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********************************************************************** COPYRIGHT NOTICE! THE DATA IN THIS CATALOG ARE SUPPLIED FREE OF CHARGE TO ALL USERS. ANY THIRD PARTY WHO SUPPLIES MATERIAL FROM 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 TO ANY USER. ********************************************************************** CATALOG OF PARAMETERS FOR MILKY WAY GLOBULAR CLUSTERS: THE BIBLIOGRAPHY Compiled by William E. Harris, McMaster University This revision: December 2010 The data file for the clusters is also found on this website. Go to either of the following links and click on "Catalogue": http://physwww.mcmaster.ca/\~harris/Databases.html http://www.physics.mcmaster.ca/?page=globular The correct 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. This is the best way I have of keeping track of the number of uses and citations. When you cite the catalog in your text, please refer to it as "Harris 1996 (2010 edition)". Source lists, calibration parameters, and conversion relations for the cluster data files are described below. Please send me any corrections or additions you know about to harris@physics.mcmaster.ca ______________________________________________________________________ _______________________________________________________________________ CLUSTER IDENTIFICATIONS - Seven new clusters have been added, bringing the total to 157. The new additions are Whiting 1, Koposov 1 and 2, FSR1735, BH261, and GLIMPSE-01 and 02. Although some of these need further confirmation of their identities as globular clusters, enough evidence exists for them to be classified this way. - Over the past decade several other star clusters, or possible star clusters, have been suggested as globular cluster candidates, but to this point the evidence for them is not yet convincing. Decisions about the nature of these objects can still be somewhat arbitrary and depend very much on their location within the Galactic disk, bulge, or halo, their luminosity, and their structural parameters as well as color-magnitude diagrams. Some of these may be ultra-faint dwarf satellites of the Milky Way, some may be old open clusters in the disk. In this "uncertain" category I include: FSR 584 02 27 15 +61 37 28 Source: Bi07 Segue 1 10 07 04 +16 04 55 Be07 Will 1 10 49 24.0 +51 03 00 Wi05 SDSSJ1257+3419 12 57 09.6 +34 19 12 Sa06 FSR 1716 16 10 29.0 -53 44 48 Fr08b FSR 1767 17 35 43 -36 21 28 Bo07 PWM 2 Pfleider 2 17 58 40 -05 04 30 Or09 FSR 190 20 05 31.3 +33 34 09 Fr08a Sources: Be07 = Belokurov, V. et al. 2007, ApJ 654, 897 Bi07 = Bica, E., Bonatto, C., Ortolani, S., and Barbuy, B. 2007, AAp 472, 483 Bo07 = Bonatto, C., Bica, A., Ortolani, S., and Barbuy, B. 2007, MNRAS 381, L45 Fr08a = Froebrich, D., Meusinger, H., and Davis, C. 2008, MNRAS 383, L45 Fr08b = Froebrich, D., Meusinger, H., and Scholz, A. 2008, MNRAS 390, 1598 Or09 = Ortolani, S., Bonatto, C., Bica, E., and Barbuy, B. 2009, AJ 138, 889 Sa06 = Sakamoto, T., and Hasegawa, T. 2006, ApJ 653, L29 Wi05 = Willman, B. et al. 2005, AJ 129, 2692 _______________________________________________________________________ CLUSTER COORDINATES The adopted list of coordinates has undergone a major revision for this edition of the Catalog, thanks to numerous papers over the past decade that provide distinct improvements. At present the center coordinates for the clusters are now uncertain to typically 1-2 arcseconds, and better than 1" in a few cases that have attracted especially intensive study. The working definition of the "cluster center" that I use here is the center of the overall light distribution, as defined for example by concentric-aperture photometry, ellipse contour fitting, or light profile fitting. In a few special cases now in the literature alternate definitions have arisen, such as the "center of gravity" from starcounts or the point around which the velocity dispersion would be maximized at zero radius. At the level of 1" or so, these different definitions may disagree. Here is the current list of 157 clusters, along with the literature source for the adopted coordinates of each one (see end of list for key to references): NGC 104 Mc06 NGC 288 Go10 NGC 362 Go10 Whiting 1 Ca05 NGC 1261 Go10 Pal 1 Go10 AM 1 Hi06 Eridanus Dj93 Pal 2 Go10 NGC 1851 Go10 NGC 1904 La07 NGC 2298 Go10 NGC 2419 Ba09 Ko 2 Ko07 Pyxis We95 NGC 2808 Go10 E 3 Go10 Pal 3 Hi06 NGC 3201 Go10 Pal 4 Sh86 Ko 1 Ko07 NGC 4147 Go10 NGC 4372 Sh86 Rup 106 Dj93 NGC 4590 Go10 NGC 4833 Go10 NGC 5024 Go10 NGC 5053 Go10 NGC 5139 An10 NGC 5272 Go10 NGC 5286 Go10 AM 4 Ca09 NGC 5466 Go10 NGC 5634 Sh86 NGC 5694 NG06 IC 4499 Sh86 NGC 5824 NG06 Pal 5 Sh86 NGC 5897 NG06 NGC 5904 Go10 NGC 5927 Go10 NGC 5946 Sh86 BH 176 Ha10 NGC 5986 Go10 Lynga 7 Go10 Pal 14 Hi06 NGC 6093 Go10 NGC 6121 Go10 NGC 6101 Go10 NGC 6144 Sh86 NGC 6139 Sh86 Terzan 3 Te71 NGC 6171 Go10 1636-283 Ha10 NGC 6205 Go10 NGC 6229 Sh86 NGC 6218 Go10 FSR 1735 Fr07 NGC 6235 Sh86 NGC 6254 Go10 NGC 6256 Sh86 Pal 15 Ha10 NGC 6266 Pi95 NGC 6273 Pi95 NGC 6284 NG06 NGC 6287 NG06 NGC 6293 Pi95 NGC 6304 Go10 NGC 6316 Pi95 NGC 6341 Go10 NGC 6325 Sh86 NGC 6333 NG06 NGC 6342 Sh86 NGC 6356 Sh86 NGC 6355 Sh86 NGC 6352 Go10 IC 1257 Ha97 Terzan 2 Pi95 NGC 6366 Go10 Terzan 4 Pi95 HP 1 Dj93 NGC 6362 Go10 Liller 1 Pi95 NGC 6380 Dj93 Terzan 1 Te71 Ton 2 Dj93 NGC 6388 Go10 NGC 6402 Sh86 NGC 6401 Pi95 NGC 6397 Go10 Pal 6 Dj93 NGC 6426 Sh86 Djorg 1 Dj87 Terzan 5 Co02 NGC 6440 Pi95 NGC 6441 Go10 Terzan 6 Te71 NGC 6453 Pi95 UKS 1 Ma80 NGC 6496 Go10 Terzan 9 Dj93 Djorg 2 Dj87 NGC 6517 Sh86 Terzan 10 Te71 NGC 6522 Sh86 NGC 6535 Go10 NGC 6528 NG06 NGC 6539 Sh86 NGC 6540 Dj87 NGC 6544 Sh86 NGC 6541 Go10 2MS-GC01 Hu00 ESO-SC06 Or00 NGC 6553 Be01 2MS-GC02 Hu00 NGC 6558 Pi95 IC 1276 Sh86 Terzan 12 Te71 NGC 6569 Pi95 BH 261 Or06 GLIMPSE02 Ku08 NGC 6584 Go10 NGC 6624 Go10 NGC 6626 NG06 NGC 6638 Pi95 NGC 6637 Go10 NGC 6642 Pi95 NGC 6652 Go10 NGC 6656 Go10 Pal 8 Dj93 NGC 6681 Go10 GLIMPSE01 Ko05 NGC 6712 NG06 NGC 6715 Go10 NGC 6717 Go10 NGC 6723 Go10 NGC 6749 Dj93 NGC 6752 Go10 NGC 6760 Sh86 NGC 6779 Go10 Terzan 7 Go10 Pal 10 Dj93 Arp 2 Go10 NGC 6809 Go10 Terzan 8 Go10 Pal 11 Dj93 NGC 6838 Go10 NGC 6864 Sh86 NGC 6934 Go10 NGC 6981 Go10 NGC 7006 Sh86 NGC 7078 Go10 NGC 7089 Go10 NGC 7099 Go10 Pal 12 Go10 Pal 13 Sh86 NGC 7492 Sh86 Sources: An10 = Anderson, J., and van der Marel, R. 2010, ApJ, 710, 1032 Ba09 = Baumgardt, H. et al. 2009, MNRAS 396, 2051 Be01 = Beaulieu, S. et al. 2001, AJ 121, 2618 Ca05 = Carraro, G. 2005, ApJ 621, L61 Ca09 = Carraro, G. 2009, AJ 137, 3809 Co02 = Cohn, H.N., Lugger, P.M., Grindlay, J.E., and Edmonds, P.D. 2002, ApJ 571, 818 Dj87 = Djorgovski, S. 1987, ApJ 317, L13 Dj93 = Djorgovski, S., and Meylan, G. 1993, in Structure and Dynamics of Globular Clusters, ASP Conf.Ser. 50, p.325 Fr07 = Froebrich, D., Meusinger, H., and Scholz, A. 2007, MNRAS 377, L54 Go10 = Goldsbury, R., Richer, H.B., Anderson, J., Dotter, A., Sarajedini, A., and Woodley, K. 2010, AJ 140, 1830 Ha97 = Harris, W.E. et al. 1997, AJ 113, 688 Ha10 = Harris, W.E. 2010, measured from DSS R image Hi06 = Hilker, M. 2006, AAp 448, 171 Hu00 = Hurt, R.L. et al. 2000, AJ 120, 1867 Ko05 = Kobulnicky, H.A. et al. 2005, AJ 129, 239 Ko07 = Koposov, S. et al. 2007, ApJ 669, 337 Ku08 = Kurtev, R., Ivanov, V., Borissova, J., and Ortolani, S. 2008, AAp 489, 583 La07 = Lanzoni, B. et al. 2007, ApJ, 663, 1040 Ma80 = Malkan, M., Kleinmann, D.E., and Apt, J. 1980, ApJ 237, 432 Mc06 = McLaughlin, D.E. et al. 2006, ApJS 166, 249 NG06 = Noyola, E., and Gebhardt, K. 2006, AJ 132, 447 Or00 = Ortolani, S., Bica, E., and Barbuy, B. 2000, AAp 361, L57 Or06 = Ortolani, S., Bica, E., and Barbuy, B. 2006, ApJ 646, L115 Pi95 = Picard, A., and Johnston, H.M. 1995, AApS 112, 89 Sh86 = Shawl, S.J., and White, R.E. 1986, AJ 91, 312 Te71 = Terzan, A. 1971, AAp 15, 336 We95 = Weinberger, R. 1995, PASP 107, 58 ___________________________________________________________________ FOREGROUND REDDENING E(B-V) Major 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 in the next section below) were employed whenever they appeared to be well calibrated. These discussions, which employ a wide variety of semi-independent methods, now agree extremely well with other methods 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. I do NOT use reddenings derived from all-sky reddening maps (e.g. Schlegel et al. 1998, ApJ 500, 525; or Burstein and Heiles 1982, AJ 87, 1165). 