DIRECT IMAGING DISCOVERY OF A "SUPER-JUPITER" AROUND THE LATE B-TYPE STAR κ And*

J. Carson, C. Thalmann, M. Janson, T. Kozakis, M. Bonnefoy, B. Biller, J. Schlieder, T. Currie, M. Mcelwain, M. Goto, T. Henning, W. Brandner, M. Feldt, R. Kandori, M. Kuzuhara, L. Stevens, P. Wong, K. Gainey, M. Fukagawa, Y. KuwadaT. Brandt, J. Kwon, L. Abe, S. Egner, C. Grady, O. Guyon, J. Hashimoto, Y. Hayano, M. Hayashi, S. Hayashi, K. Hodapp, M. Ishii, M. Iye, G. Knapp, T. Kudo, N. Kusakabe, T. Matsuo, S. Miyama, J. Morino, A. Moro-martin, T. Nishimura, T. Pyo, E. Serabyn, H. Suto, R. Suzuki, M. Takami, N. Takato, H. Terada, D. Tomono, E. Turner, M. Watanabe, J. Wisniewski, T. Yamada, H. Takami, T. Usuda, M. Tamura

Research output: Contribution to journalArticlepeer-review

Abstract

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 κ 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 ~1700 K. The galactic kinematics of the host star are consistent with membership in the Columba Association, implying a corresponding age of 30+20 –10 Myr. The system's age, combined with the companion photometry, points to a model-dependent companion mass ~12.8 M Jup. The host star's estimated mass of 2.4-2.5 M ☉ 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.
Original languageEnglish
Article numberL32
JournalAstrophysical Journal Letters
Volume763
Issue number2
DOIs
Publication statusPublished - 1 Feb 2013

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