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Astron. Astrophys. 315, L277-L280 (1996)

Shockingly bright [OI] 63 tex2html_wrap_inline36m lines from the supernova remnants W44 and 3C391*

William T. Reach1, and Jeonghee Rho2

1 Institut d'Astrophysique Spatiale, Bât. 121, Université Paris XI, F-91405 Orsay Cedex, France
2 Service d'Astrophysique, CEA, DSM, DAPNIA, Centre d'Etudes de Saclay, F-91191 Gif-sur-Yvette Cedex, France

Received 4 July 1996 / Accepted 31 July 1996

Abstract. The brightness of the [OI] 63 img1.gifm line was measured for the supernova remnants W44 and 3C391 with the ISO\ Long-Wavelength Spectrometer. Bright lines, img2.gif erg cm-2 sr-1, were detected in the 20 positions observed toward both remnants. The lines are brightest at the edges of the remnants, but they are also bright towards the remnant interior. Continuum emission from collisionally-heated dust is detected, and the dust temperature is 50 K for 3C391. Comparison to theoretical models that predict the [OI] line brightness suggests pre-shock densities img5.gif cm-3 and ram pressures of order img7.gif dyne cm-2, as might occur for a supernova blast wave interacting with a molecular cloud.

Key words: ISM: supernova remnants - infrared: interstellar: lines - infrared: interstellar: continuum - ISM: individual objects: 3C391 - ISM: individual objects: W44

* Based on observations with the Infrared Space Observatory (ISO). ISO is an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA.

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Last change: December 16, 1996
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