Lightcones for Munich Galaxies
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Transcript of Lightcones for Munich Galaxies
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Lightcones for Munich Galaxies
Bruno Henriques
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OutlineOutline
1. Model to data - stellar populations and photometry
2. Model to data - from snapshots to lightcones
4. Results - all-sky cones
3. Results - pencil beams
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April 21, 2023
Luminosity of a stellar population
Stellar Population Synthesis
Metallicity + Age +IMF
Dust Model
3
€
Aλ = −2.5log1− exp−τ λ secθ
τ λ secθ
⎛
⎝ ⎜
⎞
⎠ ⎟
Mass to LightMass to Light
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Direct comparison to observed frame apparent magnitudesTest SED fitting / K-corrections
Reliability of assumed star formation histories
Test determinations of mass
Full Emission SpectraFull Emission Spectra
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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)
In past evolutionary population synthesis codes,
the K-band was mostly determined by old
populations (e.g. Bruzual & Charlot 2003, PEGASE,
Starburst99)
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Test the impact of stellar populations modelling in the observed galaxy properties.
K
Ji z
(see also Henriques, Maraston, Monaco et al. (2010))
Different Stellar populationsDifferent Stellar populations
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z=0
z=5.7
z=1.4
The semi-analytic is built on top of the dark matter distribution and has outputs only at given snapshots.
to lightcones
From snapshot/box output
(despite galaxy properties being computed in smaller steps ~ 6 Myr )
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LightconesLightcones
Comoving distance
Redshifts - snapshots
(zi+zi-1)/2<z<(zi+zi+1)/2
dcom
zi
zn
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LightconesLightcones
Mass to light
obs_frame
rest_frame
only few replications, distant in redshift
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Number Counts & ZdistNumber Counts & Zdist
bright near-by and faint distant galaxies
Intermediate redshifts dominated by faint
objects
First tests can be performed directly in the observed frame with only few derivations applied to data.
Henriques, White, Lemson, et al. 2012
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Rest-frame Colours and LFsRest-frame Colours and LFs
Optical-near-infrared color, separates passive
from dust obscured galaxies
Large differences
between stellar populations
More informative tests can be done for rest-frame properties in order to obtain a comprehensive picture.
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Allsky LightconesAllsky Lightcones
Selection in iAB< 21.0 - 100deg2 - comparable to modern wide surveys
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BOSSBOSS
observed-frame color selection criteria can be
matched
The model can be used to analyze the selection in
terms of fundamental quantities Maraston, Pforr, Henriques, et al. 2012
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Stellar Mass of Massive EllipticalsStellar Mass of Massive Ellipticals
The numbers of massive galaxies are similar in model and data reflecting the slow evolution of these objects at
later times
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ConclusionsConclusions
Narrow and wide lightcones constructed to match modern surveys.
Wide photometric coverage that can be used to test derivation of fundamental quantities from observations.
Large range of properties can be closely compared with available data to identify possible tensions in theory.
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Simulations to Observations Simulations to Observations
Boxes to cones
Mass to light
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MotivationMotivation
Because we should. The physics of galaxy formation are complex but observations suggest they must obey simple relations.
Why use a phenomenological approach to study galaxy formation?
Still, we do not have a good understanding and cannot work from first principles, so models must be
observationally based.
Fast method to compute the evolution of the galaxy population across cosmic time for samples as large as modern surveys.
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Many aspects of the physics that govern galaxy formation depend simply on galaxy and dark matter properties as indicated by
observed scaling relations.
Tully-Fisher
BlackHole-BulgeMass
SFR-Gas
Scaling RelationsScaling Relations
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Even if direct simulations reach high resolution and significant volumes they face the same problems due
to un-resolved physics!
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TB-AGB
TB-AGB + RHeB
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SSP
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Van der Wel, Franx, Wuyts, et al. 2006
Chandra Deep Field - South
ACS+IRAC+J&H filters
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Older then the Universe! Undetected in MIPS!
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Maraston, Daddi, Renzini, et al. 2006
What are the implications for galaxy formation models?
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MUSYC – Gawiser et al. 2006GOODS – Giavalisco et al. 2004
Optical to mid-infrared data
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Marchesini 2009Marchesini 2009
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CB07
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BC03
CB07
M05
Henriques, Maraston, Monaco, et al. (Astro-ph: 1009.1392)