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Chapter 22
Star Clusters
Hugh C. Harris and William E. Harris
22.1
Open Clusters . . . . . . . . . . . . . . . . . . . . . . . 545
22.2
Globular Clusters in the Milky Way . . . . . . . . . . 554
22.3
Globular Clusters in Other Galaxies . . . . . . . . . . 562
The classification of star clusters as “open” or “globular” was originally based on their appearance
in the sky. However, in the Milky Way Galaxy, the common properties of open clusters (location in
the galactic disk, disk kinematics, near solar metallicity, and younger age) are fairly distinct from the
properties of globular clusters (often in the galactic spheroid, often metal-poor, older age). Here we
designate clusters with ages 10 Gyr and younger as “open” and older clusters as “globular.” However,
cases of ambiguous or inadequate data exist (e.g., for clusters Berkeley 17, Pal 1, BH176, Lyngå 7, see
tables below), and there is no single rigorous definition that can be used to classify every star cluster.
22.1
OPEN CLUSTERS
Open star clusters have been cataloged many times, but lists of newly discovered clusters continue to
appear. In the Milky Way, the extensive 1987 Lyngå–Lund Observatory catalog [1] containing 1154
clusters is the most recent comprehensive listing. We have started with this catalog, using the cluster’s
names from this catalog, and updated it with the many recent references through 1996. Beyond the
Milky Way, only the Magellanic Clouds are close enough to have relatively complete searches made
for open clusters. In this chapter, we concentrate on Milky Way clusters.
Unlike the case for globular clusters, the catalog of open clusters in the Milky Way is far from
final. The first deficiency is that almost 200 clusters are noted in the catalog or in other literature as
“doubtful.” Many (perhaps 20% of the catalog or more) are not true clusters of physically associated
and gravitationally bound stars. In Tables 22.2–22.4 clusters noted as “doubtful” have been omitted.
The second deficiency of the catalog is incompleteness. At visible wavelengths, deeper sky surveys
reveal new clusters, most of which will prove to be distant open clusters. The ESO Uppsala Survey [2]
cataloged 129 new clusters south of declination −17.5◦ and outside of the Magellanic Clouds. Only
545
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S TAR C LUSTERS
a few of these clusters have been studied yet, and two (AM2 = 368-SC07 and 092-SC18) have been
added to Table 22.4. Inaccurate coordinates for many clusters have added to confusion in cluster
identifications that is slowly being resolved (e.g., [3]). Undoubtedly many more new clusters will be
found on the POSS II northern sky survey. At present, omitting doubtful clusters, we have 488 clusters
with a distance determination (of which 445 also have an age determination) and 498 without a reliable
distance.
Interstellar absorption is, of course, the major cause for incomplete discovery of open clusters.
Infrared data can help alleviate this problem, and new clusters not already identified at visible
wavelengths have been incorporated here (see notes to Table 22.2). For heavily obscured clusters,
large uncertainties usually exist in their distances and in their membership (and, hence, in whether they
are, or will become, bound clusters rather than unbound groups or associations). From very preliminary
studies so far (e.g., [4, 5]), we can guess that several hundred clusters in the second and third quadrants
of the Galaxy will be discovered with infrared data, and undoubtedly many more will be found in the
first and fourth quadrants. Most of these clusters will have ages less than 107 yr.
Age determinations for open clusters can be quite uncertain. An accurate cluster distance is often
needed because, for younger clusters, the absolute magnitude of the cluster turnoff is the primary age
discriminator. For young clusters, the status adopted for the most bright and hot main-sequence stars
(cluster member versus nonmember, and main sequence versus evolved) can have a large effect on the
derived cluster age. In at least some young clusters, prolonged star formation complicates assigning a
unique age. Here the youngest clusters are all listed with an arbitrary age of 106 yr. For clusters with
ages ∼ 109 yr and older, the difference in magnitude between the turnoff and red-giant clump can be
used [6, 7]. Again, the status adopted for a few stars can affect the derived age. Cluster ages depend
ultimately on calibration from stellar evolutionary models. The adopted model parameters (mass loss,
convective overshoot, etc.) introduce systematic differences in the derived ages. Generally, recent
models have been converging toward reasonably good agreement within about 25% (e.g., [8]). In the
tables here, cluster ages have been taken directly from the most recent or most reliable literature study
without adjustment.
Few open clusters have been studied to determine their structural and dynamical parameters. Thus,
accurate data on radii, velocity dispersions, densities, and masses are lacking for all but a few clusters.
22.1.1
Parameters for Open Clusters
This section summarizes some parameters describing the system of open clusters in the Milky Way.
We begin with the surface density projected onto the galactic plane of open clusters of different ages
in the solar neighborhood within 1200 pc of the sun (Table 22.2). Note, however, that clusters are
distributed nonuniformly. The youngest clusters are more common in regions like the Perseus spiral
arm than in the solar neighborhood; the oldest clusters are more common in the outer disk. The last
entry, the corrected total (corrected for incompleteness), is based on the distribution of cluster distances
in Table 22.2, a distribution that indicates increasing incompleteness beyond 600 pc.
Projected surface density (Table 22.2; see also [9, 10]):
0–19 Myr
20–49 Myr
50–99 Myr
100–199 Myr
200–499 Myr
500–1999 Myr
(26 clusters)
(21 clusters)
(23 clusters)
(24 clusters)
(27 clusters)
(20 clusters)
5.5 kpc−2 .
4.5 kpc−2 .
4.9 kpc−2 .
5.1 kpc−2 .
5.7 kpc−2 .
4.2 kpc−2 .
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22.1 O PEN C LUSTERS / 547
≥ 2000 Myr
Unknown Age
All clusters
Corrected total
(2 clusters)
(13 clusters)
(156 clusters)
0.4 kpc−2 .
2.8 kpc−2 .
33.1 kpc−2 .
50. kpc−2 .
The median age in the solar neighborhood (Table 22.2) is:
∼ 108 yr.
The cluster formation rate [9–11] is:
∼ 0.5 kpc−2 Myr−1 .
The cluster destruction time scale (e-folding time) in the solar neighborhood [11, 12] is:
∼ 107 yr for low-mass clusters,
∼ 108 yr for typical clusters,
∼ 109 yr for rich (populous) clusters.
There is no significant dependence for metallicity as a function of age [9, 13] nor for metallicity as a
function of z distance [9, 13].
The metallicity as a function of galactocentric radius is:
All clusters [9]: −0.07 dex kpc−1 .
Old clusters [13, 14]: −0.09 dex kpc−1 .
The scale height for clusters is:
Young clusters (< 3 × 108 yr), solar neighborhood [9]: 55 pc.
Young clusters (< 3 × 108 yr), outer disk [9]: Larger, but not well known.
Old clusters (> 109 yr) [15]: 375 pc.
Kinematics of young clusters (< 3 × 107 yr) are described by [16]:
Oort constant A: 17 km s−1 kpc−1 .
Second-order term: −2 km s−1 kpc−2 .
One-dimensional radial velocity dispersion: 11 km s−1 .
Kinematics of old clusters (> 1 Gyr) [17] are consistent with the same rotation curve for young clusters,
and with
One-dimensional radial velocity dispersion: 28 km s−1 .
Dynamical properties of one typical and one rich (populous) open cluster are given in Table 22.1.
Table 22.1. Dynamical properties of two open clusters.
Property
Core radius (pc):
Half-mass radius (pc):
Central density (M pc−3 ):
Central one-dimensional velocity dispersion (km s−1 ):
Half-mass relaxation time (yr):
Total mass (M ):
Typical
(Hyades [18])
Rich
(M11 [19])
2.1
4.3
3
0.2
108
350
0.8
2.7
500
1.2
108
7000
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S TAR C LUSTERS
Open clusters in the Large Magellanic Cloud (LMC) have:
Total population [20, 21]: 4200 clusters.
Peak face-on surface density [20]: 200 kpc−2 .
Median age [22, 23]: ∼ 109 yr.
