Cited by 4,500Stellar, planetary, and galactic studiesGalaxies: Formation, Evolution, PhenomenaAstronomy and Astrophysical Research

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A Catalog of Parameters for Globular Clusters in the Milky Way

Harris, William E.·1996·The Astronomical Journal

DOI 10.1086/118116

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Abstract

A database of parameters for globular star clusters in the Milky Way is described which is available in electronic form through the WorldWideWeb. The information in the catalog includes up-to-date measurements for cluster distance, reddening, luminosity, colors and spectral types, velocity, structural and dynamical parameters, horizontal branch morphology, metallicity, and other quantities. This catalog will be updated regularly and maintained in electronic form for widest possible accessibility.

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THE SEGUE STELLAR PARAMETER PIPELINE. I. DESCRIPTION AND COMPARISON OF INDIVIDUAL METHODS
Lee, Y. S., Beers, T. C., Sivarani, T., Prieto, C. A., Koesterke, L., Wilhelm, R., Fiorentin, P. R., Bailer‐Jones, C. A. L., Norris, J. E., Rockosi, C. M., et al. (2008) · The Astronomical Journal · doi:10.1088/0004-6256/136/5/2022 · Cited by 505
“The solid red line is the literature value of metallicity, reported by Harris (1996) for M 15 and M 13, and Gratton (2000) for NGC 2420 and M 67, while the dashed green line indicates the Gaussian mean SSPP [Fe/H] for the likely member stars (solid dots).”
Background
THE RADIAL VELOCITY EXPERIMENT (RAVE): FIFTH DATA RELEASE
Kunder, A., Kordopatis, G., Steinmetz, M., Zwitter, T., McMillan, P. J., Casagrande, L., Enke, H., Wojno, J., Valentini, M., Chiappini, C., et al. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/153/2/75 · Cited by 503
“The open cluster properties come from the Milky Way global survey of star clusters (Kharchenko et al. 2013) and the globular cluster properties come from the Harris catalog (Harris 1996, 2010 update).”
Method
The Dark Energy Survey: Data Release 1
Abbott, T., Abdalla, F., Allam, S., Amara, A., Annis, J., Asorey, J., Ávila, S., Ballester, O., Banerji, M., Barkhouse, W., et al. (2018) · Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aae9f0 · Cited by 514
“Table 5 lists five classical globular clusters within the DES DR1 footprint with integrated V-band magnitude brighter than 10 (Harris 1996, 2010 edition).”
Background
A New Milky Way Dwarf Galaxy in Ursa Major
Willman, B., Dalcanton, J. J., Martínez‐Delgado, D., West, A. A., Blanton, M. R., Hogg, D. W., Barentine, J. C., Brewington, H., Harvanek, M., Kleinman, S. J., et al. (2005) · The Astrophysical Journal · doi:10.1086/431760 · Cited by 497
“…half-light size of the Ursa Major dwarf is also quite similar to those of the known Milky Way dSphs, but is nearly an order of magnitude larger than those of either the largest Milky Way globular clusters (Harris 1996) or the newly discovered extended star clusters around M31 (Huxor et al. 2004).”
Background
THE ACS SURVEY OF GALACTIC GLOBULAR CLUSTERS. VII. RELATIVE AGES
Marín-Franch, A., Aparicio, A., Piotto, G., Rosenberg, A., Chaboyer, B., Sarajedini, A., Siegel, M., Anderson, J., Bedin, L. R., Dotter, A., et al. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/694/2/1498 · Cited by 494
“Column 6 lists the Galactocentric distance (rGC, in kpc), taken from Harris (1996).”
Method
THE AGES OF 55 GLOBULAR CLUSTERS AS DETERMINED USING AN IMPROVED $\Delta V^{\rm HB}_{\rm TO}$ METHOD ALONG WITH COLOR-MAGNITUDE DIAGRAM CONSTRAINTS, AND THEIR IMPLICATIONS FOR BROADER ISSUES
