OC 0339
0.30
UTI
0.27
CN
0.37
Cdens
1.0
CC3
0.25
Clit
0.7
Cdup
Stellar density (N50/rad)
1.9 [N/pc2]
- CN 0.27 Poorly populated
- Cdens 0.37 Loose
- CC3 1.0 Very high quality
- Clit 0.25 Poorly studied
- Cdup 0.7 Likely unique
Overview
OC 0339 is a poorly populated, loose object of very high C3 quality. Its parallax locates it at a very close distance, below the mid-plane, affected by moderate 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.
Note: This is likely a unique object, which shares a moderate percentage of members with at least one previously reported entry. See table with shared members information.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999â | 83.1 | -0.477 | 2.753 | 1.586 | -0.977 | 20.798 |
| Hunt & Reffert | 2024 | 83.119 | -0.419 | 2.759 | 1.667 | -1.028 | 29.1 |
| Cavallo et al. | 2024 | 83.271 | -0.537 | 2.758 | â | â | â |
| Hunt & Reffert | 2023 | 83.119 | -0.419 | 2.759 | 1.667 | -1.028 | 29.1 |
| Hao et al. | 2022 | 83.047 | -0.304 | 2.714 | 1.478 | -0.863 | 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 | 0.36 | 1.54 | 1.58 | 20 | 0.137 | 56 | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 56(1) | â | â |
| Cavallo et al. | 2024 | 0.37 | 1.37 | â | 20 | 0.000 | â | â | â |
| Hunt & Reffert | 2023 | 0.35 | 2.73 | 1.58 | 79 | â | â | â | â |
| Hao et al. | 2022 | â | 1.54 | â | 6 | 0.274 | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
MOCA


Palma et al. (2025)
Part of multiple system G10, along with ASCC_19, ASCC_20, OCSN_61 and UBC_17a.
Cavallo et al. (2024)
Silver sample.