A Catalog of Parameters for Globular Clusters in the Milky Way
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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Maraston, C. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09270.x · Cited by 1,907 · see citing works
“…focuses on sub-solar chemical compositions, it has to be expected that if a fundamental problem 10 as derived from the HBR parameter listed in the Harris (1996) in the treatment of the opacity would be responsible for the colour offset, this would be even more serious at higher metallicities.”
BackgroundConroy, C., Gunn, J. E., & White, M. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/699/1/486 · Cited by 1,891 · see citing works
The Dartmouth Stellar Evolution Database
Dotter, A., Chaboyer, B., Jevremović, D., Kostov, V., Baron, E., & Ferguson, J. W. (2008) · The Astrophysical Journal Supplement Series · doi:10.1086/589654 · Cited by 1,765 · see citing works
“Plotted on top of the M 13 data in Figure 11 are isochrones with [Fe/H]=-1.5, [α/Fe]=+0.2 at 11 and 13 Gyr assuming a distance modulus of 14.4 in agreement with Harris (1996).”
MethodInfluentialMedium-resolution Isaac Newton Telescope library of empirical spectra
Sánchez–Blázquez, P., Peletier, R. F., Jiménez-Vicente, J., Cardiel, N., Cenarro, A. J., Falcón‐Barroso, J., Gorgas, J., Selam, S. O., & Vazdekis, A. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10699.x · Cited by 1,580 · see citing works
FERMI LARGE AREA TELESCOPE THIRD SOURCE CATALOG
Acero, F., Ackermann, M., Ajello, M., et al. (2015) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/218/2/23 · Cited by 1,480 · see citing works
Fermi Large Area Telescope Fourth Source Catalog
Abdollahi, S., Acero, F., Ackermann, M., et al. (2020) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ab6bcb · Cited by 1,355 · see citing works
“…et al. (2019) Low-mass X-ray binaries 187 Liu et al. (2007) Point-like SNR 158 Green (2014)c Extended SNRd 295 Green (2014)c Globular clusters 160 Harris (1996) Dwarf galaxiesd 100 McConnachie (2012) Nearby galaxies 276 Schmidt et al. (1993) IRAS bright galaxies 82 Sanders et al. (2003) BZCAT…”
BackgroundMasses, Radii, and the Equation of State of Neutron Stars
Özel, F., & Freire, P. C. C. (2016) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081915-023322 · Cited by 1,365 · see citing works
The Milky Way Tomography with SDSS. I. Stellar Number Density Distribution
Jurić, M., Ivezić, Ž., Brooks, A. M., Lupton, R. H., Schlegel, D. J., Finkbeiner, D. P., Padmanabhan, N., Bond, N., Sesar, B., Rockosi, C. M., et al. (2008) · The Astrophysical Journal · doi:10.1086/523619 · Cited by 1,318 · see citing works
“We require a loworder polynomial fit that is roughly consistent with the three relations at the red end and properly reproduces the SDSS observations of the position of the turnoff (median Mr ¼ 5 at r i ¼ 0:10) for globular cluster M13 (using a distance of 7.1 kpc; Harris 1996).”
MethodInfluentialFERMI LARGE AREA TELESCOPE SECOND SOURCE CATALOG
Nolan, P. L., Abdo, A. A., Ackermann, M., Ajello, M., Allafort, A., Antolini, E., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., et al. (2012) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/199/2/31 · Cited by 1,296 · see citing works
FERMI LARGE AREA TELESCOPE FIRST SOURCE CATALOG
Abdo, A. A., Ackermann, M., Ajello, M., Allafort, A., Antolini, E., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., et al. (2010) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/188/2/405 · Cited by 1,318 · see citing works
Abdurrouf, Accetta, K., Aerts, C., Aguirre, V. S., Ahumada, R., Ajgaonkar, N., Ak, N. F., Alam, S., Prieto, C. A., Almeida, A., et al. (2022) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ac4414 · Cited by 1,296 · see citing works
Star-Formation Histories, Abundances, and Kinematics of Dwarf Galaxies in the Local Group
Tolstoy, E., Hill, V., & Tosi, M. (2009) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082708-101650 · Cited by 1,179 · see citing works
Zwart, S. P., McMillan, S., & Gieles, M. (2010) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081309-130834 · Cited by 926 · see citing works
Conroy, C., & Gunn, J. E. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/712/2/833 · Cited by 1,190 · see citing works
Masses, Radii, and the Equation of State of Neutron Stars
Özel, F., & Freire (2016) · MPG.PuRe (Max Planck Society) · Cited by 1,057 · see citing works
The Dark Energy Survey: more than dark energy - an overview
Abbott, D., Abdalla, F., Aleksic, J., Allam, S., Amara, A., Bacon, D., Balbinot, E., Banerji, M., Bechtol, K., Benoit-Lévy, A., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw641 · Cited by 766 · see citing works
The Kinematics of the Ultra‐faint Milky Way Satellites: Solving the Missing Satellite Problem
Simon, J. D., & Geha, M. (2007) · The Astrophysical Journal · doi:10.1086/521816 · Cited by 974 · see citing works
“In comparison, Galactic globular clusters follow no such relationship (Harris 1996).”
