EDP Sciences
Free Access
Issue
A&A
Volume 541, May 2012
Article Number A45
Number of page(s) 19
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201118636
Published online 26 April 2012

Online material

Appendix A: Comparison between MOOG and CALRAI abundances

The abundances of Mn that were uncorrected for the HFS were computed with both codes calrai and moog for the same atmosphere models. Therefore, it is possible to compare the results and check the consistency between the two codes.

For Fornax, the raw (i.e. uncorrected for HFS) Mn abundances given by the two codes prove to be perfectly consistent (Fig. A.1).

thumbnail Fig. A.1

Comparison between the Mn abundances (not corrected for HFS) obtained for the Fornax dSph galaxy using the moog code, and the ones obtained using the calrai code, for each of the 4 lines Mn iλ5407, λ5420, λ5432, and λ5516. In both cases, the abundances were determined using spherical atmosphere models.

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For Sculptor, however, there is a systematic shift of about 0.1 to 0.2 dex, in the sense that the moog abundances are lower than the calrai ones for all four lines. The slopes are very close to 1, but tend to be slightly above unity.

The reason why the systematic zero-point shift is much larger in Sculptor than Fornax lies in the atmosphere models used. While spherical models were used in connection with the moog spectral synthesis code for both galaxies, plane-parallel models were used in connection with the calrai code in the case of Sculptor, leading to the overestimated abundances seen in Fig. A.2.

thumbnail Fig. A.2

Same as Fig. A.1, but for the Sculptor dSph galaxy. Here the calrai abundances were determined using plane-parallel atmosphere models, while the moog abundances are based on spherical models.

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Table A.1

Equivalent widths, HFS corrections (labeled “HFS” on top of the respective columns), and Mn abundance for the Mn i λ5407 and λ5420 lines observed for the stars of the Fornax dSph galaxy.

Table A.2

Equivalent widths, HFS corrections (labeled “HFS” on top of the respective columns), and Mn abundance for the Mn i λ5432 and λ5516 lines observed for the stars of the Fornax dSph galaxy.

Table A.3

Equivalent widths, HFS corrections (labeled “HFS” on top of the respective columns), and Mn abundance for the Mn i λ5407 and λ5420 lines observed for the stars of the Sculptor dSph galaxy.

Table A.4

Equivalent widths, HFS corrections (labeled “HFS” on top of the respective columns), and Mn abundance for the Mn i λ5432 and λ5516 lines observed for the stars of the Sculptor dSph galaxy.

Table A.5

Equivalent widths, HFS corrections (labeled “HFS” on top of the respective columns), and Mn abundance for the Mn i λ5407, λ5420, λ5432, and λ5516 lines observed for the stars of the Sextans dSph galaxy.

Table A.6

Equivalent widths, HFS corrections (labeled “HFS” on top of the respective columns), and Mn abundance for the Mn i λ5407, λ5420, λ5432, and λ5516 lines observed for the stars of the Carina dSph galaxy.


© ESO, 2012

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