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We study the molecular gas content and distribution in the Coma clusterspiral galaxy NGC 4848. Plateau de Bure interferometric CO(1-0) observationsreveal a lopsided H_2 distribution with an off-center secondary maximumcoincident with the inner part of the HI. NGC 4848 is not at all deficient inmolecular gas as it contains M_H_2~4x10^9 M_solar. At the interface between theCO and HI emission regions, about 8 kpc NW of the center, however, strong starformation is present as witnessed by Halpha and radio continuum emission. Thisis the region in which earlier Fabry-Perot observations revealed adouble-peaked Halpha line, indicating gas at two different velocities at thesame sky position. In order to understand these observations, we present theresults of numerical simulations of the ISM-ICM interaction. We suggest thatNGC 4848 already passed through the center of the cluster about 4x10^8 yearsago. At the observed stage ram pressure has no more direct dynamical influenceon the galaxy's ISM. We observe the galaxy when a fraction of the stripped gasis falling back onto the galaxy. Ram pressure is thus a short-lived event withlonger-lasting consequences. The combination of ram-pressure and rotationresults in gas at different velocities colliding where the double-peaked Halphaline is observed. Ram-pressure can thus result, after re-accretion, indisplaced molecular gas without the H_2 itself being pushed efficiently by theICM. A scenario where two interactions take place simultaneously is alsoconsistent with the available data but less probable on the basis of ournumerical simulations.Comment: 15 pages with 20 figures. A&A, in pres

$\mathsf{^{12}}$CO(1-0) observations of NGC 4848: A Coma galaxy after stripping