A Catalog of Parameters for Globular Clusters in the Milky Way

“Only 5 of the 83 stars of Do et al. (2015) are compatible with the metallicity [Fe/H] » -0.75 (Harris 1996, C. Johnson 2016, private communication) of bulge globular clusters.”

“FSR 1758 appears to be quite large, perhaps rivaling in size with the largest Galactic GCs ω Cen and NGC 2419 (e.g. Harris 1996, Ripepi et al. 2007).”

“At the 16-Mpc distance of Virgo, an average GC half-light diameter of 5 pc (Harris 1996) is equivalent to 0.06′′, which in turn corresponds to a FWHM of 0.04′′ for an average King-model concentration log(rt/rc) = 1.5 (Larsen 1999).”

“The quantitative King model (von Hoerner 1957; King 1962, 1966) concentration parameter is a notably, but not uniquely, low 0.52 (King et al. 1968; Woltjer 1975; Harris 1996).”

“…for M87 UCDs (m = 2×106 M⊙ or 5×106 M⊙) with projected half-mass radius rh = 10 pc (Figure 21). rL ideally represents the radius beyond which the stellar density of a cluster is zero, but in practice rL is an extrapolated radius from either King or other model profile fitting (e.g. Harris 1996).”

“In the Milky Way globular clusters, [Fe/H] ranges from −2.37 to 0.0 dex with a median at [Fe/H]=−1.32 dex (Harris 1996, 2010 edition).”

“Candidate stars from the globular clusters M 13 (e.g., Sandage 1970; Lupton et al. 1987; Shetrone 1994; Harris 1996; Binney & Merrifield 1998) appear on SEGUE plates 2174, 2185, and 2255; from the globular cluster M 2 (e.g., Harris 1996; Lázaro et al. 2006) on SEGUE plate 1961; and from the open…”

“In all cases, we fix the distance to the globular at 10 kpc, a representative distance to the globulars around our Galaxy (actual distances vary from 2.2 kpc to 122 kpc, with roughly 55% being less than 10 kpc distant; see Harris 1996).”

“We used the (B R)0 color index, which is a powerful physical diagnostic sensitive to metallicity in old stellar populations such as globular clusters (e.g., Harris 1996).”

“We split the sample at [Z/H] = −0.6, corresponding to the dip in the Milky Way globular cluster metallicity distribution (Harris 1996), into metal-poor and metal-rich globular clusters.”

“The total integrated luminosity of the Milky Way GC system is about 1.5 × 107LV (using data from Harris 1996), which corresponds to a mass of 2.2×107M for an average visual massto-light ratio of ΥV = 1.45 (McLaughlin 2000).”

“Our own Galaxy contains a few thousand star-forming molec- ular clouds (Rice et al. 2016; Miville-Deschênes et al. 2017), a comparable number of young stellar clusters (Kharchenko et al. 2013), and just over 150 globular clusters (Harris 1996, 2010 edition).”

“The centers of the clusters (from Goldsbury et al. 2010, with the exception of NGC 5897 and NGC 6791, for which we used the coordinates from the Harris 1996 catalog, 2010 edition, and the Simbad database,20 respectively) were placed at a specific position, for example (5000, 5000), so as to always…”

“This is not an unreasonable assumption: if the notably high reddening value of Harris (1996) is omitted, the unweighted average of the Schlegel et al. (1998) value and two the values from Gratton et al. (2003) gives E(B−V)=0.029 ±0.005.”

“The velocity components with respect to the LSR are determined using distances from R. Zinn (1995, private communication) and Harris (1996) and heliocentric radial velocities from Pryor & Meylan (1993) and Harris (1996).”

“To check how NGC 188 fits in the context of evolved star clusters, we compare its concentration parameter with those of 141 Galactic globular clusters (compiled by Harris 1996)4, which also includes the globular cluster sample of Trager et al. (1995).”

“The globular cluster distances were calculated from the ‘compromise’ relation between the horizontal branch magnitude and metallicity advocated in the current (June 1999) version of the Harris (1996) electronic catalogue: MV (HB) = 0.15[Fe/H] + 0.80 .”

“The latter value was determined by assuming a mass of 0.84 M⊙, a reddening E(B − V ) = 0.04 (Harris 1996) and bolometric corrections taken from a 14 Gyr isochrone with [Fe/H] = −1.54 from VandenBerg et al. (2000).”

“Globular clusters in the Milky Way generally have [M/H] of about -1.0 to -2.0 (Harris 1996).”

“As done in Paper I, using our distance estimates and the (l, b) Galactic coordinates from Harris (1996), and assuming a distance R0=8 kpc to c© 2008 RAS, MNRAS 000, 1–12”

“The values for M3 and M5 are taken from the compilation of Harris (1996) ; each of the Ðve is likely to be externally uncertain at the ^0.15 dex level at least (see Paper I).”

