Photometry of low-mass stars in Praesepe

Details Photometry of low-mass stars in Praesepe Photometry of low-mass stars in Praesepe

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982pasp...94..678s&link_type=abstract

Astronomical Society of the Pacific, Publications, vol. 94, Aug. 1982, p. 678-681.

Mathematics

Probability

17

Astrometry, Star Clusters, Stellar Spectrophotometry, Astronomical Catalogs, Stellar Color, Stellar Magnitude

Scientific paper

The results of a program of BVRI photometry of a set of relatively faint stars in the Praesepe cluster are reported. The program stars were selected to be high-probability members of the cluster based on a new proper-motion study by Jones and Cudworth (1982). Those membership identifications appear to have been quite accurate, since all but two of the stars observed have colors and magnitudes consistent with cluster membership. The new photometry, combined with previous data from Upgren, Weis, and DeLuca (1979) and Weis (1981) are used to show that the intrinsic width of the Praesepe main sequence remains quite narrow within 0.15 magnitude up to at least magnitude 10.5.

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