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). However, even the lowest-reddening cases are not better known than +-0.01 mag. ___________________________________________________________________ DISTANCES: HORIZONTAL-BRANCH MAGNITUDE V_HB The primary distance indicator used here is the mean V magnitude of the horizontal branch, V_HB. In all but a few extreme cases, the HB level is measured directly from a color-magnitude diagram or from the mean magnitude of the RR Lyrae stars. 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. For the 2010 edition, 53 new entries for V_HB levels have been made, but in most cases these are only refinements of previous values; few major changes have occurred. !! IMPORTANT !! Please note that V(HB) here is defined to be the mean magnitude of the HB stars AS DIRECTLY OBSERVED FROM THE COLOR-MAGNITUDE DIAGRAM. It is NOT adjusted to any predicted ZAHB (zero-age horizontal branch) level, which requires bringing in stellar evolution models. If the cluster has few or no RR Lyraes, for blue-HB clusters, V(HB) 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. Several very low-luminosity clusters do not have a large enough number of stars even to populate the HB; that is, even their brightest stars are only subgiant or main-sequence turnoff stars. In those cases, I have used the best-estimate distance modulus as determined from main-sequence fitting to predict the mean magnitude that the HB stars would have if they were present. DISTANCE SCALE: The absolute calibration of V_HB adopted here uses a dependence of absolute V magnitude on metallicity as follows: M_V(HB) = 0.16 [Fe/H] + 0.84 This is a slight change (0.00-0.05 mag fainter depending on metallicity) from previous editions of the Catalog. Readers should be aware that many recent papers discuss the level and slope of the ZAHB as determined from stellar models, rather than the HB as observed. When the HB magnitude is 'corrected' to the unevolved ZAHB, 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. 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. For example, Carney et al. 1992 (ApJ 386, 663) give an empirical correction as Delta(V)(ZAHB - ) = 0.05 [Fe/H] + 0.20 and numerous theory papers can be found giving M_V(ZAHB) relations as a function of [Fe/H]. I do not use any of these. Ultimately, calibrations of M_V(HB) need to rely on distances to Milky Way globular clusters measured more directly in a variety of possible ways. The recent sources used for the calibration quoted above are: (1) Main-sequence fitting to metal-poor field subdwarfs: Bergbusch & Stetson 2009, AJ 138, 1455 (47 Tuc) Gratton 2003, AAp 408, 529 (NGC 6397, NGC 6752, 47 Tuc) Grundahl et al. 2002, AAp 395, 481 (47 Tuc, NCG 6838) Harris 2000, Saas-Fee Lectures (M3) Layden et al. 2005, ApJ 632, 266 (M5) (2) Trigonometric parallax for field RR Lyrae stars: Feast et al. 2008, MNRAS 386, 2115 Gratton 1998, MNRAS 296, 739 (3) Dynamical parallax: McLaughlin et al. 2006, ApJS 166, 249 (47 Tuc) Rees 1996, ASP Conf.Ser. 92, 289 (6 clusters) van de Ven et al. 2006, AAp 445, 513 (omega Centauri) van den Bosch et al. 2006, ApJ 641, 852 (M15) (4) Eclipsing binary solution: Thompson et al. 2001, AJ 121, 3089 (omega Centauri) Thompson et al. 2010, AJ 139, 357 (47 Tuc) (5) RR Lyraes (Fourier analysis of light curves or Baade-Wesselink): Arellano Ferro et al. 2010, MNRAS 402, 226 (NGC 5053) Cacciari et al. 2005, AJ 129, 267 (M2) Dekany & Kovacs 2009, AAp 507, 803 (NGC 5024) Olech et al. 2001, MNRASS 321, 421 (NGC 6362) Zorotovic et al. 2010, AJ 139, 357 (NGC 5286) (6) HB levels in M31 globular clusters (in this case an intrinsic distance modulus (m-M)_0 = 24.47 is assumed for M31): Rich et al. 2005, AJ 129, 2670 present homogenous HST photometry and metallicities for 19 clusters. An unweighted fit of the M_V(HB) values versus metallicity, including all the Milky Way and M31 data above, gives M_V(HB) = (0.179 +- 0.036) [Fe/H] + (0.873 +- 0.054) (n=39) A weighted fit using the uncertainties quoted in the papers above gives M_V(HB) = (0.160 +- 0.033) [Fe/H] + (0.844 +- 0.049) (n=39) A weighted fit for ONLY the Milky Way clusters (not including M31) gives M_V(HB) = (0.165 +- 0.045) [Fe/H] + (0.863 +- 0.071) (n=23) These all show excellent internal agreement. The rms scatter around the best-fit relation is +-0.11 mag in M_V. The absolute uncertainty of M_V(HB) for even the best cases is probably +-0.1 mag, even if the apparent magnitude V_HB is much more precisely known. There may in fact be no "single" HB luminosity calibration that can be applied universally, since mixtures of ages, mass loss rates, etc. among the clusters will produce slight differences in the HB luminosity even if other parameters (such as metallicity) are equal (see Demarque et al. 2000, AJ 19, 1398). 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 Distances to 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 Bellazzini M., Fusi Pecci F., Ferraro F.R., Galleti S., Catelan M., and Landsman W.B. 2001, AJ 122, 2569 NGC 362 Bellazzini M., Fusi Pecci F., Ferraro F.R., Galleti S., Catelan M., and Landsman W.B. 2001, AJ 122, 2569 Whiting 1 Carraro, G., Zinn, R., and Moni Bidin, C. 2007, AAp 466, 181 NGC 1261 Ferraro F.R., Clementini G., Fusi Pecci F., Vitiello E., and Buonanno R. 1993, MNRAS 264, 273 Pal 1 Sarajedini, A. et al. 2007, AJ 133, 1658 AM 1 Dotter, A., Sarajedini, A., and Yang, S-C. 2008, AJ 136, 1407 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 Sarajedini, A. et al. 2007, AJ 133, 1658 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 Ripepi, V. et al. 2007, ApJ 667, L61 Koposov 2 Koposov, S. et al. 2007, ApJ 669, 337 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 Walker A.R. 1999, AJ 118, 432 E 3 Sarajedini, A. et al. 2007, AJ 133, 1658 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 Layden, A.C., and Sarajedini, A. 2003, AJ 125, 208 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 Koposov 1 Koposov, S. et al. 2007, ApJ 669, 337 NGC 4147 Stetson, P.B., Catelan, M., and Smith, H.A. 2005, PASP 117, 1325 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 Melbourne J., Sarajedini A., Layden A., and Martins D.H. 2000, AJ 120, 3127 NGC 5024 Kopacki G. 2000, AAp 358, 547 NGC 5053 Arellano Ferro, A., Giridhar, S., and Bramich, D. M. 2010, MNRAS 402, 226 NGC 5139 Weldrake, D.T.F., Sackett, P.D., and Bridges, T.J. 2007, AJ 133, 1447 (RR Lyraes) NGC 5272 Cacciari, C., Corwin, T.M., and Carney, B.W. 2005, AJ 129, 267 (RR Lyraes) NGC 5286 Zorotovic, M. et al. 2010, AJ 139, 357 (RR Lyraes) AM 4 Carraro, G. 2009, AJ 137, 3809 NGC 5466 Fekadu, N., Sandquist, E.L., and Bolte, M. 2007, ApJ 663, 277 NGC 5634 Bellazzini M., Ferraro F.R., and Ibata R. 2002, AJ 124, 915 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 Clement C.M., and Rowe J.F. 2001, AJ 122, 1464 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, 347, 455 (The mean HB level is used here, not their differentially dereddened one, along with their mean reddening) NGC 5946 Piotto G. et al. 2002, AAp 391, 945 BH 176 Phelps, R., and Schick, M. 2003, AJ 126, 265 NGC 5986 Alves, D.R., Bond, H.E., and Onken C. 2001, AJ 121, 318 Lynga 7 Sarajedini, A. et al. 2007, AJ 133, 1658 Pal 14 Dotter, A., Sarajedini, A., and Yang, S-C. 2008, AJ 136, 1407 NGC 6093 Brocato, E., Castellani, V., Scotti, G.A., Saviane, I., Piotto, G., and 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 Sarajedini, A. et