“The metallicity [Fe/H], the colour excess E(B − V), and the magnitude of the horizontal branch V(HB) were adopted from Harris (1996).”

“In addition, it is among the closest globulars (around 4.7 kpc; Harris 1996) and thus is well resolved by small telescopes and contains bright main-sequence objects for study (V k17:0 mag).”

“The half-mass relaxation time at 12Gyr is ≈ 2.1Gyr, where we utilize the half-light radius to to calculate this number as suggested by Djorgovski (1993) and Harris (1996).”

“The pursuit of a solution to the enigma of GC formation and its connections with the formation of the Galaxy itself will receive a great boost once a massive data base of chemistry and kinematics of members of all Galactic GCs is in place.”

“There are some 150 globular clusters (GCs) distributed throughout the MW’s baryonic components (Harris 1996, 2010 edition, hereafter H10).”

“THE INTERNAL KINEMATICS OF THE FIVE SUBPOPULATIONS To avoid edge effects, we consider hereafter only stars within 2×rh = 96′′ (Harris 1996, 2010 edition).”

“In order to determine whether it is a dwarf galaxy or a globular cluster, it is vital to determine the photo- 1 We plot the compilation data of Harris (1996) and Willman et al. (2005b) for the GCs and that of Mateo (1998), Willman et al. (2005a), Zucker et al. 2006), and Belokurov et al. (2006) for…”

“We compared the distribution of UCD ellipticities (in Table 1) with those for MW GCs (Harris 1996), NGC5128 GCs (Holland et al. 1999, Harris et al. 2002) and M31 GCs (Barmby et al. 2007).”

“However, since genuin Globular Clusters have spectral types earlier than K0 (Harris (1996)), they clearly cannot be M31 GCs, and we classify all of them as (likely foreground) stars (RBC class 6).”

“The distance moduli were taken from the Harris (1996) catalogue.”

“The only MW star clusters with even lower luminosities are Muñoz 1 (MV ∼ −0.4; Muñoz et al. 2012), Koposov 2 (MV ∼ −0.4; Harris 1996, and 2010 edition), Segue 3 (MV ∼ 0.0; Fadely et al. 2011), and Kim 1 (MV ∼ 0.3; Kim & Jerjen 2015).”

“NGC 2419 resides at 90 kpc from the center of our Galaxy, has a half-mass radius and tidal radius of 20 pc and 230 pc, respectively, and a V-band luminosity of 5 × 105 L (Harris 1996), which implies a total stellar mass of ≈106 M .”

“This procedure requires assumptions about the distance modulus (we adopted (m−M)V = 16.33 from Harris 1996 for the cluster members), the bolometric corrections (from Alonso et al. 1999), and the masses (we assumed a mass of 0.9 M⊙, close to the value given by isochrone fitting).”

“If dynamical effects are involved, the high luminosity and central concentration of this cluster (Harris 1996) make it among the most likely to harbor RRL.”

“Even for the GGCs, the metallicity distribution has a long tail extending to Z (Harris 1996).”

“M15 is “core-collapsed”, i.e., it has an extremely high stellar density near its center (Harris 1996, 2010 edition), which provides a good environment for DNS formation.”

“Note that the central densities (log ρ = 3.51 vs. 3.33, Harris 1996) and concentration (c = log rt/rc = 1.84 vs. 1.51, Harris 1996) parameters for M3 and M13 are very similar despite their apparent difference in σM on the HB.”

“The latter case might be considered more appropriate if the canonical reddening value from Harris (1996) were adopted—implying larger relative ages with respect to M5 (see below).”

“Values are from the catalog of Harris 1996 except for the core radii of 47 Tuc (Howell, Guhathakurta, & Gilliland 2000), NGC 6440 (Trager, Djorgovski, & King 1993), and NGC 6752 (Trager et al. 1993). each of the bands was 580 cm 2 (X soft ), 455 cm 2 (X med ), and 368 cm 2 (X hard ).”

“The entire sample covers a range in metallicity of [Fe/H] from∼–2.3 to –1.1 (Harris 1996, 2010 edition).”

“Assuming E(B−V)=0.01 (Harris 1996) we have obtained (m−M)0=15.64±0.05, values well in agreement with both Ferraro et al. (1999) and Harris (1996).”

“Optically the NGC 6397 CVs are faint, despite being expected to have even brighter secondaries than 47 Tuc (because of the low metallicity, [Fe/H ¼ 1:95; Harris 1996).”

“Our frequency is∼3 times higher than that found by Dolphin et al. (2003), with the number of RR Lyraes compared either to the number of RGB stars (the metric of Dolphin et al. 2003) or the total luminosity of the field (the metric of Harris 1996).”

“…cluster: ω Centauri. ω Cen is unique in the wealth of information available – it is comparatively nearby at a relatively well-known distance of ∼5 kpc (Harris 1996; van Leeuwen et al. 2000; van de Ven et al. 2006; Del Principe et al. 2006); its high radial velocity of vLSR = +232 km s −1…”

“0) of the cluster center mainly taken from Harris (1996), except for Pal 14 (Hilker 2006) and NGC 7089 (Dalessandro et al. 2009).”

