AGN/Galaxy Co-Evolution. Fabio Fontanot (HITS)

Transcription

1 AGN/Galaxy Co-Evolution Fabio Fontanot (HITS) 21/11/2012

2 AGN activity in theoretical models of galaxy formation Represents a viable solution for a number of long-standing theoretical problems Properties of AGN and Galaxy population are similar Joint evolution of Galaxies and AGNs

3 Outline of review talk AGNs in theoretical models of galaxy formation

4 Outline of (biased) review talk AGNs in theoretical models of galaxy formation

5 Outline of (biased) review talk AGNs in theoretical models of galaxy formation Semi-Analytic Models of galaxy formation SMBH growth Modes of AGN feedback Popular models

6 Outline of (biased) review talk AGNs in theoretical models of galaxy formation Semi-Analytic Models of galaxy formation SMBH growth Modes of AGN feedback Popular models Testing evidences for co-evolution Local Universe (z~0) Intermediate Universe (z<5) Early Universe (z>5)

7 Theory

8

9

10

11

12 Baryonic Gas Falls into the potential well of Dark Matter Haloes Adapted from Frenk & White 91 See also Baugh06

13 Baryonic Gas Falls into the potential well of Dark Matter Haloes Baryonic gas is shock-heated to the virial temperature (but see Keres+06)

14 Radiative Cooling drives gas towards the center of DMHs

15 Radiative Cooling drives gas towards the center of DMHs

16 Radiative Cooling drives gas towards the center of DMHs

17 Radiative Cooling drives gas towards the center of DMHs Star Formation begins in Disk like Structure

18 Galactic Winds Stellar Feedback Thermal processes in the baryonic gas Star Formation Infall of cold material

19 TIME Dark Matter Haloes Merger Tree

20 Interaction with enviroment - modifies galactic structures - removes angular mom. - leads to bulge formation (DeLucia+11; Fontanot+11) Tidal Stripping Dynamical Friction Merging

21

22 Active Galactic Nuclei & Quasars Compact and luminous sources (L~ erg/s) Accretion of gas onto a Supermassive Black Hole (106-9 Msun) at the center of galaxies Strong Connection with host galaxy formation and evolution (feedback, energy transfer) Courtesy Padovani & Urry 1995

23 Galaxy Luminosity Functions Mk Croton+06 Munich group Mbj

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

25 Bimodality Croton+06 Munich group

26 Bimodality Croton+06 Munich group

27 Different regimes for AGN feedback

28 Different regimes Radio -mode Low-accretion

29 Different regimes Radio -mode Low-accretion Development of radio jets

30 Different regimes Radio -mode Low-accretion Development of radio jets Keep massive galaxies red Hot Haloes Dry Mergers? LargeScales (DMH)

31 Different regimes Radio -mode Low-accretion Development of radio jets Keep massive galaxies red Hot Haloes Dry Mergers? LargeScales (DMH) Long

32 Different regimes Radio -mode Low-accretion Development of radio jets Keep massive galaxies red Hot Haloes Dry Mergers? LargeScales (DMH) Long Steady state accretion rate or cyclic behaviour?

33 Different regimes Quasar -mode High-accretion Bright-phase Galaxy Mergers

34 Different regimes Quasar -mode High-accretion Bright-phase Galaxy Mergers Springel+05 Hopkins+05,06,07,08

35 Different regimes Quasar -mode High-accretion Bright-phase Galaxy Mergers Secular processes?

36 Different regimes Quasar -mode High-accretion Bright-phase From blue to red Galaxy Mergers Secular processes?

37 Different regimes Quasar -mode High-accretion Bright-phase From blue to red Galaxy Mergers Secular processes? Small Scales (~kpc) Triggering galactic winds? Rapid

38 Different regimes Radio -mode Quasar -mode Low-accretion High-accretion Development of radio jets Bright-phase Keep massive galaxies red From blue to red Hot Haloes Galaxy Mergers Dry Mergers? LargeScales (DMH) Long Steady state accretion rate or cyclic behaviour? Secular processes? Small Scales (~kpc) Triggering galactic winds? Rapid

