大阪大のMOAの経験と今後への教訓

Takahiro Sumi (Osaka Univ.)
2017/3/28, Workshop on Studies on variable stars and extinction law in the Milky Way and nearby galaxies @University of Tokyo

Gravitational Microlensing
Science, 1936
✧If a lens is a star,elongation of images is anorder of 100µarcsec.
✧Just see a star magnifiedstar
100µarcsec.

✧Einstein predicted 1936, but concluded
impossible to observe. Event rate is 1/1M

lensobserver

distortion of space due to gravityl 1986
Watch Millions starsPaczynski

planetary microlensing

Time scale: tp~M1/2 ~1day(MJ)~a few hours (ME)Sensitive to Cold planets
outside of snowline (~3asnow)

MOA (until ~1500)（NZにいた世界１大きな鳥）

l 体長:3.5ｍ

l 体重: 250kg
l 飛べないl 5００年前に絶滅
l （マオリ族が食べ尽くした）

MOA(since 1995)（Microlensing Observation in Astrophysics）（ New Zealand/Mt. John Observatory, Latitude： 44°S, Alt: 1029m ）Seeing ~2arcsec
Clear night: ~50%

なぜ？

Halo Dark Matter & Paczynski’s Idea
20〜40 times more dark matter than visible mass.

MAssive Compact Halo Objects (MACHOs） çè WINPs• MACHO can be observed by Microlensing.（Paczynski 1986)• t〜１０−６ è then watch 10M stars!.

50kpc
LMC

3 surveys started and found MACHO is not the majority of the galactic DM
But it opened the era of massive time-domain survey.

MOA 0.6m telescope（New Zealand/Mt. John Observatory ）Mirror : 0.6m
CCD : 4k x 6k pix.
FOV : 1.3 square deg.
2000-2005 (約6年間)

MOA(since 1995)（Microlensing Observation in Astrophysics）（ New Zealand/Mt. John Observatory, Latitude： 44°S, Alt:

2006~1029m ）Mirror : 1.8mCCD : 80M pix.
FOV : 2.2 deg.2
cadence: 15-50 min.

Earth & Sky - 星空は宇宙への窓

Earth&Sky

2017/07/25 7:28

Earth & Sky と共に宇宙の不思議を体験してみませんか？頭上に広がる夜空を見上げる「星空ツアー」、テカポの雄大な自然を見下ろせる「アストロカフェ」。私たちは常に宇宙の力、科学を学びそれらを共有しています。カンタベリー大学が管理・運営するマウント ジョン天文台にて星々や私たちの住むこの惑星について楽しみながら知識を高めてみましょう。
- 小澤 英之, Directing Manager

天文台星空ツアー(/index.php/ja/tours)

小澤さんが立ち上げた星空ツアー会社：• MOA-II観測室
建設• 現地観測員• MOA-II見学

テカポにあるMt.John(マウントジョン)天文台やCowan’s(コーワンズ)天文台で南半球ならではの星空をご案内いたします。ツ
アーの中では望遠鏡を使って天体をご覧いただいたり、また条件が許せばマウントジョンに設置されている、ニュージーランドで一番大きな望遠鏡のある天文台の施設を見学していただけます。

アストロカフェへようこそ(/index.php/ja/astro-cafe)
マウントジョンの山頂にある見晴らしの良いカフェ、絶景を見ながら美味しいコーヒーでほっと一息つけるテカポの名所です。 新鮮なテカポの空気と360°広がるパノラマをお楽しみ下さい。
「きっと世界で最も素晴らしい場所にあるカフェかもしれな
い」 by "Lonely Planet (ガイドブック)"http://www.earthandsky.co.nz/ja/

2/4 ページ

建設
望遠鏡とレンズを現地で初めて組み立て2005年
光学調整難航カメラーレンズ間に１cmのギャップ！
NZのPIの友達が発見

Lens3+4とlens1+2のアライメントー＞ハルトマン
テストで調整主焦点カメラ冷えない。60Hz->50Hz

冷凍機をアップグレード

シャッター破れる

幕巻取機

破れないシャッター１号機

破れないシャッター破れる

破れないシャッター２号機

強風

1. ⇧⌃" BCD✓⇡⇢ E5⌅! ◆6F⌃⇣⌘: 300sec ◆6 60sec @ G⌅
$K⇡H 1/5 LM7 NO 1P->QJ"F⌃⇣⌘ ⇡⌅ (RSTUVWXL Y◆ ⇡⌅⌧✓◆

迷光O1H✓IJ

遮光装置１号

୺㙾ഃ䛛䜙ぢ䛘䜛䛸▮༳䛾㠃䠄❆ഃ䛾㠃䠅䛾䝔䜹䝸䛜Ẽ䛻䛺䛳䛯䚹䛣䜜䜎䛷䛾ㄪᰝ䛷䚸䛱䜗䛖䛹䛣䛾㠃䛾䛒䛯䜚䛻୺㙾ീ䛜෗䜛䛯䜑䚹཯ᑕ⋡䛜ᑠ䛥䛟䛶䜒㠃䛜Ⲩ䜜䛶䛔䛺䛔䛸CCDୖ䛻䝕䝣䜷䞊䜹䝇䛥䜜䛯ീ䛜⤖ീ䛧䛶䛧䜎䛖ྍ⬟ᛶ䛜䛒䜛䚹

遮光装置2号

Observation by MOA•50 deg.2(20Mstars)
G.C.

