WFIRST
Wide-Field InfraRed
SurveyInfra
Telescope- Red Survey Telescope)
(Wide
Field
Astrophysics Focused Telescope Assets

WFIRST-AFTA
米国Decadal
survey大型衛星1位
Final Reportby theHST,JWSTにつづくNASA最優先の次期旗艦大型衛星	
Science Definition Team (SDT) and WFIRST Project

近赤外広視野サーベイ衛星
2024年ごろの打ち上げ•暗黒エネルギー/修正重力•系外惑星•近赤外サーベイ
住 貴宏 (大阪大学), WFIRST連絡会、WACO WG
April 30, 20132015/9/15 [光赤天連シンポジウム] NAOJ

Temperature
170 K

8 positions(6 filters, GRS
grism, blank)
Grism R = 550-800(2 pixel)

6x3 FPA;Ea. square is a 4kx4k,
10µm pixel size SCA;
302 Mpix; 120K;
0.6-2.0µm bandpass
0.28 deg2 active areaand heaters. The telescope control electronics arelocated in an electronics box in the spacecraft andperform higher control functions such as commanding
Wide Field Science Channel
actuators and managing thermal set-points. Thesehigher-level commands are sent through cabling to
75 mas/pix;
Slicer
Prism
Relay
f/21
Assembly
Spectrographlocal boxes on the telescope where they are convert1 2kx2k, 18µm pixel size SCA;
R = ~100 (2 pixel)
4 Mpix; <115K;
ed to low-level signals and sent to the devices them0.6-2.0µm bandpass;
Integral Field Unit Spectrograph Channel
FOV 3.00x3.15 arcsec
selves. Each subsystem has a similar functional content with heaters, thermal sensors, and actuators. The
Optional Coronagraph Instrument
WFIRST-AFTA exception to this overall architecture is control of teleFigure 3-4: The telescope components without the outer
Relay w/
Low order
Pupil Mask
scope survival heaters. They are controlled directly bybarrel assembly.
Fixed DM
DM/FSM
WFS& Filters
the spacecraft avionics to ensure operation in theevent of an intermediate electronic failure.
and thermal distortions while providing superior stiff1kx1k, Si low noise FPA; 150K;
Imaging
IWA 0.25/λ arcsec, λ (0.4-1.0µm)
The cost, schedule, and technical risk associatedness and stability. The structure has active thermal
Detector
OWA 2.5 arcsec
Flipwith the telescope development have already been
2kx2k, Si low noisecontrol
FPA, 150K; (heaters) and is isolated from the solar array
MirrorIFS
IFS Detector 0.4-1.0µm bandpass;significantly mitigated; the telescope hardware andR~70, 17 masec samplingby the OBA to minimize heat transfer into the teleWFIRST-AFTA
supporting GSE largely exists and spare parts arescope and instrument bay.
optical block diagram.
available for most of the components. New stray light
The two telescope mirrors feed both a wide fieldaturely ending thebaffles, new thermal blankets, and new electronics
instrument (see Figure 3-6), with a wide field of view
ray/sunshield thatderived from commercial products are low risk modifichannel and an integral field unit, and an optionald of regard (seecations.
nearly on-axis (in field) coronagraph instrument. Thet the WFIRST-2.4
widefield channel includes a tertiary so that the sysTelescope&
3.3 Wide-Field Instruments study, it was detem acts as a three mirror anastigmat (TMA); the othdule level, i.e. an
The wide-field instrument is divided into two
er channels correct the residual aberrations in the firstmodule containing
Solar&Array&/&
modules, a cold instrument module (referred to as thetwo mirrors. The overall three-mirror system is able to Figure
Sunshield&
ularity will also be
3-5: The telescope entrance pupil
achieve excellent optical performance over a relativeof the observatod side, an instruly wide FOV. The most important performance re- and heaters. The telescope control electronics arech to the existing
3-5: The telescope entrance pupil
quirement for the telescope to enable the WFIRST- locatedFigure
in anelectronics box in the spacecraft andaces and provide
2.4 science is stability. Based on the low expansion
heaters.control
The telescope
controlsuch
electronics
ares. The instrument
performandhigher
functionsas commanding
materials,
located in an electronics box in the spacecraft and
Wide&Field& the thermal design, and the active heater, with design herandmanaging
thermalInstrument&
perform
highercontrol functions
such as set-points.
commanding These
control,
the wavefront stability delivered to the wide actuators
strument modules
Coronagraph&
actuatorscommands
and managingare
thermal
These
Instrument&Carrier&sentset-points.
throughcabling tofield imager is modeled to be <0.15 nm rms over one higher-level
Instrument&route power and(blue&truss)&
higher-levelcommands
aresent
throughcablinge instrument mod24-hour GEO orbit thermal cycle.
local boxeson thetelescope
where
they
areto convertlocal
boxes
on
the
telescope
where
they
are
convertbetween the two
The telescope electronics were not included with ed to low-levelsignalssent
to devices
the devices
ed to low-levelsignals andand sent
to thethem- themSpacecra3&
the 2.4-m telescope. The current plan is to upgrade
selves.
Eachsubsystemhasasimilarfunctional
conedge, and stability
selves. Each subsystem has a similar functional
conBus&mostoftheelectronics
withthecurrent
commercial
tent
with
heaters,
thermalsensors,
andactuators.
The
apes and precisetent withheaters,
sensors,is control
and actuators.
The
exception
to thisthermal
overall architectureof teleproducts.
TheFigureelectronics
is a traditional
Figure 3-3: WFIRST-2.4 Observatory configuration
featurnd SN fields and3-4: The architecture
telescope components
without the outerFigure
3-6:
Ray
trace
throughthetelescope
to
the
wide
$10M
overavionics
FY13through& $56M
over
FY14
forTheyWFIRSTing the 2.4-m telescope, two modular instruments
and adesign
scopetosurvival
heaters.
are controlledisdirectly
by of teleexception
thisoverallarchitecture
controlhierarchicalfrom spacecraft
between 54˚ andbarrelassembly.
Figure3-4:
The
telescopecomponents
without
the
outer
field
channelintermediate
focus.
modularspacecraft.
bus
thespacecraft
avionics
toensureoperationintheervation of microtelescope control to local boxes to peripheral devices scope survival heaters. They are controlled directly by
Guiding in imaging mode performed
using guiding functions contained in the
6x3 science SCAs

