current status of spica fpi mechanical i/f & resources
DESCRIPTION
Current Status of SPICA FPI Mechanical I/F & resources. April 6 th 2010 Hideo Matsuhara (ISAS/JAXA) & FPI team. Japanese, Korean, European. SPICA Focal Plane Instruments - overview. MIRACLE (Mid- InfRAred Camera w/o LEns ). Now 5’x5’ is baseline. 2K x 2K. - PowerPoint PPT PresentationTRANSCRIPT
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Current Status of SPICA FPIMechanical I/F & resources
April 6th 2010Hideo Matsuhara (ISAS/JAXA) & FPI team
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SPICA FOCAL PLANE INSTRUMENTS - OVERVIEW
Japanese, Korean, European
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MIRACLE (Mid-InfRAred Camera w/o LEns)
MIRACLE is a mid-IR instrument with imaging and low-resolution spectroscopy consisting of two channels:
• Filter-wheel : imaging band (R~5) & spectroscopy with grism/prism (R~100)
2K x 2K
Now 5’x5’ is baseline
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MIRMESMid-IR Medium-resolution Echelle Spectrograph
ARM-S ARM-L
array format Si:As (2k x 2k) 25 mm/pix
Si:Sb (1k x 1k) 18 mm/pix
Wavelength coverage 10.0mm-19.9mm 19.9mm-35.0mm Spectral resolution (R=l/Dl) ~1400 ~750 pixel scale 0.409 (“/pix) 0.413 (“/pix) Slit width 1”.7 (4.2pixel) 2”.5 (6.1pixel)
FOV size 12” x 8”.5 14” x 12”.5
Arm-S Echelle order lmin (mm) lmax (mm) 4 15.53 19.97 5 12.71 15.53 6 10.75 12.71 7 (9.98) 10.75※ lmin and lmax are defined as the wavelength at which the grating efficiency drops to 40%
of the peak
Arm-L Echelle order lmin (mm) lmax (mm) 5 29.4 35.0 6 24.4 29.4 7 21.2 24.4 8 (19.9) 21.2
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MIRHESMid-IR High-resolution Echelle Spectrograph
Japanese-led ( Univ. Tokyo/ISAS ) Detector array : 2Kx2K Si:As IBC Immersion Grating for L-mode is very difficult with
the material high-blaze grating(~30cm long)
Short(S)-mode Long(L)-mode
Wavelengths 4 – 8mm 12 – 18mmSpectral Resolving Power (R=l/Dl)
30,000 20,000 – 30,000
Slit width 0.72” 1.20”
Slit length 3.5” 6.0”
Disperser ZnSe Immersion GratingHigh-blaze reflective
Grating
Cross-disperser Reflective Reflective
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FPC-G, FPC-S Leaded by KASI, Korea
FPC-G Specification (goal) Noteswaveband I-band preliminaryDetector InSb 1024 x 1024
FOV 5’ x 5’ To obtain sufficient # (>10) of guide stars
Output interval 1Hz Typical - trade-off with 0.4HzSensitivity
(25σ) 18.6 mag (AB) Defocused to measure the
centroid in 0”.05 accuracyFPC-S Specification (goal) Notes
Wavelength
0.8 - 5mm 10pos. Filter wheel (JHKLM & LVF)
Spectral Resolution
~ 50 With LVF, and spatial slow-scanning
Detector InSb 1024 x 1024 FOV 5’ x 5’ 1 pix = 0.3 arcsec
Sens.(3σ) Imaging 26.3 mag(AB) Spectroscopy 6.84x10-20l-1W.m-2
100sec integration(l:mm)
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SCISPICA Coronagraph Instrument
A mid-IR coronagraph instrument with both imaging & low-res. spectroscopic capability.
Major goal : direct imaging & spectroscopy at 3.5-27mm
Coronagraph method Binary-shaped pupil mask (baseline) Contrast > 10-6
Field of View: 1.0 x 1.0 arcmin2
Spectral resolution : 20-200
Current status : Draft optical, structure design finished improved Tip-tilt design
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SAFARI SPICA Far-infrared
Instrument
Leaded by SAFARI consortium in Europe Imaging Fourier-transform spectrometer
covering 35-210mmFOV : 2 x 2 arcmin2
Wavelength resolution 2000 at 100 mm is maximum
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SAFARI Design @Phase-A1 conclusion
Current cold mass : 38.8kg (22% margin to 50kg allocation)
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FPI resources / Interface issues
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FPI Cold Volume
FPIA = FPI + IOBAIOBA = IOB + PoM (+ 5K shield…)
IOB : instrument optical benchPoM : Pick-off Module
f 230
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Critical I/F issues on FPIA
Stringent stiffness requirement of FPIA 150Hz (Z) / 100Hz (X, Y) !! The original concept of IOB plate (ribbed Aluminum plate) itself
does not satisfy the requirement. To overcome the above problem, two options:
[Option A] IOB made of SiC (or CFRP) [Option B] MIRACLE (& MIRMES, MIRHES) base plate will be a
part of the IOB structure (made of Aluminum)
FPI Assembly / Integration: need of Common Pick-off Module (PoM) separated from each FPI, but mechanically I/F to IOB PoM is a sub-system of IOBA No moving parts
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Concept of common PoM
Pick-off location is 100-150mm below the surface of IOB, so the PoM looks like a cylinder?
f 230
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FPI footprint on IOBEnvelopes of FPIs are now OLD
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IOB & FPI structure study – under progress..
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Field-of-Views (updated 11 Mar. 2010)
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3D Optical config. with New SCI (green)
SCI
FPC-SMIRACLE-short
MIRACLE-long
FPC-G
SAFARI
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FPI Cold Mass Allocation
FPI Weight (kg) comment
MIRACLE
60.0 with 20% margin
MIRMES
MIRHESSCI 30.0 FPC 10.0 SAFARI 50.0 US-lead instrument 30.0 (optional FPI)IOB, FPI cover 50.0 with 20% marginTotal 200 excluding US instr.
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Cold stage heat generation
Assumption: Baseline : No parallel mode Any observations will be executed by using single
FPI, excluding FPC-GCurrent Status
<15mW @ 4.5K for any observation modeExceeds [email protected] (baseline allocation for
1.7K stage) but less than 10mW
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Heat load (max/average) @4.5K stage (09/12/28)
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Heat load (max/average) @1.7K stage (09/12/28)
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Warm Electronics I/F
Located at Bus system Total Weight: 120kg, incl. 20% margin
Electric Power (=heat dissipation) Total 199W with maturity margins
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ICS-FPI
ICS (interface control specification) document should be prepared for SRR Operation mode & Observing Mode definition I/F with STA (mechanical/optical), CRYO (thermal), BM
(bus module: electrical), AOCS (pointing control I/F) Also resources for warm electronics
MIRACLE, MIRMES, MIRHES,SCI, (& FPC) will be put in ICS-FPI
For US-lead instrument, resources & I/F are described in ICS-FPI (part A)
Dedicated ICS for SAFARI (& FPC)