CWNU 1

0.00 UTI

0.32

C_N

1.0

C_dens

0.75

C_C3

0.0

C_lit

0.0

C_dup

C3 classification BA

Number of members (P>50%) 32

Radius (P>50% members) 3.0 [arcmin]

C_N 0.32 Poorly populated
C_dens 1.0 Very dense
C_C3 0.75 High quality
C_lit 0.0 Rarely studied
C_dup 0.0 Very likely duplicate

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

Overview

CWNU 1 is a poorly populated, very dense object of high C3 quality. Its parallax locates it at a relatively close distance, near the mid-plane, affected by high extinction. It is catalogued as a metal-poor, intermediate-age cluster (see Parameters). It is rarely studied in the literature.

⚠️ Warning: This is very likely a duplicate object, which shares a large percentage of members with at least one previously reported entry. See table with shared members information.

Relatively close High extinction Metal-poor Intermediate age

Data

Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	–	259.266	-41.693	0.6	-0.04	-3.595	-30.225
He et al.	2022	259.257	-41.692	0.6	-0.03	-3.58	-18.1

💡 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	1.32	3.12	–	200	-0.642	–	–	–

💡 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
UBC 1563	100.0	259.26	-41.7	0.6	-0.05	-3.59	-30.23	0.65
CWWDL 13348	84.4	259.26	-41.7	0.6	-0.03	-3.59	-39.28	0.0

💡 Note: The % column shows the percentage of members that CWNU 1 shares with each listed object.

Visualization

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