The multiplicity of planet host stars – new low-mass companions to planet host stars†

  1. M. Mugrauer1,*,
  2. A. Seifahrt1,2,
  3. R. Neuhäuser1

Article first published online: 19 JUN 2007

DOI: 10.1111/j.1365-2966.2007.11858.x

Issue

Monthly Notices of the Royal Astronomical Society

Monthly Notices of the Royal Astronomical Society

Volume 378, Issue 4, pages 1328–1334, July 2007

Additional Information

How to Cite

Mugrauer, M., Seifahrt, A. and Neuhäuser, R. (2007), The multiplicity of planet host stars – new low-mass companions to planet host stars. Monthly Notices of the Royal Astronomical Society, 378: 1328–1334. doi: 10.1111/j.1365-2966.2007.11858.x

Author Information

  1. 1

    Astrophysikalisches Institut, Universität Jena, Schillergäßchen 2-3, 07745 Jena, Germany

  2. 2

    European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany

* E-mail: markus@astro.uni-jena.de

  • †

    Based on observations obtained on La Silla in ESO programs 075.C-0098(A), 077.C-0572(A) and 078.C-0376(A), as well as on Paranal in ESO programs 070.C-0557(A), 076.C-0057(A) and 078.C-0376(B).

Publication History

  1. Issue published online: 19 JUN 2007
  2. Article first published online: 19 JUN 2007
  3. Accepted 2007 April 12. Received 2007 April 2; in original form 2007 March 8

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Keywords:

  • binaries: visual;
  • stars: individual: HD 16141;
  • stars: individual: HD 65216;
  • stars: individual: HD 101930;
  • stars: low-mass, brown dwarfs;
  • planetary systems

ABSTRACT

We present new results from our ongoing multiplicity study of exoplanet host stars, carried out with the infrared camera SofI (Son of ISAAC) at European Southern Observatory-New Technology Telescope (ESO-NTT). We have identified new low-mass companions to the planet host stars HD 101930 and HD 65216. HD 101930 AB is a wide binary system composed of the planet host star HD 101930 A and its companion HD 101930 B which is a M0 to M1 dwarf with a mass of about 0.7  M⊙ separated from the primary by ∼73 arcsec (2200 au projected separation). HD 65216 forms a hierarchical triple system, with a projected separation of 253 au (angular separation of about 7 arcsec) between the planet host star HD 65216 A and its close binary companion HD 65216 BC, whose two components are separated by only ∼0.17 arcsec (6 au of projected separation). Two Very Large Telescope-National Aeronautical Charting Office (VLT-NACO) images separated by 3 yr confirm that this system is comoving to the planet host star. The infrared photometry of HD 65216 B and C is consistent with a M7 to M8 (0.089  M⊙) and a L2 to L3 dwarf (0.078  M⊙), respectively, both close to the substellar limit. An infrared spectrum with VLT-Infrared Spectrometer and Array Camera (VLT-ISAAC) of the pair HD 65216 BC, even though not resolved spatially, confirms this late spectral type. Furthermore, we present H- and K-band ISAAC infrared spectra of HD 16141 B, the recently detected comoving companion of the planet host star HD 16141 A. The infrared spectroscopy as well as the apparent infrared photometry of HD 16141 B are both fully consistent with a M2 to M3 dwarf located at the distance of the planet host star.

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