Open clusters in the Small Magellanic Cloud (SMC) have:
Total population [24]: 2000 clusters.
Peak face-on surface density [24]: 200 kpc−2 .
Median age [25]: ∼ 109 yr.
22.1.2
Selected Open Clusters in the Milky Way
This section provides data for selected open clusters in the Milky Way. Data are taken from the
literature through the end of 1996, plus distances to 14 clusters measured with the Hipparcos satellite
published in 1997 [26, 27]. Table 22.2 lists 156 clusters believed to be within 1200 pc of the Sun.
Table 22.3 lists 54 clusters with estimated ages 3 × 106 yr and less. Table 22.4 lists 52 clusters with
estimated ages more than 109 yr. All tables have the same format.
Column (1) gives the cluster name, usually as given by [1], with other common names. Names
changed or added to [1] are indicated in the table notes.
Columns (2) and (3) give the right ascension and declination (J2000). Positions are taken from [1],
given to the nearest 1 arcmin in declination, except for clusters south of declination −17.5◦ measured
on the ESO southern sky survey [2], and other clusters measured by [28]. For the latter clusters [2, 28],
positions are given to 0.1 arcmin in declination.
Columns (4) and (5) give the galactic latitude and longitude in degrees.
Column (6) gives the distance from the Sun in parsecs, taken first from a recent study in the
literature, or second from Janes, Duke, and Lyngå, as given by [1].
Column (7) gives the distance from the galactic center (GC) in kiloparsecs. We adopt R0 = 8.0
kpc [29] for the distance of the Sun from the galactic center.
Column (8) gives the foreground interstellar reddening, E(B − V ), taken from the same source as
the distance, if available.
Column (9) gives the angular diameter in arc minutes, taken first from [30] measured on sky survey
prints, or second from a selected diameter from the literature. These estimates are approximate and
can be biased by field-star contamination.
Column (10) gives the approximate number of cluster members estimated by [30].
Column (11) gives the richness class given by [12], defined from 5 (very rich cluster with high star
density) to 1 (very sparse cluster).
Column (12) gives the logarithm (base 10) of the cluster age in years.
Table 22.2. Nearby Galactic open clusters.
(1)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
Cluster
(2)
RA
(h m s)
(12)
b
Dist.
RGC
Red.
Dia.
Mem.
Rich.
Age
Ber 59
Bla 1(ζ Scl)
NGC189
NGC225
NGC381
0 02 10
0 04 07
0 39 36
0 43 30
1 08 18
67 25.2
−29 49.9
61 05.7
61 47.0
61 35.0
118.3
15.6
121.5
122.0
124.9
4.9
−79.3
−1.8
−1.1
−1.2
880
252
1080
525
1060
8.45
7.95
8.61
8.29
8.65
0.02
0.54
0.25
0.36
10
70
5
15
7
40
30
15
15
50
1
3
2
6.30
7.70
7.30
8.08
9.00
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22.1 O PEN C LUSTERS / 549
Table 22.2. (Continued.)
(1)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
Cluster
(2)
RA
(h m s)
b
Dist.
RGC
Red.
Dia.
Mem.
Rich.
Age
NGC559
Col 463
NGC752
Sto 2
Mar 6
Tru 2
NGC1039(M34)
NGC1027
Mel 20(α Per)
NGC1333a
NGC1342
IC348
Pleiades(M45)
NGC1502
NGC1528
NGC1545
Hyades
LHA 101a
NGC1647
NGC1662
NGC1664
NGC1746
NGC1901
Col 69(λ Ori)
NGC1981
Trapeziumb
Col 70
NGC2024a
NGC2068a
NGC2071a
NGC2112
NGC2169
NGC2168(M35)
NGC2215
NGC2232
Col 96
NGC2264
NGC2287(M41)
NGC2281
NGC2301
NGC2302
Col 121
NGC2323(M50)
NGC2335
NGC2343
NGC2353
Col 132
NGC2360
Col 140
Rup 18
NGC2395
NGC2409c
NGC2422(M47)
NGC2423
1 29 30
1 47 36
1 57 48
2 15 00
2 29 40
2 36 53
2 42 00
2 42 36
3 24 19
3 29 01
3 31 42
3 44 36
3 47 29
4 07 50
4 15 19
4 20 57
4 26 54
4 30 12
4 46 00
4 48 29
4 51 06
5 03 36
5 17 48
5 35 00
5 35 12
5 35 16
5 35 36
5 41 42
5 46 42
5 47 12
5 53 46
6 08 25
6 08 48
6 20 50
6 28 02
6 30 18
6 40 59
6 46 04
6 48 18
6 51 46
6 51 54
6 54 12
7 03 12
7 06 50
7 08 07
7 14 31
7 15 20
7 17 44
7 23 12
7 24 39
7 27 13
7 31 37
7 36 36
7 37 07
63 18.0
71 46.0
37 41
59 16
60 42.4
55 54.9
42 47
61 35.7
49 51.7
31 19
37 20
32 18
24 06.3
62 19.9
51 12.7
50 15.3
15 52
35 15
19 05
10 55.8
43 40.6
23 49
−68 26
9 56
−4 26.0
−5 23.4
−1 05
−1 54
0 06
0 19
0 24.6
13 57.9
24 20
−7 17.0
−4 50.8
2 52
9 53.7
−20 45.5
41 04.7
0 27.6
−7 05.0
−24 24.6
−8 20
−10 01.7
−10 37.0
−10 16.0
−30 40.8
−15 38.5
−32 02.2
−26 11.9
13 36.5
−17 11.4
−14 29.0
−13 52.3
127.2
127.4
137.2
133.4
134.7
137.4
143.6
135.8
146.9
158.3
155.0
160.4
166.6
143.6
152.0
153.4
180.1
165.4
180.4
187.7
161.7
179.0
279.0
195.1
208.1
209.0
205.0
206.5
205.3
205.2
205.9
195.6
186.6
216.0
214.4
208.0
202.9
231.0
175.0
212.6
219.3
235.2
221.7
223.6
224.3
224.7
243.0
229.8
245.0
239.9
204.6
232.5
231.0
230.5
0.8
9.6
−23.4
−1.9
0.0
−3.9
−15.6
1.5
−7.1
−20.5
−15.4
−17.7
−23.5
7.6
0.3
0.2
−22.4
−9.0
−16.8
−21.1
−0.4
−10.6
−33.6
−12.0
−19.0
−19.4
−17.4
−16.4
−14.3
−14.1
−12.6
−2.9
2.2
−10.1
−7.7
−3.4
2.2
−10.4
17.1
0.3
−3.1
−10.3
−1.2
−1.3
−1.2
0.4
−8.8
−1.4
−7.9
−4.9
14.0
0.8
3.1
3.5
900
600
440
316
485
600
465
1000
184
320
550
320
116
875
800
800
46
800
542
400
1200
420
300
500
400
435
430
400
400
400
750
1020
870
1000
320
1100
800
700
460
750
1100
1170
910
1000
1000
1200
411
1070
380
1028
1200
828
460
870
8.57
8.37
8.30
8.22
8.35
8.45
8.36
8.74
8.15
8.28
8.48
8.29
8.10
8.71
8.71
8.72
8.04
8.77
8.52
8.37
9.15
8.41
7.96
8.47
8.34
8.36
8.37
8.35
8.35
8.35
8.66
8.99
8.86
8.82
8.26
8.98
8.74
8.45
8.44
8.64
8.88
8.71
8.70
8.75
8.74
8.89
8.19
8.73
8.17
8.56
9.07
8.53
8.30
8.58
0.90
0.19
0.03
0.38
0.52
0.30
0.10
0.32
0.09
2.00
0.27
1.50
0.04
0.75
0.29
0.34
0.00
7
30
75
45
6
17
25
15
300
60
40
60
50
6
20
60
40
50
4
2
2
4
1
3
3
2
4
17
8
120
20
18
12
329
40
20
100
45
40
20
2
1
4
2
3
2
4
0.33
0.32
0.24
40
12
18
40
40
70
28
47
140
200
35
3
2
4
9.10
8.18
9.26
8.23
7.40
7.89
8.26
8.54
7.72
6.00
8.48
6.48
8.00
6.85
8.43
8.29
8.79
6.00
8.04
8.48
8.48
1
8.70
1
6.60
2
4
2
1
1
2
3
3
1
1
1
3
1
2
2
1
3
1
1
1
1
1
4
6.00
6.00
6.00
9.60
7.20
8.03
8.55
7.30
7.40
6.60
8.30
8.48
8.03
7.80
6.18
7.89
8.20
8.00
7.90
7.40
9.00
7.30
8.10
7.70
7.40
7.89
8.55
0.05
0.09
0.05
0.60
0.20
0.22
0.31
0.02
0.46
0.04
0.06
0.11
0.04
0.24
0.01
0.26
0.38
0.19
0.12
0.03
0.08
0.05
0.67
0.69
0.19
0.08
0.12
18
6
25
8
45
12
40
40
25
15
5
90
15
7
6
18
80
14
30
8
15
16
25
12
20
40
20
20
100
50
30
200
40
20
15
40
80
30
80
30
20
80
35
20
30
25
80
30
40
30
30
30
40
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S TAR C LUSTERS
Table 22.2. (Continued.)
