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Aims. A census of molecular hydrogen flows across the entire Orion A giant molecular cloud is sought. With this paper we aim to associate each flow with its progenitor and associated molecular core, so that the characteristics of the outflows and outflow sources can be established. Methods. We present wide-field near-infrared images of Orion A, obtained with the Wide Field Camera, WFCAM, on the United Kingdom Infrared Telescope. Broad-band K and narrow-band H(2) 1-0S(1) images of a contiguous similar to 8 square degree region are compared to mid-IR photometry from the Spitzer Space Telescope and (sub) millimetre dust-continuum maps obtained with the MAMBO and SCUBA bolometer arrays. Using previously- published H(2) images, we also measured proper motions for H(2) features in 33 outflows, and use these data to help associate flows with existing sources and/or dust cores. Results. Together these data give a detailed picture of dynamical star formation across this extensive region. We increase the number of known H(2) outflows to 116. A total of 111 H(2) flows were observed with Spitzer; outflow sources are identified for 72 of them (12 more H(2) flows have tentative progenitors). The MAMBO 1200 mu m maps cover 97 H(2) flows; 57 of them (59%) are associated with Spitzer sources and either dust cores or extended 1200 mu m emission. The H(2) jets are widely distributed and randomly orientated. The jets do not appear to be orthogonal to large-scale filaments or even to the small-scale cores associated with the outflow sources (at least when traced with the 11 '' resolution of the 1200 mu m MAMBO observations). Moreover, H(2) jet lengths (L) and opening angles (theta) are not obviously correlated with indicators of outflow source age-source spectral index, alpha (measured from mid-IR photometry), or (sub) millimetre core flux. It seems clear that excitation requirements limit the usefulness of H(2) as a tracer of L and gamma (though jet position angles are well defined). Conclusions. We demonstrate that H(2) jet sources are predominantly protostellar sources with flat or positive mid-IR spectral indices, rather than disc-excess (or T Tauri) stars. Most protostars associated with molecular cores drive H(2) outflows; however, not all molecular cores are associated with protostars or H(2) jets. On statistical grounds, the H(2) jet phase may be marginally shorter than the protostellar phase, though it must be considerably (by an order of magnitude) shorter than the prestellar phase. In terms of range and mean value of alpha, H(2) jet sources are indistinguishable from protostars. The spread in alpha observed for both protostars and H(2) outflow sources is probably a function of inclination angle as much as source age. The few true protostars without H(2) jets are almost certainly more evolved than their H(2)-jet-driving counterparts, although these later stages of protostellar evolution (as the source transitions to being a "disc-excess" source) must be very brief, since a large fraction of protostars do drive H(2) flows. We also find that the protostars that power molecular outflows are no more (nor no less) clustered than protostars that do not. This suggests that the H(2) emission regions in jets and outflows from young stars weaken and fade very quickly, before the source evolves from protostar to pre-mainsequence star, and on time-scales much shorter than those associated with the T Tauri phase, the Herbig-Haro jet phase, and the dispersal of young stellar objects.

Observations of the 1.083-micron He I line in WR140 (HD 193793) show P-Cygni profiles which varied as the binary system went through periastron passage. A sub-peak appeared on the normally flat-topped emission component and then moved across the profile consistent with its formation in the wind-collision region. Variation of the absorption component provided constraints on the opening angle (theta) of the wind-collision region. Infrared (2-10 micron) images observed with a variety of instruments in 2001-04 resolve the dust cloud formed in 2001, and show it to be expanding at a constant rate. Owing to the high eccentricity of the binary orbit, the dust is spread around the orbital plane in a 'splash' and we compare the dust images with the orientation of the orbit., Comment: 5 pages, 6 figures, contribution to "Massive Stars in Interacting Binaries", eds. N. St-Louis and A. F. J. Moffat, ASP Conference Series