1 / 19

Color Magnitude Relations of early type galaxies in galaxy clusters

SDSS KSG Workshop 2007. Color Magnitude Relations of early type galaxies in galaxy clusters. 20 Feb 2007 Taehyun Kim , Narae Hwang, & Myung Gyoon Lee. Department of Physics and Astronomy, Seoul National University. Abell 168, z=0.045. Out of the blue line, they are not member galaxies.

dinah
Download Presentation

Color Magnitude Relations of early type galaxies in galaxy 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. SDSS KSG Workshop 2007 Color Magnitude Relations of early type galaxies in galaxy clusters 20 Feb 2007 Taehyun Kim , Narae Hwang, & Myung Gyoon Lee Department of Physics and Astronomy, Seoul National University

  2. Abell 168, z=0.045

  3. Out of the blue line, they are not member galaxies Mpc Within the blue curved line, they are clusters member galaxies Select Member Galaxies Using redshift& number density distribution, we can select members

  4. 0.2 0.8r r 1.25r Early type galaxies • We chose early type galaxies as follows, (Bernardi et al, 2003) • Photometric parameter (frac_dev) > 0.8 • Spectral classification parameter (eclass) < -0.06 • For magnitudes & colors, we took Petrosian magnitude

  5. Color- Magnitude Diagram Red Sequence galaxies

  6. Abell clusters in DR6 , z<0.2 • Member • Early type

  7. 193/223 Clusters containing>5 ETGs

  8. Slope ofColor-Magnitude relation

  9. Early type member gals: 10~30 Early type member gals: 50~80 Early type member gals: 30~50 CMR slopes of clusters Rich Clusters (GR4) shows slope evolution in (u-r),(g-r),(r-i)

  10. Early type member gals: 10~30 CMR slopes of clusters

  11. 0.65 0.92 0.59 1.22 Zero points ofCMR at r=18~colors of galaxies in clusters

  12. CMR zero points of 193 clustersat r=18 ZPs (g-r, r-i colors at r=18) of cluster CMR increase with z!

  13. Cluster member galaxies including all types of galaxies in SDSS DR5, Here, only foreground reddenning was corrected Hwang et al. (2007, ApJS submitted)

  14. We can estimate ‘z’ of cluster red sequence galaxies with zero points, slopes of our results Hwang et al.(2007, ApJS submitted)

  15. Hwang et al. (2007, ApJS submitted) Applying to find galaxy clusters; Newly found Galaxy clusters, ‘NEPX1’,using CFHT on NEP Field

  16. Colors - Redshift (g-r) = C0 + C1*redshift

  17. A1656 A2199 A85 (Merging) A2142 (Merging) A2151, A2152 (Hercules Supercluster) CMR scatterof 193 clusters

  18. Summary • Rich Clusters shows slope evolution in (u-r)0,(g-r)0,(r-i)0 . • ZPs (g-r, r-i colors at r=18) of cluster CMR increase with z! • Colors ( g-r, r-i) & mean slope of CMR can be used to estimate redshift of red-sequence galaxies in clusters which do not have spectroscopic data • 6 Rich clusters (GR4) shows similar scatter around CMR

  19. Thank you very much  Coma cluster (z=0.0231)

More Related