2019 9 13 13:48-14:00
2019.9.13
13 48 14 00
E 会場
UTokyo, Dept. of Astronomy
AAstrobiologybi lCCenter off NINSNAOJ of NINS

Motohide Tamura

Ｋ（１０russh2）
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immaging Phase
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DDirectimmaging phase
pK
Keplerpplanetr
releasend Jupiter (Suubaru)

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Keplerpplanetrrush

8

Dettection method
dsDiscovery Year22

1Planeet Nuumber (/Yeear）

Various techniques have discovered>4000 planets (confirmed) with various methodsVarious Planets detected by Various Techniques

Jovian Planets
HotJupiters

JupiterSuper-Earths
NeptuneEarth3

Direct Imaging can now image wide-orbit planets

4

Jovian Planets

Wide-Orbit Planets((Directlyect y Imaging;ag g;
SCExAO)Hot
Jupiters

JupiterSuper-Earths
NeptuneEarthDirectly Imaged Planets Gallery(not full list & SEEDS planets introduced in detail later)

HR 8799 bcde

(A star ;Marois+08,10)

β Pic b(A star; Lagrange+10)

Fomalhaut b ??

GJ504 b(A star; Kalas+08,13)(G star; Kuzuhara+13)
HiCIAO

Marois+08, 10©NRC HIA, Marois©NRC‐HIA,& Keck Observatory

51 Eir b(F star; Macintosh+15)©ESO/Lagrange© NASA/ESA/Kalas

2M1207 b(BD; Chauvin+04,05)

Kappa And b(B star; Carson+12)
HiCIAO©NAOJ/Subaru/ABC

ROX 42B b(YSO; Currie+14)©Gemini©ESO/VLT©NAOJ/Subaru

Wide‐orbit planets can be detected currently only by direct imaging;
Many are a>=100 AU; only handful for Solar‐system‐scale orbit planets.

Major Results of Planet Formation Sites
SEEDS has observed scattered light from disks and revealed
many disk structures of less than 100AU scale that are possible
signs of planet formation in such young (a few Myr) systems!
Many directly-maged small gaps/spirals in disks since 2010.
Hubble Telescope image
is not enough to study
disk structure…

UScoJ1640‐2130
Gap
Ring100AU

Mayama+12

SAO206462□ Gaps
A disk gap may be evidence fordynamical interactions between
a planet and its gaseous disk.
□ Spirals
A gravitational perturbation froman embedded planet generate
spiral density waves.

Muto+12

SEEDS has revealed gaps & rings of <100AU scale in many disks bypolarimetric imaging (Res.~0.06”, IWA~0.1”) since 2010
NNotethath ALMA HL TTau imagei(2015) isi thermalhl emissioni i .

ALMAHL Tau&TWHyaDirect Imaging instruments SCExAO/CHARIS
Enabling direct spectroscopy on Subaru
Open use on Subaru, Publication rush now.
Extreme adaptive optics SCExAO

HR8799Kappa And
HR8799の３つの惑星の画像

Kappa And b
CHARIS spectrum
Integral field spectrometer
HIP 79977
CHARIS
面分光器 CHARIS
Uyama et al. 2019; Currie et al. 2019, ApJ; Asensio-Torres et al. 2018, A&A; Currie et al. 2018, AJ;
Goebel et al. 2018, AJ; Guyon 2018, ARAA; Rich et al. 2018, AJ.

Direct Imaging with TMT (but not excatly)

Jovian Planets

Wide-Orbit Planets((Directlyect y Imaging;ag g;PSI)

Hot
Jupiters

JupiterSuper-Earths
NeptuneEarth9Our Strategy to “2nd Earth” Imaging
Develop andValidate CriticalTechnologies

Measured
on-skyperformance

EnableObserve Giant
Planets in reflected
light @ SubarupTelescope

Validate

HR 8799 c,d,e(SCExAO/CHARIS)
Self‐lluminous planets(not in reflected light)

Technologyrequirements

Coordinate withTMT International
ObservatoryExperience in onsky operation andscientific analysis

Sciencemeasurements,t
Exoplanet targets

Instrument
designdesign,
deployment plan

Formulate Detailed Planfor Probing forExtrasolar Life with TMT
From Guyon

SCExAO/TMT vs. Future Missions

Star-Planet Contrrast□ Current Ground‐based Surveys:‐ GPI survey‐ SPHERE survey‐ Current SCExAO□ Future missions:‐ JWST
coronagraph‐ WFIRST
coronagraphh□ Subaru SCExAO goal:‐ 10^‐8 at 0.1”
□ Earth‐like planets:
p‐ TMT+PSI/b (M stars)‐ 10^‐8 at 0.01”

Ｆｒｏｍ Ｅｘｏ－Ｃ ｒｅｐｏｒｔ

GJ504bKnown RV planets

PSI: a modular 2nd Earth Imager

PSI/blue spec
PSI/blWavelength: 0.6‐1.8 um
Contrast: 10^(‐8) at 1‐2λ/DOwn DM (tweeter): maybe MEMS
‐ 100 x 100 actuators minimum‐ Stroke: > 1 um
‐ Speed: 5 kHz, ‐ Actuator pitch: < 0.5mm

Common DM spec
Common DM (woofer)‐ 120 x 120 actuators‐ Stroke: 10um WF to correct for full TMT pupil‐ Speed: 2 kHz‐ actuator pitch: 1.5mm (pupil size 180mm diameter)

MODHIS as TMT 1st light exoplanet instrument
NFIRAOSStrehl=0.3, 0.4, 0.5, 0.75 (Y,J,H,K)

Fiber Injection
jUnit
5x5 multi object

PSI
第2期装置
Extreme AO

Spectrometer
0.95‐2.5um, R=100,000• 0.97-2.5um, R=100,000, mini IFU 5x5 NIR spectrometer• Combined with AO (NFIRAOS),(NFIRAOS) To be combined with PSI• Single mode fiber-fed, so no modal noise and very compact((40x80x30 cm^3)) instrument• Successor (for TMT) of Keck/HISPEC and Subaru/IRD• NIR-RV (10cm/s), CC spectroscopy, planet surface map

SummarySuay
Dedicated exoplanet
i tinstrumentst willill bbe
critical for TMT even atits first light phase↓
・MODHIS・PSI (and MICHI thermal)
in two phases↓Imaging & Spectroscopy ofTemperate Rocky Exoplanets
Synergy with WFIRST/CGI

TMT and ALMA are in fact astrobiology telescopes.