CATALOG OF PARAMETERS FOR MILKY WAY GLOBULAR CLUSTERS Compiled by William E. Harris, McMaster University This revision: June 22, 1999 The proper reference to this catalog is: Harris, W.E. 1996, Astronomical Journal, 112, 1487. Please refer to that paper in any published use you make of this catalog. THE DATA IN THIS CATALOG ARE SUPPLIED FREE OF CHARGE TO ALL USERS. ANY THIRD PARTY WHO SUPPLIES THIS CATALOG IN TURN TO OTHER USERS MUST REFER TO THE ORIGINAL SOURCE, WHICH IS THIS WEBSITE, AND MUST DO SO WITHOUT CHARGE OF ANY FEE. Source lists, calibration parameters, and conversion relations for the cluster data are described below. The author would welcome being informed about any errors or omissions that you find in this catalog. Please communicate by e-mail to harris@physics.mcmaster.ca The cluster data are contained in the file `mwgc.dat' which is also on this website. Go to: http://physun.physics.mcmaster.ca/Globular.html and click on "Catalogue". ______________________________________________________________________ REVISIONS AND HIGHLIGHTS FOR JUNE 1999 EDITION: - The adopted DISTANCE SCALE, based on the luminosity level of the horizontal branch, has been revised once again. PLEASE SEE THE "DISTANCES" SECTION BELOW FOR DETAILED EXPLANATION. IT IS IMPORTANT THAT YOU READ THAT SECTION BEFORE USING ANY OF THE DISTANCE INFORMATION CONTAINED IN THIS CATALOG. - New DYNAMICAL RELAXATION TIMES for the core and half-mass radii have been calculated, replacing the ones in Djorgovski's (1993) compilation. The half-mass relaxation time contains the correction for the ln(10) error that existed in the old lists. - A newly included quantity is the TIDAL RADIUS. I am indebted to Ivan King for supplying advice and an initial list of references. The sources used for r_c, r_t, and c are still likely to be incomplete, and I would appreciate being told of ones that I have inadvertently missed. - New work on color-magnitude photometry, particularly for clusters that have not been well studied, continues apace. This 1999 edition includes almost 30 updates and revisions to the cluster distances and reddenings thanks to such work. Notably, this is the first time that distance moduli can now be listed for *every* globular cluster in the catalog. ______________________________________________________________________ _______________________________________________________________________ CLUSTER IDENTIFICATIONS AND COORDINATES Sources: Djorgovski S., and Meylan G. 1993, in Structure and Dynamics of Globular Clusters, ASP Conf.Series 50, ed.G.Meylan and S.Djorgovski (San Francisco: A.S.P.), 325 Webbink R.F. 1985, in Dynamics of Star Clusters, IAU Symposium 113, ed. J.Goodman and P.Hut (Dordrecht: Reidel), 541 The objects in this catalog adopted as Milky Way globular clusters essentially follow Djorgovski and Meylan, with the exceptions noted above. The cluster coordinates are taken from Djorgovski and Meylan unless otherwise noted. See the comments above for individual deletions and additions in various editions of the catalog. The present catalog contains 147 objects adopted as certain or highly probable Milky Way globular clusters. It should be emphasized that some objects -- the ones with virtually no data entries in the catalog -- still have somewhat uncertain identities, and that the adoption of a final candidate list continues to be a matter of some arbitrary judgment for certain objects. The sources given above should be consulted for excellent discussions of these individually troublesome objects, as well as lists of other less likely candidates. FOREGROUND REDDENING E(B-V) Sources: Reed B.C., Hesser J.E., and Shawl S.J. 1988, PASP 100, 545 [85 clusters] Webbink R.F. 1985, in Dynamics of Star Clusters, IAU Symposium 113, ed. J.Goodman and P.Hut (Dordrecht: Reidel), 541 [135 clusters] Zinn, R. 1985, ApJ 293, 424 [112 clusters] In addition to the three major sources listed above, measurements of E(B-V) from the individual color-magnitude studies (listed below) were employed whenever they appeared to be well calibrated [120 clusters]. These discussions, which employ a wide variety of semi-independent methods, now agree extremely well for all but a few cases. The final adopted reddenings are the averages of the given sources (up to 4 per cluster), with double weight given to the reddenings from color-magnitude diagrams. The typical uncertainty in the reddening for any cluster is on the order of 10 percent, i.e. delta[E(B-V)] = 0.1 E(B-V). DISTANCES: HORIZONTAL-BRANCH MAGNITUDE V_HB The primary distance indicator used here is the mean V magnitude of the horizontal branch (or RR Lyrae stars), V_HB. Wherever possible, the HB level is measured directly from a color-magnitude diagram; in a few cases where CMDs are not yet available, it can be evaluated from single-color photometry of the RR Lyrae variables, or more roughly predicted from the magnitude level of the brightest red giants. Whenever one of these latter two methods was used, it is noted in the list below. For many clusters, there are several CMD studies to be found in the literature, and in some cases the CMD study used here may not be the "best" one for the given cluster according to some other criterion. For example, it may not provide the best or most precise study of the main sequence, cluster age, metallicity, or some other feature. The sources listed below are simply those which, in the author's judgment, give the best available definition of the horizontal-branch level. THE DISTANCE SCALE: The absolute calibration of V_HB adopted here uses a modest dependence of absolute V magnitude on metallicity, M_V(HB) = 0.15 [Fe/H] + 0.80 (1) !! IMPORTANT !! Please note that V(HB) here denotes the mean magnitude of the HB stars, without further adjustments to any predicted ZAHB level: Wherever possible, it denotes the mean magnitude of the RR Lyrae stars directly. For blue-HB clusters, it denotes the mean magnitude of the HB stars at the blue edge of the RR Lyrae gap. For