Variable Star Detection in Open Clusters

On September 17, 1996, I observed the open star cluster M 29 for a period of two hours. Thirty data points were collected in both the visual and red filters. Mira was used for all image calibrations and photometry. Nine bright standard stars were also observed so that extinction and transformation coefficients could be computed. These were then used to standardize the photometry for the cluster. Twenty-four stars were observed including the comparison star. Using the comparison star, I then produced differential light curves for the remaining 23 stars in both filters.
Greg Sherman