1 / 43

The Build-up of the Red Sequence at z<1.3

Masayuki Tanaka ( ESO, not STScI ) + Taddy Kodama (NAOJ). The Build-up of the Red Sequence at z<1.3. galaxies come in two flavours. red. blue. bright. faint. Conclusion.

cady
Download Presentation

The Build-up of the Red Sequence at z<1.3

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. Masayuki Tanaka (ESO, not STScI) + Taddy Kodama (NAOJ) The Build-up of the Red Sequence at z<1.3

  2. galaxies come in two flavours... red blue bright faint

  3. Conclusion • The bright end of the red sequence appears first and it extends to fainter mags., and the build-up of the red sequence is ‘delayed’ in low density environments. • Galaxy-galaxy interactions may be a primary driver of this build-up. Environment Mass

  4. 0 – Introduction 1 – PISCES project 2 – Large-scale structures around distant clusters 3 – Build-up of the red sequence at z<1.3 4 – Spectral Diagnostics 5 – Summary Outline of this talk

  5. outline 0 – introduction 1 – pisces prject 2 – large-scale structures in the distant universe 3 – the build-up of the colour-magnitude relation 4 – spectral diagnostics 5 – summary large-scale structure in the local universe 0 – Introduction

  6. Galaxies in low-density environments... NGC5668

  7. Galaxies in high-density environments... Coma cluster

  8. Clusters at higher redshifts CL0016 at z=0.55 taken with WFPC2 on HST

  9. ? ? ? ? ? Clusters at higher redshifts Cluster outskirts and surrounding clumps/filaments remain unexplored. Also, faint galaxies at high redshifts have not been extensively examined yet. We carried out a wide and deep cluster survey. CL0016 at z=0.55 taken with WFPC2 on HST

  10. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – summary Pi·sces[pahy-seez, pis-eez] -n.   1. A constellation in the equatorial region of the Northern Hemisphere near Aries and Pegasus. Also called Fishes. 2. a. The 12th sign of the zodiac in astrology. Also called Fishes. b. pl.Pisces One who is born under this sign. 3. A deep, wide-field survey of galaxy clusters at 0.4<z<1.3. 1 – PISCES project

  11. PISCES project (in A&A abstract format) Aims: Methods: Results: Conclusions: Our goal is to quantify galaxy properties as functions of environment, mass, and time and understand how and when the environmental dependence of galaxy properties is established. We carry out a systematic, deep (~M*+4), wide-field (30’x30’), optical-nearIR imaging + spectroscopic survey of distant clusters. Some of our recent results are presented in this talk. Our survey is not finished yet, so…..we will see. For details, see Kodama+ 2005 PASJ, 57, 309

  12. ACS/HST CL0016+16 at z=0.55 BVRiz photometry + 150 spec. objects

  13. RXJ1716 at z=0.81 VRizK, H photometry + AKARI IR photometry

  14. RXJ0152-13 at z=0.83 VRizK photometry + 200 spec. objects

  15. RDCSJ0910 at z=1.1 VRizK photometry + some spec. objects

  16. RDCSJ1252 at z=1.24 VRizK photometry + some spec. objects

  17. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – summary Large-scale structure in the local Universe 2 – Large-scale structures around distant clusters

  18. ~70,700 objects ~3,600 objects Large-Scale Structures at z=0.55 CL0016 at z=0.55 (Tanaka+ MNRAS, 2007, 379, 1546)‏ 0.48<zphot<0.60

  19. cluster redshift Large-Scale Structures at z=0.55 ~3,600 objects CL0016 at z=0.55 (Tanaka+ MNRAS, 2007, 379, 1546)‏ 0.48<zphot<0.60

  20. red galaxies Large-Scale Structures at z=0.83 bluegalaxies RXJ0153 at z=0.83 Tanaka+ 2006 MNRAS, 365, 1392 0.76<zphot<0.88

