A Catalog of Parameters for Globular Clusters in the Milky Way

“…e.g., the Galaxy, M31, M87, and old elliptical galaxies, the CLF shape is well-established: it is roughly Gaussian, with the peak or turnover magnitude at M0V ≃ −7.4 mag and a Gaussian FWHM of ∼ 3 mag (Whitmore et al. 1995, Harris 1996, 2001, Ashman & Zepf 1998, Harris, Harris & McLaughlin 1998).”

“This is much bluer than typical old globular clusters, which have The uniformity of(B[R)0D 1.2 (Harris 1996).the colors suggests that the clusters were formed in a single burst of relatively short duration rather than an ongoing or continuous process. shows the magnitude andFigure 5 color evolution…”

“These values are larger than the values listed in the Harris (1996) catalogue and those given by McLaughlin & van der Marel (2005).”

“Median magnitudes were transformed into masses using a Darthmouth isochrone (Dotter et al. 2008) with [Fe/H]=−1.26, E(B−V )=0.06, primordial He abundance, and age of 11.46 Gyr (as in, e.g., WagnerKaiser et al. 2017).”

“We then distributed the half-mass radius of GCs at present-day by using a log-normal distribution with parameters 〈rh〉 = 6.1 pc and σ = 0.63 which give a best-fit with the distribution of Harris (1996) GGCs in the MGC-ρh plane.”

“An average Galactic GC today has a half-mass radius of ≈4 pc and a total mass of 4 × 104 M (Harris 1996, 2003 revision, assuming a mass-to-light ratio of 1.5), resulting in a stellar mass density within rh of ≈70 M pc−3.”

“The reddenings and V magnitudes of the horizontal branches of the globular clusters were adopted from either the photometric catalogs or from the 1999 version of the compilation by Harris (1996).”

“Canterna (1977) with reddenings from Harris (1996), the GCs of M87 (data from Hanes et al. 2001) and those of M49 (data from Geisler, Lee & Kim 1996), adopting the reddenings for M87 and for M49 from Schlegel, Finkbeiner & Davis (1998).”

“The σobs for Milky Way GCs from Pryor & Meylan (1993), along with absolute magnitudes (MV ) listed by Harris (1996) are plotted as open circles.”

“NGC 6440 is a globular cluster near the Galactic Center, at a distance of 8.5 kpc (Ortolani et al. 1994), with NH = 5.9 × 10 21 cm−2 (Harris 1996).”

“The spatial structure of GCs has been extensively studied within the Local Group, leading to the discovery of numerous scaling relations (Trager, King & Djorgovski 1995; Harris 1996) and the constraining of the GC fundamental plane (Djorgovski & Meylan 1994; McLaughlin 2000).”

“The inferred radial velocities are fully consistent with those listed by Harris (1996;1999), namely –53 and –94 km s−1 for Terzan 4 and Terzan 5, respectively.”

“From the datasets of Paust et al. (2010) and De Marchi, Paresce & Portegies Zwart (2010), combined with the Harris GC catalog (Harris 1996, 2010 update), we have the present-day total stellar mass (via the integrated V-band magnitude of the clusters) and values of α for 33 Galactic globular…”

“M22 has an average reddening E(B − V) = 0.34 (Harris 1996); such a large reddening value is rarely uniform over a cluster face.”

“These clusters range from 7 to 12 kpc in distance and −1.2 to −2.1 in [Fe/H] (Harris 1996).”

“…Gyr (σ∼3 Gyr; e.g., Rosenberg et al. 1999; Salaris & Weiss 2002; De Angeli et al. 2005; Maŕın– Franch et al. 2009; VandenBergh et al. 2013), but also span about a factor of 300 in metallicity (e.g., Zinn & West 1984; Harris 1996; Carretta & Gratton 1997; Kraft & Ivans 2003; Carretta et al. 2009a).”

“We find an average value of +320.2 ± 1.3 km s−1 (σ = 4.8 km s−1) which agrees with values from the literature: +320.5 ± 0.6 km s−1 (Harris 1996, updated in 2010) catalogue; +320.26 km s−1 (rms = 3.74 km s−1) (Carretta et al. 2011); +320.0 ± 0.4 km s−1 (Scarpa et al. 2011); +318.2 ± 0.5 km s−1…”

“We estimated the absolute magnitudes for each star using equation (7) of Lee et al. (1990) and the metallicities, reddenings, and VHB given in Harris (1996).”

