The WFC3 infrared spectroscopic parallel survey (WISPS) identifies strong emission line galaxies over cosmic noon (tracking H-alpha at z~1). This enables us to select more directly on current star formation rate (SFR), unlike previous surveys which have typically selected on stellar mass through a broad-band magnitude limit. WISPS allows us to assess any bias in previous SFR studies, which can potentially miss high SFR systems which have low stellar mass, and which may contribute significantly to SFR density through bursty star formation histories. However many WISPS galaxies have only single line detections (usually assumed to be H-alpha), and we have been conducting follow up optical spectroscopic observations to eliminate any ambiguity in the redshift. Our multi-slit optical spectroscopy with VLT-FORS2 and Gemini-GMOS provides the rest-optical lines H-beta, [OIII]5007 and [OII]3727 measurements, in addition to the H-alpha from the slitless WISPS spectra. We can use emission line diagnostics to determine the metallicity and ionisation conditions, estimate the extinction, and assess AGN contamination. Hence we can determine the nature of the z~1 star-forming population of galaxies, selected on their star formation rates rather than broad-band magnitudes.