Notes. This photometry is obtained from the WISE All-Sky Atlas Image Inventory Table (W1-W4 bands) using the procedures detailed in Section 3.1. Uncertainties (±) represent the standard deviation within each galaxy dataset. The ’integrated’ and ’central’ columns refer to integrated and central aperture fluxes, respectively (see Section 3.1.4), and number of image pixels considered. Central apertures typically comprise < 5 % of the pixel integrated apertures. Excitation classes (’class’) are based on central aperture mIRdds (Section 4.1). Stellar masses (M_*) are obtained as described in Section 2.3.2, while morphological types (’Morph.’) are taken from (1), (2) and NED (if available). For GMP3016 (barely detected by WISE), integrated flux densities are used. The ’galaxy cluster’ column lists the host cluster. Undergoing perturbation (2): RP (ram pressure), M (merging), H (harassment). RPS acting solely might indicate process strength. When multiple perturbing mechanisms are at place, the first one reported has been identified as the dominant. WHAN excitation classes taken from (2) (see Appendix C).

Reference. (1) Boselli et al. (2010); (2) Boselli et al. (2022).