ARGOS is the observing program started by Edward Nather and Don Winget. Their aim was to use the prime focus of the 82” for high-accuracy time series photometry of white dwarf stars, able to complete compete with the throughput of a typical 4 m telescope’s optical path through multiple mirrors. The ARGOS program continues to be successful, using Princeton Instrument’s ProEM camera.
ProEM is a 1024x1024 frame transfer camera with 13 micron pixels and optional electron multiplication readout, although we have never used that feature except on the commissioning run to observe the Crab pulsar. The camera is triggered by a GPS-disciplined double-oven quartz oven clockclock. The setup used most often is 4x4 binning for an effective pixel size of about 1/3 arcsecond. At the Cassegrain focus - currently the only available configuration - the plate scale of 7.2 arcsec/mm yields an image about 1.5 arcminutes on a side. Data are acquiring using Princeton Instrument’s Lightfield, and a separate program provides realtime aperture photometry analysis of the divided light curve and its Fourier transform.
Two filter sets are available. A manually-controlled wheel contains the Johnson-Bessel filters UBVRI, and an automated FLI wheel contains the standard Sloan filters and BG40. Most observers using UBVRI substitute a clear near-red blocking filter for U. When using the FLI wheel, this filter is removed.
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