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Determining the locations of the major snowlines in protostellar environmentsis crucial to fully understand the planet formation process and its outcome.Despite being located far enough from the central star to be spatially resolvedwith ALMA, the CO snowline remains difficult to detect directly inprotoplanetary disks. Instead, its location can be derived from N$_2$H$^+$emission, when chemical effects like photodissociation of CO and N$_2$ aretaken into account. The water snowline is even harder to observe than that forCO, because in disks it is located only a few AU from the protostar, and fromthe ground only the less abundant isotopologue H$_2^{18}$O can be observed.Therefore, using an indirect chemical tracer, as done for CO, may be the bestway to locate the water snowline. A good candidate tracer is HCO$^+$, which isexpected to be particularly abundant when its main destructor, H$_2$O, isfrozen out. Comparison of H$_2^{18}$O and H$^{13}$CO$^+$ emission toward theenvelope of the Class 0 protostar IRAS2A shows that the emission from bothmolecules is spatially anticorrelated, providing a proof of concept thatH$^{13}$CO$^+$ can indeed be used to trace the water snowline in systems whereit cannot be imaged directly.

Imaging the water snowline in protostellar envelopes