Abundance Variations within Globular Clusters
Gratton, R., Sneden, C., & Carretta, E. (2004) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.42.053102.133945 · Cited by 885 · see citing works
“…AR222-AA42-10.sgm LaTeX2e(2002/01/18) P1: IKH ABUNDANCES IN GLOBULAR CLUSTERS 393 two clusters are relatively young, outer-halo clusters (Harris 1996)2 that might not share a common origin with the majority of Galactic GCs. Rup 106 and Pal 12 are more notably underabundant in α elements…”
BackgroundMethodBabusiaux, C., van Leeuwen, F., Barstow, M. A., Jordi, C., Vallenari, A., Bossini, D., Bressan, A., Cantat-Gaudin, T., van Leeuwen, M., Brown, A. G. A., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832843 · Cited by 873 · see citing works
Toward Better Age Estimates for Stellar Populations: The Y2 Isochrones for Solar Mixture
Yi, S., Demarque, P., Kim, Y.-C., Lee, Y.-W., Ree, C., Lejeune, T., & Barnes, S. (2001) · The Astrophysical Journal Supplement Series · doi:10.1086/321795 · Cited by 705 · see citing works
“Figure 18 shows the mean integrated colors of Galactic globular clusters (Harris 1996) compared with the models.”
MethodStellar population models of Lick indices with variable element abundance ratios
Thomas, D., Maraston, C., & Bender, R. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06248.x · Cited by 839 · see citing works
“In this section we compare the total metallicities [Z/H] derived here for the galactic globular cluster sample with the metallicities given in the Harris (1996) catalog, which are based on the Zinn & West (1984, hereafter ZW84) scale.”
MethodVazdekis, A., Sánchez–Blázquez, P., Falcón‐Barroso, J., Cenarro, A. J., Beasley, M. A., Cardiel, N., Gorgas, J., & Peletier, R. F. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16407.x · Cited by 802 · see citing works
“The obtained ages and metallicities fully agree with the CMD-derived es- timates of the Harris (1996) catalog.”
ResultCats and Dogs, Hair and a Hero: A Quintet of New Milky Way Companions
Belokurov, V. A., Zucker, D. B., Evans, N. W., Kleyna, J. T., Koposov, S. E., Hodgkin, S. T., Irwin, M. J., Gilmore, G. F., Wilkinson, M. I., Fellhauer, M., et al. (2007) · The Astrophysical Journal · doi:10.1086/509718 · Cited by 800 · see citing works
Multiple populations in globular clusters
Gratton, R., Carretta, E., & Bragaglia, A. (2012) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-012-0050-3 · Cited by 765 · see citing works
“Some fraction of the stars should be removed from the cluster within a relaxation time, typically ∼5 × 108 yr (see the compilation by Harris 1996).”
BackgroundResultCarretta, E., Bragaglia, A., Gratton, R., et al. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912096 · Cited by 791 · see citing works
“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).”
BackgroundMethodInfluentialDynamical evolution of star clusters in tidal fields
Baumgardt, H., & Makino, J. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06286.x · Cited by 775 · see citing works
“Beside the names, we have listed the present-day masses, calculated from the absolute lu- minosities given in the compilation of Harris (1996) and an assumed mass-to-light ratio of 2.”
