Implications of the nanoHertz Gravitational-Wave Background for Galactic Feedback and Massive Black Hole Growth
Rutgers University（罗格斯大学）；Flatiron Institute（平顿研究所）；Yale University（耶鲁大学）；University of Connecticut（康涅狄格大学）；Center for Astrophysics — Harvard & Smithsonian（哈佛-史密森尼天体物理中心）；Durham University（杜伦大学）；HUN-REN CSFK Konkoly Observatory（匈牙利研究与教育网络科学研究中心孔科利天文台）；Ecole Polytechnique（巴黎综合理工学院）；Institut Polytechnique de Paris（巴黎理工学院）
Megan Taylor Tillman, Blakesley Burkhart, Chiara M. F. Mingarelli, J. Andrew Casey-Clyde, Lars Hernquist, Sownak Bose, Enikő Regős, César Hernández-Aguayo
We investigate how pulsar timing array (PTA) measurements of the nanoHertz gravitational-wave background (GWB) can constrain models for the growth history of supermassive black holes (SMBHs) and how active galactic nucleus (AGN) and stellar feedback models can affect GWB predictions. Feedback regulates supermassive black hole (SMBH) growth, altering the black hole mass function (BHMF). Using BHMFs drawn from multiple cosmological simulation suites including IllustrisTNG, MillenniumTNG, Simba, and CAMELS, and combining these with a quasar-based SMBH binary population framework, we predict the resulting GWB amplitude under a range of different stellar and AGN feedback prescriptions. We find that the choice of both stellar and AGN feedback models alters the high-mass end of the BHMF and changes the predicted GWB amplitude by up to a factor of 2 for the fiducial simulations and a factor 10 for extreme feedback variations in CAMELS. Models with inefficient or absent AGN feedback produce abundant SMBHs and yield GWB amplitudes consistent with PTA data, yet fail in producing realistic galaxies. Fiducial models of AGN and stellar feedback suppress SMBH growth too much and under-predict the expected signal, an effect which could possibly be mitigated by more realistic black hole seeding and growth prescriptions. The mismatch between the GWB amplitudes predicted by cosmological simulations and that inferred by PTA measurements suggests that SMBH growth is more efficient or occurs earlier than captured by current models. This demonstrates that PTA measurements provide a powerful new probe of not only the SMBH population but also feedback physics.
Big Galaxies and Big Black Holes: The Massive Ends of the Local Stellar and Black Hole Mass Functions and the Implications for Nanohertz Gravitational Waves
A new constraint on the $y$-distortion with FIRAS: implications for feedback models in galaxy formation and cosmic shear measurements
School of Physics and Astronomy, Cardiff University（卡迪夫大学物理与天文学院）；Kavli Institute for Cosmology Cambridge（剑桥宇宙学卡弗里研究所）；Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学粒子天体物理与宇宙学卡弗里研究所）；SLAC National Accelerator Laboratory（史拉夫国家加速器实验室）；Department of Physics, Stanford University（斯坦福大学物理系）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Department of Astronomy, Columbia University（哥伦比亚大学天文学系）；Department of Physics, Columbia University（哥伦比亚大学物理系）；Institute of Astronomy（天文学研究所）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo（东京大学宇宙物理数学卡弗里研究所（WPI）、东京大学高级研究院（UTIAS））；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学数据驱动发现中心、宇宙物理数学卡弗里研究所（WPI）、东京大学高级研究院）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理学科学系）
The Characteristic Mass and Energy Conversion Efficiency in the Cusp-Core Transition of Dark Matter Haloes: Implications for Scaling Relations and Supernova feedbacks
University of Tsukuba（筑波大学）；National Institute of Technology, Sendai College（国立仙台高等专门学校）；Tohoku University（东北大学）；The University of Tokyo（东京大学）
Implication of a galaxy-scale negative feedback by one of the most powerful multi-phase outflows in a hyper-luminous infrared galaxy at the intermediate redshift
本文通过 Gemini 和 ALMA 观测发现中等红移超亮红外星系 J1126 中存在快速电离与高质量损失率分子外流并存的多相外流，揭示其由 AGN 热风或辐射压力驱动，能引发电离激波并增强气体解离，产生星系尺度负反馈，具长期调节宿主增长潜力。
Tracing AGN Feedback Power with Cool/Warm Outflow Densities: Predictions and Observational Implications
Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Newcastle University（纽卡斯尔大学）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理中心）
Co-evolution of Supermassive Black Holes and their Host L* galaxies: implications for Milky Way and M31
Universidad de Buenos Aires, Facultad de Ciencias Exactas y Naturales（布宜诺斯艾利斯大学，理学院）；CONICET-Universidad de Buenos Aires, Instituto de Astronomía y Física del Espacio (IAFE)（阿根廷国家科学研究委员会-布宜诺斯艾利斯大学，天体物理学与空间物理研究所（IAFE））；Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔斯大学，天体物理研究所）
Appreciating mergers for understanding the non-linear $M_{\rm bh}$-$M_{\rm *,spheroid}$ and $M_{\rm bh}$-$M_{\rm *,galaxy}$ relations, updated herein, and the implications for the (reduced) role of AGN feedback
Discovery of O stars in the tidal Magellanic Bridge: Stellar parameters, abundances, and feedback of the nearest metal-poor massive stars and their implication for the Magellanic System ecology
Feeding and feedback from little monsters: AGN in dwarf galaxies
探测形成类星体的种子黑洞是极具挑战性的;然而，那些没有成长为超大质量的种子应该是在本地矮星系中发现的100-10 $^5$ M $_{\odot}$的中等质量黑洞（IMBH）。深多波长巡天的使用揭示了至少在$z\sim$ 3以外的矮星系中存在着一群积极吸积的IMBH（低质量活动星系核）。这些星系的黑洞占有率表明，早期宇宙种子黑洞是由气体直接坍缩形成的，这是由低质量端的黑洞-星系标度关系的可能平坦化所加强的。然而，这种情况受到了AGN反馈可以对矮星系产生强烈影响的发现的挑战，这意味着矮星系中的低质量AGN可能不是早期种子黑洞未受影响的遗迹。这对种子黑洞形成模型有重要的意义。
Tracing ionized gas kinematics in Lyman-Break Analogs. Implications for star formation compactness and outflow properties
Universidad de La Serena（拉塞雷纳大学）；Instituto de Astrofísica de Andalucía (CSIC)（安达卢西亚天体物理研究所）；Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理学研究中心）；INAF - Osservatorio Astronomico di Roma（意大利国家天文台罗马天文台）；Michigan Institute for Data Science, University of Michigan（密歇根大学数据科学研究所）
