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The extended X-ray emission from 'the Cap' region located 11' (11.6 kpc)above the disk of the starburst galaxy M82 has been observed with Suzaku andXMM-Newton. Owing to the good energy resolution and the large collecting areaof the XIS on Suzaku, combined with similar properties of the EPIC instrumenton XMM-Newton, we have clearly detected K-shell emission lines from O VII, OVIII, Ne X, Mg XI, Mg XII and the Fe-L complex. Two optically-thin thermalplasma components are required to fit the observed X-ray spectra. We havedetermined the metal abundances of O, Ne, Mg, Si and Fe in this region for thefirst time. Their metal abundance ratios agree well with those of metal-poorstars and the model prediction of metals synthesized by type-II supernovae, butthey are not consistent with the metallicities of type-Ia supernovae. Thisresult is support for the idea that the origin of the metals in the Cap istype-II supernovae explosions occurring in the starburst regions in the M82galaxy. We discuss the possible contribution from sputtered dust grains to themetals in the Cap. An emission line consistent with the C VI transition of n=4to 1 at 0.459 keV is marginally detected, although it is not statisticallysignificant at the 99% confidence level; the presence of this line wouldsuggest charge-exchange processes in the Cap.Comment: 16 pages, 10 figuer

X-Ray Spectral Study of the Extended Emission, ‘the Cap’, Located 11.6 kpc above the Disk of M82