Targets for PlanetDisk Studies YSOs t110 Myr samples

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Targets for Planet/Disk Studies? YSOs (t1-10
Myr samples) ?

• Hiro Takami1, Tomoyuki Kudo2,3, Yoshiko Okamoto3,
  Motohide Tamura2, HiCIAO Science Team

1) ASIAA 2) GUAS 3) NAOJ 4) Ibaraki Univ.
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Searches for Exoplanets toward YSOs
10-40 MJ
40 MJ
DH Tau (Itoh et al. 2006)
GQ Lup (Neuhauser et al. 2005)
100 AU

• Extensive observations will allow for
  understanding
• What are the population and separation of
  extremely low-mass stellar companions
• How their formation is related to BDs/sub-BDs
  (hopefully)

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Searches for Exoplanets toward YSOs

• Why do we need YSO samples?
• This will allow for
• Exploring the lowest mass limit

(Open Clusters)
(YSO/SFR)
Credit Taro Matsuo
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Searches for Exoplanets toward YSOs

• Why do we need YSO samples?
• This will allow for
• Exploring the lowest mass limit
• Investigating the relationship
• with-
• Disk structures
• Population (and binarity) of
• BDs/sub-BDs
• in the same SFR

10 100 1000 MJup
Luhman et al. (2007)
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Searches for Exoplanets toward YSOs

• Previous Large Coronagraphic Surveys
• Subaru Disks and Planets Survey (SDPS)
• Subaru CIAOAO36, 60-80 targets
• HST NICMOS survey(?)
• 26 optically-thick disk candidates

A HiCIAO survey will definitely provide
significantly better detection limit!
(Credit Taro Matsuo)
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Searches for Exoplanets toward YSOs

• Criteria for Target Selection
• D lt 200 pc, t lt 10 Myr
• Dec. gt -40 deg. (El. gt 30 deg.), R lt 15 mag.
• Number of Targets 100
• 50 from a T association, 50 from an OB
  association

Taurus (140 pc)
Oph/Sco (140-150 pc)
TW Hya (60 pc)
Corona Australis (130 pc)
Lupus (190 pc)
Chamaeleon (170 pc)
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Searches for Exoplanets toward YSOs

• Taurus (d140 pc)
• One of the best studied T-associations
• Dec20-30 deg. ? the best performance is expected
  for AO correction (i.e., the elevation reaches up
  to 80-90 deg.)
• Upper Scorpius (d150 pc)
• A sub-cluster in one of the nearest OB
  associations
• Only the central region is selected to adjust the
  number of targets
• Spectral Types of Targets
• A/F/G/K (i.e., M0.5-2 Msolar)

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Searches for Exoplanets toward YSOs
Spectral Types
Taurus
Upper Sco
Mother Sample
Selected
R Magnitudes
Upper Sco
Taurus
Rejected due to the performance of AO
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Studies of Protoplanetary Disks
FN Tau
HD 142527
AB Aur
(Fukagawa et al. 2006)
(Kudo et al. 2008)
(Fukagawa et al. 2004)
HD 141569A
HD 100546
(Grady et al. 2001)
(Clampin et al. 2003)
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Studies of Protoplanetary Disks
FN Tau
HD 142527
AB Aur
(Fukagawa et al. 2006)
(Kudo et al. 2008)
(Fukagawa et al. 2004)
Simulated by Indiana Univ.
(Augereau et al. 2004)
http//www.newscientist.com/
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Studies of Protoplanetary Disks

• Key Questions
• How do these disks evolve?
• What determine the observed structures?
• Are these structures related to the formation of
  extremely low-mass companions?
• Are these structures related to the evolution of
  the inner disk region?

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Studies of Protoplanetary Disks

• Key Questions
• How do these disks evolve?
• What determine the observed structures?
• Are these structures related to the formation of
  extremely low-mass companions?
• Are these structures related to the evolution of
  the inner disk region?

S
IR CO emission (Najita et al. 2003)
SED (Calvet et al. 2002)

• Notes on Observations to Date
• Despite interesting results, most disks appear to
  remain undetectable in the scattered light
• It is not clear if the detactability is
  correlated with the other disk signatures like mm
  CO/dust emission, Ha

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Studies of Protoplanetary Disks
Major Survey
(1) 40 CTTSs in the Taurus-Auriga Region

• Best declination (20-30 deg.) for AO correction
• One of the nearest best-studied star-forming
  regions
• High Resolution (7AU in H-band)
• Easily performed comparisons with
  other data (Spitzer etc.)
• Almost unbiased!
• all B/A/F/K YSOs with EWHagt10 Å (and Rlt15
  mag.)

(2) 20 Previously-Detected Disks in Taurus

• High signal-to-noise is guaranteed
• Observed for detailed studies
  (e.g., J/H/K-bands)

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Studies of Protoplanetary Disks
Major Survey (continued)
(3) 20 Polarized Targets

• Based on previous NIR surveys (e.g., SIRIUS)

(4) Additional 30 Nearby HAeBe Stars (B5-A9,
lt200 pc)

• Extending the understanding to intermediate-mass
  YSOs, and relationship with debris disks

Back-up or Demonstration
(5) 10 YSOs with early B types (B0-B5)

• Distant (up to 500 pc), but likely to host large
  disks (up to 1000 AU)

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Studies of Protoplanetary Disks

• Other Note
• Observations will be made using PDI Mode,
  thereby-
• Allowing for studying dust properties
• Minimizing false detection due to imperfect AO PSF

b Pic (Tamura et al. 2006)