al. 2007, AJ 133, 1658 NGC 6139 Zinn, R., and Barnes, S. 1998, AJ, 116, 1736 Terzan 3 Valenti, E., Ferraro, F. R., and Origlia, L. 2007, AJ 133, 1287 NGC 6171 Cudworth K.M., Smetanka J.J., and Majewski S.R., 1992, AJ 103, 1252 ESO452-SC11 Cornish, A.S.M. et al. 2006, AJ 131, 2543 NGC 6205 Sandquist, E.L. et al. 2010, AJ 139, 2374 NGC 6218 Brocato, E., Buonanno, R., Malakhova, Y., and Piersimoni, A.M. 1996, AAp, 311, 778 FSR 1735 Froebrich, D., Meusinger, H., and Scholz, A. 2007, MNRAS 377, L54 NGC 6229 Borissova, J., Catelan, M., andValchev T. 2001, MNRAS 324, 77 NGC 6235 Howland, R. et al. 2003, AJ 125, 801 (RR Lyraes) NGC 6254 Hurley D.J.C., Richer H.B., and Fahlman G.G., 1989, AJ 98, 2124 NGC 6256 Valenti, E., Ferraro, F. R., and Origlia, L. 2007, AJ 133, 1287 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 Valenti, E., Ferraro, F. R., and Origlia, L. 2007, AJ 133, 1287 NGC 6284 Piotto G. 2002, AAp 391, 945 NGC 6287 Piotto G. 2002, AAp 391, 945 NGC 6293 Janes K.A., and Heasley J.N., 1991, AJ 101, 2097 NGC 6304 Ortolani S., Momany Y., Bica E., and Barbuy B. 2000, AAp 357, 495 NGC 6316 Valenti, E., Ferraro, F. R., and Origlia, L. 2007, AJ 133, 1287 NGC 6325 Ortolani, S., Bica, E., and Barbuy, B. 2003, AAp 402, 565 NGC 6341 Carney B.W., Storm J., Trammell S.R., and Jones R.V., 1992, PASP 104, 44 NGC 6333 Clement C.M., and Shelton I. 1999, AJ 118, 453 NGC 6342 Heitsch, F., & Richtler, T. 1999, AAp, 347, 455 (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 Ortolani, S., Bica, E., and Barbuy, B. 2003, AAp 402, 565 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 Valenti, E., Ferraro, F. R., and Origlia, L. 2010. MNRAS 402, 1729 NGC 6366 Harris H.C., 1993, AJ 106, 604 Terzan 4 Valenti, E., Ferraro, F. R., and Origlia, L. 2010. MNRAS 402, 1729 NGC 6362 Olech A., Kaluzny J., Thompson E.B., Pych W., Krzeminski W., and Schwarzenberg-Czerny A. 2001, MNRAS 321, 421 HP 1 Barbuy, B. et al. 2006, AAp 449, 349 Liller 1 Valenti, E., Ferraro, F. R., and Origlia, L. 2010. MNRAS 402, 1729 NGC 6380 Ortolani, S., Bica, E., and Barbuy, B. 1998, AApS, 127, 471 Terzan 1 Valenti, E., Ferraro, F. R., and Origlia, L. 2010. MNRAS 402, 1729 Ton 2 Bica, E., Ortolani, S., and Barbuy, B. 1996, AApSuppl, 120, 153 NGC 6388 Pritzl B.J., Smith H.A., Catelan M., and Sweigart A.V. 2002, AJ 124, 949 NGC 6402 Piotto G. et al. 2002, AAp 391, 945 NGC 6401 Barbuy B., Ortolani S., Bica E., and Desidera S. 1999, AAp 348, 783 NGC 6397 Alcaino G., Buonanno R., Caloi V., Castellani V., Corsi C.E., Iannicolo G., and Liller W., 1987, AJ 94, 917 Pal 6 Lee J-W., Carney B.W. 2002, AJ 123, 3305 NGC 6426 Papadakis I., Hatzidimitriou D., Croke B.F.W., and Papamastorakis I. 2000, AJ 119, 851 Djorg 1 Valenti, E., Ferraro, F. R., and Origlia, L. 2010. MNRAS 402, 1729 Terzan 5 Valenti, E., Ferraro, F. R., and Origlia, L. 2007, AJ 133, 1287 NGC 6440 Ortolani, S., Barbuy, B., and Bica, E. 1994, AApSuppl 108, 653 NGC 6441 Pritzl B.J., Smith H.A., Catelan M., and Sweigart A.V. 2001, AJ 122, 2600 Terzan 6 Valenti, E., Ferraro, F. R., and Origlia, L. 2007, AJ 133, 1287 NGC 6453 Valenti, E., Ferraro, F. R., and Origlia, L. 2010. MNRAS 402, 1729 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 Valenti, E., Ferraro, F. R., and Origlia, L. 2010. MNRAS 402, 1729 Djorg 2 Valenti, E., Ferraro, F. R., and Origlia, L. 2010. MNRAS 402, 1729 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., and Sadler, E.M. 19989, AJ, 115, 1476 NGC 6535 Testa V., Corsi C.E., Iannicola G., Marconi G., Piersimoni A.M., and Buonanno R. 2001, AJ 121, 916 NGC 6528 Feltzing S., Johnson R.A. 2002, AAp 385, 67 (The mean HB level here is corrected for differential reddening and should be used in combination with their fiducial mean reddening of E(B-V)=0.54) NGC 6539 Armandroff T.E., 1988, AJ 96, 588 NGC 6540 Valenti, E., Ferraro, F. R., and Origlia, L. 2010, MNRAS 402, 1729 NGC 6544 Valenti, E., Ferraro, F. R., and Origlia, L. 2010, MNRAS 402, 1729 NGC 6541 Lee, J-W., and Carney, B.W. 2006, AJ 132, 2171 2MASS-GC01 Ivanov V.D., Borissova J., and Vanzi L. 2000, AAp 362, L1 ESO280-SC06 Ortolani S., Bica E., and Barbuy B. 2000, AAp 361, L57 NGC 6553 Zoccali M., Renzini A., Ortolani S., Bica E., and Barbuy B. 2001, AJ 121, 2638 (The mean HB level is corected for differential reddening and should be used in combination with their fiducial reddening of E(B-V)=0.63) 2MASS-GC02 Borissova, J. et al. 2007, AAp 474, 121 NGC 6558 Rich, R.M., Ortolani, S., Bica, E., and Barbuy, B. 1998, AJ, 116, 1295 IC 1276 Barbuy, B., Ortolani, S., and Bica, E. 1998, AApS, 132, 333 Terzan 12 Ortolani, S., Bica, E., and Barbuy, B. 1998, AApS, 127, 471 NGC 6569 Ortolani, S., Bica, E., and Barbuy B. 2001, AAp 374, 564 BH 261 Ortolani, S., Bica, E., and Barbuy, B. 2006, ApJ 646, L115 GLIMPSE 2 Kurtev, R., Ivanov, V. D., Borissova, J., and Ortolani, S. 2008, AAp 489, 583 NGC 6584 Sarajedini A., and Forrester, W.L. 1995, AJ 109, 1112 NGC 6624 Heasley J.N., Janes K.A., Zinn R., Demarque P., Da Costa G.S., and Christian C.A. 2000, AJ 120, 879 NGC 6626 Testa V., Corsi C.E., Iannicola G., Marconi G., Piersimoni A.M., and Buonanno R. 2001, AJ 121, 916 NGC 6638 Piotto G. et al. 2002, AAp 391, 945 NGC 6637 Heasley J.N., Janes K.A., Zinn R., Demarque P., Da Costa G.S., and Christian C.A. 2000, AJ 120, 879 NGC 6642 Piotto G. et al. 2002, AAp 391, 945 NGC 6652 Chaboyer B., Sarajedini A., and Armandroff T.E. 2000, AJ 120, 3102 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 GLIMPSE 1 Ivanov, V. D., Kurtev, R., and Borissova, J. 2005, AAp 442, 195 NGC 6712 Cudworth K.M., 1988, AJ 96, 105 NGC 6715 Sollima, A., Cacciari, C., Bellazzini, M., and Colucci, S. 2010, MNRAS 406, 329 (RR Lyraes) NGC 6717 Ortolani S., Barbuy, B., and Bica E. 1999, AApS 136, 237 NGC 6723 Alcaino G., Liller W., Alvarado F., Mironov A., Ipataov A., Piskunov A., Samus N., and 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, 347, 455 (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 Sarajedini, A. et al. 2007, AJ 133, 1658 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 Lewis, M.S., Liu, W.M., Paust, N.E.Q., and Chaboyer, B. 2006, AJ 131, 2538 NGC 6838 Geffert M., and Mainz G. 2000, AApS 144, 227 NGC 6864 Catelan M., Borissova J., Ferraro F.R., Corwin T.M., Smith H.A., Kurtev R. 2002, AJ 124, 364 NGC 6934 Kaluzny J., Olech A., and Stanek K.Z. 2001, AJ 121, 1533 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 Siegel M.H., Majewski S.R., Cudworth K.M., and Takamiya M. 2001, AJ 121, 935 NGC 7492 Cote P., Richer H.B., and Fahlman G.G., 1991, AJ 102, 1358 INTEGRATED VISUAL MAGNITUDE V_t All data from the sources below are used, with the exception of the clusters specifically mentioned (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. Sources: Bellazzini, M. et al. 2007, ApJ 667, L61 [NGC 2419] Bonatto, C., and Bica, E. 2008, AAp 479, 741 [Lynga 7, ESO280-SC06, 2MASS-GC01, 2MASS-GC02, GLIMPSE-C01] Carraro, G. 2009, AJ 137, 3809 [AM-4] Carraro, G., Zinn, R., and Moni Bidin, C. 2007, AAp 466, 181 [Whiting 1] Froebrich, D., Meusinger, H., and Scholz, A. 2007, MNRAS 377, L54 [FSR 1735] Kobulnicky, H.A. et al. 2005, AJ 129, 239 [GLIMPSE-C01] Koposov, S. et al. 2007, ApJ 669, 337 [Ko 1,2] 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] Ortolani, S., Bica, E., and Barbuy, B. 2006, ApJ 646, L115 [BH 261] 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] 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 METALLICITIES: [Fe/H] VALUES The heavy-element abundance scale adopted here is the one established by Carretta et al. 2009 (AAp 508, 695). This represents a fundamental shift from the older Zinn and West (1984) metallicity scale used in previous editions of the catalog and by most other writers before the past decade. The arguments for making this change of base are well detailed by Carretta et al. (2009 and earlier papers), but essentially reduce to the fact that the traditional Zinn/West scale was