Monday, June 3, 2013

1305.7264 (Timothy D. Brandt et al.)

The Moving Group Targets of the SEEDS High-Contrast Imaging Survey of Exoplanets and Disks: Results and Observations from the First Three Years    [PDF]

Timothy D. Brandt, Masayuki Kuzuhara, Michael W. McElwain, Joshua E. Schlieder, John P. Wisniewski, Edwin L. Turner, J. Carson, T. Matsuo, B. Biller, M. Bonnefoy, C. Dressing, M. Janson, G. R. Knapp, A. Moro-Martín, C. Thalmann, T. Kudo, N. Kusakabe, J. Hashimoto, L. Abe, W. Brandner, T. Currie, S. Egner, M. Feldt, T. Golota, M. Goto, C. A. Grady, O. Guyon, Y. Hayano, M. Hayashi, S. Hayashi, T. Henning, K. W. Hodapp, M. Ishii, M. Iye, R. Kandori, J. Kwon, K. Mede, S. Miyama, J. -I. Morino, T. Nishimura, T. -S. Pyo, E. Serabyn, T. Suenaga, H. Suto, R. Suzuki, M. Takami, Y. Takahashi, N. Takato, H. Terada, D. Tomono, M. Watanabe, T. Yamada, H. Takami, T. Usuda, M. Tamura
We present results from the first three years of observations of moving group targets in the SEEDS high-contrast imaging survey of exoplanets and disks using the Subaru telescope. We achieve typical contrasts of ~10^5 at 1'' and ~10^6 beyond 2'' around 63 proposed members of nearby kinematic moving groups. We review each of the kinematic associations to which our targets belong, concluding that six, \beta Pictoris (~12 Myr), AB Doradus (~100 Myr), Columba (~30 Myr), Tucana-Horogium (~30 Myr), TW Hydrae (~10 Myr), and Ursa Majoris (~500 Myr), are sufficiently well-defined to constrain the ages of individual targets. Somewhat less than half of our targets are high-probability members of one of these moving groups. For all of our targets, we combine proposed moving group membership with other age indicators where available, including Ca II HK emission, X-ray activity, and rotation period, to produce a posterior probability distribution of age. SEEDS observations discovered a substellar companion to one of our targets, \kappa And, a late B star. We do not detect any other substellar companions, but do find seven new close binary systems, of which one still needs to be confirmed. A detailed analysis of the statistics of this sample, and of the companion mass constraints given our age probability distributions and exoplanet cooling models, will be presented in a forthcoming paper.
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