(Wide Field Infra Red Survey Telescope)
Recommended by Decadal survey astro2010
NASA’s flagship mission following HST, JWST
Launch in 2025
•Dark Energy•Exoplanet Microlensing•Exoplanet Coronagraph•Guest Observing Prog.
Takahiro Sumi (Osaka U.), PI: JAXA WFIRST WG
2018/6/6 [Galaxy evolution Workshop] @Ehime Universiyt

WFIRST =++David Bennett, PI

JDEM
Joint Dark Energy Mission

MPF
Microlensing Planet Finder

NIRSS
Near InfraRed Sky Survey

uiding in imaging mode performed
ng guiding functions contained in the
6x3 science SCAs

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

Wide Field Science Channel

Ea. square is a 4kx4k,
10µm pixel size SCA;
302 Mpix; 120K;
0.6-2.0µm bandpass
0.28 deg2 active area

2.4m
WFIRST
Diameter: 2.4m given from NRO (National Reconnaissance Office)

SlicerAssembly

Relay

Prism
Spectrograph
R = ~100 (2 pixel)

ntegral Field Unit Spectrograph Channel

75 mas/pix;
f/21
1 2kx2k, 18µm pixel size SCA;
4 Mpix; <115K;
0.6-2.0µm bandpass;
FOV 3.00x3.15 arcsec

WFIRST-AFTA
Wavelength: λ=0.6-2μm
WFI: (FOV：0.281deg.2)
Coronagraph
Orbit: L2
WFIRST-AFTA
Mission life time: 5 years: Serviceable
ely ending the
Optional Coronagraph Instrument

Relay w/
DM/FSM

Fixed DM

Flip
MirrorImaging
Detector
IFS

Low order
WFS

Pupil Mask
& Filters

1kx1k, Si low noise FPA; 150K;
IWA 0.25/λ arcsec, λ (0.4-1.0µm)
OWA 2.5 arcsec
2kx2k, Si low noise FPA, 150K;
IFS Detector 0.4-1.0µm bandpass;
R~70, 17 masec sampling

cal block diagram.

sunshield thatregard (seeWFIRST-2.4
dy, it was delevel, i.e. anle containing
ty will also be
he observatode, an instruo the existingand provide
he instrument
h design herment modules
e power andtrument modween the twoand stability
and preciseN fields andween 54˚ andion of micro-

Telescope&

Solar&Array&/&
Sunshield&

Figure 3-5: The telescope entrance pupil

and heaters. The telescope control electronics are
3-5: The telescope entrance pupil
locatedFigure
in anelectronics box in the spacecraft andandheaters.
The telescope
controlsuch
electronics
areperform higher control
functionsas commanding
located in an electronics box in the spacecraft and
Wide&Field&
actuators
andmanaging
thermalInstrument&
perform
highercontrol functions
such as set-points.
commanding These
Coronagraph&
actuatorscommands
and managingare
thermal
These
Instrument&Carrier&higher-level
sentset-points.
throughcabling toInstrument&(blue&truss)&
higher-level commands are sent through cabling tolocal boxeson the telescope where they are convertlocal boxes on the telescope where they are converted to low-levelsignalssent
to devices
the devices
ed to low-levelsignals andand sent
to thethem- themSpacecra3&
selves.
Eachsubsystemhasasimilarfunctional
conselves. Each subsystem has a similar functional
conBus&tent with heaters, thermal sensors, and actuators. The
withheaters,
sensors,is control
and actuators.
The
exception
to thisthermal
overall architectureof teleFigure 3-3: WFIRST-2.4 Observatory configuration featur-Figure 3-4: The telescope components without the tent
outer
ing the 2.4-m telescope, two modular instruments and abarrel assembly.
scopetosurvival
heaters. They
are controlledisdirectly
by of teleexception
this overallarchitecture
control
modular spacecraft. busFigure 3-4: The telescope components without the outerthe spacecraft avionics to ensure operation in thescope survival
heaters. They are controlled directly bybarrel assembly.
event of an intermediate electronic failure.
and thermal distortions while providing superior stiffto technicalensureriskoperation
The cost,avionics
schedule, andassociated in theness and stability. The structure has active thermalthe spacecraft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_q ~ 100 arcsec/micron
4288 Mpixels total