2.4m WFIRST-AFTA(Astrophysics Focused Telescope Assets )	

• 口径：2.4m (HSTと同じ)、NRO（国家偵察局）から譲渡 	• 28.5 度傾斜静止軌道(ロボットサービス) or L2(アトラス V 541 )	
• 広視野分光撮像・コロナグラフ装置 	
可視光・近赤外（0.6-2μm）270K	
• 寿命：５年＋１年	

barrel assembly.

event of an intermediate electronic failure.
and thermal distortions while providing superior stiffthe
spacecraft
to technicalensureriskoperation
The cost,avionics
schedule, andassociated in theness and stability. The structure has active thermal
withthetelescopedevelopment
havealreadybeen
control (heaters) and is isolated from the solar array0.788° wide
0.427° highX gaps 2.5mm
Y gaps 8.564mm

4k x 4k pixel
H4RG-10 IR検出器を18 個
6x3 H4RG @ 0.11"/p, 0.328 sq.deg
0.11 arcsec/pixel
0.28 deg2

Moon (average size seen from Earth)

HST/ACS

HST/WFC3

JWST/NIRCAM

Each square is a H4RG-10~90 × bigger than HST–ACS FOV,~200 × bigger than IR channel of WFC3 4k x 4k, 10 micron pitch
Slitless spectroscopy with grism in filter wheel
R_θ ~ 100 arcsec/micron
3

288 Mpixels total

Flux Fν (µ Jy)

Hubble x 200 Discovery of High-z Galaxies	
DRM1

WFIRST-2.4

Wavelength (µm)

z = 10.8 Galaxy!

High zまで	
銀河のクラスタリング	
構造進化	
を高精度で観測	4

Euclid

HST WFC3/IR CLASH cluster, simulated to WFIRST-2.4

AFTA: 15x more sensitive
10x sharper弱重力レンズによる暗黒物質分布

WFIRSTで５億個の	銀河の形を測定 	

Figure 2-12: Mass density contours around the cluster MACS J1206.2-0848 derived from a ground-based weaklensing survey with Subaru (red) vs. a weak lensing study with HST/ACS+WFC3 (white). The 10x higher surface density of lensed galaxies achieved from space yields ~3x higher spatial resolution maps. The HST data
shown here is representative of the WFIRST-2.4 HLS. WFIRST-2.4 will make a map of this quality over 2,000
square degrees as part of its high latitude survey, a thousand-fold increase over the HST COSMOS mass map.

