1 / 21

ASIAA Research Highlights and Prospects with HSC

Explore the major ASIAA projects and highlights with HSC, including AMiBA SZE Interferometer, Weak Lensing, Dust in ICM, and High-z Galaxies. Delve into the research prospects and latest findings.

lestere
Download Presentation

ASIAA Research Highlights and Prospects with HSC

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

  2. Outline • Introduction – Major ASIAA Projects • 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 SuprimeCam: 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 SZ Decrement = -150 ~ -300 mJy (@94GHz) 6 nearby clusters detected with the 7-element AMiBA by the AMiBA team (April-August 2007)

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

  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) Cluster Galaxies Mass (~DM) Relaxed, massive cluster with large qE=45” (zs=1): NFW fit: Mvir=2.1x1015Msun, Cvir=13 5.5Mpc Umetsu & Broadhurst 2007 Surprisingly high concentration, difficult to accommodate with LCDM (cvir~5) r=10-2000 (rvir) kpc/h Subaru Subaru+ACS

  10. DM Ring Cluster CL0024 (z=0.4) Strong lensing cluster with large qE=32” (zs=1.6): Cluster Galaxy density map, with mass contours overlayed NFW fit: Mvir=1.1x1015Msun, Cvir=14 qE Observed large qE, implying large Cvir, challenging for LCDM Umetsu et al. 2008 in prep.

  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(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 cf. Schneider 1998, Fan 2003; Hoekstra+ 2002 (RCS+VIRMOS), Sheldon+ 2004 (SDSS), Simon+ 2007 (GaBoDS) Feasibility study on the detectability of the r-parameter

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

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

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

  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 < zphot < 0.8 with photo-z accuracy: dzphot/(1+zphot) < 0.06 Results: For galaxies behind clusters… <E(B-R)> = 0.005 +- 0.008 <E(V-Z)> = 0.000 +- 0.008 <Av> = 0.004 +- 0.010 within 1 R200 NO signature for DUST in the ICM Red: behind cluster Blue: reference

  18. Future Prospects: How to Improve? • - More clusters to allow a sample selection based on cluster properties: mass, X-ray, merger, etc..  wider • - 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: Search for galaxies at z > 7 • Field: Extended Chandra-Deep Field South (ECDFS) • Observations: CFHT/WIRCam “J” (24.9 ABmag, seeing ~0.7”) • Sky area: ~ 500 arcmin^2 • Data from other bands: GEMS ACS: V (28.4), z’ (27.1) SIMPLE (Spitzer): 3.6um (25.1) • 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 4-band imaging (griz), including the overhead time 3000deg^2 1000deg^2 400deg^2

More Related