Quenching as a Contest between Galaxy Halos and their Central Black Holes
| Autor: | Sandro Tacchella, Fengshan Liu, Dale D. Kocevski, Fangzhou Jiang, Bryan A. Terrazas, Mauro Giavalisco, Jerome J. Fang, Viraj Pandya, S. M. Faber, Zhijian Luo, Guillermo Barro, A. van der Wel, Samir Salim, Chenggang Shu, Marc Huertas-Company, Aldo Rodríguez-Puebla, David C. Koo, Lin Lin, Henry C. Ferguson, Joel R. Primack, Rachel S. Somerville, Joanna Woo, Camilla Pacifici, Avishai Dekel, Zhu Chen, Eric F. Bell, Susan A. Kassin, Hassen M. Yesuf, Yicheng Guo, Yifei Luo |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2019 |
| Předmět: |
Physics
Supermassive black hole 010504 meteorology & atmospheric sciences Stellar mass Star formation FOS: Physical sciences Astronomy and Astrophysics Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Astrophysics - Astrophysics of Galaxies Galaxy Physical cosmology Black hole Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) 0103 physical sciences Galaxy formation and evolution Halo 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences |
| Popis: | Existing models of galaxy formation have not yet explained striking correlations between structure and star-formation activity in galaxies, notably the sloped and moving boundaries that divide star-forming from quenched galaxies in key structural diagrams. This paper uses these and other relations to ``reverse-engineer'' the quenching process for central galaxies. The basic idea is that star-forming galaxies with larger radii (at a given stellar mass) have lower black-hole masses due to lower central densities. Galaxies cross into the green valley when the cumulative effective energy radiated by their black hole equals $\sim4\times$ their halo-gas binding energy. Since larger-radii galaxies have smaller black holes, one finds they must evolve to higher stellar masses in order to meet this halo-energy criterion, which explains the sloping boundaries. A possible cause of radii differences among star-forming galaxies is halo concentration. The evolutionary tracks of star-forming galaxies are nearly parallel to the green-valley boundaries, and it is mainly the sideways motions of these boundaries with cosmic time that cause galaxies to quench. BH-scaling laws for star-forming, quenched, and green-valley galaxies are different, and most BH mass growth takes place in the green valley. Implications include: the radii of star-forming galaxies are an important second parameter in shaping their black holes; black holes are connected to their halos but in different ways for star-forming, quenched, and green-valley galaxies; and the same BH-halo quenching mechanism has been in place since $z \sim 3$. We conclude with a discussion of black hole-galaxy co-evolution, the origin and interpretation of BH scaling laws. 45 pages, 20 figures, 2 tables, accepted for publication in ApJ |
| Databáze: | OpenAIRE |
| Externí odkaz: |
|