CWNU 126

0.22 UTI

0.27

C_N

0.48

C_dens

0.38

C_C3

0.0

C_lit

1.0

C_dup

C3 classification CB

Number of members (P>50%) 27

Radius (P>50% members) 6.2 [arcmin]

C_N 0.27 Poorly populated
C_dens 0.48 Loose
C_C3 0.38 Low quality
C_lit 0.0 Rarely studied
C_dup 1.0 Unique

📥 Members 📊 Colab 🔬 Bayestar19 🔍 SciX 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview

CWNU 126 is a poorly populated, loose object of low C3 quality. Its parallax locates it at a relatively close distance, near the mid-plane, affected by moderate extinction. It is catalogued as a near-solar metallicity, young cluster (see Parameters). It is rarely studied in the literature.

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

⚠️ Warning: the low UTI value and no obvious signs of duplication (C_dup=1.0) indicate that this is quite probably an asterism, moving group, or artifact, and not a real open cluster.

Relatively close Moderate extinction Near-solar metallicity Young

Data

Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	–	85.482	30.278	0.536	0.47	-2.485	–
He et al.	2022	85.47	30.265	0.53	0.47	-2.48	–

💡 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	1.82	2.28	–	25	0.169	–	–	–

💡 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.

Cluster	%	RA	DEC	Plx	pmRA	pmDE	Rv	UTI
Theia 1798	100.0	85.47	30.28	0.53	0.47	-2.48	-41.97	0.08

💡 Note: The % column shows the percentage of members that CWNU 126 shares with each listed object.

Visualization

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