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Figure 1: UVES 2006 spectrum of the oxygen triplet  7771-5 ( top), the O I  8446 line ( middle), and the region around 8700 Å, containing many lines of the -elements. We have indicated the major constituents of the line blends, plotting the -element indicators and identifications below those of the other elements. The overabundance of oxygen is obvious, while the abundances of the other -elements are comparable with the abundances in HD 156098 (solid line). These three regions correspond almost exactly to the plots of the 1998 Keck-HIRES spectrum (Israelian et al. 1999, Fig. 1), with a few modifications due to UVES inter-order gaps.

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In the text

Figure 2: One of the single UVES 2006 spectrum of GRO J1655-40 (symbols) with the F6IV broadened stellar template of HD 156098 (solid line). Also plotted are two model spectra with [Mg/Fe] = 0.0 (dotted line) and [Mg/Fe] = 0.5 (dot-dashed line). The apparent wavelength shift is caused by the blending of several lines with the magnesium ones. It has however no influence on Mg abundances. Below are plotted the residuals after subtracting the HD 156098 template spectrum from the GRO J1655-40 spectrum.

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In the text

Figure 3: UVES 2006 spectrum of GRO J1655-40 (symbols) with the F6IV broadened stellar template of HD 156098 (lower continuous line) in the region of the S I triplet. The upper continuous line show the same stellar template, but on which the difference between two acceptable normalizations of the GRO J1655-40 spectrum has been applied. It shows the amplitude of uncertainties in the continuum level in this region, and that in both cases HD 156098 is a providing a good match. Below are plotted the residuals after subtracting the HD 156098 spectrum from the best-fitting GRO J1655-40 spectrum.

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In the text