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Subaru Weak Lensing Survey: Hyper Suprime-Cam

Subaru Weak Lensing Survey: Hyper Suprime-Cam. Masahiro Takada (Tohoku U.) Takashi Hamana (NAOJ) Satoshi Miyazaki (NAOJ) on behalf of HSC WLWG. Aug ? 07 @ JPL. Hyper Suprime-Cam (HSC). Replace the Subaru prime focus camera with the new one (HSC) PI: S. Miyazaki (NAOJ)

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Subaru Weak Lensing Survey: Hyper Suprime-Cam

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  1. Subaru Weak Lensing Survey: Hyper Suprime-Cam Masahiro Takada (Tohoku U.) Takashi Hamana (NAOJ) Satoshi Miyazaki (NAOJ) on behalf of HSC WLWG Aug ? 07 @ 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: 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

  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: 150-300 nights (starting from 2011 for 3-5 years) Targeted Fields: TBD • 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 *Limiting mag. is for 10 detection of 1 square arcsecond aperture *i’-band data is used for weak lensing analysis

  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

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