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SCI (SPICA coronagraph instrument)

SCI (SPICA coronagraph instrument). Keigo Enya & SCI team. Outline. A mid-IR coronagraph instrument with both imaging and low-resolution spectroscopic capability at 3.5-27microns Scientific Objectives - Targets& Required Specifications Concept Study, Current Status

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SCI (SPICA coronagraph instrument)

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  1. SCI (SPICA coronagraphinstrument) Keigo Enya & SCI team

  2. Outline • A mid-IR coronagraph instrument with both imaging and low-resolution spectroscopic capability at 3.5-27microns • Scientific Objectives - Targets& Required Specifications • Concept Study, Current Status • Resource Requirements • Development and Test Plan • Observing Program

  3. Scientific Objectives/Targets & Required Specifications

  4. Scientific Targets • Direct Detection and Characterization of Jovian Exoplanets by - Coronagraphic imaging - Coronagraphic spectroscopy - Monitoring of planetary transit

  5. Consistency with MRD • Description in MDR Objective #1: Direct Detection and Characterization of Exoplanets To understand the diversity of the exo-planetary systems, we will attempt direct detection and characterization of exoplanets in the infrared wavelengths. Complement al two methods, coronagraphic observation and planetary transit monitoring, are described as key observations. • Therefore very consistent

  6. Specification of Instrument Parameter Specification Core wavelength (λ) 3.5−27 micron Observation mode w/wo Coronagraph, Imaging/ Spectroscopy Coronagraphic mode binary shaped pupil mask Inner working angle (IWA) ~3.3×λ/D Outer working angle (OWA) 16×λ/D Throughput ~20% Contrast 10-6 @PSF ( ~10-7 after subtraction) Detector 1k×1k Si:As, InSb array Field of View ~1’ x 1’ Spectral resolution ~20 and ~200 Filter Band pass filters Disperser for spectroscopy transmissive devices (e.g. grism) in filter whele Active optics cryogenic DM and TTM

  7. Concept Study Current Status

  8. Optics & Optical Elements (1) • Overview Beamsplitter

  9. Optics & Optical Elements (2) • Coronagraph mask (Binary shaped pupil mask) • Laboratory demonstrated with visible light Pupil mask PSF PSF (simulation) Pupil shape design Non-corona grahic direction Discovery angle Coronagrahic direction Dark region

  10. Optics & Optical Elements (3) • Active optics - Deformable mirror - Tip-tilt mirror • Other devices - Mirrors (Collimetion/Focusing) - Beamsplitter (Short/Long channel) - Disperser (Grism, Prism, etc.) - Science filters

  11. Detectors • Commercailly available detectors will be used. Detector format num. usage InSb 1k x 1k (2k x 2k is OK) 1 science short channel InSb 1k x 1k (2k x 2k is OK) 1 tip-tilt sensor Si:As 1k x 1k (2k x 2k is OK) 1 science long channel

  12. Volume & Structure • Volume & structure: see below • Weight: 30 kg (including 20% margin)

  13. Thermal Design • Cooled by only 4.5K stage • Heat load: to be updated - 16.36mW @the last report - Design to reduce heat load is ongoing. - Film Print Cable for DM control (parastic heat) - New tip-tilt mirror design (heat generation)

  14. Expected Performance Parameter Specification Core wavelength (λ) 3.5−27 micron Observation mode w/wo Coronagraph, Imaging/ Spectroscopy Coronagraphic mode binary shaped pupil mask Inner working angle (IWA) ~3.3×λ/D Outer working angle (OWA) 16×λ/D Throughput ~20% Contrast 10-6 @PSF ( ~10-7 after subtraction) Detector 1k×1k Si:As, InSb array Field of View ~1’ x 1’ Spectral resolution ~20 and ~200 Filter Band pass filters Disperser for spectroscopy transmissive devices (e.g. grism) in filter whele Active optics cryogenic DM and TTM

  15. Resource Requirements

  16. Field-of-View Requirement • Area: 1’ x 1’ (TBC) • Location: center of FOV

  17. Thermal & Cryogenic Requirement • Cooled by only 4.5K stage • Heat load: to be updated - 16.36mW @the last report - Design to reduce heat load is ongoing. - Film Print Cable for DM control (parastic heat) - New tip-tilt mirror design (heat generation)

  18. Pointing / Attitude control Requirement Both pointing accuracy and stability are determined By 1/10 x λ/D @ 5um To be realized with a internal tip-tilt mirror

  19. Structural Requirement • Volume & structure: see below • Weight: 30 kg (including 20% margin)

  20. Data Generation Rate & Data Handling Requirement • TBD • Roughly ~ half of 1 channel of MIRACLE

  21. Warm Electronics • Function component - Array driver - Deformable mirror driver - Tip-tilt mirror driver - Mask changer • Weight: 25kg including 20% margin • Volume: 400 x 500 x 200 [mm^3]

  22. Operation & Observing Mode • Coronagrahic - Imaging - Spectroscopy • Non-coronagraphic (including monitor obs.) - Imaging - Spectroscopy

  23. Development and Test Plan

  24. Key Technical Issues & TRL • Cryogenic tip-tilt mirror - Design and test are ongoing. • Cryogenic deformable mirror - Demonstrated with a proto-device • Coronagraphic optics - Demonstrated with visible light

  25. Development Plan • Cryogenic tip-tilt mirror - Design and test are ongoing. • Cryogenic deformable mirror - Demonstrated with a proto-device (32ch@95K) - Demo. of 1K ch. device @5K is in preparation. - Development of film print cable in ongoing (to reduce parasitic heat) • Coronagraphic optics - High contrast demonstrated with visible light - MIR demonstration in a cryo-chamber is in preparation.

  26. Test & Verification Plan • TBD • Roughly similar to MIRACLE + DM operation + TTM operation

  27. Development Cost • TBD • Roughly (1 channel of MIRACLE) – (detectors) + TTM + DM

  28. Observing Program

  29. Observation Plan to perform Science Targets • Coronagraphic imaging - the direct detection - Coronagraphic spectroscopy • Non-coronagrapic monitor - Planetary transit

  30. Outline of Ground Data Processing • Normal date reduction for MIR observation.

  31. Organization & Structure for Development • Scientists and engineers in JAXA, community of astronomy. • Finding and Involving engineers in companies. • K. Enya, T. Kotan, T. Nakagawa, H. Kataza, T. Wada(ISAS/JAXA), • K. Haze (SOUKENDAI, ISAS/JAXA), S. Higuchi (Univ. of Tokyo, ISAS/JAXA), • T. Miyata, S. Sako, T. Nakamura (IoA/Univ. Tokyo), M. Tamura, J. Nishikawa, • T. Yamashita,N. Narita, H. Hayano (NAOJ), Y. Itoh (Kobe Univ.), T. Matsuo(JPL), • M. Fukagawa, H. Shibai (Osaka Univ.), M. Honda (Kanagawa Univ.), • N. Baba, N. Murakami(Hokkaido Univ.), • L. Abe (Nice Univ), O. Guyon (NAOJ/SUBARU) • T. Yamamuro (Optcraft), P. Bierden (BMC), SPICA coroangarph team • To be updated

  32. Summary • We are developing SPICA Coronagraph Instrument (SCI) • Main targets of SCI is detection and characterization of exo-planets. It’s consistent with MDR. • Current design of SCI is presented. • R&Ds of key technology is successfully done or ongoing including cryo-TTM and DM. • SCI team is consisting of many scientists and engineers in JAXA, community of astronomy, companies.

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