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. on behalf of the PRIME collaboration 1 Jul 1, 2019

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Summary Ø The first dedicated NIR microlensing survey Ø First light in 2020 Ø Mirror: 1.8m @SAAO (1.4”), H limit =18.7mag, Y limit =19.6mag (5σ, 100sec) Ø Prime Focus NIR Camera Ø Use four H4RG, f/2.29 à 1.25° x 1.25° = 1.56 deg 2 (0.5”/pix) Ø Z, Y, J, H-band, three narrow band filters (TBD) Ø Conduct microlensing survey when the bulge is visible Ø NIR RV survey for planets around M-dwarfs o Follow up transients (GW, GRB, SNe, …) (TBD) o NIR BB / NB surveys (TBD) 3

Schedule (as of 2019 Jul) Ø 2019 manufacture, construction Ø 2020 camera install, first light Ø 2021 microlensing survey starts Ø 2023 create event rate map in the bulge Ø 2025 WFIRST launch, concurrent obs. starts Ø 2030 continue to the end of the WFIRST 4

Planetary Micr crolensing Time scale: t p ~ M 1/2 ~1day( M J ) ~a few hours ( M E ) Brightness Sensitive to Cold planets outside of snowline (~3 a snow ) Time 5

Planetary Micr crolensing Time scale: t p ~M 1/2 ~1day(M J ) ~a few hours (M E ) Brightness Sensitive to Cold planets outside of snowline (~3a snow ) Time 6

Discovered Planets and micr crolensing Sensitivity current •RV •Transit (Kepler) •Direct imaging •Microlensing Mass measurements Mass by Bayesian WFIRST 7

Wh Why y NIR microlensi nsing ng pl plane net sur survey? y? Ø Less 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 Jung+19 1 day 8 Suzuki+16

Wh Why y NIR microlensi nsing ng pl plane net sur survey? y? Ø Less 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 Ø Optimize the WFIRST microlensing field (Precursor Obs.) Ø Concurrent observations with WFIRST 9

Precursor obs. Optimize WFIRST micr crolensing survey fiel elds s by y ma mapping g the e even ent rate e in NIR IR G.C. Galactic disk WFIRST b � degree � Event rate map in optical l (degree) (Sumi & Penny 2016) Event rate varies by a factor of 2 � peak is at l = 1 ） 10

Precursor obs. Optimize WFIRST micr crolensing survey fiel elds s by y ma mapping g the e even ent rate e in NIR IR PRIME Survey (TBD) G.C. Galactic disk WFIRST b � degree � l (degree) (Sumi & Penny 2016) Event rate varies by a factor of 2 � peak is at l = 1 ） 11

Precursor obs. Optimize WFIRST micr crolensing survey fiel elds s by y ma mapping g the e even ent rate e in NIR IR PRIME Survey (TBD) G.C. Galactic disk WFIRST b � degree � • 21 fields (27 deg 2 ) / hr • 3 fields (3.9 deg 2 ) / 15 min + 9 fields (11.6 deg 2 ) / hr l (degree) (Sumi & Penny 2016) Event rate varies by a factor of 2 � peak is at l = 1 ） 12

Concurrent obs. Spitzer-Ground delay = 20 days 13

Concurrent obs. GAIA (at L2) – Earth parallax measurement Ø ��������������������������������� ���������������� • ��������������������������� 14 Wyrzykowski+19

������ ���������� ��������� Funded by JSPS ��������������������������������� ����������� Ø Primary diameter: 1.8m (f/2.29) Ø FOV: 1.56 deg 2 (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 15 ���������������������������

������ NBs, Z , Dark, blank Y , J , H , blank ���������� ��������� Funded by JSPS ��������������������������������� ����������� Ø Filter wheel 1 • Ø Filter wheel 2 • Combination of 3 NBs Each filter wheel has 4 slots Transmittance Wide band wavelength 16

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] 17

Welcome other idea! 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] 18

Possible Idea 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 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! 19

Galactic bulge surveys in 2020s PRIME survey field (TBD) PRIME FOV S-JASMINE 20 Ranc+18

Summary2 • FOV = 1.56 deg 2 , 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 21