PA of $75 \pm
8^\circ$. Repeating the process, but using the best fit Gaussian for the 70$\mu$m image yields an inclination of $44 \pm 6^\circ$ and PA of $68 \pm 9^\circ$. Though the inclination of the disk is similar to the binary, the position angle is significantly different from the binary line of nodes of $41 \pm 2 ^\circ$. This difference means that the disk and binary orbital planes are misaligned.

As a check on the above approach, we can correct for the correlated noise directly. @2002PASP..114..144F show that for a map that has sufficiently many dithers (corresponding in our case to many timeline samples across each pixel), a noise “correction” factor of $r/\left(1-1/3r\right)$ can be derived, where $r$ is the ratio of natural to actual pixel scales and is 3.2 for our PACS maps. A correction factor of 3.6 for the measured pixel to pixel noise is therefore required when estimating the uncertainty on a fitted Gaussian. Including this factor at 70$\mu$m and calculating the uncertainty by the standard $\Delta \chi^2$ method yields an inclination of $42 \pm
7^\circ$ and a PA of $68 \pm 9^\circ$. At 100$\mu$m the result is an inclination of $44
\pm 6^\circ$ and a 