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 5 20 10:00-10:30 2009.5.20 10:00 2009.5.20 10:00 10:30 10:30 10:30 M. Tamura M. Tamura M. Tamura M. Tamura National Astronomical Observatory of Japan National Astronomical Observatory of Japan
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 1. Highlights of Subaru high-contrast sciences so far sciences so far - Diversity of protoplanetary disk - Diversity of protoplanetary disk morphology morphology p p gy gy - Low-mass companions - Low-mass companions 2 Next step 2 Next step 2. Next step 2. Next step - HiCI AO & SEEDS - HiCI AO & SEEDS - SEEDS status - SEEDS status SEEDS status SEEDS status 3. Summary 3. Summary
1. Clouds collapse under gravity Current Paradigm of Star and Planet Formation DIRECT OBS. Need < 1” resolution DIRECT OBS. Need < 1 resolution Currently best studied at NIR 2 Protoplanetary disks 2. Protoplanetary disks 3. Comets & m asteroids form 10,000 yr Kaguya or IRSF/SIRIUS Vega-like stars Vega l ke stars 1 Myr Subaru/CIAO Subaru/CIAO 4. Planetary system 10 Myr Subaru/CIAO/POL 100 Myr ~270 systems 0. Cloud and cloud cores (NRO) known
Subaru has an AO Coronagraph since 2001 CI AO + 36-actuator AO at Cass. First dedicated cold coronagraph on 8-m telescopes Fi t d di t d ld h 8 t l Compact disk around Compact disk around Diversity of proto- Di it f t Young very low-mass Y l massive YSOs Planetary disks Companion
Subaru+CIAO+AO36 Science Summary Disk - morphological diversity of young and debris disks 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). Binary disks: GG Tau, UY Aur, etc. (I toh, Hioki, Mayama) i di k ( h i ki ) 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 BN, S140I R, I RAS23033, S255I RS1&3, N7538I RS1 : Ubiquity Ubi i of compact disks around massive (at least up to ~ 10 Mo) YSOs (Jiang et al. 2005, 2007).
Spiral-shape disk around 2Mo-4Myr Herbig Ae star: AB Aur Herbig Ae star: AB Aur Fukagawa, Hayashi, Tamura+ 2004, ApJ 12CO f i t fainter 100 AU 100 AU Velocity field Corder+2006 OVRO star brighter 1.6 μm flared disk (d 144 (d=144 pc) ) 700 AU disk with spiral arms (r=450 AU) disk with spiral arms (r=450 AU) trailing arm ← com. w/radio data + brighter forward scattering 1000 AU no nearby companions in our images; b i i i but see Oppenheimer+08 Grady+ 1999
Submm follow Submm follow- -up and planet formation up and planet formation scenario revisited scenario revisited scenario revisited scenario revisited Gravitational instability? (instability condition) ： (instability condition) ： c G s 1 Q 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) y ( y ) Matsuo+ 2007, ApJ Also note recent imaging White contours: White contours: White contours: White contours: M disk discovery of outer (> 10AU) 345 GHz dust continuum (SMA) 345 GHz dust continuum (SMA) ~0.15M planets around A stars Lin+ 2006, ApJ Lin+ 2006, ApJ (Marois; Kalas).
NE W type of disk: HD142527 – banana split H Herbig Ae star in Lupus (d=200pc) bi A i L (d 200 ) 1550 AU disk gap central gap disk asymmetry disk asymmetry confirmed at MI R λ =1.65 micron λ =24.5 micron Subaru/CIAO Subaru/COMICS (Fukagawa+2006, ApJ) (Fujiwara+2006, ApJ)
Where is the snow line in protoplanetary disks? in protoplanetary disks? Honda+ 2009, ApJ
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 snow << ～ 140AU R << 140AU Honda+ 2009
Subaru+CIAO+AO36 Science Summary Disk - morphological diversity of young and debris disks 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). Binary disks: GG Tau, UY Aur, etc. (I toh, Hioki, Mayama) i di k ( h i ki ) 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 BN, S140I R, I RAS23033, S255I RS1&3, N7538I RS1 : Ubiquity Ubi i of compact disks around massive (at least up to ~ 10 Mo) YSOs (Jiang et al. 2005, 2007).
QG Lup B DH Tau B & GQ Lup B & E K60: Planets or Brown Dwarfs ? 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 age/luminosity - then DH Tau, GQ Lup, ~ 15MJ EK60 are three of the lowest and nearly lowest and nearly ~ 10MJ 10MJ planetary-mass companions. observed w/ CI AO w/ CI AO - But they are very far But they are very far DH Tau B from star (>100AU) Itoh, Tamura, Hayashi+05 Neuhauser+05 Luhman+06 Kuzuhara+09 H -band (1.6 μ m) image
Then, finally "planets" imaged around A stars: HR8799, Fomalhaut, b Pic A stars: HR8799 Fomalhaut b Pic GEMINI+KECK HST VLT 3 5 3.5 EK60 3 CT Cha B 1RXSJ1609 B DH Tau B AB Pic B 2.5 CHXR73 B U)) GQ Lup B GQ Lup B log (a(AU 2 1.5 1 1 SEEDS main target space SEEDS i t t 0.5 0 0 0 5 5 10 10 15 15 20 20 25 25 30 30 Mass (M_Jup) Subaru/CIAO in 2002 July
Subaru new coronagraph - HiCIAO Nasmyth platfo rm Nasmyth platfo rm War War m m Co Cold ld aph aph ast ast odule odule tr tr le le onagr onagr r r igh Cont igh Cont Module O Module e Modul Modul esc o pe e esc o pe ptic s Mo ptic s Mo a a o mmo n o mmo n Camer Camer ptic s + ptic s + Module Module Cor Cor C C ele ele Op Op Hi Hi M Co Co C AO AO O IR IR T T Hawaii 2 Hawaii 2- -R R G G 188 ac tuator 188 ac tuator s s Cor Cor onagr onagr aph aph Differ Differ ential optic s ential optic s k k 2k array 2k array 2k 2k array array F F o c al masks o c al masks (Wo llasto n prisms (Wo llasto n prisms ( ( i i AO AO ASIC Sidec ar ASIC Sidec ar Contr Contr oller oller Pupil sto ps Pupil sto ps - single / single / do uble ) do uble ) F F uture uture : Co mple me ntary Co mple me ntary F F ilter ilter s s M DM (32 32 ME ME M DM (32 32) ) Co mmo n+Diffe re ntial Co mmo n+Diffe re ntial Co mmo n+Diffe re ntial Co mmo n+Diffe re ntial Camera Wollaston Prism
HiCIAO Specifications IR Nasmyth （ w/ AO188 ） th （ / AO188 ） Focus F IR N Wavelength 0.85 – 2.50 microns Observation modes Observation modes DI PDI SDI ADI (w/ & w/o coronagraph) DI, PDI, SDI, ADI (w/ & w/o coronagraph) Resolution 0.03" (J), 0.04" (H), 0.055" (K) Strehl ratio Strehl ratio 0.2 (J), 0.3 (H), 0.5 (K) with AO 0.2 (J), 0.3 (H), 0.5 (K) with AO Field of view 20"x20" (DI), 20"x10" (PDI), 5"x5" (SDI) 10 3.8 at 0.1", 10 5.5 at 1.0" (SDI w/ Contrast 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) 1.625um 10" 5" 5 1.600um 5" 1.575um 1.644um
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