red-HB clusters, it denotes the mean magnitude of the RHB stars directly. How does this distance scale compare with other recently published ones? In some recent discussions, the adopted slope of the M_V(HB)-[Fe/H] relation is steeper (although values in the range 0.15 - 0.25 are common). It is extremely important to realize the reasons for this difference. A factor in setting the slope is that most other authors `correct' the observed HB magnitude to an unevolved ZAHB level. The correction must employ some sort of stellar models to step from the (evolved, more luminous) position of the mean HB stars to the (fainter, unevolved) zero-age HB. Furthermore, the amount of the shift depends on position on the HB, being larger for redder stars. As a result, the slope of the `corrected' ZAHB level ends up steeper -- and fainter by typically 0.05 - 0.15 mag on the average -- than the uncorrected HB level. Carney et al. 1992 (ApJ 386, 663) give an empirical correction as Delta(V)(ZAHB - ) = 0.05 [Fe/H] + 0.20 which when added to my equation for M_V(HB) gives M_V(ZAHB) = 0.20 [Fe/H] + 1.00 . This relation in turn is close to published theoretical stellar models for the ZAHB: for example, M_V(ZAHB) = 0.17 [Fe/H] + 0.82 (Lee et al 1990, ApJ 350, 155) M_V(ZAHB) = 0.21 [Fe/H] + 0.91 (Salaris et al. 1997, ApJ 479, 665) M_V(ZAHB) = 0.26 [Fe/H] + 0.91 (Caloi et al 1997, AAp 320, 823) My adopted distance scale is therefore basically in line with what theoretical stellar models would predict for normal compositions. I have adopted the approach that the *directly measured*, unadjusted, mean HB value is simpler to use and relates much more directly to the observations. Therefore, I do not make any adjustments to the mean V magnitude of the horizontal branch before using it to estimate the distance of the cluster through equation (1). What about comparisons with other kinds of direct observations? The adopted value of the **slope** (0.15) matches the following sets of data used for the calibration: - homogeneously calibrated CMD photometry for 10 globular clusters in the M31 halo (Fusi Pecci et al 1996, AJ 112, 1461; and Holland et al 1997, AJ 114, 1488). A direct plot of their mean V(HB) against [Fe/H] gives a slope of 0.10 +- 0.08. - calibrations of distances to Milky Way globular clusters using recent Hipparcos parallax data for subdwarfs. For detailed discussions, see Gratton et al. 1997, ApJ 491, 749 Carretta et al. 1999, astro-ph/9902086 Reid 1997, AJ, 114, 161 For example, Gratton et al. find a slope 0.125 +- 0.055. - astrometric (coupled radial velocity and proper motion) distance solutions to 6 Milky Way clusters by Rees 1996 (ASP Conf. Proc. 92, 289). The **zero point** is not so easy to pin down confidently. My adopted value (0.80) pegs the horizontal branch at M_V(HB) ~ 0.5 for the most metal-poor clusters and M_V(HB) ~ 0.8 for the most metal-rich. The `true' value of this number continues to generate considerable dispute, and what I use here is very definitely a compromise among various options: it leaves the HB *brighter* by 0.1-0.2 mag than the levels favored by statistical parallax and Baade-Wesselink measurements of field RR Lyrae stars (e.g. Carney, Storm, and Jones 1992, ApJ, 386, 663; Skillen et al. 1993, MNRAS, 265, 301; Layden et al. 1996, AJ, 112, 2110). For example, Carney et al. from their Baade-Wesselink solutions give M_V(RR) = 0.16 [Fe/H] + 1.02 . On the other hand, my choice is *fainter* by about 0.1-0.2 mag than the levels favored by the various published analyses of Hipparcos subdwarf parallaxes (see the references cited above). The zero point adopted here does, however, match reasonably well with calibrations of the RR Lyrae luminosity level if the **Cepheids** are used to set distances to the various Local Group galaxies (e.g. Walker 1992, ApJ, 390, L81; van den Bergh 1995, ApJ, 446, 39; Fusi Pecci et al. 1996, AJ, 112, 1461). Interestingly, it also agrees well with the distance scale set by the **white-dwarf** sequence in NGC 6752 (Renzini et al. 1996, ApJ, 465, L23). The absolute uncertainty of the predicted M_V(HB) is, thus, +-0.1 mag at best, and may still be as large as +-0.2 mag in extreme cases. The ~0.4-mag discrepancy between the Hipparcos scale and (e.g.) statistical parallaxes and astrometric distances continues to be very disturbing, and no obvious unifying solution has yet emerged. For recent comprehensive discussions, see Harris 1999, Saas-Fee Lectures on Star Clusters (Springer, in press) Carretta et al. 1999, astro-ph/9902086 Note that for a few clusters (mostly ones in the Galactic bulge region with very heavy reddening), no good [Fe/H] estimate is currently available; for these cases, a value [Fe/H] = -1 is simply assumed, with the hope that the resulting M_V(HB) estimate will not be too far wrong. Source List for Individual Clusters: NGC 104 Hesser J.E., Harris W.E., VandenBerg D.A., Allwright J.W.B., Shott P., and Stetson P.B. 1987, PASP, 99, 739 NGC 288 Bergbusch P.A. 1993, AJ 106, 1024; also Kaluzny, J. 1996, AApSuppl, 120, 83 NGC 362 Harris W.E. 1982, ApJSuppl 50, 573 NGC 1261 Ferraro F.R., Clementini G., Fusi Pecci F., Vitiello E., and Buonanno R. 1993, MNRAS 264, 273 Pal 1 Rosenberg, A., Saviane, I., Piotto, G., Aparicio, A., and Zaggia, S.R. 1998, AJ, AJ, 115, 648 AM 1 Madore B.F., and Freedman W.L., 1989, ApJ 340, 812 Eridanus Stetson, P.B., Bolte, M., Harris, W.E., Hesser, J.E., van den Bergh, S., VandenBerg, D.A., Bell, R.A., Johnson, J.A., Bond, H.E., Fullton, L.K., Fahlman, G.G. & Richer, H.B. 1999, AJ, 117, 247 Pal 2 Harris, W.E., Durrell, P.R., Petitpas, G.R., Webb, T.M., and Woodworth, S.C. 1997, AJ, 114, 1043 NGC 1851 Walker, A.R. 1998, AJ, 116, 220 NGC 1904 Ferraro F.R., Clementini G., Fusi Pecci F., Sortino R., and Buonanno R., 1992, MNRAS 256, 391 NGC 2298 Janes K.A., and Heasley J.N., 1988, AJ 95, 762 NGC 2419 Harris, W.E., Bell, R.A., VandenBerg, D.A., Bolte, M., Stetson, P.B., Hesser, J.E., van den Bergh, S., Bond, H.E., Fahlman, G.G., and Richer, H.B. 1997, AJ, 