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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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Items 201–300 of 1,002
The second and third parameters of the horizontal branch in globular clusters
Gratton, R., Carretta, E., Bragaglia, A., Lucatello, S., & D’Orazi, V. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912572 · Cited by 233
“When making this derivation, w simply used the HB level listed by Harris (1996).”
MethodInfluentialGuillot, S., Servillat, M., Webb, N. A., & Rutledge, R. E. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/772/1/7 · Cited by 325
“…distances, distance modulii, etc.) • The GC M28 does not have a dynamical distance measurement, but its distance has been estimated in different works: 5.1±0.5 kpc (Rees & Cudworth 1991), 4.8–5.0 kpc (Davidge et al. 1996) and 5.5 kpc (Harris 1996; Testa et al. 2001), all using photometric methods.”
BackgroundMethodResultInfluentialOn the formation of globular cluster systems in a hierarchical Universe
Beasley, M., Baugh, C. M., Forbes, D. A., Sharples, R. M., & Frenk, C. S. (2002) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2002.05402.x · Cited by 232
“We calculate total numbers of GCs (since we do not have explicit luminosity information), and adopt a mean GC mass, 〈MGC〉, corresponding to that of the Milky Way GC system of ∼ 3.0 × 105M⊙ (from the McMaster catalogue of Harris 1996; May 15th, 1997 version).”
MethodInfluentialGaia Data Release 2 Specific characterisation and validation of all-sky Cepheids and RR Lyrae stars
Clementini, G., Ripepi, V., Molinaro, R., Garofalo, A., Muraveva, T., Rimoldini, L., Guy, L. P., Jevardat de Fombelle, G., Nienartowicz, K., Marchal, O., et al. (2019) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · doi:10.1051/0004-6361/201833374 · Cited by 4
galev evolutionary synthesis models - I. Code, input physics and web interface
Kotulla, R., Alvensleben, U. F., Weilbacher, P. M., Anders, P., & the galev team (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.14717.x · Cited by 232
“…and Lilly & Fritze (2006), Lick indices for SSPs as calculated by galev agree well with Galactic and M31 globular cluster data as compiled by (Harris 1996) in his online catalog1 . galev models for star clusters also show good agreement at an evolutionary age of ∼ 12 − 13 Gyr with the…”
MethodAnderson, J., & van der Marel, R. P. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/710/2/1032 · Cited by 231
“Harris (1996) reports (13:26.45.9, −47:28:37) for the center in his on-line catalog. van Leeuwen et al. (2000) found a center of (13:26:45.756, −47:28:42.780) using the positions of the giant stars brighter than B = 16.”
BackgroundMethodInfluentialDetailed abundances of a large sample of giant stars in M 54 and in the Sagittarius nucleus
Carretta, E., Bragaglia, A., Gratton, R., Lucatello, S., Bellazzini, M., Catanzaro, G., Leone, F., Momany, Y., Piotto, G., & D’Orazi, V. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014924 · Cited by 226
“We note that almost all these stars are well within the the tidal radius of M 54 (7.47 arcmin, Harris 1996).”
BackgroundInfluentialTHE NUCLEUS OF THE SAGITTARIUS DSPH GALAXY AND M54: A WINDOW ON THE PROCESS OF GALAXY NUCLEATION
Bellazzini, M., Ibata, R., Chapman, S. C., Mackey, D., Monaco, L., Irwin, M. J., Martin, N. F., Lewis, G. F., & Dalessandro, E. (2008) · The Astronomical Journal · doi:10.1088/0004-6256/136/3/1147 · Cited by 229
“Particularly noticeable, however, is the very bright (MV = −10.0, Harris 1996) metal-poor ([Fe/H ] = −1.55) (Brown, Wallerstein & Gonzalez 1999) globular cluster M54 (NGC6715), located exactly at the center of the light distribution of the Sgr galaxy.”
BackgroundInfluentialThe Dark Matter Crisis: Falsification of the Current Standard Model of Cosmology
Kroupa, P. (2012) · Publications of the Astronomical Society of Australia · doi:10.1071/as12005 · Cited by 230
“Considering the GCs of the MW these can be differentiated into the bulge and disk (BD) GCs, into the old halo (OH) GCs and into the young halo (YH) GCs (Mackey & van den Bergh 2005 for the classification; Harris 1996, 2003 update, for positional data).”
