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Dust grains play an important role in the synthesis of molecules in theinterstellar medium, from the simplest species to complex organic molecules.How some of these solid-state molecules are converted into gas-phase species isstill a matter of debate. Our aim is to directly compare ice and gas abundancesof methanol (CH$_3$OH) and CO, and to investigate the relationship between iceand gas in low-mass protostellar envelopes. We present Submillimeter Array andAtacama Pathfinder EXperiment observations of gas-phase CH$_3$OH and CO towardsthe multiple protostellar system IRAS05417+0907 located in the B35A cloud. Weuse archival AKARI ice data toward the same target to calculate CH$_3$OH and COgas-to-ice ratios. The CO isotopologues emissions are extended, whereas theCH$_3$OH emission is compact and traces the giant outflow emanating fromIRAS05417+0907. A discrepancy between submillimeter dust emission and H$_2$Oice column density is found for B35A$-$4 and B35A$-$5, similar to what haspreviously been reported. B35A$-$2 and B35A$-$3 are located where thesubmillimeter dust emission peaks and show H$_2$O column densities lower thanfor B35A$-$4. The difference between the submillimeter continuum emission andthe infrared H$_2$O ice observations suggests that the distributions of dustand H$_2$O ice differ around the young stellar objects in this dense cloud. Thereason for this may be that the sources are located in different environmentsresolved by the interferometric observations: B35A$-$2, B35A$-$3 and inparticular B35A$-$5 are situated in a shocked region plausibly affected bysputtering and heating impacting the submillimeter dust emission pattern, whileB35A$-$4 is situated in a more quiescent part of the cloud. Gas and ice mapsare essential to connect small-scale variations in the ice composition withlarge-scale astrophysical phenomena probed by gas observations.

Linking ice and gas in the Lambda Orionis Barnard 35A cloud