(1)
Cluster
NGC2447(M93)
NGC2482
NGC2516
Col 173
NGC2527
NGC2547
NGC2546
NGC2548(M48)
NGC2579
Pis 4
NGC2632b
IC2391
IC2395
Col 197
NGC2669
Tru 10
NGC2682(M67)
NGC2925
NGC2972
NGC3033
NGC3114
NGC3228
vBH 99
IC2602
NGC3532
NGC3680
Rup 98
Mel 111(Coma)
Hog 14
Har 5
NGC4463
Rup 108
NGC5316
NGC5460
Lyn 2
NGC5662
Col 285(UMa)
Hog 18
NGC5764
NGC5822
NGC6025
NGC6087
NGC6124
ρ Opha
NGC6134
NGC6152
NGC6178
NGC6204
NGC6208
NGC6242
NGC6249
NGC6250
NGC6268
NGC6281
(2)
RA
(h m s)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
b
Dist.
RGC
Red.
Dia.
Mem.
Rich.
Age
7 44 31
7 55 15
7 58 07
8 02 49
8 04 58
8 10 10
8 12 16
8 13 44
8 22 12
8 34 36
8 40 24
8 40 32
8 42 31
8 44 51
8 46 23
8 47 54
8 51 24
9 33 13
9 40 14
9 48 35
10 02 30
10 21 22
10 37 54
10 42 58
11 05 48
11 25 39
11 58 40
12 25 06
12 28 36
12 27 10
12 29 58
13 32 11
13 53 57
14 07 28
14 24 35
14 35 38
14 40 54
14 50 43
14 53 32
15 04 21
16 03 18
16 18 51
16 25 20
16 26 54
16 27 46
16 32 46
16 35 47
16 46 09
16 49 28
16 55 33
16 57 41
16 57 56
17 02 10
17 04 41
−23 51.7
−24 15.7
−60 45.2
−46 22.8
−28 08.8
−49 12.3
−37 35.7
−5 45.0
−36 24
−44 25.4
19 40.0
−53 02.1
−48 09.0
−41 13.4
−52 56.8
−42 27.4
11 49.0
−53 24.0
−50 19.5
−56 25.8
−60 07.8
−51 44.0
−59 11
−64 23.6
−58 46.2
−43 14.1
−64 35.1
26 07
−59 49.1
−60 45.8
−64 47.5
−58 27.7
−61 52.1
−48 20.5
−61 20.0
−56 37.1
69 34
−52 16.0
−52 40.2
−54 23.8
−60 25.9
−57 56.1
−40 39.2
−24 35
−49 09.1
−52 38.6
−45 38.6
−47 01.0
−53 43.7
−39 27.6
−44 48.7
−45 56.2
−39 43.7
−37 59.1
240.0
241.6
273.8
261.4
246.1
264.5
254.9
227.9
254.7
262.9
205.5
270.4
266.7
261.5
270.8
262.8
215.6
275.9
274.7
279.6
283.3
280.7
286.6
289.6
289.6
286.8
297.3
221.2
300.1
300.0
300.6
308.3
310.2
315.8
313.9
316.9
109.9
320.8
321.0
321.6
324.5
327.7
340.7
353.0
334.9
332.9
338.4
338.6
333.8
345.5
341.5
340.7
346.0
347.7
0.1
2.0
−15.9
−8.2
1.9
−8.6
−2.0
15.4
0.3
−2.4
32.5
−6.8
−3.6
1.0
−6.1
0.7
31.7
−1.3
1.8
−2.1
−3.9
4.5
−0.6
−4.9
1.3
16.9
−2.3
84.0
2.9
2.0
−2.0
4.0
0.1
12.6
−0.4
3.4
44.7
6.4
5.9
3.6
−5.9
−5.4
6.0
16.7
−0.2
−3.2
1.2
−1.0
−5.8
2.5
−1.2
−1.9
1.3
2.0
860
800
348
330
600
420
1000
610
1000
600
177
148
1050
1000
1000
380
830
810
1200
1100
940
500
425
147
417
850
400
88
912
1029
1180
700
1170
790
1100
740
20
1100
1000
740
780
860
563
160
760
1030
904
1180
1000
1120
1019
1020
1100
502
8.46
8.41
7.98
8.06
8.26
8.05
8.32
8.41
8.32
8.10
8.13
8.00
8.13
8.21
8.05
8.06
8.58
7.96
7.99
7.89
7.84
7.92
7.89
7.95
7.87
7.80
7.83
8.01
7.58
7.54
7.47
7.59
7.30
7.47
7.28
7.48
8.00
7.19
7.25
7.43
7.38
7.29
7.47
7.85
7.32
7.10
7.17
6.92
7.12
6.92
7.04
7.05
6.94
7.51
0.00
0.03
0.13
0.09
0.09
0.05
0.10
0.05
0.20
0.02
0.04
0.01
0.12
0.56
0.18
0.04
0.03
0.05
0.33
0.58
0.04
0.03
0.05
0.04
0.04
0.08
0.16
0.00
0.28
0.18
0.44
0.17
0.34
0.14
0.19
0.31
0.00
0.50
0.48
0.15
0.16
0.20
0.80
10
10
22
369
10
25
70
30
8
25
70
60
17
25
20
30
25
15
5
12
35
5
20
100
50
7
15
120
3
5
6
10
15
35
10
30
80
40
80
4
2
4
8.78
8.60
8.15
40
80
40
80
20
45
50
30
40
40
40
40
200
40
25
50
2
2
3
1
1
1
4
2
2
1
2
1
5
2
1
1
2
1
9.00
7.76
7.62
8.48
7.10
7.40
8.90
7.48
7.20
6.80
7.80
7.67
9.65
7.90
8.60
8.60
8.18
7.62
8.00
7.48
8.49
9.28
8.50
8.65
8.50
7.60
7.40
8.10
8.08
8.30
7.50
7.85
8.21
7.70
0.35
6
25
5
6
18
9
6
10
6
8
0.24
0.51
0.17
0.39
0.45
0.38
0.39
0.16
5
3
35
15
15
40
15
40
60
150
30
50
80
30
15
80
40
30
70
15
12
150
60
40
100
70
12
45
60
30
60
2
5
2
1
2
1
1
1
1
3
2
2
4
1
1
4
3
3
2
4
9.15
8.08
7.85
8.00
6.00
8.90
1
2
4
3
1
2
3
3
6.80
8.08
9.00
7.70
7.40
7.15
7.40
8.34
Sp.-V/AQuan/1999/10/11:11:34
Page 551
22.1 O PEN C LUSTERS / 551
Table 22.2. (Continued.)