Galactic Globular Cluster Relative Ages
Rosenberg, A., Saviane, I., Piotto, G., & Aparicio, A. (1999) · The Astronomical Journal · doi:10.1086/301089 · Cited by 229
“All the other cluster parameters used in this paper have been extracted from Harris (1996), in the revised version of 2003.”
MethodAbundances in a Large Sample of Stars in M3 and M13
Cohen, J. G., & Meléndez, J. (2004) · The Astronomical Journal · doi:10.1086/426369 · Cited by 224
“We adopt current values from the online database of Harris (1996) for the distances of 10.4 (7.5) kpc for M3 (M13) with a reddening of E(B V ) ¼ 0:01 (0.02) mag.”
BackgroundMethodInfluentialQuantifying the coexistence of massive black holes and dense nuclear star clusters
Graham, A. W., & Spitler, L. R. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15118.x · Cited by 229
Böker, T., Sarzi, M., McLaughlin, D. E., van der Marel, R. P., Rix, H., Ho, L. C., & Shields, J. C. (2004) · The Astronomical Journal · doi:10.1086/380231 · Cited by 228
“8 The Milky Way GC data are taken from the February 2003 version of the online catalog compiled by Harris (1996), which contains 141 clusters with known values for angular half-light radius and heliocentric distance, King concentration index, absolute V-band magnitude, and (B V ) color and excess.”
BackgroundMethodNEW LIMITS ON AN INTERMEDIATE-MASS BLACK HOLE IN OMEGA CENTAURI. II. DYNAMICAL MODELS
van der Marel, R. P., & Anderson, J. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/710/2/1063 · Cited by 227
Korn, A. J., Grundahl, F., Richard, O., Mashonkina, L., Barklem, P. S., Collet, R., Gustafsson, B., & Piskunov, N. (2007) · The Astrophysical Journal · doi:10.1086/523098 · Cited by 220
“NGC 6397 has a non-negligible reddening and several estimates are available in the literature (Harris 1996).”
BackgroundResultInfluentialA detached stellar-mass black hole candidate in the globular cluster NGC 3201
Giesers, B., Dreizler, S., Husser, T.-O., et al. (2017) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slx203 · Cited by 223
“Since the Sun’s distance to the globular cluster NGC 3201 is 4.9 kpc (Harris 1996), the orbital movement of the target star is of the order of 0.2 mas.”
BackgroundMethodResultInfluentialSiegel, M. H., Dotter, A., Majewski, S. R., Sarajedini, A., Chaboyer, B., Nidever, D. L., Anderson, J., Marín-Franch, A., Rosenberg, A., Bedin, L. R., et al. (2007) · The Astrophysical Journal · doi:10.1086/522003 · Cited by 219
“INTRODUCTION M54 (NGC 6715) is the second most massive Galactic globular cluster and, at first blush, a canonical “old halo” cluster: ancient, metal-poor, and with a very extended blue horizontal branch (HB; Harris 1996).”
BackgroundTHE LEAST-LUMINOUS GALAXY: SPECTROSCOPY OF THE MILKY WAY SATELLITE SEGUE 1
Geha, M., Willman, B., Simon, J. D., Strigari, L. E., Kirby, E. N., Law, D. R., & Strader, J. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/692/2/1464 · Cited by 233
“The metallicity of the single RGB star in our sample if [Fe/H] = −3.3 dex, well below that of any known globular cluster (Harris 1996).”
BackgroundInfluentialHarris, W. E., Whitmore, B. C., Karakla, D., Okoń, W., Baum, W. A., Hanes, D. A., & Kavelaars, J. J. (2005) · The Astrophysical Journal · doi:10.1086/498058 · Cited by 219
“However, the red-cluster population clearly exhibits a much larger internal dispersion in the giant ellipticals than in the Milky Way, perhaps reflecting the series of major mergers and starbursts that the galaxy was built from in a hierarchical-merging scenario (e.g., Beasley et al. 2002, 2003).”
BackgroundMethodInfluentialSelf-citationOn the metallicity of open clusters
Netopil, M., Paunzen, E., Heiter, U., et al. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201526370 · Cited by 221
“From the UB Vc sample we excluded Berkeley 42, which is a globular cluster (Harris 1996).”
