CWNU 1091

0.13 UTI

0.27

C_N

0.11

C_dens

0.25

C_C3

0.0

C_lit

1.0

C_dup

C3 classification DB

Number of members (P>50%) 27

Radius (P>50% members) 127.8 [arcmin]

C_N 0.27 Poorly populated
C_dens 0.11 Very loose
C_C3 0.25 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 1091 is a poorly populated, very loose object of low C3 quality. Its parallax locates it at a very close distance, below the mid-plane, affected by low extinction. It is catalogued as an intermediate-age cluster (see Parameters). It is rarely studied in the literature.

Note: This object shares a significant 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.

Low extinction Intermediate age

Data

Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	–	333.23	12.605	5.255	15.085	-10.85	-2.469
He et al.	2022	332.61	12.116	5.238	14.904	-10.696	–

💡 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	–	0.25	–	126	–	–	–	–

💡 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
HSC 598	59.3	335.01	13.29	5.31	15.51	-11.2	5.54	0.06

💡 Note: The % column shows the percentage of members that CWNU 1091 shares with each listed object.

Visualization

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