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G.T. van Belle (JPL)
Predicting the angular sizes of stellar sources is a tool of particular utility for astronomical interferometry in the optical and infrared. Methods for estimating angular sizes of main sequence and giant stars are presented, including: linear radius as a function of spectral type or V-K color, blackbody estimators, and mV=0 apparent angular size as a function of V-K color. The latter method is an empirically determined relationship that draws upon existing measurements of stellar angular diameters from both interferometry and lunar occultations. Deviations of more evolved objects such as Mira variables and carbon stars from that relationship are also presented. These angular sizes are incorporated in visibility normalizations, and the sources of uncertainty in visibility normalization for interferometric data are examined in detail. Acceptable levels of uncertainty are derived from rigorously determined errors associated with each method. These angular size determinations are equally valid for other applications as well, such as lunar occultations and speckle imaging.
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