BackgroundKamann, S., Husser, T.-O., Dreizler, S., et al. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2719 · Cited by 220
“A comparison of the dynamical distances to the values of Harris (1996) is shown in Fig.”
BackgroundMethodInfluentialWillman, B., & Strader, J. (2012) · The Astronomical Journal · doi:10.1088/0004-6256/144/3/76 · Cited by 234
Precession of the Sagittarius stream
Belokurov, V. A., Koposov, S. E., Evans, N. W., Peñarrubia, J., Irwin, M. J., Smith, M. C., Lewis, G. F., Gieles, M., Wilkinson, M. I., Gilmore, G. F., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1862 · Cited by 221
“While our slightly higher distance estimate is mildly inconsistent with the value provided by Harris (1996), we are in agreement with the most recent RR Lyrae measurement by Di Criscienzo et al. (2011).”
BackgroundResultInfluentialThe Gaia -ESO Survey: The analysis of high-resolution UVES spectra of FGK-type stars
Smiljanić, R., Korn, A. J., Bergemann, M., Frasca, A., Magrini, L., Masseron, T., Pancino, E., Ruchti, G. R., Roman, I. S., Sbordone, L., et al. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201423937 · Cited by 215
Mass and shape of the Milky Way’s dark matter halo with globular clusters from Gaia and Hubble
Posti, L., & Helmi, A. (2019) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201833355 · Cited by 233
“For both sets of clusters we compute heliocentric distances s from the (extinction-corrected) distance moduli in the V-band, taken from the latest version of the catalogue compiled by Harris (1996), and we assume the uncertainty to be 0.05 mag for each object.”
BackgroundMethodInfluentialON THE SHOULDERS OF GIANTS: PROPERTIES OF THE STELLAR HALO AND THE MILKY WAY MASS DISTRIBUTION
Kafle, P. R., Sharma, S., Lewis, G. F., & Bland-Hawthorn, J. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/794/1/59 · Cited by 215
“The distance moduli are taken to be 14.64 for M92, 14.38 for M13 (Carretta et al. 2000), 12.86 for M71 (Grundahl et al. 2002) and 13.02 for NGC6791 (Harris 1996).”
InfluentialThe luminosity function of the Milky Way satellites
Koposov, S. E., Belokurov, V. A., Evans, N. W., Hewett, P. C., Irwin, M. J., Gilmore, G. F., Zucker, D. B., Rix, H., Fellhauer, M., Bell, E. F., et al. (2008) · Max Planck Institute for Plasma Physics · Cited by 215
Milone, A. P., Marino, A. F., Renzini, A., D'Antona, F. A., Anderson, J., Barbuy, B., Bedin, L. R., Bellini, A., Brown, T. M., Cassisi, S., et al. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2573 · Cited by 217
Photospheric radius expansion X-ray bursts as standard candles
Erik Kuulkers, A., den Hartog, P. R., Zand, J. J. M. I. ’., et al. (2002) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361:20021781/pdf · Cited by 215
Self-citationThe Ages and Abundances of a Large Sample of M87 Globular Clusters
Cohen, J. G., Blakeslee, J. P., & Ryzhov, A. (1998) · The Astrophysical Journal · doi:10.1086/305429 · Cited by 214
“The UBV RI colors for the galactic globular clusters are taken from the compilation of Harris (1996).”
MethodMyeong, G. C., Evans, N. W., Belokurov, V., Sanders, J. L., & Koposov, S. E. (2018) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aad7f7 · Cited by 213
Mackey, A. D., & Gilmore, G. F. (2004) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2004.08343.x · Cited by 213
“We have also filled out the database of HB indices, and structural and metallicity measurements provided by Harris (1996) for the Galactic globular clusters, by using a combination of literature results and new calculations.”
BackgroundMethodInfluentialGrundahl, F., Catelan, M., Landsman, W. B., Stetson, P. B., & Andersen, M. I. (1999) · The Astrophysical Journal · doi:10.1086/307807 · Cited by 220
“The cluster metallicity [Fe/H], reddening E(B[V ), core concentration c, log of the central density (ino c L _pc~3), and Galactocentric distance (in kpc) are given inRGCcolumns (3)È(7) (data from Harris 1996).”
