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SCI (SPICA coronagraph instrument)

The SPICA coronagraph instrument, led by Keigo Enya and the SCI team, aims to provide advanced imaging and low-resolution spectroscopy capabilities in the mid-infrared range of 3.5-27 microns. The primary objective is the direct detection and characterization of Jovian exoplanets using coronagraphic imaging and spectroscopy methods. Current status includes ongoing design and testing of critical components such as cryogenic mirrors. The instrument is expected to significantly enhance our understanding of exoplanetary systems and their diversity through high-contrast observations and transit monitoring.

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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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