WFIRST-AFTA観測計画概要

Ø 暗黒エネルギー/修正重力(~2.5年)

u High Latitude Survey (HLS)（銀河分布）

2000平方度、撮像(YJH)＋分光 (R~800) Y<26.7, J<26.9, H<26.7, F184W<26.2
・弱い重力レンズ現象（WL）
暗黒物質、構造進化	
・Red shift space distortion (RSD)!"#$%&&#'#(%)*+,$#-.%+/*0+$01$)"#$2+*3
・Baryon Acoustic Oscillation (BAO)

uIa型超新星探査

️宇宙の加速膨張史	

L0+'#H$#)$%'$6FDD$$456$789%$"

5, 9, 27平方度、撮像モニタリング＋IFU分光 (R~100)Ø 系外惑星：u 重力マイクロレンズ観測 (~1年)
銀河系中心方向、大軌道半径惑星の分布u コロナグラフ観測(~1年)
可視、コントラスト 10-9, IWA 0.2”

Ø Guest Observer 観測（25%,1.5年）
7	

/01'2*%31,+1'%+'4##1$1,4-%*5''4-'
67787779'#)*:%&1*#1'$131$'

!"-$$

$

91$$!<$=$>?#"=$&)#$$!$!<$$&'0/#$)0$$@!""#"$%&"'()"*+(,-."$$!$8##A$"*,"$.(#&*/*0+$A%)%$)0$B+0C$*1$/$!<$=$DEFF$!$%..%(#+)$%&&#'#(%)*0+$.(0AG&#A$;H$%$I&0//$!<$*/$+0)$&0+/)%+)$!$0,"0&"1234560*5+"2578"-4-793:"(7#/$)"#$/0G(&#$01$)"#$%..%(#+)$%&&#'#(%)*0+$*/$+0)$$IA%(B$#+$$$!"#$%&'("$)*+(%,--)./)0%(,1234"))))))))))))
MG&'*A$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$9>N2$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$

2015/09/15	

期待される成果の例	

Figure 2-10: Cumulative
numberof high-z galaxies ex高銀緯領域サーベイ(HLS)
での高赤方偏移銀河数
pected in the HLS. JWST will be able to follow-up onの累積分布。高赤方偏移銀河は、
JWST や TMT
these high z galaxies and make detailed observations ofで詳細な追観測が可能。初期銀河の理解には、
their properties. For understanding the earliest galaxies,
広視野のWFIRST-AFTAと大口径のや
the synergy of a wide-field telescope
thatJWST
can discover
TMTとのシナジーが非常に強力である。
	 aperluminousor highly magnified systems and a large	 ture telescope that can characterize them is essential;
WFIRST-2.4 and JWST are much more powerful thaneither one alone.

Figure 2-7: Δχ2 = 1 error ellipses on the value of the darkenergy equation-of-state parameter w at redshift z = 0.47
FigureTheof the cumulative
WFIRST
で期待される暗黒(theredshift 2-11:
at which
it isratio
best determined
by WFIRST- number o
2.4)
and its derivative
withdetected
respect to withexpansion
factorredshiftgalaxies
WFIRST-2.4
to theエネルギーの状態方程式パラメータ
dw/da.
The
green
ellipse,centered
here
on
the
cosmologberdw/da)
detected with a smaller DRM1 version of WF(w,
ical
constant model の制限の予想。
(w = -1, dw/da = 0), represents cur2.4 m aperture
to 20 times
more
rentThestate-of-the-art
constraintsyields
from a up
combination
of
(w
=
−1,
dw/da
=
0
の場合
CMB,
SN, BAO, and H0 data.20 For this figure, we havegalaxies.
imaginedthat the true cosmology is w(z=0.47) = -1.022
が宇宙定数に対応)	
and dw/da = -0.18, well within current observational conhigher
densitywillerror
allow
the fordark matterstraints.
The galaxy
black ellipse
shows theforecast
the baseline WFIRST-2.4 SN, GRS, and WL surveys, commapped to a spatial resolution of ~40 – 50 kpc.
bined with CMB data from Planck, a local supernova cali-重力マイクロレンズによる系外惑星探査