BackgroundA Second Galaxy Missing Dark Matter in the NGC 1052 Group
van Dokkum, P., Danieli, S., Abraham, R. G., Conroy, C., & Romanowsky, A. J. (2019) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab0d92 · Cited by 243
ARGOS – IV. The kinematics of the Milky Way bulge
Ness, M., Freeman, K. C., Athanassoula, E., Boer, E. W.-D., Bland‐Hawthorn, J., Asplund, M., Lewis, G. F., Yong, D., Lane, R. R., Kiss, L. L., et al. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt533 · Cited by 210
Baumgardt, H. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2488 · Cited by 213
“The literature distances were taken mostly from Ferraro et al. (1999), however we obtain a similar difference when using the Harris (1996) distances.”
MethodA DeepChandraSurvey of the Globular Cluster 47 Tucanae: Catalog of Point Sources
Heinke, C. O., Grindlay, J. E., Edmonds, P. D., et al. (2005) · The Astrophysical Journal · doi:10.1086/429899 · Cited by 212
“The globular cluster 47 Tuc is massive (M 106 M , Pryor & Meylan 1993) and of relatively high stellar concentration, although not core collapsed (Harris 1996).”
The ACS Survey of Galactic Globular Clusters. XII. Photometric Binaries along the Main-SequencePreprint
Milone, A. P., Piotto, G., Bedin, L. R., et al. (2011) · arXiv (Cornell University) · doi:10.48550/arxiv.1111.0552 · Cited by 212
“…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.”
MethodInfluentialAccreted versus in situ Milky Way globular clusters
Forbes, D. A., & Bridges, T. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16373.x · Cited by 310
“2 we compare the metallicity distribution for 148 GCs from the latest version of the Harris (1996) catalogue with our final sample.”
BackgroundMethodModeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog
Kremer, K., Ye, C. S., Rui, N. Z., et al. (2020) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ab7919 · Cited by 211
“In Figure 2, we compare various features of our models to the MW GC data taken from Baumgardt & Hilker (2018).8 The size of the circle coinciding with a given MW cluster is scaled by the integrated V-band magnitude of that cluster (taken from Harris 1996).”
BackgroundMethodResultInfluentialA helium spread among the main sequence stars in NGC 2808Preprint
Bellazzini, M., Caloi, V., Pecci, F. F., et al. (2005) · Cited by 211
Helmi, A., Irwin, M. J., Tolstoy, E., Battaglia, G., Hill, V., Jablonka, P., Venn, K., Shetrone, M. D., Letarte, B., Arimoto, N., et al. (2006) · The Astrophysical Journal · doi:10.1086/509784 · Cited by 205
“This conjecture would also seem to be supported by the metallicity distribution of Galactic halo globular clusters which does not extend below−2.4 dex (e.g. Harris 1996).”
BackgroundInfluentialThe evolution of binary fractions in globular clusters
Ivanova, N., Belczyński, K., Fregeau, J. M., et al. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.08804.x · Cited by 210
“For this cluster we adopted a core mass of105M⊙ and a total cluster mass of106M⊙ at present (Freire et al. 2001); we also taketrh = 109 yr (Harris 1996) and an age of11Gyr (Gratton et al. 2003).”
MethodPancino, E., Carrera, R., Rossetti, E., et al. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200912965 · Cited by 210
“The resolution of their spectra (R 10000) was much lower than ours, but if we trust their analysis in a relative sense, and consider more recent metallicity estimates for 47 Tuc and M 71 (–0.76 and –0.73 respectively, Harris, 1996), we would then place NGC 2420 around [Fe/H]≃–0.1 or –0.2.”
