NGC 2682

(Melotte 94; Collinder 204; MWSC 1585; Messier 67; M 67; OCL 549)

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1.0 UTI
1.0
CN
1.0
Cdens
1.0
CC3
1.0
Clit
1.0
Cdup
Nm (P>50%) 1650
Core radius and density 1.2 [pc], 48 [pc-2]
C3 classification AA
  • CN 1.0 Very rich
  • Cdens 1.0 Very dense
  • CC3 1.0 Very high quality
  • Clit 1.0 Very well-studied
  • Cdup 1.0 Unique
đŸ“Ĩ Members 📊 Colab đŸ”Ŧ Bayestar19 MOCAMOCA 🔍 CDS 🔍 Simbad 🔍 CDS (Îą, δ) 🔍 Simbad (Îą, δ)

Overview
ℹī¸
NGC 2682 is a very rich, very dense object of very high C3 quality. Its parallax locates it at a close distance, above the mid-plane, affected by low extinction. It is catalogued as a massive, near-solar metallicity, old cluster, but with a large variance across recent sources for the absorption, 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 significant percentage of members with 7 later reported entries. See table with shared members information.

Malhotra et al. (2026)
Lowest/Highest stellar mass in the catalogue with a mass-ratio estimate: 0.44/1.2 Msun

Yan et al. (2026)
Number of WDs: expected from single-star evolution N=244, with probability of formation through binary evolution >=0.5 N=2.

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

Cavallo et al. (2024)
Gold sample.

Hunt & Reffert (2024)
Classified as open cluster. CMD class: 0.98 (50th percentile).

Rain et al. (2024)
Many BSSs are known binaries, consistent with their close match to binary evolution tracks. Two YSSs are also present and interpreted as evolved binary systems.

Hunt & Reffert (2023)
Classified as open cluster. CMD class: 0.98 (50th percentile).

Hu et al. (2021)
Ellipticities (core, all): e_core=0.25, e_all=0.12.

Ahumada & Lapasset (2007)
= M67. This cluster has a number of well-known blue stragglers, a detailed spectral analysis of which can be found in (1991A&A...245..467M). The photometry listed in (1989RMxAA..17...31S) was used; it includes all the stars with a membership probability greater than 50% according to the proper motion study (1977A&AS...27...89S). The adopted cluster centre is star 1023 of (1977A&AS...27...89S). All the stars with probability greater than 80% are listed in our catalogue. Note that the WEBDA numbers are the often-quoted Fagerholm numbers (e.g.: star 1284 = F190). The following are the membership probabilities: star 145(94%), 277(93%), 740(87%), 751(96%), 752(95%), 821(89%), 856(90%), 968(95%), 975(90%), 977(93%), 984(95%), 997(93%), 1005(95%), 1031(91%), 1036(91%), 1066(90%), 1072(95%), 1082(99%), 1165 (93%), 1183(95%), 1195(96%), 1263(89%), 1267(93%), 1273(91%), 1280(93%), 1284(95%), 1434(91%), 1440(94%), 1947(86%), 2204 (83%). Most of these stars are also catalogued as stragglers by (1994AJ....108.1828M). A possible relation between the blue stragglers and the `clump' stars is discussed in (1981ApJ...247..503E). In the IR study (1984ApJ...279..237P) of the five bluest stragglers, two of them (1284 and 1434) are found to show infrared excesses that are interpreted as signs of the presence of evolved companions (i.e. they may be Algol-type binaries). In the case of 1284, the binary character has received support from the discovery of radial velocity variations, which have been interpreted (1992PASP..104.1268M) as manifestations of a binary of period 4.18 days and eccentricity 0.205. This star is a good example in support of the mass transfer theory to explain some stragglers (1992PASP..104.1268M). However, star 977 is above the magnitude limit that the same theory predicts, although its membership is under discussion (1991A&A...245..467M). Stars 1280 and 1284 are small-amplitude pulsating variables of Delta Sct type (1992AJ....103.1945G). In (1986AJ.....92.1364M) it is shown that the spatial distribution of the blue stragglers (strong central concentration) is similar to that of the cluster binaries;an evolutionary relation between the two populations is suggested (1986AJ.....92.1364M). Stars 997 (2004A&A...418..509V) and 1082 (1993A&A...269..175B) are X-ray sources; star 1082 is also a triple star, two components of which would be blue stragglers (2003AJ....125..810S). Several `red stragglers' are pointed out in (1989AJ.....97..431E), and in (1986AJ.....92.1364M) star F136 is associated with an evolutionary stage related to the blue strag- glers (it is a binary star).Through the determination of lithium abundances on some stragglers, a form of mixing affecting their external layers has been proposed (1981ApJ...247..503E). Star 984 would not be an unresolved pair,but a single, `genuine' blue straggler (2000AJ....120.1913S). These authors analyse high-resolution spectra of stragglers and main-sequence turnoff stars, and find that their metallicities and abundance ratios are not significantly different. Based on arguments from hydrodynamical models of stellar collisions, they claim that the upper limits for the lithium abundances of all blue stragglers are consistent with a formation process without mixing. In reference (1997ApJ...481L..93L) is made a detailed analysis of the spectroscopic binary and `red straggler' 1040 (ref. 352), and it is proposed that it originated as a short-period binary and evolved through a blue straggler phase to its present state. According to (1998AJ....116..789L), stars 975 and 1082 have hot subluminous companions; this is confirmed for star 1082 in (1999A&A...347..866V).

