发表机构
Canadian Institute for Theoretical Astrophysics, University of Toronto; David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto; Department of Astronomy and Astrophysics, University of California Santa Cruz; Dunlap Institute for Astronomy and Astrophysics, University of Toronto（多伦多大学理论天体物理研究所; 多伦多大学戴维·A·邓普尔天文与天体物理系; 加州大学圣克鲁斯分校天文与天体物理系; 多伦多大学邓普尔天文与天体物理研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过分析8万余个宽吸收线槽，发现辐射压驱动类星体风，但其动能光度仅为有效反馈所需水平的1/50，不足以抑制恒星形成，挑战了现有星系形成模型。
AI 中文摘要
大多数宇宙学模拟将类星体驱动的风视为抑制大质量星系恒星形成的主要机制，并假设风动量通量接近辐射压最大值 $L/c$。利用SDSS-IV DR16类星体目录中的81,388个宽吸收线槽以及详细的模拟槽光谱，我们在60%至70%的槽中探测到线锁定现象，这是辐射压驱动外流的光谱特征，表明辐射线驱动主导风加速，并排除了其他机制。对风能量收支的直接测量得出，动能光度中位数仅为辐射光度的0.01%，比有效反馈所需水平低50倍。因此，线驱动的类星体风不足以抑制恒星形成，这对星系形成模型中黑洞反馈所依赖的主要物理机制提出了挑战。
英文摘要
Most cosmological simulations invoke quasar-driven winds as the primary mechanism quenching star formation in massive galaxies, assuming wind momentum flux approaches the radiation-pressure maximum, $L/c$. Using 81,388 broad absorption line troughs from the SDSS-IV DR16 quasar catalog and detailed mock trough spectra, we detect line locking, a spectral signature of radiation-pressure-driven outflows, in 60 to 70 percent of troughs, demonstrating that radiative line driving dominates wind acceleration and ruling out alternative mechanisms. Direct measurement of the wind energy budget yields a median kinetic luminosity of only 0.01 percent of bolometric luminosity, 50 times below the level required for effective feedback. Line-driven quasar winds are therefore insufficiently powerful to quench star formation, challenging the primary physical mechanism invoked for black hole feedback in galaxy formation models.
Comments21 pages, 5 figures; supplementary material: 31 pages, 17 figures, 2 tables. Submitted to Science Advances