“11, the three brightest red giants in M5 fall quite close to the cluster center (recall that M5’s half-light radius is 1.77 arcmin; Harris 1996, 2010 update), and can thus be plausibly affected by crowding.”

“For this model, rc = 1.85 pc and rhl = 4.42 pc, which are in exact agreement with the rc and rhl values for NGC 3201 given in Harris 1996 (2010 edition).”

“…in star cluster formation is why star clusters in excess of 106M formed in the early history of the Milky Way, now present as globular clusters (Harris 1996), but the mass scale of the most massive young star clusters in the present-day Milky Way is two orders of magnitude less (Portegies…”

“The adopted distance estimate of 23.2 kpc is derived from photometry of its horizontal branch stars (providing a distance modulus of 16.82 mag, Harris 1996).”

“The [Fe/H] values are taken from Harris (1996) (the 2003 version of the McMaster catalog).”

“We assume a fiducial distance to NGC 5139 of 5 kpc, between the extremes of 4.9 and 5.3 kpc that are typically quoted (Djorgovski &Meylan 1993; Harris 1996).”

“The metallicity of M92 is [Fe/H] = −2.28 (Harris 1996), and the age is estimated as 14.2±1.2 Gyr (Paust, Chaboyer, & Sarajedini 2007).”

“This will allow us to carry out a more direct comparison with the groundbased data that define rc in the Harris (1996) catalog.”

“(1) With distances adopted from Harris (1996) and six additional open and globular cluster data from Vandenberg & Clem (2003), they derive the following absolute magnitude correction: ΔMr ([Fe/H]) = 4.50 − 1.11[Fe/H] − 0.18[Fe/H]2.”

“…of Figure 1 also show the expected nGC3 signature for all known GCs and dwarf galaxies present in each distance bin, calculated using positions and distances from Harris (1996) and proper motions from Balbinot & Gieles (2017) for GCs; and using all data from McConnachie (2012) for dwarf galaxies.”

“In the Milky Way roughly 150 GCs are currently known (Harris 1996, 2010) and they have a long history of being used in the context of stellar evolution (e.g. Baraffe et al. 1998), the structure and chemical evolution of the Milky Way (e.g. Innanen et al. 1983; Searle & Zinn 1978, respectively) and…”

“Figure 2(d) displays the R-band luminosity function of the Galactic globular clusters which is derived from the compiled data of Djorgovski & Meylan (1993) and Harris (1996).”

“…the cluster center, equivalent to about 1.4 half-mass radii or 24 core-radii, assuming a core radius c = 6:007 (Lugger, Cohn & Grindlay 1995), a half-mass radius hm = 11500 (Djorgovski 1993), and an optical center for the cluster of (J2000) R.A.=19h 10m 51:s8 and Dec.=−59 580 5500 (Harris 1996).”

“Given the resolution and the uncertainty due to the use of a (not filled) slit, they well compare to the value of 93.6 km s−1 reported by Harris (1996).”

“In Figure 16, we show clusters in the M − RG plane using data from the 2010 version of the Harris catalogue10 (Harris 1996), where we adopted a mass-to-light ratio of 2 to convert luminosities to masses (McLaughlin & van der Marel 2005).”

“Interestingly, there is a slightly larger spread between light- and mass weighted metallicities, especially around [Z/H] ∼ −1 where there is also a spread in the HB morphology (eg Harris 1996).”

“…which gives for each cluster the adopted iron content [Fe/H] [from Carretta & Gratton (1997) or from Zinn & West (1984) and Rutledge, Hesser & Stetson (1997) values transformed into the Carretta & Gratton metallicity scale], HB type (Harris 1996) and mean visual magnitude kVRRl of RR Lyrae stars.”

“The ellipticities of Galactic globular clusters are now given in the Harris catalogue (see Harris 1996).”

“This yields a true (unreddened) distance modulus of (m−M)0 = 15.60± 0.2, which corresponds to a distance of 13.2± 1.2 Kpc (to be compared with 10 Kpc quoted by Harris 1996).”

