1. ASIAA Research Highlights and Prospects with HSC Keiichi Umetsu, ASIAA SAC HSC Science Workshop 29.01.20078

2. Outline 1.Introduction – Major ASIAA Projects 2.Highlights and Prospects with HSC – AMiBA SZE Interferometer – Weak Lensing (HSC WLWG collaboration) – Search for Dust in the ICM – Search for High-z Galaxies – (Galaxy Pair Statistics – talk by Li-Hwai) 3. Summary

3. 1. Major ASIAA Projects (1994-2008) SMA : Array Completed, Upgrading AMiBA : 7-element Dedicated, 13-element underway TIARA; SIS Junction : 230, 345, 400, 690, 900 GHz TAOS : 4 Telescopes Working; Moving? CFD-MHD : 2-D Hydro Codes WIRCam : Science operation started ALMA-J : FEIC started; band-10 ALMA-NA: Funded, Negotiating Hyper Suprime Cam: Proposing ASMAB: on schedule to finish 2008 SAO NTU NTHU NCU ASIM CFHT NAOJ NRAO NAOJ NTU (NAOJ, PMO) (SAO, Yonsei)

4. 2. ASIAA Research Highlights and Prospects with HSC

5. 2-1. Scam/HSC + AMiBA SZE ASIAA & NTU (Taiwan) Collaboration

6. AMiBA SZE Cluster Observations 6 nearby clusters detected with the 7-element AMiBA by the AMiBA team (April-August 2007) SZ Decrement = -150 ~ -300 mJy (@94GHz)

7. Synergy with S-Cam and HSC: SZE and WL Probing Cluster Physics z=0.228 z=0.183 Mass map from Subaru/Scam data z=0.091 z=0.224

8. 2-2. Cluster Weak Lensing for Probing DM Halo Profiles References Broadhurst, Takada, Umetsu et al. 2005 (ApJL) Umetsu & Broadhurst 2007 (ApJ, submitted) Umetsu, Medezinski, Broadhurst, & Okabe 2008 in prep.

9. Strong(est) Lensing Cluster A1689 (z=0.18) Mass ( ~ DM) Cluster Galaxies Relaxed, massive cluster with large  E =45” (zs=1): 5.5Mpc r=10-2000 (r vir ) kpc/h Umetsu & Broadhurst 2007 Subaru Subaru+ACS Surprisingly high concentration, difficult to accommodate with LCDM (c vir ~5) NFW fit NFW fit: M vir =2.1x10 15 M sun, C vir =13

10. DM Ring Cluster CL0024 (z=0.4) NFW fit NFW fit: M vir =1.1x10 15 M sun, C vir =14 Strong lensing cluster with large  E =32” (zs=1.6): Cluster Galaxy density map, with mass contours overlayed Observed large  E, implying large C vir, challenging for LCDM Umetsu et al. 2008 in prep. EE

11. Prospects for HSC Attaining a larger sample of clusters from the HSC survey, improving up on the statistical constraints, providing a stringent test of LCDM on small scales (~1Mpc) Much wider FoV (1.5deg) of HSC, allowing to map out “very” nearby clusters out to virial radii e.g., 1 HSC FoV  ~ 2.5Mpc/h (>2Rvir) @ z=0.07 cf., S-Cam WL study of a z=0.05 cluster (Okabe & Umetsu 2008)

12. 2.3 Cross Correlating the Cosmic Shear and Galaxy Density Fields for Probing the Statistical Matter-Galaxy Relation The HSC WLWG team

13. Bias Parameters HSC Survey HSC Survey (1000-3000 deg^2): - Deep I-band imaging for cosmic shear statistics - Multicolor imaging for deriving photo-z of individual (fore/back) galaxies Basic quantities on the statistical matter-galaxy relation available from the HSC survey Feasibility study on the detectability of the r-parameter cf. Schneider 1998, Fan 2003; Hoekstra+ 2002 (RCS+VIRMOS), Sheldon+ 2004 (SDSS), Simon+ 2007 (GaBoDS)

14. Forecasts (1): Detection of r-parameter Large scale Small scale Total detection S/N HSC Deep DES HSC Shallow By Nishioka (ASIAA)

15. Forecasts (2): Superior HSC Sensitivity in Higher Redshifts Sensitivity in z-space (  ap =10’) Redshift HSC Shallow HSC Deep DES By Nishioka (ASIAA)

16. 2.4 Search for Dust in the ICM Reference: Muller, Wu, Hsieh et al. 2008 (ApJ, in press) Foreground clusters Galaxies behind the clusters Reference background

17. Application to the RCS Survey (33deg^2) Method: Background color statistics w/ CFHT RCS BVRz’ data (33.6deg^2) - Statistical sample of 458 clusters @ z < 0.5 - 90,000 background galaxies @ 0.5 < z phot < 0.8 with photo-z accuracy: dz phot /(1+z phot ) < 0.06 Results: For galaxies behind clusters… = 0.005 +- 0.008 = 0.000 +- 0.008 = 0.004 +- 0.010 within 1 R 200 NO signature for DUST in the ICM Red: behind cluster Blue: reference

18. Future Prospects: How to Improve? wider - More clusters to allow a sample selection based on cluster properties: mass, X-ray, merger, etc..  wider more filters - More reliable photo-z measurements  more filters On-going CFHT RCS2 survey: wider sky coverage 30 deg2  1000 deg2 Future HSC survey: deeper, wider sky coverage with more accurate photo-z measurements

19. 2.5 Ongoing CFHT Project Bau-Ching Hsieh, Wei-Hao Wang, et al. (CFHT S07B) Goal Goal: Search for galaxies at z > 7 Field Field: Extended Chandra-Deep Field South (ECDFS) Observations Observations: CFHT/WIRCam “J” (24.9 ABmag, seeing ~0.7”) Sky area Sky area: ~ 500 arcmin^2 Data from other bands Data from other bands: GEMS ACS: V (28.4), z’ (27.1) SIMPLE (Spitzer): 3.6um (25.1) Criteria for candidates Criteria for candidates: z'-J>2.0, -0.5 < J-3.6um < 1.2 A combination of matched depths, and “deep z’-imaging” is important to make sure z’- dropout

20. Summary Targeted AMiBA SZE follow up observations for the HSC cluster survey Cluster Weak Lensing Weak Lensing vs. Galaxy Cross Correlation Dust in the ICM High-z Galaxies

21. HSC Survey Parameters 3000deg^2 1000deg^2 400deg^2 4-band imaging (griz), including the overhead time