# Presentation: 657309

## High Contrast Imaging Activities in Japan

**A****BE****1****/T****AMURA****1****/N****ISHIKAWA****1****/M****URAKAMI****1****E****NYA****2****/T****ANAKA****2****/N****AKAGAWA****2****/K****ATAZA****2****/G****UYON****3****/B****ABA****4**

- 1*National Astronomical Observatory, Mitaka, Japan*2*Institute of Space and Astronautical Sciences, Sagamihara, Japan*3*Subaru telescope/NAOJ, Hilo, Hawaii*4*Hokkaido University, Sapporo, Japan*

***NAVIGATOR PROGRAM FORUM-2007******NASA Ames, May 17******th******-18******th****** 2007***

_***Email to***_***:****** abe@optik.mtk.nao.ac.jp***

## Our Exoplanet/Disk Exploration Approaches: Vis & IR  

**Our Exoplanet/Disk Exploration Approaches: Vis & IR **** **

***1999***

***~2014***

***200******6***

**Subaru/**
**AO188 & ExAO/**
**HiCIAO**

***~2018***

***4. Direct observations ***
***of Earth-like planets***

***2A. Direct imaging of ***
***disks & young massive planets***
***ongoing and near-future***

***Ground***

**JELT?**

***1. Indirect detection ***
***of exoplanets***
***Doppler (N2K survey)***
***&***
***Transit ongoing***

## Subaru/HiCIAO

**Ground-based Projects**
**Subaru/HiCIAO**

## HiCIAO Concept

*Nasmyth platform*

*Telescope*

*Common**Optics +** ****AO****** Module***

***Coronagraph Module***

***IR Camera******Module***

***High Contrast Optics Module***

***Warm***

***Co******ld***

***Coronagraph***
*Focal masks**Pupil stops*

***Differential ******optics****(Wollaston prisms)*

***Hawaii 2-RG****2**k **** **2**k** array**ASICS Controller****Filters****Common+Differential****Pupil Viewer***
*In/out position*

***188 actuators***
***AO***_*Future*_*:**Complementary**MEM DM (32****32?)*

**HiCIAO Concept**

***Merits***
***Modular style***
***Flexible coronagraph***
***Differential Imaging***
***High performance array & controller***

*ABE Lyu, NAOJ, **NASA Navigator Forum**, **May** **18**th** **200**7*

## HiCIAO Specifications in Brief

**Wavelength Coverage**
**zJHKs bands (0.9-2.3 micron)**
**Optimized at H**** band (because of warm optics)**
**Contrast Goal**
**10^4 at 0.1” and ****10^5.5 at 1”****  with SDI/PDI mode**
**Observing Modes**** (all 0.01” / pixel scale)**
**Direct**** Imaging (DI): 20”x20”**
**High throughput imaging**
**Polarization**** Differential Imaging (PDI): 10”x20”**
**Polarizied source imaging**
**Spectral**** Differential Imaging (SDI): 5”x5”**
**Unpolarized source imaging**
**All modes with or without ****coronagraph**
**Spatial Resolution & Strehl Ratio**
**0.03”(J), ****0.04”(H)****, 0.055”(Ks)**
**0.6(J), ****0.7****(H), 0.8(Ks) @0.5" seeing**
**Detection limit**
**H>****24 mag**** (5 sigma, 1 hour)**

## HiCIAO Mechanical Design

**HiCIAO Mechanical Design**

***Warm Optics***
*** ******Field lens, mask, collimator***
*** ******Pupil***
*** ******Wollaston prism***

***Cold Optics & Detector***
*** ******Common filters***
*** ******Pupil viewer***
*** ******Differential filters***
*** ******Detector array***