114, 1030 Pyxis Irwin, M.J., Demers, S., and Kunkel, W.E. 1995, ApJ 453, L21; Da Costa, G.S. 1995, PASP 107, 937; Sarajedini, A., and Geisler, D. 1996, AJ, 112, 2013 NGC 2808 Ferraro F.R., Clementini G., Fusi Pecci F., Buonanno R. and Alcaino G., 1990, AApSuppl 84, 59 E 3 McClure R.D., Hesser J.E., Stetson P.B., and Stryker L.L., 1985, PASP 97, 665 Pal 3 Stetson, P.B., Bolte, M., Harris, W.E., Hesser, J.E., van den Bergh, S., VandenBerg, D.A., Bell, R.A., Johnson, J.A., Bond, H.E., Fullton, L.K., Fahlman, G.G. & Richer, H.B. 1999, AJ, 117, 247 NGC 3201 Brewer J.P., Fahlman G.G., Richer H.B., Searle L., and Thompson I., 1993, AJ 105, 2158 Pal 4 Stetson, P.B., Bolte, M., Harris, W.E., Hesser, J.E., van den Bergh, S., VandenBerg, D.A., Bell, R.A., Johnson, J.A., Bond, H.E., Fullton, L.K., Fahlman, G.G. & Richer, H.B. 1999, AJ, 117, 247 NGC 4147 Friel E.D., Heasley J.N., and Christian C.A., 1987, PASP 99, 1248 NGC 4372 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 Rup 106 Sarajedini, A., and Layden, A. 1997, AJ, 113, 264 NGC 4590 McClure R.D., VandenBerg D.A., Bell R.A., Hesser, J.E., and Stetson, P.B., 1987, AJ 93, 1144 NGC 4833 Menzies J., 1972, MNRAS 156, 207 NGC 5024 Rey, S.-C., Lee, Y.-W., Byun, Y.-I., & Chun, M.-S. 1998, AJ, 116, 1775 NGC 5053 Sarajedini, A., and Milone, A.A.E. 1995, AJ 109, 269 NGC 5139 Butler D., Dickens R.J., and Epps E., 1978, ApJ 225, 148 (RR Lyraes) NGC 5272 Johnson, J.A., & Bolte, M. 1998, AJ, 115, 693 NGC 5286 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 AM 4 Inman R.T., and Carney B.W., 1987, AJ 93, 1166 NGC 5466 Mateo M., Harris H.C., Nemec J. and Olszewski E.W., 1990, AJ 100, 469 NGC 5634 Racine R., 1976, unpublished CMD NGC 5694 Ortolani S., and Gratton R., 1990, AApSuppl 82, 71 IC 4499 Walker, A.R., and Nemec, J.M 1996, AJ, 112, 2026 NGC 5824 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 Pal 5 Smith G.H., McClure R.D., Stetson P.B., Hesser J.E., and Bell R.A., 1986, AJ 91, 842 NGC 5897 Ferraro F.R., Fusi Pecci F., and Buonanno R., 1992, MNRAS 256, 376 NGC 5904 Brocato, E., Castellani, V., and Ripepi, V. 1996, AJ, 111, 809; and Sandquist, E.L., Bolte, M., Stetson, P.B., and Hesser, J.E. 1996, ApJ, 470, 910 NGC 5927 Heitsch, F., & Richtler, T. 1999, AAp, preprint (astro-ph/9904404) (The mean HB level is used here, not their differentially dereddened one, along with their mean reddening) NGC 5946 Alcaino G., Liller W., Alvarado F., and Wenderoth E., 1991, AJ 102, 1371 BH 176 Ortolani, S., Bica, E., and Barbuy, B. 1995, AAp 300, 726 NGC 5986 Bond H., Harris W.E., Harris G.L.H., Mittermeier R., and Palmer K., 1994, unpublished Lynga 7 Ortolani, S., Bica, E., and Barbuy, B. 1993, AAp 273, 415 see also Tavarez, M., and Friel, E.D. 1995, AJ 110, 223 Pal 14 Holland S., and Harris W.E., 1992, AJ 103, 131 NGC 6093 Brocato, E., Castellani, V., Scotti, G.A., Saviane, I., Piotto, G., & Ferraro, F.R. 1998, AAp, 335, 929 NGC 6101 Sarajedini A., and DaCosta G.S., 1991, AJ 102, 628 NGC 6121 Cudworth K.M., and Rees R., 1990, AJ 99, 1491 NGC 6144 Alcaino G., 1980, AApSuppl 39, 315 NGC 6139 Zinn, R., & Barnes, S. 1998, AJ, 116, 1736 Terzan 3 Barbuy, B., Ortolani, S., & Bica, E. 1998, AApS, 132, 333 NGC 6171 Cudworth K.M., Smetanka J.J., and Majewski S.R., 1992, AJ 103, 1252 ESO452-SC11 Bica, E., Ortolani, S., & Barbuy, B. 1999, AApS, 136, 363 NGC 6205 Paltrinieri, B., Ferraro, F.R., Fusi Pecci, F., & Carretta, E. 1998, MNRAS, 293, 434 NGC 6218 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 NGC 6229 Borissova, J., CAtelan, M., ferraro, F.R., Spassova, N., Buonanno, R., Iannicola, G., Richtler, T., & Sweigart, A.V. 1999, AAp, 343, 813 NGC 6235 Liller M.H., 1980, AJ 85, 673 NGC 6254 Hurley D.J.C., Richer H.B., and Fahlman G.G., 1989, AJ 98, 2124 NGC 6256 Ortolani, S., Barbuy, B., & Bica, E. 1999, AApS, 136, 237 Pal 15 Harris W.E., 1991, AJ 102, 1348 NGC 6266 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 NGC 6273 Harris W.E., Racine R., and de Roux J., 1976, ApJSuppl 31, 13 NGC 6284 Harris H.C., and Harris W.E., 1994, unpublished CMD NGC 6287 Stetson P.B., and West, M.J. 1995, PASP 106, 726 NGC 6293 Janes K.A., and Heasley J.N., 1991, AJ 101, 2097 NGC 6304 Davidge T.J., Harris W.E., Bridges T.J., and Hanes D.A., 1992, ApJSuppl 81, 251 NGC 6316 Heitsch, F., & Richtler, T. 1999, AAp, preprint (astro-ph/9904404) (The mean HB level is used here, not their differentially dereddened one, along with their mean reddening) NGC 6325 Mittermeier R., Harris G.L.H., Bond H., Harris W.E., and Palmer K., 1994, unpublished CMD NGC 6341 Carney B.W., Storm J., Trammell S.R., and Jones R.V., 1992, PASP 104, 44 NGC 6333 Janes K.A., and Heasley J.N., 1991, AJ 101, 2097 NGC 6342 Heitsch, F., & Richtler, T. 1999, AAp, preprint (astro-ph/9904404) (The mean HB level is used here, not their differentially dereddened one, along with their mean reddening) NGC 6356 Bica, E., Ortolani, S., and Barbuy, B. 1994, AApSuppl 106, 161 NGC 6355 Harris W.E., 1980, in Star Clusters, IAU Symposium 85 ed. J.E.Hesser (Dordrecht: Reidel), 81 (Brightest Giants) NGC 6352 Fullton, L.K., Carney, B.W., Olszewski, E.W., Zinn, R., Demarque, P., Janes, K.A., Da Costa, G.S., and Seitzer, P. 1995, AJ 110, 652 IC 1257 Harris, W.E., Phelps, R.L., Madore, B.F., Pevunova, O., Skiff, B.A., Crute, C., Wilson, B., and Archinal, B. 1997, AJ, 113, 688 Terzan 2 Ortolani, S., Bica, E., and Barbuy, B. 1997, AAp, 326, 614, S.E. 