multi-wavelength approach to joint formation and evolution of galaxies and agns fabio fontanot...
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![Page 1: Multi-wavelength Approach to joint formation and evolution of Galaxies and AGNs Fabio Fontanot Max-Planck-Institute fuer Astronomie, Heidelberg Lubiana,](https://reader035.vdocuments.us/reader035/viewer/2022070418/56649f485503460f94c6a47c/html5/thumbnails/1.jpg)
Multi-wavelength Approachto joint formation and evolution
of Galaxies and AGNs
Fabio Fontanot Max-Planck-Institute
fuer Astronomie, HeidelbergLubiana, 25/03/08
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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
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Galaxy Formation and Evolution
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1. Baryonic gas falls in the
gravitational potential of Dark
Matter Halos
2. Baryonic gas is shock-
heated to the virial
temperature
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3. Radiative Cooling puts gas
toward the center
4. Star Formation
begins in disk-like structure
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Dark Matter Halos Merger Tree
TIME
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Tidal StrippingDynamical
Friction
Merging
5. Interaction of galaxies with
the enviroment: instabilities
modify galactic structures
(bulge formation)
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Galactic Winds
Infall
Feedback
6. Thermal processes in the
baryonic gas
Stellar
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Active Galactic Nuclei
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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
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AGN – Host Galaxy connection
Marconi & Hunt 2004
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Observational Constraints
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“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)
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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
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MORGANAModel for the Rise of GAlaxies aNd Agns
(Monaco, Fontanot & Taffoni, 2007)
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1: ComplexityMass flowsOutside the integration
disc instabilitiesminor and major mergerstidal stripping and disruptionquasar winds
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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
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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
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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
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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
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3: Feedback
QSO feedbackAccretion on central BHEnergy Input
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1. Black Hole (BH) seed in every model galaxy
2. Creation of Gas Reservoir
following instabilities(Granato+ 2004)3. QSO shining &
Feedback
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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”?)
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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”)
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4: Diffuse Stellar Component
Monaco, Murante, Borgani, Fontanot, 2006
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Hopkins 2004
Cosmic Star Formation Rate
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Stellar Mass Function
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Fontana+ 2006
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The effect of stellar feedback
and quasar windson the AGN population(Fontanot, Monaco, Cristiani & Tozzi 2006)
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Hard X-ray and Optical LF
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Space Density Evolution
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Effect of Kinetic Feedback
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Black Hole – Bulge Relation
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Evolution of theBlack Hole – Bulge
RelationPeng+ 2006
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The assembly of massive galaxies in hierarchical
cosmology(Fontanot, Monaco, Silva & Grazian 2007)
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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
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Redshift DistributionCimatti+ 2002
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K-band LFs
Pozzetti+ 2003
Cirasuolo+ 2006
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SCUBA counts
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Downsizing?
MORGANA Predictions
GOODS-MUSIC data
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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