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Fig. 11.


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Three toy profiles that illustrate our structure detection method. Left panel: smooth galaxy without structure, middle panel: strongly perturbed galaxy, and right panel: slightly perturbed object. For each profile, its luminosity is plotted as a function of the distance to the galaxy centre in arbitrary units (blue solid lines). Their corresponding first and second derivatives are also plotted (orange and green solid lines, respectively). We can see that the number of roots in the second derivative is a good indicator of perturbed galaxies.

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