The Collimated Wind in NGC 253

Details The Collimated Wind in NGC 253 The Collimated Wind in NGC 253

2003-02-04

arxiv.org/abs/astro-ph/0302050v1

Astrophys.J. 584 (2003) L9-L12

Astronomy and Astrophysics

Astrophysics

12 pages, 6 figures, ApJL in press (February 10th 2003)

Scientific paper

10.1086/368271

Near-infrared Fabry-Perot imaging has revealed H2 emission extended to about 130 pc from the disk of NGC 253. It is closely related to the hot plasma observed in soft X-rays: filamentary H2 features are found at the edges of the hot plasma. These are the places of direct interaction between a superwind and its surrounding molecular gas. We suggest that the filamentary features actually trace a more or less conical shell-like structure, whose tangential line of sight to us is intensely observed. The H2 emission shell is most likely from the molecular gas blown out or swept to the side by the hot plasma outflow. Dust is associated with this molecular gas structure. The outflow is tilted with respect to the disk, possibly suggesting the inhomogeneous nature of the interstellar medium in which the starburst takes place.

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