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J.E.Hesser (Dordrecht: Reidel), 81 (Brightest Giants) Terzan 6 Barbuy, B., Ortolani, S., and Bica, E. 1997, AApSuppl, 122, 483 UKS 1 Ortolani, S., Bica, E., and Barbuy, B. 1997, AApSuppl 126, 319 NGC 6496 Sarajedini A., and Norris J.E., 1994, ApJSuppl 93, 161 also Friel E.D., and Geisler D., 1992, AJ 101, 1338 Terzan 9 Liu, T., McLean, I., and Becklin, E. 1994, in Infrared Astronomy with Arrays, ed. I.McLean (Kluwer), 101 Djorg 2 Ortolani, S., Bica, E., and Barbuy, B. 1997, AApSuppl 126, 319 NGC 6517 Kavelaars J.J., Hanes D.A., Bridges T.J., and Harris W.E. 1995, AJ, 109, 2081 Terzan 10 Ortolani, S., Bica, E., and Barbuy, B. 1997, AApSuppl 126, 319 NGC 6522 Terndrup, D.M., Popowski, P., Gould, A., Rich, R.M., & Sadler, E.M. 19989, AJ, 115, 1476 NGC 6535 Sarajedini A., 1994, PASP, 106, 404 NGC 6528 Heitsch, F., & Richtler, T. 1999, AAp, preprint (astro-ph/9904404) (The mean HB level is used here, not their differentially dereddened one, along with their mean reddening) NGC 6539 Armandroff T.E., 1988, AJ 96, 588 NGC 6540 Bica E., Ortolani S., and Barbuy B. 1994, AA 283, 67 NGC 6544 Alcaino G., 1983, AApSuppl 52, 105 NGC 6541 Alcaino G., Liller, W., Alvarado, F., Kravtsov, V., Ipatov, A., and Samus, N. 1997, AJ, 114, 2638 NGC 6553 Heitsch, F., & Richtler, T. 1999, AAp, preprint (astro-ph/9904404) (The mean HB level is used here, not their differentially dereddened one, along with their mean reddening) NGC 6558 Rich, R.M., Ortolani, S., Bica, E., & Barbuy, B. 1998, AJ, 116, 1295 IC 1276 Barbuy, B., Ortolani, S., & Bica, E. 1998, AApS, 132, 333 Terzan 12 Ortolani, S., Bica, E., & Barbuy, B. 1998, AApS, 127, 471 NGC 6569 Hazen-Liller M.L., 1985, AJ 90, 1807 (RR Lyraes) NGC 6584 Sarajedini A., and Forrester, W.L. 1995, AJ 109, 1112 NGC 6624 Sarajedini A., and Norris J.E., 1994, ApJSuppl 93, 161 NGC 6626 Rees R.F., and Cudworth K.M., 1991, AJ 102, 152 NGC 6638 Alcaino G., and Liller W., 1983, AJ 88, 1166 ; also Smith H.A., and Stryker L.L., 1986, PASP 98, 453 NGC 6637 Ferraro, F.R., Fusi Pecci, F., Guarnieri, M.D., Moneti, A., Origlia, L., and Testa, V. 1994, MNRAS 266, 829 NGC 6642 Hazen M.L., 1993, AJ 105, 557 (RR Lyraes) NGC 6652 Ortolani S., Bica E., and Barbuy B. 1994, AA 286, 444 NGC 6656 Cudworth K.M., 1986, AJ 92, 348 Pal 8 Armandroff T.E., 1988, AJ 96, 588 NGC 6681 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 NGC 6712 Cudworth K.M., 1988, AJ 96, 105 NGC 6715 Sarajedini, A., and Layden, A.C. 1995, AJ 109, 1086 NGC 6717 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 NGC 6723 Fullton L.K., 1996, unpublished CMD; also Alcaino, G., Liller, W., Alvarado, F., Mironov, A., Ipatov, A., Piskunov, A., Samus, N., & Smirnov, O. 1999, AApS, 136, 461 NGC 6749 Kaisler, D., Harris, W.E., and McLaughlin, D.E. 1997, PASP, 109, 920 NGC 6752 Buonanno R., Caloi V., Castellani V., Corsi C., Fusi Pecci F., and Gratton R., 1986, AApSuppl 66, 79 NGC 6760 Heitsch, F., & Richtler, T. 1999, AAp, preprint (astro-ph/9904404) (The mean HB level is used here, not their differentially dereddened one, along with their mean reddening) Terzan 7 Buonanno, R., Corsi, C.E., Pulone, L., Fusi Pecci, F., Richer, H.B., and Fahlman, G.G. 1995, AJ 109, 663 NGC 6779 Wehlau A., and Sawyer Hogg H., 1985, AJ 90, 2514 Pal 10 Kaisler, D., Harris, W.E., and McLaughlin, D.E. 1997, PASP, 109, 920 Arp 2 Sarajedini, A., and Layden, A. 1997, AJ, 113, 264 NGC 6809 Lee S-W., 1977, AApSuppl 29, 1 Terzan 8 Montegriffo, P., Bellazzini, M., Ferraro, F.R., Martins, D., Sarajedini, A., and Fusi Pecci, F. 1998, MNRAS, 294, 315 Pal 11 Cersosimo S., Lydon T.J., Sarajedini A., and Zinn R., 1993, Bull.AAS 25, 884 NGC 6838 Hodder P.C., Nemec J.M., Richer H.B., and Fahlman G.G., 1992, AJ 103, 460 NGC 6864 Harris W.E., 1975, ApJSuppl 29, 397 NGC 6934 Piotto, G., Zoccali, M., King, I.R., Djorgovski, S.G., Sosin, C., Dorman, B., Rich, R.M., & Meylan, G. 1999, AJ, 117, 264 NGC 6981 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 NGC 7006 Buonanno R., Fusi Pecci F., Cappellaro E., Ortolani S., Richtler T., and Geyer E.H., 1991, AJ 102, 1005 NGC 7078 Durrell P.R., and Harris W.E., 1993, AJ 105, 1420 NGC 7089 Harris W.E., 1975, ApJSuppl 29, 397 NGC 7099 Bolte M., 1987, ApJ 319, 760 Pal 12 Stetson P.B., VandenBerg D.A., Bolte M., Hesser J.E., and Smith G.H., 1989, AJ 97, 1360 Pal 13 Borissova, J., Markov, H., and Spassova, N. 1997, AApSuppl, 121, 499 NGC 7492 Cote P., Richer H.B., and Fahlman G.G., 1991, AJ 102, 1358 INTEGRATED VISUAL MAGNITUDE V_t Sources: Mallen-Ornelas G., and Djorgovski S. 1993, in Structure and Dynamics of Globular Clusters, ASP Conf.Series 50, ed. S.G.Djorgovski and G.Meylan (San Francisco: A.S.P.), 313 [Djorg 1, 2, 3, Liller 1, HP 1] Peterson C., and Reed, B.C. 1987, PASP 99, 20 [73 clusters; not including NGC 362,4590,4833,5946,6218, 6235,6522,6535,6717] van den Bergh S., Morbey C., and Pazder J. 1991, ApJ 375, 594 [97 clusters; not including NGC 6401] Webbink R.F. 1985, in Dynamics of Star Clusters, IAU Symposium 113, ed. J.Goodman and P.Hut (Dordrecht: Reidel), 541 [131 clusters; not including NGC 5694, 5824, Pal 1, Pal 3, Pal 15, E3, AM4] All data from the given sources are used, with the exception of the clusters specifically mentioned above (in these latter instances the V_t values are significantly discrepant compared with the other studies. The three major sources (Peterson and Reed, van den Bergh et al., Webbink) all use similar original databases (mostly concentric-aperture photometry of the clusters), but calculate total magnitudes independently by a variety of curve-of-growth methods. For several sparse or low-luminosity clusters (Pal 1, AM-1, E3, Pal 3, AM-4, Pal 14, Pal 15, IC 1257, Ter 12, Pal 12), the cluster luminosity function (from the color-magnitude study or other data in the literature) has been used by the present author to estimate V_t. The adopted integrated magnitudes are the straight averages of the data from all sources. INTEGRATED COLORS (U-B, B-V, V-R, V-I) The integrated colors U-B and B-V are on the standard Johnson system, and V-R, V-I on the Kron-Cousins system. The adopted values are the straight average of the two sources; see Peterson (1993) for a discussion of the (good) internal agreement of the databases and additional references. In a few cases, the integrated colors are derived from direct addition of stars in the color-magnitude diagrams (usually for very sparse clusters with no direct color measurements). Sources: Peterson C.J. 1993, in Structure and Dynamics of Globular Clusters, ASP Conf.Series 50, ed. S.G.Djorgovski and G.Meylan (San Francisco: A.S.P.), 337 Reed B.C. 1986, PASP 97, 120 INTEGRATED SPECTRAL TYPES Integrated spectral types are taken from: Hesser, J.E., and Shawl, S.J. 1985, PASP 97, 465 SPECIFIC FREQUENCY OF RR LYRAE STARS, S_RR S_RR is the number of RR Lyrae stars in the cluster, normalized to a total cluster luminosity M_Vt = -7.5; i.e. S_RR = N_RR * 10**(0.4 (7.5 + M_Vt)) The data source for N_RR is the comprehensive discussion of Suntzeff, Kinman, and Kraft 1991, ApJ, 367, 528. The resulting values for S_RR in the present catalog differ noticeably from theirs in some cases because of revisions in the cluster distance and (thus) luminosity. A few updates for N_RR have been taken from the more recent literature. HORIZONTAL BRANCH MORPHOLOGY The HBR parameter defined by Lee (1990, ApJ 363, 159) is equal to (B-R)/(B+V+R), where in this case B denotes the number of horizontal-branch stars on the blue side of the RR Lyrae region; V the number of stars in the RR Lyrae region; and R the number of stars on the red side of the RR Lyrae region. The adopted HBR value is the direct average of the sources listed. Sources: Lee Y.-W., Demarque P., and Zinn R. 1994, ApJ, 423, 248 Fusi Pecci F., Ferraro F.R., Bellazzini M., Djorgovski S, Piotto G., and Buonanno R. 1993, AJ, 105, 1145 Preston G.W., Schectman S.A., and Beers T.C. 1991, ApJ, 375, 121 The morphological type of the horizontal branch as originally defined by Dickens (1972, MNRAS 157, 281) is on an integer scale from 1 to 7, where 1 denotes a cluster with a completely blue HB (all stars on the blue side of the RR Lyrae region) and 7 denotes a completely red HB. From the individual color-magnitude studies listed above, the HB type has been evaluated anew by the present author for the purpose of this catalog. In addition, a new type "0" has also been introduced, to denote any cluster with an extremely blue extension of the HB. In a few cases, where the distribution of stars along the HB is bimodal, the cluster is assigned two simultaneous HB types. In general, the distribution of stars along the HB cannot be described adequately by any one parameter or ratio. Many recent investigations have shown that the relative proportions of stars in different parts of the HB depend on radius within the cluster; the blue HB can show very distinct gaps or clumps; many clusters at a wide range of metallicities have highly extended blue BHB tails; several clusters have now been found to have clearly bimodal HB distributions with large populations of both blue and red stars but few or none in the intermediate (RR Lyrae) region. For thorough discussion, see the papers of Fusi Pecci et al. 1993 (AJ 105, 1145) or Borissova et al. 1997 (AJ 113, 692). The former paper in particular defines several additional HB parameters which are not listed in this catalog. METALLICITIES: [Fe/H] VALUES The heavy-element abundance scale adopted here is basically the one established by Zinn and West (1984, ApJSuppl, 55, 45). READERS PLEASE NOTE: This scale has recently been reinvestigated as being nonlinear when calibrated against the best modern measurements of [Fe/H] from high-dispersion spectra (see Carretta and Gratton 1997, AApSuppl 121, 95 and Rutledge, Hesser, and Stetson 1997, PASP 109, 907). In particular, these authors suggest that the Zinn-West scale overestimates the metallicities of the most metal-rich clusters. However, the present catalog maintains the older (Zinn-West) scale until a new consensus is reached in the primary literature. Readers should also see Carretta & Bragaglia 1998, AAp 329, 937 for prescriptions to transform the older metallicity scale into the new Gratton et al. one. In addition to the two major compilations of cluster metallicities listed below on the Zinn-West scale, data of two types are used: (1) [Fe/H] values from spectroscopy of individual cluster stars, from various more recent papers (listed below); and (2) metallicity estimates from the color-magnitude diagrams, in cases where the CMD is precise and well calibrated (references given in the V_HB section above). The final adopted [Fe/H] for each cluster is the straight average of the available measurements. Major Sources: Armandroff, T.E., and Zinn, R. 1988, AJ 96, 92 [27 clusters] Zinn, R. 1985, ApJ 293, 424 [111 clusters] Additional Sources: Armandroff, T.E., and Da Costa, G.S. 1991, AJ 101, 1329 [Eridanus, Pal 12] Armandroff, T.E., Da Costa, G.S., and Zinn, R. 1992, AJ 104, 164 [Pal 3,4,11,14] Barbuy, B., Castro, S., Ortolani, S., and Bica, E. 1992, AAp 259, 607 [NGC 6553] Barbuy, B., Castellani, V., Scotti, G.A., Saviane, I., Piotto, G., & Ferraro, F.R. 1998, AAp, 335, 929 [NGC 6553] Beers, T.C., Preston, G.W., Shectman, S.A., and Kage, J.A. 1990, AJ, 100, 849 [NGC 3201,6121,6341,6397,6752] Brown, J.A., and Wallerstein, G. 1992, AJ 104, 1818 [NGC 104, 6121, 6656] Brown, J.A., Wallerstein, G., and Zucker, D. 1997, AJ, 114, 180 [Rup 106, Pal 12] Caldwell, S.P., and Dickens, R.J. 1988, MNRAS 234, 87 [NGC 288,362,6397,6809] Cannon, R. 1996, quoted in Walker, A.R., and Nemec, J.M 1996, AJ, 112, 2026 [IC 4499] Clementini, G., Merighi, R., Gratton, R., and Carretta, E. 1994, MNRAS 267, 43 [NGC 6121] Costar, D., and Smith, H.A. 1988, AJ 96, 1925 [NGC 104,6838] Cote, P. 1999, preprint [NGC 6540, IC 1276, Terzan 3] Da Costa, G.S., and Armandroff, T.E. 1995, AJ 109, 2533 [NGC 6218, 6366, 6626, 6715, Pal 11, 12, 15, Ter 7, Ter 8, Arp 2] Da Costa, G.S., Armandroff, T.E., and Norris, J.E. 1992, AJ 104, 154 [Rup 106] Da Costa, G.S., and Seitzer, P. 1989, AJ 97, 405 [NGC 6366] D'Odorico, S., Gratton, R., and Ponz, D. 1985, AAp 142, 232 [NGC 104] Drake, J.J., Smith, V.V., and Suntzeff, N.B. 1994, ApJ, 430, 610 [NGC 6121] Francois, P. 1991, AAp 247, 56 [NGC 1904,5927,6352] Francois, P., Danziger, J., Buonanno, R., and Perrin, M.N. 1997, AAp, 327, 121 [Rup 106] Geisler, D., Piatti, A.E., Claria, J.J., and Minniti, D. 1995, AJ 109, 605 [NGC 2298, 4372, 4833, 5053, 5694, 5897, 6101, 6144] Geisler, D., Claria, J.J., and Minniti, D. 