CATALOG OF PARAMETERS FOR MILKY WAY GLOBULAR CLUSTERS Compiled by William E. Harris, McMaster University This revision: May 15, 1997 This catalog is described in the literature by: Harris, W.E. 1996, AJ, 112, 1487. Please refer to that paper in any published use you make of this catalog. 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 in this anonymous ftp directory. Both files are also accessible through WorldWideWeb. The URL label is: http://www.physics.mcmaster.ca/Globular.html ______________________________________________________________________ REVISIONS AND HIGHLIGHTS FOR MAY 1997 EDITION: - IC 1257, previously listed as an open cluster, has been shown to be a globular cluster (Harris et al. 1997, AJ, 113, 688) - A major new set of radial velocities (Rutledge et al. 1997, PASP in press) has been added to the database. - Galactic coordinates (l,b) are now given to 2 decimal places. - A new DISTANCE SCALE has been adopted, to correspond to the brighter horizontal-branch luminosity now favored by subdwarf parallaxes (both Hipparcos and ground-based data), the matching of the RR Lyrae luminosities to the Cepheid distance scale in Local Group galaxies, and theoretical models for HB star luminosities. See the "Distances" section below for explanation. - Many new entries have been made for cluster distances, thanks to continuing activity in color-magnitude studies for the less well known clusters. Of the 147 cataloged clusters, there are now only two remaining (NGC 6380 and Terzan 12) which have no useful distance estimates at all. ______________________________________________________________________ REVISIONS FOR APRIL 1996 EDITION: - The Pyxis system is added, as a newly discovered globular cluster by Irwin, Demers, & Kunkel 1995 (ApJ 453, L21) - BH 176 is reinstated as a probable globular cluster (Ortolani, Bica, and Barbuy 1995, A&A 300, 726). - Lynga 7, sometimes thought to be an old open cluster, is now more likely a globular (Tavarez and Friel 1995, AJ 110, 223) - ESO 452-SC11 is reinstated as a probable globular cluster on the basis of evidence by Minniti, Olszewski, and Rieke 1995 (AJ 110, 1686) - Terzan 10 is reinstated as a globular cluster on the basis of infrared photometry by Liu et al. 1995 (see the reference given below in the section on distances) Deletions: - AM-2 is excluded, since it is clearly an old open cluster (Ortolani, Bica, and Barbuy 1995, A&A 300, 726). - Reticulum is excluded as more likely belonging to the LMC (e.g. Walker 1992, AJ 103, 1166). - A candidate globular cluster announced by Bica (1994, AA 285, 868) was added to earlier versions of this catalog as 'Bica 1', but new data (Bica et al. 1995, A&A 303, 747) show that it is not a cluster. Certain other objects in the catalog of Webbink (1985) proposed as globular cluster candidates have been shown not to be clusters or are improbable globulars, including TJ5, TJ15, TJ16, TJ17, TJ23, TBJ3, Kodaira 1, Grindlay 1, ESO 166-SC11 (UKS2), and ESO 093-SC08. See the discussions of Djorgovski and Meylan (1993), Minniti, Olszewski, and Rieke 1995 (AJ 110, 1686), Bica et al. 1995 (A&A 303, 747), and Kodaira, Greene, and Tokunaga 1995 (PASJ 47, 29). ______________________________________________________________________ NOTES FROM PRE-1996 EDITIONS: - Terzan 12 is restored to its original designation; it has mistakenly been labelled as Terzan 11 in several previous catalogs (including Kukarkin 1974, Harris and Racine 1979, Webbink 1985, and Djorgovski and Meylan 1993). To add to the potential confusion, the object number 11 in Terzan's lists is actually a rediscovery of Terzan 5; furthermore, the `Terzan 12' designation has sometimes been applied, quite wrongly, to NGC 6256, which is a completely different object. To avoid all such identification problems, it seems preferable to keep the original notation for these objects. - Djorgovski 3 has now been cross-identified as NGC 6540 (Bica, Ortolani, and Barbuy 1994, AA 283, 67). - A serious error in the coordinates of Palomar 14 has been corrected, using data from the HST Guide Star Catalog. They are now accurate to +-5". _______________________________________________________________________ _______________________________________________________________________ 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 [114 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 straight averages of the given sources (up to 4 per cluster). 