We find, from high-resolution hydro simulations, that winds from AGN effectively heat the inner parts (~100 pc) of elliptical galaxies, reducing infall to the central SMBH; and radiative (photoionization and X-ray) heating reduces cooling flows at the kpc scale. Including both types of feedback with (peak) efficiencies of 3 10^{-4} < epsilon_mech < 10^{-3} and of epsilon_rad ~10^{-1.3} respectively, produces systems having duty-cycles, central SMBH masses, X-ray luminosities, optical light profiles, and E+A spectra in accord with the broad suite of modern observations of massive elliptical systems. Our main conclusion is that mechanical feedback (including all three of energy, momentum and mass) is necessary but the efficiency, based on several independent arguments must be a factor of 10 lower than is commonly assumed. Bursts are frequent at z>1 and decline in frequency towards the present epoch as energy and metal rich gas are expelled from the galaxies into the surrounding medium. For a representative galaxy of final stellar mass ~3 10^{11} Msun, roughly 3 10^{10} Msun of recycled gas has been added to the ISM since z~2 and, of that, roughly 63% has been expelled from the galaxy, 19% has been converted into new metal rich stars in the central few hundred parsecs, and 2% has been added to the central SMBH, with the remaining 16% in the form hot X-ray emitting ISM. The bursts occupy a total time of ~170 Myr, which is roughly 1.4% of the available time. Of this time, the central SMBH would be seen as an UV or optical source for ~45% and ~71$% of the time, respectively. Restricting to the last 8.5 Gyr, the burst occupy ~44 Myr, corresponding to a fiducial duty-cycle of ~5 10^{-3}.
Nonlinear Color-Metallicity Relations of Globular Clusters. III. On the Discrepancy in Metallicity between Globular Cluster Systems and their Parent Elliptical Galaxies
Accretion onto Black Holes from Large Scales Regulated by Radiative Feedback. III. Enhanced Luminosity of Intermediate Mass Black Holes Moving at Supersonic Speeds
An Improved [O III] Line Width to Stellar Velocity Dispersion Calibration: Curvature, Scatter, and Lack of Evolution in the Black-Hole Mass Versus Stellar Velocity Dispersion Relationship
Astraeus III: The environment and physical properties of reionization sources
在本文中，我们使用了N体dArk martEr模拟中星系形成和再电离的数值辐射传递耦合框架，它耦合了前十亿年的星系形成和再电离。探索了一些模型的再电离反馈和逃逸分数的电离辐射从银河系环境（$f_\mathrm{esc}$），我们量化的贡献的恒星形成星系{（与晕质量$M_h>10^{8.2}$ M $_\odot$）}再电离依赖于辐射反馈模型，$f_\mathrm{esc}$，和环境的过密度。我们的主要发现是：（i）对于常数$f_\mathrm{esc}$模型，中等质量星系（晕质量为$M_h\simeq10^{9-11}$ M $_\odot$，绝对紫外强度为$M_{UV} \sim -15$至$-20$）在中密度区域驱动再电离;（ii）$f_\mathrm{esc}$随着晕质量的降低而增加的情况下，星系人口将驱动再电离至低质量星系（$M_h\lesssim10^{9.5}$ M $_\odot$）与较低的光度（$M_{UV} \gtrsim-16$）和过密度;（iii）再电离印记其拓扑结构的电离发射率的低质量星系（$M_h\lesssim10^{9}$ M $_\odot$）通过辐射反馈。低质量星系经历辐射反馈对恒星形成的更强抑制，在过密区域表现出较低的电离发射率;（iv）$f_\mathrm{esc}$随星系性质的变化对再电离源及其可探测性的影响最大，辐射反馈强度和环境过密起着次…
