Outflow sources in the Vela region

We have observed (CO)-C-12(1-0), (CO)-C-13(1-0), (CO)-O-18(1-0), and CS(2-1 ) towards nine sources in the Vela region for which the (CO)-C-12(1-0) spec tra by Wouterloot & Brand (1989) suggested the presence of strong line wing s (towards two of those sources only CS or (CO)-C-12 and (CO)-C-13 were obs erved). The sources are located in or behind the Vela Molecular Ridge at di stances between about 0.6 and 6.7 kpc. In all transitions we made small map s, typically several arcminutes in size. Towards five sources the (CO)-C-12 emission is confused by unrelated compon ents at other velocities (not visible in CS and (CO)-O-18) which we subtrac ted from the line profiles before analysing the wing emission. The presence of outflow emission was studied by also subtracting the contribution of a central Gaussian line component. We conclude that of the eight sources obse rved in CO, seven show outflows, one does not. For one of the sources only the blue wing could be studied due to the confusing presence of other stron g line components. For the outflow sources we derive the physical parameter s. Wing emission has a relative outflow velocity up to about 16 kms(-1), bu t the average (weighted with line intensity) is about 4 kms(-1). Masses of the outflows range from 1 to 150 M-circle dot. CS and (CO)-O-18 Were detected towards all eight (resp. seven) sources obse rved in these molecules. Five sources show single clumps in both transition s, two sources show several clumps in one of the transitions (the other was not mapped completely) and one source shows only weak emission (probably d ue to its distance). Clump masses and radii range from several 10 M-circle dot to about 1000 M-circle dot and 0.2 pc to 2 pc. Five of the sources show a velocity gradient in CS and (CO)-O-18 indicative of rotation.