Euclid/WFIRST
光赤外広視野サーベイ衛星への参加
Wide-Field InfraRed Survey TelescopeAstrophysics Focused Telescope Assets•Dark Energy
WFIRST-AFTA•Exoplanet Microlensing
Final Reportby the•Near Infrared Sky Survey
Science Definition Team (SDT) and WFIRST Project

住 貴宏 (Osaka Univ)
宮崎 聡 (NAOJ)
高田 昌広 (IPMU)
2013/8/7 [光赤天連シンポジウム] 国立天文台

April 30, 2013

Euclid/WFIRST explore the Late 20th
century’s biggest discoveries!"#$%&&#'#(%)*+,$#-.%+/*0+$01$)"#$2+*3

Accelerating expansion of universe

L0+'#H$#)$%'$6FDD$$456$789%$"•Cosmic acceleration history via•Weak lensing (WL)
•Supernovae (SN)•Baryon Acoustic Oscillation (BAO)•Red shift space distortion (RSD)
91$$! =$>?#"=$&)#$$•Structure growth via WL, RSD!$! $$&'0/#$)0$$@!""#"$%&"'()"*+(,-."$$•Test Einstein’s gravity and Modified Gravity!$8##A$"*,"$.(#&*/*0+$A%)%$)0$B+0C$*1$/01'2*%31,+1'%+'4##1$1,4-%*5''4-'
67787779'#)*:%&1*#1'$131$'

!"-$$

$

<$
<

Exoplanets/$!<$=$DEFF$!$%..%(#+)$%&&#'#(%)*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$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$9>N2$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$•Complete statistical census of Planetarysystems which Kepler startedà Complementary to direct observation

Euclid/WFIRST difference
EuclidWFIRST(Dark Energy mission, 2020~) (General observatory, 2023~)

Primary: 2.4m
Primary: 1.2m
Life time: 5yr (+1 with Coronagraph)
Life time: 6.25yr
Optical (550-900)Im +IR(YJH)Im,Spec IR(0.7-2.0) Im(4band), Spec(grism+IFU)
FOV:
0.28deg2 (18H4RG)
FOV:
0.54deg2
Wide 15kdeg2 ,MAB=24.5,YJHAB=24 High latitude 2000deg2 ,YJHAB=26.7
Deep 40deg2 ,MAB=26.5,YJHAB=26 Galactic Plane 1240deg2 ,YJHAB=26
Supernova wide 27.4deg2,Y=27.1,J=27.5
Supernova mid 9.0deg2 , J=27.6,H=28.1
Supernova deep 5.0deg2,J=29.3,H=29.4
Galactic Bulge 2.8deg2•Dark Energy•Dark Energy•Weak Lensing•Weak Lensing•Baryon Acoustic Oscillation•Baryon Acoustic Oscillation•Super Novae•（Exoplanet Microlensing)(extended)•Exoplanet Microlensing•General Observer Program (~28%)	

Selected 	!"#$%&'(')*))+',-.-/'!"#$%&'()*+),-%".'!"#$$%&%%$'$()*+#$$%&%%$'$()*+#,-./01$'$()*+#$$,-./01$'$()*+#,-./01$'$()*+2$$,-./01$'$()*+2,-./01$034567$89$(:#$54/4;067$<0//$=4>6$?=6$7436$@678/-?08A$47$%&%%$034567$4?$(:*+*"$4A1$B6$4?$/647?$C$345A0?-167$166D6@+$!"#$%&'("$)*+(%,--)./)0%(,1234")))))))))))))
56)7!"#

!"#$%&'()*+),-%".'!"#$%&'()'*+,&%#-,&'*,+./+012#,3'
9,#/23-+"#-,&':1$1;<'*/=,+'3*,#-+"0'4544677'89(':1$1;%,3''''''''''''''''6''''''''''''''''''''''''!"#$%&''!'>,..'"#?@'A6B'(*#B'"#$%&#'()*+)#,-(.#/0//'!'9,&3A%.-3'CD!DE'/(%8("$,9() 2:;;(%("8() <(=>(8$(2) !) '(,#&%(2?)>34(%)#>(8$%&'7))%(83+(%(2)$3)@A)B)!"#$%&'("$)*+(%,--)./)0%(,1234")))))))))))))

56)7!"#!"#$%&''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''7FGH'''''''''''''''''''''''''''''''''''''''''''I"2,''?3-''EC?E'

!"#$%&'!"#$%&'())*+,%&)'-"./)0-'1)2-%3$)'%4'567'0)2.-''()*+),-%".'

