Wide-field Imaging + Spectroscopic Survey of Distant Clusters

1. Masayuki Tanaka (ESO) Wide-field Imaging + Spectroscopic Survey of Distant Clusters

2. 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 – From the Cradle to the Grave 6 – Summary Outline of this talk

3. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – from the cradle to the grave 6 – 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

4. 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

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

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

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

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

9. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – from the cradle to the grave 6 – summary Large-scale structure in the local Universe 2 – Large-scale structures around distant clusters

10. ~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

11. 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

12. 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

13. 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

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

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

16. Close-up views of the clumps

17. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – from the cradle to the grave 6 – summary galaxies come in two flavours... red blue bright faint 3 – Build-up of the red sequence

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

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

20. 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

21. 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

22. 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 – from the cradle to the grave 6 – summary 4 – Spectral Diagnostics

23. composite spectra of red galaxies at z~0.8

24. composite spectra of red galaxies at z~0.5

25. composite spectra of red galaxies at z=0

26. 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.

27. 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

28. 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

29. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – from the cradle to the grave 6 – summary 5 – From the Cradle to the Grave

30. Clusters at z=0 are filled with red and dead galaxies. Clusters at High/Low Redshifts Proto-clusters at z=5.7 can be traced by young, forming galaxies (Ouchi+ '05).

31. Galaxy clusters change their nature from the cradle to the grave... Key question : “How and when do they change?”

32. PKS1138 cluster at z=2.16 (Kurk+ '04): Red and blue gals co-exit? Key epoch: redshift around 2 Probing z~2 clusters would give us a hint for the origin of the environmental dependence of galaxy properties. RDCSJ1252 cluster at z=1.24 (Tanaka+ '07): Red gals have already become the dominant population.

33. outline 1 – pisces project 2 – large-scale structures around distant clusters 3 – the build-up of the red sequence 4 – spectral diagnostics 5 – from the cradle to the grave 6 – summary Oktoberfest in Munich 6 – Summary

34. Summary • Galaxies follow the 'environment-dependent down-sizing' evolution. • Galaxy-galaxy interactions may be the driving process of this evolution. • Probing clusters at z~2 with next generation surveys would be interesting. Environment Mass