A Multiwavelength Radial Velocity Search for Planets around the Brown Dwarf LP 944-20 | Zendy

E. L. Martı́n | Zendy; E. W. Guenther | Zendy; M. R. Zapatero Osorio | Zendy; H. Bouy | Zendy; R. J. Wainscoat | Zendy

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A Multiwavelength Radial Velocity Search for Planets around the Brown Dwarf LP 944-20

Author(s) -

E. L. Martı́n,

E. W. Guenther,

M. R. Zapatero Osorio,

H. Bouy,

R. J. Wainscoat

Publication year - 2006

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/505343

Subject(s) - brown dwarf , radial velocity , physics , planet , astrophysics , astronomy , circumbinary planet , amplitude , dwarf planet , dispersion (optics) , infrared , stars , wavelength , optics

The nearby brown dwarf LP 944-20 has been monitored for radial velocityvariability at optical and near-infrared wavelengths using the VLT/UVES and theKeck/NIRSPEC spectrographs, respectively. The UVES radial velocity dataobtained over 14 nights spanning a baseline of 841 days shows significantvariability with an amplitude of 3.5 km s$^{-1}$. The periodogram analysis ofthe UVES data indicates a possible period between 2.5 hours and 3.7 hours,which is likely due to the rotation of the brown dwarf. However, the NIRSPECdata obtained over 6 nights shows an rms dispersion of only 0.36 km s$^{-1}$and do not follow the periodic trend. These results indicate that thevariability seen with UVES is likely to be due to rotationally modulatedinhomogeneous surface features. We suggest that future planet searches aroundvery low-mass stars and brown dwarfs using radial velocities will be betterconducted in the near-infrared than in the optical.Comment: accepted by ApJ Letter

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