Notes: Column (1): object designation in the Infrared Astronomical Satellite (IRAS) Faint Source Catalog (FSC). Column (2): other identification. Column (3): morphological classification based on Spitzer and HST images. The galaxies are classified using the scheme shown in Fig. A.1. Column (4): Hα visual kinematic classification from Bellocchi et al. (2013). The sources are classified as rotating disk (RD), perturbed disk (PD) or complex kinematics (CK). Column (5): Hα kinemetry classification from Bellocchi et al. (2016). The galaxies are classified as disk (D), merger (M), disk* (D*) or merger* (M*). The star (*) symbol identifies the galaxies which belong to the transition region (i.e., the area where disks and mergers coexist, making their classification more uncertain; see Bellocchi et al. 2016 for details). Column (6): CO(2–1) visual kinematic classification (this work). We used the same criteria used for the Hα line from Bellocchi et al. (2013). Column (7): final composite classification: the morphological and kinematic information are merged together. Four different classes are defined: isolated rotating disks ‘0 (RD)’, isolated perturbed disks ‘0 (PD)’, interacting systems ‘1’ and and post-coalescence mergers ‘2’ (see text for details).