Volume 442, Number 2, November I 2005
|Page(s)||539 - 548|
|Section||Interstellar and circumstellar matter|
|Published online||07 October 2005|
The nature of the X-ray halo of the plerion G21.5–0.9 unveiled by XMM-Newton and Chandra
INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy e-mail: firstname.lastname@example.org
2 FOM – Institute for Plasma Physics Rijnhuizen, PO Box 1207, 3430 BE Nieuwegein, The Netherlands
3 School of Physics and Astronomy, The University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
4 Department of Astronomy, University of Virginia, PO Box 3818, Charlottesville, VA 22903, USA
5 INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
Accepted: 15 July 2005
The nature of the radio-quiet X-ray halo around the plerionic supernova remnant G21.5-0.9 is under debate. On the basis of spatial and spectral analysis of a large Chandra and XMM-Newton dataset of this source, we have developed a self-consistent scenario which explains all the observational features. We found that the halo is composed by diffuse extended emission due to dust scattering of X-rays from the plerion, by a bright limb which traces particle acceleration in the fast forward shock of the remnant, and by a bright spot (the “North Spur”) which may be a knot of ejecta in adiabatic expansion. By applying a model of interaction between the PWN, the remnant and the supernova environment, we argue that G21.5-0.9 progenitor may be of Type IIP or Ib/Ic, and that the remnant may be young (200–1000 yr).
Key words: ISM: supernova remnants / ISM: dust, extinction / X-rays: ISM / X-rays: individuals: G21.5-0.9 / stars: supernovae: general / radiation mechanisms: non-thermal
© ESO, 2005
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