Table 2
Stellar parameters and main results obtained from ISIS spectra.
| Star | Teff | log g | ξ | [Fe/H] SYNTHE | E WCaIIK | A(Ca)MOOG | A(Ca)SYNTHE | A(C)SYNTHE | ||||
| [K] | [cm s-2] | [ km s-1] | [Å] | |||||||||
|
|
||||||||||||
| SDSS J010505+461521 | 5480 | 1.9 | 2.0 | −3.7 ± 0.2 | 1.2 ± 0.1 | 3.1 ± 0.4 | 3.0 ± 0.2 | − | ||||
| SDSS J014036+234458 | 6090 | 4.7 | 2.0 | −3.6 ± 0.2 | 0.7 ± 0.1 | 3.0 ± 0.4 | 3.2 ± 0.2 | 5.9 ± 0.4 | ||||
| SDSS J021958−084955 | 5700 | 4.0 | 2.0 | −3.6 ± 0.2 | 1.3 ± 0.1 | 3.2 ± 0.4 | 3.2 ± 0.2 | < 5.6 | ||||
| SDSS J040114−051259 | 5850 | 5.0 | 2.0 | −3.6 ± 0.2 | 1.0 ± 0.1 | 3.0 ± 0.4 | 3.2 ± 0.2 | − | ||||
| SDSS J044655+113741 | 5970 | 2.9 | 2.0 | −3.2 ± 0.2 | 0.9 ± 0.1 | 3.3 ± 0.4 | 3.6 ± 0.2 | − | ||||
| SDSS J063055+255243 | 5410 | 1.9 | 2.0 | −3.6 ± 0.2 | 1.4 ± 0.1 | 3.0 ± 0.4 | 3.2 ± 0.2 | − | ||||
| SDSS J075818+653906 | 6080 | 3.9 | 2.0 | −3.0 ± 0.2 | 1.2 ± 0.1 | 3.5 ± 0.4 | 3.8 ± 0.2 | − | ||||
| SDSS J101600+172901 | 5420 | 4.9 | 2.0 | −3.5 ± 0.2 | 2.1 ± 0.1 | 3.1 ± 0.4 | 3.3 ± 0.2 | 5.1 ± 0.2 | ||||
| SDSS J120441+120111 | 5850 | 3.9 | 2.0 | −3.7 ± 0.2 | 1.0 ± 0.1 | 2.9 ± 0.4 | 3.1 ± 0.2 | − | ||||
| SDSS J123055+000547 | 6200 | 4.2 | 2.0 | −3.4 ± 0.2 | 0.9 ± 0.1 | 3.3 ± 0.4 | 3.4 ± 0.2 | < 5.8 | ||||
| SDSS J132250+012343 | 5250 | 2.0 | 2.0 | −3.7 ± 0.2 | 1.7 ± 0.1 | 3.2 ± 0.4 | 3.1 ± 0.2 | − | ||||
| SDSS J164234+443004 | 6280 | 5.0 | 2.0 | −4.0 ± 0.2 | 0.5 ± 0.1 | 2.8 ± 0.4 | 2.8 ± 0.2 | − | ||||
| SDSS J165618+342523 | 5010 | 2.1 | 2.0 | −3.3 ± 0.2 | 2.7 ± 0.1 | 3.3 ± 0.4 | 3.5 ± 0.2 | 5.2 ± 0.2 | ||||
| SDSS J183455+421328 | 5370 | 4.9 | 2.0 | −3.8 ± 0.2 | 1.5 ± 0.1 | 2.8 ± 0.4 | 2.9 ± 0.2 | − | ||||
| SDSS J214633−003910 | 6470 | 4.9 | 2.0 | −3.6 ± 0.2 | 0.7 ± 0.1 | 3.2 ± 0.4 | 3.2 ± 0.2 | − | ||||
| SDSS J220646−092545 | 4980 | 1.9 | 2.0 | −3.0 ± 0.2 | 3.2 ± 0.1 | 3.5 ± 0.4 | 3.8 ± 0.2 | 5.4 ± 0.2 | ||||
Notes. The Teff has been adopted from the FERRE results (see Table 1). The log g has been adopted from the FERRE results in way shows in Sect. 2. The Teff and log g uncertainties are described in Sect. 2. The [Fe/H] has been derived from the [Ca/H] assuming [α/ Fe] = 0.4, following the expression [Fe/H] = [Ca/H]–[α/ Fe] The [C/Fe] has been derived only in the cases the quality of the ISIS spectra is high enough.
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