GLOBULAR CLUSTER SYSTEMS IN OTHER GALAXIES Compiled by William E. Harris McMaster University This Revision: March 1996 This catalog contains a brief summary of available data for 73 galaxies in which old-halo globular cluster populations have been found. It is based on the extensive literature survey of Harris 1991 (see reference [12] below), updated to the present with more recent changes and additions. In particular, the adopted distance scale is slightly different from the 1991 listing (the Virgo distance modulus is now set at 31.0, and provides a baseline of comparison for many other galaxies in the list). The present list of cluster populations and specific frequencies has been recalculated in all such cases. Calculating the total cluster population usually involves an extrapolation of the directly observed totals over all magnitudes and radial ranges. These differ considerably from one galaxy to the next; however, as a general rule, for E galaxies we adopt a `turnover' (peak point of the cluster luminosity distribution of M_V = -7.2 and a Gaussian standard deviation sigma = 1.4 mag; while for spiral galaxies, we adopt M_V(turnover) = -7.4 and sigma = 1.2 mag (see [11]). column (1): Galaxy (NGC number or other identification) column (2): Name of group (if any) that the galaxy belongs to. Local Group members are listed first; succeeding galaxies are in order of right ascension, with the exception that group members are listed together. column (3): Galaxy type (primarily from the RC3) column (4): Heliocentric radial velocity column (5): Apparent visual distance modulus. For nearby galaxies ( Virgo and in), individual distance measurements are adopted. For more distant ones, the primary distance indicator is the radial velocity, with H_0 = 75 km/s/Mpc. The Virgo distance is set at (m-M)_v = 31.0, following the Cepheid, planetary nebula, and surface brightness fluctuation methods. column (6): Absolute integrated magnitude of galaxy column (7): Total number of globular clusters estimated to be in the galaxy, integrated over all luminosities (magnitudes) and all radii column (8): Estimated uncertainty in N_gc column (9): Specific frequency, defined as in [12,15]: number of globular clusters per unit galaxy luminosity. column (10): Estimated uncertainty in S_N column (11): Reference source for the globular cluster count data. See the list at the end of the table. NGC Group T V_0 (m-M)v M_V^T N_gc +- S_N +- Ref Galaxy Local Sbc -21.3 160 20 0.5 0.1 12 LMC Local Sm 12 18.64 -18.6 15: 0.5: 12 SMC Local Im -30 18.92 -16.9 2 1 0.4 0.2 12 Fornax Local dE0 -51 20.70 -13.7 5 1 17 7 26 Sgr Local dE 140 17.44 -13: 3 1 19: 9 147 Local dE5 89 24.45 -15.0 4 1 4.0 1.0 12 185 Local dE3 39 24.40 -15.2 8 2 6.5 1.6 12 205 Local dE5 -1 24.49 -16.5 12 1 2.3 0.3 12 221 Local E2 35 24.54 -16.3 <3 <0.8 12 M31 Local Sb -59 24.54 -21.7 350 100 0.7 0.2 12 M33 Local Scd 3 24.75 -19.2 30: 0.6: 12 55 Sculptor Sm 106 25.75 -19.0 2 >0.1: 12 253 Sculptor Sc 260 26.8 -20.4 22: 0.2 0.1 12 524 CfA13 S0 2600 32.7 -22.1 4430 950 6.4 1.4 12 720 T52-9 E5 1660 31.4 -21.2 660 190 2.2 0.9 20 1052 