a self consistent model of galaxy formation across cosmic time
DESCRIPTION
A self consistent model of galaxy formation across cosmic time. Bruno Henriques Simon White, Peter Thomas Raul Angulo, Qi Guo, Gerard Lemson, Volker Springel. Croton et al. 2006. The Munich Model. AGN feedback model (suppression of cooling). De Lucia & Blaizot 2007. dust model. - PowerPoint PPT PresentationTRANSCRIPT
A self consistent model of galaxy
formation across cosmic timeBruno Henriques
Simon White, Peter Thomas
Raul Angulo, Qi Guo, Gerard Lemson, Volker Springel
different supernova feedback (increased efficiency)
Merger treatment
The Munich ModelThe Munich Model
Guo et al. 2011
Henriques et al. 2011, 2012
different stellar populations
Croton et al. 2006
De Lucia & Blaizot 2007
AGN feedback model (suppression of cooling)
dust model
SN feedback model - reheating + ejection + reincorporation
Henriques B., White S., Lemson G., Thomas P., Guo Q., Marleau D., Overzier R.,
2012, MNRAS
LightconesLightcones
Extended photometric coverage
Multiple Stellar Populations
Pencil Beams + All Sky
http://www.mpa-garching.mpg.de
B-band Luminosity FunctionB-band Luminosity Function
Stellar Mass FunctionStellar Mass Function
K-band Luminosity FunctionK-band Luminosity Function
Semi-analytic modelling
MCMC
Complex galaxy
formation physics
Choose parameters to sampleStar formation, SN feedback, AGN feedback efficiency, Metals yield
Choose observational constraintsStellar Mass Function, K-band & B-band Luminosity Functions
MCMC Parameter SamplingMCMC Parameter SamplingHenriques B., Thomas P., Oliver S., Roseboom I., MNRAS, 2009
Henriques B., Thomas P., MNRAS, 2010
Constrain the model at multiple redshifts
Large Volume
Across Cosmic Time
Time varying parametersTime varying parametersA clear & unique change was revealed by the pre-
processing stepReincorporation of gas after ejection by SN feedback ( high-z low-z )All other parameters have consistent regions at all z
Any other parametrisation with time is ruled out, for example, in our model, a change in star formation efficiency is ruled
out.
New parametrizationNew parametrization
Reincorporation time scaling with Mvir, due to the slow down of outgoing material caused by
dynamical friction.
Single SetSingle SetStrong ejection + no reincorporation set the low mass end at high-z
Strong reincorporation at later times produces the required build up for z<1
ResultsResults
Colors and SFRColors and SFR
The delayed reincorporation of
gas shifts star formation towards
lower redshift.
Dwarfs are bluer, have higher star formation
rates and younger ages.
ClusteringClustering
Dwarf galaxies form later, in higher mass halos that are less
cluster.
Galaxy formation physics, and not just cosmology, have a strong impact on galaxy clusterin.
ConclusionsConclusions
Extend the MCMC sampling to multiple redshifts for a wide range of observations, taking full advantage of the self-consistent evolution of galaxies
Pre-processing step that shows Guo11 parametrization to be nearly optimal at z=0. Reincorporation change required by the evolution of galaxy properties.
Simple adjustment to the model allows us to get a reasonable fit at all redshifts for the masses, K-band and B-band luminosities.
There is no longer an excess of dwarfs at high redshift
Evolution of the massive end is reproduced across cosmic time
Extended MCMC CapabilitiesExtended MCMC Capabilities
Observational constraints at multiple redshifts
Time-evolution of parameters (pre-processing step)
Stellar mass and luminosity functions constraints from z=3 to z=0 Takes full advantage of the self-consistent evolution of galaxies
If not needed, the current parametrisation is not ruled out by observationsIf needed, a different parametrisation is required (it rules out any others)
If a good fit can not be found, the current model is ruled out
M05 vs BC03
Gas
TB-AGB
TB-AGB + RHeB