of $\sim40$ post-mergers (PM) presented by Ellison et al. (2015).We have also used 279 galaxies (of 2839, matched with our ANN’s input parameter space) from the Nancay Interstellar Baryons Legacy Extragalactic Survey (NIBLES) sample, presented by van Driel et al. (2016). They use a sample in the redshift range z$<$0.04 selected on z-band magnitude ($-24 < \rm{M_z} < -13.5$) as a proxy for stellar mass. Galaxies in the NIBLES sample are at the bright end of the SDSS distribution. All of the above samples have large amounts of ancillary information available, which may be used as input variables for the  estimation, from the following sources:

-   Photometry is taken from SDSS DR7. Structural parameters, such as bulge fractions and galaxy sizes are taken from the re-processed SDSS images by Simard et al. (2011) and Mendel et al. (2014). The fluxes in different bands ($u, g, r, i, z$) are all corrected for Galactic extinction.

-   Stellar masses are taken from Mendel et al. (2014) based on their re-assessment of SDSS photometry.

-   Total star formation rates were taken from the MPA/JHU catalogs, which applied a colour dependent aperture correction to account for the light outside of the SDSS fibre (Brinchmann 