Table 5.
Globular clusters used in our comparison (Figs. 3–6).
| RGC | [Fe/H] | |||
|---|---|---|---|---|
| ID | [kpc] | [dex] | Progenitor (a) | Abundance source |
| NGC 2419 | 89.9 | −2.09 | Sgr | Cohen & Kirby (2012) |
| NGC 5824 | 25.9 | −2.38 | Sgr | Roederer et al. (2016) |
| NGC 6715 | 18.9 | −1.51 | Sgr | Carretta et al. (2014) |
| Terzan 7 | 15.6 | −0.61 | Sgr | Sbordone et al. (2007) |
| Arp 2 | 21.4 | −1.80 | Sgr | Mottini et al. (2008) |
| Terzan 8 | 19.4 | −2.27 | Sgr | Carretta et al. (2014) |
| Pal 12 | 15.8 | −0.82 | Sgr | Cohen (2004) |
| NGC 5466 | 16.3 | −1.97 | Seq | Lamb et al. (2015) |
| IC 4499 | 15.7 | −1.59 | Seq | Dalessandro et al. (2018) |
| NGC 7006 | 38.5 | −1.55 | Seq | Kraft et al. (1998) |
| FSR 1758 | 11.8 | −1.58 | Seq | Villanova et al. (2019) |
| NGC 288 | 12.0 | −1.39 | G-E | Shetrone & Keane (2000) |
| NGC 362 | 9.4 | −1.17 | G-E | Carretta et al. (2013) |
| NGC 1261 | 18.1 | −1.19 | G-E | Filler et al. (2012) |
| NGC 1851 | 16.6 | −1.17 | G-E | Carretta et al. (2011) |
| NGC 1904 | 18.8 | −1.46 | G-E | Francois (1991) |
| NGC 2298 | 15.8 | −1.91 | G-E | McWilliam et al. (1992) |
| NGC 2808 | 11.1 | −1.27 | G-E | Marino et al. (2017) |
| NGC 4833 | 7.0 | −2.25 | G-E | Roederer & Thompson (2015) |
| NGC 5897 | 7.4 | −2.04 | G-E | Koch & McWilliam (2014) |
| NGC 6205 | 8.4 | −1.50 | G-E | Cohen & Meléndez (2005a) |
| NGC 6229 | 29.8 | −1.13 | G-E | Johnson et al. (2017) |
| Pal 15 | 38.4 | −1.94 | G-E | Koch et al. (2019b) |
| NGC 6341 | 9.6 | −2.70 | G-E | Roederer & Sneden (2011) |
| NGC 6779 | 9.2 | −1.90 | G-E | Khamidullina et al. (2014) |
| NGC 6864 | 14.7 | −1.16 | G-E | Kacharov et al. (2013) |
| NGC 7089 | 10.4 | −1.44 | G-E | Yong et al. (2014) |
| NGC 7099 | 7.1 | −2.28 | G-E | Lovisi et al. (2013) |
| NGC 7492 | 25.3 | −1.82 | G-E | Cohen & Melendez (2005b) |
| NGC 5272 | 12.0 | −1.39 | H99 | Cohen & Meléndez (2005a) |
Notes. Only those GCs from the list of Massari et al. (2019) that have available abundance information are listed.
Following the assignments of Massari et al. (2019) to the Sgr dSph (Sgr), the Sequoia accretion event (Seq), Gaia-Enceladus (G-E), and the Helmi streams (H99).
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