Issue |
A&A
Volume 508, Number 1, December II 2009
|
|
---|---|---|
Page(s) | 401 - 408 | |
Section | Stellar atmospheres | |
DOI | https://doi.org/10.1051/0004-6361/200912518 | |
Published online | 15 October 2009 |
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
|
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.
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