The diffuse ionized gas (DIG) is an important component of the interstellar medium, and it can be affected by many physical processes in galaxies. Measuring its distribution and contribution in emission allows us to properly study both its ionization and star formation in galaxies. Here, we measure for the first time the DIG emission in 38 gas-stripped galaxies in local clusters drawn from the GAs Stripping Phenomena in galaxies with the MUSE survey (GASP). These galaxies are at different stages of stripping. We also compare the DIG properties to those of 33 normal galaxies from the same survey. To estimate the DIG fraction (CDIG) and derive its maps, we combine the attenuation-corrected H{alpha} surface brightness with the [SII]/H{alpha} line ratio. Our results indicate that we cannot use either a single H{alpha} or [SII]/H{alpha} value, or a threshold in equivalent width of H{alpha} emission line to separate spaxels dominated by DIG and non-DIG emission. Assuming a constant surface brightness of the DIG across galaxies underestimates CDIG. Contrasting stripped and nonstripped galaxies, we find no clear differences in CDIG. The DIG emission contributes between 20% and 90% of the total integrated flux and does not correlate with the galactic stellar mass and star formation rate (SFR). The CDIG anticorrelates with the specific SFR, which may indicate an older (>108yr) stellar population as the ionizing source of the DIG. The DIG fraction shows anticorrelations with the SFR surface density, which could be used for a robust estimation of integrated CDIG in galaxies.

Cone search capability for table J/ApJ/907/22/table1 (Galaxies from the control sample)

Cone search capability for table J/ApJ/907/22/table2 (Stripped galaxies)