Modelling the cosmological coevolution of supermassive black holes and galaxies

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Modelling the cosmological co-evolution of
supermassive black holes and galaxies
Federico Marulli
Collaborators Lauro Moscardini (Università di
Bologna) Enzo Branchini (Università Roma
Tre) Silvia Bonoli, Volker Springel, Simon D. M.
White (Max-Planck-Institut fuer Astrophysik,
Garching)

• Dipartimento di Astronomia
• Università di Bologna

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Contents

• Aim of the study
• Modelling the co-evolution of supermassive black
  holes and galaxies in the ?CDM cosmology
• Understanding the role of the AGN feedback in the
  evolution of galaxies and clusters
• Working strategy
• Hybrid models dark halos (N-body) galaxies
  BHs
• Observational data
• BH scale relation and fundamental plane
• BH mass function
• AGN luminosity function
• AGN clustering function

Federico Marulli Torino May 2008
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Hybrid models DM galaxies BH
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
Millennium Simulation GADGET-2 code (Springel
2005), at the Computing Centre of the Max-Planck
Society in Garching, Germany Dynamical evolution
of 21603 ? 1e10 DM particles with mass 8.6x1e8
Msun/h in a periodic box of 500 Mpc/h on a side,
in a LCDM concordance cosmological framework
(2-degree Field Galaxy Redshift Survey (2dFGRS)
(Colless et al. 2001) and first-year WMAP data
(Spergel et al. 2003), as shown by Sanchez et al.
(2006)) Mass resolution DM halo of 0.1L?
galaxies with 100 particles Spatial
resolution co-moving scale of 5
kpc/h Hierarchical merging trees extracted from
this simulation DM haloes and subhalos
identified with, respectively, a
friends-of-friends (FOF) group-finder and an
extended version of the SUBFIND algorithm
(Springel et al. 2001)
http//www.mpa-garching.mpg.de/millennium
Federico Marulli Torino May 2008
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Hybrid models DM galaxies BH
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
Croton, Springel, White, De Lucia, Frenk, Gao,
Jenkins, Kauffmann, Navarro, Yoshida 2006 De
LuciaBlaizot 2007
Gas cooling (White-Frenk 1991, Springel et al.
2001)
Photon-ionization heating (Kravtzov et al. 2004)
Star formation (Kauffmann 1996)
Gas reated by supernovae
Energy released by supernovae
Disk instability (Mo et al. 1998)
Fraction of gas turned into stars after a
merger (Cox 2004)
Federico Marulli Torino May 2008
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Hybrid models DM galaxies BH
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
quasar mode
radio mode
Federico Marulli Torino May 2008
Croton et al. 2006, De Lucia-Blaizot 2007
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BH scale relations at z0
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
Black dots observations Black dashed lines
best fit to the observational datasets Red dots
model output Blue solid lines fit to the
model prediction K- and B-band bulge
magnitude Marconi et al. (2004) sigma
Ferrarese Ford (2005) Mbulge Haring Rix
(2004) Vc Baes et al. (2003) Mbh Ferrarese
(2002) equations 4 (cyan), 6 (green) and 7
(magenta) and Baes et al. (2003) (red)
Federico Marulli Torino May 2008
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BH fundamental plane
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
Black dashed lines Hopkins et al. (2007) Red
dots model outputs Blue solid lines best-fits
to the model outputs
The galaxy stellar mass is given in units of 1e11
Msun, the bulge velocity dispersion is in units
of 200 km/s
Federico Marulli Torino May 2008
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BH mass function
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
Federico Marulli Torino May 2008
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AGN luminosity function
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
Optical Kennefick et al. 1995 Schmidt et al.
1995 Koehler et al. 1997 Grazian et al. 2000
Fan et al. 2001 Wolf et al. 2003 Hunt et al.
2004 Cristiani et al. 2004 Croom et al. 2005
Richards et al. 2005, 2006 Siana et al. 2006
Fontanot et al. 2007 Shankar Mathur 2007
Bongiorno et al. 2007 Infra-red Brown et al.
2006 Matute et al. 2006 Babbedge et al. 2006
Soft X-ray Miyaji et al. 2000, 2001 Silverman
et al. 2005b Hasinger et al. 2005 Hard X-ray
Barger et al. 2003 Ueda et al. 2003 Barger et
al. 2003 Nandra et al. 2005 Sazonov
Revnivtsev 2004 Silverman et al. 2005a La
Franca et al. 2005 Shinozaki et al. 2006
Beckmann et al. 2006 Emission lines Hao et al.
2005
Federico Marulli Torino May 2008
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AGN clustering function
Marulli, Branchini, Gilli, Moscardini, Bonoli in
preparation
CDFs AGN clustering Gilli et al. 2005
Federico Marulli Torino May 2008
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Summary
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
BH scaling relations
BH mass function
BH fundamental plane
AGN luminosity function
AGN clustering
Federico Marulli Torino May 2008
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Summary
Marulli, Bonoli, Branchini, Moscardini, Springel
2008, MNRAS.368.1269M
Galaxy luminosity function at z0 Galaxy
evolution - downsizig Cooling flows in clusters
Croton et al. 2006
Radio mode BH feedback - Not triggered by
mergers - Low z - High mass DM halos
BH scaling relations BH mass functions AGN
evolution downsizing AGN clustering
Marulli et al. 2008
Federico Marulli Torino May 2008
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Conclusions

• The cosmological co-evolution of BHs, AGN and
  galaxies can be well described within the ?CDM
  model
• At redshifts zgt1, the evolution history of DM
  halo fully determines the overall properties of
  the BH and AGN populations. The AGN emission is
  triggered mainly by DM halo major mergers and, on
  average, AGN shine at their Eddington luminosity
• The cold gas fraction accreted by BHs at high
  redshifts seems to be larger than at low
  redshifts
• At redshifts zlt1, BH growth decouples from
  halo growth. Galaxy major mergers cannot
  constitute the only trigger to accretion episodes
  in this phase
• When a static hot halo has formed around a
  galaxy, a fraction of the hot gas continuously
  accretes onto the central BH, causing a
  low-energy radio'' activity at the galactic
  centre, which prevents significant gas cooling
  and thus limiting the mass of the central
  galaxies and quenching the star formation at late
  time

The end! thanks!
Federico Marulli Torino May 2008