SPICA装置検討状況と展望 H. Kataza (ISAS/JAXA) SPICA検討チーム 1 Scientific Goals Where are we from ? How did the Universe originate and what is it made of ? Are we alone ? What are the conditions for stellar and planetary formation and emergence of life? 2 SPICA Scientific objectives (Mission Definitions) Resolution of Birth and Evolution of Galaxies Transmigration of Dust in the Universe Thorough Understanding of Planetary System Formation 3 Requirements High spatial resolution → 3m-class telescope High sensitivity → T<10K Wavelength coverage 5 to 200mm Wide Field of View Unique capabilities Instruments on board SPICA MCS : Mid Infrared Camera and Spectrometer SAFARI : Far Infrared Imaging Fourier Spectrometer Wide field Imaging spectrometer wavelength coverage : 34-210mm SCI : SPICA Coronagraph Instrument Wide field Imaging, mid and high res. spectroscopy wavelength coverage : 5-38mm Coronagraphic imaging and spectroscopy wavelength coverage : 3.5-27mm Dedicated instrument for exoplanets study FPC-S : NIR Focal Plane Camera for Sience Wide field Imaging and Low Res. Spec. with LVF wavelength coverage : 0.7-5.2mm 5 Focal Plane Instruments Wavelength coverage vs Resolving Power Herschel l/dl (dv) MCS/HRS 10000 (30 km s-1) SPICA JWST 1000 (300 km s-1) MCS/MRS US Inst 100 (3000 km s-1) SCI FPC-S 2 mm SAFARI MCS/WFC/LRS 20 mm 200 mm Wavelength Unique Capability of SPICA/FPIs λ SPICA PLM (payload module) 7 FPIA: Focal Plane Instrument Assembly 8 Focal Plane map 9 MCS 10 Unveiling the Role of Environment in the Early Universe Wide Field of View 5’x5’ Imager MCS explore the star formation activities of galaxies along the large-scale structures in the high-z Universe up to z ~5, taking advantage of wide-field imaging capability and excellent sensitivity at > 20 micron. z=1 z=5 JWST/MIRI MCS/WFC Yahagi et al. (2005) M=6×10^14 Msun, 20Mpc×20Mpc (co-moving) 11 Life cycle of dust revealed by Infrared Spectral Features in the MIR How the materials of various physical phases evolves in the Universe? SNe as dust budgets in the early universe? Process of dust nucleation, grain growth and destruction of Dust Chemical Evolution of the ISM Mid-R Spec. from 12 to 38m ionized gas ;[NeII] 12.81mm, [Ne III] 15.56mm, 36.01mm, [NeV] 14.32 mm, [S III] 33.48mm, 18.71mm, [SIV] 10.51mm, [PIII] 17.89mm, [ArIII] 21.83mm,[ArV] 13.07mm, [OIV] 25.89mm, [SiII] 34.82mm, [Fe II] 25.99 mm, 35.35mm, 17.94mm, 24.5mm, [FeIII] 22.93mm, 33.04mm molecular gas;H2 S(0) 28.219mm, S(1) 17.035mm, S(2) 12.279mm, C2H2 (n5=1-0)13.7mm, HCN (n2=1—0) 14.04mm, 12CO2 14.9mm 12 solid phase molecules and dust grains; GEMS, MgS, FeS, PAHs, crystalline silicates Formation Mechanism of Gas Giant Planets Initial Conditions Required for Terrestrial High-R Spec. at MIR Planet Formation Observing the dissipation of gas and their structural evolution in planet-forming regions The profiles of molecular emission lines (CO, H2O, HCN, CO2, C2H2) in the MIR useful to understand how the structure of gas disks evolve in the course of planet formation 13 MCS : Instrument Overview 5 -- 38mm Camera and Spectrometer Wide Field Camera 5 arcminutes square FOV x 2, ll 5--25 and 20--38mm Mid Resolution Spectrograph IFU by image slicer R:(1900--3000)+(1100 --31500) ll (12.2--23.0)+(23.0--37.5)mm at once High Resolution Spectrograph R : 20,000 ~ 30,000 ll 4--8 mm and 12--18mm Low Resolution Spectrograph R ~ 50--100 ll 5-26mm and (20-38 or 25-38(or 48))mm 14 Fore-Optics Fore-Optics LRS 15 Design: Optical architecture (full option) 16 Design: Optical architecture (base line) 17 Fore-Optcs Relay optics with Collimator + Camera Free-surface mirror Wide FOV including WFC+(MRS/HRS)+LRS Compensate telescope aberrations 18 WFC-S FOV: 5’ x 5’ Diffraction limited image Zodiacal light limit noise 5 -- 25mm Si:As 2048x2048 0.”146 fov/pix 19 WFC-L FOV: 5’ x 5’ x 2 