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The diffuse ionized gas (DIG) is an important component of the interstellarmedium and it can be affected by many physical processes in galaxies. Measuringits distribution and contribution in emission allows us to properly study bothits ionization and star formation in galaxies. Here, we measure for the firsttime the DIG emission in 38 gas-stripped galaxies in local clusters drawn fromthe GAs Stripping Phenomena in galaxies with MUSE survey (GASP). These galaxiesare at different stages of stripping. We also compare the DIG properties tothose of 33 normal galaxies from the same survey. To estimate the DIG fraction(C$_{DIG}$) and derive its maps, we combine attenuation corrected H$\alpha$surface brightness with $\rm [SII]/H\alpha$ line ratio. Our results indicatethat we cannot use neither a single H$\alpha$ or $\rm [SII]/H\alpha$ value, nora threshold in equivalent width of H$\alpha$ emission line to separate spaxelsdominated by DIG and non-DIG emission. Assuming a constant surface brightnessof the DIG across galaxies underestimates C$_{DIG}$. Contrasting stripped andnon-stripped galaxies, we find no clear differences in C$_{DIG}$. The DIGemission contributes between 20\% and 90\% of the total integrated flux, anddoes not correlate with the galactic stellar mass and star-formation rate(SFR). The C$_{DIG}$ anti-correlates with the specific SFR, which may indicatean older ($>10^8$ yr) stellar population as ionizing source of the DIG. The DIGfraction shows anti-correlations with the SFR surface density, which could beused for a robust estimation of integrated C$_{DIG}$ in galaxies.

GASP XXXII. Measuring the diffuse ionized gas fraction in ram-pressure stripped galaxies