  We describe the general structure of the well known S255IR high mass star
forming region, as revealed by our recent ALMA observations. The data indicate
a physical relation of the major clumps SMA1 and SMA2. The driving source of
the extended high velocity well collimated bipolar outflow is not the most
pronounced disk-like SMA1 clump harboring a 20 M$_\odot$ young star (S255
NIRS3), as it was assumed earlier. Apparently it is the less evolved SMA2
clump, which drives the outflow and contains a compact rotating structure
(probably a disk). At the same time the SMA1 clump drives another outflow, with
a larger opening angle. The molecular line data do not show an outflow from the
SMA3 clump (NIRS1), which was suggested by IR studies of this region.
