Contribution function for a T_eff = 1900K, log(g) = 5, f_sed = 2, solar metallicity, and solar C/O ratio atmosphere. The pressures probed by the HST wavelengths (1.1-1.67 μm), highlighted by the vertical white lines, probe deeper than longer wavelengths that are accessible to JWST. Observations at longer wavelengths that probe the upper atmosphere may be more sensitive to auroral signatures.