Online Material

Appendix A: The Balmer lines of HR 6000 observed on the UVES spectra

Figure A.1 shows the UVES spectra of HR 6000 reduced by the UVES pipeline Data Reduction Software (version 2.5, Ballester et al. 2000) that were used by Castelli & Hubrig (2007) and also in this paper. All spectra are FLUXCAL_-SCIENCE products. Those at 3290-4520 Å and 4780-5650 Å are flux-calibrated spectra in 10^-16 erg s^-1 cm^-2 A^-1 corrected for terrestrial extinction. The red spectrum at 5730-7560 Å is in non-physical units ``quasi-ADU'' because the flux calibration procedure is not implemented in the reduction software for the REDL and REDU data taken with the red mosaic CCD's. The sizable distortions in UVES spectra make the difficulty in drawing a true continuum over H and H evident. The use of H also causes problems because of the position of this line at the left end of the spectrum order. Only H does not have significant problems.

Computed spectra from the final ATLAS12 model ([13450, 4.3], Sect. 2.2) are also plotted in Fig. A.1 to show the different slopes of the observed and computed continua. The computed fluxes were scaled by a given arbitrary quantity to be roughly overimposed on the UVES spectra.

	Figure A.1: The observed UVES spectra of HR 6000 (black line) are plotted together the computed spectra (red line) in order to show the different slopes of the observed and computed continua. The computed fluxes are scaled by a given arbitrary quantity to be roughly overimposed on the UVES spectra. The ATLAS12 final model with parameters  = 13450 K,  = 4.3 was used for the computations.
Open with DEXTER

Appendix B: Lines used for the abundance analysis

Table B.1 lists the lines examined in the spectra of HR 6000 and 46 Aql to derive the stellar abundances. The wording ``not obs'' is given for lines not present in the spectra, while the wordings ``profile'' and ``blend'' are given for lines well observed in the spectra that do not have measurable equivalent widths either because they are too weak to be measurable or because other components affects the line. These wordings also indicate lines for which adequate equivalent widths cannot be computed, as in the cases of Mg II at 4481 Å and most O I lines, which are blends of transitions belonging to the same multiplet. The abundances from the final ATLAS12 models derived from the equivalent widths or from the profiles are given in the table, as well as upper abundance limits for lines not observed, but predicted at solar abundance by the synthetic spectrum. For Fe I and Fe II, -values were taken from Fuhr & Wiese (2006) (FW06) when available. Otherwise Kurucz's last determination was adopted (Kurucz 2009), except for Fe II at 5257.119 Å. In this case, the previous values (Kurucz 2007) produce synthetic profiles in closer agreement with the observations.

Table B.1:   Analyzed lines in the stellar spectra, measured equivalent widths in mÅ, and relative abundances.He I is not included.

Table 4:   Astrophysical -values for a sample of (⁵D)4d-(⁵D)4f lines of Fe II observed in HR 6000 and 46 Aql. The values of from the two stars are averaged and compared with experimental -values from Johansson (2002) and calculated -values from Kurucz (2009) (K09) (footnote 7) and from Raassen & Uylings (1998) (RU98).

Table 5:   Lines due to (³H)4d-(³H)4f transitions of Fe II.

Table 6:   More new Fe II identified lines.