Galaxy Activity in Semi Analytical Models. Fabio Fontanot (INAF OATs) Ljubljana 05/04/11

Transcription

1 Galaxy Activity in Semi Analytical Models Fabio Fontanot (INAF OATs) Ljubljana 05/04/11

2 Part I: Theoretical background

3

4 1. Baryonic gas falls in the gravitational potential of Dark Matter Halos 2. Baryonic gas is shock-heated to the virial temperature

5 3. Radiative Cooling Gas infalls towards the center 4. Star Formation begins in disk-like structure

6 TIME Dark Matter Halos Merger Tree

7 Galactic Winds Stellar Feedback Infall 6. Thermal processes in the baryonic gas

8 AGN activity in theoretical models of galaxy formation Represents a viable solution for a number of long-standing problems

9 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

10 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

11 Mk Croton+06 Munich group Mbj

12 AGN feedback OFF Bower+06 Durham group AGN feedback ON Mbj Mk

13 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

14 Croton+06 Munich group

15 Croton+06 Munich group

16 Semi analytical models 2 Different regimes for AGN feedback

17 Semi analytical models 2 Different regimes for AGN feedback QSO -mode or bright -mode Bright-phase

18 Bright mode High accretion events Galaxy Mergers

19 Bright mode High accretion events Galaxy Mergers

20 Bright mode High accretion events Galaxy Mergers Springer, Di Matteo, Hernquist+05 (see also Hopkins+05,06,07,08)

21 Bright mode High accretion events Galaxy Mergers Destabilize large amount of cold gas Drive it to the center

22 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

23 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

24 QSO LF & AGN Downsizing Hasinger+05 Redshift Redshift

25 QSO LF & AGN Downsizing Monaco&Fontanot05; Fontanot+06

26 Semi analytical models 2 Different regimes for AGN feedback QSO -mode Bright-phase Radio -mode Low-accretion Efficiency Radio-jets

27 Radio mode Low accretion events Development of Radio Jets

28 Radio mode Low accretion events Development of Radio Jets

29 Radio mode Low accretion events Development of Radio Jets Efficient transport of energy from central regions to the outskirt of the halo

30 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

31 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

32 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?

33 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

34 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

35 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

36 Kang+08 Bright -mode As in Croton+06 and Wang+08 Radio -mode Radio luminosity proportional to Halo mass

37 Kang+08 Bright -mode As in Croton+06 and Wang+08 Radio -mode Radio luminosity proportional to Halo mass

38 Kang+08 Bright -mode As in Croton+06 and Wang+08 Radio -mode Radio luminosity proportional to Halo mass New modeling of strangulation

39 Somerville+08 Bright -mode QSO Light curve model for BH accretion Hopkins

40 Somerville+08 Bright -mode QSO Light curve model for BH accretion Hopkins

41 Somerville+08 Bright -mode QSO Light curve model for BH accretion Hopkins Radio -mode Bondi-Hoyle Accretion of hot gas

42 Somerville+08 Bright -mode QSO Light curve model for BH accretion Hopkins Radio -mode Bondi-Hoyle Accretion

43 MORGANA Unified accretion scheme Based on Umemura+01 and Granato+04

44 MORGANA Unified accretion scheme Based on Umemura+01 and Granato+04 Gas accretion from a reservoir by viscosity

45 2) Reservoir Formation 3) Gas accretion (turbulence, magnetic field, radiation drag) determined by viscosity of accretion disk 4) Feedback 1) Onset of Cooling Flows

46 MORGANA Unified accretion scheme Based on Umemura+01 and Granato+04 Gas accretion from a reservoir by viscosity

47 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

48 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

49 Bright mode Munich triggered by major and minor mergers KauffmannHaehnelt00 Croton+06 Somerville+08 triggered by major mergers Hopkins 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

50 Bright mode Munich triggered by major and minor mergers KauffmannHaehnelt00 Croton+06 Somerville+08 triggered by major mergers Hopkins 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

51 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)

52 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)

53 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/ )

54 Pasquali+09 Yang+07 group catalogue Estimates for stellar and halo mass Activity Classes SFG e AGN HRA e LRA

55 Pasquali+09 Yang+07 group catalogue Estimates for stellar and halo mass Activity Classes SFG e AGN HRA e LRA

56 Pasquali+09 Yang+07 group catalogue Estimates for stellar and halo mass Activity Classes SFG e AGN HRA e LRA

57 Converting Model Prections Star Forming Galaxies SFR = 0.5x 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 (!!)

58 Conversions OIII line Luminosity Radio Power

59 Conversions OIII line Luminosity Radio Power

60 Conversions OIII line Luminosity Radio Power

61 Conversions OIII line Luminosity Radio Power

62 Conversions OIII line Luminosity Radio Power

63 Conversions OIII line Luminosity Radio Power

64 Central Galaxies

65 Central Galaxies MORGANA

66 Central Galaxies Somerville+08

67 Central Galaxies All Models

68 Central Galaxies All Models MORGANA

69 ψ = Lkin / Lheat

70 Duty Cycles! 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

71 2) Reservoir Formation 1) Onset of Cooling Flows 6) Quenching of Cooling Flows 3) Viscosity; Gas accretion T 5) Jet Development 4) Feedback

72 Satellite Galaxies

73 Satellite Galaxies Kang+08

74 Satellite Galaxies MORGANA

75 Bidimensional Distributions

76 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