  Recently, we introduced PLanetary Atmospheric Tool for Observer Noobs
(PLATON), a Python package that calculates model transmission spectra for
exoplanets and retrieves atmospheric characteristics based on observed spectra.
We now expand its capabilities to include the ability to compute secondary
eclipse depths. We have also added the option to calculate models using the
correlated-$k$ method for radiative transfer, which improves accuracy without
sacrificing speed. Additionally, we update the opacities in PLATON--many of
which were generated using old or proprietary line lists--using the most recent
and complete public line lists. These opacities are made available at R=1000
and R=10,000 over the 0.3--30 um range, and at R=375,000 in select near IR
bands, making it possible to utilize PLATON for ground-based high resolution
cross correlation studies. To demonstrate PLATON's new capabilities, we perform
a retrieval on published HST and Spitzer transmission and emission spectra of
the archetypal hot Jupiter HD 189733b. This is the first joint transit and
secondary eclipse retrieval for this planet in the literature, as well as the
most comprehensive set of both transit and eclipse data assembled for a
retrieval to date. We find that these high signal-to-noise data are
well-matched by atmosphere models with a C/O ratio of $0.66_{-0.09}^{+0.05}$
and a metallicity of $12_{-5}^{+8}$ times solar where the terminator is
dominated by extended nanometer-sized haze particles at optical wavelengths.
These are among the smallest uncertainties reported to date for an exoplanet,
demonstrating both the power and the limitations of HST and Spitzer exoplanet
observations.
