新学術シンポジウム @Kavli IPMU, Sep 21, 2015 JST Naoyuki Tamura (Kavli IPMU) Prime Focus Instrument PFI On behalf of PFS collaboration Cobra engineering model module Camera cryostat Fiber connectors Spectrograph system
Subaru Telescope on Mauna Kea, Hawaii
ubaru + Instrument (e.g. PFS) = Telescope + eye piece + eyes + optic nerves Scientific instruments
What is PFS? Key word #1: Spectrometer Intensity of light pectroscopy is very owerful to know: Redshift (~distance) Strength of starforming activity Chemical composition of gas & stars etc Wavelength
What is PFS? Key word #2 -- Subaru Prime Focus Hyper Suprime Cam (HSC) is now in operation. 1.5 deg on sky cf. Full Moon = ~0.5 deg
What is PFS? Key word #3: Optical fibers n n n Light is transmitted efficiently & flexibly.
Courtesy of K. Yabe (Kavli IPMU) What is PFS? How it works Telescope focal plane Fiber slit
The SuMIRe project Subaru Measurement of Images and Redshifts HSC + PFS Exploiting the ~1.5 deg field of view on the prime focus of the 8.2m Subaru Telescope. Wide-field imager Hyper-Suprime Cam (HSC) ~0.9 billion pixels 300 nights in 2014--2018 1400 sq. degrees, ~1B galaxies Wide-field multi-object spectrometer Prime Focus Spectrograph (PFS) 2400 optical fibers 300? nights from 2019? ~4M galaxy redshifts ~1M stars in MW, M31, dsphs. SDSS-like survey at z>1 & Galactic Archaeology to address cosmic evolution & dark sector. Enables Subaru to be a world-leading facility out to the next decade making effective synergy with TMT, SPICA, LSST, JWST, Euclid, WFIRST, etc. HSC CCD array PFS Fiber array
PFS Fast facts Subaru Prime Focus Spectrograph Wide field: ~1.3 deg diameter Highly multiplexed: 2400 fibers Quick fiber reconfiguration: ~60 sec (TBC) Optical-NIR coverage: 380-1260nm simultaneously Developed by international collaboration, under the initiative of Kavli IPMU Cosmology, Galaxy/AGN evolution, Galactic Archaeology as the key science areas in the PFS collaboration Aiming to start science operation from 2019, as a facility instrument on Subaru. 9
Scientific drivers: Three Pillars All are based on a spectroscopic follow-up of objects from the HSC images. Cosmology (~100 nights): 1400 sq. degrees ~4M redshifts of emission-line galaxies BAO at each of 6 redshift bins over 0.8<z<2.4 Cosmology with the joint experiment of WL and galaxy clustering (HSC/PFS) Galaxy Evolution (~100 nights): ~20 deg 2 A unique sample of galaxies (~0.5M) up to z~2, with the aid of the NIR arm Dense sampling of faint galaxies (also many pairs of foreground/background galaxies) Studying cosmic reionization with a sample of LAEs, LBGs and QSOs Galactic Archaeology (~100 nights): Milky Way/M31/dSphs ~1M star spectra for measuring their radial velocities going fainter & farther. Use the 6D phase-space structure, in combination with GAIA in order to study the origin of Milky Way (also with studies of dsphs & M31) Use a medium-resolution-mode survey of ~0.1M stars to study the chemodynamical evolution of stars in Milky Way And various others too, expected from the general communities. 10
PFS Collaboration 11
PFS organization chart PFS Steering Committee PI & one representative from PFS partner, Subaru, NAOJ + PS + PM Kavli IPMU Murayama (PI) NAOJ & Subaru Hayashi, Arimoto PFS Science Team PFS Project Office Subaru Divisions Co-Chairs: Takada [PS] (Kavli IPMU) & Ellis (ESO) Cosmology Galactic Archaeology Galaxies & AGNs Tamura [PM, SE], Shimono, Ishizuka Yabe, Moritani (Kavli IPMU) Takato (Subaru), Ueda (NAOJ), Sakamoto (NAOJ/IPMU) New Development Takato, Minowa Tel. Eng., Inst., OCS, CDM, Management Team Tamura, Shimono and 1-2 representatives per institution Systems Engineering Team Tamura, Shimono and 1-2 representatives per institution Fiber Positioner CIT/JPL Fiber System USP/LNA Prime Focus Instrument ASIAA/CIT/JPL Metrology Camera System ASIAA Spectrograph System LAM Detectors & Dewars PU /JHU System Software IPMU Exposure Targeting Software MPA/IPMU Data Reduction Pipeline PU/LAM Database & data archive TBD/IPMU/NAOJ
PFS logistics for system integration Dewars & detectors Spectrograph system Fiber positioner system Prime Focus Instrument & metrology camera Fiber slit Telescope fiber cable Focal plane fibers Systems engineering is clearly the key. Parts/components/subsystem will be validated at each site before their delivery to Subaru (cf. so-called systems engineering V -model).
