Integrated J- and H-band spectra of globular clusters in the LMC: implications for stellar population models and galaxy age dating

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Volume 543 (July 2012)

A&A, 543 (2012) A75

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Table 1

Target globular clusters in the LMC.

Name	Age (Gyr)	[Fe/H]	L_mosaic (L_⊙)	r_h	r_t	S/N_J	S/N_H
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)

NGC 1806	1.1¹, 1.7⁸, 1.5⁹, 1.9², 0.5^e	–0.23^b, –0.71^e	3.4 × 10⁴	–	–	>60^*	>45^*
NGC 2162	1.1¹, 1.3³, 2², 0.9⁴, 1.25⁵	–0.23^b, –0.46^f	0.5 × 10⁴	2137	1972	>45^*	>40^*
NGC 2173	2¹, 2.1³, 1.6⁶, 4.1², 1.5⁷, 1.1⁴, 1.6⁵	–0.24^b, –0.42^f, –0.51^g	0.9 × 10⁴	3435	3935	>80^*	>45^*
NGC 2019	10¹, 16¹⁰, 13.3¹¹, 16.3^a, 17.8^b	–1.23^a, –1.18^b, –1.37^c, –1.10^d	6.7 × 10⁴	972	1216	95	150
NGC 2005	10¹, 6.3¹⁰, 16¹¹, 15.5^a, 16.6^b	–1.35^a, –1.92^b, –1.80^c, –1.33^d	3.9 × 10⁴	865	988	140	–
NGC 1754	10¹, 7¹⁰, 14¹¹, 15.6^a^b	–1.42^a, –1.54^b	2.7 × 10⁴	112	1429	80	–

Notes. (1) Cluster name, (2) age of the cluster in Gyr, derived using different methods: (3) [Fe/H] derived using different methods: (4) sampled bolometric luminosity within the clusters central mosaics in L_⊙, (5) half-light radius and (6) tidal radius of the King-model cluster fit from the catalogue of McLaughlin & van der Marel (2005), (7) and (8) S/N of the integrated spectra in J- and H-band, respectively; .

⁽¹⁾

Frogel et al. (1990) – based on the SWB type;

⁽²⁾

Leonardi & Rose (2003) – integrated spectroscopy;

⁽³⁾

Geisler et al. (1997),

⁽⁴⁾

Girardi et al. (1995),

⁽⁵⁾

Kerber et al. (2007),

⁽⁶⁾

Bertelli et al. (2003),

⁽⁷⁾

Woo et al. (2003),

⁽⁸⁾

Mackey et al. (2008),

⁽⁹⁾

Milone et al. (2009) – all CMDs,

⁽¹⁰⁾

Beasley et al. (2002) – integrated spectroscopy (Hβ-Mgb),

⁽¹¹⁾

Beasley et al. (2002) – integrated spectroscopy (Hγ- ⟨ Fe ⟩ ),

^(a)

Olsen et al. (1998) – slope of the RGB,

^(b)

Olszewski et al. (1991) – low-resolution Ca II triplet,

^(c)

Johnson et al. (2006) – high-resolution Fe I,

^(d)

Johnson et al. (2006) – high-resolution Fe II,

^(e)

Dirsch et al. (2000) – Strömgren photometry,

^(f)

Grocholski et al. (2006) – low-resolution Ca II triplet,

^(g)

Mucciarelli et al. (2008) – high-resolution spectroscopy

^(*)

lower threshold, see Sect. 2.3 for an explanation

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