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Direct E Direct E xplorations of xplorations of E E xoplanets and Disks xoplanets and Disks p with Subaru with Subaru Suba u Suba u Joint Subaru/ Gemini Science Conference Joint Subaru/ Gemini Science Conference 2009 5 20 10:00 2009

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SLIDE 1

Direct E xplorations of Direct E xplorations of E xoplanets and Disks E xoplanets and Disks p with Subaru with Subaru Suba u Suba u

Joint Subaru/ Gemini Science Conference Joint Subaru/ Gemini Science Conference 2009 5 20 10:00 2009 5 20 10:00-10:30 10:30 2009.5.20 10:00 2009.5.20 10:00 10:30 10:30

  • M. Tamura
  • M. Tamura
  • M. Tamura
  • M. Tamura

National Astronomical Observatory of Japan National Astronomical Observatory of Japan

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SLIDE 2

Talk Outline Talk Outline Talk Outline Talk Outline

1 Highlights of Subaru high contrast 1 Highlights of Subaru high contrast

  • 1. Highlights of Subaru high-contrast

sciences so far

  • 1. Highlights of Subaru high-contrast

sciences so far

  • Diversity of protoplanetary disk

morphology

  • Diversity of protoplanetary disk

morphology p gy

  • Low-mass companions

2 Next step p gy

  • Low-mass companions

2 Next step

  • 2. Next step
  • HiCI AO & SEEDS

SEEDS status

  • 2. Next step
  • HiCI AO & SEEDS

SEEDS status

  • SEEDS status
  • 3. Summary
  • SEEDS status
  • 3. Summary
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SLIDE 3
  • 1. Clouds collapse under gravity Current Paradigm of Star

and Planet Formation

DIRECT OBS. Need < 1” resolution

2 Protoplanetary disks

DIRECT OBS. Need < 1 resolution Currently best studied at NIR

  • 2. Protoplanetary disks
  • 3. Comets &

10,000 yr IRSF/SIRIUS m asteroids form

  • r

Vega-like stars Kaguya Vega l ke stars 1 Myr Subaru/CIAO

  • 4. Planetary

system Subaru/CIAO 10 Myr Subaru/CIAO/POL 100 Myr

  • 0. Cloud and cloud cores (NRO)

~270 systems known

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SLIDE 4

Subaru has an AO Coronagraph since 2001

CI AO + 36-actuator AO at Cass.

Fi t d di t d ld h 8 t l

 First dedicated cold coronagraph on 8-m telescopes

Di it f t Compact disk around Y l Diversity of proto- Planetary disks Compact disk around massive YSOs Young very low-mass Companion

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SLIDE 5

Disk - morphological diversity of young and debris disks

Subaru+CIAO+AO36 Science Summary

p g y y g

AB Aur: spiral structure in protoplanetary (PP) disk revealed (Fukagawa et al. 2004).

HD142527: new-type of PP disk morphology discovered

HD142527: new-type of PP disk morphology discovered (Fukagawa et al. 2006) & imaging of ice (Honda et al. 2009).

FN Tau: first PP disk around lowest-mass (0.1 Mo) star directly imaged (Kudo et al 2007) directly imaged (Kudo et al. 2007).

Beta Pic: First NI R polarimetry with coronagraph revealed nature of debris disk dust (Tamura et al. 2006). i di k ( h i ki )

Binary disks: GG Tau, UY Aur, etc. (I toh, Hioki, Mayama)

Exoplanets/ brown dwarfs - new types of companions?

DH Tau, GQ Lup, EK60: "boundary objects" between planets

DH Tau, GQ Lup, EK60: boundary objects between planets and brown dwarfs around T Tauri stars discovered (I toh et al. 2005; Neuhauser et al. 2005; Kuzuhara et al. 2009 - see his poster). poster).

HR8799 image in 2002 (Fukagawa et al. 2009).

Massive star disk - evidence for formation by accretion

BN S140I R I RAS23033 S255I RS1&3 N7538I RS1 Ubi i

BN, S140I R, I RAS23033, S255I RS1&3, N7538I RS1 : Ubiquity

  • f compact disks around massive (at least up to ~ 10 Mo)

YSOs (Jiang et al. 2005, 2007).

