Extended Data Fig. 2: The best-fit three-component model of VCC 1672.
From: An evolutionary continuum from nucleated dwarf galaxies to star clusters
The right panels display, from top to bottom, images of the data overlapped with isophotes, the best-fit model, and the residuals. North is up and east to the left. The left panels display the isophotal analysis of the 2D images and model fitting. From top to bottom, the panels show radial profiles of the axis ratio (q), the position angle (PA), the g′-band surface brightness, and the fitting residuals. For an illustration of the breaks in position angle and axis ratio, the effective radius of envelope components and outer components are plotted as vertical dot-dashed lines. Ellipses represent the effective radius of each individual component shown in the model image, which uses the same colour legend as in the surface brightness plot. We note that the shifts in both q and PA roughly correspond to the radius at which the outer component begins to dominate over the central envelope, at Re ∼ 500 pc. Error bars represent 1σ uncertainties.
