Na-O anticorrelation and HB - IX. Kinematics of the program clusters A link between systemic rotation and HB morphology?

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Volume 538 (February 2012)

A&A, 538 (2012) A18

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Table 1

The sample and its internal RV accuracy.

Clus.	[Fe/H]	N_tot^a	F(r ≤ r_h)^b	⟨ ΔRV_HR13−HR11 ⟩	σ_Δ	N_HR13−HR11^c	Notes^d
				[km s^-1]	[km s^-1]

NGC 104	–0.76	147	0.37	–0.38	0.24	84	L10a^e
NGC 288	–1.32	110	0.39	–0.19	0.52	50	L10b
NGC 1851	–1.16	84	0.00	–	–	–	INT(I76,D97), 184 stars from Scarpa et al. (2011)
NGC 1904	–1.58	58	0.09	–0.81	1.55	40	INT(D97), 146 stars from Scarpa et al. (2011)
NGC 2808	–1.18	123	0.06	–0.43	0.54	63	INT(I76,Z92)
NGC 3201	–1.51	149	0.48	–0.09	0.87	56	420 stars from Côté et al. (1995)
NGC 4590	–2.27	121	0.23	–1.21	2.70	98^*	L09
NGC 5904	–1.33	136	0.13	–1.78	0.30	86	INT(Dub97), 46 stars from Rastorguev & Samus (1991)
NGC 6121	–1.18	103	0.67	–0.81	0.60	63	L10b
NGC 6171	–1.03	33	0.00	–0.07	0.30	27	71 stars assembled from various sources by PM93^f
NGC 6218	–1.33	79	0.02	2.61	0.38	56	L10b
NGC 6254	–1.57	147	0.32	–0.36	0.63	61	25 stars from Rastorguev & Samus (1991)
NGC 6388	–0.45	36	0.00	–0.07	0.55	23	INT(I76)
NGC 6397	–1.99	144	0.35	–1.30	1.59	73^*	INT(D97), 127 stars from Meylan & Mayor (1991)
NGC 6441	–0.44	30	0.00	–	–	–	INT(I76,D97)
NGC 6752	–1.55	137	0.29	–0.42	0.46	69	L10b
NGC 6809	–1.93	156	0.42	–0.25	0.40	72	L10a
NGC 6838	–0.82	39	0.49	0.19	0.15	28	>100 stars assembled from various sources by PM93
NGC 7078	–2.33	84	0.13	–0.26	4.57	58^*	1773 stars form van den Bosch et al. (2006)
NGC 7099	–2.33	65	0.20	0.10	1.63	30	L09

Notes.

^(a)

Total number of stars with a valid RV measure.

^(b)

Fraction of sample stars lying within the cluster half-light radius r_h.

^(c)

Number of stars having RV measure both from HR11 and HR13.

^(d)

Reference to the most recent and/or largest sample of radial velocities available for the cluster, and used to study the cluster kinematics (PM93 = Pryor & Meylan 1993). INT indicates the presence of an estimate of the central velocity dispersion from integrated spectra; the associated reference is reported within brackets [I76 = Illingworth 1976; P89 = Peterson et al. 1989; Z92 = Zaggia et al. 1992; D97 = Dubath et al. 1997]. The INT references are reported only when large samples of individual velocities are lacking. NGC 6171 and NGC 6254 lack INT estimates.

^(e)

Clusters included in the L09, L10a and L10b papers have been studied using samples of RV estimates several hundreds individual stars per cluster. We refer to that series of papers for further references.

^(f)

Preliminary results from a sample of 107 stars have been presented by Scarpa et al. (2004).

^(*)

Clusters with lower quality RV estimates (see text).

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