Data
🔍 Search references for NGC 2682 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– 132.847 11.818 1.152 -10.97 -2.914 33.912
Yan et al. 2026 132.85 11.817 1.15 -10.965 -2.906 –
Malhotra et al. 2026 132.848 11.815 – – – –
Bijavara Seshashayana et al. 2025 132.959 11.769 – – – –
Otto et al. 2026 132.85 11.817 – -10.99 -2.96 34.3
Nizovkina et al. 2025 132.85 11.817 – – – –
Li et al. 2025 132.846 11.814 1.135 -10.986 -2.964 –
Guerco et al. 2025 133.0 11.8 1.15 -11.0 -2.92 34.2
Hu & Soubiran 2025 132.839 11.827 – – – –
Yang et al. 2025 132.85 11.817 – – – –
Wei et al. 2025 132.846 11.824 1.153 -10.976 -2.919 –
Carrasco-Varela et al. 2025 133.07 11.731 – – – –
Almeida et al. 2025 132.848 11.814 – – – –
Alfonso et al. 2024 132.845 11.822 1.112 -10.971 -2.922 –
Zhang et al. 2024 132.85 11.817 – – – –
Hunt & Reffert 2024 132.85 11.817 1.15 -10.965 -2.906 33.767
Cavallo et al. 2024 132.839 11.827 1.151 – – –
Rain et al. 2024 132.846 11.82 1.152 -10.971 -2.913 –
Hunt & Reffert 2023 132.85 11.817 1.15 -10.965 -2.906 33.767
Almeida et al. 2023 132.835 11.813 – – – –
Angelo et al. 2023 132.871 11.837 – -10.96 -2.91 –
Cordoni et al. 2023 132.848 11.814 1.138 -11.001 -2.963 –
Just et al. 2023 132.84 11.818 – – – –
He et al. 2022 132.845 11.819 1.153 -10.972 -2.922 –
Tarricq et al. 2022 132.855 11.813 1.15 -10.969 -2.919 –
Jadhav & Subramaniam 2021 132.846 11.814 – – – –
Jaehnig et al. 2021 132.843 11.818 1.162 -10.962 -2.955 –
Netopil et al. 2022 132.825 11.8 – – – 34.18
Rain et al. 2021 132.846 11.814 1.135 -10.986 -2.964 –
Dias et al. 2021 132.848 11.814 1.138 -11.001 -2.963 34.045
Spina et al. 2021 132.841 11.816 1.136 -10.985 -2.961 –
Cantat-Gaudin et al. 2020 132.846 11.814 1.135 -10.986 -2.964 –
Donor et al. 2020 132.847 11.815 – -11.05 -2.98 33.9
Zhong et al. 2020 132.846 11.814 – -10.986 -2.964 28.145
Cantat-Gaudin & Anders 2020 132.846 11.814 1.135 -10.986 -2.964 –
Bossini et al. 2019 132.846 11.814 – – – –
Soubiran et al. 2018 132.846 11.814 – – – 33.8
Bica et al. 2019 132.847 11.834 – – – –
Cantat-Gaudin et al. 2018 132.846 11.814 1.135 -10.986 -2.964 –
Angelo et al. 2019 132.838 11.813 – – – –
Dias et al. 2018 – – – -10.21 -3.0 –
Dib et al. 2018 132.847 11.815 – – – –
Loktin & Popova 2017 132.825 11.801 – -9.4 -4.87 33.6
Sampedro et al. 2017 132.825 11.8 – -8.4 -4.47 –
Joshi et al. 2016 132.847 11.815 – – – –
Kharchenko et al. 2016 132.84 11.818 – – – –
Netopil et al. 2016 132.825 11.8 – – – –
Dias et al. 2014 132.825 11.8 – -9.4 -4.87 –
Kharchenko et al. 2013 132.847 11.815 – -7.31 -5.92 33.6
Gozha et al. 2012 132.825 11.8 – – – –
Bukowiecki et al. 2011 132.85 11.807 – – – –
Piskunov et al. 2008 132.849 11.807 – – – –
Kharchenko et al. 2007 132.82 11.8 – 0.31 – 32.3
Piskunov et al. 2007 132.849 11.807 – – – –
Ahumada & Lapasset 2007 132.825 11.8 – – – –
van den Bergh 2006 132.825 11.8 – – – –
Kharchenko et al. 2005 132.85 11.8 – -8.31 -4.81 32.3
Kharchenko et al. 2003 132.87 11.84 – -8.83 -4.96 –
Chen et al. 2003 132.716 11.813 – -6.47 -6.27 33.6
Dias et al. 2002 132.825 11.8 – -9.4 -4.87 33.62
Lynga 1987 132.619 11.816 – – – 32.0
Sulentic et al. 1973 132.767 11.806 – – – –

