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SPICA 装置検討状況と展望. H. Kataza (ISAS/JAXA) SPICA 検討チーム. 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?. - PowerPoint PPT Presentation
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SPICA 装置検討状況と展望
H. Kataza (ISAS/JAXA)
SPICA 検討チーム
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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?
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SPICA Scientific objectives (Mission Definitions)
Resolution of Birth and Evolution of Galaxies
Transmigration of Dust in the Universe Thorough Understanding of Planetary
System Formation
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Requirements High spatial resolution
→ 3m-class telescope
Wavelength coverage 5 to 200m Wide Field of View Unique capabilities
→ 3m-class telescope
High sensitivity→ T<10K
Instruments on board SPICA MCS : Mid Infrared Camera and Spectrometer
Wide field Imaging, mid and high res. spectroscopy wavelength coverage : 5-38m
SAFARI : Far Infrared Imaging Fourier Spectrometer Wide field Imaging spectrometer wavelength coverage : 34-210m
SCI : SPICA Coronagraph Instrument Coronagraphic imaging and spectroscopy wavelength coverage : 3.5-27m Dedicated instrument for exoplanets study
FPC-S : NIR Focal Plane Camera for Sience Wide field Imaging and Low Res. Spec. with LVF wavelength coverage : 0.7-5.2m
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Focal Plane InstrumentsWavelength coverage vs Resolving Power
λ
v
2 m 20 m 200 m
100(3000 km s-1)
1000(300 km s-1)
10000(30 km s-1)
Herschel
JWST
SPICA
FPC-S
MCS/HRS
SCISAFARI
MCS/WFC/LRS
MCS/MRS
Wavelength
US Inst
Unique Capability of SPICA/FPIs
SPICA PLM (payload module)
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FPIA: Focal Plane Instrument Assembly
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Focal Plane map
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MCS
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Unveiling the Role of Environment in the Early Universe
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 = 5 z = 1
Yahagi et al. (2005)M=6×10^14 Msun, 20Mpc×20Mpc (co-moving)
MCS/WFC
JWST/MIRI
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Wide Field of View 5’x5’ Imager
Life cycle of dust revealed by Infrared Spectral Features in the MIR
ionized gas ; [NeII] 12.81m, [Ne III] 15.56m, 36.01m, [NeV] 14.32m, [S III] 33.48m, 18.71m, [SIV] 10.51m, [PIII] 17.89m, [ArIII] 21.83m,[ArV] 13.07m, [OIV] 25.89m, [SiII] 34.82m, [Fe II] 25.99m, 35.35m, 17.94m, 24.5m, [FeIII] 22.93m, 33.04m molecular gas ; H2 S(0) 28.219m, S(1) 17.035m, S(2) 12.279m, C2H2 (5=1-0)13.7m, HCN (2=1—0) 14.04m, 12CO2 14.9m solid phase molecules and dust grains ; GEMS, MgS, FeS, PAHs, crystalline silicates
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Mid-R Spec. from 12 to 38
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
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
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Formation Mechanism of Gas Giant Planets Initial Conditions Required for Terrestrial Planet Formation High-R Spec. at MIR
MCS : Instrument Overview
5 -- 38m Camera and Spectrometer Wide Field Camera
5 arcminutes square FOV x 2, 5--25 and 20--38m Mid Resolution Spectrograph
IFU by image slicer R:(1900--3000)+(1100 --31500) (12.2--23.0)+(23.0--37.5)m at once
High Resolution Spectrograph R : 20,000 ~ 30,000 4--8 m and 12--18m
Low Resolution Spectrograph R ~ 50--100 5-26m and (20-38 or 25-38(or 48))m
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Fore-OpticsFore-Optics
HR
S
WFC
-S
MR
SW
FC-L
LRS
Design: Optical architecture (full option)
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Design: Optical architecture (base line)
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Fore-Optcs
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Relay optics with Collimator + Camera
Free-surface mirror
Wide FOV including WFC+(MRS/HRS)+LRS
Compensate telescope aberrations
WFC-S
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FOV: 5’ x 5’
Diffraction limited image
Zodiacal light limit noise
5 -- 25m
Si:As 2048x2048 0.”146 fov/pix
WFC-L
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FOV: 5’ x 5’ x 2 field
Diffraction limited image
Zodiacal light limit noise
20 -- 38m
Si:Sb 1024x1024 0.”293 fov/pix
Medium Resolution Spectrograph (MRS)
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MRS-S 12.2 – 23.0 m R 1900 – 3000 Si:As 2k x 2k pixel scale 0”.403MRS-L 23.0 – 37.5 m R 1100 – 1500 Si:Sb 1k x 1k pixel scale 0”.485Image 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,
High Resolution Spectrometer (HRS)
HRS-L HRS-S
Array format Si:As (2k x 2k) Si:As (2k x 2k)
Wavelength coverage 12-18 μm 4-8 μm
Spectral resolution (R=λ/Δλ) 20,000-30,000 30,000
Pixel scale 0.48“/pix 0.288“/pix
Slit length x width 6.0” x 1.2” 3.5” x 0.72”
Main disperser CdTe or CdZnTe immersion grating ZnSe immersion grating
Specifications of HRS
Optical layout
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Spec.: Low Resolution Spectrograph (LRS)
Wide wavelength coverage High sensitivity LRS-S 5 -- 26 m covered by KBr prism 2’.5 x 1”.40 long slit R ~ 50 -- 100
LRS-L 20 -- 50 m prism CsI 2’.5 x 2”.66 long slit R ~ 50 – 100
S and L shares the same FOV 25
LRS optics and configuration
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WFC expected performance
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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 25m.