(1)
Cluster
NGC6322
IC4651
NGC6405(M6)
NGC6416
IC4665
NGC6425
Bas 5
NGC6475(M7)
NGC6494(M23)
Tru 31
Boc 14
NGC6546
NGC6613(M18)
NGC6633
Ser 1a
IC4725(M25)
IC4756
NGC6709
NGC6716
Ber 82
NGC6811
NGC6866
Ros 5
NGC6885
Dol 6
Ber 87
S 106a
NGC6997c
Col 428
NGC7031
NGC7039
Bas 14
NGC7063
NGC7086
NGC7092(M39)
IC1396
IC5146
NGC7160
NGC7209
NGC7243
NGC7261
NGC7686
NGC7762
(2)
RA
(h m s)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
b
Dist.
RGC
Red.
Dia.
Mem.
Rich.
Age
17 18 26
17 24 49
17 40 21
17 44 20
17 46 12
17 47 02
17 52 27
17 53 51
17 57 05
17 59 48
18 01 59
18 07 22
18 19 54
18 27 42
18 30 00
18 31 47
18 38 54
18 51 30
18 54 34
19 11 24
19 38 12
20 03 42
20 10 00
20 12 00
20 20 48
20 21 36
20 27 24
20 56 30
21 03 12
21 07 18
21 11 12
21 21 12
21 24 30
21 30 30
21 32 12
21 39 00
21 53 30
21 53 48
22 05 12
22 15 18
22 20 24
23 30 12
23 49 54
−42 56.0
−49 56.3
−32 15.3
−32 21.7
5 43
−31 31.8
−30 05.8
−34 47.6
−18 59.1
−28 09.6
−23 41.8
−23 17.8
−17 06
6 34
1 14
−19 06.9
5 26
10 20
−19 54.1
13 04
46 34
44 00
33 46
26 29
41 23
37 22
37 23
44 37
44 35
50 50
45 39
44 49
36 30
51 35
48 27
57 30
47 16
62 36
46 30
49 53
58 05
49 07
68 01
345.3
340.1
356.6
356.9
30.6
357.9
359.8
355.9
9.9
2.3
6.4
7.3
14.1
36.1
31.6
13.7
36.4
42.2
15.4
46.8
79.4
79.5
71.4
65.5
78.9
75.7
76.4
85.5
86.2
91.3
88.0
88.6
83.1
94.4
92.5
99.3
94.4
104.0
95.5
98.9
104.0
109.5
117.2
−3.1
−7.9
−0.8
−1.5
17.1
−1.6
−1.9
−4.5
2.8
−2.3
−0.5
−1.4
−1.0
8.3
5.3
−4.4
5.3
4.7
−9.6
1.6
11.9
6.9
0.3
−4.1
2.7
0.3
−0.6
−0.5
−1.4
2.3
−1.7
−3.6
−9.9
0.2
−2.3
3.7
−5.5
6.4
−7.3
−5.6
0.9
−11.6
5.8
1200
780
600
800
350
800
850
292
660
1000
1150
830
1200
292
310
560
289
950
550
980
900
1200
300
590
980
946
600
500
480
1000
675
1030
635
1200
263
800
1000
750
900
880
900
1000
800
6.85
7.28
7.40
7.20
7.71
7.20
7.15
7.71
7.35
7.00
6.86
7.18
6.84
7.77
7.74
7.46
7.77
7.33
7.48
7.36
7.89
7.87
7.91
7.77
7.87
7.82
7.88
7.98
7.98
8.08
8.00
8.04
7.95
8.18
8.02
8.17
8.14
8.21
8.13
8.18
8.26
8.38
8.39
0.51
0.14
0.16
0.31
0.18
0.48
0.33
0.06
0.36
0.42
1.62
0.72
0.42
0.17
5
10
20
15
70
10
5
80
30
5
2
15
5
20
30
80
80
40
30
35
30
80
150
25
10
150
20
30
2
4
4
4
2
2
2
2
3
0.48
0.20
0.32
0.17
1.01
0.14
0.13
0.06
0.07
3.00
2.00
30
40
15
10
3
15
15
50
10
6
10
30
80
40
20
20
70
80
15
30
12
30
4
5
3
2
7.00
9.28
7.71
8.50
7.78
7.80
9.10
8.34
8.48
9.10
6.00
7.60
7.50
8.80
6.00
7.95
8.92
7.89
8.00
7.85
8.73
8.36
0.61
8
10
15
15
5
9
12
30
90
20
5
15
30
6
15
15
40
20
50
50
15
12
50
30
50
20
12
25
40
30
20
40
0.79
0.07
0.62
0.08
0.66
0.01
0.58
0.66
0.36
0.20
0.18
0.96
0.88
1
2
2
3
4
2
2
6.00
6.60
6.30
2
3
3
3
3
1
1
2
3
2
2
3
7.75
8.10
1
9.26
8.15
7.93
8.48
6.00
8.36
6.85
8.48
8.03
7.60
Notes
a Clusters added to [1] list: NGC1333 (Lada et al. 1996, AJ, 111, 1964); LHA 101 (Barsony et al. 1991, ApJ, 379, 221);
NGC2024, NGC2068, and NGC2071 (Lada et al. 1991, ApJ, 371, 171); S 269 (Eiroa et al. 1995, A&A, 303, 87); AM 2
(Ortolani et al. 1995, A&A, 300, 726); 092-SC18 (Kassis et al. 1996, AJ, 111, 820); NGC3576 (Persi et al. 1994, A&A, 282,
474); ρ Oph (Williams et al. 1995, ApJ, 454, 144); GM 24 (Tapia et al. 1991, A&A, 242, 388); Ser 1 (Eiroa et al. 1992, A&A,
262, 468); S 106 (Hodapp et al. 1991, AJ, 102, 1108).
b Trapezium = NGC1976 and NGC2632 = Praesepe.
c Cluster name changed from that used in [1]. NGC2409 is Boc 4 and NGC6997 is NGC6996.
Sp.-V/AQuan/1999/10/11:11:34
Page 552
552 / 22
S TAR C LUSTERS
Table 22.3. Young galactic open clusters.
(1)
Cluster
Ber 59
NGC637
Ber 7
IC1805
IC1848
NGC1333a
IC348
LHA 101a
NGC1893
NGC2024a
NGC2068a
NGC2071a
NGC2175
S 269a
NGC2244
Col 121
NGC2367
NGC2384
Boc 5
Boc 6
Boc 15
Haf 18
Rup 44
Rup 55
Mar 18
Wes 2(NGC3247)b
NGC3324
Col 228
Tru 14
Col 232
Tru 16(η Car)
Boc 11
NGC3503(Pis 17)b
Col 240
NGC3576a
NGC3603
Col 272
ρ Opha
NGC6193
NGC6200
Lyn 14
GM 24a
Pis 24
Boc 14
NGC6530(M8)
NGC6611(M16)
NGC6618(M17)
Ser 1a
Biu 2
Ber 86
Dol 6
S 106a
IC1396
NGC7380
(2)
RA
(h m s)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
b
Dist.
RGC
Red.
Dia.
Mem.
Rich.