VandenBerg, D. A., Brogaard, K., Leaman, R., & Casagrande, L. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/775/2/134 · Cited by 487
“…13.25±1.00, and 13.25±1.00 Gyr for 47 Tuc, M 15, and M 92, respectively, using an isochrone-fitting procedure that permitted small adjustments to the distances, reddenings, and metallicities from initial estimates of these quantities given in the 2003 revision of the Harris (1996) catalog.”
BackgroundMethodInfluential
Detection of Massive Tidal Tails around the Globular Cluster Palomar 5 with Sloan Digital Sky Survey Commissioning Data
Odenkirchen, M., Grebel, E., Rockosi, C., Dehnen, W., Ibata, R., Rix, H., Stolte, A., Wolf, C., Anderson, J. E., Bahcall, N., et al. (2000) · The Astrophysical Journal · doi:10.1086/319095 · Cited by 173
Na-O Anticorrelation and HB. VII. The chemical composition of first and second-generation stars in 15 globular clusters from GIRAFFE spectra
Carretta, E., Bragaglia, A., Gratton, R., et al. (2009) · HAL (Le Centre pour la Communication Scientifique Directe) · doi:10.48550/arxiv.0909.2938 · Cited by 491
“Finally, the range in mass covers more than one order of magnitude, from M 71 (NGC 6838, absolute magnitudeMV = −5.60 (Harris 1996) up to NGC 6441 (MV = −9.64).”
BackgroundMethodInfluential
The Observed Properties of Dark Matter on Small Spatial Scales
Gilmore, G. F., Wilkinson, M. I., Wyse, R. F. Ġ., Kleyna, J. T., Koch, A., Evans, N. W., & Grebel, E. K. (2007) · The Astrophysical Journal · doi:10.1086/518025 · Cited by 488
The ACS survey of Galactic globular clusters
Milone, A. P., Piotto, G., Bedin, L. R., et al. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201016384 · Cited by 484
“…involved in this analysis are the absolute visual magnitudeMV , the ellipticity (e), the central concentration (c), the core relaxation timescale,τc, the half-mass relaxation timescaleτhm, and the logarithm of the central luminosity densityρ0, and are taken from the Harris (1996) compilation.”
MethodInfluential
Gaia EDR3 view on galactic globular clusters
Vasiliev, E., & Baumgardt, H. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1475 · Cited by 492
“Out of 157 objects in the Harris (1996, 2010) catalogue, we could not determine the PM for only a few clusters which are located in highly extincted regions and are not visible to Gaia: 2MASS–GC01, 2MASS–GC02, GLIMPSE01 and GLIMPSE02.”
Background
TheHubble Space TelescopeUV Legacy Survey of Galactic globular clusters – IX. The Atlas of multiple stellar populations
Milone, A. P., Piotto, G., Renzini, A., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2531 · Cited by 477
“All these quantities are taken from the 2010 edition of the Harris (1996) catalog.”
Background
THE DISRUPTION OF GIANT MOLECULAR CLOUDS BY RADIATION PRESSURE & THE EFFICIENCY OF STAR FORMATION IN GALAXIES
Murray, N., Quataert, E., & Thompson, T. A. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/709/1/191 · Cited by 476
“30Myr) and old (& 30Myr) clusters in M51 with masses in the range 103 − 106M⊙ (Scheepmaker et al. 2007), for super star clusters in M82 withMcl = 105 − 4× 106M⊙ (McCrady et al. 2003; McCrady & Graham 2007), and in globular clusters with masses∼ 105 − 106M⊙ (Harris 1996).”
Background
Space Velocities of Globular Clusters. III. Cluster Orbits and Halo Substructure
Casetti‐Dinescu, D. I., Girard, T. M., & van Altena, W. F. (1999) · The Astronomical Journal · doi:10.1086/300807 · Cited by 460
