NGC 188

(Melotte 2; Collinder 6; MWSC 74; OCL 309; FoF 651)

1.0 UTI

1.0

C_N

1.0

C_dens

1.0

C_C3

1.0

C_lit

1.0

C_dup

N₅₀ (P>50% members) 1337

Stellar density (N₅₀/rad) 63.2 [N/pc²]

C3 classification AA

C_N 1.0 Very rich
C_dens 1.0 Very dense
C_C3 1.0 Very high quality
C_lit 1.0 Very well-studied
C_dup 1.0 Unique

📥 Members 📊 Colab 🔬 Bayestar19

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

Overview

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NGC 188 is a very rich, very dense object of very high C3 quality. Its parallax locates it at a relatively close distance, well above the mid-plane, affected by low extinction. It is catalogued as a massive, near-solar metallicity, very old cluster, but with a large variance across recent sources for the metallicity and mass parameters (see Parameters). It is very well-studied in the literature.

Note: This object contains blue stragglers according to at least one source.

Note: This object shares a large percentage of members with a later reported entry. See table with shared members information.

Relatively close Low extinction Massive Near-solar metallicity Very old Contains BSS

Almeida et al. (2025)
Mass determination: good fit. Isochrone match: good fit. Gold sample.

Cavallo et al. (2024)
Gold sample.

Hunt & Reffert (2024)
Classified as open cluster. CMD class: 1.00 (50th percentile).

Rain et al. (2024)
Well-studied BSSs are distributed across regions intersected by multiple binary evolution tracks, reinforcing the interpretation that many BSSs far from the ZAMS originate from binary evolution.

Ahumada & Lapasset (2007)
Membership probabilities according to (2003AJ....126.2922P) and (1972AJ.....77...74U): star 1003, 90%; 1032, 98%; 1043, 98%; 1050, 97%; 1093, 98%; 1102, 98%; 2008, 97%; 2020, 97%; 2024, 97%; 2031, 93%; 2046, 99%; 2069, 98%; 2074, 92%; 2082, 98%; 2105, 98%; 2119, 93%; 2127, 98%; 2138, 94%; 2151, 97%; 3074, 95%; 3115, 98%; 3135, 93%; 3151, 98%. Star 2189 is given 90% in (1972AJ.....77...74U) but 0% in (2003AJ....126.2922P). In the photometric study (1969ApJ...158..669E) the following stars are cited as blue stragglers: 1003, 1005, 1032, 1033, 1043, 1093, 1102, 1103, 1112, and 2046. Star 2127 is a W Ursae Majoris eclipsing binary (2003AJ....126..276K). An hyphothetical relation between the blue stragglers and the apparent lack of bright giants in the cluster nucleus is discussed in (1990AcA....40...61K). In (1989AJ.....97..759T) and (1972AJ.....77...74U) it is suggested that the cluster is somewhat younger than is usually agreed, so several stars that appear as blue stragglers would not be such. In the proper motion study (1996AJ....111.1205D) it is found that the stragglers are not more centrally concentrated than the red giants. In the CCD study (1990AcA....40...61K) the discovery of a probable FK Comae variable (star V8) is reported; this star may be a `red straggler' candidate.

Data

🔍 Search references for NGC 188 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–	11.786	85.243	0.525	-2.32	-1.007	-41.837
Otto et al.	2026	11.837	85.251	–	-2.31	-0.96	-41.9
Nizovkina et al.	2025	11.837	85.251	–	–	–	–
Li et al.	2025	11.798	85.244	0.507	-2.307	-0.96	–
Guerco et al.	2025	12.0	85.2	0.52	-2.34	-1.04	-41.8
Hu & Soubiran	2025	11.858	85.25	–	–	–	–
Wei et al.	2025	11.729	85.239	0.522	-2.305	-0.962	–
Carrasco-Varela et al.	2025	12.536	85.322	–	–	–	–
Almeida et al.	2025	11.824	85.241	–	–	–	–
Hunt & Reffert	2024	11.837	85.251	0.523	-2.318	-1.015	-41.127
Cavallo et al.	2024	11.858	85.25	0.523	–	–	–
Rain et al.	2024	11.775	85.243	0.526	-2.322	-1.015	–
Hunt & Reffert	2023	11.837	85.251	0.523	-2.318	-1.015	-41.127
Angelo et al.	2023	11.825	85.233	–	-2.32	-1.01	–
Cordoni et al.	2023	11.824	85.241	0.509	-2.302	-0.955	–
Just et al.	2023	11.821	85.252	–	–	–	–
Jadhav & Subramaniam	2021	11.798	85.244	–	–	–	–
Jaehnig et al.	2021	11.786	85.244	0.537	-2.308	-0.952	–
Rain et al.	2021	11.798	85.244	0.507	-2.307	-0.96	–
Dias et al.	2021	11.824	85.241	0.509	-2.302	-0.955	-41.602
Spina et al.	2021	11.791	85.244	0.509	-2.303	-0.953	–
Cantat-Gaudin et al.	2020	11.798	85.244	0.507	-2.307	-0.96	–
Sánchez et al.	2020	11.867	85.255	–	-2.415	-1.032	–
Donor et al.	2020	11.85	85.255	–	-2.33	-0.92	-41.4
Cantat-Gaudin & Anders	2020	11.798	85.244	0.507	-2.307	-0.96	–
Liu & Pang	2019	11.767	85.245	0.508	-2.308	-0.95	–
Bossini et al.	2019	11.798	85.244	–	–	–	–
Soubiran et al.	2018	11.798	85.244	–	–	–	-41.7
Bica et al.	2019	11.943	85.261	–	–	–	–
Cantat-Gaudin et al.	2018	11.798	85.244	0.507	-2.307	-0.96	–
Angelo et al.	2019	12.004	85.246	–	–	–	–
Loktin & Popova	2017	11.865	85.255	–	0.554	-1.476	-45.0
Kharchenko et al.	2016	11.821	85.252	–	–	–	–
Dias et al.	2014	11.867	85.255	–	-3.0	-0.37	–
Kharchenko et al.	2013	11.85	85.255	–	0.15	-1.43	-45.0
Gozha et al.	2012	11.867	85.255	–	–	–	–
Kharchenko et al.	2012	11.85	85.255	–	0.11	-1.84	-45.0
Bukowiecki et al.	2011	11.733	85.244	–	–	–	–
Kharchenko et al.	2007	11.86	85.25	–	0.14	–	–
Ahumada & Lapasset	2007	11.875	85.25	–	–	–	–
van den Bergh	2006	12.108	85.255	–	–	–	–
Chen et al.	2003	11.242	85.35	–	-1.48	-0.56	-44.0
Dias et al.	2002	11.867	85.255	–	-0.21	0.17	-42.35
Lynga	1987	11.135	85.33	–	–	–	-50.0
Sulentic et al.	1973	11.11	85.337	–	–	–	–

