The chemical composition of globular clusters in the Local Group

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Volume 660 (April 2022)

A&A, 660 (2022) A88

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Table 4.

Summary of model assumptions.

Cluster	t_iso	[Fe/H]_iso	[α/Fe]_iso	HB	σ_br	v_hel
	(Gyr)				(km s⁻¹)	(km s⁻¹)
NGC 104	11	−0.8	+0.4	NGC 104	12.3	−17 ⁽¹⁾
NGC 362	11	−1.1	+0.4	NGC 362	8.5	+225 ⁽¹⁾
NGC 6254	13	−1.5	+0.4	NGC 6254	7.3	+75 ⁽¹⁾
NGC 6388	13	−0.6	+0.2	NGC 6388	18.1	+83 ⁽¹⁾
NGC 6752	13	−1.8	+0.4	NGC 6752	8.7	−28 ⁽¹⁾
NGC 7078	13	−2.3	+0.4	NGC 7078	13.3	−105 ⁽¹⁾
NGC 7099	13	−2.3	+0.4	NGC 7099	6.2	−184 ⁽¹⁾
M 31 006−058	13	−0.6	+0.4	NGC 104	12.1	−238 ⁽²⁾
M 31 012−064	13	−1.8	+0.4	NGC 6093	19.2	−359 ⁽²⁾
M 31 019−072	11	−0.7	+0.4	NGC 104	18.0	−222 ⁽²⁾
M 31 058−119	13	−1.0	+0.4	NGC 362	20.0	−221 ⁽²⁾
M 31 082−144	11	−0.7	+0.4	NGC 104	25.8	−373 ⁽²⁾
M 31 163−217	13	−0.2	+0.2	NGC 6388	18.2	−163 ⁽²⁾
M 31 171−222	13	−0.2	+0.2	NGC 6388	15.1	−267 ⁽²⁾
M 31 174−226	13	−1.0	+0.4	NGC 362	14.7	−491 ⁽²⁾
M 31 225−280	11	−0.4	+0.4	NGC 6388	27.6	−160 ⁽²⁾
M 31 338−076	13	−1.1	+0.4	NGC 362	19.9	−266 ⁽²⁾
M 31 358−219	13	−2.2	+0.4	NGC 7078	11.8	−315 ⁽²⁾
M 31 EXT8	13	−2.8	+0.4	N/A	13.7	−204 ⁽³⁾
M 33 H38	10	−1.1	+0.4	NGC 362	6.0	−241 ⁽⁶⁾
M 33 M9	13	−1.7	+0.4	NGC 6093	6.4	−249 ⁽⁶⁾
M 33 R12	10	−0.9	+0.4	NGC 104	6.9	−218 ⁽⁶⁾
M 33 U49	10	−1.4	+0.4	NGC 362	7.9	−150 ⁽⁶⁾
M 33 R14	10	−1.1	+0.4	NGC 362	10.8	−214 ⁽²⁾
M 33 U77	13	−1.8	+0.4	NGC 6093	6.4	−222 ⁽²⁾
M 33 CBF28	10	−1.2	+0.4	NGC 362	8.3	−238 ⁽²⁾
M 33 HM33B	13	−1.2	+0.4	NGC 362	4.6	−190 ⁽²⁾
NGC 147 Hodge II	13	−1.5	+0.4	NGC 6254	4.2	−207 ⁽⁶⁾
NGC 147 Hodge III	13	−2.4	+0.4	NGC 7078	7.5	−197 ⁽⁶⁾
NGC 147 PA-1	13	−2.3	+0.4	NGC 7078	7.0	−221 ⁽⁶⁾
NGC 147 PA-2	13	−1.9	+0.4	NGC 6779	7.0	−221 ⁽⁶⁾
NGC 147 SD7	13	−1.9	+0.4	NGC 6779	6.3	−197 ⁽⁶⁾
NGC 185 FJJ-III	13	−1.8	+0.4	NGC 6093	6.0	−243 ⁽²⁾
NGC 185 FJJ-V	13	−1.8	+0.4	NGC 6093	6.9	−173 ⁽²⁾
NGC 185 FJJ-VIII	13	−1.8	+0.4	NGC 6093	5.7	−188 ⁽²⁾
NGC 205 Hubble I	13	−1.4	+0.4	NGC 6254	7.6	−302 ⁽²⁾
NGC 205 Hubble II	13	−1.3	+0.4	NGC 362	8.5	−241 ⁽²⁾
NGC 6822 Hubble VII	13	−1.7	0.0	NGC 6093	9.6	−62 ⁽²⁾
NGC 6822 SC6	13	−1.7	+0.4	NGC 6093	9.4	−5 ⁽⁶⁾
NGC 6822 SC7	13	−1.1	0.0	NGC 362	9.9	−39 ⁽⁶⁾
WLM GC	13	−1.9	+0.2	NGC 6779	9.9	−109 ⁽⁵⁾
Fornax 3	13	−2.3	+0.4	NGC 7078	8.1	+60 ⁽⁴⁾
Fornax 4	13	−1.3	0.0	NGC 362	5.5	+47 ⁽⁴⁾
Fornax 5	13	−2.1	+0.4	NGC 6779	6.3	+61 ⁽⁴⁾
NGC 2403 F46	13	−1.7	+0.4	NGC 6093	12.2	+140 ⁽²⁾

Notes. For each cluster, we list the age (t_iso), metallicity ([Fe/H]_iso), and composition ([α/Fe]_iso) of the DSEP isochrone used to model the integrated-light spectrum. The HB column indicates the Galactic GC from which the horizontal branch was adopted, σ_br is the broadening applied to the model spectra, and v_hel is the heliocentric radial velocity. The broadening includes the instrumental resolution, which is typically 2−3 km s⁻¹. The BaSTI isochrone used for M 31 EXT8 already includes the HB.

References. Radial velocities: (1) Larsen et al. (2017); (2) this work; (3) Larsen et al. (2020); (4) Larsen et al. (2012); (5) determined for the analysis in Larsen et al. (2014) but not listed in that work; (6) Larsen et al. (2014).

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