2,435个DESI盘状星系中的星系-超大质量黑洞协同演化及无核球盘星系中的无并合黑洞增长
Galaxy-SMBH co-evolution in 2,435 DESI disk galaxies and merger-free BH growth in bulgeless disks
- University of Oxford（牛津大学）
- Lancaster University（兰卡斯特大学）
- University of Edinburgh（爱丁堡大学）
- Masaryk University（马萨里克大学）
- University of Toronto（多伦多大学）
- University of Louisville（路易斯维尔大学）
- Haverford College（哈弗福德学院）
- University of Utah（犹他大学）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
基于DESI数据中2,435个盘状星系样本，发现无核球星系遵循与一般盘星系相同的黑洞-恒星质量关系，表明长期演化过程而非并合主导了星系-黑洞协同演化。
AI中文摘要：
我们分析了盘主导星系的黑洞标度关系，并提出了由长期演化驱动的星系-黑洞协同演化的证据。我们通过观测无核球星系来实现这一目标，这类星系缺乏恒星核球，暗示其并合历史较为平静。我们首先从DESI数据中构建了一个包含2,435个盘主导星系且拥有光学宽线活动星系核（AGN）的样本，并发现$M_{\mathrm{BH}}$--$M_{*}$标度关系为$\log(M_{\mathrm{BH}})= - 3.7^{+0.3}_{-0.3} + 1.00^{+0.03}_{-0.03} \log(M_*)$。从中，我们识别出546个拥有AGN的无核球星系，其数量是先前样本的$\gtrsim 5$倍，并发现它们遵循与一般盘星系样本相同的$M_{\mathrm{BH}}$--$M_{*}$关系。将无核球星系与具有部分核球成分的星系进行比较，我们发现两者在$M_{\mathrm{BH}}$--$M_{*}$关系上吻合良好（在$3 \sigma$以内），但在$M_{\mathrm{BH}}$--$M_{*, \mathrm{bulge}}$关系上存在分歧（在$>7 \sigma$水平）。这与并合驱动的协同演化预期相反，表明长期演化过程在建立观测到的$M_{\mathrm{BH}}$--$M_{*}$标度关系中具有重要意义。此外，在早型星系的对照样本中，我们发现了AGN光度相对于无核球样本增加的初步证据，但在黑洞质量上没有统计差异。这表明早型星系假定的并合主导演化历史并未导致显著增强的长期黑洞增长。这些结果支持了众多近期观测和理论研究，表明长期演化过程为超大质量黑洞增长和星系-黑洞协同演化提供了重要燃料。
英文摘要：
We analyse black hole scaling relations for disk-dominated galaxies, and present evidence for secularly driven galaxy-black hole co-evolution. We do this observationally by looking at ``bulgeless'' galaxies, where the lack of a stellar bulge suggests a quiet merger history. We first compose a sample of 2,435 disk-dominated galaxies hosting optical broad line active galactic nuclei (AGN) from DESI data, and find a $M_{\mathrm{BH}}$--$M_{*}$ scaling relation of $\log(M_{\mathrm{BH}})= - 3.7^{+0.3}_{-0.3} + 1.00^{+0.03}_{-0.03} \log(M_*)$. From these, we identify 546 bulgeless galaxies hosting AGN, a factor of $\gtrsim 5$ larger than pre-existing samples, and find they follow the same $M_{\mathrm{BH}}$--$M_{*}$ relation as the general disk galaxy sample. Comparing the bulgeless galaxies to those with some bulge component, we find good agreement in the $M_{\mathrm{BH}}$--$M_{*}$ relation (within $3 σ$), but disagreement in the $M_{\mathrm{BH}}$--$M_{*, \mathrm{bulge}}$ relation (at $>7 σ$). This is the opposite of what is expected from merger-driven co-evolution, suggesting secular growth is significant in establishing observed $M_{\mathrm{BH}}$--$M_{*}$ scaling relations. Furthermore, in a control sample of early-type galaxies we find tentative evidence of increased AGN luminosity compared to the bulgeless sample, but no statistical difference in black hole mass. This suggests the assumed merger-dominated evolutionary history of early-type galaxies does not lead to significantly increased long-term BH growth. These results support numerous recent observational and theoretical studies which suggest secular processes fuel significant supermassive black hole growth and galaxy-black hole co-evolution.
