1 / 12

luminosity & color of galaxies in clusters

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

lorin
Download Presentation

luminosity & color of galaxies in clusters

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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. 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 glcw8

  4. 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 glcw8

  5. sdss clusters • > 7300 deg2 of ugriz photometric data • maxBCGclusters • red sequence matched filter (koester et al. 2007a,b) • z ≤ 0.3; Dz ~ 0.01 • mass proxy: N200 13,823 systems with N200≥ 10 and z ≤ 0.3 • 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.) glcw8

  6. galaxy properties BCG or not? radial distance luminosity color cluster properties richness total luminosity redshift BCG properties • luminosity function as f (richness, color) • blue fraction as f (richness, redshift, radius, luminosity) method • measure background-subtracted, k-corrected distribution of galaxies associated with clusters, binned by cluster& galaxy properties • comparison with ADDGALs simulations (wechsler et al.) glcw8

  7. conditional luminosity function (L|M): important ingredient for understanding how galaxies populate halos glcw8

  8. color distribution red galaxies; blue galaxies all galaxies 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 glcw8

  9. blue fraction within r200 provides constraints on models of galaxy populations and evolution in clusters glcw8

  10. blue fraction within r200 provides constraints on models of galaxy populations and evolution in clusters glcw8

  11. blue fraction, in more detail radial trend luminosity trend glcw8

  12. summary with sdss data and galaxy-populated simulations, we investigate the properties of cluster galaxies, including: • blue fraction as a function of cluster mass, redshift, radius and magnitude • conditional luminosity function for all, red & blue galaxies see hansen et al., arXiv:0706.soon glcw8

More Related