Multi-wavelength Approachto joint formation and evolution

of Galaxies and AGNs

Fabio Fontanot Max-Planck-Institute

fuer Astronomie, HeidelbergLubiana, 25/03/08

Outline

Introduction to the problem of joint Formation of

Galaxies and AGNs

Theoretical perspective

Observational Constraints

Original Results

Assembly of Massive Galaxies

Evolution of the AGN population

Galaxy Formation and Evolution

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 puts gas

toward the center

4. Star Formation

begins in disk-like structure

Dark Matter Halos Merger Tree

TIME

Tidal StrippingDynamical

Friction

Merging

5. Interaction of galaxies with

the enviroment: instabilities

modify galactic structures

(bulge formation)

Galactic Winds

Infall

Feedback

6. Thermal processes in the

baryonic gas

Stellar

Active Galactic Nuclei

AGNs & Quasars

Compact and luminous sources (L~1046-49erg/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)Padovani & Urry 1995

AGN – Host Galaxy connection

Marconi & Hunt 2004

Observational Constraints

“Downsizing”Archeological

Stellar populations in in massive galaxies are older than those in low-mass galaxiesMassive galaxies are more metal rich than low-mass counterparts (Gallazzi+ 2005)Star formation timescales are shorter in massive galaxies (Thomas+ 2005)

Stellar Mass AssemblyMassive galaxies already in place at high-z (Cimatti+ 2006, Conselice+ 2007)

Star Formation ActivitySpecific star formation rate declines more rapidly for massive galaxies (Panther+ 2007; Zheng+ 2007)

Space density of brighter AGNs peaks at higher redshift with respect to fainter ones

Most massive BH accreted their mass faster and at higher redshift with respect to low-mass ones (Shankar+ 2004)

Anti-hierarchical behavior of baryons

MORGANAModel for the Rise of GAlaxies aNd Agns

(Monaco, Fontanot & Taffoni, 2007)

1: ComplexityMass flowsOutside the integration

disc instabilitiesminor and major mergerstidal stripping and disruptionquasar winds

2: Cooling & Infall

hot polytropic gasin hydrostatic equilibrium

equilibrium computedat each time-step

gas is coldwithin the

cooling radius

the cooling radius isa dynamical variable

that takes into accountthe hot gas from feedback

Viola+ 2008

MORGANA Cooling

Simulations Gadget2 SPH code with entropy-conserving integration

60000 DM particles and 60000 gas particles inside the virial radius

Static DM halo with NFW profile

Gas profile in hydrostatic equilibrium

Radiative cooling switched on

Classical Cooling

3: Feedback

Stellar Feedback

Stars provide both thermal and kinetic energy to cold gas (by Starlight and/or SNe explosions)

Improved modeling (Monaco, 2004) with two phase treatment of star forming ISM

3: Feedback

Stellar Feedback

Stars provide both thermal and kinetic energy to cold gas (by Starlight and/or SNe explosions)

Improved modeling (Monaco, 2004) with two phase treatment of star forming ISM

Kinetic feedback

Velocity dispersion of cold clouds

σcold = σ0 t*-⅓

3: Feedback

QSO feedbackAccretion on central BHEnergy Input

1. Black Hole (BH) seed in every model galaxy

2. Creation of Gas Reservoir

following instabilities(Granato+ 2004)3. QSO shining &

Feedback

3: Feedback

QSO feedbackAccretion on central BHEnergy Input

QSO shining is able to change the physical conditions of stellar feedback in galaxies (Monaco & Fontanot, 2005)

Triggering of galactic winds (“QSO Mode”?)

3: FeedbackQSO feedback

Accretion on central BHEnergy Input

QSO shining is able to change the physical conditions of stellar feedback in galaxies (Monaco & Fontanot, 2005)

Triggering of galactic winds (“QSO Mode”?)Feedback from Radio Jets

Bringing energy from the center to the external regionsQuenching of the cooling flows (“Radio Mode”)

4: Diffuse Stellar Component

Monaco, Murante, Borgani, Fontanot, 2006

Hopkins 2004

Cosmic Star Formation Rate

Stellar Mass Function

Fontana+ 2006

The effect of stellar feedback

and quasar windson the AGN population(Fontanot, Monaco, Cristiani & Tozzi 2006)

Hard X-ray and Optical LF

Space Density Evolution

Effect of Kinetic Feedback

Black Hole – Bulge Relation

Evolution of theBlack Hole – Bulge

RelationPeng+ 2006

The assembly of massive galaxies in hierarchical

cosmology(Fontanot, Monaco, Silva & Grazian 2007)

Spectrophotometric Codes

GRASIL (Silva+ 1998)

Includes the effect of age-selective extinction (younger stellar populations are more affected by dust extinction)

Computes dust emission in infrared regions

Salpeter IMF

Redshift DistributionCimatti+ 2002

K-band LFs

Pozzetti+ 2003

Cirasuolo+ 2006

SCUBA counts

Downsizing?

MORGANA Predictions

GOODS-MUSIC data

ConclusionsModels based on Lambda CDM cosmology are able to reproduce the properties of AGN and massive galaxiesWe are able to reproduce the anti-hierarchical behavior of black hole growth

Winds are neededKinetic stellar feedback

We are able to reproduce the early assembly and late almost-passive evolution of massive galaxies

Stellar feedback Improved modeling of cooling

We are not able to reproduce the observed downsizing trend of stellar mass assembly