calibrated against only a handful of high-dispersion spectroscopic [Fe/H] values available at that time. In the subsequent 30+ years, far more high-dispersion, high signal-to-noise spectroscopic measures for vastly more clusters have been produced, along with superior abundance analysis methods based on more advanced model atmospheres. Carretta et al. (2009) publish mean [Fe/H] values for 95 clusters derived from a weighted average of (a) their own high-dispersion spectra in that paper and in earlier papers from their group, (b) the Kraft & Ivans 2003 (PASP 115, 143) spectroscopic metallicities transformed to their [Fe/H] scale, (c) the Zinn & West 1984 (ApJS 55, 45) Q39 photometric metallicity index transformed to their [Fe/H] scale, and (d) the Rutledge et al. 1997 (PASP 109, 907) W' calcium index transformed to their [Fe/H] scale. These 95 transformed and averaged values (the ones labelled as "Note 1" in their Table A.1) are used as the homogenous, modern basis for the present catalog listing. Carretta et al. 2009 also supply a suitable transformation for the Zinn/West [Fe/H] values into their new [Fe/H] scale. This transformation (the nonlinear quadratic version) is used to convert the list of values for 27 clusters from Armandroff & Zinn 1988 (AJ 96, 92), another major source of metallicity information. In addition to the major lists referred to above, spectroscopic values of [Fe/H] for many individual clusters are averaged in from all other studies not already included in the sources listed above. These other sources from the literature are listed below. Lastly, metallicities based on photometry (rather than spectroscopy) are used for several clusters in which no other estimates can be found. These are mostly the clusters in the Galactic center region that are very heavily reddened are where every kind of observation is difficult. The photometric metallicities are constructed from recent color-magnitude analyses (for which see the papers listed earlier) and use parameters such as the slope and color of the red-giant branch in various optical and near-infrared bandpasses. In constructing the mean metallicity for each cluster, the Carretta et al. 2009 values are given triple weight because they are already an average of up to four different measurements. All other entries are given unit weight. Major Sources: Carretta, E., Bragaglia, A., Gratton, R., D'Orazi, V., and Lucatello, S. 2009, AAp 508, 695 [95 clusters] Armandroff, T.E., and Zinn, R. 1988, AJ 96, 92 [27 clusters] transformed to the C2009 scale. Additional Sources for Spectroscopic Metallicities: Alves-Brito, A. et al. 2005, AAp 435, 657 [NGC 104] Alves-Brito, A. et al. 2006, AAp 460, 269 [NGC 6553] 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] Armosky, B.J., Sneden, C., Langer, G.E., and Kraft, R.P. 1994, AJ 108, 1364 [NGC 6341, 7078] Barbuy, B., Castro, S., Ortolani, S., and Bica, E. 1992, AAp 259, 607 [NGC 6553] Barbuy, B., et al. 2006, AAp 449, 349 [HP-1] Barbuy, B., et al. 2007, AJ 134, 1613 [NGC 6558] Barbuy, B., et al. 2009, AAp 507, 405 [NGC 6522] Beers, T.C., Preston, G.W., Shectman, S.A., and Kage, J.A. 1990, AJ, 100, 849 [NGC 3201,6121,6341,6397,6752] Bellazzini, M. et al. 2008, AJ 136, 1147 [NGC 6715] Boesgaard, A.M. et al. 2005, ApJ 629, 832 [NGC 6838] Borissova, J. et al. 2007, AAp 474, 121 [2MASS-GC02] 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] Brown, J.A., Wallerstein, G., and Gonzalez, G. 1999, AJ 118, 1245 [NGC 6715] Cannon, R. 1996, quoted in Walker, A.R., and Nemec, J.M 1996, AJ, 112, 2026 [IC 4499] Carraro, G., Zinn, R., and Moni Bidin, C. 2007, AAp 466, 181 [Whiting 1] Carretta, E. et al. 2010a, ApJ 714, L7 [NGC 6715] Carretta, E. et al. 2010b, ApJ 722, L1 [NGC 1851] Castilho, B.V., Pasquini, L., Allen, D.M., Barbuy, B., and Molaro, P. 2000, AAp, 361, 92 [NGC 6397] Cavallo, R.M., Suntzeff, N.B., and Pilachowski, C.A. 2004, AJ 127, 3411 [NGC 6093, 6752] Clementini, G. et al. 2005, ApJ 630, L145 [NGC 6441] Costar, D., and Smith, H.A. 1988, AJ 96, 1925 [NGC 104,6838] Cohen, J.G., and Melendez, J. 2005, AJ 129, 303 [NGC 5272, 6205] Cohen, J.G., and Melendez, J. 2005, AJ 129, 1607 [NGC 7492] Cote, P. 1999, AJ 118, 406 [NGC 6540, IC 1276, Terzan 3] Cote, P., Djorgovski, S.G., Meylan, G., Castro, S., and McCarthy, J.K. 2002, ApJ, 574, 783 [Pal 13] 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. et al. 2009, ApJ 705, 1481 [NGC 6656] Da Costa, G.S., and Seitzer, P. 1989, AJ 97, 405 [NGC 6366] Davidge, T., Ledlow, M., and Puxley, P. 2004, AJ 128, 300 [NGC 6558] Drake, J.J., Smith, V.V., and Suntzeff, N.B. 1994, ApJ, 430, 610 [NGC 6121] Feltzing, S., Primas, F., and Johnson, R.A. 2009, AAp 493, 913 [NGC 6352] 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] Hankey, W.J., and Cole, A.A. 2010, MNRAS in press [IC 4499] Haynes, S. et al. 2008, PASP 120, 1097 [NGC 6254] Idiart, T.P., Barbuy, B., Perrin, M-N, Ortolani, S., Bica, E., and Renzini, A. 2002, AAp 381, 472 [Ter 1] Ivans, I.I., Kraft, R.P., Sneden, C., Smith, G.H., Rich, R.M., and Shetrone, M. 2001, AJ 122, 1438 [NGC 5904] Ivans, I.I., Sneden, C., Kraft, R.P., Suntzeff, N.B., Smith, V.V., Langer, G.E., and Fulbright, J.P. 1999, AJ 118, 1237 [NGC 6121] Johnson, C.I., and Pilachowski, C.A. 2006, AJ 132, 2346 [NGC 6218] Johnson, C.I. et al. 2009, ApJ 698, 2048 [NGC 5139] Kirby, E.N., Guhathakurta, P., and Sneden, C. 2008, ApJ 682, 1217 [NGC 1904, 2419, 6205, 6838, 7006, 7078, 7492] Koch, A., and Cote, P. 2010, AAp 517, 59 [Pal 4] Koch, A., Cote, P., and McWilliam, A. 2009, AAp 506, 729 [Pal 3] Koch, A., and McWilliam, A. 2008, AJ 135, 1551 [NGC 104] Koch, A., and McWilliam, A. 2010, AJ 139, 2289 [NGC 5904] 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] Kurtev, R. et al. 2008, AAp 489, 583 [GLIMPSE-02] Lee, J-W., and Carney, B.W. 2002, AJ 124, 1511 [NGC 6287, 6293, 6541] Lee, J.-W., Carney, B.W., and Balachandran, S.C. 2004, AJ 128, 2388 [Pal 6] Lee, J.-W., Carney, B.W., and Habgood, M.J. 2005, AJ 129, 351 [NGC 4590] Lee, J.-W., Lapez-Morales, M., and Carney, B.W. 2006, ApJ 646, L119 [NGC 5694] 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] Lind, K. et al. 2009, AAp 503, 545 [NGC 6397] Marino, A.F. et al. 2008, AAp 490, 625 [NGC 6121] Marino, A.F. et al. 2009, AAp 505, 1099 [NGC 6656] McCarthy, J.K., and Nemec, J.M. 1997, ApJ 482, 203 [NGC 5466] McWilliam, A., Geisler, D., and Rich, R.M. 1992, PASP 104, 1193 [NGC 2298] McWilliam, A., and Bernstein, R.A. 2008, ApJ 684, 326 [NGC 104] Melendez, J. et al. 2003, AAp 411, 417 [NGC 6553] Minniti, D. 1995, A&A 303, 468 [NGC 6121, 6325, 6356, 6401, 6440, 6517, 6642, 6656] 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] Mottini, M., Wallerstein, G., and McWilliam, A. 2008, AJ 136, 614 [Arp 2, Ter 8] Origlia, L., and Rich, R.M. 2004, AJ 127, 3422 [Ter 4, 5] Origlia, L., Valenti, E., and Rich, R.M. 2005, MNRAS 363, 1276 [NGC 6342, 6528] Origlia, L., Valenti, E., and Rich, R.M. 2008, MNRAS 388, 1419 [NGC 6440, 6441] Origlia, L. et al. 2005, MNRAS 363, 897 [NGC 6539, UKS-1] Palma, C., Kunkel, W., and Majewski, S.R. 2000, PASP 112, 1305 [Pyxis] 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] Pilachowski, C.A. et al. 2003, AJ 125, 794 [NGC 5272] Preston, G.W. et al. 2006, AJ 132, 85 [NGC 7078] Ramirez, S.V., and Cohen, J.G. 2003, AJ 125, 224 [NGC 5904, 6838] Ramirez, S.V., Cohen, J.G., Buss, J., and Briley, M.M. 2001, AJ 122, 1429 [NGC 6838] Rosenberg, A., Piotto, G., Saviane, I., Aparicio, A., and Gratton, R. 1998, AJ, 115, 658 [Pal 1] Sbordone, L. et al. 2005, AAp 437, 905 [Ter 7] Searle, L., and Zinn, R. 1978, ApJ 225, 357 [NGC 5024, 5466, 6171, 6229, 6779, 6934] The [Fe/H] values from their Table 2 are converted directly to the contemporary C2009 scale by a quadratic fit using 13 overlapping clusters. Shetrone, M.D. 1996, AJ, 112, 1517 [NGC 5904,6205,6341,6838] Smith, G.H., Sneden, C., and Kraft, R.P. 2002, AJ 123, 1502 [Pal 5] 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] Sobeck, J.S. et al. 2006, AJ 131, 2949 [NGC 6528] Stephens, A.W., and Frogel, J.A. 2004, AJ 127, 925 [NGC 6256, 6539, HP-1, Liller 1, Pal 6, Ter 2, Ter 4] 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. 