  21. Redshift distribution of spec. galaxies cluster redshift RXJ0153 at z=0.83 Tanaka+ 2006 MNRAS, 365, 1392 0.76<zphot<0.88

  22. spec. objects at 0.82<z<0.85 Large-Scale Structures at z=0.83 z=0.837 z=0.844 z=0.839 z=0.844 z=0.842 z=0.782 z=0.745 z=0.835 0.76<zphot<0.88 RXJ0153 at z=0.83

  23. Large-Scale Structures at z=1.1 RDCSJ0910 at z=1.1

  24. Large-Scale Structures at z=1.2 RDCSJ1252 at z=1.24 Tanaka+ 2007a MNRAS, 377, 1206 1.17<zphot<1.31

  25. Close-up views of the clumps

  26. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – summary galaxies come in two flavours... red blue bright faint 3 – Build-up of the red sequence

  27. Cluster / Group / Field Environments For details of the definition, refer to Tanaka+2005 MNRAS

  28. red blue Colour-Magnitude Diagrams at z<0.83 bright faint Tanaka+ 2005 MNRAS, 362, 268

  29. Evolution of Fraction of red galaxies

  30. Color-Magnitude Diagrams at z=0.81 RXJ1716 cluster surrounding field Koyama et al. 2007 MNRAS submitted.

  31. Colour-Magnitude Diagrams at z=1.1 (preliminary!) RDCSJ0910 at z=1.1

  32. Colour-Magnitude Diagrams at z=1.2 RDCSJ1252 at z=1.24 18 20 22 24 Ks 18 20 22 24 26 Ks Main Cluster Lidman et al. 2004 A&A Composite Group Tanaka et al. 2007a MNRAS

  33. Colour-Magnitude Diagrams at z=1.2 1 – The bright-end of the red sequence appears first and the faint end appears later. 2 – The build-up of the red sequence is ‘delayed’ in low-density environments. Main Cluster Lidman et al. 2004 A&A Composite Clump Tanaka et al. 2007a MNRAS

  34. z=1.24 z=1.1 z=0.83 z=0.81 z=0.55 z=0 : RDCSJ1252 : RDCSJ0910 : RXJ0152 : RXJ1716 : CL0016 : Sloan Survey outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – summary 4 – Spectral Diagnostics

  35. composite spectra of red galaxies at z~0.8

  36. composite spectra of red galaxies at z~0.5

  37. composite spectra of red galaxies at z=0

  38. Spectral Diagnostics ...for details see Tanaka+07 MNRAS, 379, 1546

  39. Spectral Diagnostics No clear CMRCMR at bright endTight CMR EW[OII]=14AEW[OII]=4ANo [OII] No strong Hd Strong Hd No strong Hd CMR at bright endTight CMR Tight CMR EW[OII]=4ANo [OII] No [OII] Strong Hd No strong Hd No strong Hd Redshift Field Group Cluster z~0.8 z~0.5 z~0 Red galaxies are consistent with passive evolution no [OII], no strong Hd The strong Hd is suggestive of a sharp decline in star formation rates.

  40. Fast Facts of Environmental Mechanisms mechanisms star formation effective env. • galaxy-galaxy interactions <<1Gyr field/group • harassment ? cluster • ram-pressure stripping <<1Gyr cluster • strangulation ~1Gyr group/cluster

  41. Fast Facts of Environmental Mechanisms mechanisms star formation effective env. • galaxy-galaxy interactions <<1Gyr field/group • harassment ? cluster • ram-pressure stripping <<1Gyr cluster • strangulation ~1Gyr group/cluster For more detailed discussions, see Tanaka+ 2007 MNRAS, 379, 1546

  42. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – summary Ein Prosit, ein Prosit der Gemütlichkeit! Ein Prosit, ein Prosit der Gemütlichkeit! 5 – Summary

  43. Summary • Galaxies follow the 'environment-dependent down-sizing' evolution. • Galaxy-galaxy interactions may be the driving process of this evolution. Environment Mass

More Related