BackgroundInfluentialDistances and Metallicities of High- and Intermediate-Velocity Clouds
Wakker, B. P. (2001) · CERN Document Server (European Organization for Nuclear Research) · Cited by 210
The GALAH survey: observational overview and Gaia DR1 companion
Martell, S. L., Sharma, S., Buder, S., Duong, L., Schlesinger, K. J., Simpson, J. D., LIND, K., Ness, M., Marshall, J. P., Asplund, M., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2835 · Cited by 209
“Table 2 lists coordinates, distance moduli, metallicity (taken from Harris 1996, 2010 edition for the globular clusters and Heiter et al. 2014 for M67), number of stars observed, V magnitude range, exposure time, and dates of observation for all of the globular and open clusters observed in this…”
BackgroundThe Distribution Of Heavy Elements In Spiral And Elliptical Galaxies
Henry, R. B. C., & Worthey, G. (1999) · CERN Document Server (European Organization for Nuclear Research) · Cited by 209
Battaglia, G., Irwin, M. J., Tolstoy, E., et al. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12532.x · Cited by 208
The structure and environment of young stellar clusters in spiral galaxies
Larsen, S. S. (2004) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20034533 · Cited by 208
“Using data from the compilation by Harris (1996), the median Reff is 3.0 pc. Similarly, the diameters and masses of Galactic open clusters show no strong correlation, with typical sizes only slightly smaller than those of globular clusters (Janes et al. 1988).”
MethodInfluentialChemical tagging with APOGEE: discovery of a large population of N-rich stars in the inner Galaxy
Schiavon, R. P., Zamora, O., Carrera, R., Lucatello, S., Robin, A. C., Ness, M., Martell, S. L., Smith, V. V., García-Hernández, D. A., Manchado, A., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2162 · Cited by 206
“The bottom panel shows the MDF of Galactic GCs included in the 2010 version of the Harris catalog (Harris 1996).”
BackgroundDISSIPATIONLESS FORMATION AND EVOLUTION OF THE MILKY WAY NUCLEAR STAR CLUSTER
Antonini, F., Capuzzo‐Dolcetta, R., Mastrobuono-Battisti, A., & Merritt, D. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/750/2/111 · Cited by 217
A Multicolor and Fourier Study of RR Lyrae Variables in the Globular Cluster NGC 5272 (M3)
Cacciari, C., Corwin, T. M., & Carney, B. W. (2004) · The Astronomical Journal · doi:10.1086/426325 · Cited by 204
“It is located at ∼ 11.9 kpc from the Galactic centre, 10.0 kpc from the Sun and 9.7 kpc above the Galactic plane (Harris 1996).”
BackgroundMethodInfluentialIvans, I. I., Kraft, R. P., Sneden, C., Smith, G. H., Rich, R. M., & Shetrone, M. D. (2001) · The Astronomical Journal · doi:10.1086/322108 · Cited by 201
A systematic survey for infrared star clusters with b < 20 using 2MASS
Froebrich, D., Scholz, A., & Raftery, C. L. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.11148.x · Cited by 203
“Of the∼ 150 GlCls known in our Galaxy (e.g., Harris (1996)), only very few have been discovered using infrared data (e.g., Hurt et al. (2000), Kobulnicky et al. (2005)).”
BackgroundAn intermediate-mass black hole in the centre of the globular cluster 47 Tucanae
Kızıltan, B., Baumgardt, H., & Loeb, A. (2017) · Nature · doi:10.1038/nature21361 · Cited by 203
A MegaCam Survey of Outer Halo Satellites. III. Photometric and Structural Parameters* †
Muñoz, R. R., Côté, P., Santana, F. A., Geha, M., Simon, J. D., Oyarzún, G. A., Stetson, P. B., & Djorgovski, S. G. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aac16b · Cited by 224
“Finally, Figure 5 shows that our effective radii are often larger than the half-light values reported in Harris (1996).”
BackgroundMethodResultInfluentialThe two metallicity groups of the globular cluster M 22: a chemical perspective
Marino, A. F., Sneden, C., Kraft, R. P., et al. (2011) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201116546 · Cited by 202
“…spectroscopic gravities determined from Fe I/Fe II ionization equilibrium (log gadopted) as a function of gravities log gphotometry that were obtained with standard relations by using T(V−K), bolometric corrections from Alonso et al. (1999), and a distance modulus of (m − M)V = 13.60 (Harris 1996).”
MethodInfluentialFrew, D. J., Parker, Q. A., & Bojičić, I. S. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1516 · Cited by 201
Bellini, A., Anderson, J., van der Marel, R. P., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/797/2/115 · Cited by 201
“The velocity distribution of NGC 7078 in the central∼ 45′′ (comparable to the half-light radiusrh = 60′′; Harris 1996, 2010 edition) is close to isotropic.”
