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Table 1

Open cluster basic data observed with FLAMES sorted in terms of increasing NGC number.

Cluster Alternative Location (l,b) Dist Exp time Median S/N Stars Scales Galactic scales
name (deg) (kpc) (s) at Ca ii K used probed (arcmin) probed (pc)

NGC 330 Kron 35 SMC 302.42, –44.66 61 13 650 30 111 0.2–27.4 0.07–9.1
NGC 346 Kron 39 SMC 302.14, –44.94 61 6825 60 110 0.3–20.7 0.12– 8.9
NGC 1761 LH 09 LMC 277.23, –36.07 51 13 650 135 111 0.2–22.3 0.09–8.8
NGC 2004 KMHK 991 LMC 277.45, –32.63 51 13 650 95 111 0.2–20.0 0.05–4.6
NGC 3293 Collinder 224 Galaxy 285.85, +0.07 2.327 795 70 90 0.2–22.3 0.14–15.1
NGC 4755 The Jewel Box Galaxy 303.21, +2.50 1.976 795 80 81 0.2–21.8 0.11–12.5
NGC 6611 M 16 Galaxy 16.98, +0.80 1.749 750 50 43 0.2–23.5 0.10–12.0

Notes. Distances to Milky Way clusters are from the WEBDA database with the distances to the LMC and SMC being taken from Keller & Wood (2006). The last column corresponds to the minimum and maximum transverse star-star separation at the distance of the cluster. For the Galactic scales probed by the Magellanic objects we have assumed that the scaleheight of the Galaxy is ~800 pc (Smoker et al. 2003). Note that the Galactic scales are upper limits, as the ISM absorption can arise anywhere in the line of sight between the Earth and the cluster in question.

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