ESO 332 22
(MWSC 2537)
0.57
UTI
0.4
CN
0.99
Cdens
0.75
CC3
0.35
Clit
1.0
Cdup
Nm (P>50%)
40
Core radius and density
0.8 [pc], 5.0 [pc-2]
- CN 0.4 Poorly populated
- Cdens 0.99 Very dense
- CC3 0.75 High quality
- Clit 0.35 Poorly studied
- Cdup 1.0 Unique
đĨ Members
đ Colab
đŦ Bayestar19
MOCA
đ CDS
đ Simbad
đ CDS (Îą, δ)
đ Simbad (Îą, δ)
MOCA
đ CDS
đ Simbad
đ CDS (Îą, δ)
đ Simbad (Îą, δ)
Overview
ESO 332 22 is a poorly populated, very dense object of high C3 quality. Its parallax locates it at a relatively close distance, near the mid-plane, affected by high extinction. It is catalogued as a near-solar metallicity, young cluster, but with a large variance across recent sources for the age parameter (see Parameters). It is poorly studied in the literature.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999â | 256.893 | -40.841 | 0.596 | -0.961 | -3.206 | â |
| Hunt & Reffert | 2024 | 256.878 | -40.842 | 0.602 | -0.943 | -3.196 | â |
| Cavallo et al. | 2024 | 256.881 | -40.846 | 0.602 | â | â | â |
| Hunt & Reffert | 2023 | 256.878 | -40.842 | 0.602 | -0.943 | -3.196 | â |
| Just et al. | 2023 | 256.843 | -40.818 | â | â | â | â |
| Bica et al. | 2019 | 256.877 | -40.817 | â | â | â | â |
| Dias et al. | 2018 | â | â | â | -1.12 | -2.25 | â |
| Dib et al. | 2018 | 256.852 | -40.817 | â | â | â | â |
| Sampedro et al. | 2017 | 256.871 | -40.813 | â | 0.07 | -1.85 | â |
| Joshi et al. | 2016 | 256.852 | -40.817 | â | â | â | â |
| Kharchenko et al. | 2016 | 256.843 | -40.818 | â | â | â | â |
| Dias et al. | 2014 | 256.871 | -40.813 | â | 0.31 | -2.14 | â |
| Kharchenko et al. | 2013 | 256.852 | -40.817 | â | -3.72 | -2.69 | â |
| Morales et al. | 2013 | 256.871 | -40.813 | â | â | â | â |
đĄ Note: The UCC values are estimated from its identified members.
| Reference | Year | Dist [kpc] | Av [mag] | DAv [mag] | Age [Myr] | [Fe/H] [dex] | Mass [Msun] | Bfrac | BSS |
|---|---|---|---|---|---|---|---|---|---|
| UCC | 99999â | 1.42 | 3.04 | 1.17 | 99 | -0.230 | 202 | â | â |
| Hunt & Reffert | 2024 | 1.56 | 2.64 | 1.17 | 191 | â | 317(1) | â | â |
| Cavallo et al. | 2024 | 1.56 | 2.80 | â | 398 | -0.230 | â | â | â |
| Hunt & Reffert | 2023 | 1.56 | 2.64 | 1.17 | 191 | â | â | â | â |
| Just et al. | 2023 | â | â | â | 99 | â | 88 | â | â |
| Dib et al. | 2018 | 1.42 | â | â | 99 | â | â | â | â |
| Joshi et al. | 2016 | 1.42 | 3.28 | â | 99 | â | â | â | â |
| Kharchenko et al. | 2016 | 1.42 | 3.28 | â | 99 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.42 | 3.28 | â | 99 | â | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
Palma et al. (2025)
Part of multiple system G72, along with HSC_2863 and HSC_2861.
Cavallo et al. (2024)
Gold sample.
Hunt & Reffert (2024)
Classified as open cluster. CMD classes: 0.95 (50th percentile), true positive (human-assigned).
Hunt & Reffert (2023)
Classified as open cluster. CMD classes: 0.95 (50th percentile), true positive (human-assigned).
Morales et al. (2013)
Classified as morphological type 'OC2' (totally exposed cluster without correlation with ATLASGAL emission). Morphological flag: one or a few submm emission within the cluster area.