To be published in:
Astronomy & Astrophysics
XMM-Newton observations of the giant HII region N11 in the LMC.
E. Gosset1,*** and
1 Institut d'Astrophysique et de Géophysique - Université de Liège, Allée du 6 Août, Bât B5c, B-4000 Liège (Sart Tilman), Belgium
2 Astronomy and Astrophysics Group; Department of Physics and Astronomy; Kelvin Building, University of Glasgow; Glasgow G12 8QQ; United Kingdom
3 Astronomy Department, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, IL 61801, USA
* Research Fellow FNRS, Belgium
** On leave from Sternberg Astronomical Institute, Moscow University, Russia
** Research Associate FNRS, Belgium
+ Based on observations collected with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).
Using the sensitive XMM-Newton observatory, we have observed the
giant HII region N11 in the LMC for ~30ks. We have detected several large
areas of soft diffuse X-ray emission along with 37 point sources. One of
the most interesting results is the possible association of a faint X-ray
source with BSDL 188, a small extended object of uncertain nature.
ISM: individual objects: LMC N11 - Magellanic Clouds -
Galaxies: star clusters - Ultraviolet: stars - X-rays: general
The OB associations in the field-of-view (LH9, LH10 and LH13) are all
detected with XMM-Newton, but they appear very different from one
another. The diffuse soft X-ray emission associated with LH9 peaks near
HD 32228, a dense cluster of massive stars. The combined emission of all
individual massive stars of LH9 and of the superbubble they have created is
not sufficient to explain the high level of emission observed: hidden SNRs,
colliding-wind binaries and the numerous pre-main sequence stars of the
cluster are most likely the cause of this discrepancy. The superbubble may
also be leaking some hot gas in the ISM since faint, soft emission can be
observed to the south of the cluster. The X-ray emission from LH10 consists
of three pointlike sources and a soft extended emission of low intensity.
The two brightest point sources are clearly associated with the fastest
expanding bubbles blown by hot stars in the SW part of the cluster. The
total X-ray emission from LH10 is rather soft, although it presents a higher
temperature than the other soft emissions of the field. The discrepancy
between the combined emission of the stars and the observed luminosity is
here less severe than for LH9 and could be explained in terms of hot gas
filling the wind-blown bubbles. On the other hand, the case of LH13 is
different: it does not harbour any extended emission and its X-ray emission
could most probably be explained by the Sk -66°41 cluster alone.
Finally, our XMM-Newton observation included simultaneous observations
with the OM camera that provide us with unique UV photometry of more than
6000 sources and enable the discovery of the UV emission from the SNR N11L.