Abstract
Abstract We have extended the membership and determined the 3D structure of the large (0.19 pc) HH 269 sequence of shocks in the Orion Nebula. All of the components lie along a track that is highly tilted to the plane of the sky and emerge from within the Orion-S embedded molecular cloud. Their source is probably either the highly obscured mm 9 source associated with a high N2H+ density core (more likely) or the more distant star COUP 632 (less likely). The former must be located in the photon dominated region (PDR) underlying the ionized surface of the Orion-S Cloud, while the latter would be embedded within the Orion-S Cloud. The flows seem to be episodic, with intervals of 1900–2600 yr or 700–2600 yr if COUP 632 is the source.
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