Table 3.
Main physical parameters for each star cluster candidate using the VVV photometry.
| Cluster ID | Ks (RC) | E(J − Ks) | AKs | (m − M)0 | DVVV | RG | MKs | MV | [Fe/H] | [Fe/H]s(a) | Age | Type |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| [mag] | [mag] | [mag] | [mag] | [kpc] | [kpc] | [mag] | [mag] | dex | dex | Gyr | ||
| FSR0009 | – | 0.25 ± 0.04 | 0.11 ± 0.03 | 14.20 ± 0.04 | 6.9 ± 0.2 | 1.81 | −5.8 ± 0.7 | −3.4 | −1.2 ± 0.3 | −1.10 | 11 ± 2 | GC |
| FSR1775 | – | 0.37 ± 0.03 | 0.16 ± 0.01 | 14.75 ± 0.02 | 8.9 ± 0.2 | 1.37 | −8.0 ± 1.7 | −5.6 | −1.1 ± 0.2 | −1.10 | 10 ± 2 | GC |
| FSR1767 | 13.8 ± 0.03 | 0.66 ± 0.04 | 0.28 ± 0.03 | 15.12 ± 0.04 | 10.6 ± 0.2 | 2.70 | −8.4 ± 1.5 | −6.3 | −0.7 ± 0.2 | −0.73 | 11 ± 2 | GC |
| VVVCL110 | 14.5 ± 0.03 | 2.0 ± 0.04 | 0.86 ± 0.02 | 15.25 ± 0.04 | 11.2 ± 0.5 | 3.25 | −8.6 ± 1.6 | −6.8 | −0.1 ± 0.2 | −0.48 | 11 ± 2 | GC? |
| VVVCL119 | 14.5 ± 0.05 | 1.98 ± 0.07 | 0.85 ± 0.04 | 15.26 ± 0.06 | 11.3 ± 0.6 | 2.24 | −9.3 ± 1.8 | −7.5 | −0.1 ± 0.2 | −0.48 | 10 ± 3 | GC? |
| VVVCL128 | 14.2 ± 0.05 | 1.20 ± 0.05 | 0.51 ± 0.04 | 15.29 ± 0.06 | 11.4 ± 0.5 | 3.26 | −7.5 ± 1.6 | −5.7 | 0.0 ± 0.3 | −0.11 | 10 ± 3 | GC? |
| VVVCL131 | 13.4 ± 0.03 | 0.54 ± 0.04 | 0.23 ± 0.03 | 14.77 ± 0.04 | 9.0 ± 0.5 | 1.17 | −8.2 ± 1.5 | −5.9 | −0.6 ± 0.2 | −0.73 | 10 ± 3 | GC |
| VVVCL143 | 13.4 ± 0.03 | 0.50 ± 0.05 | 0.21 ± 0.04 | 14.74 ± 0.05 | 8.9 ± 0.5 | 1.0 | −8.2 ± 1.3 | −5.9 | −0.6 ± 0.2 | −0.61 | 10 ± 3 | GC |
| VVVCL150 | – | 1.32 ± 0.04 | 0.56 ± 0.03 | 14.54 ± 0.04 | 8.1 ± 0.5 | 0.56 | −8.7 ± 1.7 | −6.5 | −1.3 ± 0.1 | −1.35 | 12 ± 2 | GC? |
| VVVCL153 | 14.1 ± 0.02 | 1.67 ± 0.04 | 0.71 ± 0.03 | 14.99 ± 0.04 | 10 ± 0.4 | 1.90 | −8.6 ± 1.9 | −6.8 | −0.1 ± 0.1 | −0.23 | 10 ± 3 | GC? |
| VVVCL154 | 13.5 ± 0.03 | 0.85 ± 0.05 | 0.36 ± 0.04 | 14.47 ± 0.05 | 8.9 ± 0.5 | 0.78 | −9.6 ± 1.8 | −7.2 | −0.6 ± 0.2 | −0.67 | 11 ± 2 | GC? |
| VVVCL160 | – | 1.71 ± 0.04 | 0.73 ± 0.03 | 14.17 ± 0.04 | 6.8 ± 0.5 | 1.92 | −7.9 ± 1.5 | −5.5 | −1.4 ± 0.3 | −1.47 | 13 ± 2 | GC |
| ESO393-12 | 13.2 ± 0.02 | 0.54 ± 0.03 | 0.23 ± 0.02 | 14.57 ± 0.03 | 8.2 ± 0.4 | 0.98 | −7.7 ± 1.5 | −5.3 | −0.6 ± 0.2 | −0.61 | 10 ± 2 | GC |
| ESO456-09 | 13.0 ± 0.02 | 0.44 ± 0.04 | 0.18 ± 0.03 | 14.42 ± 0.04 | 7.6 ± 0.4 | 0.81 | −8.3 ± 1.5 | −6.0 | −0.6 ± 0.2 | −0.61 | 10 ± 2 | GC |
| DB044 | 13.2 ± 0.02 | 0.69 ± 0.03 | 0.30 ± 0.02 | 14.51 ± 0.1 | 8.0 ± 0.5 | 0.61 | −8.0 ± 1.6 | −6.0 | −0.1 ± 0.2 | −0.11 | 11 ± 2 | GC? |
| Kronberger49 | 13.3 ± 0.03 | 0.69 ± 0.04 | 0.30 ± 0.03 | 14.61 ± 0.04 | 8.3 ± 0.5 | 1.14 | −8.5 ± 1.5 | −6.7 | −0.2 ± 0.2 | −0.36 | 11 ± 2 | GC |
Notes. The absolute magnitude in V-band is calculated from the comparison with the well-known GCs (see Table 5). We mark with a question mark those clusters for which we need further data in order to unveil their nature.
The [Fe/H] estimates are derived from the RGB-slope using the relation by Cohen et al. (2015).
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