8)1).)4#)'-"./)0''19.'-%:%4;'-*2#)#.21<='1%42$'-"./)0'49<'0)<'-)<6'>?0'-"./)0'-<.2<);0'%4#$"&)-='''

Wide 15kdeg2 ,MAB=24.5,YJHAB=24
Deep 40deg2 ,MAB=26.5,YJHAB=26! @4-<."A)4<'#2$%3.2<%94'B%<C'-*)#%1%#'<2.;)<-'! ,%&)'24&'())*'1%)$&-'!"#$%&'("$)*+(%,--)./)0%(,1234")))))))))))))

56)7!"#!"#$%&''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''''@DEF'''''''''''''''''''''''''''''''''''''''''''G"4)''H-<''IJHI'

$%&'&()*#+,-#.#,/0123#34'4#!"#$%&'()*+),-%".'!

!#56'2041#34'4#478#9/11#647'#&9#'%8#,/0123#:2;;2&<#!#=8>/278:8<'#?@?"ABC.)D####!#!#&6'2041#E4<3#.#,/0123#FG#H#I#;/992028<'###!#J883#'&#K8'#&6'2041#34'4#97&:#K7&/<3(E4;83#'818;0&68;#!"#!"#$%&'("$)*+(%,--)./)0%(,1234")))))))))))))

56)7!"#,/0123##################################################################################L$MN###########################################H/<8##C;'##O?CO#HSC-for-Euclid Survey依頼の経緯
 Euclidサーベイは地上可視光多色サーベイ(ugriz)のパートナーが必要 南天: Dark Energy Survey (米国、5000平方度)。いずれ

LSST 北天: (1) WHT 4mをupgrade (タイムスケールが合わなくな

りつつある）(2) CFHTのupgrade (フランスを中心に科研費
申請中) (3) HSC (4) Pan-Starrs2 (1.8m 2)

 2012年6月にEuclid Consortium LeaderのYannick

Mellier氏が来日し、林台長にHSCで6000平方度(i~25,
200晩相当) をサーベイして欲しいと依頼。
 その後、SAC主導で議論してきた。

これまでの議論•活動
 2012年秋期天文学会

光天連総会で紹介

 2012年9月＠天文台

HSCサイエンス検討会で議論 2013年1月＠天文台

HSC-Euclidサイエンス検討会

 2013年2月@天文台

すばるUMで議論

 2013年4月

HSC-Euclidサイエンスコアチーム(宮崎、高田ら)がサイエンス白書を提出

 この間すばる小委員会で継続的に議論
HSC-Euclidサイエンス白書	
http://member.ipmu.jp/masahiro.takada/hsc-euclid_whitepaper.pdf	

すばる小委員会から林台長への回答（6月） 吉田SAC委員長から林台長へ送付。「Euclid計画は次世代の画期的な宇宙論研究計画であり、日本の宇宙論・天文学
コミュニティは強い関心を持っている。すばる望遠鏡Hyper
Suprime-Camがこの計画に大きな貢献をするであろうことは疑う余地がない。しかし、すばる望遠鏡は日本の天文学コミュニティの貴重な研究施設であり、その観測時間を特定のプロジェクトに大規模に投入することには慎重にならざるをえない。Euclid側からオファーがあってからコミュニティで議論を重ねてきたが、時間が不足しており、現時点では何らかの明確な意思表示をするまでに議論が成熟していない。今後、コミュニティ内で時間をかけてより深く検討したいので、Euclid側にはその旨伝えていただき
たい。」