Flux Fν (µ Jy)

Hubble x 200 Discovery of High-z Galaxies
DRM1

WFIRST-2.4

Wavelength (µm)

z = 10.8 Galaxy

Precise measurements ofGalaxy clustering
Structure evolution
up to high z

5Euclid

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

WFIRST: 15x more sensitive
10x sharper

Dark matter distribution by Weak lensing

Measure the shape
Of 500M galaxies by
WFIRST

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

WFIRST Observation strategy
Ø Dark Energy/Modified Gravity(〜2.5yr)
u High Latitude Survey (HLS)（galaxy distribution）

2000deg2、image(YJH)＋spectra(R~800) Y<26.7, J<26.9, H<26.7, F184W<26.2
・Weak Lensing（WL）
Dark matter,
・Red shift space distortion (RSD)!"#$%&&#'#(%)*+,$#-.%+/*0+$01$)"#$2
Structure growth・Baryon Acoustic Oscillation (BAO)
L0+'#H$#)$%'$6FDD$$456$789%$

uIaSNe survey"
Cosmic acceleration history

5, 9, 27deg2、imaging＋IFC (R〜100)/01'2*%31,+1'%+'4##1$1,4-%*5''4-'
67787779'#)*:%&1*#1'$131$'

Ø Exoplanets：
u Microlensing exoplanet search (〜1yr)
Complete statistical census of Planetary systems
which Kepler started

!"-$$

$

91$$!<$=$>?#"=$&)#$$!$!<$$&'0/#$)0$$@!""#"$%&"'()"*+(,-."$$!$8##A$"*,"$.(#&*/*0+$A%)%$)0$B+0C$*1$/$!<$=$DEFF$!$%..%(#+)$%&&#'#(%)*0+$.(0AG&#A$;H$%$I/$!<$*/$+0)$&0+/)%+)$!$0,"0&"1234560*5+"2578"-4-793:"(/$)"#$/0G(&#$01$)"#$%..%(#+)$%&&#'#(%)*0+$*/$+0)$$IA%(B$$$!"#$%&'("$)*+(%,--)./)0%(,1234"))))))))))))
MG&'*A$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$9>N2$$$$$$$$$$$$$$$$$$$$$$$$$u Direct observation by coronagraph(〜0.3yr)
optical、contrast 10-9, IWA 0.2”

Ø Guest Observer（25%,1.5yr）

8

2018/6/6

Figure 3-28: The footprint of the WFIRST-2.4 observations. The red region shows the HLS, the blue shows the supernova survey, and the magenta spot shows the microlensing survey. The HLS footprint area is 2054 deg2.

WFIRST Observational fields
Available for GO

Figure 3-29: The amount of time during the 5-year primary mission during which each field would be accessible by the
GO program, with no re-scheduling of other observations, as determined by a Monte Carlo analysis. Fields within 36°of the ecliptic poles are available for the great majority of this time since they always satisfy the Sun angle constraint,with only occasional cutouts due to the Earth. Fields near the Ecliptic are available only part of the year. The Galactic
bulge region near RA=270°, Dec=30° has the lowest availability because most of the time when it is accessible it isused by the microlensing program. Nevertheless it still satisfies the requirement of being available in multiple years.

critical HLS observations taking into account the distribution of GO programs will endow WFIRST-2.4 witheven more flexibility.

Section 3: WFIRST-2.4 DRM

The plan presented here is only one possible
example of what WFIRST-2.4 might do, but it
demonstrates that the strategic programs are all

82

Galactic Plane
Ecliptic Plane
Celestial Equator

Microlensing
FieldsHigh-Latitude
Survey9 Area
SN Fieldsdark energy
equation-of-stateparameter w at
redshift z = 0.47 (theredshift at which it
is best determined
by WFIRST- 2.4)
andits derivative withrespect to expansion
factor dw/da.

