Jim Gunn David Spergel Michael Strauss Jenny Greene Rachel Mandelbaum Robert Lupton Tim Heckman Chuck Bennet Rosie Wise Brice Menard Nadia Zakamska. All Japan Richard Ellis Judy Cohen Chris Hirata Mike Seiffert Olivier Dore Dan Starn Lexi Moustakas Yen-Ting Lin Tzu-Ching Chang Lihwai Lin Wei-Hao Wang. Olivier Le Fevre Jean-Paul Kneib. Raul Abramo Laerte Sodre.

Spectrograph A Wide Field PFI &NASA/JPL& AS Corrector Prime Focus Instrument &NASA/JPL Rotator Fiber Connector Caltech/JPL/ASIAA Wide Field Corrector USP/LNA LAM/Princeton/JHU (CNRS) & & Caltech/JPL (AS) Fiber Positioner Cobra (from bottom)

Number of fibers 2400 1.3 deg (hexagonal-diameter of circumscribed circle) Fiber diameter 1.13 diameter at center 1.03 at the edge Blue Red NIR Wavelength range [nm] 380-650 630-970 (706-890) 940-1260 Central resolving power ~2350 ~2900 (~5000) ~4200 Detector type CCD CCD HgCdTe Share WFC with HSC 4 spectrographs for 600 fibers each λ=0.38-1.26μm with 3 arms Now, a medium resolution mode (R~5000) for red arm is our baseline design

Brief History

From Arimoto-san s slides

PFS PDR, Feb 2013@Hilo 4 th PFS Collaboration Meeting, Mar 2013@Tokyo

Science WGs & Mailing Lists Cosmology WG: Masahiro Takada (IPMU), Chris Hirata (Caltech), Jean-Paul Kneib (LAM) Galactic Archeology WG: Masashi Chiba (Tohoku U.), Judy Cohen (Caltech) Galaxy WG: Jenny Greene (Princeton), Kevin Bundy (IPMU), John Silverman (IPMU), Masami Ouchi (U. Tokyo) AGN WG: Tohru Nagao (Kyoto U.), Michael Strauss (Princeton) Mailing lists: pfs_survey@ipmu.jp (89 registrations as of Feb 27, 2012), pfs_cosmology, _galaxy, _agn, _ga@ipmu.jp Wiki page: http://sumire.pbworks.com

Science Objectives: Three Pillars

arxiv:1206.0737 Takada, Ellis, Chiba, Greene et al.

PFS Cosmology PFS (8.2m: 100 nights) vs. BigBOSS (4m: 500nights)

DE reconstruction The wide-z coverage of PFS+BOSS enables a reconstruction of DE densities as a function of redshift constrains a broader range of DE models Ω de (z) = ρ de(z z i ) 3H 2 (z) 8πG No gap in redshift 0<z<2.4 PFS can significantly improve the accuracy of the reconstruction due to the increased z-bins 7% accuracy of Ω de (z) in each of z-bins PFS+SDSS+Planck allows a detection of dark energy up to z~2, for a Λ-type model

PFS Galaxy Evolution Studies

PFS Galactic Archaeology

Major Milestones Feb 2013: PDR Apr 2013: NAOJ Review Received the reports/comments Haven t yet responded to the comments (working in progress) Various timing (from 2013): subsystem CDRs Jul 2016: System integration, tests Jun 2017: Operational Readiness Review Jul 2017: First Light (engineering)

Funding shortfall Baseline cost: about $70M Contingency: $8.8M Committed funds from members: $60.6M About $20M short Clearly needs fund raising NAOJ support after NAOJ review Explore the way to reduce the cost (but not to increase additional risk) Additional partners (several groups show interest) Additional grants/private funds

Fund raising

MSIP

PFS: 絶好のタイミング 2020 2019 2018 2017 2016 2015 2014 2013 2012 2011 WL BAO DES HSC SDSS/BOSS LSST? Euclid PFS WFIRST? GAIA Astrometry

E-ELT & TMT Euclid(2019-)

DESI Euclid/ESA ngcfht WFIRST/NASA