  Thermal phase variations of short period planets indicate that they are not
spherical cows: day-to-night temperature contrasts range from hundreds to
thousands of degrees, rivaling their vertical temperature contrasts.
Nonetheless, the emergent spectra of short-period planets have typically been
fit using one-dimensional (1D) spectral retrieval codes that only account for
vertical temperature gradients. The popularity of 1D spectral retrieval codes
is easy to understand: they are robust and have a rich legacy in Solar System
atmospheric studies. Exoplanet researchers have recently introduced
multi-dimensional retrieval schemes for interpreting the spectra of
short-period planets, but these codes are necessarily more complex and
computationally expensive than their 1D counterparts. In this paper we present
an alternative: phase-dependent spectral observations are inverted to produce
longitudinally resolved spectra that can then be fitted using standard 1D
spectral retrieval codes. We test this scheme on the iconic phase-resolved
spectra of WASP-43b and on simulated JWST observations using the open-source
pyratbay 1D spectral retrieval framework. Notably, we take the model complexity
of the simulations one step further over previous studies by allowing for
longitudinal variations in composition in addition to temperature. We show that
performing 1D spectral retrieval on longitudinally resolved spectra is more
accurate than applying 1D spectral retrieval codes to disk-integrated emission
spectra, despite being identical in terms of computational load. We find that
for the extant Hubble and Spitzer observations of WASP-43b the difference
between the two approaches is negligible but that JWST phase measurements
should be treated with longitudinally \textbf{re}solved \textbf{spect}ral
retrieval (ReSpect).
