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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


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


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 ([email protected])

    - 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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