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Lightcones for Munich Galaxies. Bruno Henriques. Outline. 1. Model to data - stellar populations and photometry. 2. Model to data - from snapshots to lightcones. 3. Results - pencil beams. 4. Results - all-sky cones. Mass to Light. Stellar Population Synthesis. Metallicity + Age +IMF.

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Presentation Transcript
outline

Outline

1. Model to data - stellar populations and photometry

2. Model to data - from snapshots to lightcones

3. Results - pencil beams

4. Results - all-sky cones

mass to light
Mass to Light

Stellar Population Synthesis

Metallicity + Age +IMF

Luminosity of a stellar population

Dust Model

4 September 2014

3

full emission spectra
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

4 September 2014

4

different stellar populations
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 also Henriques, Maraston, Monaco et al. (2010))

4 September 2014

5

slide6

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 )

z=5.7

z=1.4

From snapshot/box output

z=0

to lightcones

4 September 2014

6

lightcones

Lightcones

dcom

zn

Comoving distance

Redshifts - snapshots

zi

(zi+zi-1)/2<z<(zi+zi+1)/2

lightcones1

Lightcones

only few replications, distant in redshift

Mass to light

obs_frame

rest_frame

number counts zdist
Number Counts & Zdist

First tests can be performed directly in the observed frame with only few derivations applied to data.

bright near-by and faint distant galaxies

Intermediate redshifts dominated by faint objects

Henriques, White, Lemson, et al. 2012

rest frame colours and lfs
Rest-frame Colours and LFs

More informative tests can be done for rest-frame properties in order to obtain a comprehensive picture.

Optical-near-infrared color, separates passive from dust obscured galaxies

Large differences between stellar populations

allsky lightcones
Allsky Lightcones

Selection in iAB< 21.0 - 100deg2 - comparable to modern wide surveys

slide12
BOSS

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

stellar mass of massive ellipticals
Stellar 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

conclusions

Conclusions

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.

simulations to observations

Simulations to Observations

Mass to light

Boxes to cones

motivation

Motivation

Why use a phenomenological approach to study galaxy formation?

Because we should. The physics of galaxy formation are complex but observations suggest they must obey simple relations.

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.

scaling relations

Scaling Relations

Tully-Fisher

Many aspects of the physics that govern galaxy formation depend simply on galaxy and dark matter properties as indicated by observed scaling relations.

SFR-Gas

BlackHole-

BulgeMass

slide18

_________________________________________________

___________________________________________________________

Even if direct simulations reach high resolution and significant volumes they face the same problems due to un-resolved physics!

slide19

TB-AGB

TB-AGB + RHeB

slide20
SSP

Van der Wel, Franx, Wuyts, et al. 2006

Chandra Deep Field - South

ACS+IRAC+J&H filters

4 September 2014

20

slide21

Maraston, Daddi, Renzini, et al. 2006

Older then the Universe!

Undetected in MIPS!

What are the implications for galaxy formation models?

4 September 2014

21

marchesini 2009
Marchesini 2009

Optical to mid-infrared data

GOODS – Giavalisco et al. 2004

MUSYC – Gawiser et al. 2006

4 September 2014

22

slide23
CB07

M05

CB07

BC03

Henriques, Maraston, Monaco, et al. (Astro-ph: 1009.1392)

4 September 2014

23