field Diffraction limited image Zodiacal light limit noise 20 -- 38mm Si:Sb 1024x1024 0.”293 fov/pix 20 Medium Resolution Spectrograph (MRS) MRS-S 12.2 – 23.0 mm R 1900 – 3000 Si:As 2k x 2k pixel scale 0”.403 MRS-L 23.0 – 37.5 mm R 1100 – 1500 Si:Sb 1k x 1k pixel scale 0”.485 Image Slicer (slit length x width x slices) MRS-S; 12” x 1”.2 x 5 MRS-L; 12” x 2”.5 x 3 sharing the same FOV, 21 High Resolution Spectrometer (HRS) Specifications of HRS Array format Wavelength coverage Spectral resolution (R=λ/Δλ) Pixel scale Slit length x width Main disperser HRS-L HRS-S Si:As (2k x 2k) Si:As (2k x 2k) 12-18 μm 4-8 μm 20,000-30,000 30,000 0.48“/pix 0.288“/pix 6.0” x 1.2” 3.5” x 0.72” CdTe or CdZnTe immersion grating ZnSe immersion grating Optical layout 23 24 Spec.: Low Resolution Spectrograph (LRS) Wide wavelength coverage High sensitivity LRS-S 5 -- 26 mm covered by KBr prism 2’.5 x 1”.40 long slit R ~ 50 -- 100 LRS-L 20 -- 50 mm prism CsI 2’.5 x 2”.66 long slit R ~ 50 – 100 S and L shares the same FOV 25 LRS optics and configuration 26 WFC expected performance For both WFC-S (Si:As 2k x 2x)/WFC-L(Si:Sb 1k x 1k) Pixel scale:0.36 arcsec Frame integration:617.3 s Background (Zodiacal light) 261K BB18MJy/str at 25mm. Total integration time:3600s Aperture photometry within the first diffraction null ring 27 MRS expected performance Pixel scale, wavelength band width : value in the optical design Frame integration time: 300s for MIR-S / 600s for MIR-L High Background : BB T=268.5K normalized to 80 MJy/sr at 25μm Low Background : BB T=274.0K normalized to 15 MJy/sr 28 HRS expected performance Pixel scale, wavelength band width : value in the optical design Fowler-16 sampling – Read noise: 5 electron/pix/read-out Frame integration time: 300s High Background : BB T=268.5K normalized to 80 MJy/sr at 25μm Low Background : BB T=274.0K normalized to 15 MJy/sr 29 MCS: 開発状況まとめ 光学設計 : よい設計解を見つけた トレランス解析結果も良好 調整方法もシミュレートし、方向性確立 構造設計: 最も複雑なMRS部分でお試し設計 意外にも軽くできそう 光学素子: エマルジョン回折格子の試作成功 ミラーの製造もうまくいきそう フィルターの開発は継続 検出器:Si:AsはJWSTからの拡張 Si:Sbは低暗電流が実現しそう 熱設計も大丈夫そう SPICA指向揺らぎ:大きい!Tip-tiltが必要に 30 MCS: Next step On-going review process mid-term report mandatory : WFC , MRS high rated option : HRS-L option : HRS-S, LRS final report within a half year Focus on the reduced function is necessary! Scientific operation plan should be developed 31 LRS LRS R ~ 50--100 ll 5-26mm and 20-38mm Full field grism/prism in WFC + Short slit at the edge of FOV Binning MRS 32 Wavelength coverage 5 12.2 23 LRS-S 37.5 LRS-L MRS Short Slit : 7arcsec WFC 293 x 300 arcsec WFC-S grism 5 -- 9 8 --14.5 WFC-L grism 13 -- 23 21 -- 38 MRS Slitless / Small Slit / Slit and LVF exchange wheel ? MCS : Collaborations with ASIAA ASIAA:検出器の供給/サイエンス検討 MCSプロポーザル改定・レガシー観測提案で共同作業 SAFARIとの協力 MCS+SAFARIでSPICAを認めてもらわねば レガシー観測提案にはSAFARIも含めよう 34 SAFARI 35 36 37 38 39 40 41 42 43 44 SCI 45 Establish MIR “Spectral Atlas” of exoplanet atmospheres Spatially resolved, spectroscopic characterization of planet atmosphere is a key to understand planet formation. NIR - MIR spectrum of the planet atmosphere is rich in various molecular features, which is difficult to access from the ground. (Hanel et al. Sci, 206, 952, 1979) MIR Spectrum of Jupiter by Voyager Detailed MIR spectrum of planet atmosphere we know so far is only from our solar planets (Jupiter, Saturn, etc). Coronagraph with Spectroscopic capabilities MIR Spectrum of exoplanets Coronagraphic observation for exoplanets in 2020’s • JWST and Large groundbased telescopes (e.g. TMT) – Powerful tools for discovery of many exopalnets – Spectroscopic capability is very limited (Marois et al. 2008) • SPICA-SCI – Unique tool for charcterization by wide IR spectroscopy with coro. Figure by Fukagawa Kalas et al. (2008) Thalman al. (2009) Fine synergy: productive and complementally! SPICA Coronagraph