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Astron. Astrophys. 324, L45-L48

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Letter to the Editor

BeppoSAX LECS/MECS X-ray spectroscopy
of the young supernova remnant N132D

F. Favata1, J. Vink2, and A. N. Parmar1 J. S. Kaastra2, and T. Mineo3

1Astrophysics Division - ESA/ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands
2Space Research Organization Netherlands, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands
3Istituto di Fisica Cosmica ed Applicazioni Informatiche, CNR, Via U. La Malfa 153, I-90146 Palermo, Italy

Received 13 May 1997 / Accepted 27 May 1997


We have analyzed an observation of the supernova remnant N132D in the Large Magellanic Cloud, performed with the Low Energy Concentrator Spectrometer (LECS) and the Medium Energy Concentrator Spectrometer (MECS) instruments on board the X-ray satellite BeppoSAX. Thanks to the good sensitivity of the LECS/MECS combination over the range 0.3-8.5 keV we were able to detect the presence of an additional hotter plasma with respect to what had been previously assumed for this remnant. This hotter component is the source of the Fe-K line emission visible in the spectrum. Using a two component NEI plasma model we find that the best fitting abundance values indicate that N132D is also O-rich from the X-ray point of view. We briefly discuss the origin of the hot component and tentatively associate it with a radio bright region.

Key words: ISM: abundances; ISM: individual objects: N132D: ISM: supernova remnants: X-rays: ISM

Send offprint requests to: F. Favata (fabio.favata@astro.estec.esa.nl)

© European Southern Observatory (ESO) 1997