ASIAA Research Highlights and ASIAA Research Highlights and Prospects with HSCProspects with HSC
Keiichi Umetsu, ASIAAKeiichi Umetsu, ASIAA
SAC HSC Science Workshop 29.01.20078
OutlineOutline
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
1. Major ASIAA Projects (1994-2008)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)
2. ASIAA Research Highlights 2. ASIAA Research Highlights and and
Prospects with HSCProspects with HSC
2-1. Scam/HSC + AMiBA SZE2-1. Scam/HSC + AMiBA SZE
ASIAA & NTU (Taiwan) Collaboration
AMiBA SZE Cluster ObservationsAMiBA 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)
Synergy with S-Cam and HSC: Synergy with S-Cam and HSC: SZE and WL Probing Cluster SZE and WL Probing Cluster
PhysicsPhysics
z=0.228
z=0.183
Mass map from Subaru/Scam data
z=0.091z=0.224
2-2. Cluster Weak Lensing 2-2. Cluster Weak Lensing for Probing DM Halo Profilesfor Probing DM Halo Profiles
References
Broadhurst, Takada, Umetsu et al. 2005 (ApJL)
Umetsu & Broadhurst 2007 (ApJ, submitted)
Umetsu, Medezinski, Broadhurst, & Okabe 2008 in prep.
Strong(est) Lensing Cluster A1689Strong(est) Lensing Cluster A1689 (z=0.18) (z=0.18)
Mass (~DM) Cluster GalaxiesRelaxed, massive cluster with large E=45” (zs=1):
5.5Mpc
r=10-2000 (rvir) kpc/h
Umetsu & Broadhurst 2007
Subaru Subaru+ACS
Surprisingly high concentration, difficult to accommodate with LCDM (cvir~5)
NFW fitNFW fit: Mvir=2.1x1015Msun, Cvir=13
DM Ring Cluster CL0024DM Ring Cluster CL0024 (z=0.4) (z=0.4)
NFW fitNFW fit: Mvir=1.1x1015Msun, Cvir=14
Strong lensing cluster with large E=32” (zs=1.6):
Cluster Galaxy density map, with mass contours overlayed
Observed large E, implying large Cvir, challenging for LCDM
Umetsu et al. 2008 in prep.
E
Prospects for HSCProspects 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)
2.3 Cross Correlating the 2.3 Cross Correlating the Cosmic Shear and Galaxy Cosmic Shear and Galaxy Density Fields for Probing Density Fields for Probing
the Statistical Matter-Galaxy the Statistical Matter-Galaxy RelationRelation
The HSC WLWG team
Bias ParametersBias Parameters
HSC SurveyHSC 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
2222
2
2
2
2
~
,~
apap
apap
gm
gm
ap
ap
m
g
NM
NMr
M
Nb
cf. Schneider 1998, Fan 2003;
Hoekstra+ 2002 (RCS+VIRMOS), Sheldon+ 2004 (SDSS), Simon+ 2007 (GaBoDS)
Forecasts (1): Forecasts (1): Detection of r-parameterDetection of r-parameter
Large scaleSmall scale
Tota
l dete
ctio
n S
/N
HSC DeepHSC Deep
DESDES
HSC ShallowHSC Shallow
By Nishioka (ASIAA)
Forecasts (2): Forecasts (2): Superior HSC Sensitivity Superior HSC Sensitivity in Higher Redshiftsin Higher Redshifts
Sensi
tivit
y in
z-s
pace
(
ap=
10
’)
Redshift
HSC ShallowHSC Shallow
HSC DeepHSC Deep
DESDES
By Nishioka (ASIAA)
2.4 Search for Dust in the ICM2.4 Search for Dust in the ICM
Reference: Muller, Wu, Hsieh et al. 2008 (ApJ, in press)
Foreground clusters
Galaxies behind the clusters
Reference background
Application to the RCS SurveyApplication to the RCS Survey (33deg^2)(33deg^2)
Method: Background color statisticsw/ 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
Future Prospects: Future Prospects: How to Improve?How to Improve?
- More clusters to allow a sample selection based on cluster properties: mass, X-ray, merger, etc.. widerwider
- More reliable photo-z measurements more more filtersfilters
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
2.5 Ongoing CFHT Project2.5 Ongoing CFHT Project
Bau-Ching Hsieh, Wei-Hao Wang, et al. (CFHT S07B) GoalGoal: Search for galaxies at z > 7
FieldField: Extended Chandra-Deep Field South (ECDFS)
ObservationsObservations: CFHT/WIRCam “J” (24.9 ABmag, seeing ~0.7”)
Sky areaSky area: ~ 500 arcmin^2
Data from other bandsData from other bands: GEMS ACS: V (28.4), z’ (27.1) SIMPLE (Spitzer): 3.6um (25.1)
Criteria for candidatesCriteria 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
SummarySummary
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
HSC Survey ParametersHSC Survey Parameters
3000deg^2
1000deg^2
400deg^2
4-band imaging (griz), including the overhead time
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