Figure 2-7: Δχ2 = 1 error ellipses on the value of the darkenergy equation-of-state parameter w at redshift z = 0.47
(the redshift at which it is best determined by WFIRST2.4) and its derivative with respect to expansion factor
dw/da. The green ellipse, centered here on the cosmological constant model (w = -1, dw/da = 0), represents current state-of-the-art constraints from a combination of
CMB, SN, BAO, and H0 data.20 For this figure, we haveimagined that the true cosmology is w(z=0.47) = -1.022
and dw/da = -0.18, well within current observational constraints. The black ellipse shows the error forecast forthe baseline WFIRST-2.4 SN, GRS, and WL surveys, combined with CMB data from Planck, a local supernova calibrator sample, and BOSS BAO and RSD measurements
at z < 0.7. The red ellipse shows the “extended” case inwhich the precision of the WFIRST-2.4 measurements(but not the Planck, local SN, or BOSS measurements) is
increased by a factor of two, as a result of a longer observing program in an extended mission, better control of

Figure 2-8: Top: Figvarious assumption
baseline case of Fo
black contour of F
shows the forecast
from Weinberg et alGalaxy Luminosity Function
WFIRST’s High-Latitude Survey will yield up to 2 orders ofmagnitude more high redshift galaxies than currently known

11

WFIRST: A Unique Probe of
Cosmic Structure Formation History
Using Observations from the High-Latitude Survey and GO Programs

Detection of Large
Sample of z > 7
Galaxies
Large-scale Distribution of
Lyman-break Galaxies
Survey of Emission-line Galaxies
Large-scale Distribution of Galaxy Clusters
Lensing Mass Function of Clusters
Dark Matter Halos of Galaxies
Present

1

4

6
billionyears

1.5
billionyears

Redshift

5

6

7
750
millionyears 12

8

>10
<500
millionyears

WFIRST – A Unique Probe of Stellar
Populations and Nearby Galaxies
Resolve and characterize stellar pops out tolarge distances (47 Tuc and SMC - Kalirai et al. 2012)
Ultra-deep imaging of galaxy halos(M63 - Martinez-Delgado et al. 2010)13

Microlensing exoplanet search

Earth mass planet by WFIRST
2 Earth mass
Earth mass
0.5 Earth mass
No 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
日

10

• 300M stars in 2.8 deg.2in the GB• 15min cadence in ２４hrs, 72 days
• ６ seasons（1.2yr total）

2
20

9.2

9.4

9.6

9.8

日

４−５hr signal by Earh mass planet

Expect 3000 exoplantes(~200 less than Earth mass）

Microlensing exoplanet search
by WFIRST
３000 exoplantes(〜200 with <ME）

All solar system planets
Except mercury

Semi-Major axis（AU）

Complete statisticalcensus of Planetary
Systems with Kepler

AFTA with Coronagraph (option)
AFTA Coronagraph Instrument

ExoPlanet Exploration Program

Telescope

Wide field
instrument

Coronagraph
Instrument

Exoplanet
Direct imaging• 400-1000nm band pass• 10-9 contrast• 100 milliarcsec inner working
angle at 400nm• R=70 spectra and polarization
at 400-1000 nm
WFIRST final report May 23, 2013
http://wfirst.gsfc.nasa.gov/

Exoplanet
Spectroscopy• Image and spectra of Nearby
gas giants, ice giants.
• Proto-planetary disk
• Technology demonstration for
LUVOIR and HaBEXAFTA Coronagraph Instrument will:• Characterize the spectra of over a dozen
radial velocity planets.
• Discover and characterize up to a dozen
more ice and gas giants.
• Provide crucial information on the physics ofplanetary atmospheres and clues to planet
formation.
• Respond to decadal survey to maturecoronagraph technologies, leading to firstimages of a nearby Earth.

8

WFIRST Yields Summary
Attributes
Imaging survey
Slitless spectroscopy

WFIRST Yields
J ~ 27 AB over 2000 sq deg
J ~ 29 AB over 3 sq deg deep fields
R~461λ over 2000 sq deg

Number of SN Ia SNe

2700 to z~1.7

Number galaxies with spectra

2x107

Number galaxies with shapes

4x108

Number of galaxies detected

few x 109

Number of massive clusters

4x104

Number of microlens exoplanets

3000

Number of imaged exoplanets

10s

18

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"<%'
6. White dwarfs.
Q%&%4<97%'+R$82'LM'%2820';*9I#%'%)'"&2'FGGS0';9&)9#'%)'"&2'FGGH/2'Q@%'4">%'@"4'?%%#')*=%'E9*')@%'4$>$&"*'#=>?%*'9E'<&=4)%*C4<"&%'4)*9#8'&%#4'4A4)%>4'+%2820'(>$)@'%)'"&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 Quasars LG'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#' $#'4)*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%*'