PFS past, present, and future Apr 2011: Project Office was established. Design study activities were formalized. Mar 2012: Conceptual Design Review (CoDR: 概念設計会議 ) @ Hilo Feb 2013: Preliminary Design Review (PDR: 基本設計会議 ) @ Hilo Mar 2013 Present: A hybrid of critical/final design phase & production phase Critical Design Review (CDR: 詳細設計会議 ) is held at subsystem level (instead no project CDR). Mar 2014: Cable A & Spectrograph System (SpS) CDR Done! Mar 2015: PFI, fiber positioner system, Cable C CDR Done! Sep 2015: Metrology camera (from tomorrow!) Late 2015: Cable B 2017-2018 : Subsystem delivery to Subaru and system integration ~Early 2018: Engineering First Light ~Mid-late 2019: Start open use & SSP 14
PFS project top-level schedule SM-N : Nth Spectrograph Module MCS : Metrology Camera System PFI : Prime Focus Instrument CAB : Fiber Cable on Telescope PFI CDR MCS CDR (Sep) CAB review (Nov?) Subsystem DEL & AIT at Subaru SM-1, 2 AIT DEL SM-1, 2 CAB DEL SM-3, 4 PFI SM-3, 4 AIT MCS? 2015 2016 2017 2018 2019 Construction, subsystem integration & test System integration Science operation On-sky commissioning 15
The Competition: Schedules Note: The schedules of the competitors are represented by their starts of science operation based on the information in the official websites etc. MOONS: GA and galaxy surveys (FL 2019, Op 2020?-) WEAVE: GA (FL 2017, Op 2018-) DESI: Cosmology (FL 2018 end, Op early 2020-) 4MOST: GA & galaxy surveys (FL 2020, Op 2021?-) eboss/hetdex: cosmology EUCLID: cosmology PFS CONSTRU CTION HSC SSP PFS COMMISS IONING PFS SCIENCE OPS (both PI-type & SSP) 2017 2018 2019 2020 2021 2022 2023 2024 16
PFS science team activities & timeline Takada et al. 2014, PASJ: A summary of the survey design studies & top-level requirements to the instrument by the time of PDR. Semi-regular discussions in the working groups and by the working group chairs. Coordinating the survey strategies of the three key science programs under one big umbrella. Preliminary timeline: 2015: Maturing survey strategies and drafting an SSP proposal. Project-wide discussions at the collaboration meeting in Dec 2016: Continuing the above and brush up the draft. 2017: Proposal submission. Start of review process. 2018 early 2019: Tweaking the survey details having inputs from engineering observations Delta review Mid-late 2019: Start of science operation & SSP These procedure & timeline are TBC, under discussions at SAC etc 17
PFS subsystems distribution in Prime focus unit POpt2 with Wide Field Corrector WFC. Spectrograph system (SpS) On the TUE floor POpt2 & WFC will be shared with Hyper Suprime Cam (HSC). Software system (Calibration system)
Prime Focus Instrument (PFI) Sits in the prime focus unit POpt2 and installed to the telescope Fiber positioner system Acquisition & Guide (AG) camera Fiber cable: Cable C & fixed fiducial fibers Fiducial fiber illuminator Field element (cf. Filter+dewar window@hsc) Cable wrapper Calibration lamp system HSC builder s blog http://anela.mtk.nao.ac.jp/hscblog/builder/
Focal plane: Fiber positioner Cobra Positioners with a 8mm pitch. Patrol areas have some overlaps. 20
Focal plane: Positioner packaging 6x CCD cameras for Acquisition & Guiding (AG) 21
Cobra Engineering model performance Fisher+ (2014, SPIE)
PFI CDR (Mar 10-11, at Caltech) Review board External x 6: T. Huang (ASIAA), F. Leger (Washington), K. Seaman (JPL), M. Colavita (JPL), R. Foehner (JPL), K. Aaron (JPL) Internal x 4: N. Takato (NAOJ), J. Gunn (Princeton), G. Murray (Durham), N. Tamura (Kavli IPMU, chair) The JPL-Caltech team successfully passed the fiber positioner system delta CDR on Jun 22. 23
PFI CDR (Mar 10-11, at Caltech) PFI Prime Focus Instrument Fiber positioner system, Fiber cable, mechanical structure, AG cameras, Calibration lamp system, Fiber positioner Cobra Mass production will start soon. Engineering model module PFI delivery to Subaru in 2017 (TBC) 24
Metrology Camera System To image all backlit fibers at one exposure and measure the current fiber positions at the prime focus. Focal plane Fibers Wide-field corrector Cs hole Primary mirror HSC builder s blog http://anela.mtk.nao.ac.jp/hscblog/builder/ Met. Cam. System in the general purpose Cs container