現在
 6月 林台長からYannick Mellier氏へ回答のレターを送付。
 6月19日 Yannick Mellier氏からの返信。
Dear Masa
Thank you very much for your letter and reminder. On our side the Euclid Consortium Board
considers working with Subara HSC as the best approach. I also sent an email very recentl proosing to
invite 40 Japanase scientists in Euclid instead of the 20-30 we discussed last year. So, if HSC agrees
to spend 200 nights for Euclid to cover the northen sly, then we can start writing an MoU. I would
be most happy to do that and I have the mandate from the Euclid Consortium Board. I am ready tovisit you in Japan anytime• HSC-for-Euclidサーベイの見返りとして、日本人４0人の参加を提案される。	

• 引き続き継続議論中。

2.4m Astrophysics Focused
Telescope Assets (AFTA) for WFIRST NASA has been studying potential uses of the 2.4m telescope assetsthat were made available to the Agency by the National
Reconnaissance Office in mid-2012
 SDT report released on May 30, 2013 http://wfirst.gsfc.nasa.gov/science/ The focused astrophysics study showed that for approximately thesame costs, the telescope assets would enable a WFIRST mission withsignificantly improved science capabilities relative to the design
described in the Astrophysics Decadal Survey
 Use of the telescope assets would also enable the addition of an
exoplanet imaging instrument (coronagraph) to WFIRST that would
enable imaging and characterization of planets around nearby stars
up to a decade earlier than contemplated in the Decadal Survey(Develop precursor coronagraph for TPF)
 NASA Approval for Further AFTA Study (4 Jun 2013)
http://science.nasa.gov/media/medialibrary/2013/06/04/
AAS_TownHall_2013-06_V7A_for_posting.pdf

 $10M over FY13 for WFIRST

using guiding functions contained in the
6x3 science SCAs

Grism R = 550-800(2 pixel)

