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In practice, we therefore applied the set of criteria below to each galaxy in order to select between the Stage 2 bulge-disk decomposition and Stage 3 bulge-diskbar decomposition. 1 lists the model chosen for each galaxy. 2 summarizes the model parameters from the best fits. For completeness, we note that for the few rare galaxies (see Sect. 2) that have just a bar and a disk, the choice of a final solution is between the Stage 2 bardisk decomposition and Stage 3 bulge-disk-bar decomposition. The same guidelines below can be used to identify the best model.

9 Columns are: (1) Indicates whether the model is for Stage 1 (pure Sérsic profile), Stage 2 (bulgeCdisk or barCdisk), or Stage 3 (bulgeCdiskCbar). (2) One of pure Sérsic profile, Sérsic bulge, exponential disk, or Sérsic bar. (3) Effective radius of the bulge/bar or disk scalelength in arcseconds. (4) Effective radius of the bulge/bar or disk scalelength in kpc. (5) The Sérsic index of the profile. (6) Axis ratio of the component. (7) Position angle in degrees of the component. Positive angles are East of North.

Pseudobulges tend to have a bulge n < 2:5 (Kormendy and Fisher 2005; Fisher and Drory 2008). One possibility for the formation of disky bulges or pseudobulges is the idea of secular evolution (Kormendy 1993; KK04; Jogee et al. 2005), where a stellar bar or globally oval structure in a non-interacting galaxy drives the gas inflow into the inner kpc via shocks and gravitational torque. Another idea for building disky bulges is that the gas inflow into the inner kiloparsec is driven by external nonsecular processes, such as tidal interaction and minor mergers.

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