SAFARI a FIR Instrument for the SPICA mission. Yasuo Doi University of Tokyo

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1 SAFARI a FIR Instrument for the SPICA mission Yasuo Doi University of Tokyo

2 SPICA a Cooled Telescope! MIR FIR

3 SAFARI Overview SAFARI optical design FPAs + det boxes Extra fold mirror Front optics: M4 to M8 Interferometer: M9 to M11+ BS1 & BS2 M12b M16b Camera optics: M14 to M16 M11b M14b M9b M14a M13b BS2 M13a M16a Dichroics M15a InstantaneousM6wavelength wavelength M10=RT coverage 35 to 210 micron M4 BS1to 5 Camera mode with R~3 EFP Multiple spectroscopy mode up to R = 2000 (goal R~10000) Field of viewm7 2x2 arcmin M11a Line sensitivity of <10 x10-20 W m-2 M3=POM (5-σ 1 hour) (goal <5x10-20 W m-2 M9a M5=BSM Continuum sensitivity of <50 M8µ Jy Instantaneous wavelength coverage 35 to 210 micron Camera mode with R~3 to 5 Multiple spectroscopy mode R = 2000 (goal R~10000) M12a Extra fold mirror Legend: EFP=Entrance focal plane POM=Pick-off mirror BSM=Beam Steering Mirror RT=Roof-Top BS=Beamsplitter FPA=Focal Plane Array Spatial resolution 3.6~11.5 arcsec Field of view 2x2 arcmin Line sensitivity of <2x10-19 W m-2 (5-σ 1 hour) (goal <5x10-20 W m-2) Continuum sensitivity of <50 ujy

4 Baseline Mechanical Design Mechanical Layout based on optical design from Marc Includes only baseline rooftop mirrors on FTS Scan mechanism Based on TES detector envelope and optics Box structure of Al6061 with mirrors mounted on 5 of the 6 sides (including lid) FTS & FW mechanisms, detector modules and cooler mount to base; BSM mounts to lid Structure mounted on kinematic mounts to SPICA Optical Bench

5 SAFARI Study Status Project History Presentation of concept study to JAXA leads to a request to a proto-consortium to study an Imaging Spectrometer ESI Instrument consortium forms Original possibility of Europe providing an Instrument on SPICA raised informally Core Science case defined, basic instrument architecture established and focused technology development initiated ESA Carry out the internal CDF Study of SAFARI SAFARI Phase-A1 Closeout Review SPICA Proposal submitted to ESA ESA Selects SPICA as a Candidate MOO within Cosmic Vision`` ESA Cosmic Vision Down selection and JAXA SPICA SRR SAFARI a European proposed instrument

6 SAFARI Study Status Study Team Current SAFARI consortium is made up of around 120 scientists and engineers The PI and Study Management roles are being carried out by the UK Bruce Swinyard (RAL): Principal Investigator Doug Griffin (RAL): Systems Engineer / Project Manager Project Science Kate Isaak (Cardiff University); Extra-galactic science Javier Goicoechea (University of Madrid): Galactic Science

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8 SPICA/SAFARI Sensitivity ( revised : UK SAFARI proposal, Aug ) SOAP : (1hr, 5σ) GOAL : 2x10-19 (1hr, 5σ)

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13 Understanding the formation and evolution of galaxies SAFARI AGN SAFARI Starburst SAFARI Key diagnostic lines out to z~3 and beyond mbandwidth multiple lines in single observation 2 x 2 multiple sources in single observation Multiplexing advantage

14 Near-by Galaxies Spatially resolved, Large-scale observations Spatial resolution: 3.6~11.5 arcsec 17~56 1Mpc 0.9~2.8 LMC (50kpc) 63~200 M81&M82 (3.6Mpc) 170~540 M51 (9.6Mpc) SPICA obs. of near-by galaxies <-> current galactic IMS study with a view of large-scale distributions Herschel has opened this new era SPICA as an cooled telescope high sensitivity for extended emission

15 Spectroscopic Observing Speed Observing time required to detect 1x10-19 W m-2 to 5-σ A Herschel B Herschel SAFARI SAFARI JWST JWST ALMA ALMA C Herschel D Herschel ALMA SAFARI JWST ALMA PPRP Oxford 25/9/08 JWST SAFARI SAFARI Known wavelength in a single source Known wavelength in a single pointing assuming: 1 source/field - JWST and ALMA 2 sources/field - PACS 8 sources/field - SAFARI. Observation covering the full band of the instrument (i.e.unknown redshift, many lines or broad features) Mapping a full 2x2 arcmin field covering the full wavelength range (SNR, ISM, circumstellar shells, local galaxies)

16 The formation of planetary systems exo-planets discovered to-date, however the formation and evolution of planetary systems is SAFARI MIR/FIR hosts unique diagnostics of the different material phases (eg. gas, dust, ice) in planetary system formation SAFARI: traces all layers Photodissociation layer major FIR cooling lines Warm molecular layer CO, HCN, CN ALMA; H2O, OH.. SAFARI Midplane ices: site of dust coagulation planet formation dust mineralogy: history of dust By tracing presence and distribution of the gas, dust and ices can: Constrain physical conditions and processes in protoplanetary disks Test planet formation and evolution theories

17 Tracing gas in circumstellar disks Key cooling lines e.g. [CII], [OI] [63,145], [SiII] Faint, but can detect out to >100pc Covering many SFRs regions, low-mass (eg.taurus) and highmass (Orion) Extensive range of host stars and disks test models

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21 Persons of intention Kate's side: extragalactic Javi's side: galactic Takashi ONAKA (U. of Tokyo) Keigo ENYA (ISAS/JAXA) Hidehiro KANEDA (Nagoya U.) Yoshiko OKAMOTO (Ibaraki U.) Mitsunobu KAWADA (Nagoya U.) Michihiro TAKAMI (Ac. Sinica) Shinki OYABU (ISAS/JAXA) Hirokazu KATAZA (ISAS/JAXA) Hideo MATSUHARA (ISAS/JAXA) Satoshi TAKITA (ISAS/JAXA) Shuji MATSUURA (ISAS/JAXA) Takashi ONAKA (U. of Tokyo) Mai SHIRAHATA (ISAS/JAXA) Yasuo DOI (U. of Tokyo) Keigo ENYA (ISAS/JAXA) Sunao HASEGAWA (ISAS/JAXA) Takehiko WADA (ISAS/JAXA) Takafumi OOTSUBO (ISAS/JAXA) Tsutomu TAKEUCHI (Nagoya U.) Tsutomu TAKEUCHI (Nagoya U.) Masatoshi IMANISHI (NAOJ) Yoshimi KITAMURA (ISAS/JAXA) Takao NAKAGAWA (ISAS/JAXA) Misato FUKAGAWA (Osaka U.) Toshinobu TAKAGI (ISAS/JAXA) Hideyuki IZUMIURA (NAOJ) Takuya YAMASHITA (NAOJ) Mitsuhiko HONDA (Kanagawa U.)