Saurer 3
(MWSC 1839)
0.59
UTI
0.76
CN
0.81
Cdens
0.75
CC3
0.32
Clit
1.0
Cdup
Nm (P>50%)
130
Core radius and density
1.9 [pc], 4.0 [pc-2]
- CN 0.76 Rich
- Cdens 0.81 Dense
- CC3 0.75 High quality
- Clit 0.32 Poorly studied
- Cdup 1.0 Unique
π₯ Members
π Colab
π¬ Bayestar19
MOCA
π CDS
π Simbad
π CDS (Ξ±, Ξ΄)
π Simbad (Ξ±, Ξ΄)
MOCA
π CDS
π Simbad
π CDS (Ξ±, Ξ΄)
π Simbad (Ξ±, Ξ΄)
Overview
Saurer 3 is a rich, dense object of high C3 quality. Its parallax locates it at a large distance, above the mid-plane, affected by moderate extinction. It is catalogued as a very massive, near-solar metallicity, old cluster, but with a large variance across recent sources for the age, metallicity, and mass parameters (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 | 99999β | 160.354 | -55.29 | 0.142 | -6.682 | 3.263 | 39.802 |
| Hu & Soubiran | 2025 | 160.394 | -55.303 | β | β | β | β |
| Hunt & Reffert | 2024 | 160.348 | -55.288 | 0.108 | -6.681 | 3.262 | β |
| Cavallo et al. | 2024 | 160.394 | -55.303 | 0.13 | β | β | β |
| He et al. | 2023 | 160.351 | -55.29 | 0.135 | -6.668 | 3.259 | β |
| Hunt & Reffert | 2023 | 160.348 | -55.288 | 0.108 | -6.681 | 3.262 | β |
| Perren et al. | 2022 | 160.375 | -55.3 | β | β | β | β |
| SΓ‘nchez et al. | 2020 | 160.354 | -55.306 | β | -6.836 | 3.34 | β |
| Bica et al. | 2019 | 160.339 | -55.288 | β | β | β | β |
| Sampedro et al. | 2017 | 160.354 | -55.306 | β | -5.81 | -2.9 | β |
| Dias et al. | 2014 | 160.354 | -55.306 | β | -6.73 | -1.62 | β |
| van den Bergh | 2006 | 160.375 | -55.3 | β | β | β | β |
| Dias et al. | 2002 | 160.354 | -55.306 | β | -6.73 | -1.62 | β |
π‘ 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 | 99999β | 6.76 | 2.3 | 1.56 | 2138 | -0.100 | 7313 | 0.86 | β |
| Hu & Soubiran | 2025 | β | β | β | β | -0.330(5) | β | β | β |
| Hunt & Reffert | 2024 | 5.65 | 2.47 | 1.56 | 1034 | β | 626(1) | β | β |
| Cavallo et al. | 2024 | 10.23 | 1.91 | β | 2138 | -0.100 | β | β | β |
| He et al. | 2023 | 6.76 | 2.30 | β | 2512 | β | β | β | β |
| Hunt & Reffert | 2023 | 5.65 | 2.47 | 1.56 | 1033 | β | β | β | β |
| Perren et al. | 2022 | 6.14 | 2.24 | β | 6457 | 0.020 | 14000 | 0.86 | β |
| van den Bergh | 2006 | 8.83 | 1.96 | β | 2818 | β | β | β | β |
| Dias et al. | 2002 | 9.55 | 2.40 | β | 1995 | β | β | β | β |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
Cavallo et al. (2024)
Gold sample.
Hunt & Reffert (2024)
Classified as open cluster. CMD class: 0.75 (50th percentile).
Hunt & Reffert (2023)
Classified as open cluster. CMD class: 0.75 (50th percentile).
Perren et al. (2022)
Also known as Saurer C; poorly studied. The CMD shows a dispersed sequence with the TO at G~19 and a clear RC at G=16.5. Members are scattered around the short main sequence, likely due to increasing Gaia photometric errors at G>19. ASteCA gives 6.1 kpc, 6.5 Gyr, and the largest binary fraction in the sample (~86%). Carraro 2003 used CCD VI photometry and reported 9.5 kpc and ~2 Gyr β both differ substantially from our values, likely because their CMD suffers from severe field star contamination spanning a broader but unreliable sequence. MWSC (7.1 kpc) is the closest catalog value. The cluster lies below 9 kpc, contradicting OC02 (~9.5 kpc, sourced from Carraro 2003).