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Recent XMM-Newton observations of the black-hole candidate 4U 1630-47 duringthe 2012 outburst revealed three relativistically Doppler-shifted emissionlines that were interpreted as arising from baryonic matter in the jet of thissource. Here we reanalyse those data and find an alternative model that, withless free parameters than the model with Doppler-shifted emission lines, fitsthe data well. In our model we allow the abundance of S and Fe in theinterstellar material along the line of sight to the source to be non solar.Among other things, this significantly impacts the emission predicted by themodel at around 7.1 keV, where the edge of neutral Fe appears, and renders thelines unnecessary. The fits to all the 2012 XMM-Newton observations of thissource require a moderately broad emission line at around 7 keV plus severalabsorption lines and edges due to highly ionised Fe and Ni, which reveal thepresence of a highly-ionised absorber close to the source. Finally, our modelalso fits well the observations in which the lines were detected when we applythe most recent calibration files, whereas the model with the threeDoppler-shifted emission lines does not.

The XMM Newton spectra of the 2012 outburst of the black-hole candidate 4U 1630-47 revisited