1986, AJ 90, 1481 [AM-1] Takeda, Y. et al. 2009, PASJ 61, 563 [NGC 6121, 6205, 7078] Tautviesiene, G. et al. 2004, AJ 127, 373 [Ter 7] Tavarez, M, and Friel, E.D. 1995, AJ 110, 223 [Lynga 7] Villanova, S., Geisler, D., and Piotto, G. 2010, ApJ 722, L18 [NGC 1851] Villanova, S. et al. 2010, NewAst 15, 520 [NGC 5139] Wachter, S., Wallerstein, G., Brown, J.A., & Oke, J.B. 1998, PASP, 110, 821 [NGC 6229, 7006] Wallerstein, G., Kovtyukh, V.V., and Anrievsky, S.M. 2007, AJ 133, 1373 [NGC 6388] Worley, C.C., and Cottrell, P.L. 2010, MNRAS 406, 2504 [NGC 362, 6388] Wylie, E.C. et al. 2006, ApJ 649, 248 [NGC 104] Yong, D., and Grundahl, F. 2008, ApJ 672, L29 [NGC 1851] Yong, D. et al. 2008a, ApJ 684, 11159 [NGC 6752] Yong, D. et al. 2008b, ApJ 689, 1020 [NGC 6712] Yong, D. et al. 2008c, ApJ 689, 1031 [NGC 5904, 6121] Yong, D. et al. 2009, ApJ 695, L62 [NGC 1851] Yong, D. et al. 2010, in preparation [NGC 5466] Zinn, R., and West, M.J. 1984, ApJS 55, 45 [NGC 5634, 6139, 6284, 6287, 6333, 6402, 6426, 6584, IC4499 Transformed to the C2009 [Fe/H] scale with the quadratic equation given by Carretta et al. Zoccali, M. et al. 2004, AAp 423, 507 [NGC 6528] Additional sources based on photometric indicators (including color-magnitude diagrams and isochrone fitting): Bellazzini M., Ferraro F.R., and Ibata R. 2002, AJ 124, 915 [NGC 5634] Bica, E., Ortolani, S., and Barbuy, B. 1996, AApSuppl, 120, 153 [Ton 2] Bica, E., Ortolani, S., and Barbuy, B. 1999, AApS 136, 363 [ESO452-SC11] Carraro, G. 2009, AJ 137, 3809 [AM4] Harris, W.E. et al. 1997, AJ, 113, 688 [IC 1257] Hatzidimitriou, D. et al. 1999, AJ 117, 3059 [NGC 6426] Howland, R. et al. 2003, AJ 125, 801 [NGC 6235] Irwin, M.J., Demers, S., and Kunkel, W.E. 1995, ApJ 453, L21 [Pyxis] Kaisler, D., Harris, W.E., and McLaughlin, D.E. 1997, PASP, 109, 920 [NGC 6749, Pal 10] Kaluzny, J., Olech, A., and Stanek, K.Z. 2001, AJ 121, 1533 [NGC 6934] Ortolani, S., Bica, E., and Barbuy, B. 1997, AApS 126, 319 [Ter 10, UKS1] Ortolani, S., Bica, E., and Barbuy, B. 1998, AApS 127, 471 [NGC 6380, Ter 12] Ortolani S., Bica E., and Barbuy B. 2000, AAp 361, L57 [ESO280-SC06] Ortolani, S., Bica, E., and Barbuy, B. 2006, ApJ 646, L115 [BH 261] Papadakis I., Hatzidimitriou D., Croke B.F.W., and Papamastorakis I. 2000, AJ 119, 851 [NGC 6426] Phelps, R., and Schick, M. 2003, AJ 126, 265 [BH 176] Sarajedini, A. 2004, AJ 128, 1228 [Lynga 7] Sarajedini, A., and Geisler, D. 1996, AJ, 112, 2013 [Pyxis] Sarajedini, A. et al. 2007, AJ 133, 1658 [NGC 6779, Pal 1, 2, E3, Lynga 7] Valenti, E., Ferraro, F.R., and Origlia, L. 2007, AJ 133, 1287 [NGC 6256, 6273, 6293, 6316, 6355, 6401, 6642, Ter 3, 5, 6] Valenti, E., Ferraro, F.R., and Origlia, L. 2010, MNRAS 402, 1729 [NGC 6540, 6544, 6453, Ter 1, 2, 4, 9, HP-1, Liller 1, Dj1, Dj2] Valenti, E., Origlia, L., and Ferraro, F.R. 2005, MNRAS 361, 272 [NGC 6304, 6569] Zinn, R. 1985, ApJ 293, 424 [AM-1, NGC 6284, 6333, 6380, 6584, Liller 1, Pal 13] Since these are all approximate values they have not been artificially converted to the C2009 scale. Zinn, R., and Barnes, S. 1998, AJ, 116, 1736 [NGC 6139] Zorotovic, M. et al. 2010, AJ 139, 357 [NGC 5286] Here are the bibliographic sources listed by cluster. For clusters with no spectroscopic sources given below, the catalog metallicity relies only on photometric indicators that are given in the separate list above. Abbreviations follow the code: Car09 = Carretta et al. 2009 W&&98 = Wachter et al. 1998 TF95 = Tavarez and Friel 1995, etc. NGC 104 Car09, AZ88, BW92, A&&05, W&&06, MB08, KM08 NGC 288 Car09, CD88, G87 NGC 362 Car09, AZ88, CD88, G87, WC10 Whiting1 CZM07 NGC 1261 Car09 Pal 1 R&&98 AM 1 SOS85 Eridanus Car09, AD91 Pal 2 NGC 1851 Car09, AZ88, GCM97, YG08, Y&&09, VGP10, C&&10b NGC 1904 Car09, F91, GCM97 NGC 2298 Car09, MGR92 NGC 2419 SKK88 Ko 2 Pyxis PKM00 NGC 2808 Car09, GCM97 E 3 Pal 3 Car09, ADZ92, KCM09 NGC 3201 Car09, B&&90, GCM97 Pal 4 Car09, ADZ92, KC10 Ko 1 NGC 4147 Car09, SKK88 NGC 4372 Car09 Rup 106 Car09, BWZ97, DAN92, F&&97 NGC 4590 Car09, M&&93, LCH05 NGC 4833 Car09, M&&93 NGC 5024 SKK88, SZ78 NGC 5053 Car09, G&&95, SKK88 NGC 5139 PN89, SK96, J&&09, V&&10 NGC 5272 Car09, K&&92, A&&94, P&&03, CM05a NGC 5286 Car09 AM 4 NGC 5466 SZ78, MN97, Y&&10 NGC 5634 ZW84 NGC 5694 Car09, AZ88, LLC06 IC 4499 C96, ZW84, HC10 NGC 5824 Car09, AZ88 Pal 5 GCM97, SSK02 NGC 5897 Car09, NGC 5904 Car09, I&&01, S96, S&&92, RC03, Y&&08c NGC 5927 Car09, AZ88, F91 NGC 5946 Car09, AZ88 BH 176 NGC 5986 Car09, GCM97 Lynga 7 TF95 Pal 14 Car09, ADZ92 NGC 6093 Car09, AZ88, GCM97, CSP04 NGC 6121 Car09, B&&90, BW92, DSS94, I&&99, M95a, Y&&08c, M&&08, T&&09 NGC 6101 Car09 NGC 6144 Car09, M&&93 NGC 6139 ZW84 Terzan 3 C99 NGC 6171 Car09, SZ78 1636-283 NGC 6205 Car09, K&&92, K&&93, K&&97, LBC91, PA96, S96, A&&94, CM05a, T&&09 NGC 6229 W&&98, SZ78 NGC 6218 Car09, DA95, JP06 FSR 1735 NGC 6235 Car09 NGC 6254 Car09, K&&95, H&&08 NGC 6256 SF04 Pal 15 Car09, DA95 NGC 6266 Car09 NGC 6273 Car09 NGC 6284 ZW84 NGC 6287 ZW84 NGC 6293 Car09 NGC 6304 Car09 NGC 6316 Car09, AZ88 NGC 6341 Car09, A&&94, B&&90, PKC90, S96, S&&91 NGC 6325 Car09, M95a NGC 6333 ZW84 NGC 6342 Car09, AZ88, OVR05 NGC 6356 Car09, AZ88, M95a NGC 6355 Car09 NGC 6352 Car09, F91, FPJ09 IC 1257 Terzan 2 AZ88, SF04 NGC 6366 Car09, DA95, DS89 Terzan 4 AZ88, SF04 HP 1 AZ88, SF04, B&&06 NGC 6362 Car09, GCM97 Liller 1 AZ88, SF04 NGC 6380 Terzan 1 AZ88, I&&02 Ton 2 NGC 6388 Car09, AZ88, WKA07, WC10 NGC 6402 ZW84 NGC 6401 Car09, M95a NGC 6397 Car09, B&&90, C&&00, M&&93, L&&09 Pal 6 LC02, SF04, LCB04 NGC 6426 ZW84 Djorg 1 Terzan 5 AZ88 NGC 6440 Car09, AZ88, M95a, OVR08 NGC 6441 Car09, AZ88, C&&05, OVR08 Terzan 6 AZ88 NGC 6453 Car09 UKS 1 O&&05 NGC 6496 Car09 Terzan 9 Djorg 2 NGC 6517 Car09, M95a Terzan 10 NGC 6522 Car09, B&&09 NGC 6535 Car09 NGC 6528 Car09, AZ1, Z&&04, OVR05, S&&06 NGC 6539 Car09, SF04, O&&05 NGC 6540 C99 NGC 6544 Car09 NGC 6541 Car09 2M-GC01 ESO-SC06 NGC 6553 Car09, B&&92, M&&03, A&&06 2M-GC02 NGC 6558 Car09, DLP04, B&&07 IC 1276 C99 Terzan 12 NGC 6569 Car09 BH 261 GLIMPSE2 K&&08 NGC 6584 ZW84 NGC 6624 Car09, AZ88 NGC 6626 DA95, M95b NGC 6638 Car09, SS86 NGC 6637 Car09, M95b NGC 6642 Car09, M95a NGC 6652 Car09, AZ88 NGC 6656 Car09, BW92, LBC91, M95a, D&&09, M&&09 Pal 8 Car09 NGC 6681 Car09 GLIMPSE1 NGC 6712 Car09, Y&&08b NGC 6715 Car09, BWG99, DA95, B&&08, C&&10a NGC 6717 Car09 NGC 6723 Car09 NGC 6749 NGC 6752 Car09, B&&90, GCM97, M&&93, CSP04, Y&&08a NGC 6760 Car09 NGC 6779 SZ78 Terzan 7 Car09, DA95, T&&04, S&&05 Pal 10 Arp 2 Car09, DA95, MWM08 NGC 6809 Car09, M&&93 Terzan 8 DA95, MWM08 Pal 11 Car09, ADZ92, DA95 NGC 6838 Car09, CS88, LOW87, R&&01, S96, S&&94, RC03, B&&05 NGC 6864 Car09, SZ78 NGC 6934 NGC 6981 Car09, GCM97 NGC 7006 Car09, K&&98, W&&98 NGC 7078 Car09, AZ88, A&&94, M&&93, S&&91, S&&97, P&&06, T&&09 NGC 7089 Car09, AZ88 NGC 7099 Car09, M&&93 Pal 12 Car09, AD91, BWZ97, DA95 Pal 13 C&&02 NGC 7492 Car09, CM05b RADIAL VELOCITY Most of the radial velocity data come from the four major sources listed below. However, numerous more recent sources are also available, and in most cases these are based on large samples of stars 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 + 8.5 cos b cos l + 13.4 cos b sin l + 6.5 sin b (Coskunoglu et al.2010, MNRAS in press) from RAVE velocity data of 82580 nearby stars. Major Sources: Carretta, E., Bragaglia, A., Gratton, R., and Lucatello, S. 2009, AAp 505, 139 [17 clusters] 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: Alves-Brito, A. et al. 2005, AAp 435, 657 [NGC 104] Alves-Brito, A. et al. 2006, AAp 460, 269 [NGC 6553] 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] Barbuy, B. et al. 2006, AAp 449, 349 [HP-1] Barbuy, B. et al. 2007, AJ 134, 1613 [NGC 6558] Baumgardt, H. et al. 2009, MNRAS 