“Intuitively, they should have formed in systems more massive than Sagittarius, if the mass of a system correlates with its mean metallicity (Gallagher & Wyse 1994) and with the mean metallicity of its globular cluster system (Harris 1996b).”
Background
THE ACS SURVEY OF GALACTIC GLOBULAR CLUSTERS. IX. HORIZONTAL BRANCH MORPHOLOGY AND THE SECOND PARAMETER PHENOMENON
Dotter, A., Sarajedini, A., Anderson, J., Aparicio, A., Bedin, L. R., Chaboyer, B., Majewski, S., Marín-Franch, A., Milone, A., Paust, N., et al. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/708/1/698 · Cited by 475
“From the Harris (1996) catalog, we extracted central luminosity density (ρ0).”
BackgroundMethodInfluential
Swings between rotation and accretion power in a binary millisecond pulsar
Papitto, A., Ferrigno, C., Bozzo, E., et al. (2013) · Nature · doi:10.1038/nature12470 · Cited by 460
Multiple populations in globular clusters. Lessons learned from the Milky Way globular clustersPreprint
Gratton, R., Carretta, E., & Bragaglia, A. (2012) · arXiv (Cornell University) · doi:10.48550/arxiv.1201.6526 · Cited by 452
“This result is supported by the good agreement, especially for the inner halo, between the metallicity distribution of halo globular clusters (data from the Harris 1996 catalogue) and of the Milky Way halo, as determined from in situ observations (Ivezic et al. 2008; see Fig.”
BackgroundResult
Age and metallicity distribution of the Galactic bulge from extensive optical and near-IR stellar photometry
Zoccali, M., Renzini, A., Ortolani, S., Greggio, L., Saviane, I., Cassisi, S., Rejkuba, M., Barbuy, B., Rich, R. M., & Bica, E. (2003) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20021604 · Cited by 444
“With the exception of the two most metal rich clusters (NGC 6528 and NGC 6553), for the GCs in Table 2 we adopted the iron abundance [Fe/H] from Harris (1996), and corrected it to [M/H] adopting an α-element enhancement [α/Fe]= 0.3 for clusters with [Fe/H] −1.0, and [α/Fe] = 0.20 for more Fig.”
MethodInfluential
The Accretion Origin of the Milky Way’s Stellar Halo
Bell, E. F., Zucker, D. B., Belokurov, V. A., Sharma, S., Johnston, K. V., Bullock, J. S., Hogg, D. W., Jahnkę, K., de Jong, J. T. A., Beers, T. C., et al. (2008) · The Astrophysical Journal · doi:10.1086/588032 · Cited by 446
“To help interpret this Hess diagram, we show two additional Hess diagrams for two globular clusters covered by these data: Pal 5 and NGC 5024 (in what follows, distances and metallicities for these and all other globular clusters are adopted from Harris 1996).”
Method
INTERMEDIATE-MASS BLACK HOLES
Miller, M. C., & Colbert, E. J. M. (2004) · International Journal of Modern Physics D · doi:10.1142/s0218271804004426 · Cited by 449
“…of interest that there are dozens of sources in globulars around NGC 1399 with LX > 10 38 erg s−1, given that neither our Galaxy (with ≈150 globulars, Harris 1996) nor M31 (with ≈300−400 globulars, Hodge 1992, Fusi Pecci et al. 1993) has any X-ray sources in globular clusters with LX >∼ 10 38 erg…”
Background
The ACS Virgo Cluster Survey. IX. The Color Distributions of Globular Cluster Systems in Early‐Type Galaxies
Peng, E. W., Jordán, A., Côté, P., Blakeslee, J. P., Ferrarese, L., Mei, S., West, M. J., Merritt, D. R., Milosavljević, M., & Tonry, J. L. (2006) · The Astrophysical Journal · doi:10.1086/498210 · Cited by 436
Origin of the system of globular clusters in the Milky Way
Massari, D., Koppelman, H. H., & Helmi, A. (2019) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201936135 · Cited by 441