WFIRSTによる地球質量惑星検出
地球の２倍
地球
地球の半分
惑星なし

3
3.5
Magnification

Magnification
by stellar lensMagnification3

2.5

Deviation Dueto Planet

2.5

2

1.5
-20

Offset from peak gives
projected separation
-10

0
日

10

銀河系バルジ内の星3億個 in 2.8 deg.2

2
20•• 15分に１回、２４時間、72日ぶっ続けで観測• ６シーズン（合計1.2年）

9.2

9.4

9.6

9.8

日

地球質量惑星による４−５時間の明るさの変化を捉える。

惑星：３千個(地球質量以下:約2百個）

WFIRSTによる惑星検出
惑星：３千個(地球質量以下:約2百個）
浮遊惑星：２千個(地球質量以下:約百個）

水星以外全ての太陽系惑星を検出可能軌道半径（天文単位）

Keplerと合わせて全ての種類の惑星の分布を解明

AFTA with Coronagraph (option)
AFTA Coronagraph Instrument

ExoPlanet Exploration Program

Telescope

Wide field
instrument

Coronagraph
Instrument

Exoplanet
Direct imaging

Exoplanet
Spectroscopy

•
•
•
•

With additional ~$100M cost	
 AFTA• Coronagraph近傍の巨大ガス惑星、氷惑星、Instrument will:• Characterize
the spectra of over a dozen
400-1000nm band pass	
超地球の撮像、分光	
radialvelocity planets.
10-9 contrast	
• Discoverand characterize up to a dozen• デブリ円盤	
more ice and gas giants.
100 milliarcsec inner working • Provide• 将来の地球型惑星直接観測
crucial information on the physics ofplanetary atmospheres and clues to planet
angle at 400nm	
formation.
（TPF）への技術実証
to decadal survey to mature• R=70 spectra and polarization • Respondcoronagraph technologies, leading to firstimages of a nearby Earth.
at 400-1000 nm	
WFIRST final report May 23, 2013
http://wfirst.gsfc.nasa.gov/

