Best-fit spectral-energy distribution for J1610 created by generating synthetic photometry (green) from our observed spectra (black) and model atmosphere (grey) and locking it to the literature photometry (red). Vertical error bars on the observed photometry correspond to uncertainties (include an estimate of the stellar variability) and horizontal errors represent the width of the filter profile. Bottom panel: residual photometry in units of standard deviations. We de-redden the calibrated spectrum before computing the bolometric flux, but the spectrum and photometry shown here are still reddened.