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Issue A&A
Volume 462, Number 2, February I 2007
Page(s) 777 - 780
Section Planets and planetary systems
DOI 10.1051/0004-6361:20066581



A&A 462, 777-780 (2007)
DOI: 10.1051/0004-6361:20066581

Direct detection of exoplanet host star companion $\gamma$ Cep B and revised masses for both stars and the sub-stellar object

R. Neuhäuser1, M. Mugrauer1, M. Fukagawa2, 3, G. Torres4, and T. Schmidt1

1  Astrophysikalisches Institut, Universität Jena, Schillergässchen 2-3, 07745 Jena, Germany
    e-mail: rne@astro.uni-jena.de
2  Spitzer Science Center, California Institute of Technology, Pasadena, CA 91125, USA
3  Division of Particle and Astrophysical Sciences, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602, Japan
4  Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

(Received 17 October 2006 / Accepted 24 October 2006 )

Abstract
Context.The star $\gamma$ Cep is known as a single-lined spectroscopic triple system at a distance of 13.8 pc, composed of a K1 III-IV primary star with V = 3.2 mag, a stellar-mass companion in a 66-67 year orbit (Torres 2007, ApJ, 654, 1095), and a substellar companion with $M_{\rm p} \sin i = 1.7$  $M_{\rm Jup}$ that is most likely a planet (Hatzes et al. 2003, ApJ, 599, 1383).
Aims.We aim to obtain a first direct detection of the stellar companion, to determine its current orbital position (for comparison with the spectroscopic and astrometric data), its infrared magnitude and, hence, mass.
Methods.We use the Adaptive Optics camera CIAO at the Japanese 8 m telescope Subaru on Mauna Kea, Hawaii, with the semi-transparent coronograph to block most of the light from the bright primary $\gamma$ Cep A, and to detect at the same time the faint companion B. In addition, we also used the IR camera $\Omega$ Cass at the Calar Alto 3.5 m telescope, Spain, to image $\gamma$ Cep A and B by adding up many very short integrations (without AO).
Results.$\gamma$ Cep B is clearly detected on our CIAO and $\Omega$ Cass images. We use a photometric standard star to determine the magnitude of B after PSF subtraction in the Subaru image, and the magnitude difference between A and B in the Calar Alto images, and find an average value of $K = 7.3 \pm 0.2$ mag. The separations and position angles between A and B are measured on 15 July 2006 and 11 and 12 Sept. 2006, B is slightly south of west of A.
Conclusions.By combining the radial velocity, astrometric, and imaging data, we have refined the binary orbit and determined the dynamical masses of the two stars in the $\gamma$ Cep system, namely $1.40 \pm 0.12$ $M_{\odot}$ for the primary and $0.409 \pm 0.018$ $M_{\odot}$ for the secondary (consistent with being a M4 dwarf). We also determine the minimum mass of the sub-stellar companion to be $M_{\rm p} \sin i = 1.60 \pm 0.13$  $M_{\rm Jup}$.


Key words: instrumentation: adapive optics -- binaries: spectroscopic -- binaries: visual -- planetary systems -- star: individual: $\gamma$ Cep



© ESO 2007


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