*1400mm*

*<150kg*

## Schedule and Operation Plan, etc.

**Development: quick (2004-2006)**
**2004****	****	****Concept design fixed**
**2005****	****	****PDR (Sept.)**
**2006****	****	****CDR (Feb.)**
**2007****	****	****First Light**** (fall)**
**Future upgrades**
**More sophisticated coronagraph ****(PIAA lenses)**
**2****nd****-stage DM for Extreme AO ****(32********32 MEMS DM)**
**Surveys: 2008-(2011 or beyond)**
**More expanded collaborations**
**Subaru (Northern hemi.) vs. Gemini-S ??**
**Space observations (Spitzer/Astro-F/TPF targets)**

*ABE Lyu, NAOJ, **NASA Navigator Forum**, **May** **18**th** **200**7*

* * *PIAA lenses*

## Other (Lab) Experiments

**Other (Lab) Experiments**

** ****FQ-PoM & Differential Polarization Imaging**
** ****Common-Path Achromatic Interfero Coronagraph**
** ****Unbalanced Nulling Interferometer (HC pre-optics)**

## Lab Experiment on Differential Polarization Imaging

**N. Murakami****1****, N. Baba****2****, Y. Sato****2**** et al.**
- 1Nat. Astron. Obs. of Japan
- 2Hokkaido University

_***Aim***_
**Extract**** exoplanet image from ****speckle noise**
_***Method***_
**Light from ****exoplanet ****is expected to be ****partially polarized****, while speckle noises are caused by ****unpolarized stellar light****. Nulling *****stellar coronagraph with a ***_***four-quadrant polarization mask***_*** is employed. ***

*ABE Lyu, NAOJ, **NASA Navigator Forum**, **May** **18**th** **200**7*

****** ****References ****Baba & Murakami  PASP v115, p1363 – Murakami et al. PASP v118, p774**

## FQ-PoM: Experimental Results (I)

_**Star model**_**: unpolarized, λ: ****wide-band (39%)**** @ 670 (****540-****800****)nm**
_**Planet model**_**: partially polarized **(**47%**)** ******** **_**6.4×10**__**-6 **__**@ 5.3λ/D**_

*ABE Lyu, NAOJ, **NASA Navigator Forum**, **May** **18**th** **200**7*

## FQ-PoM: Experimental Results (II)

***Murakami et al. (to be submitted)***

**Latest results**

*ABE Lyu, NAOJ, **NASA Navigator Forum**, **May** **18**th** **200**7*

## Common-Path Achromatic Interfero Coronagraph (CPAIC)

**A. Tavrov****1****, T. Kurokawa****2****, Nishikawa****1**
- 1Nat. Astron. Obs. of Japan
- 2TUAT, Japan

******CPAIC**

_***Aim***_
**Stable AIC (****no OPD control****)**
_***Method***_
** ****Out of plane (3D) reflections**

****** ****Reference ****Tavrov et al. Opt. Letters v27, p2070**

## CPAIC: Experimental Result (preliminary)

**Nulling Contrasts **
**(peak)   **

**Green (cooled CCD)   1.6 x 10****-3**
**HeNe (cooled CCD)    2.5 x 10****-5**** **
**HeNe (warm CCD)      4.4 x 10****-6**

**CPAIC: Experimental Result ***(preliminary)*

## Unbalanced Nulling Interferometryfor Hi-Contrast Imaging

**J. Nishikawa, L. Abe, N. Murakami, K. Yokochi**
- Nat. Astron. Obs. of Japan

_***Aim***_
**Relax optics quality requirements for a given contrast**
_***Method***_
**Use a pre-optics setup to have a twofold effect:**
**	******** ****a low nulling device**
**	******** ****phase and amplitude magnification**

