1. Subaru Weak Lensing Survey: Hyper Suprime-Cam
Masahiro Takada (Tohoku U.)
Takashi Hamana (NAOJ)
Satoshi Miyazaki (NAOJ)
on behalf of HSC WLWG
Aug ? JPL

2. Hyper Suprime-Cam (HSC)
Replace the Subaru prime focus camera with the new one (HSC)
PI: S. Miyazaki (NAOJ)
The grant (~$15M) to build the new camera was approved in 2006
Construction: 
FoV: degrees in diameter (~10  the Suprime-Cam’s FoV)
4 - 5 broad band filters (BVRiz) available
The first light in
Plan to conduct a wide-field survey (primarily for WL); hopefully starting from 2011 for 3-5 years

3. Suprime-Cam
From Y. Komiyama
2 degree FoV option

4. HSC observing conditions for WL
HSC is designed to preserve image quality of the current Suprime-Cam
Galaxy number density usable for WL as a function of exposure time
Typical seeing size ~ 0.6’’

5. One case for survey parameters
Area: ~2,000 deg^2
Limiting Mag. (AB): B~26,V~26,R~26, i’~25.8, z’~24.3
Exposure time (min): 15(B, V, R, z’), 30 (i’)
Nights: nights (starting from 2011 for 3-5 years)
Targeted Fields: TBD
*Limiting mag. is for 10 detection of 1 square arcsecond aperture
*i’-band data is used for weak lensing analysis
Survey parameters above are preliminary and DE case is considered here because it is primary science case
However, survey must be eventually optimized to also achieve several other science cases including “galaxy evolution study” in order to obtain final acceptance from Japanese astronomy community
An optimal survey design for DE case is being carefully investigated using the Suprime-Cam data

6. HSCWLS performance (WLT+CC+CMB)
9 parameters (_de, w0, wa, A_s, ns, alpha, wm, wb, tau) within a CDM model
The forecasts are for WLT + CMB (blue), cluster counting (CC) + CMB (green), WLT + CC + CMB (orange)
(w_constant)~0.05
Include the non-Gaussian errors of WLT (MT & Jain 07 in prep.) and the covariance between CC and WLT (MT & Bridle 07)
However, not include model systematics of each experiment