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22 GHz water and 6.7 GHz methanol masers are usually thought as signposts ofearly stages of high-mass star formation but little is known about theirassociations and the physical environments they occur in.  The aim was to obtain accurate positions and morphologies of the water maseremission and relate them to the methanol maser emission recently mapped withVery Long Baseline Interferometry. A sample of 31 methanol maser sources wassearched for 22 GHz water masers using the VLA and observed in the 6.7 GHzmethanol maser line with the 32 m Torun dish simultaneously. Water maserclusters were detected towards 27 sites finding 15 new sources. The detectionrate of water maser emission associated with methanol sources was as high as71%. In a large number of objects (18/21) the structure of water maser is wellaligned with that of the extended emission at 4.5 $\mu$m confirming the originof water emission from outflows. The sources with methanol emission withring-like morphologies, which likely trace a circumstellar disk/torus, eitherdo not show associated water masers or the distribution of water maser spots isorthogonal to the major axis of the ring. The two maser species are generallypowered by the same high-mass young stellar object but probe different parts ofits environment. The morphology of water and methanol maser emission in aminority of sources is consistent with a scenario that 6.7 GHz methanol maserstrace a disc/torus around a protostar while the associated 22 GHz water masersarise in outflows. The majority of sources in which methanol maser emission isassociated with the water maser appears to trace outflows. The two types ofassociations might be related to different evolutionary phases.

VLA observations of water masers towards 6.7 GHz methanol maser sources