396, 2051 [NGC 2419] Beers, T.C., Preston, G.W., Shectman, S.A., and Kage, J.A. 1990, AJ, 100, 849 [NGC 3201,5272,6121,6341,6397,6752] Bellazzini, M. et al. 2008, AJ 136, 1147 [NGC 6715] Blecha, A., Meylan, G., North, P. and Roger, F. 2004, AAp 419, 533 [Pal 13] Borissova, J. et al. 2007, AAp 474, 121 [2MASS-GC02] Carraro, G., Zinn, R., and Moni Bidin, C. 2007, AAp 466, 181 [Whiting 1] Carretta, E., Cohen, J.G., Gratton, R.G., and Behr, B.B. 2001, AJ 122, 1469 [NGC 6528] Carretta, E. et al. 2003, AAp 410, 143 [NGC 2808] Carretta, E. et al. 2006, AAp 450, 523 [NGC 2808] Carretta, E. et al. 2007, AAp 464, 927 [NGC 6752] Carretta, E. et al. 2007a, AAp 464, 939 [NGC 6218] Carretta, E. et al. 2007b, AAp 464, 967 [NGC 6388] Clementini, G., Merighi, R., Pasquini, L., Cacciari, C., and Gouiffes, C. 1994, MNRAS 267, 83 [NGC 6121] Clementini, G. et al. 2005, ApJ 630, L145 [NGC 6441] Cohen, J.G., Behr, B.B., and Briley, M.M. 2001, AJ 122, 1420 [NGC 6838] Cohen, J.G., & McCarthy, J.K. 1997, AJ, 113, 1353 [NGC 6341] Cohen, J.G., and Melendez, 2005, AJ 129, 303 [NGC 5272, 6205] Cohen, J.G., and Melendez, 2005, AJ 129, 1607 [NGC 7492] Cote, P. 1999, AJ 118, 406 [NGC 6256, 6380, 6540, 6749, IC 1257, 1276, Ter 3, Ter 12, Ton 2, Pal 10, Dj 1] Cote, P., Djorgovski, S.G., Meylan, G., Castro, S., and McCarthy, J.K. 2002, ApJ, 574, 783 [Pal 13] 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] Da Costa, G.S. et al. 2009, ApJ 705, 1481 [NGC 6656] 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] Drukier, G.A. et al. 2007, AJ 133, 1041 [NGC 6341] Dubath, P., and Meylan, G. 1994, AAp, 290, 104 [NGC 7078] Feltzing, S., Primas, F., and Johnson, R.A. 2009, AAp 493, 913 [NGC 6352] 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] Gratton, R. et al. 2005, AAp 440, 901 [NGC 6752] Gratton, R. et al. 2006, AAp 455, 271 [NGC 6441] Gratton, R. et al. 2007, AAp 464, 953 [NGC 6441] 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] Hankey, W.J., and Cole, A.A. 2010, MNRAS in press [IC 4499] Harris, H.C., Nemec, J.M., and Hesser, J.E. 1983, PASP 95, 256 [NGC 6218,6779] Idiart, T.P., Barbuy, B., Perrin, M-N, Ortolani, S., Bica, E., and Renzini, A. 2002, AAp 381, 472 [Ter 1] Ivans, I.I., Sneden, C., Kraft, R.P., Suntzeff, N.B., Smith, V.V., Langer, G.E., and Fulbright, J.P. 1999, AJ 118, 1237 [NGC 6121] Johnson, C.I., and Pilachowski, C.A. 2006, AJ 132, 2346 [NGC 6218] Johnson, C.I. et al. 2008, ApJ 681, 1505 [NGC 5139] Jordi, K. et al. 2009, AJ 137, 4586 [Pal 14] Kraft, R.P., Sneden, C., Smith, G.H., Shetrone, M.D., & Fulbright, J. 1998, AJ, 115, 1500 [NGC 7006] Lane, R.R. et al. 2010, MNRAS 406, 2732 [NGC 104, 288, 4590, 5024, 6121, 6144, 6218, 6656, 6752, 6809, 7099] Lee, J-W., and Carney, B.W. 2002, AJ 123, 3305 [Pal 6] Lee, J-W., and Carney, B.W. 2002, AJ 124, 1511 [NGC 6287, 6293, 6541] Lee, J.-W., Carney, B.W., and Balachandran, S.C. 2004, AJ 128, 2388 [Pal 6] Lee, J.-W., Lapez-Morales, M., and Carney, B.W. 2006, ApJ 646, L119 [NGC 5694] Lin, D.N.C., and Richer, H.B. 1992, ApJ 388, L57 [Rup 106] Lind, K. et al. 2009, AAp 503, 545 [NGC 6397] Lupton, R.H., Gunn, J.E., and Griffin, R.F. 1987, AJ 93, 1114 [NGC 6205] Marino, A.F. et al. 2008, AAp 490, 625 [NGC 6121] Marino, A.F. et al. 2009, AAp 505, 1099 [NGC 6656] Melendez, J., et al. 2003, AAp 411, 417 [NGC 6553] Meszaros, S., Dupree, A.K., and Szalai, T. 2009, AJ 137, 4282 [NGC 6205, 6341] 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] Milone, A.P. et al. 2006, AAp 456, 517 [NGC 6397] 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] Odenkirchen, M., Grebel, E.K., Dehner, W., Rix, H.W., and Cudworth, K.M. 2002, AJ 124, 1497 [Pal 5] 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] Origia, L., and Rich, R.M. 2004, AJ 127, 3422 [Ter 4, Ter 5] Origlia, L., Valenti, E., and Rich, R.M. 2005, MNRAS 356, 1276 [NGC 6342, 6528] Origlia, L., Valenti, E., and Rich, R.M. 2008, MNRAS 388, 1419 [NGC 6440, 6441] Origlia, L. et al. 2005, MNRAS 363, 897 [NGC 6539, UKS-1] Palma, C., Kunkel, W.E., and Majewski, S.R. 2000, PASP 112, 1305 [Pyxis] 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] Preston, G.W. et al. 2006, AJ 132, 85 [NGC 7078] 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] Ramirez, S., and Cohen, J. 2003, AJ 125, 224 [NGC 5904] Rastorguev, A.S., and Samus, N.N. 1991, Sov.Astron.Letters 17, 388 [NGC 5904,6121,6218,6254,6838] Shetrone, M. et al. 2010, AJ 140, 1119 [NGC 5466] Rosenberg, A., Piotto, G., Savianne, I., Aparicio, A., and Zaggia, S.R. 1998, AJ, 115, 658 [Pal 1] Soderberg, A.M., Pilachowski, C.A., Barden, S.C., Willmarth, D., and Sneden, C. 1999, PASP 111, 1233 [NGC 5272, 6205, 6341, 7078] Sollima, A. et al. 2005, ApJ 634, 332 [omega Cen] Sommariva, V. et al. 2009, AAp 493, 947 [NGC 6121] 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] Szekely, P. et al. 2007, AN 328, 879 [NGC 104, 288, 6218, 6809, 7099] 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] van de Ven, G. et al. 2006, AAp 445, 513 [NGC 5139] Villanova, S., Geisler, D., and Piotto, G. 2010, ApJ 722, L18 [NGC 1851] Villanova, S. Piotto, G., and Gratton, R.G. 2009, AAp 499, 755 [NGC 6752] Wallerstein, G., Kovtyukh, V.V., and Andrievsky, S.M. 2007, AJ 133, 1373 [NGC 6388] Yan, L., and Cohen, J.G. 1996, AJ, 112, 1489 [NGC 5053] Yong, D. et al. 2008, ApJ 689, 1020 [NGC 6712] 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, A&&05, Sz&&07, CBGL09, L&&10 NGC 288 W81, R&&97, M95, POA86, PMFH91, PM93, Sz&&07, CBGL09, L&&10 NGC 362 W81, HSM86, ZW84, R&&97, DMM97, FWMC93, M95 Whiting1 CZM07 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, VGP10 NGC 1904 W81, HSM86, DMM97, GPCM95, P85, POA86, PM93, ZCPS92, CBGL09 NGC 2298 W81, HSM86, R&&97, GPCM95 NGC 2419 W81, OPS93, P85, POA86, B&&09 Ko 2 Pyxis PKM00 NGC 2808 W81, HSM86, ZW84, R&&97, G82, C&&03, C&&06, CBGL09 E 3 Pal 3 W81, ADZ92, P85, POA86 NGC 3201 W81, HSM86, R&&97, BPSK90, CWFG95, CBGL09 Pal 4 W81, ADZ92, OPA86, POA86 Ko 1 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, CBGL09, L&&10 NGC 4833 W81, HSM86, ZW84, R&&97, GPCM95 NGC 5024 W81, HSM86, L&&10 NGC 5053 GPCM95, PSO91, YC96 NGC 5139 W81, HSM86, MM86, SK96, S&&05, vdV&&06, J&&08 NGC 5272 W81, HSM86, DMM97, BPSK90, M95, OPA86, POA86, S&&99, CM05a NGC 5286 W81, HSM86, ZW84, R&&97, DMM97 AM 4 NGC 5466 W81, PL86, POA86, PMFH91, PSO91, S&&10 NGC 5634 W81, HSM86, P85 NGC 5694 W81, HSM86, ZW84, DMM97, AZ88, GPCM95, LLC06 IC 4499 HC10 NGC 5824 W81, HSM86, ZW84, DMM97, AZ88 Pal 5 P85, O&&02 NGC 5897 HSM86, R&&97, GPCM95 NGC 5904 W81, HSM86, ZW84, R&&97, DMM97, OPA86, POA86, RS91, S&&93, RC03, CBGL09 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, J&&09 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, I&&99, M&&08, CBGL09, S&&09, L&&10 NGC 6101 HSM86, ZW84, R&&97, GPCM95 NGC 6144 HSM86, ZW84, R&&97, GPCM95, L&&10 NGC 6139 W81, HSM86 Terzan 3 C99 NGC 6171 HSM86, ZW84, R&&97, DS89, P&&94, PMFH87, S&&93, CBGL09 1636-283 NGC 6205 W81, LGG87, S&&99, CM05a, MDS09 NGC 6229 W81 NGC 6218 W81, HSM86, R&&97, HNH83, PMFH87, RS91, S&&93, JP06, C&&07a, Sz&&07, CBGL09, L&&10 FSR 1735 NGC 6235 HSM86, ZW84, R&&97 NGC 6254 W81, HSM86, R&&97, RS91, CBGL09 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, LC02b NGC 6293 W81, HSM86, ZW84, DMM97, LC02b NGC 6304 W81, HSM86, ZW84, R&&97 NGC 6316 HSM86, ZW84 NGC 6341 W81, BPSK90, CM97, S&&99, D&&07, MDS09 NGC 6325 HSM86, ZW84, DMM97 NGC 6333 W81, HSM86 NGC 6342 HSM86, ZW84, DMM97, EVR05 NGC 6356 W81, HSM86, ZW84, AZ88, M95 NGC 6355 HSM86, ZW84 NGC 6352 HSM86, ZW84, R&&97, FPJ09 IC 1257 C99 Terzan 2 AZ88 NGC 6366 R&&97, DA95, DS89, M95 Terzan 4 AZ88, OR04 HP 1 AZ88, B&&06 NGC 6362 W81, HSM86, ZW84, R&&97, PM93 Liller 1 AZ88 NGC 6380 C99 Terzan 1 I&&02 Ton 2 C99 NGC 6388 W81, HSM86, ZW84, WKA07, C&&07b NGC 6402 W81, HSM86, C&&97 NGC 6401 HSM86, ZW84, M95 NGC 6397 W81, HSM86, R&&97, DMM97, BPSK90, GPCM95, S&&93, M&&06, CBGL09, L&&09 Pal 6 M95, LC02a, LCB04 NGC 6426 HSM86 Djorg 1 C99 Terzan 5 AZ88, OR04 NGC 6440 