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	Figure 1: The scattering cross section, calculated using the Mie theory, at specific scattering angles vs. energy for Mg2SiO4. A single grain size of m is considered.
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In the text

	Figure 2: Comparison between model 1 ( top), and model 2 ( bottom) used to fit the oxygen region, using the RGS data. Model 1 includes three absorption edges and two absorption lines. Model 2 includes one absorption edge and four absorption lines.
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In the text

	Figure 3: ISM absorption edges predicted for using the best EPIC-pn best fit model, evaluated from the OOT events data. Mg (1.3 keV) and Si (1.84 keV) are only marginally evident in the model.
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In the text

Figure 4: EPIC-pn image of Cyg X-2 in the 0.5-3 keV band. The solid line annuli show three of the extraction regions specific for the halo spectral analysis (Fig. 7). The circles are drawn at 3.3, 4.3, 5.3, 6.3 arcmin. The dashed line annulus is the background. These regions were cut by the green rectangle across the detector (see Sect. 4.2). For the halo spatial analysis (Sect. 4.1) the annuli were instead logarithmically spaced. The barred regions were excluded from the data analysis: pile-up region (circle in the center), OOT events (box), and the serendipitous sources (points).

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In the text

	Figure 5: Ratio between single events and all events (upper dash-dotted curve) and ratio between double and all events (lower solid curve), for EPIC-pn, around 0.75 keV. The dotted lines represent the values expected in absence of pile-up.
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In the text

	Figure 6: Comparison between the PSF-model (solid line), Mrk 421 (asterisks) between 0.9 and 1 keV. For radii smaller than 30 , the flatness of the profile is mainly due to the mask used in the observation. The counts in this region are non zero due to a slight misalignment of the mask with respect to the source coordinates in this particular observation.
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In the text

Figure 7: The ratio between the halo spectra and the central source spectrum. At this stage the data are still convolved with the PSF. The spectra were extracted from annuli -  from top to bottom - centered at 3.8, 4.8, and 5.8 arcmin respectively (Fig. 4). At larger radii the PSF contribution becomes less important. Dashed vertical lines: energies of relevant ID elements (O, Fe, Mg, Si). Error bars are 68% confidence level (1). The vertical axis units are arbitrary as the absolute flux of the source could not be recovered from the OOT events (Sect. 3.1).

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In the text

	Figure 8: XMM EPIC-pn pure-scattering mirror spectrum at a radius 180 from the source, extracted from the halo-free source Mrk 421. We note a smooth increase of the scattering above 2 keV for larger radii.
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In the text

	Figure 9: The data (halo+PSF) (asterisks) compared to the PSF (dotted line) around 1 keV. The dashed and the solid thin lines are two different halo models (MRN and W01), while the solid and dashed thick lines indicate the best-fit to the total data (model+PSF) relative to MRN and WD01, respectively.
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In the text

	Figure 10: The scattering optical depth as a function of energy, as measured from the SBP of Cyg X-2 halo for the MRN model (filled squares) and WD01 (empty squares). The data were collected in energy bins 0.25 keV wide. The solid line refers to the value of the total at the center of the bin, as predicted in D03.
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In the text

	Figure 11: EPIC-pn data of the Cyg X-2 halo, extracted at 4.8 from the source and PSF subtracted (asterisks), compared with the best-fit models: WD01 (dashed dotted line), MRN (solid line), and D03+WD01 model (diamonds). O-K, Mg-K, and Si-K edge energies are indicated by dotted lines.
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In the text

	Figure 12: Relative contributions to the best-fit model, using the MRN distribution. The data are the same as in Fig. 11.
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In the text