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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
slide3
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

slide7
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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