BackgroundThe star cluster population of M 51
Bastian, N., Gieles, M., Lamers, H. J. G. L. M., Scheepmaker, R. A., & de Grijs, R. (2005) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20041078 · Cited by 220
GLOBULAR CLUSTER STREAMS AS GALACTIC HIGH-PRECISION SCALES—THE POSTER CHILD PALOMAR 5
Küpper, A. H. W., Balbinot, E., Bonaca, A., Johnston, K. V., Hogg, D. W., Kroupa, P., & Santiago, B. X. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/803/2/80 · Cited by 228
“Harris (1996) lists a distance of 23.2 kpc, which is based on CCD photometry by Smith et al. (1986).”
BackgroundMethodInfluentialBlack holes and core expansion in massive star clusters
Mackey, D., Wilkinson, M. I., Davies, M. B., & Gilmore, G. F. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13052.x · Cited by 199
The formation of ultracompact dwarf galaxies
Fellhauer, M., & Kroupa, P. (2002) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2002.05087.x · Cited by 199
CO-EVOLUTION OF GALACTIC NUCLEI AND GLOBULAR CLUSTER SYSTEMS
Gnedin, O. Y., Ostriker, J. P., & Tremaine, S. D. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/785/1/71 · Cited by 221
“More relevant is the consistency of the predicted final distribution with the observed one (from Harris 1996, the updated 2010 edition is at http://physwww.mcmaster.ca/∼harris/mwgc.dat).”
BackgroundHelmi, A., Morrison, H., Harding, P., Olszewski, E. W., Mateo, M., Freeman, K. C., Norris, J. E., & Shectman, S. A. (2008) · Cited by 229
Compact binaries in star clusters - I. Black hole binaries inside globular clusters
Downing, J. M. B., Benacquista, M., Giersz, M., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17040.x · Cited by 197
“The properties of these clusters are obtained from Harris (1996), and are shown in Table 4.”
MethodAbundances of Baade's Window Giants from Keck/HIRES Spectra: II. The Alpha- and Light Odd Elements
Fulbright, J. P., McWilliam, A., & Rich, R. M. (2006) · CERN Document Server (European Organization for Nuclear Research) · Cited by 196
THE TIMING OF NINE GLOBULAR CLUSTER PULSARS
Lynch, R. S., Freire, P. C. C., Ransom, S. M., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/745/2/109 · Cited by 195
Massive Black Holes in Star Clusters. II. Realistic Cluster Models
Baumgardt, H., Makino, J., & Ebisuzaki, T. (2004) · The Astrophysical Journal · doi:10.1086/423299 · Cited by 195
“Projected half-light radii of galactic globular clusters are taken from Harris (1996).”
BackgroundKirby, E. N., Guhathakurta, P., Simon, J. D., Geha, M., Rockosi, C. M., Sneden, C. A., Cohen, J. G., Sohn, S. T., Majewski, S. R., & Siegel, M. H. (2010) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/191/2/352 · Cited by 193
Relativistic Binaries in Globular Clusters
Benacquista, M. J., & Downing, J. M. B. (2013) · Living Reviews in Relativity · doi:10.12942/lrr-2013-4 · Cited by 194
Bellini, A., Anderson, J., & Bedin, L. R. (2011) · Publications of the Astronomical Society of the Pacific · doi:10.1086/659878 · Cited by 193
The mass of the Milky Way: Limits from a newly assembled set of halo objects
Sakamoto, T., Chiba, M., & Beers, T. C. (2003) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20021499 · Cited by 194
“For the globular clusters, we adopt the information provided by Harris (1996), including their positions and heliocentric radial velocities, their metal abundances, [Fe/H], and the apparent magnitude of the clusters’ horizontal branch (HB).”
MethodThe Halo Stars in NGC 5128. III. An Inner Halo Field and the Metallicity Distribution
Harris, W. E., & Harris, G. L. H. (2002) · The Astronomical Journal · doi:10.1086/340466 · Cited by 193
Self-citationStellar population models at high spectral resolutionPreprint
Maraston, C., & Strömbäck, G. (2016) · Cited by 193
Eight New Millisecond Pulsars in NGC 6440 and NGC 6441
Freire, P. C. C., Ransom, S. M., Bégin, S., et al. (2008) · The Astrophysical Journal · doi:10.1086/526338 · Cited by 192
“670 We calculated c for all Galactic GCs with the central luminosity densities and core radii given in Harris (1996),9 assuming a constant conversion factor between central luminosity density and central mass density.”
