$-$045440.7        1.4625                    6               4.1$\pm$0.2            62$\pm$11               190$\pm$20      0.2$\pm$0.2              10.08$\pm$0.28                             9.8$\pm$0.4
  SHiZELS-10              021739.0   $-$044443.1        1.4471                   10               2.3$\pm$0.2             64$\pm$8               30$\pm$12       0.3$\pm$0.2               9.42$\pm$0.33                             9.9$\pm$0.4
  SHiZELS-11              021821.2   $-$050248.9        1.4858                    8               1.3$\pm$0.4            190$\pm$18              224$\pm$15      0.5$\pm$0.2              11.01$\pm$0.24                            10.1$\pm$0.4
  SHiZELS-12              021901.4   $-$045814.6        1.4676                    5               0.9$\pm$0.5            115$\pm$10                 ...          0.3$\pm$0.2              10.59$\pm$0.30                             9.6$\pm$0.4
  SHiZELS-14              100051.6   +02:3334.5         2.2418                   27               4.6$\pm$0.4            131$\pm$17                 ...          0.4$\pm$0.1              10.90$\pm$0.20                            10.1$\pm$0.4
  Median                    ...          ...             1.46                  7$\pm$2            2.4$\pm$0.7            75$\pm$19               147$\pm$31      0.3$\pm$0.1              10.25$\pm$0.50                             9.8$\pm$0.2
  \[table:gal\_props\]                                                                                                                                                                                                
  ---------------------- ---------- ------------- ------------------- ------------------------- --------------- ---------------------------- ------------------ ------------- --------------------------------------- -----------------------------------------

Notes: $^{a}$H$\alpha$ star formation rate using the calibration from @Kennicutt98 with a Chabrier IMF; SFR$_{\rm
  H\alpha}$=4.6$\times$10$^{-42}$L$_{\rm H\alpha}$. $^b$H$\alpha$ half light radius, deconvolved for the PSF. $^c$Average velocity dispersion for each galaxy, corrected for beam-smearing due to the PSF. $^d$$v_{\rm asym}$ denotes the best-fit asymptotic rotation speed of the galaxy, and is corrected for inclination (see @Swinbank12a for details on the kinematic modeling of these galaxies).

In order to test whether this model provides an adequate description of our data, we fit the $\Sigma_{\rm SFR}$–$\sigma$ distribution for each galaxy in our sample. To estimate the stellar surface density, $\Sigma_{\star}$, we we follow @Sobral11 and perform a full SED $\chi^2$ fit of the rest-frame UV–mid-infrared photometry using the @Bruzual03 and Bruzual (2007) population synthesis models. We 