8GO & Archive sciences
1. Open Cluster and Star Forming Region IMFs to Planetary Mass!"#$%&'()%*#'+,-./0'1"#$%&2324)%*#567&2#"4"289:!
2. Exoplanet via transit andAstrometry"#$%&'!()&*+&'!
3. High-precision IR CMDs';"<38*9=#1'
of stellar populations.
()*9#8'8*":$)")$9#"&'&%#4$#8'$4'"'*%>"*3"?&%'7@A4$<"&'7@%#9>%#9#2'B"44$:%'9?6%<)4'1$4)9*)'47"<%C)$>%')9'
4. Quasars as a Reference
Frame for Proper Motion Studies)@%' %D)%#)' )@")' &$8@)' 49=*<%4' &A$#8' 1$*%<)&A' "&9#8' )@%' &$#%' 9E' 4$8@)' ?%@$#1' )@%>' <"#' "77%"*' >=&)$7&AC$>"8%1' +4%%' (<@#%$1%*' FGGH' E9*' "' *%:$%I/2' J@%#' )@$4' *"*%' "&$8#>%#)' 9<<=*40' I%' "*%' 8$:%#K' +L/' )@%'
(LMC,GB)9779*)=#$)A')9'"<<=*")%&A'$#E%*')@%'>"44'"#1'>"44'1$4)*$?=)$9#'9E')@%'&%#4$#8'9?6%<)M'"#1'+F/'"'>"8#$E$%1':$%I'9E')@%'&%#4%1'49=*<%0'9E)%#'7*9?$#8'&=>$#94$)$%4'"#1'4$N%'4<"&%4')@")'I9=&1'#9)'?%'"<<%44$?&%'I$)@'
5. Proper Motions and Parallaxesof Disk and Bulge Stars<=**%#)' )%<@#9&98A2' J@$&%' )@%' "77*9D$>")%&A' FGG' 8"&"DAC4<"&%' 4)*9#8' &%#4%4' I%' 3#9I' 9E' <=**%#)&A'
8%#%*"&&A'<9>%'E*9>'&9IC'*%49&=)$9#0'8*9=#1C?"4%1'4=*:%A40')@%'?=&3'9E')@%'4<$%#)$E$<'79)%#)$"&'9E')@%4%'(~10µas/yr)*"*%' 4A4)%>4' *%O=$*%4' +"#1' @"4' *%&$%1' =79#/' @$8@C*%49&=)$9#' E9&&9IC=7' 4)=1$%4' I$)@' )@%' P=??&%' (7"<%'
Q%&%4<97%'+R$82'LM'%2820';*9I#%'%)'"&2'FGGS0';9&)9#'%)'"&2'FGGH/2'Q@%'4">%'@"4'?%%#')*=%'E9*')@%'4$>$&"*'
6. White dwarfs.
#=>?%*'9E'<&=4)%*C4<"&%'4)*9#8'&%#4'4A4)%>4'+%2820'(>$)@'%)'"&2'FGGT/2''
7. Nearby Galaxies'($>7&A' >"3$#8' "' 7*%<$4%' >%"4=*%>%#)' 9E' &%#4' 4)")$4)$<4' 7*9:$1%4' <94>98*"7@$<' $#E9*>")$9#' E*9>' )@%'
8. Galaxy Structure and Morphology)9)"&' &%#4' <9=#)40' )@%' 49C<"&&%1' U&%#4' *%14@$E)' )%4)V' +%2820' W"7%&9' X' Y")"*"6"#' FGGZ/2' [E' )@%' &%#4' >"44'
1$4)*$?=)$9#' $4' I%&&C<9#4)*"$#%10' "4' $#' )@%' <"4%' 9E' U<9>79=#1' &%#4%4V0' I@%*%' >=&)$7&%' 49=*<%4' &$#%' =7'
9. Evolution of Massive Galaxies?%@$#1' )@%' &%#4$#8' 8"&"DA' 9*' <&=4)%*0' )@%' &%#4' 8%9>%)*A' <"#' ?%' =4%1' )9' >%"4=*%' *")$94' 9E' 1$4)"#<%4'\'<9>79=#1'&%#4%4'"*%'4)"#1"*1'*914'E9*'7*9?$#8')@%']#$:%*4%^4'%D7"#4$9#'3$#%>")$<4'I$)@'@$8@'7*%<$4$9#'
10.Distant, High Mass Clustersof Galaxies+_9&4%'%)'"&2'FGGF0'_":"NN$'%)'"&2'FGG`/2'P9I%:%*'8"&"DAC4<"&%'<9>79=#1'&%#4%4'"*%'*"*%0')A7$<"&&A'6=4)'La'
9E' 8"&"DAC4<"&%' &%#4%40' "#1' 9#&A' ?A' $>"8$#8' "' 4=?4)"#)$"&' E*"<)$9#' 9E' )@%' 43A' <"#' I%' E$#1' 4=<@' 89&1%#'
11. Obscured Quasars&%#4%42''
12.Strongly Lensed Quasars
JR[b(Q';"4%1'9#'P=??&%'4=*:%A4'9E'"'E%I'4O="*%'1%8*%%40'I%'
13.Strong Lensing%D7%<)'4)*9#8'&%#4%4')9'@":%'"#'"?=#1"#<%'9E'"?9=)'14.High‐Redshift QuasarsLG'7%*'4O="*%'1%8*%%'+R"=*%'%)'"&2'FGG`/0'4=88%4)$#8'
and Reionization)@")' )@%' P=??&%C%*"' 4">7&%' 9E' &%#4%4' 9?4%*:%1' ")'15.Faint End of the Quasar@$8@'*%49&=)$9#'I$&&'?%'%D7"#1%1'?A'4%:%*"&'9*1%*4'9E'
Luminosity Function'>"8#$)=1%' ?A' )@%' JR[b(Q' I%"3C&%#4$#8' 4=*:%A' +%2820' 'W"7)$9#K'()*9#8'8*":$)")$9#"&'&%#4%4'$>"8%1'I$)@'
16.Probing the Epoch of Reionization
withLyman-αB"*4@"&&' %)' "&2' FGGT/0' )@%'>"69*$)A'
9E' )@%4%' I$&&' ?%'Emitters	
P=??&%2' ' JR[b(Q' I$&&' $#<*%"4%' )@%' #=>?%*' 9E'
8"&"DAC4<"&%' &%#4%42' Q@%' #=>?%*' 9E' 9?4%*:"?&%'
8"&"DAC4<"&%' &%#4%4' $4' "' :%*A' 4)*9#8' E=#<)$9#' 9E'"#8=&"*' *%49&=)$9#K' )@%' E"<)9*' 9E' 4$D' 1%8*"1")$9#' $#'*%49&=)$9#'E*9>'"'1$EE*"<)$9#'&$>$)%1'L2TC>%)%*'47"<%C4)*9#8' &%#4%4' 3#9I#' ?A' "' E"<)9*' 9E' gLGG0' )@=4'"&49' $1%#)$EA$#8' *"*%' <9#E$8=*")$9#4' \' 4=<@' "4'&%#4%1' (Y%0' &%#4%4' I$)@' @$8@%*' 9*1%*'<")"4)*97@%4' $#' )@%$*' <"=4)$<40' "#1' <9>79=#1'

