Extended Data Fig. 6: Distribution of measured parameters for the full ALMA sample galaxies.
From: In situ spheroid formation in distant submillimetre-bright galaxies
a, Axis ratio q versus rest-frame wavelength λrest. b, Spergel index ν versus S/Nbeam. c, q versus S/Nbeam. The red squares in panel a indicate the median values of q in different wavelength bins, whereas those in panels b and c represent the median and mean values of ν and q in different S/Nbeam bins, respectively. The vertical and horizontal bars indicate the error on the average and bin width, respectively. The blue crosses in panel c represent the intrinsic distribution of q, derived from the best fit for the whole sample, perturbed by noise. The noise is assumed to be Gaussian, with the standard deviation estimated as the error on q measured at the corresponding S/Nbeam bins, with average values of 0.19, 0.16 and 0.08, respectively. The good agreement between the model and data suggests that the slight decrease in q at lower S/N levels can be attributed to the higher levels of noise observed.
