SPICA 装置検討状況と展望

1. SPICA装置検討状況と展望 H. Kataza (ISAS/JAXA) SPICA検討チーム

2. ScientificGoals • 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?

3. SPICA Scientific objectives (Mission Definitions) • Resolution of Birth and Evolution of Galaxies • Transmigration of Dust in the Universe • Thorough Understanding of Planetary System Formation

4. Requirements • High sensitivity • → T<10K • Wavelength coverage 5 to 200mm • Wide Field of View • Unique capabilities • → 3m-class telescope • High spatial resolution → 3m-class telescope

5. Instruments on board SPICA • MCS : Mid Infrared Camera and Spectrometer • Wide field Imaging, mid and high res. spectroscopy • wavelength coverage : 5-38mm • SAFARI : Far Infrared Imaging Fourier Spectrometer • Wide field Imaging spectrometer • wavelength coverage : 34-210mm • SCI : SPICA Coronagraph Instrument • 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

6. Focal Plane InstrumentsWavelength coverage vs Resolving Power Herschel l/dl (dv) MCS/HRS SPICA 10000(30 km s-1) JWST MCS/MRS 1000(300 km s-1) US Inst λ SCI SAFARI 100(3000 km s-1) FPC-S MCS/WFC/LRS 2 mm 20 mm 200 mm Wavelength Unique Capability of SPICA/FPIs

7. SPICA PLM (payload module)

8. FPIA: Focal Plane Instrument Assembly

9. Focal Plane map

10. MCS

11. Unveiling the Role of Environment in the Early Universe z = 1 z = 5 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. Wide Field of View 5’x5’ Imager JWST/MIRI MCS/WFC Yahagi et al. (2005) M=6×10^14 Msun, 20Mpc×20Mpc (co-moving)

12. Life cycle of dust revealed by Infrared Spectral Features in the MIR 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 solid phase molecules and dust grains； GEMS, MgS, FeS, PAHs, crystalline silicates 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

13. Formation Mechanism of Gas Giant Planets Initial Conditions Required for Terrestrial Planet Formation High-R Spec. at MIR 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

14. 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

15. MRS HRS Fore-Optics Fore-Optics LRS WFC-L WFC-S

16. Design: Optical architecture(full option)

17. Design: Optical architecture(base line)

18. Relay optics with Collimator + Camera Free-surface mirror Wide FOV including WFC+(MRS/HRS)+LRS Compensate telescope aberrations Fore-Optcs

19. FOV: 5’ x 5’ Diffraction limited image Zodiacal light limit noise 5 -- 25mm Si:As 2048x2048 0.”146 fov/pix WFC-S

20. FOV: 5’ x 5’ x 2 field Diffraction limited image Zodiacal light limit noise 20 -- 38mm Si:Sb 1024x1024 0.”293 fov/pix WFC-L

21. 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,

23. High Resolution Spectrometer (HRS) • Specifications of HRS • Optical layout

25. 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

26. LRS optics and configuration

27. 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 WFC expected performance

28. 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

29. 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

30. 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

31. 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

32. 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

33. Wavelength coverage 5 12.2 23 37.5 LRS-S LRS-L MRS Short Slit : 7arcsec WFC 293 x 300 arcsec WFC-S grism WFC-L grism 5 -- 9 8 --14.5 13 -- 23 21 -- 38 MRS Slitless / Small Slit / Slit and LVF exchange wheel ?

34. 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

35. SAFARI

45. SCI

46. 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. Detailed MIR spectrum of planet atmosphere we know so far is only from our solar planets (Jupiter, Saturn, etc). (Hanel et al. Sci, 206, 952, 1979) MIR Spectrum of Jupiter by Voyager Coronagraph with Spectroscopic capabilities MIR Spectrum of exoplanets

47. Coronagraphic observation for exoplanets in 2020’s • SPICA-SCI • Unique tool for charcterization by wide IR spectroscopy with coro. • JWST and Large ground-based telescopes (e.g. TMT) • Powerful tools for discovery of many exopalnets • Spectroscopic capability is very limited (Marois et al. 2008) Figure by Fukagawa Kalas et al. (2008) Thalman al. (2009) Fine synergy: productive and complementally!

48. SPICA Coronagraph Instrument (SCI) • Scientific objectives • Detection and characterization of Jupiter-like planets by direct imaging and spectroscopy • Study of physical parameters and atmospheric compositions of exoplanets • Establish “Infrared Spectral Atlas” of exoplanet atmospheres • Instrument Design • 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

49. Target of SCI: Young and matured Jupiter-like planets • Direct detection and spectroscopy of nearby Jupiter-like planets • Young (<1Gyr), ~ 1MJup planets • Matured (< 5Gyr), a few MJup planets • Survey strategy: • Young stars in young associations (<1 Gyr, <50pc) • Very nearby, Matured stars (<5Gyr, 10pc) • Over 200 target stars 1Gyr 5Gyr Planet model atmospheres and the sensitivity of SCI Figures from M. Fukagawa

50. (Marois et al. 2008) 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 Contrast of directly image exoplanets (estimation by T. Matsuo)