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
75 mas/pix;
SlicerPrism
Relay
actuators and managing thermal set-points. These
f/21
Assembly
Spectrograph
1 2kx2k, 18µm pixel size SCA;
higher-level commands are sent through cabling to
R = ~100 (2 pixel)
4 Mpix; <115K;
0.6-2.0µm bandpass;
Integral Field Unit Spectrograph Channel
local boxes on the telescope where they are convertFOV 3.00x3.15 arcsec
ed to low-level signals and sent to the devices themOptional Coronagraph Instrument
selves. Each subsystem has a similar functional content with heaters, thermal sensors, and actuators. The
Relay w/
Low order
Pupil Mask
WFIRST-AFTA
Fixed DM
exception to this overall architecture is control of teleDM/FSM
WFS& Filters
Figure 3-4: The telescope components without the outer
scope survival heaters. They are controlled directly bybarrel assembly.
1kx1k, Si low noise FPA; 150K;
the spacecraft avionics to ensure operation in the
Imaging
IWA 0.25/λ arcsec, λ (0.4-1.0µm)
Detector
OWA
2.5
arcsecevent of an intermediate electronic failure.
Flipand thermal distortions while providing superior stiff2kx2k, Si low noise FPA, 150K;
Mirror
0.4-1.0µm bandpass;
The cost, schedule, and technical risk associatedness and stability. The structure has active thermal
IFS
IFS Detector
R~70, 17 masec samplingwith the telescope development have already been
control (heaters) and is isolated from the solar array
optical block diagram.
significantly mitigated; the telescope hardware andby the OBA to minimize heat transfer into the teleWFIRST-AFTA
supporting GSE largely exists and spare parts are
aturely ending thescope and instrument bay.
ray/sunshield thatavailable for most of the components. New stray light
The two telescope mirrors feed both a wide field
ld of regard (seebaffles, new thermal blankets, and new electronics
instrument (see Figure 3-6), with a wide field of view
derived from commercial products are low risk modifichannel and an integral field unit, and an optionalt the WFIRST-2.4
Telescope&cations.
nearly on-axis (in field) coronagraph instrument. Thes study, it was dewide field channel includes a tertiary so that the sysdule level, i.e. an
3.3 Wide-Field Instrument
module containing
Solar&Array&/&
tem acts as a three mirror anastigmat (TMA); the othThe wide-field instrument is divided into two
Sunshield&
ularity will also be
er channels correct the residual aberrations in the firstof the observatomodules, a cold instrument module (referred to as thetwo mirrors. The overall three-mirror system is able to Figure
3-5: The telescope entrance pupil
d side, an instruachieve
excellent
opticalperformanceoverarelativech to the existing
ly wide FOV. The most important performance re- and heaters. The telescope control electronics areaces and provide
s. The instrument
3-5: The telescope entrance pupil
quirement for the telescope to enable the WFIRST- locatedFigure
in anelectronics box in the spacecraft and
Wide&Field&, with design her2.4
scienceisstability.
Based
on
the
low
expansion
heaters.control
The telescope
controlsuch
electronics
areInstrument&
performandhigher
functionsas commanding
strument modules
Coronagraph&materials,
thethermaldesign,andtheactiveheaterlocatedinanelectronics
box
in
the
spacecraft
andInstrument&Carrier&Instrument&route power andandmanaging
thermalperform
highercontrol functions
such as set-points.
commanding These
control,
the wavefront stability delivered to the wide actuators(blue&truss)&
e instrument modactuatorscommands
and managingare
thermalThesesentset-points.
throughcabling tofield imager is modeled to be <0.15 nm rms over one higher-leveln between the twohigher-levelcommands
aresent
throughcabling24-hour GEO orbit thermal cycle.
local boxeson thetelescope
where
they
areto convertSpacecra3&
local
boxes
on
the
telescope
where
they
are
convertedge, and stability
Bus& The telescope electronics were not included withed to low-levelsignalssent
to devices
the devices
ed to low-levelsignals andand sent
to thethem- themapes and precisethe 2.4-m telescope. The current plan is to upgrade
selves.
Eachsubsystemhasasimilarfunctional
conFigure 3-3: WFIRST-2.4 Observatory configuration featurnd SN fields andselves. Each subsystem has a similar functional
conmostoftheelectronics
withthecurrent
commercial
tent
with
heaters,
thermalsensors,
andactuators.
The
ing the 2.4-m telescope, two modular instruments and a
between 54˚ andtent withheaters,
sensors,is control
and actuators.
The
exception
to thisthermal
overall architectureof teleproducts. TheFigure
electronics
is a traditional
modular spacecraft. bus
ervation of micro3-4: The architecture
telescope components
without the outerFigure
3-6:
Ray
trace
throughthetelescope
to
the
wide
scopetosurvival
heaters. They
are controlledisdirectly
by of teleexception
thisoverallarchitecture
controlhierarchicaldesignfrom spacecraft
avionics
barrelassembly.
Figure 3-4: The
telescopecomponents
without
the throughouterfieldthechannelintermediate
focus.
spacecraft
avionics
toensureoperationinthetelescope control to local boxes to peripheral devices scope survival heaters. They are controlled directly by
Wide Field Science Channel

2.4m WFIRST-AFTA• Existing Hardware: high quality mirror and optical system• Easily used in Three Mirror Anastigmat- Wide field of view- 3rd mirror in Wide-Field Imager primary instrument

barrel assembly.

and thermal distortions while providing superior stiff58
ness and stability. The structure has active thermalthe
control (heaters) and is isolated from the solar array

event of an intermediate electronic failure.

spacecraft
to technicalensureriskoperation
The cost,avionics
schedule, andassociated in thewith the telescope development have already been

SDT #2: WFIRST-2.4

2013

2.4

0.11

9.45 as2

with GRS grism in a wheel
1 H2RG-18 IFU for SN spectra
Optional coronagraph for
exoplanet imaging

2.4m WFIRST-AFTA FOV

Table 1-1: Comparison to past WFIRST Design Reference Missions.

Figure 1-1: Field of view comparison, to scale, of the WFIRST-2.4 wide field instrument with wide field instruments on
the Hubble and James Webb Space Telescopes. Each square is a 4k x 4k HgCdTe sensor array. The field of view extent
is about 0.79 x 0.43 degrees. The pixels are mapped to 0.11 arcseconds on the sky.