WFIRST activity & schedule
•
•
•
•
•

2010/12, first WFIRST Science Definition Team(SDT), Japan rep. Sumi
2013/7, WFIRST-AFTA SDT, JAXA rep. Toru Yamada（ISAS）
2013/8, launch 「WFIRST informal WG」
2014/2, WFIRST coronagraph WACO WG at JAXA
2015/3, SDT final report• 2016/1, launch JAXA WFIRST WG(PI:Sumi)• 2016/2, NASA started phase A.
•••

2016/6, Toru Yamada became JAXA rep for NASA FSWG
2016/7 Subaru-WFIRST synergy obs. White paper
2017/9 proposal submitted to ISAS/JAXA.

• 2017/8〜１0, WIETR independent review• 2017/11, descope plan submitted to HQ• 2017/2/19, NASA WFIRSTSRR(System Requirements Review),
MDR (Mission Definition Review)

SRR explain the flow fromobjective to requirement.
MDR is reverse.

• 2018/3, President budget request to cancel WFIRST• 2018/5, NASA WFIRST passed into phase B!
• 2018/5, $150M for WFIRST in house budgetJapanese Contribution “Package” for WFIRST■ JAXA WFIRST WG (PI：Sumi）

1. Subaru-WFIRST Synergy Survey(〜100nights from 2025)
1. photo-z calibration (PFS etc.)
2. Narrow band filters (HSC etc.)

2016/11：Director of Subaru telescope and Subaru SAC、
agreed to the Commitment

２．Contribution to Coronagraph Instrument
・Polarimetry capability
・Development of Polarimetry Compensation Unit

３．Ka-band Data Downlink Station in Japan
４．Ground base microlensing data sharing（MOA）
pre/concurrent Ground microlensing obs.
with new 1.8m (PRIME)

Discussins on Subaru Synergistic Observations
l 2016/4, Workshop on synergy with Subaru and space missions
l 2016/7, Subaru-WFIRST synergy obs. White paperl 2016/9, Support in GOPIRA symposium opt/IR communityl 2016/11, Subaru Telescope and Subaru Advisory Committee
concluded the commitmentl 2016/11, Letter of Intent sent to Director of ISAS from Directorof Subaru telescope. (cc: NASA HQ)
l 2017/1 Reported in Subaru Users’ Meetingl 2017/10 1st domestic meeting for synergy workshop(20participants)
l 2017/11/15 Second domestic meeting: (34 participants)
l 2017/12/18-20 WFIRST/Subaru synergistic workshop@Mitaka(>90participants,including 16 from US)
l 2017/1/19 Subaru UM. Report and discussion.
NAOJ and JAXA prepare the Letter of Commitmentl 2018/12 2nd WFIRST/Subaru synergistic workshop

Table 3.

White paper
SubaruWFIRST
synergistic
observation
2016/5/15: callfor white paper
30 proposals by
82 people
7/16, released at
http://iral2.ess.sci.osakau.ac.jp/~sumi/Subaru-WFIRST-Synergy.pdf

Proposed Synergy Programs and required instruments on Subaru

Science Program
Cosmology/Extragalactic Astrophysics
Cosmology with large-scale structure probes
Quasars in the Reionization Era
Finding and Characterizing high-z Clusters
Searching for Bright Lensed high-z Galaxies
Protoclusters across Cosmic Time
Protoclusters in the Reionization Epoch
Precise photo-z for Weak Lensing
Low-Mass Galaxies at up to z ⇠ 1.5
Galaxy and IGM Co-Evolution
Superluminous SNe at Reionization Epoch
Mass Assembly History of Galaxies since z=4
Galactic Astrophysics / Local Volume
Milky Way Disk Flare behind the Bulge
Deep NIR Imaging of the Galactic Bulge
Hypervelocity Stars in the Galactic Bulge
Dark Matter on Dwarf Spheroidal Galaxies
Structure of the Galactic Outer Stellar Disk
Stellar Astrophysics
Low-Mass End of the Initial Mass Function
Bulge Stellar IMF & Low Mass Close Binary
Dust Condensation Region around AGB Stars
Properties of the Bulge Dwarfs by IR Spectra
Solar System
Surface Characterization of TNOs
Water Ices in the Inner Solar System
Exoplanets
Probing Dust Grains in Circumstellar Disks
Polarimetry of Planets/Protoplanetary Disks
Exoplanets Search by Astrometry
Extinction in WFIRST Microlensing Fields
Concurrent Microlensing Observations
Imaging of Microlensing Planetary Hosts
Characterization of Transiting Exoplanets
Exoplanets around Late-M Dwarfs

