| Issue |
A&A
Volume 565, May 2014
|
|
|---|---|---|
| Article Number | A63 | |
| Number of page(s) | 31 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361/201323167 | |
| Published online | 13 May 2014 | |
Online material
 |
Fig. 2a
Comparison of best-fitting model spectrum (red line) with re-normalized observation (black line) for the stars, HD 35912 (right), HD 35299 (middle), and HD 37042 (left), in the spectral range λλ 3940–4062 Å. Light colors mark regions that have been excluded from fitting due to the presence of features that are not (properly) included in our models. For the sake of clarity, only the strongest out of all lines that have been used in the analysis are labeled. The residuals χ are defined by the bracket in Eq. (2). |
| Open with DEXTER | |
 |
Fig. 2b
Same as Fig. 2a in the spectral range λλ 4060–4212 Å. |
| Open with DEXTER | |
 |
Fig. 2c
Same as Fig. 2a in the spectral range λλ 4210–4412 Å. |
| Open with DEXTER | |
 |
Fig. 2d
Same as Fig. 2a in the spectral range λλ 4410–4617 Å. |
| Open with DEXTER | |
 |
Fig. 2e
Same as Fig. 2a in the spectral range λλ 4615–4912 Å. |
| Open with DEXTER | |
 |
Fig. 2f
Same as Fig. 2a in the spectral range λλ 4910–5352 Å. |
| Open with DEXTER | |
 |
Fig. 2g
Same as Fig. 2a in the spectral range λλ 5350–5861 Å. Note the comparatively small ordinate scales. |
| Open with DEXTER | |
 |
Fig. 2h
Same as Fig. 2a in the spectral range λλ 5859–6427 Å. Strong contamination with telluric lines. |
| Open with DEXTER | |
 |
Fig. 2i
Same as Fig. 2a in the spectral range λλ 6425–6742 Å. Strong contamination with telluric lines. Nebula emission lines visible in HD 37042’s spectrum (left). |
| Open with DEXTER | |
 |
Fig. 3a
Comparison of best-fitting model spectrum (red line) with re-normalized observation (black line) for the objects, HD 119109 (right), HD 213420 (middle), and HD 75821 (left), in the spectral range λλ 3940–4062 Å. Light colors mark regions that have been excluded from the fitting due to the presence of features that are not (properly) included in our models. For the sake of clarity, only the strongest out of all lines that have been used in the analysis are labeled. Blue connection lines mark contributions of the secondary component. The residuals χ are defined by the bracket in Eq. (2). |
| Open with DEXTER | |
 |
Fig. 3b
Same as Fig. 3a in the spectral range λλ 4060–4212 Å. |
| Open with DEXTER | |
 |
Fig. 3c
Same as Fig. 3a in the spectral range λλ 4210–4412 Å. |
| Open with DEXTER | |
 |
Fig. 3d
Same as Fig. 3a in the spectral range λλ 4410–4617 Å. |
| Open with DEXTER | |
 |
Fig. 3e
Same as Fig. 3a in the spectral range λλ 4615–4912 Å. |
| Open with DEXTER | |
 |
Fig. 3f
Same as Fig. 3a in the spectral range λλ 4910–5352 Å. |
| Open with DEXTER | |
 |
Fig. 3g
Same as Fig. 3a in the spectral range λλ 5350–5861 Å. Note the comparatively small ordinate scales. |
| Open with DEXTER | |
 |
Fig. 3h
Same as Fig. 3a in the spectral range λλ 5859–6427 Å. Strong contamination with telluric lines. |
| Open with DEXTER | |
 |
Fig. 3i
Same as Fig. 3a in the spectral range λλ 6425–6742 Å. Strong contamination with telluric lines. |
| Open with DEXTER | |
© ESO, 2014
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