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Star formation is a multi-scale, multi-physics problem ranging from the sizescale of molecular clouds ($\sim$10s pc) down to the size scales of denseprestellar cores ($\sim$0.1 pc) that are the birth sites of stars. Severalphysical processes like turbulence, magnetic fields and stellar feedback, suchas radiation pressure and outflows, are more or less important for differentstellar masses and size scales. During the last decade a variety oftechnological and computing advances have transformed our understanding of starformation through the use of multi-wavelength observations, large scaleobservational surveys, and multi-physics multi-dimensional numericalsimulations. Additionally, the use of synthetic observations of simulationshave provided a useful tool to interpret observational data and evaluate theimportance of various physical processes on different scales in star formation.Here, we review these recent advancements in both high- ($M \gtrsim 8 \, M_{\rm\odot}$) and low-mass star formation.

Zooming in on Individual Star Formation: Low- and High-mass Stars