Lightcones for Munich Galaxies Bruno Henriques

Outline 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

3 July 2016 Luminosity of a stellar population Stellar Population Synthesis Metallicity + Age +IMF Dust Model 3 Mass to Light

3 July Direct comparison to observed frame apparent magnitudes Test SED fitting / K-corrections Reliability of assumed star formation histories Test determinations of mass Full Emission Spectra

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) 3 July Test the impact of stellar populations modelling in the observed galaxy properties. K J iz (see also Henriques, Maraston, Monaco et al. (2010)) Different Stellar populations

3 July 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 )

Lightcones Comoving distance Redshifts - snapshots (z i +z i-1 )/2<z<(z i + zi+1 )/2 d com zizi znzn

Lightcones Mass to light obs_frame rest_frame only few replications, distant in redshift

Number 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

Rest-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.

Allsky Lightcones Selection in i AB < deg 2 - comparable to modern wide surveys

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 The numbers of massive galaxies are similar in model and data reflecting the slow evolution of these objects at later times

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 Boxes to cones Mass to light

Motivation 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.

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 Relations

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

TB-AGB TB-AGB + RHeB

SSP 3 July Van der Wel, Franx, Wuyts, et al Chandra Deep Field - South ACS+IRAC+J&H filters

Older then the Universe!Undetected in MIPS! 3 July Maraston, Daddi, Renzini, et al What are the implications for galaxy formation models?

MUSYC – Gawiser et al GOODS – Giavalisco et al Optical to mid-infrared data 3 July Marchesini 2009

CB07 3 July BC03 CB07 M05 Henriques, Maraston, Monaco, et al. (Astro-ph: )