Morphological Classification of Local Luminous Infrared Galaxies

We present an analysis of the morphological classification of 89 luminous infrared galaxies (LIRGs) from the Great Observatories All-sky LIRG Survey (GOALS) sample using non-parametric coefficients and compare their morphology as a function of wavelength. We rely on images obtained in the optical (B- and I-band) as well as in the infrared (H-band and 5.8\(\mu\)m). Our classification is based on the calculation of \(Gini\) and the second order of light (\(M_{20}\)) non-parametric coefficients which we explore as a function of stellar mass (\(M_\star\)), infrared luminosity (\(L_{IR}\)) and star formation rate (SFR). We investigate the relation between \(M_{20}\), the specific SFR (sSFR) and the dust temperature (\(T_{dust}\)) in our galaxy sample. We find that \(M_{20}\) is a better morphological tracer than \(Gini\), as it allows to distinguish systems formed by double systems from isolated and post-merger LIRGs. The multi-wavelength analysis allows us to identify a region in the \(Gini\)-\(M_{20}\) parameter space where ongoing mergers reside, regardless of the band used to calculate the coefficients. In particular when measured in the H-band, this region can be used to identify ongoing mergers, with a minimal contamination from LIRGs in other stages. We also find that while the sSFR is positively correlated with \(M_{20}\) when measured in the mid-infrared, i.e. star-bursting galaxies show more compact emission, it is anti-correlated with the B-band based \(M_{20}\). We interpret this as the spatial decoupling between obscured and un-obscured star formation, whereby the ultraviolet/optical size of a LIRGs experience an intense dust enshrouded central starburst is larger than in the one in the mid-infrared since the contrast between the nuclear to the extended disk emission is smaller in the mid-infrared. This has important implications for high redshift surveys of dusty sources. [abridged]