1. Dipartimento di Astronomia Università di Bologna
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

2. Contents Aim of the study:
Modelling the co-evolution of supermassive black holes and galaxies in the ΛCDM 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

3. Hybrid models: DM + galaxies + BH
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
Millennium Simulation
GADGET-2 code (Springel 2005), at the Computing Centre of the Max-Planck Society in Garching, Germany
Dynamical evolution of ≃ 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)
Federico Marulli
Torino: May 2008

4. Hybrid models: DM + galaxies + BH
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
Croton, Springel, White, De Lucia, Frenk, Gao, Jenkins, Kauffmann, Navarro, Yoshida 2006
De Lucia–Blaizot 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

5. Hybrid models: DM + galaxies + BH
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
quasar mode:
radio mode:
Federico Marulli
Torino: May 2008
Croton et al. 2006, De Lucia-Blaizot 2007

6. BH scale relations at z=0
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
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

7. Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS.368.1269M
BH fundamental plane
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
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

8. Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS.368.1269M
BH mass function
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
Federico Marulli
Torino: May 2008

9. AGN luminosity function
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
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

10. AGN clustering function
Marulli, Branchini, Gilli, Moscardini, Bonoli in preparation
CDFs AGN clustering: Gilli et al. 2005
Federico Marulli
Torino: May 2008

11. Summary BH scaling relations BH fundamental plane BH mass function
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
BH scaling relations
BH fundamental plane
BH mass function
AGN luminosity function
AGN clustering
Federico Marulli
Torino: May 2008

12. Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS.368.1269M
Summary
Marulli, Bonoli, Branchini, Moscardini, Springel 2008, MNRAS M
Galaxy luminosity function at z=0
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

13. Conclusions The end! …thanks!
The cosmological co-evolution of BHs, AGN and galaxies can be well described within the ΛCDM model
At redshifts z>1, 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 z<1, 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