arXiv 2402.186432024-02-28astro-ph.GA

来自一个暗弱再电离时期星系的 [Ne V] 发射：窄线中等质量黑洞的证据

[Ne v] emission from a faint epoch of reionization-era galaxy: evidence for a narrow-line intermediate mass black hole

J. Chisholm, D. A. Berg, R. Endsley, S. Gazagnes, C. T. Richardson, E. Lambrides, J. Greene, S. Finkelstein, S. Flury, N. G. Guseva, A. Henry, T. A. Hutchison, … 展开作者

J. Chisholm, D. A. Berg, R. Endsley, S. Gazagnes, C. T. Richardson, E. Lambrides, J. Greene, S. Finkelstein, S. Flury, N. G. Guseva, A. Henry, T. A. Hutchison, Y. I. Izotov, R. Marques-Chaves, P. Oesch, C. Papovich, A. Saldana-Lopez, D. Schaerer, M. G. Stephenson

备注：: 18 pages, submitted to MNRAS. Comments encouraged

阅读 PDF

arXiv 页面 ↗HTML 原文 ↗

AI总结：

研究利用 JWST NIRSpec 高分辨率光谱，在 z=5.59 的暗弱星暴星系 GN42437 中发现7σ [Ne V] 发射，并据线比值推断存在窄线中等质量黑洞。

摘要：

我们在此展示对 GN42437 的 JWST NIRSpec 高光谱分辨率观测；GN42437 是一个位于 z=5.59 的低质量（log(M_*/M_⊙)=7.9）、致密（r_e<500 pc）极端星暴星系，共探测到13条发射线。GN42437 具有低金属丰度（5–10% Z_⊙），其静止系 Hα 等值宽度表明，几乎所有观测到的恒星质量都是在最近3 Myr内形成的。GN42437 具有异常显著的7σ [Ne V] 3427 Å 探测。该 [Ne V] 线的静止系等值宽度为11±2 Å，[Ne V]/Hα=0.04±0.007，[Ne V]/[Ne III] 3870 Å=0.26±0.04，且 [Ne V]/He II 4687 Å=1.2±0.5。大质量恒星、激波或大质量X射线双星产生的电离无法同时再现这些 [Ne V] 与低电离线比值。要重现完整的星云结构，既需要大质量恒星，也需要黑洞吸积。我们没有探测到宽线，传统诊断也没有表明 GN42437 拥有吸积黑洞。因此，甚高电离发射线可有力诊断高红移处暗弱的窄线黑洞。我们通过多种方法估算黑洞质量约为 log(M_BH/M_⊙)～5–7。该黑洞质量与黑洞质量和观测速度弥散之间的局地关系相符，但显著高于由恒星质量预测的质量。甚高电离发射线或许能揭示用于研究宇宙中首批黑洞形成与增长的样本。

英文摘要：

Here we present high spectral resolution $\textit{JWST}$ NIRSpec observations of GN42437, a low-mass (log(M$_\ast/M_\odot)=7.9$), compact ($r_e < 500$pc), extreme starburst galaxy at $z=5.59$ with 13 emission line detections. GN42437 has a low-metallicity (5-10% Z$_\odot$) and its rest-frame H$α$ equivalent width suggests nearly all of the observed stellar mass formed within the last 3 Myr. GN42437 has an extraordinary 7$σ$ significant [Ne V] 3427 $\mathring{\rm A}$ detection. The [Ne V] line has a rest-frame equivalent width of $11\pm2\mathring{\rm A}$, [Ne V]/H$α=0.04\pm0.007$, [Ne V]/[Ne III] 3870$\mathring{\rm A} = 0.26\pm0.04$, and [Ne V]/He II 4687 $\mathring{\rm A} = 1.2\pm0.5$. Ionization from massive stars, shocks, or high-mass X-ray binaries cannot simultaneously produce these [Ne V] and low-ionization line ratios. Reproducing the complete nebular structure requires both massive stars and accretion onto a black hole. We do not detect broad lines nor do the traditional diagnostics indicate that GN42437 has an accreting black hole. Thus, the very-high-ionization emission lines powerfully diagnose faint narrow-line black holes at high-redshift. We approximate the black hole mass in a variety of ways as log(M$_{\rm BH}/M_\odot) \sim 5-7$. This black hole mass is consistent with local relations between the black hole mass and the observed velocity dispersion, but significantly more massive than the stellar mass would predict. Very-high-ionization emission lines may reveal samples to probe the formation and growth of the first black holes in the universe.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

AI总结：

摘要：

英文摘要：

相关论文