Galaxy Activity in Semi Analytical Models Fabio Fontanot (INAF OATs) Ljubljana 05/04/11
Part I: Theoretical background
1. Baryonic gas falls in the gravitational potential of Dark Matter Halos 2. Baryonic gas is shock-heated to the virial temperature
3. Radiative Cooling Gas infalls towards the center 4. Star Formation begins in disk-like structure
TIME Dark Matter Halos Merger Tree
Galactic Winds Stellar Feedback Infall 6. Thermal processes in the baryonic gas
AGN activity in theoretical models of galaxy formation Represents a viable solution for a number of long-standing problems
AGN activity in theoretical models of galaxy formation Represents a viable solution for a number of long-standing problems Quenching cooling flows in massive halos
AGN activity in theoretical models of galaxy formation Represents a viable solution for a number of long-standing problems Quenching cooling flows in massive halos Bright-end of luminosity function
Mk Croton+06 Munich group Mbj
AGN feedback OFF Bower+06 Durham group AGN feedback ON Mbj Mk
AGN activity in theoretical models of galaxy formation Represents a viable solution for a number of long-standing problems Quenching cooling flows in massive halos Bright-end of luminosity function Red colors and SFRs in local massive galaxies
Croton+06 Munich group
Croton+06 Munich group
Semi analytical models 2 Different regimes for AGN feedback
Semi analytical models 2 Different regimes for AGN feedback QSO -mode or bright -mode Bright-phase
Bright mode High accretion events Galaxy Mergers
Bright mode High accretion events Galaxy Mergers
Bright mode High accretion events Galaxy Mergers Springer, Di Matteo, Hernquist+05 (see also Hopkins+05,06,07,08)
Bright mode High accretion events Galaxy Mergers Destabilize large amount of cold gas Drive it to the center
Bright mode High accretion events Galaxy Mergers Destabilize large amount of cold gas Drive it to the center Thermal Feedback Triggering of galactic winds Cold gas depletion
Bright mode High accretion events Galaxy Mergers Destabilize large amount of cold gas Drive it to the center Thermal Feedback Triggering of galactic winds Cold gas depletion Result Elliptical Morphology (?) BH-Bulge correlation Starburst & Sudden stop of SFR N.B. No direct link with low-z properties
QSO LF & AGN Downsizing Hasinger+05 Redshift Redshift
QSO LF & AGN Downsizing Monaco&Fontanot05; Fontanot+06
Semi analytical models 2 Different regimes for AGN feedback QSO -mode Bright-phase Radio -mode Low-accretion Efficiency Radio-jets
Radio mode Low accretion events Development of Radio Jets
Radio mode Low accretion events Development of Radio Jets
Radio mode Low accretion events Development of Radio Jets Efficient transport of energy from central regions to the outskirt of the halo
Radio mode Low accretion events Development of Radio Jets Efficient transport of energy from central regions to the outskirt of the halo Injection of mechanical energy Perseus Cluster Fabian+04
Radio mode Low accretion events Development of Radio Jets Efficient transport of energy from central regions to the outskirt of the halo Injection of mechanical energy Fundamental for quenching cooling flows in massive halos Keeps red galaxies red! Not well understood
Radio mode Low accretion events Development of Radio Jets Efficient transport of energy from central regions to the outskirt of the halo Injection of mechanical energy Fundamental for quenching cooling flows in massive halos Keeps red galaxies red! Not well understood Steady state accretion rate or cyclic behaviour?
