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This work aims to determine how the galaxy main sequence (MS) changes usingseven different commonly used methods to select the star-forming galaxieswithin VIPERS data over $0.5 \leq z < 1.2$. The form and redshift evolution ofthe MS will then be compared between selection methods. The star-forminggalaxies were selected using widely known methods: a specific star-formationrate (sSFR), Baldwin, Phillips and Terlevich (BPT) diagram, 4000\AA\ spectralbreak (D4000) cut and four colour-colour cuts: NUVrJ, NUVrK, u-r, and UVJ. Themain sequences were then fitted for each of the seven selection methods using aMarkov chain Monte Carlo forward modelling routine, fitting both a linear mainsequence and a MS with a high-mass turn-over to the star-forming galaxies. Thiswas done in four redshift bins of $0.50 \leq z < 0.62$, $0.62 \leq z < 0.72$,$0.72 \leq z < 0.85$, and $0.85 \leq z < 1.20$. The slopes of all star-formingsamples were found to either remain constant or increase with redshift, and thescatters were approximately constant. There is no clear redshift dependency ofthe presence of a high-mass turn-over for the majority of samples, with theNUVrJ and NUVrK being the only samples with turn-overs only at low redshift. Nosamples have turn-overs at all redshifts. Star-forming galaxies selected withsSFR and u-r are the only samples to have no high-mass turn-over in allredshift bins. The normalisation of the MS increases with redshift, asexpected. The scatter around the MS is lower than the $\approx$0.3~dextypically seen in MS studies for all seven samples. The lack, or presence, of ahigh-mass turn-over is at least partially a result of the method used to selectstar-forming galaxies. However, whether a turn-over should be present or not isunclear.

Influence of star-forming galaxy selection on the galaxy main sequence