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Feedback of massive stars on the ISM: a XMM-Newton view of the LMC superbubble N 51D

Published online by Cambridge University Press:  26 May 2016

Dominik J. Bomans ,
Jörn Rossa ,
Kerstin Weis  and
Konrad Dennerl
Dominik J. Bomans
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Universitätsstraße 150/NA7, D-44780 Bochum, BRD
Jörn Rossa
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Universitätsstraße 150/NA7, D-44780 Bochum, BRD
Kerstin Weis
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, BRD
Konrad Dennerl
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching-bei-München, BRD

Abstract

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N 51D (= DEM L 192) appears at first glance as a nearly circular, 120 pc diameter bubble of ionized gas around the LMC OB association LH 54. A deeper look reveals a complex web of filaments and deviations from radial expansion. Using a deep XMM-Newton pointing centered on N 51D we find that diffuse soft X-ray emitting gas fills the whole superbubble as delineated by the Hα filaments. Contrary to recent findings for galactic winds, the correlation between Hα and X-ray surface brightness is not good. The X-ray spectrum of this diffuse gas cannot be fitted with the LMC abundance pattern, but implies an overabundance of at least oxygen and neon, consistent with recent enrichment from supernovae Type II. Some indications for enhanced mixing at the brightest region of the Hα shell and for a beginning outflow of the hot gas were also detected.

Type
Part 4. Feedback from Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 637 - 641
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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