AbstractResults are presented from our ongoing studies of Titan using ALMA during the period 2012-2015, including a confirmation of the previous detection of vinyl cyanide (C₂H₃CN), as well as the first spatial map for this species on Titan. Simultaneous mapping of HC₃N, CH₃CN and C₂H₅CN reveal characteristic abundance patterns for each species that provide insight into their individual photochemical lifetimes, and help inform our understanding of Titan’s unique, time-variable atmospheric chemistry and global circulation. A time-sequence of HC₃N maps covering 38 months reveals a dramatic change in the distribution of this gas consistent with high-altitude photochemical production followed by advection towards the southern (winter) pole, combined with rapid loss in the north after Titan’s 2009 seasonal equinox. The 2015 C₂H₃CN and C₂H₅CN maps show abundance peaks in Titan’s southern hemisphere, similar to those observed for the short-lived HC₃N molecule. The longer-lived CH₃CN, on the other hand, remains more concentrated in the north.