Age
0 02 10
1 43 04
1 54 12
2 32 42
2 51 11
3 29 01
3 44 36
4 30 12
5 22 46
5 41 42
5 46 42
5 47 12
6 09 39
6 14 36
6 32 19
6 54 12
7 20 09
7 25 10
7 31 47
7 32 00
7 40 16
7 52 39
7 58 51
8 12 27
9 00 32
10 24 02
10 37 23
10 42 04
10 43 56
10 44 59
10 44 58
10 47 12
11 01 17
11 11 40
11 11 33
11 15 08
13 30 26
16 26 54
16 41 20
16 44 07
16 55 04
17 17 00
17 25 32
18 01 59
18 04 31
18 18 48
18 20 48
18 30 00
20 09 12
20 20 24
20 20 48
20 27 24
21 39 00
22 47 00
67 25.2
64 02.2
62 22.2
61 27.4
60 24.1
31 19
32 18
35 15
33 25.2
−1 54
0 06
0 19
20 29.3
13 50
4 51.4
−24 24.6
−21 52.8
−21 01.2
−16 59.8
−19 26
−33 32.6
−26 23.0
−28 35.0
−32 35.1
−48 58.9
−57 45.6
−58 37.4
−59 55.2
−59 32.8
−59 33.4
−59 43.0
−60 05.8
−59 50.7
−60 18.6
−61 21.8
−61 15.6
−61 19.0
−24 35
−48 45.8
−47 27.8
−45 14.4
−36 21
−34 24.5
−23 41.8
−24 21.6
−13 45
−16 09
1 14
35 29
38 42
41 23
37 23
57 30
58 06
118.3
128.6
130.1
134.7
137.2
158.3
160.4
165.4
173.6
206.5
205.3
205.2
190.2
196.5
206.4
235.2
235.6
235.4
232.6
234.8
248.0
243.1
245.8
250.7
269.2
284.3
286.2
287.4
287.4
287.5
287.6
288.0
289.5
290.9
291.3
291.6
307.6
353.0
336.7
338.0
340.9
350.5
353.1
6.4
6.1
17.0
15.1
31.6
72.8
76.7
78.9
76.4
99.3
107.1
4.9
1.7
0.4
0.9
0.9
−20.5
−17.7
−9.0
−1.7
−16.4
−14.3
−14.1
0.4
−1.9
−2.0
−10.3
−3.8
−2.4
0.7
−0.2
−5.5
0.4
0.5
0.8
−1.8
−0.3
−0.2
−1.0
−0.6
−0.5
−0.7
−0.9
0.1
0.2
−0.8
−0.5
1.2
16.7
−1.6
−1.1
−1.1
1.0
0.6
−0.5
−1.3
0.8
−0.7
5.3
1.4
1.3
2.7
−0.6
3.7
−0.9
880
2880
2580
2340
2200
320
320
800
4400
400
400
400
2200
4000
1880
1170
2000
2000
2290
4000
3767
6900
4600
4400
1600
7900
3300
2100
3240
3240
3240
3470
4200
2559
2400
7200
2900
160
1410
2400
2300
2000
2100
1150
1800
2020
2000
310
1500
1900
980
600
800
3700
8.45
10.05
9.86
9.79
9.73
8.28
8.29
8.77
12.38
8.35
8.35
8.35
10.17
11.89
9.72
8.71
9.27
9.28
9.57
10.81
10.03
12.71
10.74
10.33
8.18
9.76
7.76
7.64
7.68
7.67
7.67
7.67
7.70
7.48
7.49
8.57
6.64
7.85
6.73
5.84
5.88
6.04
5.92
6.86
6.21
6.10
6.09
7.74
7.69
7.78
7.87
7.88
8.17
9.75
10
3
4
20
18
40
20
18
40
10
8
20
1
0.53
25
60
4
0.50
22
60
1
0.49
0.01
0.33
0.30
0.63
0.70
0.55
0.50
0.67
0.52
0.74
1.70
0.43
0.64
0.50
0.50
0.50
0.59
0.49
0.41
3.00
1.44
0.87
30
90
5
5
5
10
3
2
10
6
5
2
5
14
5
4
10
22
1
20
100
20
30
15
12
40
12
15
40
12
30
12
2
1
1
1
1
1
1
1
1
2
1
1
2
2
3
30
2
1
1
1
4
10
30
40
2
3
0.49
0.60
1.43
14
15
3
40
15
1
1
1
1.66
1.62
0.28
0.90
5
2
14
6
25
15
10
0.41
0.80
3.00
20
7
6
10
30
12
1
0.58
0.64
90
20
50
40
1
3
0.65
0.80
0.87
0.63
2.00
1.50
20
3
3
3
1
1
3
1
40
6.30
6.30
6.30
6.30
6.00
6.00
6.48
6.00
6.40
6.00
6.00
6.00
6.00
6.30
6.30
6.18
6.00
6.00
6.00
6.00
6.00
6.00
6.00
6.00
6.00
6.48
6.34
6.00
6.48
6.48
6.48
6.48
6.00
6.00
6.00
6.48
6.30
6.00
6.48
6.00
6.00
6.00
6.00
6.00
6.48
6.30
6.00
6.00
6.00
6.40
6.00
6.30
6.00
6.30
Sp.-V/AQuan/1999/10/11:11:34
Page 553
22.1 O PEN C LUSTERS / 553
Table 22.4. Old galactic open clusters.
(1)
Cluster
Kin 15
NGC188
Kin 2
NGC559
IC166
NGC752
Ber 66
NGC1193
IC361
NGC1817
Ber 17
Ber 19
Ber 20
Ber 21
NGC2112
Ber 22
NGC2141
NGC2158
NGC2204
NGC2243
NGC2236
Tru 5
Ber 29
Biu 7(Ber 31)
Biu 8(Ber 32)
Tom 2
Mel 66
NGC2420
AM 2a (068-SC07)
Ber 39
NGC2506
Pis 3
NGC2682(M67)
NGC2818
092-SC18a
NGC3680
Har 6(Col 261)
NGC5822
IC4651
Bas 5
Tru 31
NGC6791
NGC6802
NGC6819
NGC6939
Ber 54
IC1369
NGC7044
NGC7142
Kin 11
NGC7762
NGC7789
(2)
RA
(h m s)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
b
Dist.
RGC
Red.
Dia.
Mem.
Rich.
Age
0 33 07
0 47 30
0 50 57
1 29 30
1 52 22
1 57 48
3 04 05
3 05 56
4 18 51
5 12 27
5 20 30
5 24 03
5 32 37
5 51 45
5 53 46
5 58 27
6 02 56
6 07 26
6 15 35
6 29 35
6 29 40
6 36 31
6 53 04
6 57 37
6 58 07
7 03 05
7 26 23
7 38 24
7 38 46
7 46 50
8 00 02
8 31 22
8 51 24
9 16 11
10 14 58
11 25 39
12 37 57
15 04 21
17 24 49
17 52 27
17 59 48
19 20 48
19 30 36
19 41 18
20 31 24
21 03 12
21 12 12
21 13 00
21 45 54
23 47 48
23 49 54
23 57 00
61 51.2
85 14.5
58 11.5
63 18.0
61 51.3
37 41
58 44.5
44 23.0
58 15.0
16 41.0
30 34.7
29 34.2
0 11.3
21 48.7
0 24.6
7 45.4
10 26.8
24 05.8
−18 39.8
−31 17.2
6 49.8
9 28.9
16 55.7
8 17.3
6 25.9
−20 49.2
−47 40.3
21 34.4
−33 50.6
−4 40.5
−10 46.2
−38 39.3
11 49.0
−36 37.7
−64 36.8
−43 14.1
−68 22.4
−54 23.8
−49 56.3
−30 05.8
−28 09.6
37 51
20 17
40 11
60 38
40 28
47 44
42 29
65 48
68 37
68 01
56 43
120.8
122.8
122.9
127.2
130.1
137.2
139.4
146.8
147.5
186.1
175.6
176.9
203.5
186.8
205.9
199.8
198.1
186.6
226.0
239.5
204.4
202.9
198.0
206.3
207.9
232.8
259.6
198.1
248.1
223.5
230.6
257.9
215.6
262.0
287.1
286.8
301.7
321.6
340.1
359.8
2.3
70.0
55.3
74.0
95.9
83.1
89.6
85.9
105.4
117.2
117.2
115.5
−0.9
22.5
−4.7
0.8
−0.2
−23.4
0.2
−12.2
5.7
−13.1
−3.7
−3.6
−17.3
−2.5
−12.6
−8.1
−5.8
1.8
−16.1
−18.0
−1.7
1.0
8.0
5.1
4.4
−6.9
−14.3
19.6
−5.9
10.1
9.9
0.5
31.7
8.6
−6.7
16.9
−5.5
3.6
−7.9
−1.9
−2.3
11.0
0.9
8.5
12.3
−4.1
−0.4
−4.1
9.4
6.5
5.8
−5.4
2880
1680
5700
900
3300
440
5200
4800
2559
1750
4400
4000
8400
8700
750
6000
4200
4800
3100
3750
3400
2400
10500
5200
3100
6200
4475
2410
12400
4340
2750
1300
830
2300
9500
850
2300
740
780
850
1000
3750
1840
2200
1250
2300
1500
3500
1900
2190
800
2200
9.79
8.94
12.07
8.57
10.43
8.30
12.42
12.20
10.24
9.70
12.38
11.99
15.69
16.66
8.66
13.74
12.04
12.78
10.29
10.28
11.18
10.25
18.17
12.85
10.83
12.70
9.76
10.18
17.02
11.48
9.94
8.37
8.58
8.62
10.42
7.80
7.07
7.43
7.28
7.15
7.00
7.58
7.12
7.69
8.22
8.05
8.13
8.49
8.69
9.20
8.39
9.16
0.46
0.12
0.31
0.90
0.77
0.03
1.23
0.12
0.55
0.33
0.50
0.40
0.12
0.70
0.60
0.62
0.35
0.55
0.08
0.01
0.44
0.67
0.21
0.13
0.16
0.30
0.16
0.04
0.44
0.10
0.09
1.35
0.03
0.18
0.26
0.08
0.30
0.15
0.14
0.33
0.42
0.17
0.80
0.45
0.48
0.77
0.50
0.65
0.41
1.00
0.88
0.35
3
15
4
7
8
75
4
3
7
20
8
4
2
6
18
2
10
5
10
5
8
15
2
4
5
3
15
6
3
8
12
6
25
8
5
7
9
35
10
5
5
10
5
5
10
4
5
7
12
6
15
25
12
120
40
60
120
60
30
40
60
60
100
40
20
40
50
20
100
80
100
50
150
20
30
70
50
200
100
120
150
50
200
40
30
100
150
80
30
25
300
50
80
30
40
60
100
50
40
300
5
4