“Most notably, the distance to M5 (a globular cluster at 7.5 kpc; Harris 1996) may place it in front of the Fermi Bubble; this would be the case if the radial (line-of-sight) extent of the Fermi Bubble was the same size as its tangential extent on the sky.”

“…VRGBB,predicted| 0.2, (13) where the third constraint has a VRGBB,predicted derived from the metallicity of the cluster and the V-band apparent distance modulus to the cluster (Harris 1996, 2010 edition), and the bestfit relation for those two parameters obtained by a linear fit to the gold sample.”

“…where each mechanism dominates), we adopt the observed parameters for the Galactic GC M22 (NGC 6656), including a central luminosity density log ρ0 = 3.63 (Harris 1996, 2010 update), a core radius 1.7 pc (Harris 1996, 2010 update) and a core binary fraction fb = 0.046 ± 0.006 (Milone et al. 2012).”

“…luminosity density of the Sextans dSph (0.002 L pc 3; Mateo 1998) is significantly lower than that of globular clusters (e.g., 3200 L pc 3 for M3; Harris 1996), so that the collision rates must be much lower and the dynamical evolution must be much slower in the Sextans dSph than in globular…”

“Since EðB VÞ is very small for NGC 6752 (= 0.04, according to Harris 1996), the latter is a negligible effect for this cluster.”

“…and halo mass from Freeman & Bland-Hawthorn 2002) as there is in globular cluster stars with second-generation abundances (67% × 160 clusters × 5 × 105M⊙ per cluster, secondgeneration percentage from Carretta et al. 2010a and globular cluster number and typical mass from Harris 1996, 2010 edition).”

“We have argued in Section 2.2 that the average stellar mass is expected to be comparable to (but slightly less than) the mass of the MSTO in old OCs and low-mass GCs.”

“They all have absolute magnitudes brighter than ω Centauri (NGC 5139), the brightest Milky Way globular cluster (Harris (1996) gives MV = −10.29 mag for ω Cen).”

“In this respect, the low velocity dispersion of NGC 6397, σc ∼ 4.5 km s−1 (Harris 1996), is a challenge because the squared ratio of the uncertainties and the intrinsic dispersion determines the influence of the former.”

“For our tagging technique, we randomly select particles following a steep density profile, ρGC ∝ r−3.5, which is consistent with the distribution of GCs around the Milky Way according to the GC catalog in Harris (1996).”

“…to note that the values so obtained forMV (HB) cannot be used to derive an independent MV versus [Fe/H] relationship, since they actually reflect the relationship adopted by Harris (1996) to determine the distances of the GGCs used in the reference grid, namely,MV ¼ ð0:15 0:05Þ½Fe/H þð0:76 0:07Þ.”

“These models reproduce well the tight metallicity-CaT correlation observed for globular clusters (open blue squares; from Armandroff & Zinn 1988, transformed using the relation given by C01; [Z/H] from Harris 1996).”

“The McMaster catalog (Harris 1996) lists 11 clusters with [Fe/H] −2, a fraction of only 7% of the Milky Way GC system.”

“In Figure 4(a), we plot the relation between MV and rh for the MW globular clusters (dots) taken from Harris (1996), and dwarf galaxies in the MW (filled squares) and M31 (open squares) from McConnachie (2012), the recent DES work (Bechtol et al. 2015; Koposov et al. 2015; Drlica-Wagner et al.…”

“G A ] 7 M ay 2 01 4 log of Milky Way GCs by Harris (1996) (hereafter H96) and for which surface brightness estimates (Trager et al. 1995; Noyola & Gebhardt 2006) led to reasonable exposure times (< 6 h).”

“The cluster data (projected half-light radii, total luminosities, galactocentric distances) were taken from the 2003 version of the globular cluster data base of Harris (1996), supplemented by additional data for a few clusters from Bonatto & Bica (2008).”

“Membership was assessed in Harbeck et al. (2003) based on radial velocity (unfortunately only 18.7 km s 1 for 47 Tuc; Harris 1996) and position in the CMD (within 0.025 mag of the cluster fiducial).”

“106M⊙pc −3, Harris 1996) or young clusters such as the Arches (3 × 105M⊙pc −3, Figer et al. 1999).”

“It is based on a homogeneous data set derived from ∼2000 modern spectra, and is gaining considerable favour – see e.g. its adoption by Harris (1996) for his online GC catalogue at http://www.physics.mcmaster.ca/~harris/mwgc.data.”

“While the discrepancy arising from the zero point calibration of the Fourier technique is substantial, the distance modulus obtained for RRab stars is consistent with the value of (m − M)V = 14.33 (Harris 1996).”

“Data for the Milky Way were obtained from Pryor & Meylan (1993) and Harris (1996).”