1obs./night.(>MJup)•1obs./95min.(Mjup)
1obs./47min. (Mnep)
1obs./15min. (MÅ)è~600events /yr

http://www.massey.ac.nz/~iabond/alert/alert.html

Survey & follow-up to detect exoplanetsMOA-2009-BLG-266Lb
MOA foundplanetarydeviation inrealtime

q~5.8x10-5
s~0.91

Followed
up bytelescopes
around theworld
データの即時公開：
共同研究：

Planetary signal

w/o planet

100を超えるオーサー
紛争もあるが。

Muraki et al.(2011)

PRIME (PRime-focus Infrared
Microlensing Experiment)

Takahiro Sumi (Osaka Univ.)
2017/3/28, Workshop on Studies on variable stars and extinction law in the Milky Way and nearby galaxies @University of Tokyo

PRIME Wide FOV
1.8m Telescope at SAAO
Sothern African
Astronomical  !
Observatory!

Diameter: 1.8m, (f/2.29)
FOV:1.25°x1.25°=1.56deg2(0.5”/pix)(6xfull moon) World Largest FOV
H-band Hi-res spectrograph

Alt. 1761m

Expected picturePRIME (PRime-focus InfraredMicrolensing Experiment)
Objectives:
1. Microlensing Exoplanets (〜50%)•••••

Study low-mass planets outside of snowline
Plant frequency in the Galaxy Center
WFIRST microlensing survey field optimization
Concurrent observations with WFIRST
Characterize H4RG detectors

2. Other sciences (〜50%)

PRIME collaboration

lOsaka Univ.: T Sumi (PI), H. Shibai, T. Matsuo
lABC (Astro-Biology Center): M. Tamura (U Tokyo)
à望遠鏡
lNASA GSFC: D. Bennett, R. K. Barry , A. Kutyrev,
lU of Maryland: Sylvain Veilleux, Drake Deming
àカメラ製作lSAAO: Ted Williams (Director)+àDome + building
Bond(Massey U), N. Rattenbury (U Auckland), J-P. Beaulieu (IAP), A. Fukui (NAOJ),
T. Nagayama (Kagoshima U), N. Matsunaga, Norio Narita (U Tokyo), Yasushi
Muraki, Fumio Abe (Nagoya U), Mikio Kurita (Kyoto U), Joachim Wambsganss,
Luigi Mancini (U Heidelberg), Eamonn Kerins (U Manchester), David Charbonneau（Harvard、Mearth PI、TESS CoI）、Cullen Blake (Pennsylvania、TESS CoI)

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

disk

Galactic bulge is highly obscured.

NIR

u More stars & more events at GC.
（〜2400events/yr, 〜12planets/yr）
u Smaller radius source (redder) enable us
to detect low(Earth)-mass planets. (smallfinite source effect)u Planet frequency at GC.
u Select WFIRST fields.
u Simultaneous observation with WFIRST tomeasure lens mass.
u Mass Function at GC （planet-Black Hole）

The World Widest FOV in NIR withWorld Largest class NIR camera
Loan Four Teledyne HgCdTe 4kx4k H4RG-10 (10μm pitch)
Wide-Field
InfraRed Survey
Telescopefrom
WFIRSTteam(NASA)
Astrophysics Focused Telescope Assets
WFIRST-AFTA
Final Reportby theScience Definition Team (SDT) and WFIRST Project

Four H4RG-10 which WFIRSTTeam owns. (1 chip is dummy)

Diameter:1.8m, f/2.29,
FOV:1.25°x1.125°, 0.5arcsec/pix
April 30, 2013
Will be Manufactured by NASA @GSFC

Camerawill be Manufactured by NASA @GSFC• Operational temperature: 90-100K• the normal outputs can probably go
as high as 500 kHz, but likely
something like 300-400 kHz.
• The system reads out the full array in
11 seconds at 100 KHz.
• 16 Read-out ports per chip (64outputs are available.)• 16x4chips=64 read out ports.
• I asumme 4seconds for read out w/300 kHz.
• Leach controller or Sidecar

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 with Spitzer
We can do sameobservations
with WFIRST

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

– 25 –

OGLE-2015-BLG-0966/MOA（Street et al. 2015)
2015-BLG-281
Spitzer

Neptune mass planetOff-bulge season sciencesl Transit search for M-dwarfs:• Search for habitable planets around M-dwarf which is bright in IR• Follow-up transit candidates by HAT-South, Mearth projects forselect real planets and measure the atmosphere.
• Systematics due to Sunspot and limb darkening is smaller in IR.
• Wide FOV enable us to observe many reference stars for highprecision photometry.
• Follow-up TESS candidates. TESS is optical. Need IR for Mdwarfs. Collaborators:
David Charbonneau（Harvard、Mearth PI、TESS CoI）、
Cullen Blake (Pennsylvania、TESS CoI)、
Narita（NAOJ, TESS CoI）、Fukui（Okayama）

l Search for counterparts of high-z GRB, GW etc. ….
l H-band spectrograph: RV for giant planets around M-dwarf.

Gravitational Wave counter part

Schedule
2016 detail design2017 manufacture
Agreement of academic exchange withSAAO and University of Maryland
2018 manufacture, construction2019 install, first light. observation start〜
2023 create event rate map in the bulge
2025 WFIRST launch,Concurrent observation start
2031 continue to the end of the WFIRST

Summary
中小プロジェクトは、l 現地コラボレーターが大事à維持費が大事 （ベストではないが）l サイエンスコラボレータが大事àデータ公開が大事