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Transcript of GALAXIES IN DIFFERENT ENVIRONMENTS: VOIDS TO CLUSTERS: Simulations will require to model full...
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GALAXIES IN DIFFERENT GALAXIES IN DIFFERENT ENVIRONMENTS: ENVIRONMENTS:
VOIDS TO CLUSTERS:VOIDS TO CLUSTERS: Simulations will require to model full physics:
Cooling, heating, star formation feedbacks… Large dynamical range: resolving galaxies in
different density environments. Important problems to address:
Excess of small scale structure in CDM models: making small halos invisible?.
Hubble sequence (formation of disks) Interactions galaxy -ICM
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GALAXIES IN VOIDSGALAXIES IN VOIDS
M. Hoeft, G. Yepes, S. Gottlober and V. SpringelM. Hoeft, G. Yepes, S. Gottlober and V. Springelastro-ph / 0501394astro-ph / 0501394
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Void dwarf dark halos.Void dwarf dark halos.
Gottlöber et al 03Void dwarf galax
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Halo Mass function in VoidsHalo Mass function in Voids
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The missing dwarf galaxy problemin VOIDS
● No galaxies brighter than Mb=-15 found.
● What happens with baryons of small halos in voids?– Are they visible but faint?. Magnitude, colors. (Red Dwarfs)
– Are they just baryonless dark halos?
● What are the physical mechanism – Gas evaporation by UV photoionization
– Supernova feedback (e.g Dekel & Silk)
● What is the typical halo mass for this to happen?
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VOIDS FROM A 80/h Mpc Box
1024102433 effective particle in void region effective particle in void region MMgas gas = = 5.5106 M MMdark dark = = 3.4107 M Smoothing= 2-0.8 kpcSmoothing= 2-0.8 kpc
10/h Mpc10/h Mpc Simulations done with GADGET2Simulations done with GADGET2Primordial CoolingPrimordial CoolingPhotoionization Photoionization Multiphase mediumMultiphase mediumStar formationStar formationFeedback Feedback
ThermalThermalKinetic (Winds)Kinetic (Winds)
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• 20483 effective particles
• RUN with 10243
– Mgas = 1.5106 M
– Mdark= 8.2106 M
Spatial smoothing= 0.5 kpc
Different feedback params.
• Same void was resimulated
with full resolution 20483 – Mgas 2 105 M
– Mdark 106 M
– Spatial smoothing= 0.5 kpc
(ULTRA)HIGH-RESOLUTION SIMULATIONS OF A VOID IN THE 50/h Mpc Box
10/h Mpc10/h Mpc
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The missing dwarf galaxy problemin VOIDS
● No galaxies brighter than Mb=-15 found.
● What happens with baryons of small halos in voids?– Are they visible but faint?. Magnitude, colors. (Red Dwarfs)
– Are they just baryonless dark halos?
● What are the physical mechanism – Gas evaporation by UV photoionization
– Supernova feedback (e.g Dekel & Silk)
● What is the typical halo mass for this to happen?
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Baryon fractionBaryon fraction
Halos belowfew times109 Msun
arebaryon-poor
Characteristicmass scaledepends onredshift
Baryon fract
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Characteristic massCharacteristic mass Mc
baryon-rich
baryon-poor
Mc risessignificantlywith z
Halo may startbaryon-richand becomelaterbaryon-poor
Char mass
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Tentry
Density temperature phase spaceDensity temperature phase space
Cold modeof galactic gasaccretion:gas creeps alongthe equilibriumline betweenheating and cooling(Keres et al. 04)
Rho T
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Max gas temperature
Relate radius to mass
Prediction for Mc
Measurement Mc
Condition for suppression
How to suppress gas condensation?How to suppress gas condensation?How to
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Entry temperature versus characteristic massEntry temperature versus characteristic mass
General scaling:factor 1.3
High redshift:empty halos has todevelop
T entry
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Mass accretion historyMass accretion historyMass accr hist
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Baryon poor small halosBaryon poor small halosMAH, several
total mass baryonic (condensed) mass
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Age of starsAge of stars
In small halosstars can onlybe formed at highredshift
Age
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Thermal feedbackThermal feedback
Strong wind modelStrong wind model
z=0z=0
Luminosity functionLuminosity function
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Color evolutionColor evolution
z=0z=0
z=1z=1
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SOME CLUES ABOUT DWARF SOME CLUES ABOUT DWARF GALAXIES IN VOIDSGALAXIES IN VOIDS
Halos below Mlim~ 7x109 M (vc ~27 km/s) are photo-evaporated and have almost no baryon content, either cold gas or stars. This mass scale decreases with redshift. Very small dependence of UV flux.
