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Title:
Differential Radial Velocities and Stellar Parameters of Nearby Young Stars
Authors:
Paulson, Diane B.; Yelda, Sylvana
Affiliation:
AA(NASA Goddard Space Flight Center, Code 693.0, Greenbelt, MD 20771; ), AB(Department of Astronomy, University of Michigan, 830 Dennison Building, Ann Arbor, MI 48109; )
Publication:
The Publications of the Astronomical Society of the Pacific, Volume 118, Issue 843, pp. 706-715. (PASP Homepage)
Publication Date:
05/2006
Origin:
UCP
PASP Keywords:
Stars: Planetary Systems, Techniques: Radial Velocities, Stars: Activity, stars: individual (IC 2391), stars: individual (β Pictoris), Stars: Individual: Name: Castor, stars: individual (Ursa Major), Stars: Abundances
DOI:
10.1086/504115
Bibliographic Code:
2006PASP..118..706P

Abstract

Radial velocity searches for substellar-mass companions have focused primarily on stars older than 1 Gyr. Increased levels of stellar activity in young stars hinders the detection of solar system analogs, and therefore until recently there has been a prejudice against inclusion of young stars in radial velocity surveys. Adaptive optics surveys of young stars have given us insight into the multiplicity of young stars, but only for massive, distant companions. Understanding the limit of the radial velocity technique, restricted to high-mass, close-orbiting planets and brown dwarfs, we began a survey of young stars of various ages. While the number of stars needed to carry out full analysis of the problems of planetary and brown dwarf population and evolution is large, the beginning of such a sample is included here. We report on 61 young stars ranging in age from the β Pictoris association (~12 Myr) to the Ursa Major association (~300 Myr). This initial search resulted in no stars showing evidence of companions larger than ~1MJup-2MJup in short-period orbits at the 3 σ level. We also present derived stellar parameters, as most have unpublished values. The chemical homogeneity of a cluster, and presumably of an association, may help to constrain true membership, so we present [Fe/H] abundances for the stars in our sample.
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