| Issue |
A&A
Volume 572, December 2014
|
|
|---|---|---|
| Article Number | A88 | |
| Number of page(s) | 28 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/201423919 | |
| Published online | 02 December 2014 | |
Online material
Appendix A: Tables
Abundance ratios for Arcturus (median S/N) determined by Van der Swaelmen et al. (2013) compared to our results for Arcturus obtained in the same way as for our Fornax sample.
Atmospheric parameters for α Cet and γ Sge in the Gaia benchmark sample (GBS) determined by Jofre et al. (2014) compared to our results obtained in the same way as for our Fornax sample.
Positional, photometric, and kinematic data for our targets.
Atmospheric parameters (derived from photometry) for stars in our sample.
Individual abundances for the RGB stars in our sample, listed together with their associated errors and the number of lines used in the analysis for a given element.
Appendix B: Figures
 |
Fig. B.1
Abundances ratios vs. Teff for RGB stars with –1.0 < [Fe/H] < –0.5 dex in our sample, in blue; and in the sample of Letarte et al. (2010), in cyan. We also show the values determined for Arcturus by Van der Swaelmen et al. (2013) in green; and by ourselves, using the same method as for our Fornax sample, in red. |
| Open with DEXTER | |
 |
Fig. B.2
Typical sample spectra for stars with different Teff (mem0704: 4330 K, rgb0522: 4220 K, mem0631: 4035 K, mem0604: 3730 K, mem0606: 3640 K) are shown to illustrate how molecular features change as a function of Teff. The spectra have been offset at arbitrary fluxes. The three coolest stars in this sample have similar, relatively high metallicities (–0.82, –0.74 and –0.62 dex) while the two hottest stars are metal-poor (–2.55 and –1.87 dex). |
| Open with DEXTER | |
© ESO, 2014
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