MethodTarget Selection For The Apache Point Observatory Galactic Evolution Experiment (APOGEE)
Wilson, J. C. (2016) · Repository of the Academy's Library (Library of the Hungarian Academy of Sciences) · doi:10.15781/t2d51w · Cited by 188
Ferraro, F. R., Montegriffo, P., Origlia, L., et al. (2000) · The Astronomical Journal · doi:10.1086/301269 · Cited by 190
“The reddening corrections have been computed using the latest compilation by Harris (1996).”
BackgroundMethodAccreted versus in situ Milky Way globular clustersPreprint
Forbes, D. A., & Bridges, T. J. (2024) · doi:10.25916/sut.26218271 · Cited by 190
Two distinct sequences of blue straggler stars in the globular cluster M 30
Ferraro, F. R., Beccari, G., Dalessandro, E., et al. (2009) · Nature · doi:10.1038/nature08607 · Cited by 188
The AIMSS Project – I. Bridging the star cluster–galaxy divide★†‡§¶
Norris, M. A., Kannappan, S. J., Forbes, D. A., Romanowsky, A. J., Brodie, J. P., Faifer, F. R., Huxor, A. P., Maraston, C., Moffett, A. J., Penny, S. J., et al. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1186 · Cited by 188
“We include the MV and Re values for MW GCs from Brodie et al. (2011) and add the measured central velocity dispersions of the clusters from Harris (1996) (2010 edition).”
MethodDotter, A., Sarajedini, A., & Anderson, J. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/738/1/74 · Cited by 209
“…Camera 2 (WFPC2) photometry to derive the ages of GCs with RGC > 50 kpc. Harris et al. (1997) presented deep photometry of NGC 2419 (RGC ∼ 90 kpc; Harris 1996, 2010 revision) and concluded that it is coeval with the similarly metal-poor GC M92 based on a differential comparison of their…”
BackgroundArendt, R. G., Odegard, N., Weiland, J. L., Sodroski, T. J., Hauser, M. G., Dwek, E., Kelsall, T. J., Moseley, S. H., Silverberg, R. F., Leisawitz, D., et al. (1998) · The Astrophysical Journal · doi:10.1086/306381 · Cited by 186
Milone, A. P., Marino, A. F., Piotto, G., et al. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/808/1/51 · Cited by 187
“We assumed for NGC 2808 a metallicity of [Fe/ H] = −1.14 (Harris 1996, 2010 edition), an average reddening E(B V- ) = 0.19 (Bedin et al. 2000) and a distance modulus m M( ) 15.59V- = (Harris 1996, 2010 edition).”
InfluentialA general catalogue of extended objects in the Magellanic System
Bica, E., Bonatto, C., Dutra, C. M., et al. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13612.x · Cited by 187
“Additionally, we consider as well the tidal radii of 11 faint GCs (not included in Harris 1996) derived by Bonatto & Bica (2008), and the recently studied GC FSR 1767 (Bonatto et al. 2007).”
MethodComplexity on Small Scales: The Metallicity Distribution of the Carina Dwarf Spheroidal Galaxy
Koch, A., Grebel, E. K., Wyse, R. F. Ġ., et al. (2006) · The Astronomical Journal · doi:10.1086/499490 · Cited by 186
“For this object, different values for [Fe/H] are found in the literature, reaching from −1.37dex (Rutledge et al. 1997b on the CG scale) to −1.69dex (loc. cit., ZW-scale), whereas Harris (1996) cites an average metallicity of −1.57dex from all available sources.”
BackgroundSpectroscopic ages and metallicities of stellar populations: validation of full spectrum fitting
Koleva, M., Prugniel, P., Ocvirk, P., et al. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.12908.x · Cited by 184
“We adopted the limit between the red and the blue HB morphology clusters at HBR > −0.5 in order to attach clusters like NGC 2808 (HBR = −0.49, Harris 1996) known to have blue tail (Castellani et al. 2006) to the ’blue’ group.”
