2008 - Judit Bakos et al, Color Profiles of Spiral Galaxies: Clues on Outer-Disk Formation Scenarios[1]
We estimate that the fraction of stellar mass outside the break radius is ~15% for truncated galaxies and ~9% for antitruncated galaxies.
2009 - Stelios Kazantzidis et al, Cold Dark Matter Substructure and Galactic Disks II: Dynamical Effects of Hierarchical Satellite Accretion[2]
These include (1) considerable thickening and heating at all radii, with the disk thickness and velocity ellipsoid nearly doubling at the solar radius; (2) prominent flaring associated with an increase in disk thickness greater than a factor of 4 in the disk outskirts; (3) surface density excesses at large radii, beyond ~5 disk scale lengths, resembling those of observed antitruncated disks; (4) lopsidedness at levels similar to those measured in observational samples of disk galaxies; and (5) substantial tilting.
2010 - Marina A. Startseva et al, Structure of the Galaxies in the NGC 80 Group[3]
In most of the galaxies, more precisely in all of them more luminous than M(B) -18, two-tiered (antitruncated) stellar disks are detected, whose radial surface brightness profiles can be fitted by two exponential segments with different scalelengths -- shorter near the center and longer at the periphery.
2011 - David T. Maltby et al, "Anti-truncated stellar light profiles in the outer regions of STAGES spiral galaxies: bulge or disc related?" arXiv
In the established classification scheme, antitruncated mu(r) profiles (Type III) have a broken exponential disc with a shallower region beyond the break radius r_brk.
