When did round disk galaxies form?

When and how galaxy morphology such as disk and bulge seen in the present-day universe emerged is still not clear. In the universe at \(z\gtrsim 2\), galaxies with various morphology are seen, and star-forming galaxies at \(z\sim2\) show an intrinsic shape of bar-like structure. Then, when did round disk structure form? Here we take a simple and straightforward approach to see the epoch when a round disk galaxy population emerged by constraining the intrinsic shape statistically based on apparent axial ratio distribution of galaxies. We derived the distributions of the apparent axial ratios in the rest-frame optical light (\(\sim 5000\) \AA) of star-forming main sequence galaxies at \(2.5>z>1.4\), \(1.4>z>0.85\), and \(0.85>z>0.5\), and found that the apparent axial ratios of them show peaky distributions at \(z\gtrsim0.85\), while a rather flat distribution at the lower redshift. By using a tri-axial model (\(A>B>C\)) for the intrinsic shape, we found the best-fit models give the peaks of the \(B/A\) distribution of \(0.81\pm0.04\), \(0.84\pm0.04\), and \(0.92\pm0.05\) at \(2.5>z>1.4\), \(1.4>z>0.85\), and \(0.85>z>0.5\), respectively. The last value is close to the local value of 0.95. Thickness (\(C/A\)) is \(\sim0.25\) at all the redshifts and is close to the local value (0.21). The results indicate the shape of the star-forming galaxies in the main sequence changes gradually, and the round disk is established at around \(z\sim0.9\). Establishment of the round disk may be due to a cease of violent interaction of galaxies or a growth of a bulge and/or a super-massive black hole resides at the center of a galaxy which dissolves the bar structure.