@@ -1,1 +1,1 @@ - +Similarly, in addition to the noise-dependent Gaussian fitting uncertainties on the fluxes (Condon 1997), the uncertainty in the measured flux densities all consists of a noise-independent component. Errors in the phase calibration introduce uncertainties in the source positions. These are added quadratically to the Gaussian-fit position uncertainties in the catalogue. FLOATSUPERSCRIPT. We select and present further stars that may be Boötes III members based on their combined proper motion and position in the color magnitude diagram, but we caution against assigning membership to stars that are not confirmed spectroscopically, as we demonstrate that there are contaminating stars from the disrupting globular cluster NGC 5466 in the vicinity of the main body of Boötes III. Of the 194 stars from the Carlin et al. I mean even the name Torin Plush makes you think it’s a little heavier. 2.0± 2.0 kpc distance range about the mean of 46.5 kpc. 46.5 ± 2.0 kpc. 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