Tracing star formation (and not) on resolved galactic scales

The star-formation rate (SFR) of galaxies is one of the key parameters in understanding their evolution, yet issues still exist in measuring the SFR, including extinction by dust and the specific calibration of the tracer. I will introduce results from our PHANGS collaboration using MUSE, ASTROSAT, HST and ground-based imaging showing how, on ~100 pc scales, we can resolve the individual tracers of star-formation such as Halpha, UV, dust (extinction and emission) and determine how these direct and indirect tracers, with different timescale correlations relate and break-down as a function of scale and environment.