Ruprecht 3

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0.05 UTI
0.0
CN
0.02
Cdens
0.25
CC3
0.0
Clit
1.0
Cdup
Stellar density (N50/rad) 0.1 [N/pc2]
  • CN 0.0 Sparse
  • Cdens 0.02 Very loose
  • CC3 0.25 Low quality
  • Clit 0.0 Rarely studied
  • Cdup 1.0 Unique

Overview

â„šī¸
Ruprecht 3 is a sparse, very loose object of low C3 quality. Its parallax locates it at a large* distance, well below the mid-plane, affected by low extinction. It is catalogued as a low-mass, old cluster (see Parameters). It is rarely studied in the literature, with no articles listed in the last 7 years.

(*): The parallax distance estimate (~6.63 kpc) differs significantly from the median photometric distance (~1.56 kpc).

Note: This object shares a very small percentage of members with a later reported entry. See table with shared members information.

âš 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.

Cantat-Gaudin & Anders (2020)
Appears as a tight group of bright stars, but Gaia DR1 and DR2 parallaxes and proper motions show it is an asterism. More details in Appendix A of the article.

Data

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Reference Year RA [deg] DEC [deg] Plx [mas] pmRA [mas/yr] pmDE [mas/yr] Rv [km/s]
UCC 99999– 100.479 -29.466 0.151 -0.874 1.535 –
Angelo et al. 2019 100.533 -29.452 – – – –
Bukowiecki et al. 2011 100.529 -29.452 – – – –

💡 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 99999– 1.56 0.0 – 1449 – 24 – –
Angelo et al. 2019 2.29 – – 1120 – 24 – –
Bukowiecki et al. 2011 0.83(1) 0.00 – 1778 – – – –

(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.

Cluster % RA DEC Plx pmRA pmDE Rv UTI
Ruprecht 2 4.0 100.3 -29.51 0.12 -0.47 1.79 69.32 0.17

💡 Note: The % column shows the percentage of members that Ruprecht 3 shares with each listed object.

Visualization

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