22$\mu$m and 51$\pm$10$\mu$Jy at 24$\mu$m for JD2.

The sharp increase in flux density between 16$\mu$m and 22$\mu$m can either be due to the entrance of polycyclic aromatic hydrocarbons into the 22 and 24[$\mu$m]{} bandpasses or the 9.7$\mu$m silicate absorption feature entering the 16$\mu$m bandpass. A third possibility is the decreasing contribution from hot dust surrounding an AGN because the dust is close to its sublimation temperature. We evaluate each of these possibilities in the following sections.

We note that the IRS is calibrated with respect to a constant $\nu$F$_{\nu}$ source spectrum. Color correction terms to the observed flux are smaller than 1% for the 16$\mu$m and 22$\mu$m data for the observed source spectrum and can be neglected. Furthermore, when we estimate fits to the observed photometry, we integrate template spectra over the filter bandpasses (Figure 2).

Derived Source Parameters
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The optical/near-infrared photometry of JD2 has been discussed in @Mobasher and @Dunlop. Spectral energy distribution fits to the photometry, which provide a photometric redshift solution, show a bimodal distribution of minimum $\chi^{2}$ values at $z\sim2.5$ and $z\sim6.5$. One set of $\chi^{2}$ values are favored over the other depending on the choice of optical photometry. @Mobasher, with their stringent $BViz$ limits, 