The Evolution of the Luminosity Function in Semi-Analytic models

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The Evolution of the Luminosity Function in
Semi-Analytic models
Bruno Henriques

• Simon White, Gerard Lemson, Peter Thomas,
• Roderick Overzier, Qi Guo, Claudia Maraston

Henriques, Maraston, Monaco, et al., Astro-ph
1009.1392
Henriques, et al., 2011, in prep.
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Guo et al. 2010
Stars
Reincorporation
Hot Gas
Reheating
Cooling
Stars
Ejected Gas
Star Formation
Recycling
Cold Gas
Ejection
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Supernovae Feedback
Cold Gas Reheating
Energy Released by a Supernovae
Gas Reincorporation
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Mergers
0
0
1
2
0
0
2
1
1
2
0
2
3
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1 Two isolated Galaxies
2 Gas Striping and Disruption on type 1
3 Merger Clock and Stellar Disruption triggered
on type 2, no gas left
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Mass to Light
Stellar Population Synthesis
Knowing Metallicity Age IMF
Luminosity of a given mass of stars
Dust Model
ISM Birth Clouds
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The semi-analytic is built on top of the dark
matter distribution and has outputs only at
given snapshots.
(despite galaxy properties being computed in
smaller steps 6 Myr )
z5.7
z1.4
From snapshot/box output
z0
to lightcones
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Full Emission Spectra
Direct comparison to observed frame apparent
magnitudes
Test SED fitting / K-corrections
Reliability of assumed star formation histories
Test determinations of mass
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Different Stellar Populations
Test the impact of stellar populations modelling
in the observed galaxy properties.
In past evolutionary population synthesis codes,
the K-band was mostly determined by old
populations (e.g. Bruzual Charlot 2003, PEGASE,
Starburst99)
The inclusion of the TP-AGB phase means that
intermediate-age populations will contribute
significantly to the near infra-red emission from
galaxies (Marasto 2005, Charlot Bruzual 2007)
i
z
J
K
(see Henriques et al. (2010), Tonini et al.
(2008, 2009), Fontanot Monaco 2010)
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10x
5x
0.5
1.0
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M05
CB07
BC03
Henriques, Maraston, Monaco, et al. (Astro-ph
1009.1392)
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Redshift Distribution
K-band selected Galaxies
Guo10 M05
Guo10 BC03
From previous plot
zlt1.0 -
two stellar populations are identical
z1.5 -
bright galaxies are brighter fro M05
zgt2.0 -
all galaxies are brighter for M05
1.11
0.74
0.55
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Redshift Distribution
8.0µm-band selected Galaxies
Around z2.0 the observed 8.0µm starts receiving
light from the JHK region
TP-AGB stars significantly increase emission
J
K
4.0
2.67
2.0
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TP-AGB stars
re-emission by dust
zlt0.75
zgt0.75
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Number Counts in Redshift Intervals
K-band
At low z galaxies are dominated by intermediate
to old stellar populations M05 and BC03
converge.
At high z the observed K-band receives flux from
rest-frame optical where M05 and BC03 also agree.
At low z (rest-frame 8.0µm), BC03 gives brighter
galaxies than M05.
8.0µm
At high z (rest-frame K-band), the emission from
TP-AGB stars means that M05 gives higher number
counts
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The Ages of Galaxies
Light Weighted Ages
Mass Weighted Ages
BC03
M05
Average!!!
M05
TP-AGB
Henriques, Maraston, Monaco, et al. (Astro-ph
1009.1392)
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Summary
Light cones will soon be available
at http//gavo.mpa-garching.mpg.de/MyMillennium3/

Wide range of filters and multiple stellar
populations for observed frame magnitudes
self-consistent model of galaxy evolution.
The model matches the mass and luminosity
evolution of galaxies over the cosmic history
reasonably well.
Understand the interplay of different physics at
different epochs
Test Evolutionary Populations Synthesis models,
SED fitting, K-corrections, mass determinations.
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10x
5x
0.5
1.0
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Van der Wel, Franx, Wuyts, et al. 2006
Chandra Deep Field - South
ACSIRACJH filters
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Maraston, Daddi, Renzini, et al. 2006
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The Stellar Mass Function Marchesini et al. 2009
Optical to mid-infrared data
Goods Giavalisco et al. 2004
Musyc Gawiser et al. 2006
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K-band Luminosity Function
The contours follow the MCMC sampling in
parameter space
The colours represent the maximum likelihood
projected along the hidden dimensions
Less gas available to form stars in dwarfs
Higher ejection
Lower reincorporation
Lower virial velocity cut off
Constant amount of cold gas available
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Bulge Black Hole Mass
The maximum likelihood region is incompatible
with previous test
There is a region with lower likelihood that is
bigger, so more likely in a Bayesian sense
10 July, 2014
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3 - Tidal Disruption
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Original De Lucia 2007 with Disruption
K-band Luminocity Function
Fraction of Red Galaxies
Metallicity
ICL fraction
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Likelihood Distribution
Model Likelihood from 0.037 to 0.15 !!!
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Predictions for the Best Fit with Disruption
K-band LF
Metallicity
ICL
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Predictions for the Best Fit with Disruption
Best Fit Model with Disruption
Observations
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