[originally assembled for FEPS by eric mamajek February 2001]
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Ages are best recent estimates, and italicized ages are from the Lithium Depletion Boundary (LDB) method. Italicized ages with a * are simply 1.6 times the most recent non-LDB method ages. This factor comes from the new estimates of the ages for IC 2391, Pleiades and alpha Persei clusters, which increased the classical age estimates by 50-65%.
CLUSTER/ASSOC | DIST | Age | Gal Lat | Notes / Membership |
AB Dor | 15 | 80-120 | -33 | |
Beta Pic | 10-50 | 10-20 | +17 | |
Her-Lyr | ? | ? | -33 | Fuhrmann 2004 |
Ursa Major | 20-25 | 162-300 | +60 | |
Castor | 5-30 | 100-300 | +22 | |
Tucanae | 45 | 10-40 | widespread | probable and improbable members of Zuckerman & Webb 2000 |
Hyades | 46 | 650 | -22 | |
TW Hya | 55 | 10 | widespread around +23 | |
Horologium | 60 | 30 | ? | Torres et al. 2000 |
MBM 12 | ~60-100 | <10 | -34.3 | |
Coma Ber | 87 | ~600? | +84.0 | |
Eta Cha | 97 | 8 | -21.7 | |
Epsilon Cha | 108 | 5-15 | -15.6 | |
a Car | 130 | 60 | -7 | Platais et al 1998; 11 B2-F5 members only |
Pleiades | 118 | 125 | -23.5 | |
Lower Cen Crux | 118 | 11 | +5 | |
Upper Cen Lup | 140 | 15 | +10 | |
Upper Sco | 145 | 5 | +18 | |
Lupus T Assn | 160 | <10 | +10 | |
Rho Oph OB Assn | 150 | 0-2? | +16.5 | |
Tau-Aur T Assn | 140 | <10 | ? | |
Cha I T Assn | 160 | <2 | -15.6 | |
Cha II T Assn | 180 | <10 | -14.4 | |
Praesepe/M44 | 181 | 400-900 | +32.5 | |
IC 2602/Theta Car | 152 | 35(56*) | -4.9 | |
IC 2391/Omicron Vel | 146 | 53 | -6.9 | note Platais et al 2007 membership study |
Alpha Per | 191 | 65 90 | -7.1 | |
Cas-Tau | 180 | 70-90 | -10 | |
NGC 2451A | 189 | 36-100 | -6.7 | |
NGC 6475/M7 | 280 | 129-224 | -4.5 | |
IC 348/Omicron Per | 261 | 0.5-12 | -17.7 | |
Blanco 1/Zeta Scu | 263 | 90(145*) | -79.3 | |
Collinder 135 | 276 | 80? | -11.2 | |
Stock 2 | 303 | 800? | -1.9 | |
NGC 7092/M39 | 311 | 269-407 | -2.2 | |
Delta Lyra/Stephenson 1 | 315 | 25-40 | +15.5 | |
NGC 2232 | 325 | 22-71 | -7.4 | |
IC 4756 | 330 | 600 | +5.3 | |
Ruprecht 98 | 335 | 500? | -2.2 | |
NGC 2264 | 350 | 3-20 | +2.2 | |
Collinder 463 | 350 | 300? | +9.4 | |
Roslund 5 | 350 | 100? | +0.3 | |
NGC 752 | 364 | 2000? | -23.4 | |
IC 4665 | 327-430 | 36-40 | +17.1 | |
NGC 6633 | 383 | 450? | +8.3 | |
NGC 1662 | 395 | 300? | -21.1 | |
Collinder 140 | 410 | 22-40 | -7.9 | |
Trumpler 10 | 365 | 15-47 | +0.6 | |
NGC 2451B | 360 | 100 | +3.4 | Baumgardt 1998says it probably doesn't exist, but Platais et al 1998 recovered a membership of 5 through HIP. |
NGC 2516 | 346 | 62-126 | -15.9 | |
Collinder 132 | 411 | 78 | -9.2 | |
NGC 1901 | 415 | 830? | -33.6 | |
NGC 2547 | 433 | 23-55 | -8.5 | |
Gamma Vel | 440 | 2-4 | -7.7 | |
Sigma Ori | 480 | 2-4 | -17.3 | |
Lambda Ori | 480 | 4-5 | -12.0 | |
Orion A/M42/NGC 1976 | 399 | 13 | -19.4 | |
Orion B/NGC 2024 | ? | ? | -16.4 | |
NGC 1039/M34 | 440-501 | 250(400) | -15.6 | |
NGC 2164 | 466 | 100 | -6.0 | |
NGC 6494/M23 | 475 | 340 | +2.9 | |
NGC 2422/M47 | 498 | 78-100 | +3.1 | |
NGC 3532 | 405 | 251-347 | +1.4 | |
NGC 6405/M6 | 484 | 100 | -0.7 | |
Collinder 121 | 556-592 | 1.5-10 | -10.4 |