Astronomy & Astrophysics

All Tables

Table 1: Coordinates, photometric data, and heliocentric radial velocities for target stars in M 13 (Grundahl et al. 1998 [G]; Piotto et al. 2002 [WF3035, WF3485]; this paper [WF3085, WFPC2 data reduced as described by Dolphin 2000]). H $\beta$ indices with a large (> $\rm 0\hbox{$.\!\!^{\rm m}$ }05$ ) uncertainty are marked with a colon.
Table 2: Coordinates, photometric data, and heliocentric radial velocities for the target stars in M 3 (Buonanno et al. 1994).
Table 3: Atmospheric parameters for our programme stars in M 3 (B) and M 13 (G, WF) as derived from photometry (Cols. 2 and 3) and fits to the Balmer line profiles using metal-poor, $\alpha$ -enhanced model atmospheres with solar helium abundances. Columns 5 and 6 list the results obtained with model spectra which contain only hydrogen and helium lines, while Cols. 7 and 8 give the results obtained with model spectra that also include metal lines for [Fe/H] = -1.5 and [ $\alpha$ /Fe] = +0.4. For those stars where we could obtain a meaningful fit we also obtained iron abundances from spectrum synthesis (Cols. 4 and 9, see text for details). Given are abundances using microturbulent velocities of 3 km s^-1 and (in brackets) for 0 km s^-1. The errors are statistical errors only.
Table 4: Atmospheric parameters for our programme stars in M 3 (B) and M 13 (G, WF) as derived from fits to Balmer and helium lines using enriched scaled-solar model spectra ([M/H] = +0.5). Columns 2-4 give the results obtained with model spectra containing only hydrogen and helium lines, Cols. 6-8 give the results obtained with model spectra including metal lines. For those stars where we could obtain a meaningful fit we also obtained iron abundances from spectrum synthesis (Col. 5, see text for details). Given are abundances using microturbulent velocities of 3 km s^-1 and (in brackets) for 0 km s^-1. The errors are statistical errors only.
Table 5: Magnesium abundances for our programme stars in M 3 (B) and M 13 (G, WF) for microturbulent velocities of 3 km s $^{\rm -1}$ and (in brackets) 0 km s^-1. We also give the atmospheric parameters used for the abundance determinations.