feedback & large surveys harry ferguson (stsci). feedback behroozi+ 2011 halo quenching quasar...
TRANSCRIPT
Feedback
Behroozi+ 2011
Halo quenching
Quasar mode AGN
Radio Mode AGN
(SNe)
SNe
Satellites: Ram
pressure, tides,
shocks…
UV back-
ground
AGN feedback in SAMs
Somerville+ 2008
AGN quenching successfully reduces the stellar masses at the bright end.
Somewhat degenerate with simple “halo quenching”
Mergers & QSOs
Hopkins+ 2006 used numerical simulations to determine the relation between merger lifetimes & luminosities and QSO lifetimes & luminosities.
Inferred contribution of mergers to the SFRD at z~2 is 30-50%.
Quenching high-mass galaxies
Successful models of feedback affect star-formation differentially along the mass sequence.
Therefore statistical constraints on SFR(t,M) have the potential to distinguish between mechanisms.
Gabor+ 2010
Successes of Feedback models Qualitative understanding of:
For galaxies: Mass-metallicity relation Star-formation efficiency as a function of halo mass Red-sequence/blue-sequence Clustering of SMGs, Early type galaxies, QSOs
For AGN: QSO lifetimes AGN column-density distributions QSO clustering
Cluster entropy floor
Example: Clustering
Hickox+ 2012Correlation length of sub-millimeter galaxies, QSOs & bright ellipticals are comparable
Evolutionary scenario for high-mass galaxies:
Key Observational tests? Measurements of feedback
Wind momenta Galaxy ICM temperatures
BH-mass stellar-mass relations with redshift
Improved clustering measurements
Red-sequence Evolution
AGN Host morphologies
Metallicity-dependent SFRs
Challenges Observational
Disk galaxy properties Simultaneously matching disk galaxy mass function,
mass-metallicity, Tully Fisher relation & bulge fraction
Spheroidal galaxy sizes & evolution SMGs are disks? (not mergers – Targett+ 2011,12) Morphologies of AGN hosts (Kocevski 2012) Moderate-luminosity AGN
Merger or instability driven? Is feedback from these AGN inportant?
Theoretical Dynamic range Microphysics of feedback
CANDELS AGN Hosts at z~2 • Undisturbed disks are the
most common morphology• AGN hosts do not show
irregular morphologies any more often than a mass-matched sample of non-active control galaxies.
• Merger fraction is unexpectedly low.
• Implication for AGN fueling theory: If disks have not experienced major merger in recent past, then stochastic internal accretion may play a greater role in fueling AGN activity at z~2 than expected.
Kocevski+ 2012
Challenges: Disk galaxy properties
Scannapieco+ 2012
With the same initial conditions, different models built very different galaxies.None particularly successful.