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 absolute calibration of V_HB adopted here uses a modest dependence of absolute V magnitude on metallicity, M_V(HB) = 0.15 [Fe/H] + 0.85 Please note that M_V(HB) here denotes the mean magnitude of the HB stars, without further adjustments to any predicted ZAHB level: 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. The zero point adopted here 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 slope of 0.15 matches the body of recent evidence both from 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) and from theoretical stellar models of HB stars (e.g. Lee, Demarque, and Zinn 1990, ApJ, 350, 155; Dorman 1992, ApJSuppl, 81, 221; Salaris, Degl'Innocenti, and Weiss 1997, ApJ, 479, 665). The zero point adopted here matches the horizontal-branch models referred to above, as well as calibrations of the RR Lyrae luminosity level by Cepheids in 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). It is ~0.2 mag brighter than the statistical-parallax and Baade-Wesselink measurements referred to above would give, but it is also (perhaps) the same amount fainter than recent Hipparcos calibrations of M_V(HB) through field subdwarfs and other halo stars (e.g. Reid 1997, Feast and Catchpole 1997, Pont et al. 1997; the Hipparcos-based analyses are just starting to reach the literature at time of writing, and these various discussions are not yet in full agreement). The currently adopted zero point is a compromise among these many different calibrations, and further revision may yet be required. 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. 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: 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 Borissova, J., and Spassova, N. 1995, AApSuppl 110, 1 AM 1 Madore B.F., and Freedman W.L., 1989, ApJ 340, 812 Eridanus Ortolani S., and Gratton R., 1989, AApSuppl 79, 155 Pal 2 Harris, W.E., Durrell, P.R., Petitpas, G.R., Webb, T.M., and Woodworth, S.C. 1997, AJ, submitted NGC 1851 Walker A.R., 1992, PASP 104, 1063 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 Christian C.A., and Heasley J.N., 1988, AJ 95, 1422; also 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, submitted 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 Ortolani S., and Gratton R., 1989, AApSuppl 79, 155 NGC 3201 Brewer J.P., Fahlman G.G., Richer H.B., Searle L., and Thompson I., 1993, AJ 105, 2158 Pal 4 Christian C.A., and Heasley J.N., 1986, ApJ 303, 216 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 Heasley J.N., and Christian C.A., 1991, AJ 101, 967 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 Sandage A., and Katem B., 1982, AJ 87, 537 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 Sandquist, E.L., Bolte, M., Stetson, P.B., and Hesser, J.E. 1996, ApJ, 470, 910 NGC 5927 Sarajedini A., and Norris J.E., 1994, ApJSuppl 93, 161; also Friel E.D., and Geisler D., 1991, AJ 101, 1338 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 Harris W.E., and Racine R., 1974, AJ 79, 472 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 Samus, N.N., Kravtsov, V.V., Pavlov, M.V., Alcaino, G., Liller, W., and Alvarado, F. 1996, Astron.Letters, 22, 686 Terzan 3 Webbink R.F., 1985, in Dynamics of Star Clusters, IAU Symposium 113, ed. J.Goodman and P.Hut (Dordrecht: Reidel), 541 (Brightest Giants) NGC 6171 Cudworth K.M., Smetanka J.J., and Majewski S.R., 1992, AJ 103, 1252 ESO452-SC11 Peterson, C.J. 1986, PASP 98, 1258 (from unpublished data of Webbink and Hunter) NGC 6205 Sandage A., 1970, ApJ 162, 841 NGC 6218 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 NGC 6229 Carney B.W., Fullton L.K., and Trammell S.R., 1991, AJ 101, 1699 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 Alcaino G., 1983, AApSuppl 53, 47 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, in preparation 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 Davidge T.J., Harris W.E., Bridges T.J., and Hanes D.A., 1992, ApJSuppl 81, 251 NGC 6325 Mittermeier R., Harris G.L.H., Bond H., Harris W.E., and Palmer K., 1994, unpublished 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 Armandroff T.E., 1988, AJ 96, 588 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 Kuchinski, L.E., Frogel, J.A., Terndrup, D.M., and Persson, S.E. 1995, AJ 109, 1131 NGC 6366 Harris H.C., 1993, AJ 106, 604 Terzan 4 Ortolani, S., Barbuy, B., and Bica, E. 1997, AAp, 319, 850 NGC 6362 Alcaino G., and Liller W., 1986, AJ 91, 303 HP 1 Ortolani, S., Bica, E., and Barbuy, B. 1997, MNRAS, 284, 692 Liller 1 Frogel, J.A., Kuchinski, L.E., and Tiede, G.P. 1995, AJ 109, 1154 (see Ortolani, S., Bica, E., and Barbuy, B. 1996, AAp 306, 134 for improved reddening estimate) Terzan 1 Ortolani S., Bica E., and Barbuy B., 1993, AAp 267, 66 NGC 6388 Silbermann, N.A., Smith, H.A., Bolte, M., and Hazen, M.L. 1994, AJ 107, 1764 Ton 2 Bica, E., Ortolani, S., and Barbuy, B. 1996, AApSuppl, 120, 153 NGC 6402 Shara M.M., Moffat A.F.J., Potter M., Hogg H.S., and Wehlau A., 1986, ApJ 311, 796 NGC 6401 