4
2
3
4
2
1
5
5
5
5
4
5
5
5
5
5
4
2
4
4
2
5
3
5
4
4
4
1
5
9.48
9.81
9.78
9.10
9.18
9.26
9.54
9.69
9.10
9.08
9.90
9.58
9.78
9.45
9.60
9.48
9.40
9.08
9.34
9.59
9.10
9.10
9.60
9.90
9.78
9.38
9.65
9.38
9.65
9.81
9.53
9.30
9.65
9.04
9.70
9.28
9.95
9.15
9.28
9.10
9.10
9.90
9.18
9.49
9.34
9.60
9.10
9.18
9.70
9.70
9.26
9.23
Sp.-V/AQuan/1999/10/11:11:34
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22.2
S TAR C LUSTERS
GLOBULAR CLUSTERS IN THE MILKY WAY
Globular star clusters are the old, populous clusters found throughout the halo and spheroid of our
Galaxy. According to current stellar models, all of them are older than 10 Gyr, and have lower heavyelement abundances than the Sun by factors anywhere from 2 to 200. Figures 22.1–22.5 show the
ranges covered by some important properties. In Table 22.5, basic data are summarized for 146 objects
generally accepted to be Milky Way globular clusters, following the catalogs of [31] and [32]. Some
globular clusters may yet be discovered, especially near the galactic center at low latitude where the
foreground reddening is extremely high, but the possible numbers of these remain quite uncertain.
However, recent discussions [31, 33] suggest that the currently known clusters may now represent
80%–90% of the true total in the Milky Way.
Table 22.5 provides basic parameters for known globular clusters in the Milky Way. The literature
survey is complete to 1996. The available measurements for individual clusters are constantly
improving, and readers should refer to the dynamic catalog of [32] for more comprehensive and recent
listings.
Column (1) shows the most often used cluster catalog number (usually NGC), and any other
common name. The source list for cluster names and coordinates is [31].
Columns (2) and (3) show the right ascension and declination (J2000). The typical uncertainty of
cluster center is 5 arcsec.
Columns (4) and (5) show the galactic latitude and longitude in degrees.
Column (6) lists the apparent V magnitude of the horizontal branch, measured from individual
color-magnitude studies of each cluster, or (in a few cases) from the mean magnitude of the RR Lyrae
stars or the brightest red giants. Measurement uncertainties in VHB differ widely but are typically
±0.1 mag.; values thought to be more uncertain than about 0.3 mag. are marked with colons.
Figure 22.1. Spatial distribution of the globular clusters in the Milky Way Galaxy, projected onto the Y Z -plane.
(In this graph, we are looking toward the center of the Galaxy along the X -axis, i.e., along the line joining the Sun
and the galactic center.) The disk and central bulge of the Milky Way are drawn in schematically. The globular
clusters form a roughly spherical distribution through the galactic halo, but with a high central concentration: most
clusters are within a few kiloparsecs of the galactic center. Only a few remote clusters lie outside the borders of
this plot.
Sp.-V/AQuan/1999/10/11:11:34
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22.2 G LOBULAR C LUSTERS IN THE M ILKY WAY / 555
Figure 22.2. Histogram of globular-cluster luminosities MV . Here N is the number of Milky Way globular
clusters per 0.4-magnitude bin. The distribution is strongly peaked at a characteristic absolute magnitude
MV −7.2, with an extended tail to the faint end. These very low-luminosity objects are the sparse Palomar-type
clusters found preferentially in the outer halo.
Figure 22.3. Histogram of globular-cluster metallicity [Fe/H] in the Milky Way. This distribution is strongly
bimodal, with peaks at [Fe/H] −1.5 and −0.6. Almost all the “metal-rich” clusters ([Fe/H] > −0.8) lie in the
central galactic bulge region and form a distinct subpopulation with overall disk-like kinematics; see [34].
Sp.-V/AQuan/1999/10/11:11:34
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S TAR C LUSTERS
Figure 22.4. Histogram of internal relaxation times for the Milky Way globular clusters. Here th (in years) is the
dynamical relaxation time due to normal two-body encounters, at the cluster half-mass radius rh . The majority of
clusters have characteristic relaxation times th in the range 2 × 108 –2 × 109 yr, implying that the inner parts of
most globular clusters must be near-Maxwellian relaxed systems.
Figure 22.5. Histogram of central luminosity density ρ L ,0 (in units of solar luminosities per cubic parsec) for the
Milky Way globular clusters. The central densities of most clusters fall in the broad range 102 –106 L /pc3 , with
a peak near 10 000L /pc3 . See [35] for a general discussion of calculation techniques with references.
Sp.-V/AQuan/1999/10/11:11:34
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22.2 G LOBULAR C LUSTERS IN THE M ILKY WAY / 557
Column (7) gives the foreground reddening from [34, 36, 37], and the individual color-magnitude
studies. The measurement uncertainty in E(B − V ) increases in proportion to the reddening and is
typically 15%.
Column (8) gives the heavy-element abundance (metallicity [Fe/H]) of the cluster. Major sources
are [34, 38]. Many additional data have been taken from numerous more recent (1986–1993)
spectroscopic studies of the giant stars for individual clusters, plus estimates from the individual color
magnitude diagram studies. The typical uncertainty in [Fe/H] is ±0.10.
Column (9) gives the integrated spectral type (ST) of the cluster, from [39]. The internal precision
is typically one spectral subclass.
Column (10) gives the heliocentric radial velocity in km s−1 . Sources are [40–43], plus numerous
other papers published in the interval 1982–1995 for smaller lists of clusters. See [32] for a complete
bibliography. Measurement uncertainties in vr differ widely, from less than 1 km s−1 up to more than
30 km s−1 depending on the method and epoch of measurement.
Column (11) gives the cluster number, repeated from column (1).
