of the spectral energy distribution (SED). The model is separated into two components; a stellar atmosphere and a disk. Due to being fairly bright ($V\sim5$mag) the system is saturated in the 2MASS catalogue. However, sufficient optical photometry for each individual star and the pair exists [@1993AJ....106..773H; @1997yCat.2215....0H; @1997ESASP1200.....P; @2006yCat.2168....0M], as well as infra-red measurements of the AB pair from AKARI and IRAS . These data were used to find the best fitting stellar models via $\chi^2$ minimisation. This method uses synthetic photometry over known bandpasses and has been validated against high S/N MIPS 24$\mu$m data for DEBRIS targets, showing that the photospheric fluxes are accurate to a few percent for AFG-type stars. The stellar luminosities ($L_{\star,A}=1.96L_\odot$, $L_{\star,B}=0.14L_\odot$) and IR fluxes of the individual components are consistent with the fit for the pair ($L_{\star,AB}=2.08L_\odot$). The fit for the AB pair is shown in Figure \[fig:sed\].

The spatial structure of the disk can be modelled with dust at a single radial distance of 120AU (i.e. thin compared to *Herschel’s* resolution, §\[s:spatial\]), so disk SED modelling can be decoupled from the resolved modelling once this radial distance is known. Because we have measurements of the disk emission at only five wavelengths, we cannot 