“Within the Galactic globular clusters, M4 has a typical luminosity (i.e., mass), MV ¼ 7:20, while M5 is one of the more luminous (i.e., massive) clusters,MV ¼ 8:81 (Harris 1996).3 The space velocities for these two clusters are considerably different.”

“…et al. 2004; 20 Ortolani et al. 2007; 21 Alves-Brito et al. 2006; 22 Ortolani et al. 1996; 23 Origlia et al. 2002; 24 Ortolani et al. 2003; 25 Harris 1996; 26 Barbuy et al. 2006b; 27 Present work; * Note that Davidge (2000) obtained [Fe/H]=-2.2 for Djorgovski 1. cluster E(B-V) d⊙ [Fe/H] vr…”

“1 shows the distribution of OCs (using the on-line database by Dias et al. 2002, updated as in Table 1) and GCs (from the latest on-line compilation by Harris 1996).”

“We adopted the reddenings of Walker (1992a) for our LMC clusters and E(B[V )\ 0.02 mag for M92 (Harris 1996).”

“…vast majority of the known pulsars in globular clusters are MSPs – about 120 MSPs discovered in 28 globular clusters.1 The Milky Way globular cluster NGC 6624 is located 7.9 kpc away from the Earth, and 1.2 kpc away from the Galactic Centre based on optical observations (Harris 1996, 2010 edition).”

“The central relaxation times have been empirically estimated as in equation (10) of Djorgovski (1993), adopting 0.3M⊙ as average stellar mass, M/LV = 2 as V -band mass-to-light ratio, the integrated V magnitudes listed in Harris (1996), and the structural parameters listed in Table 1.”

“Following van de Ven et al. (2006), we further correct the proper motions for perspective rotation – using a distance of D = 5.0 ± 0.2 kpc (Harris 1996) and systemic velocities µsysα = −3.97 ± 0.41 mas yr−1, µsysδ = −4.38±0.41 mas yr −1(both van Leeuwen et al. 2000) and µsysLOS = 232 km s −1(Reijns…”

“Located in the bulge like its cluster twin NGC 6441, NGC 6388 is a luminous object (MV = −9.42 according to the updated on-line version of the Harris 1996 catalog) at about 3 kpc from the Galactic center, at 10 kpc from the Sun and at slightly more than 1 kpc from the Galactic plane.”

“The hydrogen column density was fixed to NH = 5.9× 1021 cm−2 (Harris 1996).”

“The best fit Wilson model gives a projected half-light radius of rh=2.23’±0.14 ′=46.1 ±2.9 pc which is the largest among those listed by Harris (1996) for Galactic GCs.”

“In order to properly cover the whole range of observed morphologies at low metallicities, the theoretical HB-AGB tracks by Castellani et al. (1991) have been compared to the morphological classification of HBs for a large number of Galactic GCs (Harris 1996).”

“The distance derived by E. Dalessandro et al. (2007, in 1km s preparation) and adopted here is 25% larger than that from Harris (1996), so the resulting proper motions would be∼0.3 mas yr 1.”

“At the distance of NGC 2808 (d ∼ 9.6 Kpc, Harris 1996, update 2003), binary stars are completely unresolved, and the light from both stars combines to form a single point-like source.”

“We adopt the metallicity ½Fe/H ¼ 2:2 dex, also from Harris (1996); Sneden et al. (1997), in a high dispersion abundance analysis of a large sample of stars on the upper giant branch of M15, found a somewhat lower value.”

“We adopted the published spectroscopically determined metallicity of [Fe/H] = -1.50 (Harris 1996).”

“These values are all[Z/Z _ ] higher than the [Fe/H] values give by Harris (1996) ; the large positive value for NGC 6528 is especially so.”

“Based on the Harris (1996) catalog, 31 Galactic GCs satisfy these stringent requirements in terms of relaxation time and rt/rhl.”