Column (12) shows the intrinsic distance modulus, calculated from the horizontal-branch magnitude VHB , foreground reddening, and metallicity: (m − M)0 = VHB − MV (HB) − A V , where we
adopt A V = 3.1E(B − V ) for the ratio of total to selective absorption. The assumed distance scale for
the absolute magnitude of the horizontal branch (or RR Lyrae stars) is MV (HB) = 0.2[Fe/H] + 1.0,
following both observational and theoretical calibrations [44–46].
Column (13) gives the distance of the cluster from the galactic center, in kiloparsecs. We adopt
R0 = 8.0 kpc [29] for the distance of the Sun from the galactic center.
Column (14) gives the integrated V magnitude of the cluster. Sources of integrated photometry
include [37, 47, 48]; for a few of the sparser clusters, a variety of individual color-magnitude or
luminosity-function studies were used to calculate an integrated magnitude. The typical measurement
uncertainty is ±0.15 mag.
Column (15) gives the absolute visual magnitude of the cluster, MV = V − (m − M)V .
Column (16) shows the integrated apparent color index (B − V ) of the cluster (not corrected for
reddening) from [49–51]. Uncertainties in the integrated colors are typically ±0.02 mag.
Column (17) gives the half-mass radius rh , in arc minutes, from [48, 52]. For a few faint or
sparse clusters, we have estimated the half-mass radius from the core radius rc and the correlation
between the cluster central concentration c (see below) and the ratio (rh /rc ). The rh values have
typical uncertainties of 10%.
Column (18) shows the core radius rc , in arc minutes, For some clusters that have undergone core
collapse, rc is strictly not well defined.
Column (19) gives the central concentration parameter, c = log(rt /rc ), where rt is the cluster tidal
radius and rc the core radius, from [52]. Typical uncertainties in c are ±0.2. Clusters believed to have
undergone core collapse are indicated by “c” [52].
Column (20) gives the logarithm (base 10) of the dynamical relaxation time, in years, at the halfmass radius rh , from [35]. These values are indicative time scales only and may be uncertain by up to
a factor of 2 for individual clusters; see the discussion in [35].
Column (21) shows the central surface brightness in V magnitudes per square arc second
from [37, 52]. These are uncertain at typically ±0.15 mag. (colons if more than ±0.4 mag.).
Column (22) gives the horizontal-branch population ratio (HBR) (B − R)/(B + V + R), where
B is the number of HB stars bluer than the RR Lyrae region, V is the number of RR Lyrae stars, and
R is the number of HB stars redder than the RR Lyrae region. Sources are [45, 53–55]. The typical
uncertainty is ±0.05.
Column (23) gives the specific frequency of RR Lyrae stars, from [56]. SRR is defined as the
number of RR Lyrae variables in the cluster per unit (MV = −7.5) cluster luminosity.
Sp.-V/AQuan/1999/10/11:11:34
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S TAR C LUSTERS
Table 22.5. Galactic globular clusters.a
(1)
Cluster
NGC104(47 Tuc)
NGC288
NGC362
NGC1261
Pal 1
AM 1(E1)
Eridanus
Pal 2
NGC1851
NGC1904(M79)
NGC2298
NGC2419
Pyxis
NGC2808
E3
Pal 3
NGC3201
Pal 4
NGC4147
NGC4372
Rup 106
NGC4590(M68)
NGC4833
NGC5024(M53)
NGC5053
NGC5139(ω Cen)
NGC5272(M3)
NGC5286
AM 4
NGC5466
NGC5634
NGC5694
IC4499
NGC5824
Pal 5
NGC5897
NGC5904(M5)
NGC5927
NGC5946
BH 176
NGC5986
Lyngå 7
Pal 14(AvdB)
NGC6093(M80)
NGC6121(M4)
NGC6101
NGC6144
NGC6139
Terzan 3
NGC6171(M107)
1636-283(E452-SC11)
NGC6205(M13)
NGC6229
NGC6218(M12)
NGC6235
NGC6254(M10)
(2)
RA
(h m s)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
b
VHB
Red.
[Fe/H]
ST
vr
00 24 05.2
00 52 47.5
01 03 14.3
03 12 15.3
03 33 23.0
03 55 02.7
04 24 44.5
04 46 05.9
05 14 06.3
05 24 10.6
06 48 59.2
07 38 08.5
09 07 57.8
09 12 02.6
09 20 59.3
10 05 31.4
10 17 36.8
11 29 16.8
12 10 06.2
12 25 45.4
12 38 40.2
12 39 28.0
12 59 35.0
13 12 55.3
13 16 27.0
13 26 45.9
13 42 11.2
13 46 26.5
13 55 50.1
14 05 27.3
14 29 37.3
14 39 36.5
15 00 18.5
15 03 58.5
15 16 05.3
15 17 24.5
15 18 33.8
15 28 00.5
15 35 28.5
15 39 07.3
15 46 03.5
16 11 03.0
16 11 04.9
16 17 02.5
16 23 35.5
16 25 48.6
16 27 14.1
16 27 40.4
16 28 40.1
16 32 31.9
16 39 25.5
16 41 41.5
16 46 58.9
16 47 14.5
16 53 25.4
16 57 08.9
−72 04 51
−26 35 24
−70 50 54
−55 13 01
+79 34 50
−49 36 52
−21 11 13
+31 22 51
−40 02 50
−24 31 27
−36 00 19
+38 52 55
−37 13 17
−64 51 47
−77 16 57
+00 04 17
−46 24 40
+28 58 25
+18 32 31
−72 39 33
−51 09 01
−26 44 34
−70 52 29
+18 10 09
+17 41 53
−47 28 37
+28 22 32
−51 22 24
−27 10 22
+28 32 04
−05 58 35
−26 32 18
−82 12 49
−33 04 04
−00 06 41
−21 00 37
+02 04 58
−50 40 22
−50 39 34
−50 03 02
−37 47 10
−55 18 52
+14 57 29
−22 58 30
−26 31 31
−72 12 06
−26 01 29
−38 50 56
−35 21 13
−13 03 13
−28 23 52
+36 27 37
+47 31 40
−01 56 52
−22 10 38
−04 05 58
305.9
152.3
301.5
270.5
130.1
258.4
218.1
170.5
244.5
227.2
245.6
180.4
261.3
282.2
292.3
240.1
277.2
202.3
252.9
301.0
300.9
299.6
303.6
333.0
335.7
309.1
42.2
311.6
320.1
42.2
342.2
331.1
307.4
332.6
0.9
342.9
3.9
326.6
327.6
328.4
337.0
328.8
28.8
352.7
351.0
317.7
351.9
342.4
345.1
3.4
351.9
59.0
73.6
15.7
358.9
15.1
−44.9
−89.4
−46.2
−52.1
19.0
−48.5
−41.3
−9.1
−35.0
−29.4
−16.0
25.2
7.0
−11.3
−19.0
41.9
8.6
71.8
77.2
−9.9
11.7
36.1
−8.0
79.8
78.9
15.0
78.7
10.6
33.5
73.6
49.3
30.4
−20.5
22.1
45.9
30.3
46.8
4.9
4.2
4.3
13.3
−2.8
42.2
19.5
16.0
−15.8
15.7
6.9
9.2
23.0
12.1
40.9
40.3
26.3
13.5
23.1
14.06
15.38
15.43
16.70
16.13
20.96
20.23
20.70:
16.15
16.15
16.11
20.45
19.25
16.19
14.80:
20.45
14.80
20.65
17.01
15.30
17.85
15.68
15.45
16.90
16.65
14.53
15.65
16.65
18.00:
16.62
17.75
18.50
17.65
18.60
17.51
16.35
15.06
16.60
17.80:
19.00:
16.50
17.25
20.04
15.86
13.45
16.60
16.60
17.80:
18.80:
15.70
16.66
14.90
18.00
14.90
16.70
14.65
0.04
0.03
0.05
0.02
.15
0.00
0.02
1.36
0.02
0.01
0.13
0.03
0.25
0.23
0.30
0.03
0.21
0.01
0.02
0.45
0.21
0.04
0.33
0.01
0.03
0.12
0.01
0.24
0.04
0.00
0.05
0.09
0.24
0.14
0.03
0.08
0.03
0.47
0.55
0.77
0.27
0.73
0.04
0.18
0.36
0.04
0.32
0.75
0.32
0.33
0.50
0.02
0.01
0.17
0.36
0.28
−0.76
−1.24
−1.16
−1.35
−0.80
−1.80
−1.46
G4
F9
F7
−19
−46
223
53
−1.26
−1.54
−1.85
−2.12
−1.20
−1.37
−0.80
−1.66
−1.45
−1.48
−1.83
−2.09
−1.69
−2.06
−1.79
−2.07
−2.29
−1.57
−1.57
−1.79
−2.00
−2.22
−1.82
−1.86
−1.62
−1.85
−1.38
−1.80
−1.33
−0.37
−1.38
F7
F5
F5
F5
116
−24
−133:
321
207
149
−20
F7
100
−1.67
−0.62
−1.52
−1.62
−1.18
−1.82
−1.73
−1.65
F5
F6
F8
F5:
F5/6
F6/7
92
8
77
7
70
361
189
7
−1.04
G0
−34
−1.56
−1.44
−1.48
−1.40
−1.52
F6
F7
F8
F9:
F3
−247
−154
−43
87
75
F5
F6
F5
83
494
75
183
73
−44
−95
201
−79
43
232
−147
54
F3/4
F4
108
−45
−146
F6
F2/3
F5
F2/3
F3
F6
F4
F7
F7
G2
F7/8
−38
−55
102
52
−100
119
Sp.-V/AQuan/1999/10/11:11:34
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22.2 G LOBULAR C LUSTERS IN THE M ILKY WAY / 559
Table 22.4. (Continued.)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
(18)
(19)
(20)
(21)
(22)
(23)
Cluster
DM
RGC
V
MV
Col.