BackgroundMethodInfluentialMcLaughlin, D. E., & van der Marel, R. P. (2005) · The Astrophysical Journal Supplement Series · doi:10.1086/497429 · Cited by 727 · see citing works
“Column 4 gives the observed (B−V) color of the cluster whenever such a measurement exists (taken either from the aperture-photometry sources in Table 3 above, or from Harris 1996, for the Milky Way globulars)).”
BackgroundMethodResultInfluentialGlobal survey of star clusters in the Milky Way
Kharchenko, N. V., Piskunov, A. E., Schilbach, E., Röser, S., & Scholz, R. ‐. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201322302 · Cited by 715 · see citing works
“Furthermore, we included embedded and globular clusters taken from the catalogues by Lada & Lada (2003) and Harris (1996)[edition 2010]2 in our target list.”
MethodA Gaia DR2 view of the open cluster population in the Milky Way
Cantat-Gaudin, T., Jordi, C., Vallenari, A., Bragaglia, A., Balaguer-Núñez, L., Soubiran, C., Bossini, D., Moitinho, A., Castro-Ginard, A., Krone-Martins, A., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201833476 · Cited by 750 · see citing works
“We verified that both objects are absent from the updated web page of the globular cluster catalogue of Harris (1996).”
BackgroundThe Runaway Growth of Intermediate‐Mass Black Holes in Dense Star Clusters
Zwart, S. P., & McMillan, S. L. W. (2002) · The Astrophysical Journal · doi:10.1086/341798 · Cited by 694 · see citing works
“The current half-mass relaxation time of M15 is about 2.5 Gyr (Harris 1996), which is far more than our 100 Myr limit for forming a massive central object from a collision runaway.”
BackgroundInfluentialIntrinsic iron spread and a new metallicity scale for globular clusters
Carretta, E., Bragaglia, A., Gratton, R., D’Orazi, V., & Lucatello, S. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200913003 · Cited by 677 · see citing works
“6 and we give metallicity values on our new scale for all GCs in the Harris (1996) catalogue in the Appendix.”
BackgroundMethodInfluentialMultiple Stellar Populations in Globular Clusters
Bastian, N., & Lardo, C. (2018) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081817-051839 · Cited by 693 · see citing works
Accurate masses for dispersion-supported galaxies
Wolf, J., Martinez, G. D., Bullock, J. S., Kaplinghat, M., Geha, M., Muñoz, R. R., Simon, J. D., & Avedo, F. F. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16753.x · Cited by 691 · see citing works
Stellar Population Inference with Prospector
Johnson, B. D., Leja, J., Conroy, C., & Speagle, J. S. (2021) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/abef67 · Cited by 697 · see citing works
“We fix the distance to the value given by Harris (1996) since for integrated SEDs at non-cosmological distances the distance and mass are perfectly degenerate.”
MethodFormation and dynamical evolution of multiple stellar generations in globular clusters
D’Ercole, A., Vesperini, E., D'Antona, F. A., McMillan, S. L. W., & Recchi, S. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13915.x · Cited by 652 · see citing works
“However if we plausibly adopt the current central relaxation time of ω Cen (∼ 1 Gyr, see e.g. Harris 1996) as an estimate of the initial half-mass relaxation time of the SG subsystem, T/trh,SG(0) ≈ 10.”
MethodPietrinferni, A., Cassisi, S., Salaris, M., & Castelli, F. (2006) · The Astrophysical Journal · doi:10.1086/501344 · Cited by 655 · see citing works
“12), who use their own SBF models, [Fe/H] and distances from the Harris (1996) catalog.”