💡 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–	1.86	0.25	0.43	5164	0.089	3295	0.48	18
Otto et al.	2026	–	–	–	7079	0.080⁽¹⁵⁾	–	–	–
Nizovkina et al.	2025	1.76⁽⁴⁾	0.39⁽⁴⁾	–	5164⁽⁴⁾	-0.093⁽⁴⁾	–	–	–
Li et al.	2025	1.82	0.26	–	6352	0.062	–	–	–
Guerco et al.	2025	–	–	–	7080	0.070	–	–	–
Hu & Soubiran	2025	–	–	–	–	-0.100⁽⁵⁾	–	–	–
Wei et al.	2025	2.00	0.31	–	3550	0.250	1660	0.48	–
Carrasco-Varela et al.	2025	1.86	0.23	–	6194	0.200	–	–	18⁽¹⁾
Almeida et al.	2025	1.86	0.23	–	6194	–	3478	–	–
Hunt & Reffert	2024	–	–	–	–	–	3655⁽¹⁾	–	–
Cavallo et al.	2024	1.79	0.32	–	3802	0.180	–	–	–
Rain et al.	2024	1.74	0.25	–	7904	–	14860	0.33	–
Hunt & Reffert	2023	1.83	0.23	0.43	2630	–	–	–	–
Angelo et al.	2023	1.70	0.35	–	6310	0.050	26⁽¹⁾	–	–
Cordoni et al.	2023	1.86	0.23	–	6194	0.112	1583	0.51	17⁽¹⁾
Just et al.	2023	–	–	–	4467	–	3112	–	–
Spina et al.	2022	–	–	–	–	0.090	–	–	–
Jadhav & Subramaniam	2021	1.70	0.21	–	7079	–	7464	–	14⁽¹⁾
Jaehnig et al.	2021	1.87⁽¹⁾	–	–	–	–	–	–	–
Rain et al.	2021	1.86	0.11	–	7586	–	–	–	22
Dias et al.	2021	1.86	0.23	–	6194	0.112	–	–	–
Spina et al.	2021	1.97	–	–	7079	0.088⁽²⁰⁾	–	–	–
Cantat-Gaudin et al.	2020	1.70	0.21	–	7079	–	–	–	–
Kounkel et al.	2020	1.85	0.40	–	4786	–	–	–	–
Donor et al.	2020	–	–	–	–	0.090	–	–	–
Cantat-Gaudin & Anders	2020	1.86	–	–	–	–	–	–	–
Liu & Pang	2019	–	–	–	4370	0.250	–	–	–
Bossini et al.	2019	1.67	0.08	–	7534	0.110	–	–	–
Soubiran et al.	2018	1.86	–	–	–	–	–	–	–
Cantat-Gaudin et al.	2018	1.86	–	–	–	–	–	–	–
Angelo et al.	2019	1.82	–	–	7080	–	323	–	–
Loktin & Popova	2017	2.10	0.28	–	4130	–	–	–	–
Kharchenko et al.	2016	2.00	0.27	–	4467	–	–	–	–
Kharchenko et al.	2013	2.00	0.27	–	4467	-0.010	–	–	–
Bukowiecki et al.	2012	–	–	–	–	–	3902	–	–
Gozha et al.	2012	2.05	–	–	4285	0.120	–	–	–
Kharchenko et al.	2012	2.00	0.27	–	4467	-0.010	–	–	–
Bukowiecki et al.	2011	2.08⁽¹⁾	0.22	–	3162	–	–	–	–
Ahumada & Lapasset	2007	–	0.25	–	4266	–	–	–	24
van den Bergh	2006	2.05	0.25	–	4266	–	–	–	–
Chen et al.	2003	2.05	0.26	–	4280	-0.020⁽¹⁾	–	–	–
Dias et al.	2002	1.71	0.11	–	7586	0.120	–	–	–
Lynga	1987	1.55	0.13	–	5012	-0.060	–	–	–

(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.

Cluster	%	RA	DEC	Plx	pmRA	pmDE	Rv	UTI
CWWDL 3252	76.1	11.78	85.24	0.53	-2.32	-1.02	-42.0	0.0

💡 Note: The % column shows the percentage of members that NGC 188 shares with each listed object.

Visualization

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