Metrology Camera System 380mm aperture Schmidt type Mech. design is being finalized. CANON 50M pixel CMOS sensor 8960 5778, 3.2um pixel 28.67 18.49mm ~3 sec per iteration (depending on exposure time) Dome seeing measurement using FMOS & test camera Critical Design Review: 9/22-23@ASIAA+TV
Spectrograph System (SpS) Red Mid. Res mode in the red arm Blue NIR Bench size: 1.9m x 2.4m
SpS What s happening now JHU Winlight One channel Integration Mangin Collimator Cryostat assembly, pump-down and cool-down before shipping First lab spectra are expected soon (within this year). First red camera arrival from Winlight LAM First fiber slit assembly arrival from LNA and installed on the optical bench with Hexapod.
SpS: Configuration at Subaru 4x spectrograph modules (SM) are accommodated in a temperature-controlled clean room. Clean room IR4 floor IR3 floor IR-side Nasmyth floor (not shown here) T. Tamura+ (Subaru)
PFS system Software Test plan Software PFS system Subsystem Flowdown/Cascade of requirements/specifications Software Test plan Subsystem Kavli IPMU, NAOJ, Project Office Software Prduction, Integration & test Parts, tools Now Software Time
Can be done w/ Eng. fibers Can be done daytime Need night runs Need attention MCS only Abbreviations EL: Elevations MC: Metrology Camera PFI: Prime Focal Instrument ROA: Rotation Angle SCR: Spectrograph Clean Room SM: Spectrograph Module SpS: Spectrograph Subsystem TPA: Telescope Pointing Analysis Planning system integration & 01/04/2015 01/07/2015 01/10/2015 01/01/2016 01/04/2016 01/07/2016 01/10/2016 01/01/2017 01/04/2017 01/07/2017 01/10/2017 01/01/2018 01/04/2018 01/07/2018 01/10/2018 01/01/2019 01/04/2019 01/07/2019 01/10/2019 engineering observation 2/2017-7/2017 11/2017-4/2018 MCS commission (M-xx) SM1,2 commission (S-xx) 8/2018-10/2018 AM3,4l commission (S-xx) 2/2018-7/2018 8/2018-1/2019 PFI commission (P-xx) All System commission (A-xx) 7/2016 ICS system ready 6/2016 FMOS decommission 2/2017 MCS Ready 12/2017 Cable B ready 2/2018 PFI ready 2/2018 Engeneering FL 11/2017 SM1,2 ready 7/2018 SM3,4 ready 2/2019 Science FL? (M-1) Off-telescope characterization and check basic function of MCS (M-2) MC installation to Telescope (M-3) Check basic function of MC on Telescope (M-4) verify MCS function by measuring fibre position of FMOS Repeat at different observing runs and check stability against PFI and POpt2 installation read detector PFI only PFI and MCS (P-1) Off-telescope characterization and check basic function of PFI (P-2) PFI installation to POpt2 and POpt2 installation to Telescope (P-3) Check basic function of PFI (back-illumination, Cobras & AG cameras) on Telescope (P-4) Measurement of PFI x/y offset w.r.t the rotator axis (P-5) Measurement of PFI z offset and tilt from the nominal position (probably hard) (P-6) Measure MC-PFI distortion by imaging backlit fibers by MC (P-7) Point Telescope to bright star(s). Try focusing AG camera and check image quality & focal plane tilt (P-8) Validate auto guiding function (P-9) Carry out 1-/5- point TPA (P-10) Repeat (P-9) at various EL and ROA. Tweak Hexapod operation if necessary (P-11) Carry out 5-/32- point TPA (P-14) Slew Telescope to a field of bright stars. take deep exposures (~10-30s?) by AG cameras to male 1 st -pass distortion map power, network, lamp, rotator, sensor with back illumination of science/fiducial fibers, measure rotator center (Xrot, Yrot) in MC Repeat at various EL and ROA to characterize the dependency Using defocused image, check and correct shift/tilt of WFC w.r.t M1 Validate Telescope pointing, target acquisition and auto guiding functions. execute MA if needed Validate Telescope pointing, target acquisition and auto guiding functions. Repeat on various fields to refine the 1 st -pass distortion map as functions of EL and ROA Moritani, Yabe, Tamura, Project Office, PFS team SpS only (S-1) Check basic function of SCR and SM Cool SCR and cryostats, and check basic functions under low temperature check image quality and confirm stability and repeatability by repeating temperature cycle (S-2) Check focus on the detector of