  The $^{12}$CO rotational lines in protoplanetary discs are good tracers of
the total spatial extension of the gas component, and potentially planet-disc
interactions. We present ALMA long baseline observations of the $^{12}$CO(2-1)
line of ten protoplanetary discs from the Ophiuchus DIsc Survey Employing ALMA
(ODISEA) project, aiming to set constraints on the gas distribution of these
sources. The position angle of the gaseous disc can be inferred for five
sources using high-velocity channels, which trace the gas in the inner part of
the disc. We compare the high-velocity PAs to the orientations inferred from
the continuum, representative of the orientation over $\sim$ 53 to 256 au in
these resolved discs. We find a significant difference in orientation for DoAr
44, which is evidence of a tilted inner disc. Eight discs show evidence of gas
inside inner dust cavities or gaps, and the disc of ISO-Oph 196 is not detected
in $^{12}$CO(2-1), except for the compact signal located inside its dust
cavity. Our observations also point out a possible outflow in WLY 2-63.
