ESO 589 26
(MWSC 2786)
0.83
UTI
0.82
CN
1.0
Cdens
0.75
CC3
0.79
Clit
1.0
Cdup
Radius (P>50% members)
3.3 [arcmin]
- CN 0.82 Rich
- Cdens 1.0 Very dense
- CC3 0.75 High quality
- Clit 0.79 Well-studied
- Cdup 1.0 Unique
Overview
ESO 589 26 is a rich, very dense object of high C3 quality. Its parallax locates it at a moderate 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 and mass parameters (see Parameters). It is well-studied in the literature.
Relatively close
High extinction
Near-solar metallicity
Young
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | â | 270.562 | -21.927 | 0.337 | -0.174 | -2.717 | -0.316 |
| Almeida et al. | 2025 | 270.561 | -21.925 | â | â | â | â |
| Hunt & Reffert | 2024 | 270.56 | -21.918 | 0.329 | -0.164 | -2.729 | 12.017 |
| Cavallo et al. | 2024 | 270.56 | -21.934 | 0.325 | â | â | â |
| Hunt & Reffert | 2023 | 270.56 | -21.918 | 0.329 | -0.164 | -2.729 | 12.017 |
| Just et al. | 2023 | 270.562 | -21.918 | â | â | â | â |
| Dias et al. | 2021 | 270.561 | -21.925 | 0.325 | -0.203 | -2.694 | â |
| Cantat-Gaudin et al. | 2020 | 270.56 | -21.922 | 0.336 | -0.216 | -2.695 | â |
| Cantat-Gaudin & Anders | 2020 | 270.56 | -21.922 | 0.336 | -0.216 | -2.695 | â |
| Bica et al. | 2019 | 270.565 | -21.92 | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 270.56 | -21.922 | 0.336 | -0.216 | -2.695 | â |
| Kharchenko et al. | 2016 | 270.562 | -21.918 | â | â | â | â |
| Dias et al. | 2014 | 270.558 | -21.915 | â | 0.33 | -1.07 | â |
| Kharchenko et al. | 2013 | 270.57 | -21.917 | â | 4.56 | -4.12 | â |
| Dias et al. | 2002 | 270.558 | -21.915 | â | 4.56 | -4.12 | 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] | Bfr | BSS |
|---|---|---|---|---|---|---|---|---|---|
| Almeida et al. | 2025 | 2.17 | 3.17 | â | 249 | â | 713 | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 2478* | â | â |
| Cavallo et al. | 2024 | 2.34 | 4.49 | â | 89 | -1.160 | â | â | â |
| Hunt & Reffert | 2023 | 2.70 | 4.15 | 2.46 | 89 | â | â | â | â |
| Just et al. | 2023 | â | â | â | 3 | â | 455 | â | â |
| Dias et al. | 2021 | 2.17 | 3.17 | â | 249 | 0.386 | â | â | â |
| Cantat-Gaudin et al. | 2020 | 2.67 | 3.15 | â | 200 | â | â | â | â |
| Cantat-Gaudin & Anders | 2020 | 2.74 | â | â | â | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 2.74 | â | â | â | â | â | â | â |
| Kharchenko et al. | 2016 | 2.43 | 3.55 | â | 3 | â | â | â | â |
| Kharchenko et al. | 2013 | 2.43 | 3.55 | â | 3 | â | â | â | â |
| Dias et al. | 2002 | 2.43 | 3.55 | â | 3 | â | â | â | â |
(*): Indicates that this parameter is assigned more than one value in the corresponding reference.


Almeida et al. (2025)
Mass determination: invalid due to poor quality CMD. Isochrone match: worst fit.
Cavallo et al. (2024)
Silver sample.