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We report results from the analysis of XMM-Newton and INTEGRAL data of IGRJ16479-4514. The unpublished XMM-Newton observation, performed in 2012,occurred during the source eclipse. No point-like X-ray emission was detectedfrom the source, conversely extended X-ray emission was clearly detected up toa size distance compatible with a dust scattering halo produced by the sourceX-ray emission before being eclipsed by its companion donor star. The diffuseemission of the dust-scattering halo could be observed without anycontamination from the central point X-ray source, compared to a previousXMM-Newton observation published in 2008. Our comprehensive analysis of the2012 unpublished spectrum of the diffuse emission as well as of the 2008re-analysed spectra extracted from three adjacent time intervals and differentextraction regions (optimized for point-like and extended emission) allowed usto clearly disentangle the scattering halo spectrum from the residualpoint-like emission during the 2008 eclipse. Moreover, the point-like emissiondetected in 2008 could be separated into two components attributed to thedirect emission from the source and to scattering in the stellar wind,respectively. From archival unpublished INTEGRAL data, we identified a verystrong (3$\times$10$^{-8}$ erg cm$^{-2}$ s$^{-1}$) and fast (25 minutesduration) flare which was classified as giant hard X-ray flare since themeasured peak-luminosity is 7$\times$10$^{37}$ erg s$^{-1}$. Giant X-ray flaresfrom SFXTs are very rare, to date only one has been reported from a differentsource. We propose a physical scenario to explain the origin in the case of IGRJ16479-4514.

Dust-scattering halo and giant hard X-ray flare from the Supergiant Fast X-ray Transient IGR J16479-4514 investigated with XMM-Newton and INTEGRAL