Mittermeier R., Harris G.L.H., Bond H., Harris W.E., and Palmer K., 1994, unpublished NGC 6397 Alcaino G., Buonanno R., Caloi V., Castellani V., Corsi C.E., Iannicolo G., and Liller W., 1987, AJ 94, 917 Pal 6 Ortolani, S., Bica, E., and Barbuy, B. 1995, AAp 296, 680 NGC 6426 Zinn, R., and Barnes, S. 1996, AJ, 112, 1054 Djorg 1 Ortolani, S., Bica, E., and Barbuy, B. 1995, AAp 296, 680 Terzan 5 Ortolani, S., Barbuy, B., and Bica, E. 1996, AAp, 308, 733 NGC 6440 Ortolani, S., Barbuy, B., and Bica, E. 1994, AApSuppl 108, 653 NGC 6441 Hesser J.E., and Hartwick F.D.A., 1976, ApJ 203, 97 NGC 6453 Harris W.E., 1980, in Star Clusters, IAU Symposium 85, ed. J.E.Hesser (Dordrecht: Reidel), 81 (Brightest Giants) Terzan 6 Fahlman, G.G., Douglas, K.A., and Thompson, I.B. 1995, AJ 110, 2189 UKS 1 Liu, T., McLean, I., and Becklin, E. 1994, in Infrared Astronomy with Arrays, ed. I.McLean (Kluwer), 101 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 Mallen-Ornelas G., and Djorgovski S., 1993, ASP Conf. Series 50, Structure and Dynamics of Globular Clusters, ed. G.Meylan and S.Djorgovski (San Francisco: ASP), 313 (Brightest Giants) NGC 6517 Kavelaars J.J., Hanes D.A., Bridges T.J., and Harris W.E. 1995, AJ, 109, 2081 Terzan 10 Liu, T., McLean, I., and Becklin, E. 1994, in Infrared Astronomy with Arrays, ed. I.McLean (Kluwer), 101 NGC 6522 Terndrup, D., and Walker A., 1994, AJ, 107, 1786 NGC 6535 Sarajedini A., 1994, PASP, 106, 404 NGC 6528 Ortolani S., Bica E., and Barbuy B., 1992, AApSuppl 92, 441 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., 1979, AApSuppl 35, 233 NGC 6553 Ortolani S., Barbuy B., and Bica E., 1990, AAp 236, 362 NGC 6558 Hazen, M.L. 1996, AJ, 111, 1184 [RR Lyraes] IC 1276 Kinman T.D., and Rosino L., 1962, PASP 74, 499 (RR Lyraes) 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, in preparation NGC 6749 Kaisler, D., Harris, W.E., and McLaughlin, D.E. 1997, PASP, in press NGC 6752 Buonanno R., Caloi V., Castellani V., Corsi C., Fusi Pecci F., and Gratton R., 1986, AApSuppl 66, 79 NGC 6760 Armandroff T.E., 1988, AJ 96, 588 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, in press Arp 2 Sarajedini, A., and Layden, A. 1997, AJ, 113, 264 NGC 6809 Lee S-W., 1977, AApSuppl 29, 1 Terzan 8 Ortolani S. ,and Gratton R., 1990, AApSuppl 82, 71 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 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 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 called into serious question as possibly 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, in press). 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. 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] 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] 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] 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] Geisler, D., Piatti, A.E., Claria, J.J., and Minniti, D. 1995, AJ 109, 605 [NGC 2298, 4372, 4833, 5053, 5694, 5897, 6101, 6144] 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] 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] 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] 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] 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: Armandroff, T.E., and Zinn, R. 1988, AJ 96, 92 [27 clusters] Hesser, J.E., Shawl, S.J., and Meyer, J.E. 1986, PASP 98, 403 [90 clusters] 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.] Rutledge, G.A., Hesser, J.e., Stetson, P.B., Mateo, M., Simard, L., Bolte, M., Friel, E.D., and Copin, Y. 1997, PASP, in press [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.] 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] 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] Cote, P., Hanes, D.A., McLaughlin, D.E., Bridges, T.J., Hesser, J.E., and Harris, G.L.H. 1997, ApJLett, 476, L15 Cote, P., Pryor, C., McClure, R., Fletcher, J.M., and Hesser, J.E. 1996, AJ, 112, 574 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] 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] 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] 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] Suntzeff, N., and Kraft, R.P. 1996, AJ, 111, 1913 [NGC 5139] 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] 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] STRUCTURAL AND DYNAMIC PARAMETERS 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 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 their lists arbitrarily adopt c = 2.50 for such clusters, and these have been carried over to the present catalog. The relaxation times in the core and at the half-mass radius, t(r_c) and t(r_h), are taken from Djorgovski (1993). 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.