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Parallaxes of metal-poor main-sequence stars

Published online by Cambridge University Press:  26 February 2013

Brian Chaboyer ,
G. Feiden ,
G. F. Benedict ,
B. E. McArthur ,
T. E. Harrison ,
A. McWilliam ,
E. P. Nelan ,
R. J. Patterson  and
A. Sarajedini
Brian Chaboyer
Affiliation:
Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA email: [email protected]
G. Feiden
Affiliation:
Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA email: [email protected]
G. F. Benedict
Affiliation:
McDonald Observatory, University of Texas, Austin, TX 78712, USA
B. E. McArthur
Affiliation:
McDonald Observatory, University of Texas, Austin, TX 78712, USA
T. E. Harrison
Affiliation:
Department of Astronomy, New Mexico State University, Las Cruces, NM 88003, USA
A. McWilliam
Affiliation:
The Observatories of the Carnegie Institute of Washington, Pasadena, CA 91101, USA
E. P. Nelan
Affiliation:
Space Telescope Science Institute, Baltimore, MD 21218, USA
R. J. Patterson
Affiliation:
Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA
A. Sarajedini
Affiliation:
Department of Astronomy, University of Florida, Gainesville, FL 32611, USA
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Abstract

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Our team was awarded 108 orbits of Hubble Space Telescope time to obtain parallaxes and photometry of nine metal-poor stars with [Fe/H] < −1.5 dex. The parallaxes are obtained from observations with the Fine Guidance Sensor (FGS 1r; 11 orbits per star) and photometry was obtained with the Advanced Camera for Surveys (one orbit per star). The first data were obtained in October 2008, and the data collection is ongoing. It is anticipated that the observations will be complete in June 2013. Preliminary data reduction has been completed for five of our target stars. The parallax errors vary from 0.12 to 0.16 milli-arcseconds, and the parallaxes are at least an order of magnitude more accurate than existing Hipparcos parallaxes for these stars. The errors in the true distance modulus range from 0.02 to 0.03 mag. Ground-based high-resolution spectra have been analyzed to obtain accurate abundances for three stars. The properties of the two stars with accurate abundances and parallaxes are in excellent agreement with those predicted by stellar evolution models.

Keywords

stars: Population IIstars: distancesastrometryglobular clusters: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 87 - 90
Copyright
Copyright © International Astronomical Union 2013

References

Arellano Ferro, A., Figuera Jaimes, R., Giridhar, S., Bramich, D. M., Hernández Santisteban, J. V., & Kuppuswamy, K. 2011, MNRAS, 416, 2265CrossRefGoogle Scholar
Benedict, G. F., McArthur, B. E., Feast, M. W., et al. 2011, AJ, 142, 187CrossRefGoogle Scholar
Catelan, M., Pritzl, B. J., & Smith, H. A. 2004, ApJS, 154, 633CrossRefGoogle Scholar
Carretta, E., Gratton, R. G., Clementini, G., & Fusi Pecci, F. 2000, ApJ, 533, 215CrossRefGoogle Scholar
Clementini, G., Gratton, R., Bragaglia, A., Carretta, E., Di Fabrizio, L., & Maio, M. 2003, AJ, 125, 1309Google Scholar
Dotter, A., Chaboyer, B., Jevremović, D., Kostov, V., Baron, E., & Ferguson, J. W. 2008, ApJS, 178, 89Google Scholar
Feast, M. W., Laney, C. D., Kinman, T. D., van Leeuwen, F., & Whitelock, P. A. 2008, MNRAS, 386, 2115Google Scholar
Gratton, R. G., Bragaglia, A., Carretta, E., Clementini, G., Desidera, S., Grundahl, F., & Lucatello, S. 2003, A&A, 408, 529Google Scholar
Krauss, L. M. & Chaboyer, B. 2003, Science, 299, 65Google Scholar
Larson, D., Dunkley, J., Hinshaw, G., et al. 2011, ApJS, 192, 16CrossRefGoogle Scholar
Latham, D. W., Stefanik, R. P., Torres, G., Davis, R. J., Mazeh, T., Carney, B. W., Laird, J. B., & Morse, J. A. 2002, AJ, 124, 1144CrossRefGoogle Scholar
Poznanski, D., Prochaska, J. X., & Bloom, J. S. 2012, MNRAS, 426, 1465CrossRefGoogle Scholar
Sarajedini, A., Bedin, L. R., Chaboyer, B., et al. 2007, AJ, 133, 1658CrossRefGoogle Scholar