PRIME PRime-focus Infrared Microlensing Experiment Daisuke Suzuki - - PowerPoint PPT Presentation

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, Y. Hirao, M. Nagakane, Y. Satoh, S. Miyazaki, I. Kondo, H. Suematsu, T. Yamawaki, H. Shoji, R. Kirikawa (Osaka U), et al.

• n behalf of the PRIME collaboration

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()

Jul 1, 2019

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Summary

ØThe first dedicated NIR microlensing survey ØFirst light in 2020 ØMirror: 1.8m @SAAO (1.4”), Hlimit=18.7mag, Ylimit=19.6mag (5σ, 100sec) ØPrime Focus NIR Camera ØUse four H4RG, f/2.29 à 1.25° x 1.25° = 1.56 deg2 (0.5”/pix) ØZ, Y, J, H-band, three narrow band filters (TBD) ØConduct microlensing survey when the bulge is visible ØNIR RV survey for planets around M-dwarfs

• Follow up transients (GW, GRB, SNe, …)

(TBD)

• NIR BB / NB surveys

(TBD)

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Schedule (as of 2019 Jul)

Ø2019 manufacture, construction Ø2020 camera install, first light Ø2021 microlensing survey starts Ø2023 create event rate map in the bulge Ø2025 WFIRST launch, concurrent obs. starts Ø2030 continue to the end of the WFIRST

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Time scale: tp~M1/2 ~1day(MJ) ~a few hours (ME) Sensitive to Cold planets

• utside of snowline (~3asnow)

Planetary Micr crolensing

Brightness Time

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Time scale: tp~M1/2 ~1day(MJ) ~a few hours (ME) Sensitive to Cold planets

• utside of snowline (~3asnow)

Planetary Micr crolensing

Brightness Time

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• RV
• Transit (Kepler)
• Direct imaging
• Microlensing

Mass measurements Mass by Bayesian

WFIRST current

Discovered Planets and micr crolensing Sensitivity

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Wh Why y NIR microlensi nsing ng pl plane net sur survey? y?

ØLess extinction

• More stars -> more microlensing events -> more planet detections
• More faint /weak signals -> smaller planets

à Study Earth-mass planets outside snowline à Planet frequency toward the Galactic Center

Suzuki+16 Jung+19

1 day

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Wh Why y NIR microlensi nsing ng pl plane net sur survey? y?

ØLess extinction

• More stars -> more microlensing events -> more planet detections
• More faint /weak signals -> smaller planets

à Study Earth-mass planets outside snowline à Planet frequency toward the Galactic Center

ØOptimize the WFIRST microlensing field (Precursor Obs.) ØConcurrent observations with WFIRST

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

(Sumi & Penny 2016)

Event rate map in optical

G.C. Galactic disk

l (degree) bdegree

Optimize WFIRST micr crolensing survey fiel elds s by y ma mapping g the e even ent rate e in NIR IR

WFIRST

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Precursor obs.

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

(Sumi & Penny 2016)

G.C.

PRIME Survey (TBD)

Galactic disk

l (degree) bdegree

Optimize WFIRST micr crolensing survey fiel elds s by y ma mapping g the e even ent rate e in NIR IR

WFIRST

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Precursor obs.

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

(Sumi & Penny 2016)

G.C.

PRIME Survey (TBD)

Galactic disk

l (degree) bdegree

Optimize WFIRST micr crolensing survey fiel elds s by y ma mapping g the e even ent rate e in NIR IR

WFIRST

• 21 fields (27 deg2) / hr
• 3 fields (3.9 deg2) / 15 min

+ 9 fields (11.6 deg2) / hr

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Precursor obs.

Spitzer-Ground delay = 20 days

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Concurrent obs.

GAIA (at L2) – Earth parallax measurement

Wyrzykowski+19

Ø

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Concurrent obs.

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• Funded by JSPS

Ø Primary diameter: 1.8m (f/2.29) Ø FOV: 1.56 deg2 (0.5”/pix) Ø Ave. Seeing: 1.4” ( 0.7”(best), 1.2” (50%) ) Ø Detector: 4 x H4RG Ø Filters: Z, Y, J, H, narrow-bands

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• Funded by JSPS

Ø Filter wheel 1

• NBs, Z, Dark, blank

Ø Filter wheel 2

• Y, J, H, blank

wavelength Transmittance Combination of 3 NBs Wide band Each filter wheel has 4 slots

PRIME Narrow Band filters (TBD)

• Observations w/ NB in Z and Y-band can be done by HSC (using CCD)

Y-band: 1.06µm low OH J-band: 1.19µm low OH, Lyα@z=9, [OII]@z=2.2, Hβ@z=1.5 J-band: 1.28µm Pa β H-band: 1.62 µm Hα@z=1.5 H-band: 1.64µm [Fe II]

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PRIME Narrow Band filters (TBD)

• Observations w/ NB in Z and Y-band can be done by HSC (using CCD)

B-band: 0.38µm (HSC/NB387) Lyα@z=2.2 z-band: 0.92µm (HSC/NB921) [OII]@z=1.5 Y-band: 1.06µm low OH J-band: 1.19µm low OH, Lyα@z=9, [OII]@z=2.2, Hβ@z=1.5 J-band: 1.28µm Pa β H-band: 1.62 µm Hα@z=1.5 H-band: 1.64µm [Fe II]

Welcome other idea!

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Off-bulge season/time sciences (50% of time)

• NIR RV planet survey (12% for ABC time)
• 12% for Osaka U time

(roughly 44 nights /yr)

• 12% for UMD/NASA/WFIRST time
• 14% for SAAO time

Possible Idea Ø LAE z~9 survey w/ 1.19µm Ø PRIME-TAO(SWIMS)-Subaru(HSC/ULTIMATE) synergy Ø J, H-band survey (a few mag deeper than 2MASS) Ø Your idea!

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Ranc+18

Galactic bulge surveys in 2020s

PRIME FOV PRIME survey field (TBD) S-JASMINE

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Summary2

• FOV = 1.56 deg2, D= 1.8m, seeing= 1.4”, Z,Y,J,H-bad
• 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

• These are TBD. Welcome other idea!!
• Off-bulge time science
• NB surveys, J,H-band surveys…
• Possible synergy between PRIME, S-JASMINE, and other NIR instruments

toward the galactic bulge

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