2019

PRIME

PRime-focus Infrared Microlensing Experiment
Daisuke Suzuki(ISAS/JAXA)
Takahiro Sumi (PI, Osaka U), D. Bennett, A. Kutyrev, R.K. Barry (NASA/GSFC), I. Bond(Massey U), N. Rattenbury (U Auckland), F. Abe, Y. Muraki (Nagoya U), A. Fukui, N.
Koshimoto, M. Tamura, N. Matsunaga, N. Narita (U Tokyo), T. Nagayama (Kagoshima U),
M. Kurita (Kyoto U), H. Shibai, T. Matsuo, S. Itoh, Y. Hirao, M. Nagakane, Y. Satoh, S.
Miyazaki, I. Kondo, H. Suematsu, T. Yamawaki, H. Shoji, R. Kirikawa, Y. Tanaka (OU), et al.
on behalf of the PRIME collaboration1

Sep 24, 2019

Status in 2019 Spring2

Status in 2019 Autumn

3

Status in 2019 Autumn

PRIME:First dedicated NIR microlensing planet survey
to study low-mass planets outside snowline
Ø Wide FOVØ NIR (mainly H-band for the survey)
Ø SAAO
4

Discovered Planets and microlensing Sensitivity
current•RV•Transit (Kepler)•Direct imaging•Microlensing
Mass measurements
Mass by BayesianSuzuki+16

WFIRST (space NIR)

5

Precursor obs.

Optimize WFIRST microlensing survey
fields by mapping the event rate in NIR
Galactic disk

G.C.

bdegreeWFIRST

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

Event rate varies by a factor of 2 peak is at l = 1）

6

Precursor obs.

Optimize WFIRST microlensing survey
fields by mapping the event rate in NIR
G.C.

WFIRSTbdegree

Galactic disk

PRIME Survey(TBD)

l (degree)(Sumi & Penny 2016)

Event rate varies by a factor of 2 peak is at l = 1）

7

Concurrent obs.

Spitzer-Grounddelay = 20 days8Udalski+15

Galactic bulge surveys in 2020s
PRIME survey field (TBD)
PRIME FOV

S-JASMINE

Ranc+18

9PRIME Objectives
Bulge Season (primarily Apr-Sep)ØThe first dedicated NIR microlensing survey• Study Earth-mass planets outside snowline• Planet frequency toward the Galactic Center• Optimize the WFIRST microlensing field (Precursor Obs.)• Concurrent observations with WFIRST

10PRIME Objectives
Bulge Season (primarily Apr-Sep)ØThe first dedicated NIR microlensing survey• Study Earth-mass planets outside snowline• Planet frequency toward the Galactic Center• Optimize the WFIRST microlensing field (Precursor Obs.)• Concurrent observations with WFIRST

Off Bulge Season (primarily Oct-Mar)ØNIR RV for habitable planets around M-dwarfs (SAND)
ØNIR transit for M-dwarfs
ØTransient GW, High-z GRB, SNe, etc (TBD)
11Off-bulge season/time sciences (50% of time)• NIR RV planet survey (12% for ABC time)• 12% for Osaka U time
• 12% for UMD/NASA/WFIRST time
• 14% for SAAO time12    !
ØØØØØ  
Funded by JSPS

Primary diameter: 1.8m (f/2.29)
FOV: 1.56 deg 2 (0.5”/pix)
Ave. Seeing: 1.4” (best: 0.7”)
Detector: 4 x H4RG
Filters: Z , Y , J, H , Narrow-bands
Ø 1.06µm
low OHØ 1.19µm
low OH, Lyα@z=9, [OII]@z=2.2, Hβ@z=1.5
Ø 1.62µm
Hα@z=1.5

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Schedule (as of 2019 Sep)
Ø2019
Ø2020
Ø2021

manufacture, construction
camera install, first lightmicrolensing survey starts

Ø2023
Ø2025

create event rate map in the bulge
WFIRST launch, concurrent obs. starts

Ø2030

continue to the end of the WFIRST
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Updates…
ØPrimary Mirror• Ready to be exported to Japan from RussiaØLenses   • AR coating for L1-L4 is done
• Transmittance in Z-band (AR coating for L2-4) is worse than
expected, but negligible for the microlensing survey• Will be shipped to Japan from NZ soon.

ØDome and Building• Construction will start in FY2019ØTest Camera
15Summary
PRIME: PRime-focus Infrared Microlensing Experiment• @SAAO, FOV = 1.56 deg2, D= 1.8m, seeing= 1.4”, NIR• ZAB, Lim= 21.7, YAB, Lim= 21.0 , JAB, Lim= 21.0 , HAB, Lim= 20.4 (5σ, 300s exp., TBD)
• NB filter:• 1.06µm (Y-band)
low OH• 1.19µm (J-band)
low OH, Lyα@z=9, [OII]@z=2.2, Hβ@z=1.5• 1.62µm (H-band)
Hα@z=1.5• Off-bulge time science…
• NIR RV planet survey (w/ SAND), NIR transit planet survey, transient (GW, GRB, SNe… ),Narrow Band survey, etc• First Light in 202016

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