CATALOG OF PARAMETERS FOR MILKY WAY GLOBULAR CLUSTERS

Compiled by William E. Harris, McMaster University Last revision: June 1994

Source lists, calibration parameters, and conversion relations for the cluster data are described below.

CLUSTER IDENTIFICATIONS AND COORDINATES

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 following exceptions:

AM-2 is excluded, since it is almost certainly an old open cluster (Gratton and Ortolani 1988, AASuppl. 74, 299).

Reticulum is excluded as more likely belonging to the LMC (e.g. Walker 1992, AJ 103, 1166).

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. 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 (Djorgovski and Meylan 1994, AJ, in press). With the changes noted, the present catalog contains 141 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.

The cluster coordinates are taken from Djorgovski and Meylan (1993).

FOREGROUND REDDENING E(B-V)

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 [86 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).

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 (113 clusters); in a few cases where CMDs are not yet available, it can be evaluated from single-color photometry of the RR Lyrae variables (5 clusters), or more roughly predicted from the magnitude level of the brightest red giants (16 clusters). 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) = 0.2 [Fe/H] + 1.00

which matches the body of recent evidence both from distance measurements of field RR Lyrae stars (e.g. Carney, Storm, and Jones 1992, ApJ, 386, 663; Skillen et al. 1993, MNRAS, 265, 30) and from theoretical stellar models of HB stars (e.g. Lee 1990, ApJ, 363, 159). The absolute uncertainty of the predicted M_V(HB) is +-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 M_V(HB) = 0.8 is simply assumed.

NGC 104 Hesser J.E., Harris W.E., VandenBerg D.A., Allwright J.W.B., Shott P., and Stetson P.B., 1987, PASP, 94, 739
NGC 288 Bergbusch P.A., 1993, AJ 106, 1024
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 Ortolani S., and Rosino L., 1985, Mem.Soc.Astr.Ital. 56, 105
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., 1980, PASP 92, 43 (Brightest Giants)
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
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 Alcaino G., Liller W., Alvarado F., and Wenderoth E., 1991, AJ 102, 159
Rup 106 Buonanno R., Buscema G., Fusi Pecci F., Richer H.B., and Fahlman G.G., 1990, AJ 100, 1811
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 Sandage A., Katem B., and Johnson H.L., 1977, AJ 82, 389
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 Harris W.E., Racine R., and de Roux J., 1976, ApJSuppl 31, 13
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 Sarajedini A., 1993, AJ 105, 2172
NGC 5824 Cannon R.D., Sagar R. and Hawkins M.R.S., 1990, MNRAS 243, 151
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 Storm J., Carney B.W., and Beck, J., 1991, PASP 103, 1264
NGC 5927 Sarajedini A., and Norris J.E., 1994, ApJSuppl, in press; 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
NGC 5986 Bond H., Harris W.E., Harris G.L.H., Mittermeier R., and Palmer K., 1994, in preparation
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 Hazen M., 1991, AJ 101, 170 (RR Lyraes)
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
NGC 6205 Sandage A., 1970, ApJ 162, 841
NGC 6218 Racine R., 1971, AJ 76, 331
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 Caloi V., Castellani V., and Piccolo F., 1987, AApSuppl 67, 181
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. 1994, PASP, preprint
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, in preparation
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 Sandage A., and Wallerstein G., 1960, ApJ 131, 598
NGC 6355 Harris W.E., 1980, in Star Clusters, IAU Symposium 85 ed. J.E.Hesser (Dordrecht: Reidel), 81 (Brightest Giants)
NGC 6352 Sarajedini A., and Norris J.E., 1994, ApJSuppl, in press
Terzan 2 Christian C.A., and Friel E.D., 1992, AJ 103, 142
NGC 6366 Harris H.C., 1993, AJ 106, 604
NGC 6362 Alcaino G., and Liller W., 1986, AJ 91, 303
HP 1 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)
Liller 1 Ortolani S., Bica E., and Barbuy B. 1994, Messenger 75, 26
Terzan 1 Ortolani S., Bica E., and Barbuy B., 1993, AAp 267, 66
NGC 6388 Alcaino G., 1981, AApSuppl 44, 33
Ton 2 Webbink R.F., 1985, in Dynamics of Star Clusters, IAU Symposium 113, ed. J.Goodman and P.Hut (Dordrecht: Reidel), 541 (Brightest Giants)
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, in preparation
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. 1994, Messenger 75, 26
NGC 6426 Harris W.E., 1980, in Star Clusters, IAU Symposium 85, ed. J.E.Hesser (Dordrecht: Reidel), 81 (Brightest Giants)
Djorg 1 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 6440 Martins D.H., Harvel C.A., and Miller D.H., 1980, AJ 85, 521
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)
NGC 6496 Sarajedini A., and Norris J.E., 1994, ApJS, in press; also Friel E.D., and Geisler D., 1992, AJ 101, 1338
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. 1994, in preparation
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 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 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 Harris W.E., 1980, in Star Clusters, IAU Symposium 85, ed. J.E.Hesser (Dordrecht: Reidel), 81 (Brightest Giants)
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., 1994, preprint
NGC 6624 Sarajedini A., and Norris J.E., 1994, ApJSuppl, in press
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 Sarajedini A., and Norris J.E., 1994, ApJSuppl, in press
NGC 6642 Hazen M.L., 1993, AJ 105, 557 (RR Lyraes)
NGC 6652 Harris W.E., 1980, in Star Clusters, IAU Symposium 85, ed. J.E.Hesser (Dordrecht: Reidel), 81 (Brightest Giants)
NGC 6656 Cudworth K.M., 1986, AJ 92, 348
Pal 8 Armandroff T.E., 1988, AJ 96, 588
NGC 6681 Mittermeier R., Harris G.L.H., Bond H., Harris W.E., and Palmer K., 1994, in preparation
NGC 6712 Cudworth K.M., 1988, AJ 96, 105
NGC 6715 Harris W.E., 1975, ApJSuppl 29, 397
NGC 6717 Jensen N., Harris W.E., and Bond H., 1994, in preparation
NGC 6723 Fullton L.K., and Carney B.W., 1993, Bull. AAS, 25, 1407
NGC 6749 Canterna R., and Rosino L., 1981, AApSuppl 45, 53 (Brightest Giants)
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 Webbink R.F., 1985, in Dynamics of Star Clusters, IAU Symposium 113, ed. J.Goodman and P.Hut (Dordrecht: Reidel), 541 (Brightest Giants)
NGC 6779 Wehlau A., and Sawyer Hogg H., 1985, AJ 90, 2514
Pal 10 Canterna R., and Rosino L., 1981, AApSuppl 45, 53 (Brightest Giants)
Arp 2 Seitzer P., and Phillips M.M., 1984, unpublished
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 Harris W.E., and Racine R., 1973, AJ 78, 242
NGC 6981 Dickens R.J., 1972, MNRAS 157, 281
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 Ortolani S., Rosino L., and Sandage A., 1985, AJ 90, 473
NGC 7492 Cote P., Richer H.B., and Fahlman G.G., 1991, AJ 102, 1358

