NGC 2180
(MWSC 765)
0.18
UTI
0.0
CN
0.02
Cdens
0.25
CC3
0.32
Clit
1.0
Cdup
Nm (P>50%)
20
Core radius and density
4.3 [pc], 0.1 [pc-2]
- CN 0.0 Sparse
- Cdens 0.02 Very loose
- CC3 0.25 Low quality
- Clit 0.32 Poorly studied
- Cdup 1.0 Unique
Overview
NGC 2180 is a sparse, very loose object of low C3 quality. Its parallax locates it at a moderate* distance, well below the mid-plane, affected by low extinction. It is catalogued as a low-mass, old cluster (see Parameters). It is poorly studied in the literature.
(*): The parallax distance estimate (~4.95 kpc) differs significantly from the median photometric distance (~1.88 kpc).
â ī¸ Warning: the low UTI value and no obvious signs of duplication (Cdup=1.0) indicate that this is quite probably an asterism, moving group, or artifact, and not a real open cluster.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999â | 92.454 | 4.788 | 0.202 | 0.156 | 0.2 | 48.648 |
| Just et al. | 2023 | 92.43 | 4.806 | â | â | â | â |
| Bica et al. | 2019 | 92.45 | 4.806 | â | â | â | â |
| Angelo et al. | 2019 | 92.433 | 4.823 | â | â | â | â |
| Dias et al. | 2018 | â | â | â | 0.61 | -3.01 | â |
| Dib et al. | 2018 | 92.437 | 4.805 | â | â | â | â |
| Loktin & Popova | 2017 | 92.445 | 4.807 | â | 0.039 | -0.495 | â |
| Sampedro et al. | 2017 | 92.45 | 4.807 | â | -1.85 | -3.93 | â |
| Kharchenko et al. | 2016 | 92.43 | 4.806 | â | â | â | â |
| Dias et al. | 2014 | 92.45 | 4.807 | â | -1.55 | -3.55 | â |
| Kharchenko et al. | 2013 | 92.437 | 4.805 | â | 0.6 | 0.19 | â |
| Piskunov et al. | 2008 | 92.436 | 4.81 | â | â | â | â |
| Kharchenko et al. | 2005 | 92.44 | 4.81 | â | 1.34 | -1.83 | 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 | 1.88 | 0.92 | â | 2002 | â | 31 | â | â |
| Just et al. | 2023 | â | â | â | 2265 | â | 35 | â | â |
| Angelo et al. | 2019 | 1.05 | â | â | 710 | â | 27 | â | â |
| Dib et al. | 2018 | 1.88 | â | â | 2265 | â | â | â | â |
| Loktin & Popova | 2017 | 1.96 | 0.92 | â | 126 | â | â | â | â |
| Kharchenko et al. | 2016 | 1.88 | 1.25 | â | 2265 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.88 | 1.25 | â | 2265 | â | â | â | â |
| Piskunov et al. | 2008 | 0.91 | 0.00 | â | 1738 | â | â | â | â |
| Kharchenko et al. | 2005 | 0.91 | 0.00 | â | 1738 | â | â | â | â |
MOCA

Cantat-Gaudin & Anders (2020)
Investigated multiple times as a dissolving cluster, but Gaia DR2 proper motions and parallaxes show no coherent group; confirmed as an asterism. More details in Appendix A of the article.