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Fig. 2.


Left: XMM-Newton pn (black), MOS1 (red), and MOS2 (green) X-ray spectra of T CrB data with the best spectral model (solid line) and the contribution of each model’s component (dotted lines). The model consists of a blackbody plus an optically thin cooling-flow and a Gaussian profile centered at the Fe Kα energy of 6.4 keV. All components are absorbed by interstellar and local, partial covering absorption (see Table 1 for resulting parameters). Right: alternative model, with a soft blackbody, a hard thermal plasma component, and a medium energy optically thin thermal component to take into account photons in the ~0.6–3 keV region. The soft optically thick and medium energy, optically thin components are modified by mostly interstellar absorption, while the hard, cooling flow is also affected by a partial covering absorber. Both bottom panels show the fit residuals in units of .

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