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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.

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slide1

A self consistent model of galaxy formation across cosmic time

Bruno Henriques

Simon White, Peter Thomas

Raul Angulo, Qi Guo, Gerard Lemson, Volker Springel

the munich model

Croton et al. 2006

The Munich Model

AGN feedback model (suppression of cooling)

De Lucia & Blaizot 2007

dust model

SN feedback model - reheating + ejection + reincorporation

Guo et al. 2011

different supernova feedback (increased efficiency)

Merger treatment

Henriques et al. 2011, 2012

different stellar populations

lightcones

Lightcones

Henriques B., White S., Lemson G., Thomas P., Guo Q., Marleau D., Overzier R., 2012, MNRAS

Extended photometric coverage

Multiple Stellar Populations

Pencil Beams + All Sky

http://www.mpa-garching.mpg.de

mcmc parameter sampling

Henriques B., Thomas P., Oliver S., Roseboom I., MNRAS, 2009

MCMC Parameter Sampling

Henriques B., Thomas P., MNRAS, 2010

Complex galaxy formation physics

Semi-analytic modelling

MCMC

Large Volume

Across Cosmic Time

Constrain the model at multiple redshifts

Choose observational constraints

Stellar Mass Function, K-band & B-band Luminosity Functions

Choose parameters to sample

Star formation, SN feedback, AGN feedback efficiency, Metals yield

time varying parameters

Time varying parameters

A clear & unique change was revealed by the pre-processing step

Reincorporation 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 parametrization

New parametrization

Reincorporation time scaling with Mvir, due to the slow down of outgoing material caused by dynamical friction.

single set

Strong ejection + no reincorporation set the low mass end at high-z

Single Set

Strong reincorporation at later times produces the required build up for z<1

colors and sfr

Colors and SFR

The delayed reincorporation of gas shifts star formation towards lower redshift.

Dwarfs are bluer, have higher star formation rates and younger ages.

clustering

Clustering

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.

conclusions

Conclusions

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 capabilities

Extended MCMC Capabilities

Observational constraints at multiple redshifts

Stellar mass and luminosity functions constraints from z=3 to z=0

Takes full advantage of the self-consistent evolution of galaxies

Time-evolution of parameters (pre-processing step)

If not needed, the current parametrisation is not ruled out by observations

If 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

slide19

TB-AGB

TB-AGB + RHeB