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SLIDE 6

Spiral-shape disk around 2Mo-4Myr Herbig Ae star: AB Aur Herbig Ae star: AB Aur

12CO

100 AU Fukagawa, Hayashi, Tamura+ 2004, ApJ

f i t Velocity field

Corder+2006 OVRO

100 AU

fainter star brighter

(d 144 )

1.6 μm

flared disk

 disk with spiral arms (r=450 AU) 700 AU (d=144 pc)  disk with spiral arms (r=450 AU)  trailing arm ← com. w/radio data

+ brighter forward scattering b i i i

1000 AU  no nearby companions in our images;

but see Oppenheimer+08

Grady+ 1999

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SLIDE 7

Submm follow Submm follow-

  • up and planet formation

up and planet formation scenario revisited scenario revisited

Gravitational instability?

(instability condition)：

scenario revisited scenario revisited

1     G c Q

s

(instability condition)：

Probably supplies of matter from the envelope maintain the weak instability.

⇒ Q ~ 2; “weak” instability

A suggestion of planet formation by gravitational instability? (for some systems)

White contours: White contours:

y

( y )

Matsuo+ 2007, ApJ Also note recent imaging

White contours: White contours: 345 GHz dust continuum (SMA) 345 GHz dust continuum (SMA) Lin+ 2006, ApJ Lin+ 2006, ApJ

discovery of outer (> 10AU) planets around A stars (Marois; Kalas). Mdisk ~0.15M

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SLIDE 8

NE W type of disk: HD142527 – banana split

H bi A i L (d 200 ) Herbig Ae star in Lupus (d=200pc) 1550 AU

disk gap central gap disk asymmetry

λ=1.65 micron λ=24.5 micron

disk asymmetry confirmed at MI R

Subaru/CIAO (Fukagawa+2006, ApJ) Subaru/COMICS (Fujiwara+2006, ApJ)

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SLIDE 9

Where is the snow line in protoplanetary disks? in protoplanetary disks?

Honda+ 2009, ApJ

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SLIDE 10

No feature

=145AU

3.1m feature

  • ice absorption everywhere

T(dust)=82 85K (by MIR; – T(dust)=82-85K (by MIR; Fujiwara+2006) – cold enough cold enough

  • Snow line is much inner

R << 140AU – Rsnow << ～140AU Honda+ 2009

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SLIDE 11

Disk - morphological diversity of young and debris disks

Subaru+CIAO+AO36 Science Summary

p g y y g

AB Aur: spiral structure in protoplanetary (PP) disk revealed (Fukagawa et al. 2004).

HD142527: new-type of PP disk morphology discovered

HD142527: new-type of PP disk morphology discovered (Fukagawa et al. 2006) & imaging of ice (Honda et al. 2009).

FN Tau: first PP disk around lowest-mass (0.1 Mo) star directly imaged (Kudo et al 2007) directly imaged (Kudo et al. 2007).

Beta Pic: First NI R polarimetry with coronagraph revealed nature of debris disk dust (Tamura et al. 2006). i di k ( h i ki )

Binary disks: GG Tau, UY Aur, etc. (I toh, Hioki, Mayama)

Exoplanets/ brown dwarfs - new types of companions?

DH Tau, GQ Lup, EK60: "boundary objects" between planets

DH Tau, GQ Lup, EK60: boundary objects between planets and brown dwarfs around T Tauri stars discovered (I toh et al. 2005; Neuhauser et al. 2005; Kuzuhara et al. 2009 - see his poster). poster).

HR8799 image in 2002 (Fukagawa et al. 2009).

Massive star disk - evidence for formation by accretion

BN S140I R I RAS23033 S255I RS1&3 N7538I RS1 Ubi i

BN, S140I R, I RAS23033, S255I RS1&3, N7538I RS1 : Ubiquity

  • f compact disks around massive (at least up to ~ 10 Mo)

YSOs (Jiang et al. 2005, 2007).

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SLIDE 12

DH Tau B & GQ Lup B & E K60: Planets or Brown Dwarfs ?

QG Lup B

Planets or Brown Dwarfs ?

  • Very low-mass

companions around companions around T Tauri Stars; what are they?

