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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