宇宙二重奏II：宇宙正午时期Gaia多峰双活动星系核的增长与吸积
Cosmic Duets II. Growth and accretion in Gaia Multi-Peak dual AGN at Cosmic Noon
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中文总结 AI 辅助
该研究对30个Gaia多峰选定的宇宙正午双活动星系核样本，结合光谱观测分析其黑洞与吸积性质，对比L-GalaxiesBH和Astrid模型发现次黑洞增长效率高于模型预测。
中文摘要 AI 辅助
我们首次对宇宙二重奏（Cosmic Duets）的物理性质进行统计表征：这类双活动星系核（dual AGN）处于红移范围0.5 ≤ z ≤ 3.0，投影间距为1-7千秒差距，对应两个AGN均应位于同一并合残余中的系统。我们分析了目前最大的同质样本，包含30个通过Gaia多峰（Gaia Multi-Peak）技术经光谱确认的宇宙二重奏。对所有目标使用静止帧紫外至光学积分场光谱，主要借助甚大望远镜多单元光谱探测器（VLT/MUSE）、甚大望远镜高分辨率红外光谱仪（VLT/ERIS）和凯克天文台光学近红外成像光谱仪（Keck/OSIRIS），我们空间分辨出两个AGN成分并提取每个系统的独立光谱。我们通过光谱拟合分解连续谱、发射线和Fe II复合体，推导得出黑洞质量log(M_BH/M_☉)约为7.4-10.1，热光度log(L_bol/erg s⁻¹)约为44.8-47.2，与相似红移下单个AGN的结果一致。我们首次将双AGN性质与半解析模型及流体动力学模拟（包括L-GalaxiesBH和Astrid）进行比较：Astrid与观测到的黑洞质量比分布匹配度更高，但其选定系统主要处于更低红移，导致在固定G波段星等下热光度更低；L-GalaxiesBH完美再现观测参数空间，但预测的对更具异质性，主黑洞热光度更高、次超大质量黑洞（SMBH）质量更低、爱丁顿比率更高，因采用的吸积方案导致近爱丁顿吸积的AGN数量过多。我们的结果表明，在GMP（Gaia Multi-Peak）选定的系统中，次SMBH的增长比当前模型预测更高效，使得两个成分间的黑洞质量和吸积功率更具可比性。
英文摘要
We present the first statistical characterization of the physical properties of Cosmic Duets: dual AGN in the redshift range 0.5 $\leq$ z $\leq$ 3.0 with projected separations of 1-7 kpc, corresponding to systems in which both AGN are expected to reside within the same merger remnant. We analyze the largest homogeneous sample currently available, consisting of 30 spectroscopically confirmed Cosmic Duets selected via the Gaia Multi-Peak technique. Using rest-frame UV-to-optical integral-field spectroscopy for all targets, primarily with VLT/MUSE, VLT/ERIS, and Keck/OSIRIS, we spatially resolve the two AGN components and extract separate spectra for each system. We decompose the continuum, emission lines, and Fe II complexes through spectral fitting. We derive black hole masses of log($M_{BH}/M_{sun}$) ~ 7.4-10.1 and bolometric luminosities of log($L_{bol}/erg s^{-1}$) ~ 44.8-47.2, consistent with those of single AGN at similar redshifts. We finally carry out the first comparison of dual AGN properties with semi-analytical models and hydrodynamical simulations, including L-GalaxiesBH and Astrid. Astrid provides a closer match to the observed black-hole mass-ratio distribution, but its selected systems are predominantly at lower redshifts, resulting in lower bolometric luminosities at fixed G-band magnitude. L-GalaxiesBH perfectly reproduce the observed parameter space, but it predicts more heterogeneous pairs, with higher primary-bolometric luminosity, lower-mass secondary SMBHs, and higher Eddington ratios, resulting in an excess of near-Eddington accreting AGN due to its adopted accretion prescription. Our results suggest that, in GMP-selected systems, secondary SMBH growth is more efficient than predicted by current models, leading to more comparable black-hole masses and accretion power between the two components.
发表机构
- University of Trento（特伦托大学）
- INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）
- Institute of Space Sciences (ICE, CSIC)（空间科学研究所（西班牙高等科研理事会））
- INAF – Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
- Institut d’Astrophysique de Paris（巴黎天体物理研究所）
- INAF - Istituto di Astrofisica e Planetologia Spaziali（意大利国家天体物理研究所天文与行星物理学研究所）
- Max Planck Institute for extraterrestrial Physics（马克斯·普朗克地外物理研究所）
- Centro de Astrobiología (CAB), CSIC–INTA（天体生物学中心（西班牙高等科研理事会-国家航空航天技术研究所））
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