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Table 2

Metallicities of the SFRs and YOCs whose membership is discussed in this paper.

Clusters l b Age Distance Ref. Rgal * ** **
(J2000) (J2000) [Myr] [kpc] [kpc] [dex] [dex] [dex]

Star forming regions

NGC 6530 6.082 1.331 12 1.5 ± 0.3 1 6.5 ± 0.3 0.041 ± 0.009 (161) 0.00 (1) 0.041 ± 0.009
Carina 287.408 0.577 13 2.7 ± 0.3 2, 3, 4, 5 7.64 ± 0.02 0.030 ± 0.016 (91) – (0) 0.030 ± 0.016
Rho Oph 353.686 +17.687 23 0.13 ± 0.01 6, 7 7.88 ± 0.01 0.07 ± 0.03 (7) 0.080 ± 0.005 (4) 0.08 ± 0.02
NGC 2264 202.935 +2.195 13 0.76 ± 0.09 8, 9 8.70 ± 0.08 0.059 ± 0.004 (114) 0.07 ± 0.02 (34) 0.060 ± 0.006

Young open clusters

IC 4665 30.619 +17.081 30 ± 5 0.36 ± 0.01 10,11 7.71 ± 0.01 0.00 ± 0.06 (3) 0.00 ± 0.02 (12) 0.00 ± 0.02
IC 2602 289.601 4.906 30 ± 5 0.15 ± 0.01 12, 13 7.95 ± 0.01 0.02 ± 0.03 (11) 0.00 ± 0.03 (8) 0.02 ± 0.02
IC 2391 270.362 6.839 55 ± 5 0.16 ± 0.01 14, 15 8.00 ± 0.01 0.013 ± 0.012 (2) 0.05 ± 0.03 (3) 0.03 ± 0.02
NGC 2547 264.435 8.625 35 ± 5 0.36 ± 0.02 16, 17, 18 8.04 ± 0.01 0.001 ± 0.010 (29) 0.015 ± 0.019 (10) 0.006 ± 0.009
NGC 2451A 252.575 7.298 5080 0.21 ± 0.01 19 8.06 ± 0.01 0.05 ± 0.02 (18) 0.04 ± 0.04 (4) 0.046 ± 0.019
NGC 2451B 252.050 6.726 50 ± 10 0.37 ± 0.01 19 8.12 ± 0.01 0.006 ± 0.012 (15) 0.002 ± 0.017 (9) 0.005 ± 0.010

Notes. The associations are sorted by Galactocentric radii.

(*)

We adopted Rgal = 8.0 kpc for the Sun.

(**)

We reported in brackets the final number of stars for each cluster and each spectrograph that we used for the metallicity determinations.

Reference. For cluster ages and distances: (1) Prisinzano et al. (2005); (2) Smith et al. (2000); (3) DeGioia-Eastwood et al. (2001); (4) Smith (2006); (5) Hur et al. (2012); (6) Mamajek (2008); (7) Erickson et al. (2011); (8) Sung et al. (1997); (9) Sung et al. (2004); (10) Manzi et al. (2008); (11) Cargile & James (2010); (12) van Leeuwen (2009); (13) Stauffer et al. (1997); (14) Barrado y Navascués et al. (1999); (15) Barrado y Navascués et al. (2004); (16) Jeffries & Oliveira (2005); (17) Lyra et al. (2006); (18) Naylor & Jeffries (2006); (19) Hunsch et al. (2003).

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