  Observations of exoplanet transit spectra are essential to understanding the
physics and chemistry of distant worlds. The effects of opacity sources and
many physical processes combine to set the shape of a transit spectrum. Two
such key processes - refraction and cloud and/or haze forward scattering - have
seen substantial recent study. However, models of these processes are typically
complex, which prevents their incorporation into observational analyses and
standard transit spectrum tools. In this work, we develop analytic expressions
that allow for the efficient parameterization of forward scattering and
refraction effects in transit spectra. We derive an effective slant optical
depth that includes a correction for forward scattered light, and present an
analytic form of this correction. We validate our correction against a
full-physics transit spectrum model that includes scattering, and we explore
the extent to which the omission of forward scattering effects may bias models.
Also, we verify a common analytic expression for the location of a refractive
boundary, which we express in terms of the maximum pressure probed in a transit
spectrum. This expression is designed to be easily incorporated into existing
tools, and we discuss how the detection of a refractive boundary could help
indicate the background atmospheric composition by constraining the bulk
refractivity of the atmosphere. Finally, we show that opacity from Rayleigh
scattering and collision induced absorption will outweigh the effects of
refraction for Jupiter-like atmospheres whose equilibrium temperatures are
above 400-500 K.
