CWNU 1157

0.01 UTI

0.0

C_N

0.25

C_dens

0.38

C_C3

0.0

C_lit

0.04

C_dup

C3 classification CB

Number of members (P>50%) 24

Radius (P>50% members) 11.8 [arcmin]

C_N 0.0 Sparse
C_dens 0.25 Loose
C_C3 0.38 Low quality
C_lit 0.0 Rarely studied
C_dup 0.04 Very likely duplicate

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

Overview

CWNU 1157 is a sparse, loose object of low C3 quality. Its parallax locates it at a relatively close distance, below the mid-plane, affected by low extinction. It is catalogued as a young 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.

Low extinction Young

Data

Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	–	106.528	-16.108	0.785	-3.106	1.781	37.615
He et al.	2022	106.501	-16.058	0.802	-3.111	1.797	–

💡 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	–	0.70	–	71	–	–	–	–

💡 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
Alessi 72	96.0	106.62	-16.16	0.76	-3.09	1.77	36.4	0.34

💡 Note: The % column shows the percentage of members that CWNU 1157 shares with each listed object.

Visualization

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