Semi analytical models QSO -mode Bright-phase Radio -mode Low-accretion Efficiency Radio-jets We consider four models Munich Wang+08 Somerville+08 Kang+08 MORGANA MonacoFontanotTaffoni07
Wang+08 Bright -mode Related to minor and major mergers Radio -mode Accretion of hot gas from static atmosphere Accretion rate proportional to halo mass (See also Croton+06) Croton+06
Wang+08 Bright -mode Related to minor and major mergers Radio -mode Accretion of hot gas from static atmosphere Accretion rate proportional to halo mass (See also Croton+06) Croton+06
Kang+08 Bright -mode As in Croton+06 and Wang+08 Radio -mode Radio luminosity proportional to Halo mass
Kang+08 Bright -mode As in Croton+06 and Wang+08 Radio -mode Radio luminosity proportional to Halo mass
Kang+08 Bright -mode As in Croton+06 and Wang+08 Radio -mode Radio luminosity proportional to Halo mass New modeling of strangulation
Somerville+08 Bright -mode QSO Light curve model for BH accretion Hopkins+05+07+09
Somerville+08 Bright -mode QSO Light curve model for BH accretion Hopkins+05+07+09
Somerville+08 Bright -mode QSO Light curve model for BH accretion Hopkins+05+07+09 Radio -mode Bondi-Hoyle Accretion of hot gas
Somerville+08 Bright -mode QSO Light curve model for BH accretion Hopkins+05+07+09 Radio -mode Bondi-Hoyle Accretion
MORGANA Unified accretion scheme Based on Umemura+01 and Granato+04
MORGANA Unified accretion scheme Based on Umemura+01 and Granato+04 Gas accretion from a reservoir by viscosity
2) Reservoir Formation 3) Gas accretion (turbulence, magnetic field, radiation drag) determined by viscosity of accretion disk 4) Feedback 1) Onset of Cooling Flows
MORGANA Unified accretion scheme Based on Umemura+01 and Granato+04 Gas accretion from a reservoir by viscosity
BRIGHT-MODE 5) Triggering of Galactic Winds 6) Quenching of Star Formation 5) Jet Development 6) Quenching of Cooling Flows Coupling between AGN and stellar feedback may lead to... RADIO-MODE
MORGANA Unified accretion scheme Based on Umemura+01 and Granato+04 Gas accretion from a reservoir by viscosity Accretion Rate determines feedback scheme High accretion rates = bright -mode Low accretion rates = radio -mode
Bright mode Munich triggered by major and minor mergers KauffmannHaehnelt00 Croton+06 Somerville+08 triggered by major mergers Hopkins+05+07 Kang+08 triggered by major mergers KauffmannHaehnelt00 MORGANA associated with Eddingtonlimited accretion rates from a cold gas reservoir Umemura00 Granato+04 Reservoir formed at major minor mergers and disc instabilities
Bright mode Munich triggered by major and minor mergers KauffmannHaehnelt00 Croton+06 Somerville+08 triggered by major mergers Hopkins+05+07 Kang+08 triggered by major mergers KauffmannHaehnelt00 MORGANA associated with Eddingtonlimited accretion rates from a cold gas reservoir Umemura00 Granato+04 Reservoir formed at major minor mergers and disc instabilities
Radio mode Munich accretion of hot gas from hidrostatic halo Croton+06 Somerville+08 Bondi-Hoyle accretion of hot gas NulsenFabian00 Kang+08 accretion of hot gas Kang+06 MORGANA associated with lowaccretion rates from a cold gas reservoir Umemura00 Granato+04 All models predicts the energy injected into the ICM (Lheat)
Radio mode Munich accretion of hot gas from hidrostatic halo Croton+06 Somerville+08 Bondi-Hoyle accretion of hot gas NulsenFabian00 Kang+08 accretion of hot gas Kang+06 MORGANA associated with lowaccretion rates from a cold gas reservoir Umemura00 Granato+04 All models predicts the energy injected into the ICM (Lheat)
Part II Comparing Models with Observations F. Fontanot, A. Pasquali, G. De Lucia, F.C. van den Bosch, R.S. Somerville, X. Kang (astro ph/1006.5717)
Pasquali+09 Yang+07 group catalogue Estimates for stellar and halo mass Activity Classes SFG e AGN HRA e LRA
Pasquali+09 Yang+07 group catalogue Estimates for stellar and halo mass Activity Classes SFG e AGN HRA e LRA
Pasquali+09 Yang+07 group catalogue Estimates for stellar and halo mass Activity Classes SFG e AGN HRA e LRA
Converting Model Prections Star Forming Galaxies SFR = 0.5x 7.9 10-42 Lhα Kennicutt98 OIII line Luminosity LHard-X/LOIII=2.15 Heckman+05 Marconi+04 Radio Power Lkin=3x1045f3/2(L151MHz)6/7 Willott+99 Lkin = Lheat (!!)
Conversions OIII line Luminosity Radio Power
Conversions OIII line Luminosity Radio Power
Conversions OIII line Luminosity Radio Power
Conversions OIII line Luminosity Radio Power
Conversions OIII line Luminosity Radio Power
Conversions OIII line Luminosity Radio Power
Central Galaxies
Central Galaxies MORGANA
Central Galaxies Somerville+08
Central Galaxies All Models
Central Galaxies All Models MORGANA
ψ = Lkin / Lheat
Duty Cycles! 0.1-0.01 Gyrs typical duty cycles of radio sources Model predicts integrated quantities Integration timescale ~0.1 Gyrs MORGANA already implements something similar to a duty cycle
2) Reservoir Formation 1) Onset of Cooling Flows 6) Quenching of Cooling Flows 3) Viscosity; Gas accretion T 5) Jet Development 4) Feedback
Satellite Galaxies
Satellite Galaxies Kang+08
Satellite Galaxies MORGANA
Bidimensional Distributions
Conclusions Model predictions are remarkably similar (despite very different assumptions for BH accretion) Models predict... Too many high-mass galaxies and halos host a luminous radio source HRA and LRA distributions are quite different AGN distributions show stronger differences among models Expand M*-OIII space currently probed by observations