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Water in outflows from protostars originates either as a result of gas-phasesynthesis from atomic oxygen at T > 200 K, or from sputtered ice mantlescontaining water ice. We aim to quantify the contribution of the two mechanismsthat lead to water in outflows, by comparing observations of gas-phase water tomethanol (a grain surface product) towards three low-mass protostars inNGC1333. In doing so, we also quantify the amount of methanol destroyed inoutflows. To do this, we make use of JCMT and Herschel-HIFI data of H2O, CH3OHand CO emission lines and compare them to RADEX non-LTE excitation simulations.We find up to one order of magnitude decrease in the column density ratio ofCH3OH over H2O as the velocity increases in the line wings up to ~15 km/s. Anindependent decrease in X(CH3OH) with respect to CO of up to one order ofmagnitude is also found in these objects. We conclude that gas-phase formationof H2O must be active at high velocities (above 10 km/s, relative to the sourcevelocity) to re-form the water destroyed during sputtering. In addition, thetransition from sputtered water at low velocities to formed water at highvelocities must be gradual. We place an upper limit of two orders of magnitudeon the destruction of methanol by sputtering effects.

Water and methanol in low-mass protostellar outflows: gas-phase synthesis, ice sputtering and destruction