  • spectroscopic temperature

spectroscopic temperature estimate is still not reliable

  • thus, we use

age/luminosity ~ 10MJ age/luminosity

  • then DH Tau, GQ Lup,

EK60 are three of the lowest and nearly ~ 15MJ 10MJ lowest and nearly planetary-mass companions. But they are very far

  • bserved

w/ CI AO

  • But they are very far

from star (>100AU)

Itoh, Tamura, Hayashi+05

w/ CI AO DH Tau B

Neuhauser+05 Luhman+06 Kuzuhara+09 H-band (1.6μm) image

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SLIDE 13

Then, finally "planets" imaged around A stars: HR8799 Fomalhaut b Pic A stars: HR8799, Fomalhaut, b Pic

3 5

HST GEMINI+KECK VLT

2.5 3 3.5 U))

EK60 CT Cha B GQ Lup B DH Tau B CHXR73 B AB Pic B 1RXSJ1609 B

1 1.5 2 log (a(AU

GQ Lup B

SEEDS i t t

0.5 1 5 10 15 20 25 30

SEEDS main target space

5 10 15 20 25 30 Mass (M_Jup)

Subaru/CIAO in 2002 July

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SLIDE 14

Nasmyth platfo rm Nasmyth platfo rm

Subaru new coronagraph - HiCIAO

e

e r aph r aph le le tr ast tr ast

  • dule
  • dule

War m War m Co Cold ld

esc o pe esc o pe

  • mmo n
  • mmo n

ptic s + ptic s +

O Module Module Cor

  • nagr

Cor

  • nagr

Modul Modul Camer a Camer a Module Module igh Cont igh Cont ptic s Mo ptic s Mo

T ele T ele

Co Co O

AO AO C IR C IR C M Hi Hi Op Op

Cor

  • nagr

aph Cor

  • nagr

aph Differ ential Differ ential optic s

  • ptic s

( i ( i Hawaii 2 Hawaii 2-

  • R

G R G 2k k   2k array array 188 ac tuator s 188 ac tuator s F

  • c al masks

F

  • c al masks

Pupil sto ps Pupil sto ps (Wo llasto n prisms (Wo llasto n prisms

  • single /

do uble ) single / do uble ) 2k k   2k array array

ASIC Sidec ar Contr

  • ller

ASIC Sidec ar Contr

  • ller

F ilter s F ilter s Co mmo n+Diffe re ntial Co mmo n+Diffe re ntial AO AO F uture F uture : Co mple me ntary Co mple me ntary ME M DM (32 ME M DM (3232 32) ) Co mmo n+Diffe re ntial Co mmo n+Diffe re ntial

Camera

Wollaston Prism

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SLIDE 15

HiCIAO Specifications

F IR N th（ / AO188） Focus IR Nasmyth（w/ AO188） Wavelength 0.85 – 2.50 microns Observation modes DI PDI SDI ADI (w/ & w/o coronagraph) Observation modes DI, PDI, SDI, ADI (w/ & w/o coronagraph) Resolution 0.03" (J), 0.04" (H), 0.055" (K) Strehl ratio 0.2 (J), 0.3 (H), 0.5 (K) with AO Strehl ratio 0.2 (J), 0.3 (H), 0.5 (K) with AO Field of view 20"x20" (DI), 20"x10" (PDI), 5"x5" (SDI) Contrast 103.8 at 0.1", 105.5 at 1.0" (SDI w/ coronagraph) Pixel scale 0.010"/pix Occulting masks 0.2", 0.3", 0.4", 0.6", 1.5" diameter Filters Y, J, H, Ks (DI, PDI), CH4, FeII, H2 (SDI)

5" 10"

1.625um

5 5"

1.600um 1.575um 1.644um

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SLIDE 16

SEEDS – Subaru Strategic Exploration of Exoplanets and Disks Exploration of Exoplanets and Disks with HiCIAO/AO188

 First "Subaru Strategic Observations"  First Subaru Strategic Observations  120 nights in 5 years on Subaru  Direct imaging and census of giant planets around solar-type g g g p yp stars in the outer regions (~4-40 AU)  Exploring protoplanetary disks and debris disks for origin of their diversity and evolution at the same radial regions  Direct linking between planets and protoplanetary disks

HiCIAO 0 6" mask 0.6" mask coronagraph images in images in ADI mode

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SLIDE 17

SE E DS Target Summary as of Jan 09

Category Planet searches (in methane SDI / ADI mode) Disk Searches (in PDI mode) Total number (a) (b) (c) (d) (e) number SFR YSOs Open cluster

& Moving Group

Nearby stars & WDs

Protoplanetary

disks Debris disks Number 90 100 140+37 130 70 567 Number 90 100 140+37 130 70 567 Distance ~140 pc <125 pc <30 pc ~140 pc <130 pc 100 M 5 M Age 1-10 Myr 10~100 Myr 100 Myr

  • 1 Gyr

1-10 Myr 5 Myr

  • 6 Gyr

Comment Tau/Sco

UPleiades/ l MG

subcategory

TTS/HAeBE/ polarized

SST/AKARI l Comment Tau/Sco

several MGs

subcategory

polarized sources

sample

RA-DEC H-mag R-mag Sp-Type

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SLIDE 18

 24 institutes 91 members (20 foreigners).

