CWWDL 13485

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0.05 UTI
0.0
CN
0.02
Cdens
0.25
CC3
0.0
Clit
1.0
Cdup
C3 classification CC
Number of members (P>50%) 10
Radius (P>50% members) 15.7 [arcmin]
  • CN 0.0 Sparse
  • Cdens 0.02 Very loose
  • CC3 0.25 Low quality
  • Clit 0.0 Rarely studied
  • Cdup 1.0 Unique
📥 Members 📊 Colab 🔬 Bayestar19 🔍 SciX 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview
CWWDL 13485 is a sparse, very loose object of low C3 quality. Its parallax locates it at a moderate distance, near the mid-plane. It is catalogued as a near-solar metallicity, young cluster (see Parameters). It was recently reported in the literature.

⚠️ 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.

Near-solar metallicity Young

Data
Reference Year RA [deg] DEC [deg] Plx [mas] pmRA [mas/yr] pmDE [mas/yr] Rv [km/s]
UCC – 284.147 -0.776 0.461 -0.343 -2.814 23.17
Chi et al. 2023 284.236 -0.745 0.478 -0.371 -2.863 40.574

💡 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
Chi et al. 2023 – – – 29 0.440 – – –

💡 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
CWWDL 13485 UCC
Galactocentric position diagram

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