Subaru Strategic E xploration of E xoplanets and Disks with HiCIAO/ AO188 DS= 種 ) ( ( SE E HiCIAO at Nasmyth 2008.11.28 Tamura & Mayama on behalf of the SE E DS team (list shown later) AO188 Today ’ s Outlines � 1.Introduction � ---How infrared observations(Subaru) collaborate with radio observations(ALMA) � 2.Previous Star & Planet formation researches by Subaru Telescope � 3.SEEDS projects (instruments, sciences, target summaries) � 4.Summary (Subaru � ALMA) 1
ALMA strategy Infrared � Radio � Infrared (Subaru)～0 ” .1 scattering light from star and disk. � -detailed morphology(disk size,inclination, color, etc.) -Provide original targets to ALMA-Japan team. Infrared observations: precursor to ALMA � Radio (ALMA)～0 ” .01 (after 2011) � -disk mass, velocity distribution etc. 1. Clouds collapse under gravity E volution diagram - from clouds to planets Currently best studied with NIR 2. Protoplanetary disks Then ALMA from ~ 2011 10,000 yr 3. Comets & Kaguya IRSF/SIRIUS asteroids form 1 Myr Subaru/CIAO 4. Planetary system 10 Myr Subaru/CIAO/POL 100 Myr 0. Cloud and cloud cores 2
Subaru has an AO Coronagraph since 2001 � CI AO + 36-actuator AO at Cass. � First dedicated cold coronagraph on 8-m telescopes Compact disk around Diversity of proto- Young very low-mass massive YSOs Planetary disks Companion Fukagawa+04,+06; Tamura+06; Kudo+07; Itoh+05; Jiang+06; + Spiral-shape Disk around 2Mo-4Myr Herbig Ae star: AB Aur Fukagawa, Hayashi, Tamura et al. (2004) 13CO fainter 100 AU Velocity field Mannings (1997) n e a r - brighter s i d e 1.6 μm flared disk (d= 144 pc) 400 AU � disk with spiral arms (r= 450 AU) � trailing arm ← com. w/radio data 1000 AU + brighter forward scattering � no nearby companions Grady et al. (1999) 3
Disk Really Spiral ? - Disk Really Spiral ? - YE YE S S Gravitational instability? (instability condition) ： Ω c = G s ≤ Q 1 π Σ Probably supplies of matter from the envelope maintain the weak instability. ⇒ Q ~ 2; “weak” instability I n fact, planets imaged A suggestion of planet White contours: contours: White around A stars (HR8799, formation by gravitational M disk 345 GHz dust continuum (SMA) 345 GHz dust continuum (SMA) Fomalhaut) at r> 25AU !! instability? (for some systems) ~0.15M � Lin et al. 200 et al. 2006, ApJ 6, ApJ Lin Marois et al./ Kalas et al. 08 Matsuo et al. 2007, ApJ Disk directly imaged even around only 0.1 Solar-Mass T Tauri Star: FN Tau H -band (1.6 μ m) image FOV = 11” x 11” mask size = 0.8” Resolution: 0.14’’ ( H =21.5@5 σ ) r=260AU face-on disk detected! - almost face-on - lowest mass star whose disk has been directly imaged. Kudo, Tamura et al. (2004) Did not expect such a bright disk around low-mass stars. Surface brightness profile: ｒ - 2.5 → Flare-disk with efficient forward scattering. 4
Subaru has an AO Coronagraph since 2001 � CI AO + 36-actuator AO at Cass. � First dedicated cold coronagraph on 8-m telescopes Compact disk around Diversity of proto- Young very low-mass massive YSOs Planetary disks Companion But after 6 years' use, we could now improve; - low order adaptive optics (AO36-> AO188+ Subaru), - lack of differential capabilities (CIAO-> HiCIAO), - limited upgrade flexibilities accepting various coronagraph ideas and AO upgrades. Fukagawa+04,+06; Tamura+06; Kudo+07; Itoh+05; Jiang+06; + HiCIAOConcept Nasmyth platfo rm Nasmyth platfo rm War War m m Cold Co ld aph aph ast ast Optic s Module Optic s Module High Contr High Contr Module Module onagr onagr Module AO Module elesc o pe elesc o pe a a Co mmo n Co mmo n Camer Camer + Optic s + Module Module Optic s Cor Cor AO IR IR T T 188 188 ac tuator ac tuator s s Cor Cor onagr onagr aph aph Differential Differential optic s optic s Hawaii 2 Hawaii 2- - R R G G k × × 2 F F o c al masks o c al masks (Wo llasto n pr (Wo llasto n pr isms) isms) 2 2k 2k k array array AO AO Pupil sto ps Pupil sto ps ASICS Sidec ar Sidec ar Contr Contr oller F F uture : uture : ASICS oller Co mple me ntary Co mple me ntary M DM (32 × × 32 ME ME M DM (32 32) ) F F ilter ilter s s Co mmo n+Diffe re ntial Co mmo n+Diffe re ntial Camera Wollaston Prism 5
