  Of the C$_{3}$H$_{x}$ hydrocarbons, propane (C${_3}$H$_{8}$) and propyne
(methylacetylene, CH$_{3}$C$_{2}$H) were first detected in Titan's atmosphere
during the Voyager 1 flyby in 1980. Propene (propylene, C$_{3}$H$_{6}$) was
first detected in 2013 with data from the Composite InfraRed Spectrometer
(CIRS) instrument on Cassini. We present the first measured abundance profiles
of propene on Titan from radiative transfer modeling, and compare our
measurements to predictions derived from several photochemical models. Near the
equator, propene is observed to have a peak abundance of 10 ppbv at a pressure
of 0.2 mbar. Several photochemical models predict the amount at this pressure
to be in the range 0.3 - 1 ppbv and also show a local minimum near 0.2 mbar
which we do not see in our measurements. We also see that propene follows a
different latitudinal trend than the other C$_{3}$ molecules. While propane and
propyne concentrate near the winter pole, transported via a global convective
cell, propene is most abundant above the equator. We retrieve vertical
abundances profiles between 125 km and 375 km for these gases for latitude
averages between 60$^{\circ}$S to 20$^{\circ}$S, 20$^{\circ}$S to
20$^{\circ}$N, and 20$^{\circ}$N to 60$^{\circ}$N over two time periods, 2004
through 2009 representing Titan's atmosphere before the 2009 equinox, and 2012
through 2015 representing time after the equinox.
  Additionally, using newly corrected line data, we determined an updated upper
limit for allene (propadiene, CH$_{2}$CCH$_{2}$, the isomer of propyne). We
claim a 3-$\sigma$ upper limit mixing ratio of 2.5$\times$10$^{-9}$ within
30$^\circ$ of the equator. The measurements we present will further constrain
photochemical models by refining reaction rates and the transport of these
gases throughout Titan's atmosphere.