日本のWFIRST参加への活動• 2010年12月、初期WFIRST Science Definition Team(SDT)に住が参加	
• 2013年 7月、WFIRST-AFTA SDTにJAXA代表として山田亨（東北大）が参加。	
	• 2013年８月、「WFIRST 連絡会」立ち上げ。	
山田亨（代表）、住（幹事）、岩田、河合、郷田、児玉、芝井、高田、田村、	
中川、宮崎、諸隈、山田（良）、塩谷、西川、村上、矢野、小谷、川原、柏川、	
田中、井上、成田、鈴木、Haze、Kwon, 大内、松尾（敬称略）他	
約３０人、2-3 か月に１回開催	

	• 2014年2月、コロナグラフ開発 WACO WG設立	
田村（PI,東大,NAOJ) 小規模プロジェクト枠（国際協力）	
早期の具体的検討が必至なコロナグラフ装置検討を先行		• 2015年3月、SDT final report（日本の潜在的興味の表明を記載、他欧州、カナダ、韓国）	
• 2015年8月NASA WFIRST Formulation Science Team公募高田(IPMU)、吉田(東大) 、住	• 2015-16年、NASAで正式に予算化される見通し。	

全般的なWFIRST WG申請中。（WACOからの発展改組）	
興味のある方は是非参加ください。	

WACOのコロナグラフ装置開発	
日本での具体的開発目標	
-日本独自技術によるマスク開発	
（１）フォトニック結晶技術によるPIAA用焦点面マスク	
（２）スーパーインクジェット技術によるOMC(BLC)用焦点面マスク	
（３）バイナリ瞳マスクコロナグラフ	
コロナグラフへの部分寄与として	
	
10	
  μm

-偏光機能の検討	
コロナグラフのための偏光機能の検討	
（装置偏光補正および偏光観測による	
コントラスト向上の検討など）	
偏光は日本が得意		-赤外PIAA 開発	
赤外線PIAAコロナグラフの光学設計	
コロナグラフバックアッププランへの寄与	

戦略的開発経費で昨年製作、村上（北大）	

Heritage of the SPICA
Coronagraph
Instrument (SCI)	
Design	Experiment	

2.7m	

1. High  stability  vacuum  testbed  in  JAXA/ISAS.
2. Pupil  masks  for  obscured  pupil  were  designed,  and  fabricaEon  of  free-­‐standing  masks  is  ready.
3. Non-­‐coronagraphic  parts,  e.g.,  mirrors,  ﬁlters,  mechanical  changers.
16
4. Experiences  are  also  important  heritage?

	日本の貢献の可能性
Hardware:

l
l
l
l

コロナグラフ(WACO)
Flight calibration system
Integral field spectrograph
Fine guidance sensor

Non-Hardware:
l
l
l
l

26GHz Ka-band downlink station (臼田、内之浦)
すばる HSC/PFS 観測による
WFIRSTのphoto-zのキャリブレーション
アーカイブ,データ解析(地上での経験)
地上近赤外観測によるWFIRST観測領域の最適化（マイクロレンズ）

Summaryl WFIRSTは、大統計量で宇宙の加速膨張、系外惑星を解明する。	l GO program à多くの分野の方の参加が可能。	
l 日本の光赤外コミュニティーは参加に強い興味。	
(WFIRST連絡会)	
l 日本のコロナグラフ関係者は参加に向けてR&Dを開始(WACO WG)	l すばるHSC/PFSサーベイが強く望まれている。	
l Subaru/PFSやTMT、SPICAの良いターゲットとなる 	

l WFIRST WG設立を申請中	
興味のある方は是非参加ください。