MethodInfluentialProperties and Astrophysical Implications of the 150 M ⊙ Binary Black Hole Merger GW190521
Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., et al. (2020) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aba493 · Cited by 635 · see citing works
Helmi, A., van Leeuwen, F., McMillan, P. J., Massari, D., Antoja, T., Robin, A. C., Lindegren, L., Bastian, U., Arenou, F., Babusiaux, C., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832698 · Cited by 628 · see citing works
Fernandes, R. C., Stasińska, G., Júnior, A. M., et al. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18244.x · Cited by 620 · see citing works
The GALAH+ survey: Third data release
Buder, S., Sharma, S., Kos, J., Amarsi, A., Nordlander, T., Lind, K., Martell, S., Asplund, M., Bland-Hawthorn, J., Casey, A., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1242 · Cited by 296 · see citing works
“However, for the intermediate [Fe/H] clusters NGC 1851, NGC 288, and NGC 362 we find disagreement with Harris (1996), for which we have no explanation.”
BackgroundInfluentialCarretta, E., Bragaglia, A., Gratton, R., & Lucatello, S. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912097 · Cited by 613 · see citing works
“The resulting heliocentric RVs and associated errors (typically a few hundred m s−1) are indicated in Table 3 for individual member stars; average values for each programme cluster (with 1σ rms scatters) are listed in Table 2 with the values from the Harris (1996) updated catalogue, as a comparison.”
MethodThe dark energy survey: data release 1
Marcos Vinícius da Silva Alves de, L. I. M. A. (2018) · LA Referencia (Red Federada de Repositorios Institucionales de Publicaciones Científicas) · doi:10.3847/1538-4365/aae9f0/meta · Cited by 620 · see citing works
Nataf, D. M., Gould, A. P., Fouqué, P., Gonzalez, O. A., Johnson, J. A., Skowron, J., Udalski, A., Szymański, M. K., Kubiak, M., Pietrzyński, G., et al. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/769/2/88 · Cited by 578 · see citing works
“4As searched for using A Galactic Globular Cluster Database: http://gclusters.altervista.org/index.php, which is based on the Harris catalog (Harris 1996, 2010 edition).”
MethodInfluentialEmpirical color transformations between SDSS photometry and other photometric systems
Jordi, K., Grebel, E. K., & Ammon, K. (2006) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20066082 · Cited by 589 · see citing works
“Moreover, Stetson and the SDSS provide photometry for the surroundings of the similarly metal-poor globular clusters NGC 2419 (−2.12 dex according to Harris (1996)) and NGC 7078 (−2.26 dex; Harris (1996)).”
BackgroundInfluentialRodriguez, C. L., Chatterjee, S., & Rasio, F. A. (2016) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.93.084029 · Cited by 581 · see citing works
EIGHT NEW MILKY WAY COMPANIONS DISCOVERED IN FIRST-YEAR DARK ENERGY SURVEY DATA
Bechtol, K., Drlica-Wagner, A., Balbinot, E., Pieres, A., Simon, J. D., Yanny, B., Santiago, B., Wechsler, R. H., Frieman, J. A., Walker, A. R., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/807/1/50 · Cited by 583 · see citing works
“The resulting seed list was compared against catalogs of known star clusters (Harris 1996, 2010 edition; Kharchenko et al. 2013) and Milky Way satellite galaxies (McConnachie 2012a) as well as catalogs of other astrophysical objects that can produce false positives, such as large nearby galaxies…”
MethodSimon, J. D. (2019) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-091918-104453 · Cited by 610 · see citing works
Galactic stellar haloes in the CDM model
Cooper, A. P., Cole, S., Frenk, C. S., White, S. D. M., Helly, J., Benson, A. J., De Lucia, G., Helmi, A., Jenkins, A., Navarro, J. F., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16740.x · Cited by 594 · see citing works
“14 the surface density profile of globular clusters in the Milky Way (Harris 1996) and M31 (confirmed GCs in the Revised Bologna Catalogue – RBC v3.”
BackgroundThe Milky Way Tomography with SDSS. II. Stellar Metallicity
Ivezić, Ž., Sesar, B., Jurić, M., Bond, N., Dalcanton, J., Rockosi, C. M., Yanny, B., Newberg, H. J., Beers, T. C., Allende Prieto, C., et al. (2008) · The Astrophysical Journal · doi:10.1086/589678 · Cited by 566 · see citing works
“These radii, and distance and metallicity data from Harris (1996), are listed in Table 6.”
BackgroundMethodInfluentialBaumgardt, H., & Hilker, M. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1057 · Cited by 561 · see citing works
“For most clusters our radial velocities are also in good agreement with the values given by Harris (1996).”