INTEGRATED VISUAL MAGNITUDE V_t

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, 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.

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

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.

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.

Lee Y.-W., Demarque P., and Zinn R. 1994, preprint
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, the distribution of stars along the HB is clearly bimodal, thus the cluster is assigned two simultaneous HB types.

METALLICITIES: [Fe/H] VALUES

The heavy-element abundance scale adopted here is basically the one established by Zinn and West (1984, ApJSuppl, 55, 45). 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.

Armandroff, T.E., and Zinn, R. 1988, AJ 96, 92 [27 clusters]
Zinn, R. 1985, ApJ 293, 424 [111 clusters]

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]
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]
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., 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]
Francois, P. 1991, AAp 247, 56 [NGC 1904,5927,6352]
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]
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 92, 338 [NGC 6838]
McWilliam, A., Geisler, D., and Rich, R.M. 1992, PASP 104, 1193 [NGC 2298]
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]
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., Prosser, C.F., and Langer, G.E. 1992, AJ 104, 1211 [NGC 5904]
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]

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 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.

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

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]

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]
Clementini, G., Merighi, R., Pasquini, L., Cacciari, C., and Gouiffes, C. 1994, MNRAS 267, 83 [NGC 6121]
Cote, P., Welch, D.L., Fischer, P., and Irwin, M. 1994, preprint [NGC 3201]
Da Costa, G.S. 1982, PASP 94, 769 [NGC 1851]
Da Costa, G.S., and Seitzer, P. 1989, AJ 97, 405 [NGC 6171,6366]
Fischer, P., Welch, D.L., Mateo, M., and Cote, P. 1993, AJ 106, 1508 [NGC 362]
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]
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STRUCTURAL AND DYNAMIC PARAMETERS

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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). The half-mass radius r_h is taken from the direct average of Trager et al. and van den Bergh et al. There are 22 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 22 objects are mostly sparse or low-luminosity clusters.

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). 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.