Deriving the true mass of a Brown Dwarf companion by AO aided astrometry

Details Deriving the true mass of a Brown Dwarf companion by AO aided astrometry Deriving the true mass of a Brown Dwarf companion by AO aided astrometry

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..549m&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Physics

Optics

Low Luminosity Stars, Subdwarfs, And Brown Dwarfs, Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers, Celestial Mechanics

Scientific paper

The true masses of non-transiting substellar companions to stars are only known for a few objects so far and they have all been determined by astrometry with the HST fine guidence sensor [1, 2]. From radial velocity detections alone one does not get all orbital parameters needed to derive the true mass of a substellar companion to a star. Additional astrometric measurements are needed to calculate the inclination i and the longitude of the ascending node Ω. The parallax and proper motion of the star must also be considered. We aim to derive the true mass of a brown dwarf candidate companion to an early M dwarf with groundbased astrometry aided by adaptive optics. We found this unique brown dwarf desert object in our UVES precision radial velocity survey of M dwarfs, inferring a minimum companion mass of 27 Jupiter masses [3]. Combining the data with HIPPARCOS astrometry, we found a probability of only 2.9% that the companion is stellar. We are therefore observing the host star and a reference field within a monitoring program with NACO at the VLT to derive the true mass of the companion and establish its nature (BD vs. star).

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