BackgroundMethodResultInfluentialKoposov, S. E., Belokurov, V. A., Torrealba, G., & Evans, N. W. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/805/2/130 · Cited by 557 · see citing works
“…all detections are cross-matched with the list of positions of known dwarf galaxies from McConnachie (2012), nearby LEDA galaxies (Paturel et al. 2003) with radial velocities less than 2000km/s, globular clusters in the catalogue of Harris (1996) as well as the globular clusters listed in Simbad.”
BackgroundMeasurements of the Hubble Constant: Tensions in Perspective
Freedman, W. L. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac0e95 · Cited by 577 · see citing works
“Preliminary E(B− V ) reddening estimates and initial distance estimates were taken from Harris (1996, 2010).”
BackgroundSEARCHING FOR DARK MATTER ANNIHILATION IN RECENTLY DISCOVERED MILKY WAY SATELLITES WITH FERMI-LAT
Albert, A., Anderson, B., Bechtol, K., Drlica-Wagner, A., Meyer, M., Sánchez-Conde, M. Á., Strigari, L. E., Wood, M., Abbott, T. M. C., Abdalla, F. B., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/834/2/110 · Cited by 539 · see citing works
EIGHT ULTRA-FAINT GALAXY CANDIDATES DISCOVERED IN YEAR TWO OF THE DARK ENERGY SURVEY
Drlica-Wagner, A., Bechtol, K., Rykoff, E. S., Luque, E., Queiroz, A., Mao, Y.-Y., Wechsler, R. H., Simon, J. D., Santiago, B., Yanny, B., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/813/2/109 · Cited by 532 · see citing works
“This large half-light radius is inconsistent with the sizes of known globular clusters (Harris 1996, 2010 edition), thus making it very likely that DES J0002–6051 is a dwarf galaxy.”
BackgroundThe O-Na and Mg-Al anticorrelations in turn-off and early subgiants in globular clusters
Gratton, R., Bonifacio, P., Bragaglia, A., Carretta, E., Castellani, V., Centurion, M., Chieffi, A., Claudi, R., Clementini, G., D'Antona, F., et al. (2001) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20010144 · Cited by 526 · see citing works
“NGC 6397 is a quite small cluster (mass ∼ 105 M , from the integrated magnitude MV = −6.58, Harris 1996, and a mass-to-light ratio of ∼2, typical for a globular cluster).”
BackgroundMethodInfluentialUV-extended E-MILES stellar population models: young components in massive early-type galaxies
Vazdekis, A., Koleva, M., Ricciardelli, E., Röck, B., & Falcón‐Barroso, J. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2231 · Cited by 517 · see citing works
“The metallicities of the clusters are taken from Harris (1996).”
BackgroundSarajedini, A., Bedin, L. R., Chaboyer, B., Dotter, A., Siegel, M. H., Anderson, J., Aparicio, A., King, I. R., Majewski, S. R., Marín-Franch, A., et al. (2007) · The Astronomical Journal · doi:10.1086/511979 · Cited by 516 · see citing works
“As a result, it is difficult for us to reconcile the rather large difference of (m M )0 ¼ 1:35 mag between our distance modulus and that of Harris (1996) for E3.”
BackgroundMethodInfluentialProperties of stellar generations in globular clusters and relations with global parameters
Carretta, E., Bragaglia, A., Gratton, R., Recio-Blanco, A., Lucatello, S., D’Orazi, V., & Cassisi, S. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200913451 · Cited by 496 · see citing works
“…be only considered a second parameter, because the global distribution of stars on the HB [as indicated e.g., by the HB ratio HBR=(BR)/(B+R+V) – see Harris 1996 and web updates] is not correlated with IQR[O/Na], i.e. with the extension of the Na-O anticorrelation, as already discussed by…”
BackgroundMethodResultInfluentialFERMI/LARGE AREA TELESCOPE BRIGHT GAMMA-RAY SOURCE LIST
Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Band, D. L., Barbiellini, G., Bastieri, D., et al. (2009) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/183/1/46 · Cited by 513 · see citing works
Piotto, G., Milone, A. P., Bedin, L. R., Anderson, J., King, I. R., Marino, A. F., Nardiello, D., Aparicio, A., Barbuy, B., Bellini, A., et al. (2015) · The Astronomical Journal · doi:10.1088/0004-6256/149/3/91 · Cited by 515 · see citing works
“The final five columns in the Table give the GalacticXYZ coordinates, the reddening, and the distance modulus (from the Harris 1996 catalog, 2010 edition).”
