Subaru Weak Lensing Survey:Subaru Weak Lensing Survey: Hyper Suprime-Cam Hyper Suprime-Cam

Masahiro Takada (Tohoku U.)

Takashi Hamana (NAOJ)

Satoshi Miyazaki (NAOJ)

on behalf of HSC WLWG

Aug ? 07 @ JPL

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Hyper Suprime-Cam (HSC)Hyper Suprime-Cam (HSC)• Replace the Subaru prime focus cam

era with the new one (HSC)

• PI: S. Miyazaki (NAOJ)

• The grant (~$15M) to build the new camera was approved in 2006

• Construction: 2006-2011

• FoV: 1.5 - 2.0 degrees in diameter (~10 the Suprime-Cam’s FoV)

• 4 - 5 broad band filters (BVRiz) available

• The first light in 2010 - 2011

• Plan to conduct a wide-field survey (primarily for WL); hopefully starting from 2011 for 3-5 years

From Y. Komiyama 2 degree FoV option

Suprime-Cam

HSC observing HSC observing conditions for WLconditions for WL

• HSC is designed to preserve image quality of the current

Suprime-Cam

Typical seeing size ~ 0.6’’

Galaxy number density usable for WL as a function of exposure time

One case for survey parameters One case for survey parameters

• 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 ot

her 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

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: 150-300 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

HSCWLS performance (WLT+CC+CMB)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), WL

T + 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