BackgroundMethodInfluentialVandenBerg, D. A. (2000) · The Astrophysical Journal Supplement Series · doi:10.1086/313404 · Cited by 184
“But therein lies a problem: Harris (1996) gives E(B[V )\ 0.02 mag for NGC 1851 while a reddening of 0.034 mag is obtained from the SFD maps.”
BackgroundMethodInfluentialMcLaughlin, D. E., Anderson, J., Meylan, G., et al. (2006) · The Astrophysical Journal Supplement Series · doi:10.1086/505692 · Cited by 183
“Thus, while the new values of r0 andµV,0 here are formally slightly smaller and brighter than the “standard” values in the literature (e.g., Harris 1996; Howell, Guhathakurta, & Gilliland 2000), the differences are at the∼ 1-σ level.”
ResultTHE COEVOLUTION OF NUCLEAR STAR CLUSTERS, MASSIVE BLACK HOLES, AND THEIR HOST GALAXIES
Antonini, F., Barausse, E., & Silk, J. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/812/1/72 · Cited by 102
“The NSC half-light radii scale with their total mass roughly as r M ,h NSC 0.5~ while globular clusters have r 3 pch » irrespective of their luminosity, albeit with a large scatter (Harris 1996).”
BackgroundMethodInfluentialThe star formation and chemical evolution history of the Fornax dwarf spheroidal galaxy
de Boer, T. J. L., Tolstoy, E., Hill, V., et al. (2012) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201219547 · Cited by 183
Geha, M., Guhathakurta, P., & van der Marel, R. P. (2002) · The Astronomical Journal · doi:10.1086/344764 · Cited by 183
Ventura, P., & D'Antona, F. A. (2009) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200811139 · Cited by 181
Paving the way for the JWST: witnessing globular cluster formation at z > 3
Vanzella, E., Calura, F., Meneghetti, M., et al. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx351 · Cited by 182
“It is known that the MW is surrounded by N 150 GCs (Harris 1996), whereas Bellini et al. (2015) have identified almost N 2000 GCs in the core of M87.”
BackgroundCapozzi, F., & Raffelt, G. G. (2020) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.102.083007 · Cited by 183
“[14] W. E. Harris, A catalog of parameters for globular clusters in the Milky Way, Astron.”
BackgroundInfluentialGlobular cluster system and Milky Way properties revisited
Bica, E., Bonatto, C., Barbuy, B., & Ortolani, S. (2006) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20054351 · Cited by 178
“Harris (1996), as updated1 in 2003 (and references therein), compiled parameters of GCs that we adopt as the starting point for this work.”
MethodSamsing, J., & D’Orazio, D. J. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2334 · Cited by 181
“The following results are derived using the method described above, applied to the scenario for which the interacting BHs are identical, with a mass 30M⊙ , and for which the population of GCs all have an escape velocity of 50 kms−1 (e.g., Harris 1996).”
MethodTHE SHAPE OF THE INNER MILKY WAY HALO FROM OBSERVATIONS OF THE PAL 5 AND GD–1 STELLAR STREAMS
Bovy, J., Bahmanyar, A., Fritz, T. K., & Kallivayalil, N. (2016) · The Astrophysical Journal · doi:10.3847/1538-4357/833/1/31 · Cited by 208
“Measurements of the distance to the Pal 5 cluster range from 20.9 kpc to 23.2 kpc (Harris 1996; Vivas & Zinn 2006; Dotter et al. 2011) and we conservatively assume a flat prior on the distance between 20 kpc and 24 kpc.”
MethodInfluentialUltracompact Dwarf Galaxies in the Fornax Cluster
Phillipps, S., Drinkwater, M. J., Gregg, M. D., et al. (2001) · The Astrophysical Journal · doi:10.1086/322517 · Cited by 180
Analysis of the Quiescent Low‐Mass X‐Ray Binary Population in Galactic Globular Clusters
Heinke, C. O., Grindlay, J. E., Lugger, P. M., et al. (2003) · The Astrophysical Journal · doi:10.1086/378885 · Cited by 180
“Physical quantities are from the catalog of Harris 1996, updated 20034, with a few additional updates, principally core radii and distances (referenced).”
BackgroundMethodResultInfluential
Metadata
- 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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