Searching double-peaked emission line profiles in the spectra of
  galaxies through the symmetry of the cross-correlation function
  The presence of double-peaked/multicomponent emission line profiles in
spectra of galaxies is commonly done by visual inspection. However, the
identification of complex emission line profiles by eye is unapproachable for
large databases such as the Sloan Digital Sky Survey (SDSS) or the integral
field spectroscopy surveys of galaxies (e.g. CALIFA or MaNGA). We describe a
quick method involving the cross-correlation technique for detecting the
presence of complex (double-peaked or multiple components) profiles in the
spectra of galaxies, deriving simultaneously a first estimation of the velocity
dispersions and radial velocities of the dominant gaseous component. We
illustrate the proposed procedure with the well-known complex [OIII]4959,5007
profiles of the central region of NGC1068.
