Table 2
Metallicities of the SFRs and YOCs whose membership is discussed in this paper.
Clusters | l | b | Age | Distance | Ref. | Rgal * |
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(J2000) | (J2000) | [Myr] | [kpc] | [kpc] | [dex] | [dex] | [dex] | ||
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Star forming regions | |||||||||
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NGC 6530 | 6.082 | −1.331 | 1−2 | 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 | 1−3 | 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 | 2−3 | 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 | 1−3 | 0.76 ± 0.09 | 8, 9 | 8.70 ± 0.08 | −0.059 ± 0.004 (114) | −0.07 ± 0.02 (34) | −0.060 ± 0.006 |
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Young open clusters | |||||||||
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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 | 50−80 | 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 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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