Feedback & Large Surveys Harry Ferguson (STScI)
Feedback Behroozi Halo quenching Quasar mode AGN Radio Mode AGN (SNe) SNe Satellites: Ram pressure, tides, shocks… UV back- ground
AGN feedback in SAMs Somerville AGN quenching successfully reduces the stellar masses at the bright end. Somewhat degenerate with simple “halo quenching”
Mergers & QSOs Hopkins 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 Correlation 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
Linking morphology to merger- driven feedback
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
SMGs are disks? Targett+ 2011,12 The mass- dominant components of SMGs appear to be disk-like
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 With the same initial conditions, different models built very different galaxies. None particularly successful.
Models already diverge at z=5
Questions What is the relative importance of ejective vs. preventative feedback? What is the relative importance of environmental quenching vs. mass quenching? What is the relative importance of mergers vs. smooth star formation? How can we tell?