Cetus E4 1400 31.3: -20.8 600 70 3.0 0.4 12 1275 Perseus Ep/cD 5450 34.9 -23.3 7750 2520 4.3 1.4 18 1374 Fornax E0 1390 31.0 -19.7 440 200 5.7 2.6 12 1379 Fornax E0 1390 31.0 -19.9 380 100 4.1 1.1 12 1387 Fornax S0 1390 31.0 -20.2 385 80 3.3 0.7 12 1399 Fornax E1/cD 1390 31.0 -21.1 5340 1780 19 6 7 1404 Fornax E1 1390 31.0 -20.7 950 140 4.3 0.7 24 1549 Doradus E0 1010 30.7: -20.8 165 60 0.8 0.3 12 1553 Doradus S0 1010 30.7: -21.2 600 134 2.0 0.5 12 2403 M81 Scd 260 27.64 -19.5 8: >0.1: 12 3031 M81 Sab 260 27.8 -21.2 210 30 0.7 0.1 23 2683 Sb 370 29.75 -20.8 310 100 1.7 0.5 12 3109 Im 130 26.35 -17.3 20: 2.4: 12 3115 S0 460 30.2 -21.1 630 150 2.3 0.5 12 3115DW1 dE1,N 460 30.2 -17.7 59 23 4.9 1.9 10 3226 CfA58 E2 1210 31.0: -19.6 480 170 7.0 2.4 12 3311 A1060 E0/cD 3420 33.4 -22.3 12400 5000 15 6 22 3377 Leo E5 630 30.00 -19.8 210 50 2.6 0.6 12 3379 Leo E1 630 30.00 -20.7 260 140 1.3 0.7 12 3384 Leo S0 630 30.00 -20.0 110 60 1.1 0.5 12 3557 T31-10 E3 2560 33.0 -22.6 400 300 0.4 0.3 12 3607 CfA77 S0 1090 31.0: -21.0 1000 700 4.0 2.8 12 3842 A1367 E3 6500 34.7 -23.1 14000 2500 7.7 1.4 8 3923 T22-4 E3 1590 31.9 -22.1 4300 1000 6.4 1.5 25 4073 MKW4 E1/cD 6090 34.6 -23.1 8290 460 4.8 0.3 6 4278 Coma I E1 910 30.0 -19.8 1050 120 12.3 1.4 12 4565 Coma I Sb 1210 30.0 -21.6 180 45 0.4 0.1 11 4216 Virgo Sb 1080 31.0 -21.7 620 310 1.3 0.7 12 4340 Virgo SB0 1080 31.0 -20.0 775 310 8.0 3.2 12 4365 Virgo W E2 1080 31.4 -21.8 2500 200 5.0 0.4 13 4374 Virgo E1 1080 31.0 -21.7 3040 400 6.6 0.9 12 4406 Virgo E3 1080 31.0 -21.8 3350 400 6.3 0.8 12 4472 Virgo E2 1080 31.0 -22.6 6300 1900 5.6 1.7 12 4486 Virgo E0 1080 31.0 -22.4 13000 500 13.9 0.5 21 4494 Virgo E0 1290 30.8 -21.0 1400 350 5.4 1.3 11 4526 Virgo S0 1080 31.0 -21.4 2700 400 7.7 1.2 12 4552 Virgo E0 1080 31.0 -21.2 2400: 8: 1 4564 Virgo E6 1080 31.0 -20.1 1000 300 10.0 3.0 12 4569 Virgo Sab 1080 31.0 -21.8 930 310 1.8 0.6 12 4621 Virgo E5 1080 31.0 -21.2 1900 400 6.3 1.2 12 4636 Virgo E0 1080 31.0 -21.4 3060 270 8.4 0.8 19 4649 Virgo E2 1080 31.0 -22.2 5100 160 6.9 0.2 12 4697 Virgo E6 1080 31.0 -21.7 2500 600 5.0 1.3 12 4594 Virgo SE Sa 840 29.9 -22.3 1900 620 2.3 0.7 5 5018 T11-0 E4p 2800 33.2: -22.4 800 300 0.9 0.3 16 5170 T11-18 Sb 1350 31.7: -21.2 390 140 1.2 0.4 12 4874 A1656 E0 6950 34.9 -23.0 22600 2700 14.3 1.7 3 4881 A1656 E0 6950 34.9 -21.6 390 40 1.0 0.1 2 4889 A1656 E4 6950 34.9 -23.5 17300 3000 6.9 1.2 3 5128 Centaurus E0p 320 28.25 -22.0 1700 400 2.6 0.6 12 5629 AWM3 E/cD 4600 34.0 -21.7 <2000 <5 6 5813 CfA150 E1 1810 32.3 -21.6 3000 750 6.9 1.7 17 5846 CfA150 E0 1810 32.3 -22.1 3120 1850 4.5 2.7 12 UGC9799 A2052 E/cD 10440 35.9 -23.4 48000 16000 21 7 14 UGC9958 A2107 E/cD 12630 36.3 -23.4 27000 13000 12 5.6 14 6166 A2199 E2/cD 9080 35.6 -23.6 10000 5000 4 2 12 7768 A2666 E2/cD 7950 35.3 -22.9 4050 2600 2.8 1.8 14 7814 Sab 1110 31.0 -21.0 500 160 2.6 0.8 4 Source List: [1] Ajhar, E.A., Blakeslee, J.P., & Tonry, J.L. 1994, AJ, 108, 2087 [2] Baum, W.A. et al. 1995, AJ, 110, 2537 [3] Blakeslee, J.P., & Tonry, J.L. 1995, ApJ, 442, 579 [4] Bothun, G. 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