Sci spica coronagraph instrument
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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


Sci spica coronagraph instrument

Resource Requirements


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


Sci spica coronagraph instrument

Development and Test Plan


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


Sci spica coronagraph instrument

Observing Program


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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