Quasar Heating in Structure Formation类星体的加热结构的形成.ppt

Quasar Heating in Structure Formation类星体的加热结构的形成
Peng Oh
UC Santa Barbara
Rob Thacker
Queen’s University
Hugh Couch2
Preheated Gas:
gas =i (T/Ti)3/2
Lx ~ T7
Mushotzky and Scharf 2019
Clusters: X-ray Emission
1 keV~ 100 keV cm2
Kaiser (1991)
AGN Heating
Radio jets
3C47, Leahy (2019)
~10%
BAL Winds
~All
Murray, Chiang, Grossman, & Voit 2019
Galaxy Clusters
Temperature/ keV
LX
1040
1042
1044
1046
LX
Quasar Luminosity Function
Fundamental differences between the semi-analytic & simulation models
1.) In the simulation we don’t eject the gas from the quasar host galaxy itself. This gas isn’t counted in the semianalytic model.
2.) In simulation shock the surrounding material that has substructure. Effect of shock impacting uniform cloud versus cloud with substructure are very different. OVERCOOLING!
IF #1 we need to do more than stop accretion
IF #2 we need either need more feedback, or….
Naab, Ostriker et al (2019)
S
Quasar-Galaxy cross correlation function
Blue=gg
Red=qg
Hash=DEEP2 (from Coil etal 06)
blue line = 2x1012 DM halos

Could this be
3-body interactions?
Seen in SDSS (Serber etal 2019)
Dynamical Friction
Dynamical Friction
Three-body interactions
Conclusions
Semianalytical models: show that quasars outflows
are a promising explanation for the antihierarchical behavior of galaxy and quasars, and the properties of clusters.
Simulations:
Merger model reproduces correlation function of quasars very well.
Cross-correlation function shows enhancement at small separations, probably due to 3 body interactions, may be a diagnostic of merger-nature
Lx-T is well reproduced
Luminosity function less well reproduced: In-shock cooling? ISM physics? (probably both are true)
Entropy – final state
Thanks to Jon Johansson,
CNS, U. of Alberta
Galaxies and Stars
Why don’t we use Gadget2?
Simulation time
Total wallclock