CWNU 1037

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0.17 UTI
0.0
CN
0.12
Cdens
0.75
CC3
0.0
Clit
1.0
Cdup
C3 classification AB
Number of members (P>50%) 21
Radius (P>50% members) 42.7 [arcmin]
  • CN 0.0 Sparse
  • Cdens 0.12 Very loose
  • CC3 0.75 High quality
  • Clit 0.0 Rarely studied
  • Cdup 1.0 Unique
📥 Members 📊 Colab 🔬 Bayestar19 🔍 SciX 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview
CWNU 1037 is a sparse, very loose object of high C3 quality. Its parallax locates it at a very close distance, near the mid-plane, affected by low extinction. It is catalogued as a young cluster (see Parameters). It is rarely studied 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.

Low extinction Young

Data
Reference Year RA [deg] DEC [deg] Plx [mas] pmRA [mas/yr] pmDE [mas/yr] Rv [km/s]
UCC – 127.767 -44.508 2.083 -6.628 6.96 13.05
He et al. 2022 127.896 -44.449 2.075 -6.608 6.96 –

💡 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
He et al. 2022 – 0.50 – 50 – – – –

💡 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
CWNU 1037 UCC
Galactocentric position diagram

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