Galaxy Formation in the PLANCK era

Bruno Henriques

Simon White, Peter Thomas, Raul Angulo,

Qi Guo, Gerard Lemson, Volker Springel

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

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)

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.

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

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.

Henriques et al. 2014, in prep

Ram pressure stripping only acting on haloes with Mvir>1014Msun

critical cold gas density threshold for star formation

red massive galaxies overcome the blue number density at high-z

lower mass galaxy populations become predominately red with decreasing redshift

AGN feedbackAGN feedbackA large fraction of intermediate mass galaxies need to assemble at z<2 and be quenched by z=0

Colours and SFRsColours and SFRs

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

More PredictionsMore Predictions

More PredictionsMore Predictions

Moster2012

Henriques13 - model

UV LFUV LF

no dust

Metallicity dependent dust

Scott Clay, Stephen Wilkins, Peter Thomas

SFRFSFRF

model

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/

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

Mass downsizi

ng

Henriques, White, Thomas et al. 2014, in prep

Age downsizing Henriques, White, Thomas et al. 2013b, in prep

K-band LFK-band LF

Henriques et al. 2011, Henriques et al. 2012, Henriques et al. 2013a

M05 or CB07Stellar populations

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

More PredictionsMore Predictions

RainforestRainforest

Brazil

Indonesia

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

Gas

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

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

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

SSFR vs Halo MassSSFR vs Halo Mass

Guo2013Guo2013Henriques2013bHenriques2013b

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

SSFR vs Halo MassSSFR vs Halo Mass

Wetzel et al. (2012) - SDSS

high mass galaxies are all redlow mass galaxies are all blue

age downsizing

mass downsizing

ClusteringClustering

Feedback ScalingFeedback Scaling

mass loadingfraction of SN energy

used

Reincorporation time-

scale

Henriques et al. 2013a