1. luminosity & color of galaxies in clusters sarah m. hansen university of chicago with erin s. sheldon (nyu) risa h. wechsler (stanford)

2. astrophysics with eV photons sarah m. hansen university of chicago with erin s. sheldon (nyu) risa h. wechsler (stanford)

3. sarah m. hansenglcw8 outline motivation sdss data & cluster sample characterizing the galaxy population luminosity function: dependence on cluster mass, galaxy color blue fraction: dependence on cluster mass, redshift, galaxy luminosity & cluster-centric radius

4. sarah m. hansenglcw8 motivation clusters as cosmological probes how to connect dark and luminous matter? how to connect stars and gas? clusters as galaxy evolution laboratories what’s happened to form such a particular cluster galaxy population? for upcoming large surveys, want to understand these details better

5. sarah m. hansenglcw8 sdss clusters > 7300 deg 2 of ugriz photometric data maxBCG clusters red sequence matched filter (koester et al. 2007a,b) z ≤ 0.3;  z ~ 0.01 mass proxy: N 200 mass - richness scaling mass function & cosmological params (rozo et al. 2007) velocity dispersion (becker et al. 2007) lensing (sheldon et al.; johnston et al.) x-ray (rykoff et al.) 13,823 systems with N 200 ≥ 10 and z ≤ 0.3

6. sarah m. hansenglcw8 method measure background-subtracted, k-corrected distribution of galaxies associated with clusters, binned by cluster & galaxy properties luminosity function as f (richness, color) blue fraction as f (richness, redshift, radius, luminosity) galaxy properties BCG or not? radial distance luminosity color cluster properties richness total luminosity redshift BCG properties comparison with ADDGALs simulations (wechsler et al.)

7. sarah m. hansenglcw8 conditional luminosity function  (L|M): important ingredient for understanding how galaxies populate halos

8. sarah m. hansenglcw8 radial color trend is due to changing number of galaxies on the red sequence vs in the blue cloud  blue fraction is the info you need color distribution red galaxies; blue galaxies all galaxies

9. sarah m. hansenglcw8 blue fraction within r 200 provides constraints on models of galaxy populations and evolution in clusters

10. sarah m. hansenglcw8 blue fraction within r 200 provides constraints on models of galaxy populations and evolution in clusters

11. sarah m. hansenglcw8 blue fraction, in more detail radial trend luminosity trend

12. sarah m. hansenglcw8 summary blue fraction as a function of cluster mass, redshift, radius and magnitude conditional luminosity function for all, red & blue galaxies with sdss data and galaxy-populated simulations, we investigate the properties of cluster galaxies, including: see hansen et al., arXiv:0706.soon