All Tables

Table 3: Reference clusters, respective metallicities (according to Harris 1996), and $\Delta (B-V)$ corresponding to the reddening of NGC 6522 derived differentially relative to the comparison clusters.
Table 4: Stellar parameters derived using the calibrations by Alonso et al. (1999; AAM99) for V-I, V-K, J-K. The dereddened colours were obtained using the reddening law by Dean et al. (1978) and Rieke & Lebofsky (1985).
Table 5: Stellar parameters and derived metallicities.
Table 7: C, N, O and heavy elements. Carbon abundances are derived from C₂ lines and nitrogen abundances from CN lines (Sect. 6). Abundances of the heavy elements Ba, La and Eu are derived using hyperfine structure (Sect. 4).
Table 8: First guess abundance ratios [X/Fe] of the program stars.
Table 9: Final abundance ratios [X/Fe] of the light elements from O to Ti.
Table 1: Positions and magnitudes from Momany et al. (2003). For each star, the first line lists the original magnitudes while the second gives dereddened magnitudes and colours adopting the reddening law by Dean et al. (1978) and Rieke & Lebofsky (1985). Star I-36 could not be measured in the H frame. $(V-I)_{\rm J}$ is Johnson, $(V-I)_{\rm C}$ is Cousins.
Table 2: Log of the spectroscopic observations carried out on 2000 June 24-26 and 2001 July 6. The quoted seeing is the mean value along the exposures.
Table 6: Abundance ratios using the "Ionization temperature'' set of parameters given in Table 5. (^a): C₆ computed using collisional broadening theory by Barklem et al. (1998, 2000).