Instrument (SCI) Scientific objectives Instrument Design Detection and characterization of Jupiterlike planets by direct imaging and spectroscopy Study of physical parameters and atmospheric compositions of exoplanets Establish “Infrared Spectral Atlas” of exoplanet atmospheres Binary pupil mask as a coronagraph Contrast after PSF subtraction = 106 (Raw contrast = 104) High-contrast coronagraphic imaging spectroscopy (R = ~ 20, 200) Project status International review is ongoing Binary Pupil Mask Target of SCI: Young and matured Jupiter-like planets Direct detection and spectroscopy of nearby Jupiter-like planets 1Gyr Young (<1Gyr), ~ 1MJup planets Matured (< 5Gyr), a few MJup planets Survey strategy: Young stars in young associations (<1 Gyr, <50pc) 5Gyr Very nearby, Matured stars (<5Gyr, 10pc) Over 200 target stars Planet model atmospheres and the sensitivity of SCI Figures from M. Fukagawa Target of SCI:Follow-up Observation of Known Exoplanets Follow-up observations of exoplanets discovered by ground-based direct imaging Complementary to NIR ground-based observations Contrast, sensitivity is enough for most of the targets IWA is a main limitation A number of targets will significantly increase in a next decade HR8799 b HR8799 c HR8799 d HR8799 e Fomalhaut b Beta pic b 2M J044144 b 2M1207 b AB Pic b UScoCTIO 108 b 1RXS 1609b (Marois et al. 2008) Ross 458AB c GSC 0621400210 b HIP78530 b CD-35 2622 b SR 12AB b CFBDS 1458 b GQ Lup b C3.5µm C4.7µm C10µm C15µm 5.89E-06 9.11E-06 1.44E-04 2.30E-04 1.70E-05 1.63E-05 2.72E-04 3.15E-04 1.70E-05 1.63E-05 2.72E-04 3.15E-04 1.20E-05 1.37E-05 2.28E-04 2.90E-04 1.49E-04 1.01E-04 1.04E-02 4.91E-03 3.15E-02 2.05E-02 1.53E-02 1.25E-02 1.78E-03 1.59E-03 1.74E-02 1.69E-02 8.55E-04 3.13E-05 5.55E-07 1.95E-04 1.21E-05 1.89E-06 4.20E-03 1.37E-04 1.43E-05 3.99E-03 1.28E-04 5.58E-05 1.11E-04 3.13E-06 3.22E-03 6.14E-03 3.83E-04 1.74E-04 4.18E-05 1.18E-06 1.18E-03 2.18E-03 1.61E-03 6.80E-05 3.41E-04 3.19E-06 1.17E-02 1.62E-02 1.39E-02 5.08E-04 3.13E-04 5.21E-06 1.11E-02 1.42E-02 5.63E-02 4.68E-04 Contrast of directly image exoplanets (estimation by T. Matsuo) Specifications of the instrument Observation mode Coronagraph method Guaranteed contrast @PSF* Spectral Resolution in Inner - Outer working angle FoV Detector and channel Wavelength coverage Coronagraphic Imaging Spectroscopy Binary pupil mask Raw contrast > 10^4 After PSF subtraction >10^6 ~ 5, 20, 200 3.3 – 12 λ/D (mask1) 1.7 – 4.5 λ/D (mask2) 1’ x 1’ Short channel: 2k x 2k InSb (λ<5μm) Long channel: 2k x 2k Si:As (λ>5μm) 3.5-27mm (Coronagraph Imaging/spectroscopy) 1-27mm (Non- coronagraph Imaging/spectroscopy) High-contrast Region Binary Pupil Mask Star PSF Current Development Status Basic optical design was finished Simplification for a robust design Deformable mirror is omitted Focal-plane mask without moving mechanism Key technology development Binary pupil mask Cryogenic testbed Diamond turning metallic mirror SCI simulation software Simulation Examples Contrast enhancement by a PSF subtraction method, under the existence of telescope pointing error = 0.06” Contrast after PSF subtraction ~ 106 (Raw contrast=104) Spectroscopy + PSF subtraction Target: K5V, PSF reference: A0V star 5um Contrast = 5.5E-7 SCI: Sumarry SPICA Coronagraph Instrument (SCI) is a high-contras imaging spectrometer for SPICA Scientific Objectives Detection and Characterization of Jupiter-like planets (<5 Gyr) by direct imaging and spectroscopy Study of physical parameters and atmospheric compositions of exoplanets Establish MIR “Spectral Atlas” of exoplanet atmospheres Development Status Basic optical design was done Simplification for a robust design (no DM, focal plane mask) Key technologies development is ongoing (Free-standing mask, cryogenic optical testbed, mirrors etc) SCI simulation software