is the same in both 160$\mu$m images, so could be real. The fact that the peak extends over several pixels is not evidence that it is real, because the pixels in these maps are correlated (see below). If real, this component of the disk or background object cannot be very bright at SPIRE wavelengths because the measured fluxes appear consistent with a blackbody fit to the disk (see §\[s:sed\]). Based on an analysis of all DEBRIS maps (that have a constant depth), the chance of a 3$\sigma$ or brighter background source appearing within 10” of 99 Her at 160$\mu$m is about 5% (Thureau et al in prep). Given that the 160$\mu$m offset is only a 2-3$\sigma$ effect (i.e. could be a 2-3$\sigma$ background source superimposed on a smooth disk), the probability is actually higher because the number of background sources increases strongly with depth. These objects have typical temperatures of 20–40K , so could easily appear in only the 160$\mu$m image, particularly if the disk flux is decreasing at this wavelength.

  Band         Flux (mJy)   Uncertainty Method
  ---------- ------------ ------------- --------------
  PACS70               93            10 15” aperture
  PACS100              87            10 15” aperture
  PACS160              80            15 17” aperture
  SPIRE250             44             6 PSF fit
  