VaST is not tied up to any external catalog and WCS (if operated in its main
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Unlike software based on the image subtraction method, VaST can be used inĬase of unstable PSF (e.g., bad guiding or with digitized wide-field photographic images). With known magnitudes in the field of view, all magnitudes can be later If data permit, period-search techniques may be employed to identify periodic variable stars among the candidates.Īll lightcurves are constructed in arbitrary magnitudes with zero magnitudeĬorresponding to the background level on the reference image. L variability index, Robust Median Statistic (RoMS)Īnd other plots may be used to visually identify variable star candidates. On each image, cross-matches lists of detected stars, performs magnitudeĬalibration with respect to the first (reference) image and constructs a lightcurve for each object.
VaST performs object detection and aperture photometry using The images in a series should overlap by at least ~40% to ensure successful cross-identification. The input images may be shifted and rotated with respect to each other, but they have to have the same Same instrument using the same filter and saved in the FITS format.ĬCD images should be calibrated (dark-subtracted and flat-fielded). The images (CCD frames or digitized photographic plates) must be taken with the VaST is a software tool for finding variable objects on a series of astronomical images.
Contents What is VaST? Screenshots Download Usage Output files VaST mailing list News/Release notes Frequently Asked Questions Publications using VaST Other useful tools VaST A software for variable star detectionįor a detailed description of the code.
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