W81, HSM86, ZW84, M95, OVR08 NGC 6441 W81, HSM86, ZW84, DMM97, C&&05, G&&06, G&&07, OVR08 Terzan 6 AZ88 NGC 6453 HSM86, ZW84 UKS 1 O&&05 NGC 6496 HSM86, ZW84, R&&97 Terzan 9 AZ88 Djorg 2 NGC 6517 HSM86, ZW84, M95 Terzan10 NGC 6522 R&&97, T&&98, EVR05 NGC 6535 HSM86, ZW84, R&&97, PM93 NGC 6528 W81, HSM86, ZW84, R&&97, AZ88, M95, CCGB01 NGC 6539 HSM86, ZW84, O&&05 NGC 6540 C99 NGC 6544 W81, HSM86, ZW84, R&&97 NGC 6541 W81, HSM86, R&&97, LC02b 2MS-GC01 ESO-SC06 NGC 6553 W81, HSM86, ZW84, R&&97, M95, M&&03, A&&06 2MS-GC02 B&&07 NGC 6558 HSM86, ZW84, DMM97, B&&07 IC 1276 C99 Terzan12 C99 NGC 6569 HSM86, ZW84 BH 261 GLIMPS02 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, D&&09, M&&09, L&&10 Pal 8 ZW84 NGC 6681 W81, HSM86, R&&97, DMM97, PMFH89 GLIMPS01 NGC 6712 W81, HSM86, ZW84, R&&97, GBML87, S&&93, Y&&08 NGC 6715 W81, HSM86, ZW84, DA95, B&&08 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, G&&05, C&&07, CBGL09, VPG09, L&&10 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, Sz&&07, CBGL09, L&&10 Terzan 8 DA95 Pal 11 W81 NGC 6838 W81, HSM86, M95, PL86, PM93, RS91, S&&93, CBB01, CBGL09 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, S&&99, P&&06, CBGL09 NGC 7089 W81, HSM86, ZW84, R&&97, AD86 NGC 7099 W81, HSM86, ZW84, R&&97, DMM97, PM93, S&&93, Sz&&07, CBGL09, L&&10 Pal 12 W81, R&&97, AD91 Pal 13 W81, C&&02, B&&04 NGC 7492 W81, R&&97, CM05b VELOCITY DISPERSIONS New for this edition, estimates of the central velocity dispersions are now included. The major starting point for this material continues to be the work of Pryor & Meylan (1993), who collected and analyzed the available velocity material up to that point. Numerous additional papers are now to be found, though in most cases these are new measurements for the same clusters as in the Pryor/Meylan compilations. More than half the clusters do not yet have a direct measurement of their internal velocity dispersion. The velocity dispersion quoted here is the estimated central value (at or near r=0), sometimes relying on small model extrapolations from velocity or proper motion data within the cluster core, or from the complete velocity dispersion profile. In recent papers much of the discussion concerns how best to model the dispersion profile with or without a central black hole, radially changing velocity anisotropy or mass-to-light ratio, etc. These considerations are at a much higher level of detail than is appropriate for this catalog; readers are advised to consult the papers concerned for any deeper study in this direction. Primary Sources: Pryor, C., and Meylan, G. 1993, in Structure and Dynamics of Globular Clusters, ASP Conf.Ser. 50, ed. S.G.Djorgovski and G. Meylan (San Francisco: A.S.P.), 357 Dubath, P., Meylan, G., and Mayor, M. 1997, AAp 324, 505 [data for 25 clusters] Additional Sources: Baumgardt, H. et al. 2009, MNRAS 396, 2051 [NGC 2419] Bellazzini, M. et al. 2008, AJ 136, 1147 [NGC 6715] Blecha, A., Meylan, G., North, P., and Royer, F. 2004, AAp 419, 533 [Pal 13] Cohen, J.G., and Melendez, J. 2005a, AJ 129, 303 [NGC 5272, 6205] Cohen, J.G., and Melendez, J. 2005b, AJ 129, 1607 [NGC 7492] Cote, P., Welch, D.L., Fischer, P., and Gebhardt, K. 1995, ApJ 454, 788 [NGC 3201] Cote, P. et al. 2002, ApJ 574, 783 [Pal 13] Drukier, G.A. et al. 1998, AJ 115, 708 [NGC 7078] Drukier, G.A., Bailyn, C.D., van Altena, W.F., and Girard, T.M. 2003, AJ 125, 2559 [NGC 6752] Drukier, G.A. et al. 2007, AJ 133, 1041 [NGC 6341] Dubath, P., Meylan, G., and Mayor, M. 1994, ApJ 426, 192 [NGC 7078] Dull, J.D. et al. 1997, ApJ 481, 267 [NGC 7078] Gebhardt, K., Pryor, C., Williams, T.B., and Hesser, J.E. 1994, AJ 107, 2067 [NGC 7078] Gebhardt, K., Pryor, C., Williams, T.B., and Hesser, J.E. 1995, AJ 110, 1699 [NGC 104, 6397, 7099] Gerssen, J. et al. 2002, AJ 124, 3270 [NGC 7078] Hankey, W.J., and Cole, A.A. 2010, MNRAS in press [IC 4499] Jordi, K. et al. 2009, AJ 137, 4586 [Pal 14] Lane, R.R. et al. 2010, MNRAS 406, 2732 [NGC 104, 288, 4590, 5024, 6121, 6218, 6656, 6752, 6809, 7099] McLaughlin, D.E. et al. 2006, ApJS 166, 249 [NGC 104] McNamara, B.J., Harrison, T.E., and Anderson, J. 2003, ApJ 595, 187 [NGC 7078] Meylan, G., Mayor, M., Duqennoy, A., and Dubath, P. 1995, AAp 303, 761 [NGC 5139] Odenkirchen, M. et al. 2002, AJ 124, 1497 [Pal 5] Peterson, R.C., and Cudworth, K.M. 1994, ApJ 420, 612 [NGC 6656] Peterson, R.C., Rees, R.F., and Cudworth, K.M. 1995, ApJ 443, 124 [NGC 6121] Piatek, S. et al. 1994, AJ 107, 1397 [NGC 6171] Ramirez, S.V., and Cohen, J.G. 2003, AJ 125, 224 [NGC 5904] Sollima, A. et al. 2009, MNRAS 396, 2183 [NGC 5139] van de Ven, G. et al. 2006, AAp 445, 513 [NGC 5139] van Leeuwen, F. et al. 2000, AAp 360, 472 [NGC 5139] Villanova, S., Piotto, G., and Gratton, R.G. 2009, AAp 499, 755 [NGC 6752] Here are the bibliographic sources, listed by cluster. The abbreviation code is: PM93 = Pryor & Meylan 1993, etc. NGC 104 PM93, G&&95, DMM97, Mc&&06 NGC 288 PM93 NGC 362 PM93, DMM97 Whiting 1 NGC 1261 Pal 1 AM 1 Eridanus Pal 2 NGC 1851 PM93, DMM97 NGC 1904 PM93, DMM97 NGC 2298 NGC 2419 PM93, B&&09 Ko 2 Pyxis NGC 2808 PM93 E 3 Pal 3 NGC 3201 PM93, C&&95 Pal 4 Ko 1 NGC 4147 PM93 NGC 4372 Rup 106 NGC 4590 PM93 NGC 4833 NGC 5024 NGC 5053 PM93 NGC 5139 PM93, M&&95, vL&&00, vdV&&06, S&&09 NGC 5272 PM93, DMM97, CM05a NGC 5286 PM93, DMM97 AM 4 NGC 5466 PM93 NGC 5634 NGC 5694 PM93, DMM97 IC 4499 WA10 NGC 5824 PM93, DMM97 Pal 5 O&&02 NGC 5897 NGC 5904 PM93, RC03, DMM97 NGC 5927 NGC 5946 PM93, DMM97 BH 176 NGC 5986 Lynga 7 Pal 14 J&&09 NGC 6093 PM93, DMM97 NGC 6121 PM93, PRC95 NGC 6101 NGC 6144 NGC 6139 Terzan 3 NGC 6171 PM93, P&&94 1636-283 NGC 6205 PM93, CM05a NGC 6229 NGC 6218 PM93 FSR 1735 NGC 6235 NGC 6254 PM93 NGC 6256 PM93, DMM97 Pal 15 NGC 6266 PM93 NGC 6273 NGC 6284 PM93, DMM97 NGC 6287 NGC 6293 PM93, DMM97 NGC 6304 NGC 6316 NGC 6341 PM93, D&&07 NGC 6325 PM93, DMM97 NGC 6333 NGC 6342 DMM97 NGC 6356 NGC 6355 NGC 6352 IC 1257 Terzan 2 NGC 6366 PM93 Terzan 4 HP 1 NGC 6362 PM93 Liller 1 NGC 6380 Terzan 1 Ton 2 NGC 6388 PM93 NGC 6402 NGC 6401 NGC 6397 PM93, G&&95, DMM97 Pal 6 NGC 6426 Djorg 1 Terzan 5 NGC 6440 NGC 6441 PM93, DMM97 Terzan 6 NGC 6453 UKS 1 NGC 6496 Terzan 9 Djorg 2 NGC 6517 Terzan 10 NGC 6522 PM93, DMM97 NGC 6535 PM93 NGC 6528 NGC 6539 NGC 6540 NGC 6544 NGC 6541 PM93 2MS-GC01 ESO-SC06 NGC 6553 2MS-GC02 NGC 6558 PM93, DMM97 IC 1276 Terzan 12 NGC 6569 BH 261 GLIMPSE02 NGC 6584 NGC 6624 PM93 NGC 6626 PM93 NGC 6638 NGC 6637 NGC 6642 NGC 6652 NGC 6656 PM93, PC94 Pal 8 NGC 6681 PM93, DMM97 GLIMPSE01 NGC 6712 PM93 NGC 6715 PM93, B&&08 NGC 6717 NGC 6723 NGC 6749 NGC 6752 PM93, DMM97, D&&98, VPG09 NGC 6760 NGC 6779 PM93 Terzan 7 Pal 10 Arp 2 NGC 6809 PM93 Terzan 8 Pal 11 NGC 6838 PM93 NGC 6864 PM93 NGC 6934 PM93 NGC 6981 NGC 7006 NGC 7078 PM93, DMM94, G&&94, DMM97, D&&97, D&&98, G&&02, MHA03 NGC 7089 PM93 NGC 7099 PM93, G&&95, DMM97 Pal 12 Pal 13 C&&02, B&&04 NGC 7492 CM05b STRUCTURAL AND DYNAMIC PARAMETERS Structural parameters include: - Core radius r_c - Half-light radius r_h (radius enclosing half the total luminosity) - Central concentration c = log(r_t/r_c) - Ellipticity - Central surface brightness mu_V(0) in magnitudes per sq arcsec, dereddened Wherever possible, these parameters refer to the ones obtained from profile fits using the King 1966 (AJ 71, 64) dynamical model. The data for r_c, r_h, c are taken primarily from the comprehensive lists of McLaughlin and van der Marel (2005) and (if not included by MV05) Trager et al. (1993, 1995). MV05 include the raw data used by TKD95, so the latter papers are used only for cases not covered by MV05. Direct comparison of the values of c, r_c, and r_h between these two sources shows good internal agreement except for a few cases where the profiles are low-S/N or complex and do not match the fundamental shape of the King model well. There are about 20 faint clusters not studied by MV05, for which r_h is not given by either source. For these, estimates of r_h have been calculated