Collinder 306

(NGC 6169; MWSC 2424; OCL 984; ESO 276 05; mu Nor)

0.18 UTI

0.0

C_N

0.07

C_dens

0.12

C_C3

0.35

C_lit

1.0

C_dup

N₅₀ (P>50% members) 13

Stellar density (N₅₀/rad) 0.4 [N/pc²]

C3 classification DC

C_N 0.0 Sparse
C_dens 0.07 Very loose
C_C3 0.12 Very low quality
C_lit 0.35 Poorly studied
C_dup 1.0 Unique

📥 Members 📊 Colab 🔬 Bayestar19

MOCA 🔍 CDS 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview

ℹ️

Collinder 306 is a sparse, very loose object of very low C3 quality. Its parallax locates it at a moderate^* distance, above the mid-plane, affected by moderate extinction. It is catalogued as a low-mass, young cluster (see Parameters). It is poorly studied in the literature.

(*): The parallax distance estimate (~3.18 kpc) differs significantly from the median photometric distance (~1.01 kpc).

⚠️ 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 Low mass Young

Cantat-Gaudin et al. (2020)
Listed in WEBDA but with no parameters. Multiple studies report inability to identify a real cluster. More details in Appendix A of the article.

Data

🔍 Search references for Collinder 306 in: SciX Simbad

ℹ️

Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	99999–	248.551	-44.088	0.315	-6.824	-4.742	-23.399
Just et al.	2023	248.517	-44.015	–	–	–	–
Bica et al.	2019	248.534	-44.054	–	–	–	–
Kharchenko et al.	2016	248.517	-44.015	–	–	–	–
Dias et al.	2014	248.517	-44.045	–	1.22	-1.04	6.3
Kharchenko et al.	2013	248.527	-44.016	–	0.69	-2.47	6.3
Dias et al.	2002	248.517	-44.045	–	1.22	-1.04	6.3

💡 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]	B_frac	BSS
UCC	99999–	1.01	2.26	–	32	–	28	–	–
Just et al.	2023	–	–	–	32	–	28	–	–
Kharchenko et al.	2016	1.01	2.26	–	32	–	–	–	–
Kharchenko et al.	2013	1.01	2.26	–	32	–	–	–	–
Dias et al.	2002	1.01	2.26	–	32	–	–	–	–

Visualization

ℹ️