Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 763, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/763/2/L32
Keywords
brown dwarfs; planets and satellites: detection; stars: massive
Categories
Funding
- MEXT, Japan
- U.S. National Science Foundation [1009203, 1008440, 1009314]
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1008440] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1009203, 0901967, 1009314] Funding Source: National Science Foundation
- Grants-in-Aid for Scientific Research [23103004, 23103002, 23103001, 21244022, 23340051, 22000005] Funding Source: KAKEN
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We present the direct imaging discovery of an extrasolar planet, or possible low-mass brown dwarf, at a projected separation of 55 +/- 2 AU (1 ''.058 +/- 0 ''.007) from the B9-type star kappa And. The planet was detected with Subaru/HiCIAO during the SEEDS survey and confirmed as a bound companion via common proper motion measurements. Observed near-infrared magnitudes of J = 16.3 +/- 0.3, H = 15.2 +/- 0.2, K-s = 14.6 +/- 0.4, and L' = 13.12 +/- 0.09 indicate a temperature of similar to 1700 K. The galactic kinematics of the host star are consistent with membership in the Columba Association, implying a corresponding age of 30(-10)(+20) Myr. The system's age, combined with the companion photometry, points to a model-dependent companion mass similar to 12.8 M-Jup. The host star's estimated mass of 2.4-2.5 M-circle dot places it among the most massive stars ever known to harbor an extrasolar planet or low-mass brown dwarf. While the mass of the companion is close to the deuterium burning limit, its mass ratio, orbital separation, and likely planet-like formation scenario imply that it may be best defined as a super-Jupiter with properties similar to other recently discovered companions to massive stars.
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