use photometry from up to 36 (COSMOS) and 16 (UDS) wide, medium and narrow bands (spanning [*GALEX*]{} far-UV and near-UV bands to [ *Spitzer*]{}/IRAC) and calculate the rest-frame spectral energy distribution, reddening, star-formation history and stellar mass [@Sobral10]. The stellar masses of these galaxies range from 10$^{9.7-11.0}$M$_{\odot}$ (Table 1; see also @Swinbank12a).

Since the stellar masses are calculated from 2$''$ aperture photometry (and then corrected to total magnitudes using aperture corrections, @Sobral10), to estimate the stellar surface density in the same area as our IFU observations, we assume that stellar light follows an exponential profile with Sersic index, n$_{\rm serc}$=1–2 and calculate the fraction of the total stellar mass within the disk radius, $R$ (which we define as two times the H$\alpha$ half light radius, $r_{\rm h}$). Allowing a range of power-law index from $n$=1.0–1.8 and a ratio of stellar- to gas- velocity dispersion of $f_{\sigma}$=1–2 [@Korchagin03], we calculate the best-fit absolute star formation efficiency, $A$ and in Fig. \[fig:SF\_galgal\] we overlay the best-fit solutions. Over the range $n$=1.0–1.8, the best fit absolute star formation efficiency for the sample is $A$=(4.1$\pm$2.4)$\times$10$^{-4}$M$_{\odot}$yr$^{-1}$kpc$^{-2}$ (where the error-bar incorporates the galaxy-to-galaxy variation, a range of $f_{\sigma}$=1–2, and the errors on the stellar masses of 