39 Different regimes Radio -mode Quasar -mode Low-accretion High-accretion Development of radio jets Bright-phase Keep massive galaxies red From blue to red Hot Haloes Galaxy Mergers Dry Mergers? LargeScales (DMH) Long Steady state accretion rate or cyclic behaviour? Regulates stellar mass Secular processes? Small Scales (~kpc) Triggering galactic winds? Rapid Regulates BH mass

40 SA Models

41 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

42 Menci+08 Bright -mode Related to galaxy interactions Mergers & Fly-bies

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

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

45 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

46 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

47 Malbon+07 Bright -mode Related to mergers and disk instabilities Radio -mode (See also Bower+06) Bower+06

48 Fanidakis+11 Accretion mode related to BH spin

49 Theory vs Observations

50 Low-Redshift

51 Different regimes Radio -mode Low-accretion Development of radio jets Keep massive galaxies red Hot Haloes Dry Mergers? LargeScales (DMH) Long Steady state accretion rate or cyclic behaviour? Regulates stellar mass

52 Galaxy Luminosity Functions Mk Croton+06 Munich group Mbj

53 Bimodality Croton+06 Munich group

54 Different regimes Radio -mode Low-accretion Development of radio jets Keep massive galaxies red Hot Haloes Dry Mergers? LargeScales (DMH) Long Steady state accretion rate or cyclic behaviour? Regulates stellar mass

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 Central Galaxies

58 Central Galaxies Fontanot+11 All Models

59 Central Galaxies Fontanot+11 All Models MORGANA

60 Central Galaxies MORGANA

61 BH-bulge relation Marconi & Hunt 2004

62 BH-bulge relation Credits Dave Alexander

63 Warning Jahnke&Maccio'11

64 Marulli+08 Fanidakis+11 Menci+08 Somerville+08

65 Intermediate-Redshift

66 Assembly of BH-bulge relation Colpi+07 Volonteri+10

67 Shankar+09 Evolution of BH-bulge relation (see also Marconi+04) Decarli+11 (see also Peng+06)

68 Evolution of BH-bulge relation Fontanot+06 Hopkins+07 Lamastra+10

69 Shankar+09 Evolution of BH-bulge relation (see also Marconi+04) Decarli+11 (see also Peng+06) Alexander+08

70 Downsizing

71 DS in stellar mass Log (M* / Msun) Log (M* / Msun)

72 The Manifestations of Downsizing DS in (specific) SFR (Cowie+96,Zheng07,Noeske+07,Drory&Alvarez08,Dunne+08,Santini+09...) DS in stellar mass (Drory+05, Cimatti+06, Fontana+06, Pozzetti+07, Conselice+07,...) Archeological DS (Thomas+05, Gallazzi+05, Panter+07,...) Chemo-Archeological DS (Carollo+93,Trager+00,Matteucci+04,Thomas+05,...) DS in metalicity (Savaglio+05,Erb+06,Maiolino+08,...) AGN DS (Ueda+03,Hasinger+05,LaFranca+05,...)

73 AGN Downsizing Hasinger+05 Redshift LaFranca+05

74 Fontanot+06 Hirschmann+12 Fanidakis+11 Menci+08

75 Fontanot+06

76 Menci+08

77 Fanidakis+11

78 Hirschmann+12

79 AGN Downsizing Different Explanations Coupling of AGN and stellar feedback Fontanot+06 Galaxy Interactions Menci+08 Dust Obscuration Fanidakis+11 Heavy BH seeds & major role of disk instabilities Hirschmann+12

80 Different regimes Quasar -mode High-accretion Bright-phase From blue to red Galaxy Mergers Secular processes? Small Scales (~kpc) Triggering galactic winds? Rapid

81 Warning: AGN hosts Schawinski+10;12 Xue+10

82 Warning: AGN hosts Schawinski+10;12

83 Mergers vs Secular Shankar+12 Schawinski+10;12

84 Conclusions Joint Evolution of Galaxy and AGNs Consensus: Key aspect for setting up both galactic and SMBH properties Disagreement: how does it happen? Data vs Models Good News: models (somehow) reproduce the data Bad News: models (somehow) reproduce the data Call for observational tests able to disentagle between the different proposed models Better knowledge of host galaxy properties Detailed knowledge of accretion physics Different calibration sets