BackgroundShetrone, M. D., Venn, K. A., Tolstoy, E., Primas, F., Hill, V., & Kaufer, A. (2003) · The Astronomical Journal · doi:10.1086/345966 · Cited by 502 · see citing works
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 · see citing works
“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).”
BackgroundTHE 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 · see citing works
“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).”
MethodThe Dark Energy Survey: Data Release 1
Abbott, T. M. C., Abdalla, F. B., Allam, S., Amara, A., Annis, J. T., Asorey, J., Avila, S., Ballester, O., Banerji, M., Barkhouse, W., et al. (2018) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/aae9f0 · Cited by 491 · see citing works
“Table 5 lists five classical globular clusters within the DES DR1 footprint with integrated V-band magnitude brighter than 10 (Harris 1996, 2010 edition).”
BackgroundA 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 · see citing works
“…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).”
BackgroundTHE 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 · see citing works
“Column 6 lists the Galactocentric distance (rGC, in kpc), taken from Harris (1996).”
MethodVandenBerg, D. A., Brogaard, K., Leaman, R., & Casagrande, L. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/775/2/134 · Cited by 487 · see citing works
“…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.”
BackgroundMethodInfluentialOdenkirchen, M., Grebel, E. K., Rockosi, C. M., Dehnen, W., Ibata, R., Rix, H., Stolte, A., Wolf, C., Anderson, J. E., Bahcall, N. A., et al. (2001) · The Astrophysical Journal · doi:10.1086/319095 · Cited by 489 · see citing works
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 · see citing works
“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).”
BackgroundMethodInfluentialThe 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 483 · see citing works
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 · see citing works
“…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.”
MethodInfluentialGaia 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 · see citing works
“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.”
BackgroundMilone, A. P., Piotto, G., Renzini, A., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2531 · Cited by 477 · see citing works
“All these quantities are taken from the 2010 edition of the Harris (1996) catalog.”
BackgroundMurray, N., Quataert, E., & Thompson, T. A. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/709/1/191 · Cited by 476 · see citing works
“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).”
BackgroundSpace 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 · see citing works
“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).”
BackgroundDotter, 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 · see citing works
“From the Harris (1996) catalog, we extracted central luminosity density (ρ0).”
BackgroundMethodInfluentialSwings 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 · see citing works
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 · see citing works
“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.”
BackgroundResultZoccali, 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 · see citing works
“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.”
MethodInfluentialThe 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 · see citing works
“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).”
MethodMiller, M. C., & Colbert, E. J. M. (2004) · International Journal of Modern Physics D · doi:10.1142/s0218271804004426 · Cited by 449 · see citing works
“…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…”
BackgroundPeng, 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 · see citing works
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 · see citing works
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 · see citing works
Baumgardt, H., Hilker, M., Sollima, A., & Bellini, A. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2997 · Cited by 436 · see citing works
“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).”
MethodResultInfluentialTHE 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 · see citing works
“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).”
BackgroundRevised 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 · see citing works
“…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…”
BackgroundProperties 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 · see citing works
“For comparison, we have also included the LF for Milky Way globular clusters (shown with dots), using data from Harris (1996).”
BackgroundMethodInfluentialCalibration 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 · see citing works
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 · see citing works
“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.”
BackgroundMethodInfluentialMapping 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 · see citing works
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 · see citing works
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 · see citing works
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 · see citing works
“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.”
MethodMERGING 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 · see citing works
“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…”
MethodResultInfluentialPhotospheric 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 · see citing works
“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-citationTHE 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 · see citing works
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 382 · see citing works
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 · see citing works
“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).”
BackgroundMethodInfluentialNeumayer, N., Seth, A., & Böker, T. (2020) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-020-00125-0 · Cited by 374 · see citing works
- 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)
- 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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