics spectroscopy and {\it Hubble Space Telescope} imaging. We place an upper limit on the BH mass of $\sim10^7M_{\odot}$ from the NIFS data, consistent with that from the $M_{\rm BH}$-radio-X-ray fundamental plane. No coronal lines are seen, but a Br$γ$ source is located at the position of the BH with a luminosity consistent with the X-ray emission. The starburst at the center of Henize 2-10 has led to the formation of several super star clusters, which are within $\sim$100 pc of the BH. We examine the fate of the nucleus by estimating the dynamical masses and dynamical friction timescales of the clusters. The most massive clusters ($\sim 10^6 M_\odot$) have $τ_{\rm dyn} \lesssim 200$ Myr, and thus Henize 2-10 may represent a rare snapshot of nuclear star cluster formation around a pre-existing massive BH.
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