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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.
Simon White, Peter Thomas
Raul Angulo, Qi Guo, Gerard Lemson, Volker Springel
AGN feedback model (suppression of cooling)
De Lucia & Blaizot 2007
SN feedback model - reheating + ejection + reincorporation
Guo et al. 2011
different supernova feedback (increased efficiency)
Henriques et al. 2011, 2012
different stellar populations
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
Henriques B., Thomas P., MNRAS, 2010
Complex galaxy formation physics
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
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.
Reincorporation time scaling with Mvir, due to the slow down of outgoing material caused by dynamical friction.
Strong reincorporation at later times produces the required build up for z<1
The delayed reincorporation of gas shifts star formation towards lower redshift.
Dwarfs are bluer, have higher star formation rates and younger ages.
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.
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
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
TB-AGB + RHeB