Total integration time:3600s Aperture photometry within the first diffraction null ring
MRS expected performance
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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
HRS expected performancePixel 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
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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
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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
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LRS
LRS R ~ 50--100 5-26m and 20-38m Full field grism/prism in WFC + Short slit at
the edge of FOV Binning MRS
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Wavelength coverage
5 12.2 23 37.5
LRS-S LRS-LMRS
WFC-S grism
MRS
5 -- 98 --14.5
13 -- 2321 -- 38
WFC-L grism
Slitless / Small Slit / Slit and LVF exchange wheel ?
Short Slit : 7arcsec WFC 293 x 300 arcsec
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
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SAFARI
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SCI
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Establish MIR “Spectral Atlas” of exoplanet atmospheres
(Hanel et al. Sci, 206, 952, 1979)
MIR Spectrum of Jupiter by Voyager
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).
MIR Spectrum of exoplanets
Coronagraph with Spectroscopic capabilities
Coronagraphic observation for exoplanets in 2020’s
• JWST and Large ground-based telescopes (e.g. TMT)– Powerful tools for discovery
of many exopalnets– Spectroscopic capability is
very limited
• SPICA-SCI– Unique tool for
charcterization by wide IR spectroscopy with coro.
Fine synergy: productive and complementally!
(Marois et al. 2008) Kalas et al. (2008)Thalman al. (2009)
Figure by Fukagawa
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
1Gyr
5Gyr
Planet model atmospheres and the sensitivity of SCIFigures from M. Fukagawa
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
Target of SCI: Young and matured Jupiter-like planets
C3.5µm C4.7µm C10µm C15µmHR8799 b 5.89E-06 9.11E-06 1.44E-04 2.30E-04HR8799 c 1.70E-05 1.63E-05 2.72E-04 3.15E-04HR8799 d 1.70E-05 1.63E-05 2.72E-04 3.15E-04HR8799 e 1.20E-05 1.37E-05 2.28E-04 2.90E-04Fomalhaut b - - - -Beta pic b 1.49E-04 1.01E-04 1.04E-02 4.91E-032M J044144 b 3.15E-02 2.05E-02 1.53E-02 1.25E-022M1207 b 1.78E-03 1.59E-03 1.74E-02 1.69E-02AB Pic b - - - -UScoCTIO 108 b 8.55E-04 1.95E-04 4.20E-03 3.99E-031RXS 1609b 3.13E-05 1.21E-05 1.37E-04 1.28E-04Ross 458AB c 5.55E-07 1.89E-06 1.43E-05 5.58E-05GSC 06214-00210 b 1.11E-04 4.18E-05 3.41E-04 3.13E-04HIP78530 b 3.13E-06 1.18E-06 3.19E-06 5.21E-06CD-35 2622 b 3.22E-03 1.18E-03 1.17E-02 1.11E-02SR 12AB b 6.14E-03 2.18E-03 1.62E-02 1.42E-02
CFBDS 1458 b 3.83E-04 1.61E-03 1.39E-02 5.63E-02GQ Lup b 1.74E-04 6.80E-05 5.08E-04 4.68E-04
(Marois et al. 2008)
Contrast of directly image exoplanets (estimation by T. Matsuo)
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
Target of SCI:Follow-up Observation of Known Exoplanets
Specifications of the instrumentObservation mode Coronagraphic Imaging SpectroscopyCoronagraph method Binary pupil maskGuaranteed contrast @PSF* Raw contrast > 10^4
After PSF subtraction >10^6Spectral Resolution in ~ 5, 20, 200 Inner - Outer working angle 3.3 – 12 λ/D (mask1)
1.7 – 4.5 λ/D (mask2) FoV 1’ x 1’Detector and channel Short channel: 2k x 2k InSb (λ<5μm)
Long channel: 2k x 2k Si:As (λ>5μm) Wavelength coverage 3.5-27m (Coronagraph Imaging/spectroscopy)
1-27m (Non- coronagraph Imaging/spectroscopy)
Binary Pupil MaskStar PSF
High-contrastRegion
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
5um
Contrast = 5.5E-7
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
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