AFTA
with
Coronagraph(option)over 10 times closer to the star (130 mas IWA for 3λ/D) and would be sensitive to detecting disks 1000
times fainter. This means that WFIRST-2.4 would be
able to obtain comparable images of disks down to thehabitable zones of many nearby stars, including ones

•
•
•
•
•
•

With additional ~$100M cost
Imaging Ice & Gas giant exoplanet
Imaging debris disks
400-1000nm band pass
10-9 contrast
100 milliarcsec inner working angle
at 400nm
Figure 2-25: HST ACS image of the debris disk aroundthe young (~100 Myr), nearby (28 pc) sun-like (G2 V0 star
HD 107146. This disk has 1000 - 10,000 times as muchdust as our own solar system, and it is distributed out toa radius of approximately 180 AU (6.4"), while light within
50 AU (1.8") is obscured by the ACS coronograph occulting mask. This system is thought to have an inner holein its disk at 31 AU106, and the WFIRST-2.4 coronagraphcould search for signs of planets within there.

Microlensing Exoplanet Survey with WFIRST•300Mstars•15min cadence•72 day continuous observation x6

Twice Earth
Earth
Half EarthNo Planet

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
Days

10

2
20

9.2

9.4

9.6
Days

9.8

Microlensing Exoplanet
Survey with WFIRST•3000 bound planet
200 (< 1 M⊕)	

•2000 free-floating planet
100 (< 1 M⊕)

Complete the census
of planetary systems
in the Galaxy

NRO 2.4 m design: factor 2 faster survey	
Performance of NRO-1 2.4-m compared to SDT WFIRST (DRM1) . The images
compare an “equal-duration, equal-area” survey of a Galactic Bulge field(assuming a 2.4-m field of 0.25 sq deg). The total area covered in 15-minutecycles is 2.5-deg, with 7 DRM1 fields or 10 2.4-m fields.

16”

Matthew Penny (OSU) 	

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'

Possible contribution to
Euclid/WFIRST from Japan

Hardware (for WFIRST):l Flight calibration systeml Integral field spectrographl Fine guidance sensorl Coronagraph4kx4k H4RG	l H4RG development by ground base IR telescopeà long-term characterization

Non-Hardware (Euclid/WFIRST)
l
l
l

Data from a wide-area sky survey by Subaru HSC, designed tocomplement the Euclid observing program
Data processing and archiving
Optimize the WFIRST fields by ground base IR telescope

Timeline of DE experiments	
2020	

2019	

2018	

2017	

2016	

2015	

2014	

2013	

BAO	

2012	

2011	
WL	

HSC	
DES	

LSST?	
SDSS/BOSS	

Euclid	PFS	
HSCサーベイ(+PFS)は世界中で計画されているDEサーベイに先駆けて実現。ダークエネ
ルギー研究で世界をリードするチャンス	WFIRST?	

コミュニティ内でのプロジェクトの位置づけ大型計画との関連・相補性• すばるHSC SSPではDEサーベイで世界に先行する。そこで育った人材を供給する事で存在感を維持する。
• WFIRST/Euclidのこれまでにないdeepな広視野サーベイデータには、高赤方偏移銀河やQSO、その他予期せぬ天体の発見が期待されている。これらは、Subaru/PFSやTMTの良いターゲットとなる。

協力・競争関係にある類似プロジェクト• WISH: 初代銀河探査、暗黒エネルギー、銀河進化• D=1.5m, FOV=0.24deg2, 0.9-5µm, survey area 100deg2,~28 AB mag• 大きな違いは、WFIRSTの感度が<2.0µmまで。
• 大口径でカバーできるかを検討。

• 中型JASMINE,

近赤外位置天文• 全面的な国際協力(WFIRST, Post-Gaia）、国内計画とのマージ（候補：WISH計画）を検討中.
• WFIRSTは、中型JASMINEの目標である近赤外線によるバルジの広域で高精度な位置天文観測が可能。WFIRSTでの目標達成可能性の検討を開始しており、可能な場合は、JASMINEチームも協力を惜しまない考えである。（郷田氏）• TPF: 地球型系外惑星の直接撮像• JTPF working groupが国際協力を模索中• WFIRST/coronagraphはTPFへのステップである。

summaryl Euclid：	l Euclidチームからは、HSC-for-Euclidサーベイを強く望まれている。 	l 参加は継続審議中。	

l WFIRST：	l は、2.4m AFTAになる可能性が高い。	
l コロナグラフの搭載が検討されている。	

l 日本の参加が望まれている。