NGC 2352

(MWSC 1143; ESO 492 05)

0.16 UTI

0.0

C_N

0.03

C_dens

0.25

C_C3

0.26

C_lit

1.0

C_dup

N_m (P>50%) 15

Core radius and density 2.5 [pc], 0.1 [pc^-2]

C3 classification CC

C_N 0.0 Sparse
C_dens 0.03 Very loose
C_C3 0.25 Low quality
C_lit 0.26 Poorly studied
C_dup 1.0 Unique

📥 Members 📊 Colab 🔬 Bayestar19

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

Overview

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NGC 2352 is a sparse, very loose object of low C3 quality. Its parallax locates it at a large^* distance, below the mid-plane, affected by moderate extinction. It is catalogued as an intermediate-age cluster (see Parameters). It is poorly studied in the literature.

(*): The parallax distance estimate (~5.09 kpc) differs significantly from the median photometric distance (~3.00 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.

Distant Moderate extinction Intermediate age

Data

🔍 Search references for NGC 2352 in: SciX Simbad

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Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	99999–	108.339	-24.037	0.196	-1.192	2.232	58.726
Just et al.	2023	108.266	-24.027	–	–	–	–
Bica et al.	2019	108.277	-24.042	–	–	–	–
Dias et al.	2018	–	–	–	-1.38	1.55	–
Loktin & Popova	2017	108.27	-24.029	–	-4.011	4.591	–
Sampedro et al.	2017	108.271	-24.038	–	–	–	–
Kharchenko et al.	2016	108.266	-24.027	–	–	–	–
Tadross	2014	108.271	-24.038	–	–	–	–
Dias et al.	2014	108.271	-24.038	–	-2.13	4.3	–
Kharchenko et al.	2013	108.271	-24.029	–	-3.34	6.75	–
Dias et al.	2002	108.271	-24.038	–	-2.13	4.3	–

💡 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–	3.0	1.88	–	358	–	665	–	–
Just et al.	2023	–	–	–	596	–	665	–	–
Loktin & Popova	2017	8.32	1.88	–	46	–	–	–	–
Kharchenko et al.	2016	3.00	2.10	–	596	–	–	–	–
Tadross	2014	1.75	1.01	–	120	–	–	–	–
Kharchenko et al.	2013	3.00	2.10	–	596	–	–	–	–
Dias et al.	2002	1.75	1.01	–	120	–	–	–	–

Visualization

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