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In the low redshift Universe (z<0.3), our view of galaxy evolution isprimarily based on fibre optic spectroscopy surveys. Elaborate methods havebeen developed to address aperture effects when fixed aperture sizes only probethe inner regions for galaxies of ever decreasing redshift or increasingphysical size. These aperture corrections rely on assumptions about thephysical properties of galaxies. The adequacy of these aperture corrections canbe tested with integral-field spectroscopic data. We use integral-field spectradrawn from 1212 galaxies observed as part of the SAMI Galaxy Survey toinvestigate the validity of two aperture correction methods that attempt toestimate a galaxy's total instantaneous star formation rate. We show thatbiases arise when assuming that instantaneous star formation is traced bybroadband imaging, and when the aperture correction is built only from spectraof the nuclear region of galaxies. These biases may be significant depending onthe selection criteria of a survey sample. Understanding the sensitivities ofthese aperture corrections is essential for correct handling of systematicerrors in galaxy evolution studies.

The SAMI Galaxy Survey: Can we trust aperture corrections to predict star formation?