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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
SCI (SPICA coronagraphinstrument)

Keigo Enya & SCI team


Outline
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


Sci spica coronagraph instrument

Scientific Objectives/Targets

& Required Specifications


Scientific targets
Scientific Targets

  • Direct Detection and Characterization of Jovian Exoplanets by

    - Coronagraphic imaging

    - Coronagraphic spectroscopy

    - Monitoring of planetary transit


Consistency with mrd
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


Specification of instrument
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


Sci spica coronagraph instrument

Concept Study

Current Status


Optics optical elements 1
Optics & Optical Elements (1)

  • Overview

Beamsplitter


Optics optical elements 2
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


Optics optical elements 3
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


Detectors
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


Volume structure
Volume & Structure

  • Volume & structure: see below

  • Weight: 30 kg (including 20% margin)


Thermal design
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)


Expected performance
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



Field of view requirement
Field-of-View Requirement

  • Area: 1’ x 1’ (TBC)

  • Location: center of FOV


Thermal cryogenic requirement
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)


Pointing attitude control requirement
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


Structural requirement
Structural Requirement

  • Volume & structure: see below

  • Weight: 30 kg (including 20% margin)


Data generation rate data handling requirement
Data Generation Rate & Data Handling Requirement

  • TBD

  • Roughly ~ half of 1 channel of MIRACLE


Warm electronics
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]


Operation observing mode
Operation & Observing Mode

  • Coronagrahic

    - Imaging

    - Spectroscopy

  • Non-coronagraphic (including monitor obs.)

    - Imaging

    - Spectroscopy



Key technical issues trl
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


Development plan
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.


Test verification plan
Test & Verification Plan

  • TBD

  • Roughly similar to MIRACLE + DM operation + TTM operation


Development cost
Development Cost

  • TBD

  • Roughly (1 channel of MIRACLE) – (detectors) + TTM + DM



Observation plan to perform science targets
Observation Plan to perform Science Targets

  • Coronagraphic imaging

    - the direct detection

    - Coronagraphic spectroscopy

  • Non-coronagrapic monitor

    - Planetary transit


Outline of ground data processing
Outline of Ground Data Processing

  • Normal date reduction for MIR observation.


Organization structure for development
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


Summary
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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