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The Vela supernova remnant (SNR) shows several ejecta fragments protrudingbeyond the forward shock (shrapnel). Recent studies have revealed high Siabundance in two shrapnel (A and G), located in opposite directions withrespect to the SNR center. This suggests the possible existence of a Si-richjet-counterjet structure. We analyzed an XMM-Newton observation of a brightclump, behind shrapnel G, which lies along the direction connecting A and G.The aim is to study the physical and chemical properties of this clump toascertain whether it is part of this putative jet-like structure. We producedbackground-corrected and adaptively-smoothed count-rate images and medianphoton energy maps, and performed a spatially resolved spectral analysis. Weidentified two structures with different physical properties. The first one isremarkably elongated along the direction connecting A and G. Its X-ray spectrumis much softer than that of the other two shrapnel, to the point of hinderingthe determination of the Si abundance, however its physical and chemicalproperties are consistent with those of shrapnel A and G. The second structure,running along the southeast-northwest direction, has a higher temperature andappears like a thin filament. By analyzing the ROSAT data, we have found thatthis filament is part of a very large and coherent structure that we identifiedin the western rim of the shell. We obtained a thorough description of the tailof Shrapnel G. In addition we discovered a coherent and very extended featurethat we interpret as a signature of an earlier interaction of the remnant withthe stellar wind of its progenitor star. The peculiar Ne/O ratio we found inthe wind residual may be suggestive of a Wolf-Rayet progenitor for Vela SNR,though further analysis is required to address this point.

X-ray emitting structures in the Vela SNR: ejecta anisotropies and progenitor stellar wind residuals