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We present the main sequence for all galaxies and star-forming galaxies for asample of 28,469 massive ($M_\star \ge 10^{11}$M$_\odot$) galaxies at cosmicnoon ($1.5 < z < 3.0$), uniformly selected from a 17.5 deg$^2$ area (0.33Gpc$^3$ comoving volume at these redshifts). Our large sample allows for anovel approach to investigating the galaxy main sequence that has not beenaccessible to previous studies. We measure the main sequence in small mass binsin the SFR-M$_{\star}$ plane without assuming a functional form for the mainsequence. With a large sample of galaxies in each mass bin, we isolatestar-forming galaxies by locating the transition between the star-forming andgreen valley populations in the SFR-M$_{\star}$ plane. This approach eliminatesthe need for arbitrarily defined fixed cutoffs when isolating the star-forminggalaxy population, which often biases measurements of the scatter around thestar-forming galaxy main sequence. We find that the main sequence for allgalaxies becomes increasingly flat towards present day at the high-mass end,while the star-forming galaxy main sequence does not. We attribute thisdifference to the increasing fraction of the collective green valley andquiescent galaxy population from $z=3.0$ to $z=1.5$. Additionally, we measurethe total scatter around the star-forming galaxy main sequence and find that itis $\sim0.5-1.0$ dex with little evolution as a function of mass or redshift.We discuss the implications that these results have for pinpointing thephysical processes driving massive galaxy evolution.

The Shape and Scatter of The Galaxy Main Sequence for Massive Galaxies at Cosmic Noon