UV-heating not able to suppress small galaxies: Problem for semianalitical models to explain substructure in the Local Group.
Thermal feedback does not play a significant role in keeping gas out of halos.
Kinetic feedback (winds) can be very efficient in inhibitting star-formation: Z agreement, redder colors,
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WORK IN PROGRESS...
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DWARF GALAXIES IN GROUPS:
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Group five
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Baryonfraction againBaryonfraction again
Baryonfraction again
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Metallicity enrichment:Metallicity enrichment:Remove baryons by feedback?Remove baryons by feedback?
Dekel+Woo
Feedback
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GALAXIES IN CLUSTERSGALAXIES IN CLUSTERS
Entropy generation from galactic feedback.
Scaling relations and non-adiabatic physics.
Understanding Intracluster light.
Effect of central Cd-galaxy on ICM radial profiles.
Cold fronts and cold flows.
How many galaxies survive in the cluster environment?
Very demanding simulations:
E.g. Cluster 6 simulated with 4.5 million particles within 3 virial radius took more than 680,000 timesteps to finished.
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STAR FORMATION IN STAR FORMATION IN CLUSTERS CLUSTERS
PhotonisationPhotonisationCoolingCoolingMultiphase mediumMultiphase mediumMetallicity Metallicity Wind modelWind model
Springel & Herquist 2003Springel & Herquist 2003
Obtain observational Obtain observational properties of dark halos from properties of dark halos from stars using BC2003 SSP stars using BC2003 SSP models models
Study Study
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CDM CLUSTER SIMULATIONSCDM CLUSTER SIMULATIONS
m=0.3; =0.7, h=0.7;
8=0.9
● 80/h Mpc box size. (Initial P(k) for 10243)
● Resample to 1283 particles.
● Identify clusters for
resimulation
GADGET (2-5 kpc)
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Z=1; =3 A=1
z=0
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LARGE-SCALE SPH SIMULATIONS
m=0.3; =0.7, h=0.7;
8=0.9, b=0.045
500/h Mpc box size. (Initial P(k) for 20483) Runs with up to 5123 particles.
# Halos=4x105 (M>1012 M)
Mdark= 7x1010 M
Identify clusters for
resimulation with 1283
Mass of clusters Mcluster 2.51015 M
Same resolution than
previous simulations 500 h500 h-1-1 Mpc Mpc
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Z=1; =3 A=1
z=0
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Lx-Tx
TTxx1.91.9
. . MMvirvir > 10 > 1015 15 MM
. 10. 1014 14 < M < Mvirvir < 10 < 101515
.2x10.2x101313 < M < Mvirvir < 10 < 101414
Clusters at 500 Mpc/h
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Lx-Tx
. . MMvirvir > 10 > 1015 15 MM
. 10. 1014 14 < M < Mvirvir < 10 < 101515
.2x10.2x101313 < M < Mvirvir < 10 < 101414
TTxx1.91.9
Observations
Clusters at 500 Mpc/h
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Lx-Tx
. . MMvirvir > 10 > 1015 15 MM
. 10. 1014 14 < M < Mvirvir < 10 < 101515
.2x10.2x101313 < M < Mvirvir < 10 < 101414
TTxx1.91.9
Observations
Clusters at 500 Mpc/h
Resimulated clusters at 80 Mpc/h
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X-ray Temperature Function
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LARGE-SCALE SPH SIMULATIONS
The MareNostrum Universe Simulation:
500/h Mpc box size. (Initial P(k) for 20483)
2x10243 particles. # Halos=106 (M>1012 M)
Mdark= 1010 M
Resolution 15 kpc.
500 h500 h-1-1 Mpc Mpc