Galaxy Formation in the PLANCK era
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Galaxy Formation in the PLANCK era
Bruno Henriques
Simon White, Peter Thomas, Raul Angulo,
Qi Guo, Gerard Lemson, Volker Springel
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dwarf galaxy population to build
up too early.
+Muzzin(2013) + Ilbert(2013)
Guo et al. 2013Guo et al. 2013
SSFR Agecolor
At z=0, dwarf galaxies are too blue, too old and are not forming enough stars
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Self-consistent model of galaxy
formation
MCMC
complex galaxy formation
physics
Monte Carlo Markov ChainMonte Carlo Markov ChainHenriques, Thomas et al. (2009), Henriques & Thomas (2010),
Henriques et al. (2013a)
large volume
across cosmic time
large number of parameters
inter-play between different physicshard to define
success and improve
Kampakoglou et al. (2008), Bower et al. (2010), Lu et al. (2011, 2012), Mutch et al (2013)
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CosmologyCosmology
Particle mass, Box size and redshift are scaled to the recently published PLANCK cosmology following Angulo & White 2010
As shown in Wang et al. 2008 and Guo et al. 2013, it doesn’t matter yet for galaxy formation.
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Stellar Mass FunctionStellar Mass FunctionThe delayed reincorporation of gas shifts star formation in
dwarfs to lower redshifts.
Strong suppress in number density at early times, same evolution at later times.
Henriques et al. 2013a
Muzzin(2013)+Ilbert(2013)Ilbert(2010)+Marchesini(2011)
same as Oppenheimer & Dave 2008, 2010
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Environmental problemsEnvironmental problems
The later build up of low mass galaxies results in a higher fraction of star forming low mass galaxies,
but satellites are still passive.
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Henriques et al. 2014, in prep
Ram pressure stripping only acting on haloes with Mvir>1014Msun
critical cold gas density threshold for star formation
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red massive galaxies overcome the blue number density at high-z
lower mass galaxy populations become predominately red with decreasing redshift
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AGN feedbackAGN feedbackA large fraction of intermediate mass galaxies need to assemble at z<2 and be quenched by z=0
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Colours and SFRsColours and SFRs
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Main sequence Main sequence of star formationof star formation
Model is consistent with the observed evolution of SFRs from z=3 to z=0
clear change at z=1, with galaxies falling of the main sequence of star formation
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More PredictionsMore Predictions
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More PredictionsMore Predictions
Moster2012
Henriques13 - model
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UV LFUV LF
no dust
Metallicity dependent dust
Scott Clay, Stephen Wilkins, Peter Thomas
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SFRFSFRF
model
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DatabaseDatabase
As usual everything will be in the database (Gerard Lemson)Also in the jobrunner (Mathias Egger, Gerard Lemson)Include full SF histories and full spectra (Sourour+Peter T.)MR observatory (Roderik Overzier, Gerard Lemson)
http://galformod.mpa-garching.mpg.de/portal/
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ConclusionsConclusions
delayed reincorporation of gas ejected from SN feedback
lower threshold for star formation
ram-pressure striping only effective in massive groups
low mass galaxies build up below z=2
low mass galaxies with large cold gas fractions can form stars
satellites in low mass groups will have fuel for star formation
new AGN radio mode feedback implmentationIntermediate mass galaxies assemble at z<2 and are quenched by z=0
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Mass downsizi
ng
Henriques, White, Thomas et al. 2014, in prep
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Age downsizing Henriques, White, Thomas et al. 2013b, in prep
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K-band LFK-band LF
Henriques et al. 2011, Henriques et al. 2012, Henriques et al. 2013a
M05 or CB07Stellar populations
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Web-based, modeler & observer friendly semi-analytic model
Combine the most robust set of dark matter numerical simulations availableStellar Mass resolution of 108M with a large enough volume to sample BAO
MS, MII & MXXL
Monte Carlo Markov Chain optimization +
Fit physical and cosmological parameters
Modular implementation of the physics
“Observer friendly” outputs Choose IMF, SPS, Bands, Dust model
GALFORMODGALFORMOD
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More PredictionsMore Predictions
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RainforestRainforest
Brazil
Indonesia
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Chemical EnrichmentChemical Enrichment
0.8 M 8 M
SN Ia + Stellar Winds SN II
Metals return timescale<100 Myr
Rob Yates, Peter Thomas, Simon White, Guinevere Kauffmann,
Bruno Henriques
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Gas
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Far-Infrared EmissionFar-Infrared EmissionPeter Thomas, Sorour Shamshir, Bruno Henriques, Qi Guo +
Sussex Infrared
Use empirical templates from Herschel to get an emission spectra for the light re-emitted by dust
Full radiative transfer code
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Cosmology Sampling with MCMCCosmology Sampling with MCMC
Incorporate the Angulo & White 2010 formalism into the semi-analytic model.
Include cosmological parameters in the sampling.
Bruno Henriques, Marcel Van Daalen, Raul Angulo, Simon
White, Volker Springel, Fabio Fontanot, Qi Guo
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Henriques, Maraston, Monaco, et al. (Astro-ph: 1009.1392)
Light – Weighted Ages Mass – Weighted Ages
TP-AGB
M05
M05BC03
Average!!!
Ages of GalaxiesAges of Galaxies
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SSFR vs Halo MassSSFR vs Halo Mass
Guo2013Guo2013Henriques2013bHenriques2013b
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SMF of satellitesSMF of satellites
Low mass red galaxies are mostly satellites at all times.
Massive red galaxies are mostly central galaxies and they determine the trends on SMD.
- AGN feedback
- environment effects
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SSFR vs Halo MassSSFR vs Halo Mass
Wetzel et al. (2012) - SDSS
high mass galaxies are all redlow mass galaxies are all blue
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age downsizing
mass downsizing
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ClusteringClustering
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Feedback ScalingFeedback Scaling
mass loadingfraction of SN energy
used
Reincorporation time-
scale
Henriques et al. 2013a