1997, PASP, 109, 799 [NGC 1851, 1904, 2808, 3201, Pal 5, 5986, 6093, 6362, 6752, 6981] Gratton, R.G. 1982, AAp 115, 171 [NGC 2808] Gratton, R.G. 1987, AAp 179, 181 [NGC 288,362,5897,6352,6362] Gratton, R.G., and Ortolani, S. 1986, AAp 169, 201 [NGC 104,5904,6121,6752,6838] Gratton, R.G., and Ortolani, S. 1989, AAp 211, 41 [NGC 1904,3201,4590,4833,6254,6397,6656] Kraft, R.P., Sneden, C., Langer, G.E., and Prosser, C.F. 1992, AJ 104, 645 [NGC 5272,6205] Kraft, R.P., Sneden, C., Langer, G.E., and Shetrone, M.D. 1993, AJ 106, 1490 [NGC 6205] Kraft, R.P., Sneden, C., Langer, G.E., Shetrone, M.D., and Bolte, M. 1995, AJ 109, 2586 [NGC 6254] Kraft, R.P., Sneden, C., Smith, G.H., Shetrone, M.D., Langer, G.E., and Pilachowski, C.A. 1997, AJ, 113, 279 [NGC 6205] Kraft, R.P., Sneden, C., Smith, G.H., Shetrone, M.D., and Fulbright, J. 1998, AJ, 115, 1500 [NGC 7006] Lehnert, M.D., Bell, R.A., and Cohen, J.G. 1991, ApJ 367, 514 [NGC 6205,6656] Leep, E.M., Oke, J.B., and Wallerstein, G. 1987, AJ 93, 338 [NGC 6838] McWilliam, A., Geisler, D., and Rich, R.M. 1992, PASP 104, 1193 [NGC 2298] Minniti, D. 1995, A&A 303, 468 [NGC 6121, 6325, 6356, 6401, 6440, 6517, 6642, 6656, Pal 6] Minniti, D. 1995, A&ASuppl 113, 299 [NGC 6637, 6626] Minniti, D., Geisler, D., Peterson, R.C., and Claria, J.J. 1993, ApJ 413, 548 [NGC 4590,4833,6144,6397,6752,6809,7078,7099] Ortolani, S., and Gratton, R.G. 1989, AApSuppl 79, 155 [Pal 3, Eridanus] Paltoglou, G., and Norris, J.E. 1989, ApJ 336, 185 [NGC 5139] Peterson, R.C., Kurucz, R.L., and Carney, B.W. 1990, ApJ 350, 173 [NGC 6341] Pilachowski, C.A., and Armandroff, T.E. 1996, AJ, 111, 1175 [NGC 6205] Rosenberg, A., Piotto, G., Saviane, I., Aparicio, A., and Gratton, R. 1998, AJ, 115, 658 [Pal 1] Shetrone, M.D. 1996, AJ, 112, 1517 [NGC 5904,6205,6341,6838] Smith, H.A., and Stryker, L.L. 1986, PASP 98, 453 [NGC 6638] Sneden, C., Kraft, R.P., Prosser, C.F., and Langer, G.E. 1991, AJ 102, 2001 [NGC 6341, 7078] Sneden, C., Kraft, R.P., Langer, G.E., Prosser, C.F., and Shetrone, M.D. 1994, AJ 107, 1773 [NGC 6838] Sneden, C., Kraft, R.P., Prosser, C.F., and Langer, G.E. 1992, AJ 104, 2121 [NGC 5904] Sneden, C., Kraft, R.P., Shetrone, M.D., Smith, G.H., Langer, G.E., and Prosser, C.F. 1997, AJ, 114, 1964 [NGC 7078] Suntzeff, N.B., and Kraft, R.P. 1996, AJ, 111, 1913 [NGC 5139] Suntzeff, N.B., Kraft, R.P., and Kinman, T.D. 1988, AJ 95, 91 [NGC 2419,4147,5024,5053] Suntzeff, N., Olszewski, E., and Stetson, P.B. 1985, AJ 90, 1481 [AM-1] Tavarez, M, and Friel, E.D. 1995, AJ 110, 223 [Lynga 7] Wachter, S., Wallerstein, G., Brown, J.A., & Oke, J.B. 1998, PASP, 110, 821 [NGC 6229, 7006] RADIAL VELOCITY Most of the radial velocity data come from the four major sources listed below. However, numerous more recent sources are also available for smaller lists of objects; in many cases these are based on large samples of stars from CORAVEL or multi-object echelle spectra with very high internal precision (+-1 km/s or less) and almost totally supersede any previous data. The adopted v_r for each cluster is the average of the available measurements, each one weighted inversely as the published uncertainty. Unlike many globular cluster parameters, it is possible to quantify the uncertainty in v_r on an individual basis reasonably well, so the calculated uncertainty in the mean v_r is also given in the data table. The quoted uncertainties should be taken as internal ones (precisions). The true external uncertainties are likely to be a factor of 2 higher in general and are harder to evaluate correctly; see the extensive discussions of Webbink (1981) and Rutledge et al. (1997). Correction of the heliocentric velocity v_r to the Solar Local Standard of Rest is calculated by v_LSR = v_r + 10.4 cos b cos l + 14.8 cos b sin l + 7.3 sin b Major Sources: Dubath, P., Meylan, G., and Mayor, M. 1997, AAp, 326, 614 [24 clusters excluding NGC 6522] Hesser, J.E., Shawl, S.J., and Meyer, J.E. 1986, PASP 98, 403 [89 clusters excluding NGC 6522] Rutledge, G.A., Hesser, J.E., Stetson, P.B., Mateo, M., Simard, L., Bolte, M., Friel, E.D., and Copin, Y. 1997, PASP, 109, 883 [52 clusters; their quoted uncertainties have been reduced by a factor of 2.3 throughout to correspond to their INTERNAL measurement uncertainties and thus to make them comparable to the other studies; see their discussion.] Webbink, R.F. 1981, ApJSuppl 45, 259 [85 clusters; complete literature survey up to 1981] Zinn, R., and West, M.J. 1984, ApJSuppl 55, 45 [58 clusters; these velocities are corrected by -5 km/s to normalize them to the more recently calibrated velocity of their adopted reference cluster, NGC 104. The adopted uncertainty of these velocities is taken to be +-15 km/sec.] Additional Sources: Armandroff, T.E., and Da Costa, G.S. 1986, AJ 92, 777 [NGC 104,1851,7078,7089] Armandroff, T.E., and Da Costa, G.S. 1991, AJ 101, 1329 [Pal 12, Eridanus] Armandroff, T.E., Da Costa, G.S., and Zinn, R. 1992, AJ 104, 164 [Pal 3,4,14] Armandroff, T.E., and Zinn, R. 1988, AJ 96, 92 [NGC 1851,5694,5824,5927,6093,6356,6528, Ter 1,2,4,5,6,9, HP1, Liller 1] Beers, T.C., Preston, G.W., Shectman, S.A., and Kage, J.A. 1990, AJ, 100, 849 [NGC 3201,5272,6121,6341,6397,6752] Clementini, G., Merighi, R., Pasquini, L., Cacciari, C., and Gouiffes, C. 1994, MNRAS 267, 83 [NGC 6121] Cohen, J.G., & McCarthy, J.K. 1997, AJ, 113, 1353 [NGC 6341] Cote, P. 1999, preprint [NGC 6256, 6380, 6540, 6749, IC 1257, 1276, Ter 3, Ter 12, Ton 2, Pal 10, Dj 1] Cote, P., Hanes, D.A., McLaughlin, D.E., Bridges, T.J., Hesser, J.E., and Harris, G.L.H. 1997, ApJLett, 476, L15 [NGC 6402] Cote, P., Pryor, C., McClure, R., Fletcher, J.M., and Hesser, J.E. 1996, AJ, 112, 574 [NGC 6656] Cote, P., Welch, D.L., Fischer, P., and Gebhardt, K. 1995, ApJ 454, 788 [NGC 3201] Da Costa, G.S. 1982, PASP 94, 769 [NGC 1851] Da Costa, G.S., and Armandroff, T.E. 1995, AJ 109, 2533 [NGC 6366, 6626, 6715, Pal 15, Ter 7, Ter 8, Arp 2] Da Costa, G.S., and Seitzer, P. 1989, AJ 97, 405 [NGC 