Authors
Takada+Matsuoka+
Oguri
Oguri
Toshikawa+Toshikawa+Tanaka+Yabe+
Ouchi+Moriya+Kodama+Matsunaga+
Nakada +Nishiyama
Hayashi+Toyouchi+TomidaIta
Ueta+
Fukui+

HSC

–
–
–
–
–
–

–
–
–

–

–
–
–

–
–
–

Terai
YoshidaMuto
Murakami+
Yamaguchi+
Suzuki+Suzuki+
Fukui+
NaritaKuzuhara+

PFS

–
–
–

–
–
–

–
–

IRD

SCE

ULT

–
–
–
–
–
–
–
–
–
–
–

–
–
–
–
–
–
–
–
–
–
–

–
–
–
–
–
–
–
–
–
–
–

–
–
–
–
–

–
–
–
–
–

–
–

–
–

–
–
–
–
–
–

–

–
–

–
–

–
–
–
–
–
–
–
–

–
–
–
–
–
–

Note. — SCE and ULT indicate the SCExAO and the ULTIMATE-Subaru, respectively.

–
–

–
–

–
–

–
–
–
–
–

–
–

–
–

Organized by JAXA WFIRST WG, Hawaii observatory, NASAWFIRST FSWG
Participants:>90, including 16 from US, WFIRST FSWG, SIT
Scope:
l Share the interests from Japan and US
l Share the requirements from Subaru & WFIRSTl Start considering the overall strategy
l Define the rough schedulel Define the organization
2018/12 2nd WFIRST/Subaru synergistic workshop

PRIME (PRime-focus Infrared
Mirolensing Experiment)Funded by JSPS
Sothern African
Astronomical  !
Observatory!

Diameter: 1.8m, (f/2.29)
FOV: 1.3 deg2, (6 x full moon)
Largest FOV in IR

標高1761m

World Largest class NIR camera by using four4kx4k H4RG arrays loaned from WFIRST teamCurrent status of telescope

More events & planets in NIR at G.C.
Optical

G.C.

disk

Galactic bulge is highly obscured.

NIR

l More stars & more
events at GC.
l Planet frequency at GC.
l Select WFIRST fields.
l Simultaneous observation
with WFIRST to measurelens mass.
l Mass Function at GC（planet-Black Hole）

Study the galactic structure &Optimize WFIRST microlensing survey fields
by mapping the event rate in NIR
Galactic disk

WFIRSTb（degree）

SurveyG.C.

Event rate map in opticall (degree)(Sumi & Penny 2016)

Event rate vary by a factor of 2 （peak is at l=1°）

Simultaneous Ground-Space
monitoring to measure lens mass
PRIME can do samewith WFIRST in IR

M = 0.23 ±0.07 Msun
DL = 3.1 ±0.4 kpc.
Yee et al.2005

Off-bulge season sciences
50% of timel Transit search for M-dwarfs
lSearch for counterparts of high-z GRB, GW.
lWFIRST calibrationlH-band spectrograph: RV for giant planets
around M-dwarf.

Welcome NEW idea!

Summaryl WFIRST will study Dark Energy/Modified Gravity,
exoplanets with massive statisticsl GO program àanyone in all field can joinàcomplimentary to SPICA, TMT
lJapanese contributions
1) Subaru synergitic survey2) Ground microlensing data and survey3) Coronagraph hard ware4) Ground station

ready
ready
on going
on going

Proposal submitted to JAXA （戦略的海外協同計画）
Welcome to join.