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Within the GASP survey, aimed at studying the effect of the ram-pressurestripping on the star formation quenching in cluster galaxies, we analyze hereALMA observations of the jellyfish galaxy JW100. We find an unexpected largeamount of molecular gas ($\sim 2.5 \times 10^{10} M_{\odot}$), 30\% of which islocated in the stripped gas tail out to $\sim$35 kpc from the galaxy center.The overall kinematics of molecular gas is similar to the one shown by theionized gas, but for clear signatures of double components along the strippingdirection detected only out to 2 kpc from the disk. The line ratio $r_{21}$ hasa clumpy distribution and in the tail can reach large values ($\geq 1$), whileits average value is low (0.58 with a 0.15 dispersion). All these evidencestrongly suggest that the molecular gas in the tail is newly born from strippedHI gas or newly condensed from stripped diffuse molecular gas. The analysis ofinterferometric data at different scales reveals that a significant fraction($\sim 40\%$) of the molecular gas is extended over large scales ($\geq 8$ kpc)in the disk, and this fraction becomes predominant in the tail ($\sim 70\%$).By comparing the molecular gas surface density with the star formation ratesurface density derived from the \Ha emission from MUSE data, we find that thedepletion time on 1 kpc scale is particularly large ($5-10$ Gyr) both withinthe ram-pressure disturbed region in the stellar disk, and in the complexesalong the tail.

GASP. XXII The molecular gas content of the JW100 jellyfish galaxy at z~0.05: does ram pressure promote molecular gas formation?