VVVX CL024

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0.03 UTI
0.0
CN
0.03
Cdens
0.12
CC3
0.0
Clit
1.0
Cdup
C3 classification DC
Number of members (P>50%) 13
Radius (P>50% members) 6.9 [arcmin]
  • CN 0.0 Sparse
  • Cdens 0.03 Very loose
  • CC3 0.12 Very low quality
  • Clit 0.0 Rarely studied
  • Cdup 1.0 Unique
📥 Members 📊 Colab 🔬 Bayestar19 🔍 SciX 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview
VVVX CL024 is a sparse, very loose object of very low C3 quality. Its parallax locates it at a moderate* distance, below the mid-plane. It is catalogued as a cluster (see Parameters). It is rarely studied in the literature, with no articles listed in the last 8 years.

(*): The parallax distance estimate (~4.46 kpc) differs significantly from the median photometric distance (~2.66 kpc).

⚠️ 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.

Relatively close

Borissova et al. (2018): Open cluster.

Data
Reference Year RA [deg] DEC [deg] Plx [mas] pmRA [mas/yr] pmDE [mas/yr] Rv [km/s]
UCC – 224.255 -61.564 0.224 -5.484 -3.042 -45.818
Borissova et al. 2018 224.245 -61.592 0.228 -5.432 -3.023 –

💡 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
Borissova et al. 2018 2.66 – – – – – – –

💡 Note: The parameters are sometimes transformed from their original values to match the format of the columns shown here, see FAQ. The columns DAv, Bfr, BSS correspond to differential extinction, binary fraction, and blue stragglers, respectively. BSS values can be listed as fractions or integers.

Visualization
VVVX CL024 UCC
Galactocentric position diagram

💡 Note: How are the galactocentric plots generated? See FAQ.