What is the SE E DS project?: First Subaru Strategic Observations � The goals of the SEEDS survey are to address the following key issues in exoplanet/ disk science: ① The detection and census of exoplanets in the outer circumstellar regions around solar-mass stars. ② The evolution of protoplanetary and debris disks. ③ The direct link between exoplanets and circumstellar disks at a few AU to 10s AU regions for the first time. Observations to be started in Early 2009. Proposed Observations in SE E DS Luminosity vs Age � To conduct a Subaru- brighter and less-contrast when young HiCI AO-AO188 imaging survey in 5 years, stars searching for giant brown planets (~ 1-13 MJ) and dwarfs protoplanetary/ debris planets disks around ~ 500 SEEDS age span nearby solar-type young stars. 1M 10M 100M 1G 10Gyr Direct imaging is � SEEDS indispensable for the contrast detection of such "young", self-luminous planets, especially planets in outer circumstellar regions (~ a few AU-~ 20AU). Note: Based on Burrow's model, but still fine with Marley's model. 6
Disk Study---Our Goals 1.To reveal the morphology of the protoplanetary disks at 15-50 AU regions. Disk structures that could be formed by planets or rather that lead to planet formation (gap, hole, warp, resonance) 2.To make a direct connection with giant planet formation where they can in fact form (not after migration) 3.To provide evidence for protoplanets as local low-polarized regions. Main Targets of Disks ～Transitional Objects Defined as the object with no or weak IR excess shortward of 10 μm and a significant excess at longer wavelengths A possible signature of planets at least in the very inner region (<a few AU)) 7
SE E DS Target Summary: Original Planet searches Disk Searches (in methane SDI / ADI mode) (in PDI mode) Total Category (a) (b) (c) (d) (e) number Protoplanetary SFR YSOs Open cluster Nearby stars Debris disks disks Number 120 116 100 105 80 521 Distance ~ 140 pc 25-180 pc < 30 pc ~ 140 pc < 130 pc 100 Myr 5 Myr Age 1-10 Myr ~ 100 Myr 1-10 Myr - 1 Gyr - 6 Gyr TTS/HAeBE/ U Ma/Hyades/ SST/AKARI Comment Tau/Sco subcategory polarized Pleiades/ α Per sample sources RA-DEC H-mag R-mag Sp-Type SUMMARY � We will conduct a 5-year legacy survey of ~ 500 solar-mass young stars for direct imaging of exoplanets and disks in 120 nights with a "all-Japan" team collaborating with several distinctive foreign researchers (including Princeton, Taiwan, MPI , 2xUH, Goddard, Washington). � Our targets consist of 5 categories, each of which includes about ~ 100 stars (enough for statistics). � We believe that we can image at least a handful of giant (< 13 MJ) exoplanets in a few to 10s AU regions and the similar radial regions of many disks in each category. � Our planet/ disk survey is not only the most extensive one so far but also about 3 years earlier than the other next generation surveys on 8-m class telescopes. Note GPI / SPHERE are both in the southern hemisphere. � Various follow-up programs should be organized, including spectroscopy with various instruments and telescopes. � The observations will start from early 2009. � Provide our original targets from SEEDS to ALMA team. Propose to observe with gas and dust at once under an early science category. 8
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