asiaa research highlights and prospects with hsc

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