Nature 311, 236 - 237 (20 September 1984); doi:10.1038/311236a0

Molecular hydrogen jets from the Orion nebula

K. N. R. Taylor^*, J. W. V. Storey^*, G. Sandell^†, P. M. Williams^‡ & W. J. Zealey^§

^*Optical Science and Technology, University of New South Wales, Kensington, 2033 Australia
^†Astrophysics Laboratory, University of Helsinki, Helsinki 13, Finland
^‡United Kingdom Infrared Telescope Unit, 900 Leilani Street, Hilo, Hawaii 96720, USA
^§Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK

The environs of interstellar space in which star formation takes place involve high-velocity gas flows. Channelled by embryonic dust toroids, these gas flows culminate in energy-losing shock processes at the interface with the ambient interstellar cloud. The excitation of molecular hydrogen transitions in this gas provides one means of observing these shocked regions and their relation to the well-known indicators of star formation such as the Herbig Haro objects and T Tauri stars. In an attempt to understand the relationship of the recently discovered complex of Herbig Haro objects in Orion¹ to the IR sources in this region, we have carried out a survey of the molecular hydrogen S(1) line distribution. These observations have led to the discovery of a previously unsuspected structure of finger-like filaments of H₂ emission extending radially outwards from a common centre at IRC9.

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