A&A 365, L242-L247 (2001)
High-resolution X-ray spectroscopy and imaging of supernova remnant N132DE. Behar1, A. P. Rasmussen1, R. G. Griffiths2, K. Dennerl3, M. Audard4, B. Aschenbach3 and A. C. Brinkman5.
1 Columbia Astrophysics Laboratory, 550 West 120th Street, New York, NY 10027, USA
2 X-Ray Astronomy Group, Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UK
3 Max-Planck-Institut für Extraterrestrische Physik, 85740 Garching, Germany
4 Laboratory for Astrophysics, Paul Scherrer Institute, Würenlingen and Villigen, 5232 Villigen PSI, Switzerland
5 Space Research Organization of the Netherlands, Sorbonnelaan 2, 3548 CA, Utrecht, The Netherlands
(Received 2 October 2000 / Accepted 30 October 2000)
The observation of the supernova remnant N132D by the scientific instruments on board the XMM-Newton satellite is presented. The X-rays from N132D are dispersed into a detailed line-rich spectrum using the Reflection Grating Spectrometers. Spectral lines of C, N, O, Ne, Mg, Si, S, and Fe are identified. Images of the remnant, in narrow wavelength bands, produced by the European Photon Imaging Cameras reveal a complex spatial structure of the ionic distribution. While K-shell Fe emission seems to originate near the centre, all of the other ions are observed along the shell. A high O6+/O7+ emission ratio is detected on the northeastern edge of the remnant. This can be a sign of hot ionising conditions, or it can reflect relatively cool gas. Spectral fitting of the CCD spectrum suggests high temperatures in this region, but a detailed analysis of the atomic processes involved in producing the O6+ spectral lines leads to the conclusion that the intensities of these lines alone cannot provide a conclusive distinction between the two scenarios.
Key words: atomic processes -line: formation -line: identification -techniques: spectroscopic -supernovae: individual: N132D -ISM: supernova remnants
Offprint request: E. Behar, firstname.lastname@example.org
© ESO 2001