“…from Galactic center; 2 horizontal branch ratio: HBR = (B − R)/(B + V + R); 3 concentration; 4 ellipticity e = 1 − (b/a); 5 core radius; 6 tidal radius; 7 central surface brightness; 8 central velocity dispersion; a Harris (1996); b Pryor & Meylan (1993); c Rosenberg et al. (1999); d Buonanno et…”

“We assume a mean V − T1 = 0.50 ± 0.05 for our clusters (which has been derived from Galactic clusters of similar C − T1 color from the lists in Harris & Canterna 1977 and Harris 1996).”

“The mean value is 16.7±4.0 km s−1, consistent with the mean radial velocity of 18.9 km s−1 given by Harris (1996).”

“Scale Radii We first briefly compare our NGC 5128 clusters with those in the Milky Way, using data from the 1999 edition of the Harris (1996) catalog.”

“The Milky Way galaxy harbors approximately 150 globular clusters (Harris 1996 and later revisions) and thousands of openclusters.”

“Following the procedure described in Djorgovski (1993; see also Beccari et al. 2006), we derive log 0 ’ 3:97, where 0 is the central luminosity density in units of L pc 3 (for comparison, log 0 ¼ 4:0 in Harris 1996; Djorgovski 1993; McLaughlin & van der Marel 2005).”

“Stars near the centre of each MXU mask, which have the smallest shifts, were used to roughly report all the mask velocities to the GGC systemicvelocity (from Harris, 1996).”

“…Table 1, we summarize our results for Ba abundances in our sample GCs; along with metallicity [Fe/H] as derived by Carretta et al. (2009a), we list the absolute magnitude of the clusters (from Harris 1996), and the mean Ba abundance for each GC with the corresponding error and the number of stars.”

“Other data are taken from the compilation by Harris (1996).”

“…between the properties of luminous objects in our REF simulation (blue circles) in comparison to Milky Way globular clusters (shown as stars) from Harris (1996) and nearby dwarf galaxies (shown as triangles), including classical dwarfs (dSphs, dEs, dIrrs) and ultra-faint dwarfs from the…”

“…11(a) shows the comparison in the size and absolute magnitude of the stellar system, measured by rh, between MW globular clusters (dots) (Harris 1996) and the known dwarf satellites (squares) (McConnachie 2012; Bechtol et al. 2015; Koposov et al. 2015; Drlica-Wagner et al. 2015; Laevens…”

“Nowadays,∼160 GCs are known in the Milky Way, with metallicities [M/H] = log(Z/X) − log(Z/X)⊙ between∼-2.3 and∼-0.25 (Harris 1996, revision 2010) and with ages ranging from ∼ 6.5 to∼13 Gyr (Aparicio et al. 2001; Chaboyer 2001; Marı́n-Franch et al. 2009; Dotter et al. 2010; Moni Bidin et al. 2011a).”

“The age of the various isochrones, the adopted distance modulus and reddening are also labeled. distance modulus and reddening taken from the compilation of Harris (1996) are also listed.”

“The distance moduli in Table 1 are those from Harris (1996) with a +0.2 mag correction, based on the new calibration by Ferraro et al. (1999).”

“M53 is the least well studied at high dispersion of the calibrators and thus might have a value for [Fe/H] in the Harris (1996) database which is incorrect by up to ±0.15 dex Even from just the 2006 slitmask, it was clear that NGC 2419 showed signs of having a spread in Ca/H.”

“We considered the following parameters to look for possible correlations with the MF slope: Position in the Galaxy (RGC , Z from the Harris catalog; Harris 1996, 2010 edition), destruction rates (ν; from Allen, Moreno & Pichardo 2006, 2008), concentration (c; from McLaughlin & van der Marel 2005),…”

“The comparison between model spectra and observations resulted in a carbon abundance compatible with the cluster abundance ([Fe/H] = −1.15, Harris 1996) except for the three most helium-rich stars W14040, W18899, and W20334.”

“The masses of the clusters and their cores are computed using the central luminosity densities and core radii tabulated by Harris (1996), and a mass-to-light ratio of 3.”

“…RRab metallicity-distribution function derived in this work with that of the 47 Galactic globular clusters (GCs) located within 3.0 kpc from the Galactic center7 (based on 2010 version of Harris 1996 catalog) and that of a sample of 403 bulge red giants (RGs) published by Zoccali et al. (2008).”