VizieR Online Data Catalog: Abundances of metal-poor stars (Matas Pinto+, 2021)

The observations of the stars we studied are described in detail in Paper I (Sbordone et al., 2010A&A...522A..26S, Cat. J/A+A/522/A26) (see their Table 1).

Briefly, observations were performed with the high-resolution spectrograph UVES at the ESO-VLT. The spectra have a resolving power R=~40000 and were centred at 390nm (spectral range: 330-451nm) and 580nm (spectral range: 479-680nm). For two stars (BS 17572-100 and HE 1413-1954) that were previously studied in the frame of the HERES program (Christlieb et al., 2004A&A...428.1027C; Barklem et al., 2005A&A...439..129B, Cat. J/A+A/439/129) from UVES spectra centred at 437nm (spectral range: 376-497nm), the blue spectra were centred at 346 nm (spectral range: 320-386nm). The S/N of the spectra at 400nm is only about half of the S/N measured at 670nm (see Table 1 in Paper I) and thus generally does not exceed 50. For two stars, CS 22188-033 and HE 0148-2611, new UVES spectra from the ESO archives, centred at 390 and 580nm, were also used, increasing the S/N ratio of the mean spectrum. The data were reduced using the standard UVES pipeline with the same procedures as used in Bonifacio et al. (2007A&A...462..851B).

Here we present the table with equivalent widths discussed in the paper.

(2 data files).