presented in Table \[info\], but because the integration time (and thus the noise) varies smoothly in these maps, the values given in Table \[info\] represent the best estimate of the noise over the full map. Finally, we used the derived RMS of each map to create contour maps overlaid on greyscale images for each core, and we present these in Figures \[f1\]-\[f9\] for the cores observed at 350 [$\mu$m]{} and in Figure \[f450\] for those observed at 450 [$\mu$m]{}. Contours start at $2\sigma$ and increase by $2\sigma$ unless otherwise indicated. We arrange the images in alphabetical order rather than by Right Ascension to make a specific map easier to find.

Calibration {#cal}
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To measure the flux densities of the sources in a given aperture in units of Jy (as opposed to the instrument units of nV), we have calculated Flux Conversion Factors (FCF) for each aperture. A brief description of the calibration method, explained in greater detail in Shirley et al. (2000), is as follows. The FCF for an aperture of diameter $\theta$, C$_{\theta}$, is defined to be the total flux density of a calibrator source (a source with a known flux density at the wavelength of the observations) 