Variable Stars in Galactic Globular Clusters
Clement, C. M., Muzzin, A., Dufton, Q. W., et al. (2001) · The Astronomical Journal · doi:10.1086/323719 · Cited by 439
Mean proper motions, space orbits, and velocity dispersion profiles of Galactic globular clusters derived from Gaia DR2 data
Baumgardt, H., Hilker, M., Sollima, A., & Bellini, A. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2997 · Cited by 452
“For each of these clusters we selected all Gaia stars within a circle of 1200 arcsec around the cluster centers given by either Goldsbury, Heyl & Richer (2013) or Harris (1996).”
MethodResultInfluential
THE ACS SURVEY OF GLOBULAR CLUSTERS. V. GENERATING A COMPREHENSIVE STAR CATALOG FOR EACH CLUSTER
Anderson, J., Sarajedini, A., Bedin, L. R., et al. (2008) · The Astronomical Journal · doi:10.1088/0004-6256/135/6/2055 · Cited by 429
“Many subsequent “surveys” have been constructed by assembling various data from the multitude of independent observations of individual clusters (e.g., Djorgovski & King 1986, Djorgovski & Meylan 1993, Trager et al. 1995, Lee et al. 1996, and Harris 1996).”
Background
Revised Catalog of GALEX Ultraviolet Sources. I. The All-Sky Survey: GUVcat_AIS
Bianchi, L., Shiao, B., & Thilker, D. (2017) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aa7053 · Cited by 451
“…taken from the compilation available at https://heasarc.gsfc.nasa.gov/ W3Browse/all/mwsc.htm, which basically includes all globular clusters from Harris (1996), which are all confirmed objects, and includes as “open clusters” confirmed, candidate or doubtful clusters, or spurious objects such…”
Background
Properties of Globular Cluster Systems in Nearby Early-Type Galaxies
Larsen, S. S., Brodie, J. P., Huchra, J. P., Forbes, D. A., & Grillmair, C. J. (2001) · The Astronomical Journal · doi:10.1086/321081 · Cited by 415
“For comparison, we have also included the LF for Milky Way globular clusters (shown with dots), using data from Harris (1996).”
BackgroundMethodInfluential
Calibration of the Tip of the Red Giant Branch
Freedman, W. L., Madore, B. F., Hoyt, T. J., Jang, I. S., Beaton, R. L., Lee, M. G., Monson, A., Neeley, J., & Rich, J. A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab7339 · Cited by 442
Dynamical Evolution of the Mass Function of Globular Star Clusters
Fall, S. M., & Zhang, Q. (2001) · The Astrophysical Journal · doi:10.1086/323358 · Cited by 405
“The latter is based on the luminosities of the 146 clusters with known distances in the most recent compilation of data by Harris (1996, 1999) and M/LV = 3.”
BackgroundMethodInfluential
Mapping the three-dimensional density of the Galactic bulge with VVV red clump stars
Wegg, C., & Gerhard, O. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1376 · Cited by 399
THE DENSE MATTER EQUATION OF STATE FROM NEUTRON STAR RADIUS AND MASS MEASUREMENTS
Özel, F., Psaltis, D., Güver, T., et al. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/820/1/28 · Cited by 404
TARGET SELECTION FOR THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT (APOGEE)
Zasowski, G., Johnson, J. A., Frinchaboy, P. M., Majewski, S. R., Nidever, D. L., Rocha–Pinto, H. J., Girardi, L., Andrews, B., Chojnowski, S. D., Cudworth, K. M., et al. (2013) · The Astronomical Journal · doi:10.1088/0004-6256/146/4/81 · Cited by 400
High‐Velocity Clouds: Building Blocks of the Local Group
Blitz, L., Spergel, D. N., Teuben, P. J., Hartmann, D., & Burton, W. B. (1999) · The Astrophysical Journal · doi:10.1086/306963 · Cited by 398
