Type Ia supernovae (SNe Ia) are bright thermonuclear explosions of carbon-oxygen white dwarfs as they accrete mass and approach the Chandrasekhar limit. Famously, these standardisable candles were used to measure the accelerating expansion of the Universe. SNe Ia are still extensively used as cosmological tools, but the precise nature of the progenitor to these explosions remains unclear and two scenarios dominate the theoretical explanations. The single-degenerate scenario involves a CO WD accreting matter from a normal or massive companion star whilst the double-degenerate scenario involves two WDs which inspiral, radiating energy via gravitational radiation, and merge. The biggest difference between the two mechanisms is the timescale on which they act and therefore, in the absence of a direct progenitor detection, the rates of SNe Ia are the most revealing insight into the so-called progenitor problem. I will present new results on the volumetric rate of SNe Ia in the local universe measured using the Palomar Transient Factory (PTF). PTF was an automated optical sky survey designed for transient discovery that spectroscopically confirmed 1800 supernovae over 2009-2012. With a 3-5 day observing cadence providing untargeted scans of the night sky, the PTF dataset is the perfect playground for a supernova rate calculation. We use three years of PTF data to construct a representative simulation of the survey in which we place Monte Carlo-ed explosions onto an artificial night sky. We re-run the survey to observe this sky, and compare the simulation results to the actual performance of PTF to weight the real supernovae, accounting for incompleteness in determining population numbers. We use this technique to calculate the most precise volumetric SN Ia rate to date.