Chemical analysis in secondary stars in LMXBs
Linelists
The linelists listed below have the same format as input files to compute synthetic spectra using the LTE code MOOG (Sneden 1973). We adopted the atomic line data from the Vienna Atomic Line Database and used a grid of local thermodynamic equilibrium (LTE) models of atmospheres provided by Kurucz (1992, private communication). To minimize the effects associated with the errors in the transition probabilities of atomic lines, we adjusted the oscillator strengths, log gf values, of the selected lines until we succeeded in reproducing the solar atlas of Kurucz et al. (1984) with solar abundances (Anders & Grevesse 1989).
Chemical analysis in metal rich stars
Linelists
Equivalent widths of spectral lines of chemical elements in metal rich stars
Data of the elements Na, Mg y Al were obtained from Beirão et al. (2005), and other elements from Bodaghee et al. (2003) y Gilli et al. (2006).
Tables with the data from the paper
by Gilli et al. (2006, A&A, 449, 723)
Na lines in the comparison sample
Mg lines in the comparison sample
Al lines in the comparison sample
Si lines in the comparison sample
Ca lines in the comparison sample
Sc lines in the comparison sample
Ti lines in the comparison sample
V lines in the comparison sample
Cr lines in the comparison sample
Mn lines in the comparison sample