“Using the compilation of Harris (1996), we Ðnd that the globular clusters have a dispersion of 134 km s~1 and a mean velocity of 9^ 12 km s~1 relative to the LSR; relative to the GSR, the dispersion is 119 km s~1 with a mean of 3^ 11 km s~1, as expected.”
Method
MERGING BLACK HOLE BINARIES IN GALACTIC NUCLEI: IMPLICATIONS FOR ADVANCED-LIGO DETECTIONS
Antonini, F., & Rasio, F. A. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/831/2/187 · Cited by 423
“Princeton Univ. Press, New Jersey, USA Blandford and Hughes, S. 2003, ApJ, 585, L101 Bogdanović, T., Reynolds, C. S., & Miller, M. C. 2007, ApJ, 661, L147 Böker, T., Sarzi, M., McLaughlin, D. E., et al. 2004, AJ, 127, 105 Bonnell, I. A., & Rice, W. K. M. 2008, Science, 321, 1060 Chandrasekhar, S. 1943, ApJ, 97, 255…”
MethodResultInfluential
Photospheric radius expansion X-ray bursts as standard candles
Kuulkers, E., den Hartog, P. R., Zand, J. J. M. I. '., et al. (2003) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20021781 · Cited by 389
“The absolute calibration of distance follow the prescription adopted by Harris (1996), namely (m−M)0 = VHB −MV (HB)− 3.1 E(B − V ) (1) where the absolute magnitude is a function of metallicity, MV (HB) = 0.15[Fe/H] + 0.80 .”
BackgroundMethodInfluentialSelf-citation
THE RADIAL VELOCITY EXPERIMENT (RAVE): FOURTH DATA RELEASE
Kordopatis, G., Gilmore, G. F., Steinmetz, M., Boeche, C., Seabroke, G. M., Siebert, A., Zwitter, T., Binney, J. J., de Laverny, P., Recio-Blanco, A., et al. (2013) · The Astronomical Journal · doi:10.1088/0004-6256/146/5/134 · Cited by 378
The present and future mass of the Milky Way halo
Wilkinson, M. I., & Evans, N. W. (1999) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1999.02964.x · Cited by 383
A New Milky Way Companion: Unusual Globular Cluster or Extreme Dwarf Satellite?
Willman, B., Blanton, M. R., West, A. A., Dalcanton, J. J., Hogg, D. W., Schneider, D. P., Wherry, N., Yanny, B., & Brinkmann, J. (2005) · The Astronomical Journal · doi:10.1086/430214 · Cited by 380
“The deeper CMD based on the APO data, shown in Figure 6, provides even more compelling evidence that the detected stellar overdensity is a turnoff at 45 kpc rather than a horizontal branch at 170 kpc. Pal 5 has an age of 11–12 Gyr (Martell et al. 2002) and an ½Fe/H ¼ 1:38 (Harris 1996).”
BackgroundMethodInfluential
Nuclear star clusters
Neumayer, N., Seth, A., & Böker, T. (2020) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-020-00125-0 · Cited by 450

Authors: Harris, W. E.
Corresponding author: Harris, William E.
ORCID: Harris, William E.
Venue: The Astronomical Journal
Publisher: American Astronomical Society
Published: 1996-10
Volume: 112
Pages: 1487
ISSN: 0004-6256 (ISSN-L)
DOI: 10.1086/118116
OpenAlex: W2066406099
Cited by: 4,500
References: 0
Citations by year: 2026: 79 · 2025: 118 · 2024: 142 · 2023: 128 · 2022: 135 · 2021: 193 · 2020: 173 · 2019: 204 · 2018: 207 · 2017: 174 · 2016: 228 · 2015: 190 · 2014: 190 · 2013: 207 · 2012: 201
FWCI: 35.37
Type: journal article
Language: en
Open access: closed
Locations: The Astronomical Journal (publishedVersion)
Topics: Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
Keywords: globular clusters, Milky Way, cluster parameters, distance, reddening, luminosity, color, spectral types, velocity, structural parameters, dynamic parameters, horizontal branch morphology, metallicity

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A Catalog of Parameters for Globular Clusters in the Milky Way

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