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We present IRAM 30m sensitive upper limits on CO emission in the ram pressurestripped dwarf Virgo galaxy IC3418 and in a few positions covering HII regionsin its prominent 17 kpc UV/Ha gas-stripped tail. In the central few arcsecondsof the galaxy, we report a possible marginal detection of about 1x10^6 M_sun ofmolecular gas (assuming a Galactic CO-to-H_2 conversion factor) that couldcorrespond to a surviving nuclear gas reservoir. We estimate that there is lessmolecular gas in the main body of IC3418, by at least a factor of 20, thanwould be expected from the pre-quenching UV-based star formation rate assumingthe typical gas depletion timescale of 2 Gyr. Given the lack of star formationin the main body, we think the H_2-deficiency is real, although some of it mayalso arise from a higher CO-to-H_2 factor typical in low-metallicity, low-massgalaxies. The presence of HII regions in the tail of IC3418 suggests that theremust be some dense gas; however, only upper limits of < 1x10^6 M_sun were foundin the three observed points in the outer tail. This yields an upper limit onthe molecular gas content of the whole tail < 1x10^7 M_sun, which is an amountsimilar to the estimates from the observed star formation rate over the tail.We also present strong upper limits on the X-ray emission of the stripped gasin IC3418 from a new Chandra observation. The measured X-ray luminosity of theIC3418 tail is about 280 times lower than that of ESO 137-001, a spiral galaxyin a more distant cluster with a prominent ram pressure stripped tail.Non-detection of any diffuse X-ray emission in the IC3418 tail may be due to alow gas content in the tail associated with its advanced evolutionary stateand/or due to a rather low thermal pressure of the surrounding intra-clustermedium.

Search for cold and hot gas in the ram pressure stripped Virgo dwarf galaxy IC3418