Galaxy Formation in the PLANCK era
Bruno Henriques
Simon White, Peter Thomas, Raul Angulo,
Qi Guo, Gerard Lemson, Volker Springel
Guo et al. 2013
+Muzzin(2013) + Ilbert(2013)
dwarf galaxy population
to build up too early.
At z=0, dwarf galaxies are too blue, too old and are not forming enough stars
color
SSFR
Age
Monte Carlo Markov Chain
Henriques, Thomas et al. (2009), Henriques & Thomas (2010), Henriques et al. (2013a)
Kampakoglou et al. (2008), Bower et al. (2010), Lu et al. (2011, 2012), Mutch et al (2013)
large number of
parameters
complex galaxy
formation physics
large volume
Self-consistent
model of galaxy
formation
across cosmic time
MCMC
inter-play between
different physics
hard to define
success and improve
Cosmology
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 Function
The 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.
Muzzin(2013)+Ilbert(2013)
Ilbert(2010)+Marchesini(2011)
Henriques et al. 2013a
same as Oppenheimer & Dave 2008, 2010
Environmental 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.
critical cold gas density threshold
for star formation
Ram pressure stripping only acting
on haloes with Mvir>1014Msun
Henriques et al. 2014, in prep
red massive galaxies overcome the
blue number density at high-z
lower mass galaxy populations
become predominately red with
decreasing redshift
AGN feedback
A large fraction of intermediate
mass galaxies need to assemble
at z<2 and be quenched by z=0
Colours and SFRs
Main sequence
of 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 Predictions
More Predictions
Moster2012
Henriques13 - model
UV LF
no dust
Scott Clay,
Stephen Wilkins,
Peter Thomas
SFRF
model
Database
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/
Conclusions
delayed reincorporation of gas ejected from SN feedback
low mass galaxies build up below z=2
lower threshold for star formation
low mass galaxies with large cold gas fractions can form stars
ram-pressure striping only effective in massive groups
satellites in low mass groups will have fuel for star formation
new AGN radio mode feedback implmentation
Intermediate mass galaxies assemble at z<2 and are quenched by z=0
Henriques, White, Thomas et al. 2014, in prep
Mass
downsizing
Age downsizing
Henriques, White, Thomas et al. 2013b, in prep
K-band LF
M05 or CB07
Stellar
populations
Henriques et al. 2011, Henriques et al. 2012, Henriques et al. 2013a
GALFORMOD
Web-based, modeler & observer friendly semi-analytic model
Combine the most robust set of dark matter numerical simulations available
Stellar 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
More Predictions
Rainforest
Brazil
Indonesia
Chemical Enrichment
SN Ia + Stellar Winds
0.8 M
SN II
8M
Metals return timescale
<100 Myr
Rob Yates, Peter Thomas, Simon White,
Guinevere Kauffmann, Bruno Henriques
Gas
Far-Infrared Emission
Peter 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 MCMC
Bruno Henriques, Marcel Van Daalen, Raul
Angulo, Simon White, Volker Springel, Fabio
Fontanot, Qi Guo
Incorporate the Angulo & White 2010
formalism into the semi-analytic model.
Include cosmological parameters in the
sampling.
Ages of Galaxies
Light – Weighted Ages
M05
Mass – Weighted Ages
BC03
M05
Average!!!
TP-AGB
Henriques, Maraston, Monaco, et al. (Astro-ph: 1009.1392)
SSFR vs Halo Mass
Henriques2013b
Guo2013
SMF of satellites
Low mass red galaxies are mostly
satellites at all times.
- environment effects
Massive red galaxies are mostly
central galaxies and they determine
the trends on SMD.
- AGN feedback
SSFR vs Halo Mass
low mass galaxies are all blue
high mass galaxies are all red
Wetzel et al. (2012) - SDSS
age downsizing
mass downsizing
Clustering
Feedback Scaling
mass loading
fraction of SN
energy used
Henriques et al. 2013a
Reincorporation
time-scale