Cal. lamp (S-3) Check PSFs on the detector using Arc lamp (S-4) Check spectral distortion on the detector using Flat lamp (S-5) Measure throughput of SpS itself using Black Body Lamp All systems (F-1) (A-1) (A-2) Illuminate each fiber Calibrate the distance Configure fibers on bright from Cable A and check b/w AG cameras and stars and do telescope the position of the fiducial fibers by raster scan to make the corresponding cobra telescope raster scan 2 nd -pass distortion mapp using MC around fiducial fibers Repeat on various fields to refine the 2 nd -pass distortion map as functions of EL and ROA. Check dependence on T and lambda (A-3) Configure fibers on a science field for performance verification Measure total throughput (A-4) Configure fibers on a science field for sicentific verification using F star, validate flux calibration check sky subtraction and estimate the accuracy Developing this chart exploiting experiences on FMOS Interactions with subsystem-level activities are critical. Individual processes will be matured with: Inputs from previous processes or subsystem tests Step-by-step procedure & required tools for analyses etc. Success criteria to go to the next process take long-time exposure and check quality
PFS website http://pfs.ipmu.jp The impressive PFS movie! Asking donation! Project top-level schedule, history, & upcoming events Instrument parameters Estimated throughput & on-sky performance Main contents are prepared for nonexperts. Collaboration with IPMU PIO team is in the scope. 32
PFS instrument parameters See the PFS web for more details http://pfs.ipmu.jp/research/parameters.html Microlens at the fiber tip slows down the beam (cf. F/2.5 at SpS collimator) Due to the parts around the fiber. Detectors: 2x(4Kx2K) Hamamatsu CCDs@VIS H4RG@NIR (1.7um cutoff) 15um pix 33
Throughput model & sensitivity estimation See the PFS web for more details http://pfs.ipmu.jp/research/parameters.html Notes: The PFS part of this has been estimated mainly based on the specs, rather than the actual models e.g. from vendors (which are better than the specs). This has not yet taken into account neither the atmosphere nor aperture effect. 34
Throughput model & sensitivity estimation See the PFS web for more details http://pfs.ipmu.jp/research/performance.html Continuum Emission line Using a PFS spectrum simulator by C. Hirata (Ohio) EL=45 deg, 0.8 arcsec seeing, dark night 850 x 4 = 3600 sec integration Point source for the continuum case (~75% flux input to the fiber) Faint galaxy profile with σ=70km/s for emission line (~61% input) 1% residual sky subtraction error 35
PFS blog http://pfs.ipmu.jp/blog/ Started just a month ago! Both English and Japanese. Trying regular updates at meetings, milestones, etc, with photos. 36
Funding situation Improving! ~90% of the total cost ($~80M) has been secured (cf. $~20M shortfall at the time of PDR). Good news! The Murayama et al. s application to Grant-in-Aid for Scientific Research on Innovative Areas ( 科研費新学術 ) has been approved! $~2M for the PFS development!! Shortfall still remains ~several M $ including contingency Looking for new partners to the collaboration: There are a couple of (promising) candidates. Continuing funding applications: Budget request for PFS to Ministry/Government via U. Tokyo ( 概算要求 ) A proposal has been submitted to NSF MSIP by the US team. Grand-in-Aid ( 科研費 ) applications again this year 37
Summary about PFS The project passed Conceptual Design Review in 2012 and Preliminary Design Review in 2013. The Spectrograph System (SpS) & the Prime Focus Instrument (PFI) also passed the subsystem Critical Design Review in 2014 & 2015, respectively. Now finalizing the design studies and proceeding with production, integration & test. Cryostat PFI CAD model Cobra positioner module PFI focal plane CAD model Integration Optics Aiming at engineering observation from early 2018 & science operation from mid-late 2019. Unique capability of Subaru for unique science via synergy w/ TMT, LSST, SPICA, JWST, Euclid, WFIRST Refer to PFS web & blog for more detailed information and updates. Individual Cobra positioners Cobra engineering model module 38