  Half of the JWST high-contrast imaging objects will only have photometric
data {{as of Cycle 2}}. However, to better understand their atmospheric
chemistry which informs formation origin, spectroscopic data are preferred.
Using HIP 65426 b, we investigate to what extent planet properties and
atmospheric chemical abundance can be retrieved with only JWST photometric data
points (2.5-15.5 $\mu$m) in conjunction with ground-based archival
low-resolution spectral data (1.0-2.3 $\mu$m). We find that the data is
consistent with an atmosphere with solar metallicity and C/O ratios at 0.40 and
0.55. We rule out 10x solar metallicity and an atmosphere with C/O = 1.0. We
also find strong evidence of silicate clouds but no sign of an enshrouding
featureless {{dust}} extinction. This work offers guidance and cautionary tales
on analyzing data in the absence of medium-to-high resolution spectral data.
