すみれ The PFS SuMIRe project The Prime Focus Spectrograph for SUBARU MEASUREMENT OF IMAGES AND REDSHIFTS Laurence Tresse (LAM) Atelier PNCG: grands relevés en optique 28 avril 2014, Paris
SuMIRe Science Driver: The Origin and Fate of the Universe Elucidate the Nature of Dark Matter and Dark Energy Precision Wide-Field Imaging with Hyper Suprime-Cam (HSC) P.I. S. Miyazaki (NOAJ) ~ $50M NOAJ, IPMU, Princeton, ASIAA 8.2m Subaru Precision MOS Spectroscopy with Prime Focus Spectrograh (PFS) P.I. H. Murayama (Kavli, IPMU) ~ $50M IPMU, NOAJ, Princeton, LAM, JHU, Caltech/JPL, LNA, ASIAA, MPA Prime Focus Unit FOV 1.5 deg 2 (in diameter) Canon Lens
SuMIRe HSC Imaging project HSC 1st light M31 Feb. 2013 Median 0.5 FWHM Wide-Field grizy Photometric Survey FOV 1.77 deg2 (1.5 deg2 in diameter) deg2 1. HSC-Wide 1400 (iab=26, 5σ) Cosmology science driver Weak lensing, strong lensing, galaxy clusters, galaxy clustering +other science 2. HSC-Deep 28 deg2 (iab~27, +NB) HSC-UltraDeep 3.5deg2 (i~28, +NB) Galaxy and AGN evolution up to z~7 High-z galaxies, QSO, reionization 5- yrs 300 nights survey started in Feb. 2014 9ll 2019 116 CCDs Pixel scale 0.17 HSC Prime Focus Unit 3 tons, 3m high
SuMIRe PFS instrument, a wide-field, fiber-fed MOS FOV 1.5 deg2 in diameter June 2017 engineering first light
SuMIRe PFS - Spectrograph System Overview Spectrograph Module 2 Entrance Unit x4 Spectrograph Module 1 Spectrograph Module 3 Bench x4 1.8m 5m Spectrograph Module 4 5m LAM people WP4.4 S. Vives - Ingénieur Système et Conception Optique F. Madec - Responsable AIT M. Jaquet - Architecte Mécano-thermique S. Pascal - Ingénieur Conception optique A. Bozier - Assistant ingénieur projeteur mécanique D. Ferrand - Ingénieur Contrôle G. Arthaud - Intégrateur Mécanique T. Pégot-Ogier - Ingénieur logiciel instrument D. Le Mignant - Chef de Projet
SuMIRe PFS - Spectrograph Module Overview Camera Unit (CU) Red 0.63-0.97 µm Camera Unit (CU) Blue 0.38-0.65 µm Camera Unit (CU) NIR 0.94-1.26 µm Entrance Unit (ENU)
4 x [15 micron pixel CCDs 4Kx4K for each chanel (blue, red, NIR)]
SuMIRe PFS 1D Data Reduction Pipeline CHALLENGE No human intervention same track as Euclid LAM people WP 4.9 Clément Vidal CDD CeSAM Pierre-Yves Chabaud - CeSAM Thomas Fenouillet - CeSAM Christophe Adami - Eq. Cosmo Vincent Le Brun - Eq. Cosmo Olivier Le Fèvre - Eq. Cosmo Laurence Tresse - Eq. Cosmo Christian Surace responsible CeSAM PFS- simulated spectrum @z=1.9
PFS: Major Milestones Jan 2011 endorsement by Subaru community Dec 2011 MOU between IPMU & NAOJ Mar 2012 CoDR Jul 2012 Collaboration MOU Oct 2012 Requirement Review Feb 2013 PDR Critical Design Review: various during 2014 System Integration Review: July 2016 Operational Readiness Review: June 2017 Engineering First Light: June 2017 Commissioning & Science Verification: July - Dec 2017 Science Surveys: Jan 2018 - Dec 2022
PFS primary science drivers BAO RSD and growth rate Courtesy S. de la Torre Synergetic cosmology between HSC & PFS : SWL, galaxy clustering, CMB lensing, etc.
PFS Science Objectives: Three Pillars See Takada et al. (2014) PASP LAM faculty members: Adami, Amram, Arnouts, Cuby, Ilbert, Le Brun, Le Fèvre, Péroux, Tresse
PFS cosmology [OII] targets S/N for [OII] flux of 5.10-17 erg/cm 2 /s Texp = 15 mn target selection 22.8<g<24.2 & -0.1<g-r<0.3 PFS-Blue PFS-Red PFS-NIR 7847 targets per the PFS FoV ~ 3x(# of PFS fibers) 8.5 σ ~75% success rate for 2 visits of each field Estimated total volume ~9 (Gpc/h) 3 ~ 2 x BOSS survey PFS-cosmology target range RedshiR
PFS and other z-surveys for DE surveys PFS & DESI DESI overlaps with BOSS @z<0.8 PFS overlaps DESI @z=0.8-1.6 Comparable power @z=1.2-1.6 PFS probes new z-range @z>1.6
PFS and other telescope/instruments From Newman et al. arxiv:1309.5384 Spectroscopic Needs for Imaging Dark Energy Experiments
PFS uniqueness From Newman et al. arxiv:1309.5384 Spectroscopic Needs for Imaging Dark Energy Experiments DES 5000 deg 2 i=25.3 LSST 30000 deg 2 i=25.3
PFS galaxy evolution studies 1. SDSS-like surveys @z~0.5-1.5 @z~1-2 eg. detection of continuum in each spectrum not only a survey of emission-line galaxies 2. High-z LBG & LAE @ z ~ 2-7
PFS galactic archaeology 1. Formation of Galactic structures Merging history of the MW Formation of old MW components (thick disk, stellar halo) Star formation history of dwarf satellites Formation of M31: is it different from the MW? from Freeman & Bland- Hawthorn 2002 2. The nature of galactic dark matter How is DM distributed in the MW DM of dwarf satellites: is CDM correct? Tidal streams Kinematics of stars reflect past galaxy collapse and/or merging events. 1 M stars V<21-22 Tolstoy et al. 2009 Alpha-elements Fe, Mg, Si, Ca, Ti Chemical abundances of stars reflect their past SFH and chemical evolution, possibly in association with the dynamical state of proto-galactic clouds. 0.1 M stars V<21-22
SuMIRe Planned Surveys HSC-300 nights PFS extragalactic surveys Galaxy/QSO PFS-100 nights 25 deg 2 Cosmology PFS-100 nights 1400 deg 2 PFS galactic survey MW & M31 PFS-100 nights 1180 & 230 deg 2
Conclusions PFS An efficient, unique wide-field (1.5 deg 2 ) fiber-fed (2400) MOS with a large 0.38-1.36 µm baseline Science objectives Three pillars: Cosmology, Galaxy evolution studies & Galactic Archaeology Cosmology with combined probes: weak lensing, galaxy clustering, redshift-space distortion, clusters, and CMB lensing LAM is a key contributor to PFS (~30 FTE over the total project) - Deliver the Spectrograph & Optics - Deliver the 1D z-measurement pipeline Based on savoir-faire on MOS & deep redshift surveys Data proprietary - Agreement between HCS & PFS for PFS target selection - Archive of Subaru under the NAOJ responsibility, but quality and distribution of the PFS products under the PFS team responsibility - Public release, not yet discussed, à la SDSS? Risk - High competition between DE programmes, the Cosmology part should not be delayed PFS is a good timely position starting in 2018 till 2022