Santa Cruz 2018

Massive black holes in massive galaxies have exhibited close relationships with the structural properties of their host. We investigate the validity of these relationships between black hole and host within simulation dwarf galaxies.

Transcript

1. Hungry Heart: Black Holes in Romulus Dwarf Galaxies Ray Sharma (adv. Alyson Brooks) Rutgers, the State University of New Jersey
3. Romulus25 •Standard physics from GASOLINE •Cosmic UV background •Star formation •Blastwave SN feedback •Low temp metal cooling Tremmel+ (2017) M star = 109.7 M ☉ , M vir = 1011 M ☉
4. Romulus Black Holes •Sub-grid dynamical friction •Bondi-Hoyle accretion + angular momentum •Physical seeding mechanism - Direct collapse motivated Tremmel+ (2017)
5. Black Hole Seeding •Seeded at 106 M ☉ if gas is: •Metal poor •High density •Temperature ~10,000 K •Seeds formed in first ~Gyr Volonteri+ (2012); Tremmel+ (2018) NASA/CXC/Scuola Normale Superiore/Pacucci
6. Black Hole Observations Schramm & Silverman (2013)
7. Romulus25 Black Holes Volonteri & Natarajan (2009)
8. Romulus25 Black Holes Volonteri & Natarajan (2009)
9. Population Over Time
10. Population Over Time
11. Growth History BH early merger history matters
12. Growth History BH early merger history matters
13. Dwarfs With and Without BHs BH = higher effective radii? BH early merger history matters
14. Dwarfs With and Without BHs BH = higher effective radii? BH early merger history matters
15. Dwarfs With and Without BHs BH = higher effective radii? BH early merger history matters
16. Dwarfs With and Without BHs BH = higher effective radii at lower masses BH early merger history matters
17. Dwarfs With and Without BHs BH = higher effective radii at lower masses BH early merger history matters BH = no change in gas fraction
18. Dwarfs With and Without BHs BH = lower central density BH early merger history matters BH = higher effective radii at lower masses BH = no change in gas fraction Central density
19. Dwarfs With and Without BHs BH = lower central density BH early merger history matters BH = higher effective radii at lower masses BH = no change in gas fraction Central density
20. Summary •Romulus provides tools to track both BHs and low-mass galaxies •We can make predictions •Black holes matter in dwarf galaxies (but how low mass?) ⚫ BHs increase galaxy size at low masses ⚫ BHs do not change gas fraction ⚫ BHs decrease central density •Sharma+ (2018) in prep, stay tuned!
21. Extra Slides
22. Romulus Simulation Suite Cosmological SPH simulation run with ChaNGa code Tremmel+ (2017); Tremmel+ (2018)
23. Romulus Simulation Suite Cosmological SPH simulation run with ChaNGa code 4 Runs 3+ Runs Tremmel+ (2017); Tremmel+ (2018)
24. Romulus Simulation Suite Cosmological SPH simulation run with ChaNGa code Tremmel+ (2017); Tremmel+ (2018)
25. With and Without BHs
26. With and Without BHs
27. Black Hole Seeding Greene (2012) NASA/CXC/Scuola Normale Superiore/Pacucci
28. Black Hole Seeding NASA/CXC/Scuola Normale Superiore/Pacucci Greene (2012)