asiaa research highlights and prospects with hsc
DESCRIPTION
ASIAA Research Highlights and Prospects with HSC. Keiichi Umetsu, ASIAA. SAC HSC Science Workshop 29 . 01 .200 78. Outline. Introduction – Major ASIAA Projects Highlights and Prospects with HSC – AMiBA SZE Interferometer – Weak Lensing (HSC WLWG collaboration) - PowerPoint PPT PresentationTRANSCRIPT
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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
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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
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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)
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2. ASIAA Research Highlights 2. ASIAA Research Highlights and and
Prospects with HSCProspects with HSC
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2-1. Scam/HSC + AMiBA SZE2-1. Scam/HSC + AMiBA SZE
ASIAA & NTU (Taiwan) Collaboration
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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)
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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
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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.
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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
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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
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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)
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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
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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)
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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)
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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)
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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
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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
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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
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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
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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
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HSC Survey ParametersHSC Survey Parameters
3000deg^2
1000deg^2
400deg^2
4-band imaging (griz), including the overhead time