## UNI

**Downstream**
**Coronagraph**

**Second AO**
**With Two DMs**

***WFS***

**Telescope**

**First AO**

**Unbalanced **
**Nulling **
**Interferometer**

***WFS***

**UNI**

**PAC**

****** ****λ/1000 optics can virtually achieve λ/10000 quality**

***λ/1000 rms***

**⇒*****λ/1000***

***λ/100***

**⇒*****λ/1000***

***λ/1000***** ⇒*****λ/100***

***λ/10000 rms***

**⇒*****λ/10000***

***Converted to Initial WF  λ/1000***

## Unbalanced Nulling Interferometer Testbed (preliminary experiment)

## Experimental Result

***Theory***

***Experiment***

***PV: λ/4.3  RMS: λ/17  ***

***g=0.20***

***PV: λ/26  RMS: λ/112***
***PV: λ/25  RMS: λ/111***

****** ****Next step: 2 DM for phase****and amplitude correction (PAC)**

**Experimental Result**
***(Error Magnification)***

****** ****Nishikawa et al., submitted**

- Unbalance factor g

## Space Missions

**Space Missions**

** ****SPICA**
** ****JTPF (HCST)**
** ****Other Projects?**
** ****Collaboration issues**

## SPICA MISSION

*SPICA telescope concept*

**S****PICA**** M****ISSION**

** ****mIR to submm astrophysics (4.5 K cryo.)******** Complementary to JWST @ >****15****mic**
****** ****Coronagraphic mode**
** ****Direct observation of outer self-luminous planets****(20~100+ UA orbits)**
** ****Goal contrast >10****6**** within the exploration area**
** ****Benefit from monolithic pupil**

**SP****ace**** ****I****nfrared telescope for ****C****osmology and ****A****strophysics**

****** ****Succes of Akari (Astro-F) launch on Feb. 22nd 2006**

## SPICA Coronagraph Project

**SPICA Coronagraph Project**

-  *Enya et al. A&A 2007*

## High Contrast Space Telescope(HCST/JTPF) Project

| Telescope | 3.5m off-axis |
| --- | --- |
| Wavelength coverage | Visible-NIR
(λc = 0.5μm、λλ=0.2-5μm)
Possibly UV coverage |
| Launch | >2015 |
| Duration | 5-10 years |
| Orbit | Sun-Earth L2  |
| 
Instruments | Visible-NIR Coronagraph |
|  | Visible-NIR wide field spectrograph |
|  | TBD: UV-Spectrograph |

**New lightweight mirror material under evaluation ******** ZPF****(zero expansion ceramics, Iye et al.)**

**○*****=Earth at 8pc***

***Subaru***

***ELT***

***HCST***

***JWST***

***Total FOV******~******15’***

## Space Mission Collaboration

**Classes of ISAS Missions ***(new classification system)*
**Large Project (e.g. SPICA) (>> 100M$)**
- Medium Project (e.g. AKARI) (~100M$)
**Small Project (5 ~ 50 M$)**
**Small Satellite Series (Total Cost ~ 50 M$)**
- With dedicated bus system and launcher
**Pre Phase-A**
**ISAS Working Groups (e.g. SPICA WG & JTPF WG)**
**Type-A WG ***(**mission Proposal within 3 years**) *
- M/L Project WG (SPICA WG) / _Small Satellite WG_ / _Small Project WG_
- Strategic R&D Fund by Competition (total ~2M$)
- Review the Proposal, and Approval : by ISAS  JAXA  Ministry
- Mission Definition Review and System Requirement Review
**Type-B WG** *(**long time scale**)*
- Mainly for International Collaboration 	(e.g. JTPF WG  TPF, Darwin)
- Limited funding mainly for e.g. traveling
**R&D by Each Group**
- NAOJ Exo-Planet Project Team
- Hokkaido Univ.     TUAT & UEC & NAOJ
**Other **
**Planned application for a COE Program by NAOJ on AO including exo-planet as a science driver (******** 1M$/y. over 5 years)**

*Basic Research Fund for Space Instrument (ISAS)**Grant-in-Aid by MEXT*

- _Contact_:
- Takao NAKAGAWA (ISAS)nakagawa@ir.isas.jaxa.jp

**Notes:**
COE Program by Subaru for AO Development including Coronagraph & related instruments has started consideration.