SE E DS Members & Stutus

( g )

  • Principal I nvestigator (PI ): M. Tamura (NAOJ)
  • Co-PI : T. Usuda, H. Takami (NAOJ)
  • Co-I : (NAOJ) T. Fujiyoshi, O. Guyon, Y. Hayano, M. I ye, M. I shii, R.

d i b k b d i h S Kandori, R. Kawabe, E. Kokubo, T. Kudo, F. Martinache, S. Mayama,

  • S. Miyama, N. Murakami, J. Morino , N. Narita, J. Nishikawa, T. S.,

Pyo, H. Saito, R. Suzuki, H. Suto, N. Takato, Y. Takeda, H. Terada, N. Ukita, K. Usuda, M. Watanabe; (GUAS) J. Hashimoto, T. Tsukagoshi, , , ; ( ) , g , (Takahashi, Suenaga); (Univ. of Air) N. Kaifu; (Hokkaido Univ.) N. Baba; (Tohoku Univ.) M. Kitamura, T. Yamada; (I baraki Univ.) Y. Okamoto, M. Momose; (Univ. of Tokyo) M. Kuzuhara , H. Makitsubo,

  • M. Ueno; (TI TECH) S. I da, B. Sato; (I SAS) K. Enya, K. Kataza, T.

; ( ) , ; ( ) y , , Nakagawa, M. Ootsubo; (Kanagawa Univ.) M. Honda; (Nagoya Univ.)

  • T. Kano, E. Kato, Y. Morishita, A. Nakajima, T. Sumi, H. Yamamoto;

(Osaka Univ.) M. Fukagawa, H. Shibai; (NCC) K. Sugitani; (Kyoto Univ.) T. Fukue, S. I nutsuka, T. Muto; (Kobe Univ.) T. Hioki , Y. I toh, Univ.) T. Fukue, S. I nutsuka, T. Muto; (Kobe Univ.) T. Hioki , Y. I toh, I . Mann, Y. Oasa,; (Princeton) A. Burrows, J. Kasdin, J. Knapp, M. McElwain, A. Moro-Martin, Y. Shen, D. Spergel, E. Turner、R. Vanderbei; (Hawaii) K. Hodapp; (JPL) T. Mastuo, G. Serabyn; (ASI AA)

  • J. Karr, N. Ohashi, M. Takami; (Max Planck) W. Brandner, J. Carson ,
  • J. Karr, N. Ohashi, M. Takami; (Max Planck) W. Brandner, J. Carson ,
  • M. Feldt, M. Goto, T. Henning, M. Janson, C. Thalmann; (Nice) L. Abe;

(Hertforshire) T. Gledhill, J. Hough, P. Lucas; (Goddard) C. Grady; (Washington) J. Wisniewski

SAC and TAC already approved! SEEDS will start in 09B as soon as PV finished.

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SLIDE 19

SUMMARY

 Various results with Subaru CI AO+ AO36 have

been reviewed: disk diversity, disk ice, nearly planetary mass companions at distance massive planetary mass companions at distance, massive star disks, and polarimetry.

 SEEDS will conduct a 5-year legacy survey of

y g y y ~ 500 solar-mass and massive young stars for direct imaging of exoplanets and disks in 120 nights with a "all-Japan" team collaborating with nights with a all Japan team collaborating with foreign researchers.

 Our targets consist of 5 categories, each of which

includes about ~ 100 stars (enough for statistics) includes about ~ 100 stars (enough for statistics).

 We believe that we can image at least a handful

  • f giant (< 13 MJ) exoplanets in a few to 10s AU

g ( ) p regions and the similar radial regions of many disks in each category.

 Various follow-up programs should be organized  Various follow-up programs should be organized,

including spectroscopy with various instruments and telescopes.