CO outflows from young stars: Confronting the jet and wind models

We have mapped the CO J = 1-0 emission from molecular outflows associated w ith five young stellar systems of class 0 to class II/III using the BIMA ar ray and the FCRAO 14 m antenna. The systems, VLA 05487, HH 212, HH 240/241, HH 111, and RNO 91, are all relatively nearby and of low luminosity, and t he majority have H-2 emission or optical jet features. The CO outflow gener ally forms a shell structure around the outflow axis with the higher veloci ty emission further out from the source. Two distinctive kinematic features are evident in position-velocity (PV) diagrams: a parabolic structure orig inating at the driving source (e.g., VLA 05487 and HH 111) and a convex spu r structure with the high-velocity tip near known H-2 bow shocks (e.g., HH 212, HH 240/241 and HH 111). The parabolic PV structure can be produced by a wide-angle-wind model, while the velocity spur structure can be modeled w ith a jet-driven bow shock model. VLA 05487, which is not associated with a ny H-2 bow shocks, shows only the parabolic structure and kinematics consis tent with the wide-angle wind-driven model. HH 212, which is associated wit h a series of H-2 bow shock structures, shows a striking morphological coin cidence between the H-2 and CO emission and velocity spurs in the PV diagra m. It is our best example of the jet-driven bow shock model, and its kinema tics can be qualitatively explained in that context. HH 240/241 is similar to HH 212 and shows a close relationship between the H-2 and CO emission. T he kinematics of its western lobe can also be explained with the jet-driven model. The kinematics of RNO 91 are similar to VLA 05487 and are broadly c onsistent with a wide-angle wind-driven model. HH 111 has both parabolic an d spur PV structures, a combination that is not easily explained in the sim plest version of either model. Thus, these observations provide examples of systems that support either th e wide-angle wind-driven or jet-driven model in the simplest interpretation . More detailed calculations are needed to understand whether one model mig ht be able to fit all systems. It is crucial to know if time-dependent or l ong-lived jet-driven bow shock models can produce the observed outflow widt hs and parabolic PV structures, or if a wide-angle wind can produce the sho ck features and velocity spur structures in our observations.