6171,6366] Drukier, G.A., Slavin, S.D., Cohn, H.N., Lugger, P.M., Berrington, R.C., Murphy, B.W., & Seitzer, P.O. 1998, AJ, 115, 708 [NGC 7078] Dubath, P., and Meylan, G. 1994, AAp, 290, 104 [NGC 7078] Fischer, P., Welch, D.L., Mateo, M., and Cote, P. 1993, AJ 106, 1508 [NGC 362] Gebhardt, K., Pryor, C., Williams, T.B., Hesser, J.E., and Stetson, P.B. 1997, AJ, 113, 1026 [NGC 7078] Geisler, D., Piatti, A.E., Claria, J.J., and Minniti, D. 1995, AJ 109, 605 [NGC 1904, 2298, 4372, 4590, 4833, 5053, 5694, 5897, 6101, 6121, 6144, 6397] Gratton, R.G. 1982, AAp 115, 171 [NGC 2808] Grindlay, J., Bailyn, C., Mathieu, R., and Latham, D. 1987, in Globular Cluster Systems in Galaxies, IAU Symposium 126, ed. J.Grindlay and A.G.D.Philip (Dordrecht: Reidel), 659 [NGC 6712] Harris, H.C., Nemec, J.M., and Hesser, J.E. 1983, PASP 95, 256 [NGC 6218,6779] Kraft, R.P., Sneden, C., Smith, G.H., Shetrone, M.D., & Fulbright, J. 1998, AJ, 115, 1500 [NGC 7006] Lin, D.N.C., and Richer, H.B. 1992, ApJ 388, L57 [Rup 106] Lupton, R.H., Gunn, J.E., and Griffin, R.F. 1987, AJ 93, 1114 [NGC 6205] Meylan, G., Dubath, P., and Mayor, M. 1991, ApJ, 383, 587 [NGC 104] Meylan, G., and Mayor, M. 1986, AAp 166, 122 [NGC 104,5139] Minniti, D. 1995, A&ASuppl 113, 299 [NGC 104, 288, 362, 1851, 5272, 6121, 6356, 6366, 6401, 6440, 6517, 6528, 6553, 6624, 6637, 6642, 6626, 6656, 6838, 7078, Pal 6] Olszewski, E.W., Peterson, R.C., and Aaronson, M. 1986, ApJ 302, L45 [NGC 5272,5904, Pal 4,14,15] Olszewski, E.W., Pryor, C., and Schommer, R.A. 1993, in The Globular Cluster - Galaxy Connection, ASP Conf.Series 48, ed. G.H.Smith and J.P.Brodie (San Francisco: ASP), 99 [NGC 2419] Peterson, R.C. 1985, ApJ 297, 309 [NGC 1904,2419,4147,5634, Pal 3,5,14, Eridanus] Peterson, R.C., and Cudworth, K.M. 1994, ApJ 420, 612 [NGC 6656] Peterson, R.C., and Latham, D.W. 1986, ApJ 305, 645 [NGC 5466,6121,6656,6838] Peterson, R.C., and Latham, D.W. 1989, ApJ 336, 178 [Pal 15] Peterson, R.C., Olszewski, E.W., and Aaronson, M. 1986, ApJ 307, 139 [NGC 288,1904,2419,4147,5272,5466,5904,6121,7078, Pal 3,4, Eridanus] Peterson, R.C., Rees, R.F., and Cudworth, K.M 1995, ApJ 443, 124 [NGC 6121] Peterson, R.C., Seitzer, P., and Cudworth, K.M. 1989, ApJ 347, 251 [NGC 7078] Piatek, S., Pryor, C., McClure, R.E., Fletcher, J.M., and Hesser, J.E. 1994, AJ 107, 1397 [NGC 6171] Pryor, C., McClure, R.D., Fletcher, J.M., and Hesser, J.E. 1987, in Globular Cluster Systems in Galaxies, IAU Symposium 126, ed. J.Grindlay and A.G.D.Philip (Dordrecht: Reidel), 661 [NGC 4147,6171,6218] Pryor, C., McClure, R.D., Fletcher, J.M., and Hesser, J.E. 1989, AJ 98, 596 [NGC 6624,6626,6681] Pryor, C., McClure, R.D., Fletcher, J.M., and Hesser, J.E. 1991, AJ 102, 1026 [NGC 288,5466,6809] Pryor, C., and Meylan, G. 1993, in Structure and Dynamics of Globular Clusters, ASP Conf.Series 50, ed. G.Meylan and S. Djorgovski (San Francisco: ASP), 357 [NGC 288,1904,4590,6362,6535,6624,6656,6779,6809, 6838,6934,7099] Pryor, C., Schommer, R.A. and Olszewski, E.W. 1991, in ASP Conf.Series 13, ed. K.Janes (San Francisco: ASP), 439 [NGC 5053,5466] Rastorguev, A.S., and Samus, N.N. 1991, Sov.Astron.Letters 17, 388 [NGC 5904,6121,6218,6254,6838] Rosenberg, A., Piotto, G., Savianne, I., Aparicio, A., and Zaggia, S.R. 1998, AJ, 115, 658 [Pal 1] Suntzeff, N., and Kraft, R.P. 1996, AJ, 111, 1913 [NGC 5139] Suntzeff, N.B.,, Mateo, M., Terndrup, D.M., Olszewski, E.W., Geisler, D., & Weller, W. 1993, ApJ, 418, 208 [NGC 4590, 5904, 5927, 6121, 6171, 6218, 6397, 6712, 6752, 6838, 7099] Suntzeff, N., Olszewski, E., and Stetson, P.B. 1985, AJ 90, 1481 [AM-1] Tavarez, M., and Friel, E.D. 1995, AJ 110, 223 [Lynga 7] Terndrup, D.M., Popowski, P., Gould, A., Rich, R.M., and Sadler, E.M. 1998, AJ, 115, 1476 [NGC 6522] Yan, L., and Cohen, J.G. 1996, AJ, 112, 1489 [NGC 5053] Zaggia, S.R., Capaccioli, M., Piotto, G., and Stiavelli, M. 1992, AAp 258, 302 [NGC 1904] Zaritsky, D., Olszewski, E.W., Schommer, R.A., Peterson, R.C., and Aaronson, M. 1989, ApJ 345, 759 [Pal 14, Eridanus] Here are the bibliographic sources, listed by cluster. The abbreviation code is: W81 = Webbink 1981, HSM86 = Hesser, Shawl, & Meyer 1986, etc. NGC 104 W81, HSM86, R&&97, DMM97, AD86, MDM91, MM86, M95 NGC 288 W81, R&&97, M95, POA86, PMFH91, PM93 NGC 362 W81, HSM86, ZW84, R&&97, DMM97, FWMC93, M95 NGC 1261 W81, HSM86, R&&97 Pal 1 R&&98 AM 1 SOS85 Eridanus W81, AD91, P85, POA86, Z&&89 Pal 2 W81 NGC 1851 W81, HSM86, DMM97, AZ88, AD86, D82, M95 NGC 1904 W81, HSM86, DMM97, GPCM95, P85, POA86, PM93, ZCPS92 NGC 2298 W81, HSM86, R&&97, GPCM95 NGC 2419 W81, OPS93, P85, POA86 Pyxis NGC 2808 W81, HSM86, ZW84, R&&97, G82 E 3 Pal 3 W81, ADZ92, P85, POA86 NGC 3201 W81, HSM86, R&&97, BPSK90, CWFG95 Pal 4 W81, ADZ92, OPA86, POA86 NGC 4147 W81, HSM86, P85, POA86, PMFH87 NGC 4372 W81, HSM86, R&&97, GPCM95 Rup 106 LR92 NGC 4590 W81, HSM86, ZW84, R&&97, GPCM95, PM93, S&&93 NGC 4833 W81, HSM86, ZW84, R&&97, GPCM95 NGC 5024 W81, HSM86 NGC 5053 GPCM95, PSO91, YC96 NGC 5139 W81, HSM86, MM86, SK96 NGC 5272 W81, HSM86, DMM97, BPSK90, M95, OPA86, POA86 NGC 5286 W81, HSM86, ZW84, R&&97, DMM97 AM 4 NGC 5466 W81, PL86, POA86, PMFH91, PSO91 NGC 5634 W81, HSM86, P85 NGC 5694 W81, HSM86, ZW84, DMM97, AZ88, GPCM95 IC 4499 NGC 5824 W81, HSM86, ZW84, DMM97, AZ88 Pal 5 P85 NGC 5897 HSM86, R&&97, GPCM95 NGC 5904 W81, HSM86, ZW84, R&&97, DMM97, OPA86, POA86, RS91, S&&93 NGC 5927 W81, HSM86, ZW84, R&&97, AZ88, S&&93 NGC 5946 HSM86, ZW84, DMM97 BH 176 NGC 5986 W81, HSM86, R&&97 Lynga 7 TF95 Pal 14 W81, ADZ92, OPA86, P85, Z&&89 NGC 6093 W81, HSM86, R&&97, DMM97, AZ88 NGC 6121 W81, HSM86, ZW84, R&&97, BPSK90, C&&94, GPCM95, M95, PL86, POA86, PRC95, RS91, S&&93 NGC 6101 HSM86, ZW84, R&&97, GPCM95 NGC 6144 HSM86, ZW84, R&&97, GPCM95 NGC 6139 W81, HSM86 Terzan 3 C99 NGC 6171 HSM86, ZW84, R&&97, DS89, P&&94, PMFH87, S&&93 1636-283 NGC 6205 W81, LGG87 NGC 6229 W81 NGC 6218 W81, HSM86, R&&97, HNH83, PMFH87, RS91, S&&93 NGC 6235 HSM86, ZW84, R&&97 NGC 6254 W81, HSM86, R&&97, RS91 NGC 6256 DMM97, C99 Pal 15 DA95, OPA86, PL89 NGC 6266 W81, HSM86, ZW84, R&&97, DMM97 