from the empirical 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 with low c-values. WARNING: The present edition of the catalog does not specifically list "tidal" or limiting radii r_t. As is discussed at length by McLaughlin & van der Marel, the formal estimate of r_t is very model-dependent for many clusters that have stellar distributions in their outer regions that do not conveniently match the basic King (1962, 1966) models. For example, the Wilson (1975) model, which is formally similar to King 1966 but uses a different formulation for the number of stars in phase space near the escape energy, generates a model with a more extended envelope and a larger r_t for the same core and half-light radii as in the King model. Readers wanting to calculate or use tidal radii should select the particular approach best suited to their goals after close reading of the primary literature. Also note that 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. The Trager et al. list arbitrarily adopts c = 2.50 for such clusters, but these do not necessarily match the real cluster structure. More useful empirical estimates for r_t can be found in McLaughlin & van der Marel 2005 and in Peterson & King 1975 (AJ 80, 427). Primary Sources: McLaughlin, D.E., and van der Marel, R. 2005, ApJS 161, 304 [85 clusters] Trager, S.C., King, I.R., and Djorgovski, S. 1995, AJ 109, 218 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.), 373 [54 clusters not listed by McLaughlin & van der Marel] Additional Sources: Bellazzini, M. 2007, AAp 473, 171 [NGC 2419] Bonatto, C., and Bica, E. 2008, AAp 479, 741 [IC 1257, Lynga 7, Ter 4, Ter 10, BH176, BH261, ESO452-SC11, ESO 280-SC06, 2MASS-GC01 and GC02, GLIMPSE-C01] Carraro, G. 2009, AJ 137, 3809 [AM-4] Carraro, G., Zinn, R., and Moni Bidin, C. 2007, AAp 466, 181 [Whiting 1] Cote, P., Welch, D.L., Fischer, P., & Gebhardt, K. 1995, ApJ, 454, 788 [NGC 3201] de Marchi, G., and Pulone, L. 2007, AAp 467, 107 [NGC 2298] Ferraro, F.R. et al. 2006, ApJ 638, 443 [NGC 5139] Froebrich, D., Meusinger, H., and Scholz, A. 2007, MNRAS 377, L54 [FSR1735] 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] Hilker, M. 2006, AAp 448, 171 [Pal 3, Pal 14, AM-1] Ivanov, V.D., Kurtev, R., and Borissova, J. 2005, AAp 442, 195 [GLIMPSE-C01] Kaisler, D., Harris, W.E., & McLaughlin, D.E. 1997, PASP, 109, 920 [NGC 6749, Pal 10] Koposov, S. et al. 2007, ApJ 669, 337 [Ko 1, 2] Kurtev, R. et al. 2008, AAp 489, 583 [GLIMPSE-C02] Lanzoni, B. et al. 2007, ApJ 663, 267 [NGC 5904] Lanzoni, B. et al. 2007, ApJ 663, 1040 [NGC 1904] Lanzoni, B. et al. 2007, ApJ 668, L139 [NGC 6388] Lanzoni, B. et al. 2010, ApJ 717, 653 [Ter 5] Lehmann, I., & Scholz, R.-D. 1997, AAp, 320, 776 [NGC 5904, 6218, 6205, 7078, 5024, 5053, 5466] McLaughlin, D.E. et al. 2006, ApJS 166, 249 [NGC 104] Tucholke, H.-J. 1992, AAp, 264, 513 [NGC 104, 362] The "eccentricity" or projected shape of the cluster is defined as e = 1 - (b/a) where a,b are the semimajor and semiminor axes of the cluster light profile. These are taken from R.E.White and S.J.Shawl 1987 (ApJ 317, 246) for 99 clusters, and from Geyer, Nelles, and Hopp 1983 (AAp 125, 359) for omega Centauri. Newer work by Chen & Chen 2010 (ApJ 721, 1790) provides ellipticities measured from 2MASS images for 95 clusters. They find generally larger e-values than White & Shawl though with lots of scatter. As Chen & Chen discuss, their IR-imaging results are less affected by foreground extinction than the optical data, but more affected by individual starcount numbers and by features at larger radius such as tidal tails or outer "stretching" of the cluster distribution. For the time being, I keep the White/Shawl list as more representative of the inner brightest parts of the clusters. The central surface brightness mu_V(0) (V magnitudes per square arcsecond at r=0) is the average of the values from Trager et al. (1995) and McLaughlin & van der Marel (2005), plus other values for individual clusters from the available literature given below. These surface brightnesses are NOT corrected for foreground extinction ("dereddened"). The values from McLaughlin & van der Marel (their Table 10) were dereddened with A_V = 3.1 E(B-V), so I have added the individual A_V values back in to their data before averaging with the other sources. Both these papers use the same raw profile data, so in this case we are averaging over two different analysis procedures rather than two independent measurements. In practice they correlate very well for the clusters of overlap. The mu_V(0) data in this catalog should be viewed as those measured from classical ground-based imaging data, with spatial resolution of about 1 arcsecond. With much better subarcsecond resolution such as from HST, many clusters reveal interesting core structures, power-law profiles rising to the center, central cusps etc. that were not resolved from the ground. In these cases the "true" mu_V(0) values can be very much brighter. Many of these are discussed, for example, by Noyola & Gebhardt (2006). Taking these into account would effectively change the meaning of mu_V(0) for a subsample of clusters, so for the sake of preserving internal consistency in the catalog, the HST data for these types of structures are not used. The earlier compilation by Webbink (1985) is used for 13 clusters for which no other central surface brightness estimates are available. The central luminosity density, rho_0, in Solar luminosities per cubic parsec, is calculated from the prescription given by Djorgovski (1993, equation 4), using the previously determined values of the central surface brightness, total cluster luminosity, and core radius. 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), i.e. his equation (10) for t(r_c) and equation (11) for t(r_h), 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) and with the calculations in McLaughlin & van der Marel 2005. 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. We conventionally assume that the (not directly observed) half-MASS radius is the same as the directly observed half-light radius r_h. Sources for surface brightness: Bellazzini, M. 2007, AAp 473, 171 [NGC 2419] Hilker, M. 2006, AAp 448, 171 [AM-1, Pal 3, Pal 14] McLaughlin, D.E., and van der Marel, R.P. 2005, ApJS 161, 304 [81 clusters excluding Pal 1, Liller 1, NGC 6539, NGC 7492] McLaughlin, D.E. et al. 2006, ApJS 166, 249 [NGC 104] Noyola, E., and Gebhardt, K. 2006, AJ 132, 447 [NGC 104, 1904, 2298, 2808, 5897, 5904, 6093, 6205, 6254, 6266, 6287, 6341, 6333, 6352, 6397, 6441, 6528, 6626, 6637, 6681, 6712, 6752] Trager, S.C., King, I.R., and Djorgovski, S. 1995, AJ 109, 218 [124 clusters excluding Pal 4] Webbink, R. 1985, in Dynamics of Star Clusters, IAU Symposium 113, p. 541 [Eridanus, E3, Rup106, AM4, BH176, Ter 3, ESO452-SC11, Pal 15, Ton 2, UKS 1, Ter 10, Ter 12, Ter 8] DELETED MATERIAL There are two types of data no longer included in this catalog: the specific frequency of RR Lyrae stars, S_RR; and the horizontal-branch type (B-R)/(B+V+R) or its equivalents. For the RR Lyraes, the reader should see the more complete variable-star catalogs by Suntzeff, Kinman, and Kraft 1991 (ApJ, 367, 528) and C.M.Clement et al. 2001, AJ 122, 2587. Christine Clement (U.Toronto) is assembling a more recent edition of the variable-star catalog as well. For the horizontal-branch types, work over the past decade has clearly revealed that a single parameter or ratio does not correctly describe the distribution of stars along the HB, and may actually be counterproductive in some cases. For example, clusters are mass-segregated and so 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, leading to bimodal or even trimodal distributions in color; and many clusters at a wide range of metallicities have highly extended blue BHB tails. Thus the classic simple HB morphology parameters appear to have outlived their usefulness. End Text of Bibliography