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.
Star Photometry log $\epsilon_{\rm Fe}$ Line profiles log $\epsilon_{\rm Fe}$
  $ {T_{\rm eff}}$ $\log {g}$   $ {T_{\rm eff}}$ $\log {g}$ $ {T_{\rm eff}}$ $\log {g}$  
  [K] [cm s-2]   [K] [cm s-2] [K] [cm s-2]  
G43 13 050 2.60   13 900$~\pm~$710 3.14$~\pm~$0.14 14 400$~\pm~$450 3.24$~\pm~$0.09 -
G129 8630 3.01 5.7 (5.6) 8000$~\pm~$  70 2.88$~\pm~$0.09 7900$~\pm~$  50 2.93$~\pm~$0.07 5.1 (5.1)
G137 8910 3.14 6.4 (6.8) 8400$~\pm~$  50 3.04$~\pm~$0.02 8400$~\pm~$  50 3.08$~\pm~$0.02 6.0 (6.4)
G195 8980 3.19 5.8 (5.8) 8200$~\pm~$  40 2.95$~\pm~$0.03 8300$~\pm~$  40 2.99$~\pm~$0.02 5.2 (5.2)
G201 9360 3.26 6.4 (6.6) 8900$~\pm~$200 3.12$~\pm~$0.12 8300$~\pm~$  50 2.82$~\pm~$0.03 5.5 (5.6)
G208 9870 3.43 6.6 (6.6) 10 900$~\pm~$200 3.73$~\pm~$0.07 10 900$~\pm~$200 3.76$~\pm~$0.07 6.9 (7.0)
G219 8970 3.22 5.8 (6.0) 10 300$~\pm~$160 3.89$~\pm~$0.07 8100$~\pm~$  60 2.85$~\pm~$0.05 4.9 (5.2)
G235 9150 3.27 5.9 (5.8) 11 300$~\pm~$130 4.12$~\pm~$0.05 11 300$~\pm~$130 4.15$~\pm~$0.05 6.8 (6.7)
G297 10 590 3.59   10 600$~\pm~$130 3.60$~\pm~$0.05 10 600$~\pm~$120 3.63$~\pm~$0.05 6.5 (6.6)
G314 10 620 3.66   10 400$~\pm~$190 3.64$~\pm~$0.07 10 500$~\pm~$180 3.68$~\pm~$0.07 6.0 (6.0)
G322 13 750 3.58   15 000$~\pm~$370 3.62$~\pm~$0.07 14 900$~\pm~$360 3.61$~\pm~$0.07 7.4 (7.5)
G342 11 520 3.69   11 300$~\pm~$140 3.71$~\pm~$0.05 11 300$~\pm~$140 3.75$~\pm~$0.05 6.2 (6.1)
G382 14 160 3.38   14 300$~\pm~$240 3.72$~\pm~$0.05 14 300$~\pm~$240 3.73$~\pm~$0.05 8.0 (8.0)
G496 17 560 4.03   18 600$~\pm~$350 4.20$~\pm~$0.05     -
G503 15 800 4.31   14 900$~\pm~$580 3.86$~\pm~$0.10 14 900$~\pm~$570 3.86$~\pm~$0.10 7.4 (7.6)
G635 18 800 4.82   19 500$~\pm~$450 4.38$~\pm~$0.07     -
G744 19 880 4.81   21 000$~\pm~$620 4.52$~\pm~$0.10     -
G781 20 390 5.00   19 700$~\pm~$820 4.61$~\pm~$0.14     -
G827 21 720 4.65   21 200$~\pm~$430 4.73$~\pm~$0.07     -
WF 3035 9550 3.51   10 300$~\pm~$240 3.74$~\pm~$0.10 10 300$~\pm~$240 3.77$~\pm~$0.10 -
WF 3085 10 260 3.66   12 900$~\pm~$300 3.36$~\pm~$0.07 12 900$~\pm~$300 3.41$~\pm~$0.07 7.5 (8.2)
WF 3485 9790 3.57   13 300$~\pm~$330 3.76$~\pm~$0.07 13400$~\pm~$330 3.78$~\pm~$0.07 7.9 (8.4)
B254 9630 3.53   10 600$~\pm~$110 3.62$~\pm~$0.05 10 600$~\pm~$110 3.67$~\pm~$0.03 6.3 (6.2)
B352 28 600 5.63   13 900$~\pm~$300 3.66$~\pm~$0.05 13 900$~\pm~$300 3.69$~\pm~$0.05 8.1 (8.6)
B445 9850 3.58   9700$~\pm~$170 3.28$~\pm~$0.09 9800$~\pm~$170 3.35$~\pm~$0.09 6.2 (6.2)
B621 10 170 3.64   12 900$~\pm~$260 3.71$~\pm~$0.07 13 000$~\pm~$250 3.75$~\pm~$0.07 7.6 (7.9)


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