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Free Access
Issue
A&A
Volume 539, March 2012
Article Number A143
Number of page(s) 57
Section Stellar atmospheres
DOI https://doi.org/10.1051/0004-6361/201118158
Published online 07 March 2012

Online material

thumbnail Fig. 4

Comparison between synthetic fluxes based on Teff and log g values from multiple ionization equilibria to observed spectral energy distributions for the sample stars with available IUE data. Displayed are wavelength-weighted fluxes λFλ from the far-UV to the near-IR in the K-band. Observations consist of IUE spectra (black lines), Johnson UBVRIJHK photometry (boxes) and 2MASS JHK photometry (circles). Model fluxes are indicated by red lines. The observations have been dereddened adopting colour excesses as indicated and the model fluxes have been normalised with respect to the observations in V. Some fluxes have been scaled for clarity, as indicated.

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thumbnail Fig. 7

Metal abundances as a function of effective temperature (left) and of surface gravity (right). Sample stars from the present work are indicated by dots, data from NS11 by open circles. Error bars are statistical 1σ-uncertainties. Average abundances from the combined samples are indicated by the dashed line, the dotted lines delineate the 1σ-scatter around the average value. See Sect. 5.2 for a discussion.

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thumbnail Fig. 8a

Comparison between global synthetic and observed spectrum for the B3 III-type star #15 = 18 Peg (Teff = 15 800 K) in the spectral range λλ 3900–4500 Å. See Sect. 5.3 for details.

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thumbnail Fig. 8b

Same as Fig. 8a in the spectral range λλ 4500–5100 Å.

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thumbnail Fig. 8c

Same as Fig. 8a in the spectral range λλ 5100–5700 Å.

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thumbnail Fig. 8d

Same as Fig. 8a in the spectral range λλ 5700–6300 Å.

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thumbnail Fig. 8e

Same as Fig. 8a in the spectral range λλ 6300–6880 Å.

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thumbnail Fig. 9a

Comparison between global synthetic and observed spectrum for the B2 IV-type star #7 =γ Peg (Teff = 22 000 K) in the spectral range λλ 3900–4500 Å. See Sect. 5.3 for details.

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thumbnail Fig. 9b

Same as Fig. 9a in the spectral range λλ 4500–5100 Å.

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thumbnail Fig. 9c

Same as Fig. 9a in the spectral range λλ 5100–5700 Å.

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thumbnail Fig. 9d

Same as Fig. 9a in the spectral range λλ 5700–6300 Å.

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thumbnail Fig. 9e

Same as Fig. 9a in the spectral range λλ 6300–6880 Å.

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thumbnail Fig. 10a

Comparison between global synthetic and observed spectrum for the B1 V-type star #1= HR 1861 (Teff = 27 000 K) in the spectral range λλ 3900–4500 Å. See Sect. 5.3 for details.

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thumbnail Fig. 10b

Same as Fig. 10a in the spectral range λλ 4500–5100 Å.

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thumbnail Fig. 10c

Same as Fig. 10a in the spectral range λλ 5100–5700 Å.

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thumbnail Fig. 10d

Same as Fig. 10a in the spectral range λλ 5700–6300 Å.

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thumbnail Fig. 10e

Same as Fig. 10a in the spectral range λλ 6300–6880 Å.

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thumbnail Fig. 11a

Comparison between global synthetic and observed spectrum for the B0.2 V-type star #6 = τ Sco (Teff = 32 000 K) in the spectral range λλ 3900–4500 Å. See Sect. 5.3 for details.

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thumbnail Fig. 11b

Same as Fig. 11a in the spectral range λλ 4500–5100 Å.

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thumbnail Fig. 11c

Same as Fig. 11a in the spectral range λλ 5100–5700 Å.

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thumbnail Fig. 11d

Same as Fig. 11a in the spectral range λλ 5700–6300 Å.

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thumbnail Fig. 11e

Same as Fig. 11a in the spectral range λλ 6300–6880 Å.

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Table 7

Spectral line analysis of the program stars.

Table 8

Example of abundance changes caused by atmospheric parameter variations for HD 886.


© ESO, 2012

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