The Gaia-ESO Survey: the present-day radial metallicity distribution of the Galactic disc probed by pre-main-sequence clusters

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Volume 601 (May 2017)

A&A, 601 (2017) A70

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Table 4

Metallicities of the associations observed by the Gaia-ESO survey whose membership is known from the literature.


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

Star forming region


Chamaeleon I	297.1559	−15.617	2−5	0.16 ± 0.01	1, 2	7.93 ± 0.01	−0.070 ± 0.017 (6)

Young open cluster


Gamma Velorum	262.8025	−07.686	10−20	0.35 ± 0.01	3	8.05 ± 0.01	−0.03 ± 0.02 (8)

Intermediate-age open clusters


Berkeley 81	34.51	−2.07	860 ± 100	3.50 ± 0.12	5, 6	5.49 ± 0.07	0.22 ± 0.02 (13)
NGC 6005	325.8	−3.00	1200 ± 300	2.7 ± 0.5	10	6.0 ± 0.3	0.155 ± 0.007 (12)
Trumpler 23	328.8	−0.50	800 ± 100	2.2 ± 0.2	4	6.25 ± 0.15	0.140 ± 0.012 (10)
NGC 6705	27.31	−2.78	300 ± 50	2.0 ± 0.2	12	6.34 ± 0.16	0.080 ± 0.013 (27)
Pismis 18	308.2	0.30	1200 ± 400	2.2 ± 0.4	10	6.85 ± 0.17	0.105 ± 0.011 (6)
Trumpler 20	301.48	2.22	1500 ± 150	3.5 ± 0.3	13	6.86 ± 0.02	0.120 ± 0.010 (42)
Berkeley 44	53.2	+3.33	2900 ± 300	2.2 ± 0.4	4	6.91 ± 0.12	0.18 ± 0.03 (4)
NGC 4815	303.63	−2.10	570 ± 70	2.50 ± 0.15	9	6.94 ± 0.04	−0.03 ± 0.03 (5)
NGC 6802	55.3	0.92	1000 ± 100	2.3 ± 0.2	4	6.96 ± 0.07	0.100 ± 0.007 (8)
NGC 6633	36.0	8.3	630 ± 100	0.36 ± 0.02	11	7.71 ± 0.01	−0.06 ± 0.02 (11)
NGC 3532	289.6	1.35	300 ± 100	0.49 ± 0.01	8	7.85 ± 0.01	−0.025 ± 0.013 (2)
NGC 2516	273.8	−15.8	163 ± 40	0.36 ± 0.02	7	7.98 ± 0.01	−0.080 ± 0.016 (15)

Notes. The associations are sorted by Galactocentric radii.

^(*)

We adopted R_gal = 8.0 kpc for the Sun.

^(**)

The metallicity values are the median of the [Fe/H] reported in iDR4 for the stellar members of the clusters. We reported in brackets the number of stars that we used for the metallicity determinations.

Reference. For cluster ages and distances: (1) Whittet et al. (1997); (2) Luhman (2007); (3) Jeffries et al. (2009b); (4) Jacobson et al. (2016); (5) Donati et al. (2014a); (6) Magrini et al. (2015); (7) Sung et al. (2002); (8) Clem et al. (2011); (9) Friel et al. (2014); (10) Piatti et al. (1997); (11) Jeffries et al. (2002); (12) Cantat-Gaudin et al. (2014); (13) Donati et al. (2014b).

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