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The nature of the radio-quiet X-ray halo around the plerionic SNR G21.5-0.9is under debate. On the basis of spatial and spectral analysis of a largeChandra and XMM-Newton dataset of this source, we have developed aself-consistent scenario which explains all the observational features. Wefound that the halo is composed by diffuse extended emission due to dustscattering of X-rays from the plerion, by a bright limb which traces particleacceleration 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. Byapplying a model of interaction between the PWN, the SNR and supernovaenvironment, 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).

The nature of the X-ray halo of the plerion G21.5–0.9 unveiled by XMM-Newton and Chandra