AAS 199th meeting, Washington, DC, January 2002
Session 129. Astrometric Surveys
Display, Thursday, January 10, 2002, 9:20am-4:00pm, Exhibit Hall

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[129.06] The RECONS Effort to Characterize the Highest Proper Motion Stars

W.C. Jao, J.P. Subasavage, T.J. Henry (Georgia State University), C. Williams (Johns Hopkins University), E. Costa (Universidad de Chile), P.A. Ianna (University of Virginia), R.A. Mendez (European Southern Observatory), RECONS Team

High proper motion is a method used for selecting probable nearby stars. There currently are 601 stars (502 systems) with proper motion faster than 1 arcsec/year (hereafter, the MOTION stars). There are 271 systems known in the northern sky and 231 systems in the southern sky. The predominance of systems in the north is because historically more proper motion surveys have been carried out in northern hemisphere. In the complete MOTION sample, 75 estimated to lie within 25 pc of the Sun, the adopted horizon for NASA's NStars (Nearby Stars) Project.

Based on available photometric and parallax observations, we know that MOTION members are primarily late type main sequence stars, with a few white dwarfs and subdwarfs. Nonetheless, it is remarkable that 16 not yet have parallax measurements. In addition, nearly 40 of the systems do not have complete VRI photometry on a standard system. In an effort to understand the complete MOTION sample, and to discover new members of the solar neighborhood, we present both astrometric and photometric results for the MOTION stars from our extensive NOAO Surveys Program known as CTIOPI (CTIO Parallax Investigation).

The support of NOAO, CTIO, the NASA-Ames Astrobiology Institute and the NASA's Space Interferometry Mission have been the crucial to the success of this research.

If you would like more information about this abstract, please follow the link to http://www.chara.gsu.edu/RECONS. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.

The author(s) of this abstract have provided an email address for comments about the abstract: jao@chara.gsu.edu

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