Ruprecht 46
(MWSC 1418; OCL 637; ESO 561 08)
0.17
UTI
0.0
CN
0.07
Cdens
0.25
CC3
0.26
Clit
1.0
Cdup
Nm (P>50%)
22
Core radius and density
1.9 [pc], 0.4 [pc-2]
- CN 0.0 Sparse
- Cdens 0.07 Very loose
- CC3 0.25 Low quality
- Clit 0.26 Poorly studied
- Cdup 1.0 Unique
Overview
Ruprecht 46 is a sparse, very loose object of low C3 quality. Its parallax locates it at a moderate* distance, above the mid-plane, affected by low extinction. It is catalogued as a low-mass, near-solar metallicity, old cluster (see Parameters). It is poorly studied in the literature.
(*): The parallax distance estimate (~3.17 kpc) differs significantly from the median photometric distance (~1.47 kpc).
Note: This object contains blue stragglers according to at least one source.
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 | 120.542 | -19.454 | 0.315 | -1.087 | 0.226 | â |
| Just et al. | 2023 | 120.541 | -19.462 | â | â | â | â |
| Bica et al. | 2019 | 120.542 | -19.461 | â | â | â | â |
| Joshi et al. | 2016 | 120.547 | -19.465 | â | â | â | â |
| Kharchenko et al. | 2016 | 120.541 | -19.462 | â | â | â | â |
| Kharchenko et al. | 2013 | 120.547 | -19.465 | â | -6.78 | 1.83 | â |
| Ahumada & Lapasset | 2007 | 120.55 | -19.467 | â | â | â | â |
| van den Bergh | 2006 | 120.542 | -19.465 | â | â | â | â |
| Chen et al. | 2003 | 120.533 | -19.466 | â | â | â | â |
| Lynga | 1987 | 120.529 | -19.48 | 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 | 1.47 | 0.93 | â | 1652 | -0.150 | 23 | â | 62 |
| Just et al. | 2023 | â | â | â | 141 | â | 23 | â | â |
| Joshi et al. | 2016 | 1.47 | 1.64 | â | 141 | â | â | â | â |
| Kharchenko et al. | 2016 | 1.47 | 1.64 | â | 141 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.47 | 1.64 | â | 141 | â | â | â | â |
| Paunzen et al. | 2010 | â | â | â | â | -0.150 | â | â | â |
| Ahumada & Lapasset | 2007 | â | 0.22 | â | 3981 | â | â | â | 62 |
| van den Bergh | 2006 | 0.75 | 0.22 | â | 3981 | â | â | â | â |
| Chen et al. | 2003 | 0.75 | 0.22 | â | 3980 | -0.040(1) | â | â | â |
| Lynga | 1987 | â | â | â | 3162 | -0.200 | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
MOCA

Cantat-Gaudin & Anders (2020)
Density enhancement without meaningful CMD features; likely not a real cluster. More details in Appendix A of the article.
Bica et al. (2019)
Web updates in DAML02, some were later removed (2003 to 2010).
Ahumada & Lapasset (2007)
The red limit of the blue straggler area is (V-I)=0.78.
Dias et al. (2002)
Asterism (Carraro, G.; Patat, F. 1995, MNRAS 276, 563); cat V3.5 (Jan 2016)