💡 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] Bfrac BSS
UCC 99999– 0.86 0.13 0.56 3549 0.010 1083 0.37 9
Yan et al. 2026 – – – 4265 – – – –
Malhotra et al. 2026 0.86 0.11 – 3548 0.020 – – –
Bijavara Seshashayana et al. 2025 – 0.07 – 4270 0.010(14) – – –
Otto et al. 2026 – – – 4266 0.010(15) – – –
Nizovkina et al. 2025 0.83(4) 0.12(4) – 4188(4) -0.041(4) – – –
Li et al. 2025 0.85 0.13 – 4130 -0.018 – – –
Guerco et al. 2025 – – – 4270 0.000 – – –
Hu & Soubiran 2025 – – – – -0.160(5) – – –
Yang et al. 2025 – – – 1698 -0.040(3) – – –
Wei et al. 2025 0.78 0.00 – 2050 0.250 1750 0.26 –
Carrasco-Varela et al. 2025 0.86 0.13 – 3758 0.150 – – 9(1)
Almeida et al. 2025 0.86 0.13 – 3758 – 1327 – –
Alfonso et al. 2024 0.89 0.07 – 3590 0.073 – – –
Zhang et al. 2024 – – – – 0.013(1) – – –
Hunt & Reffert 2024 0.82 0.10 0.56 1688 – 2779(1) – –
Cavallo et al. 2024 0.85 0.18 – 2512 0.320 – – –
Rain et al. 2024 0.80 0.08 – 5208 – 7437 0.24 –
Hunt & Reffert 2023 0.82 0.10 0.56 1687 – – – –
Almeida et al. 2023 0.84 0.16 – 3784 -0.045 1843(1) 0.56 –
Angelo et al. 2023 0.74 0.16 – 4467 0.000 20(1) – –
Cordoni et al. 2023 0.86 0.13 – 3758 0.072 1083 0.48 6(1)
Just et al. 2023 – – – 3428 – 1675 – –
He et al. 2022 – 0.10 – 4467 – – – –
Spina et al. 2022 – – – – 0.010 – – –
Tarricq et al. 2022 0.87 – – 4169 – – – –
Jadhav & Subramaniam 2021 0.89 0.07 – 4266 – 2817 – 6(1)
Jaehnig et al. 2021 0.86(1) – – – – – – –
Netopil et al. 2022 0.88(1) – – 3631 0.010(1) – – –
Rain et al. 2021 0.86 0.09 – 2818 – – – 11
Dias et al. 2021 0.86 0.13 – 3758 0.072 – – –
Spina et al. 2021 0.88 – – 4266 0.001(20) – – –
Cantat-Gaudin et al. 2020 0.89 0.07 – 4266 – – – –
Kounkel et al. 2020 0.84 0.28 – 2399 – – – –
Donor et al. 2020 – – – – 0.010 – – –
Zhong et al. 2020 0.86(1) 0.12 – 9561 -0.038 – – –
