(a) The distribution of the GAMA galaxy sample spanning 0 < z ≤ 0.25. The model tracks from the top to bottom have the following IMF slopes, α=−2, −2.35, −3. This figure is similar to fig. 1 of Hoversten & Glazebrook (2008); the scale and model IMF tracks of both figures are the same. (b) The distribution of the redshift of the SDSS main sample and the GAMA sample for 0 < z ≤ 0.25. (c) The GAMA sample colour coded according to z. This sample covers the range 0 < z ≤ 0.25. It is clear that the reason the peak in the data density in top-panel lies higher than in the corresponding diagram from Hoversten & Glazebrook (2008) is because of the higher redshift range sampled.