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The strong enhancement of the ultraviolet emission during solar flares isusually taken as an indication of plasma heating in the lower solar atmospherecaused by the deposition of the energy released during these events. Imagestaken with broadband ultraviolet filters by the {\em Transition Region andCoronal Explorer} (TRACE) and {\em Atmospheric Imaging Assembly} (AIA 1600 and1700~\AA) have revealed the morphology and evolution of flare ribbons in greatdetail. However, the spectral content of these images is still largely unknown.Without the knowledge of the spectral contribution to these UV filters, the useof these rich imaging datasets is severely limited. Aiming to solve this issue,we estimate the spectral contributions of the AIA UV flare and plage imagesusing high-resolution spectra in the range 1300 to 1900~\AA\ from the SkylabNRL SO82B spectrograph. We find that the flare excess emission in AIA 1600~\AA\is { dominated by} the \ion{C}{4} 1550~\AA\ doublet (26\%), \ion{Si}{1}continua (20\%), with smaller contributions from many other chromospheric linessuch as \ion{C}{1} 1561 and 1656~\AA\ multiplets, \ion{He}{2} 1640~\AA,\ion{Si}{2} 1526 and 1533~\AA. For the AIA 1700~\AA\ band, \ion{C}{1} 1656~\AA\multiplet is the main contributor (38\%), followed by \ion{He}{2} 1640 (17\%),and accompanied by a multitude of other, { weaker} chromospheric lines, withminimal contribution from the continuum. Our results can be generalized tostate that the AIA UV flare excess emission is of chromospheric origin, whileplage emission is dominated by photospheric continuum emission in bothchannels.

The spectral content of SDO/AIA 1600 and 1700 \AA\ filters from flare and plage observations