be subject to both short term perturbations and possible close encounters. If the mutual inclination were high enough, it would also be subject to Kozai cycles due to the secondary that could result in a high eccentricity and further affect the orbital stability.

While it may be worthy of further detection attempts, the existence of this component appears doubtful and we do not consider it further.

IR and Sub-mm Data {#s:data}
==================

Observations {#s:obs}
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![image](pacs70.eps){width="33.00000%"} ![image](pacs100.eps){width="33.00000%"} ![image](pacsall160.eps){width="33.00000%"}

*Herschel* Photodetector and Array Camera & Spectrometer data at 100 and 160$\mu$m were taken in April 2010 during routine DEBRIS observations. Subsequently, a Spectral & Photometric Imaging Receiver observation was triggered by the large PACS excess indicating the presence of a debris disk and a likely sub-mm detection. The disk was detected, but not resolved with SPIRE at 250 and 350$\mu$m. A 70$\mu$m PACS image was later obtained to better resolve the disk. Because every PACS observation includes the 160$\mu$m band, we have two images at this wavelength, which are combined to produce a single higher S/N image. All observations were taken in the standard scan-map modes for our survey; mini scan-maps for PACS data and small maps for SPIRE. Data were 