Abstract
Feedback released during the growth of supermassive black holes is expected to play a key role in shaping black hole-host galaxy co-evolution. Powerful, accretion disc driven winds have been invoked to explain both observed scaling relations (e.g., M - σ) and large-scale outflows with mass outflow rates of ∼ 100 - 1000 M⊙ yr-1 and momentum rates of up to ∼ 30 LAGN/c. Critically, how these winds couple to the host galaxy depends on if they are momentum or energy conserving. I outline observational signatures that could distinguish between these regimes and discuss their roles in establishing galaxy properties. Furthermore, I discuss high-resolution simulations exploring feedback in a multi-phase medium, highlighting how structural properties of galaxies can impact feedback efficiency. Finally, feedback, in the form of collimated jets, is expected to regulate cooling in galaxy clusters. I discuss new simulations of jet feedback using the moving-mesh code AREPO and outline the scope of our new study.
| Original language | English |
|---|---|
| Pages (from-to) | 231-234 |
| Number of pages | 4 |
| Journal | Proceedings of the International Astronomical Union |
| Volume | 12 |
| Issue number | S324 |
| DOIs | |
| Publication status | Published - 23 Jun 2017 |
Keywords
- (galaxies:) cooling flows
- (galaxies:) quasars: general
- galaxies: active
- galaxies: clusters: general
- galaxies: evolution
- galaxies: ISM
- galaxies: jets
- methods: numerical