  Convection and turbulence in stellar atmospheres have a significant effect on
the emergent flux from late-type stars. The theoretical advancements in
convection modelling over recent years have proved challenging for the
observers to obtain measurements with sufficient precision and accuracy to
allow discrimination between the various predictions.
  An overview of the current observational techniques used to evaluate various
convection theories is presented, including photometry, spectrophotometry, and
spectroscopy. The results from these techniques are discussed, along with their
successes and limitations.
  The prospects for improved observations of stellar fluxes are also given.