NGC 6273 W81, HSM86, ZW84, R&&97 NGC 6284 W81, HSM86, DMM97 NGC 6287 HSM86 NGC 6293 W81, HSM86, ZW84, DMM97 NGC 6304 W81, HSM86, ZW84, R&&97 NGC 6316 HSM86, ZW84 NGC 6341 W81, BPSK90, CM97 NGC 6325 HSM86, ZW84, DMM97 NGC 6333 W81, HSM86 NGC 6342 HSM86, ZW84, DMM97 NGC 6356 W81, HSM86, ZW84, AZ88, M95 NGC 6355 HSM86, ZW84 NGC 6352 HSM86, ZW84, R&&97 IC 1257 C99 Terzan 2 AZ88 NGC 6366 R&&97, DA95, DS89, M95 Terzan 4 AZ88 HP 1 AZ88 NGC 6362 W81, HSM86, ZW84, R&&97, PM93 Liller 1 AZ88 NGC 6380 C99 Terzan 1 AZ88 Ton 2 C99 NGC 6388 W81, HSM86, ZW84 NGC 6402 W81, HSM86, C&&97 NGC 6401 HSM86, ZW84, M95 NGC 6397 W81, HSM86, R&&97, DMM97, BPSK90, GPCM95, S&&93 Pal 6 M95 NGC 6426 HSM86 Djorg 1 C99 Terzan 5 AZ88 NGC 6440 W81, HSM86, ZW84, M95 NGC 6441 W81, HSM86, ZW84, DMM97 Terzan 6 AZ88 NGC 6453 HSM86, ZW84 UKS 1 NGC 6496 HSM86, ZW84, R&&97 Terzan 9 AZ88 Djorg 2 NGC 6517 HSM86, ZW84, M95 Terzan10 NGC 6522 R&&97, T&&98 NGC 6535 HSM86, ZW84, R&&97, PM93 NGC 6528 W81, HSM86, ZW84, R&&97, AZ88, M95 NGC 6539 HSM86, ZW84 NGC 6540 C99 NGC 6544 W81, HSM86, ZW84, R&&97 NGC 6541 W81, HSM86, R&&97 NGC 6553 W81, HSM86, ZW84, R&&97, M95 NGC 6558 HSM86, ZW84, DMM97 IC 1276 C99 Terzan12 C99 NGC 6569 HSM86, ZW84 NGC 6584 W81, HSM86 NGC 6624 W81, HSM86, ZW84, R&&97, M95, PMFH89, PM93 NGC 6626 W81, HSM86, R&&97, DA95, M95, PMFH89 NGC 6638 W81, HSM86, ZW84, R&&97 NGC 6637 W81, HSM86, ZW84, R&&97, M95 NGC 6642 W81, HSM86, ZW84, M95 NGC 6652 W81, HSM86, ZW84 NGC 6656 W81, HSM86, C&&96, M95, PC94, PL86, PM93 Pal 8 ZW84 NGC 6681 W81, HSM86, R&&97, DMM97, PMFH89 NGC 6712 W81, HSM86, ZW84, R&&97, GBML87, S&&93 NGC 6715 W81, HSM86, ZW84, DA95 NGC 6717 HSM86, ZW84, R&&97 NGC 6723 HSM86, ZW84, R&&97 NGC 6749 C99 NGC 6752 W81, HSM86, ZW84, R&&97, DMM97, BPSK90, S&&93 NGC 6760 HSM86, ZW84 NGC 6779 W81, HNH83, PM93 Terzan 7 DA95 Pal 10 C99 Arp 2 DA95 NGC 6809 W81, HSM86, ZW84, R&&97, PMFH91, PM93 Terzan 8 DA95 Pal 11 W81 NGC 6838 W81, HSM86, M95, PL86, PM93, RS91, S&&93 NGC 6864 W81, HSM86, ZW84 NGC 6934 W81, HSM86, PM93 NGC 6981 W81, HSM86, ZW84, R&&97 NGC 7006 W81, HSM86, R&&97, K&&98 NGC 7078 W81, HSM86, ZW84, DMM97, AD86, D&&98, DM94, G&&97, M95, POA86, PSC89 NGC 7089 W81, HSM86, ZW84, R&&97, AD86 NGC 7099 W81, HSM86, ZW84, R&&97, DMM97, PM93, S&&93 Pal 12 W81, R&&97, AD91 Pal 13 W81 NGC 7492 W81, R&&97 STRUCTURAL AND DYNAMIC PARAMETERS Primary Sources: Djorgovski S. 1993, in Structure and Dynamics of Globular Clusters, ASP Conf.Series 50, ed. S.G.Djorgovski and G.Meylan (San Francisco: A.S.P.), 373 Trager S.C, Djorgovski S., and King I.R. 1993, in Structure and Dynamics of Globular Clusters, ASP Conf.Series 50, ed. S.G.Djorgovski and G.Meylan (San Francisco: A.S.P.), 347 Trager, S.C., King, I.R., and Djorgovski, S. 1995, AJ 109, 218 van den Bergh S., Morbey C., and Pazder J. 1991, ApJ 375, 594 Webbink R.F. 1985, in Dynamics of Star Clusters, IAU Symposium 113, ed. J.Goodman and P.Hut (Dordrecht: Reidel), 541 The cluster core radii r_c, and the central concentration c = log(r_t/r_c), where r_t is the tidal radius, are taken primarily from the comprehensive discussion of Trager et al. (1993). Updates for a few clusters (Pal 2, N6144, N6352, Ter 5, N6544, Pal 8, Pal 10, Pal 12, Pal 13) are taken from Trager, King, and Djorgovski (1995). The half-mass radius r_h is taken from the direct average of Trager et al. and van den Bergh et al. There are about 20 clusters for which Trager et al. quote values of c and r_c, but for which r_h is not given by either source. For these, estimates of r_h have been calculated from the approximate relation log (r_h/r_c) = 0.6 c - 0.4 which is accurate to about 20%. These objects are mostly sparse or low-luminosity clusters. WARNING: The listed values of r_c and c should not be used to calculate a value of tidal radius r_t for core-collapsed clusters. King (private communication) notes that the Trager et al. list arbitrarily adopt c = 2.50 for such clusters, and these have been carried over to the present catalog. Additional sources for certain clusters are the following: Peterson C., & King, I. 1975, AJ, 80, 427 (in cases where Trager et al. list c = 2.5, this paper lists the measured tidal radius) Cote, P., Welch, D.L., Fischer, P., & Gebhardt, K. 1995, ApJ, 454, 788 [NGC 3201] Da Costa, G.S., & Freeman, K.C. 1976, ApJ, 206, 128 [NGC 5272] Harris, W.E., Durrell, P.R., Petitpas, G.R., Webb, T.M., & Woodworth, S.C. 1997, AJ, 114, 1043 [Pal 2] Harris, W.E., & van den Bergh, S. 1984, AJ, 89, 1816 [Pal 14, 15] Kaisler, D., Harris, W.E., & McLaughlin, D.E. 1997, PASP, 109, 920 [NGC 6749, Pal 10] Lehmann, I., & Scholz, R.-D. 1997, AAp, 320, 776 [NGC 5904, 6218, 6205, 7078, 5024, 5053, 5466] Meylan, G. 1988, AAp, 191, 215 [NGC 104] Sandage, A., & Hartwick, F.D.A. 1977, AJ, 82, 459 [Pal 5] Tucholke, H.-J. 1992, AAp, 264, 513 [NGC 104, 362] The central surface brightness mu_V (magnitudes per square arcsecond) is the average of the values from Trager et al. (1993) and Webbink (1985), with a few updates from Trager et al. (1995) (for HP 1, Ter 5, Pal 12, and Pal 13). The central luminosity density, rho_0, in solar luminosities per cubic parsec, is calculated from the prescription given by Djorgovski (1993), using the previously determined values of the central surface brightness, total cluster luminosity, and core radius. These are different in some cases from the values listed by Djorgovski, because of revisions to the cluster distances. The relaxation times in the core and at the half-mass radius, t(r_c) and t(r_h), are calculated using the prescriptions of Djorgovski (1993) with one correction: the coefficient in front of t(r_h) in Djorgovski's equation (11) is 2.055 x 10^6 instead of 8.933 x 10^5, which is larger by ln(10) (I thank Ivan King and Douglas Heggie for bringing this to my attention). This revision brings it in line (e.g.) with Binney and Tremaine, Galactic Dynamics, equation (8-72). A mean stellar mass of 1/3 M_sun and a mean mass to light ratio of M/L = 2 are assumed here for purposes of this calculation.