NGC 189
(Collinder 462; MWSC 62; OCL 301; FoF 2127)
0.91
UTI
0.78
CN
1.0
Cdens
0.75
CC3
1.0
Clit
1.0
Cdup
Stellar density (N50/rad)
15.8 [N/pc2]
- CN 0.78 Rich
- Cdens 1.0 Very dense
- CC3 0.75 High quality
- Clit 1.0 Very well-studied
- Cdup 1.0 Unique
Overview
NGC 189 is a rich, very dense object of high C3 quality. Its parallax locates it at a relatively close distance, near the mid-plane, affected by moderate extinction. It is catalogued as a near-solar metallicity, intermediate-age cluster, but with a large variance across recent sources for the age, metallicity, and mass parameters (see Parameters). It is very well-studied in the literature.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999â | 9.883 | 61.096 | 0.769 | 0.335 | -3.355 | -31.393 |
| Li et al. | 2025 | 9.885 | 61.09 | 0.772 | 0.338 | -3.306 | â |
| Hu & Soubiran | 2025 | 9.845 | 61.1 | â | â | â | â |
| Almeida et al. | 2025 | 9.889 | 61.097 | â | â | â | â |
| Hunt & Reffert | 2024 | 9.895 | 61.088 | 0.774 | 0.33 | -3.359 | -29.552 |
| Cavallo et al. | 2024 | 9.845 | 61.1 | 0.772 | â | â | â |
| Hunt & Reffert | 2023 | 9.895 | 61.088 | 0.774 | 0.33 | -3.359 | -29.552 |
| Almeida et al. | 2023 | 9.881 | 61.093 | â | â | â | â |
| Just et al. | 2023 | 9.861 | 61.112 | â | â | â | â |
| Tarricq et al. | 2022 | 9.873 | 61.087 | 0.773 | 0.315 | -3.356 | â |
| Jadhav & Subramaniam | 2021 | 9.885 | 61.09 | â | â | â | â |
| Richer et al. | 2021 | 9.872 | 61.097 | 0.772 | 0.357 | -3.265 | â |
| Dias et al. | 2021 | 9.889 | 61.097 | 0.779 | 0.336 | -3.315 | -29.391 |
| Cantat-Gaudin et al. | 2020 | 9.885 | 61.09 | 0.772 | 0.338 | -3.306 | â |
| Cantat-Gaudin & Anders | 2020 | 9.885 | 61.09 | 0.772 | 0.338 | -3.306 | â |
| Liu & Pang | 2019 | 9.947 | 61.101 | 0.768 | 0.323 | -3.307 | â |
| Soubiran et al. | 2018 | 9.885 | 61.09 | â | â | â | -28.71 |
| Bica et al. | 2019 | 9.876 | 61.098 | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 9.885 | 61.09 | 0.772 | 0.338 | -3.306 | â |
| Loktin & Popova | 2017 | 9.9 | 61.095 | â | -2.761 | -2.398 | â |
| Kharchenko et al. | 2016 | 9.861 | 61.112 | â | â | â | â |
| Dias et al. | 2014 | 9.896 | 61.095 | â | -0.36 | -3.02 | â |
| Kharchenko et al. | 2013 | 9.87 | 61.115 | â | -0.31 | -2.71 | â |
| Kharchenko et al. | 2012 | 9.87 | 61.115 | â | -0.31 | -2.71 | â |
| Bukowiecki et al. | 2011 | 9.871 | 61.105 | â | â | â | â |
| van den Bergh | 2006 | 9.9 | 61.067 | â | â | â | â |
| Dias et al. | 2002 | 9.896 | 61.095 | â | -0.36 | -3.02 | â |
| Lynga | 1987 | 9.921 | 61.069 | â | â | â | â |
| Sulentic et al. | 1973 | 9.687 | 61.054 | 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 | 1.23 | 1.77 | 1.43 | 486 | 0.084 | 236 | 0.61 | 0 |
| Li et al. | 2025 | 0.94 | 1.56 | â | 1200 | -0.342 | â | â | â |
| Hu & Soubiran | 2025 | â | â | â | â | -0.040(5) | â | â | â |
| Almeida et al. | 2025 | 1.25 | 1.87 | â | 486 | â | 210 | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 590(1) | â | â |
| Cavallo et al. | 2024 | 1.22 | 1.58 | â | 631 | 0.560 | â | â | â |
| Hunt & Reffert | 2023 | 1.24 | 1.78 | 1.43 | 313 | â | â | â | â |
| Almeida et al. | 2023 | 1.21 | 1.83 | â | 640 | 0.048 | 281(1) | 0.61 | â |
| Just et al. | 2023 | â | â | â | 512 | â | 16 | â | â |
| Tarricq et al. | 2022 | 1.20 | â | â | 417 | â | â | â | â |
| Jadhav & Subramaniam | 2021 | 1.23 | 1.54 | â | 398 | â | 261 | â | 0(1) |
| Richer et al. | 2021 | â | 1.76 | â | 398 | â | â | â | â |
| Dias et al. | 2021 | 1.25 | 1.87 | â | 486 | 0.119 | â | â | â |
| Cantat-Gaudin et al. | 2020 | 1.23 | 1.54 | â | 398 | â | â | â | â |
| Kounkel et al. | 2020 | 1.18 | 2.00 | â | 550 | â | â | â | â |
| Cantat-Gaudin & Anders | 2020 | 1.25 | â | â | â | â | â | â | â |
| Liu & Pang | 2019 | â | â | â | 562 | 0.250 | â | â | â |
| Soubiran et al. | 2018 | 1.25 | â | â | â | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 1.25 | â | â | â | â | â | â | â |
| Loktin & Popova | 2017 | 1.09 | 1.02 | â | 380 | â | â | â | â |
| Kharchenko et al. | 2016 | 1.30 | 2.21 | â | 512 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.30 | 2.21 | â | 512 | â | â | â | â |
| Bukowiecki et al. | 2012 | â | â | â | â | â | 150 | â | â |
| Kharchenko et al. | 2012 | 1.30 | 2.21 | â | 512 | â | â | â | â |
| Bukowiecki et al. | 2011 | 0.87(1) | 2.24 | â | 9 | â | â | â | â |
| van den Bergh | 2006 | 0.75 | 1.32 | â | 10 | â | â | â | â |
| Dias et al. | 2002 | 0.75 | 1.32 | â | 10 | â | â | â | â |
| Lynga | 1987 | 1.08 | 1.70 | â | 20 | â | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
MOCA


Almeida et al. (2025)
Mass determination: worst fit. Isochrone match: good fit.
Cavallo et al. (2024)
Gold sample.
Hunt & Reffert (2024)
Classified as open cluster. CMD class: 1.00 (50th percentile).
Richer et al. (2021)
The expected number of WDs is 18.0, 0 WD candidates found, and 0 WD candidates found in the wide search.