Cantat-Gaudin & Anders 2020 0.86 – – – – – – –
Bossini et al. 2019 0.88 0.12 – 3639 0.000 – – –
Soubiran et al. 2018 0.86 – – – – – – –
Cantat-Gaudin et al. 2018 0.86 – – – – – – –
Angelo et al. 2019 0.85 – – 3550 – 772 – –
Dib et al. 2018 0.89 – – 3428 – – – –
Loktin & Popova 2017 0.91 0.19 – 2564 – – – –
Joshi et al. 2016 0.89 0.16 – 3428 – 135 – –
Kharchenko et al. 2016 0.89 0.16 – 3428 – – – –
Netopil et al. 2016 8.57 – – 3450 0.030(2) – – –
Heiter et al. 2014 – – – – 0.000 – – –
Kharchenko et al. 2013 0.89 0.16 – 3428 -0.102 – – –
Bukowiecki et al. 2012 – – – – – 760 – –
Gozha et al. 2012 0.91 – – 2564 0.030 135 – –
Bukowiecki et al. 2011 0.84(1) 0.06 – 3548 – – – –
Paunzen et al. 2010 – – – – -0.040 – – –
Piskunov et al. 2008 0.91 0.19 – 2570 – 279(1) – –
Piskunov et al. 2007 0.91 0.19 – 2570 – 83 – –
Ahumada & Lapasset 2007 – 0.19 – 2570 – – – 30
van den Bergh 2006 0.91 0.19 – 2570 – – – –
Kharchenko et al. 2005 0.91 0.19 – 2570 – – – –
Kharchenko et al. 2003 0.91 0.19 – – – – – –
Chen et al. 2003 0.91 0.19 – 2560 0.000(1) – – –
Dias et al. 2002 0.81 0.09 – 2818 0.030 – – –
Lynga 1987 0.72 0.16 – 3981 -0.100 – – –

(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 14090 60.4 132.84 11.82 1.15 -10.98 -2.91 33.79 0.0
Chupina 1 1.6 132.62 11.9 1.16 -10.99 -2.99 34.59 0.0
Chupina 2 1.5 132.64 12.26 1.14 -11.01 -2.96 33.83 0.0
Chupina 3 1.5 132.85 11.41 1.15 -11.04 -2.83 34.39 0.0
Chupina 4 1.5 133.01 12.34 1.15 -10.93 -2.95 33.99 0.0
Chupina 5 1.5 133.19 11.87 1.15 -10.96 -2.87 34.33 0.0
NGC 2678 1.4 132.58 11.36 1.05 -10.92 -2.82 35.48 0.02

💡 Note: The % column shows the percentage of members that NGC 2682 shares with each listed object.

Visualization
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NGC 2682 UCC
NGC 2682 HUNT23
NGC 2682 CANTAT20
Galactocentric position diagram