rh
rc
c
log t
µV
HBR
SRR
13.09
14.53
14.51
15.91
14.82
20.32
19.46
15.68
15.34
15.43
15.08
19.78
17.72
14.75
13.03
19.69
13.44
19.92
16.31
13.32
16.54
14.97
13.78
16.28
16.01
13.47
14.93
15.26
17.28
16.06
16.96
17.59
16.23
17.54
16.69
15.46
14.23
14.22
15.37
15.81
15.00
14.11
19.22
14.63
15.84
11.57
14.95
14.80
17.01
13.89
14.31
14.15
13.67
17.26
14.86
13.09
7.3
11.4
9.0
17.1
15.5
117.2
83.0
21.6
16.3
18.1
15.4
97.7
37.0
10.7
7.6
89.9
8.8
98.8
20.5
6.9
17.7
9.9
6.8
18.6
16.5
6.3
11.6
8.6
24.2
16.6
20.7
27.5
14.6
26.0
17.2
7.3
6.0
4.5
6.7
8.8
4.5
4.2
64.9
3.0
10.6
6.1
3.2
3.0
17.7
3.4
2.1
8.2
4.3
27.7
2.5
4.7
3.95
8.09
6.40
8.29
13.52
15.72
14.70
13.04
7.14
7.73
9.29
10.39
12.90
6.20
11.35
14.26
6.75
14.20
10.32
7.24
10.90
7.84
6.91
7.61
9.47
3.68
6.19
7.34
15.90
9.04
9.47
10.17
9.76
9.09
11.75
8.53
5.65
8.01
9.61
14.00
7.52
−9.26
−6.54
−8.26
−7.68
−1.77
−4.60
−4.82
−6.86
−8.26
−7.73
−6.19
−9.48
−5.59
−9.26
−2.61
−5.52
−7.34
−5.75
−6.06
−7.48
−6.29
−7.25
−7.90
−8.70
−6.64
−10.16
−8.77
−8.67
−1.50
−7.02
−7.64
−7.70
−7.21
−8.88
−5.04
−7.18
−8.68
−7.66
−7.47
−4.20
−8.31
0.88
0.65
0.77
0.72
0.96
0.72
0.79
2.08
0.76
0.65
0.75
0.66
0.37
1.42
0.17
0.39
0.32
0.12
0.25
0.15
0.08
0.16
0.34
0.35
1.38
0.26
1.87
0.48
1.45
0.55
0.10
1.75
1.00
0.69
1.00
0.37
2.25
2.58
0.50
0.29
0.42
1.96
0.21
0.06
0.96
0.05
2.90
1.96
0.40
0.42
0.08
2.04
0.96
1.94c:
1.27
1.50
1.23
1.10
1.91
2.24
1.72
1.28
1.40
0.65
1.77
0.75
1.00
1.31
0.78
1.80
1.30
0.70
1.64
1.25
1.78
0.82
1.24
1.85
1.46
0.50
1.43
1.60
1.84
1.11
2.45
0.74
0.79
1.87
1.60
2.50c
9.24
8.99
8.43
8.81
7.53
9.46
14.43
19.95
14.88
17.65
22.16
23.86
22.81
19.39
14.15
16.23
18.79
19.83
−0.99
0.98
−0.87
−0.71
−1.00
−0.93
−1.00
0.4
2.4
6.4
16.1
0.0
43.4
0.0
0.0
10.9
5.7
10.0
6.0
0.74
0.72
1.31
1.29
2.79
2.22
0.81
0.75
0.48
0.50
0.40
0.28
0.52
0.80
0.78
0.73
1.35
0.76
2.06
0.66
2.68
0.54
0.43
3.90
1.10
1.55
2.41
1.11
3.50
4.18
1.12
0.69
0.42
2.25
0.54
0.33
1.50
0.36
2.96
2.11
2.11
1.15
0.69
0.90
1.05
0.63
1.22
8.78
14.74
7.33
9.16
5.63
9.01
8.99
12.00
7.93
12.00
5.78
6.70
9.39
9.97
6.60
−4.60
−7.85
−6.80
−7.06
−6.94
−8.14
−6.00
−6.98
−3.86
−8.43
−7.50
−7.90
−6.01
−7.35
1.10
0.15
1.15
0.83
0.94
0.14
1.18
0.54
0.72
1.95
0.80
1.59
1.55
1.80
0.70
1.51
9.66
8.32
9.22
8.64
8.94
8.59
1.10
1.15
0.65
1.71
3.65
1.62
0.82
1.30
2.70
0.68
0.83
0.70
1.05
0.90
1.49
2.16
0.37
0.84
1.81
0.88
0.66
0.13
0.36
0.86
1.49
1.38
1.61
1.33
1.40
8.96
8.86
8.90
8.56
8.56
NGC104
NGC288
NGC362
NGC1261
Pal 1
AM 1
Eridanus
Pal 2
NGC1851
NGC1904
NGC2298
NGC2419
Pyxis
NGC2808
E3
Pal 3
NGC3201
Pal 4
NGC4147
NGC4372
Rup 106
NGC4590
NGC4833
NGC5024
NGC5053
NGC5139
NGC5272
NGC5286
AM 4
NGC5466
NGC5634
NGC5694
IC4499
NGC5824
Pal 5
NGC5897
NGC5904
NGC5927
NGC5946
BH 176
NGC5986
Lyngå 7
Pal 14
NGC6093
NGC6101
NGC6121
NGC6144
NGC6139
Terzan 3
NGC6171
1636-283
NGC6205
NGC6218
NGC6229
NGC6235
NGC6254
0.92
0.96
0.59
1.10
0.63
0.93
0.64
0.65
0.78
0.69
0.88
0.67
0.67
0.69
0.91
0.75
0.84
0.68
1.03
0.96
1.40
8.04
8.50
8.66
8.36
10.28
8.77
9.64
8.79
9.54
8.37
9.23
8.90
8.77
9.42
9.59
9.72
9.02
8.61
9.37
8.98
8.79
9.45
9.18
9.59
9.31
9.13
8.71
8.84
8.75
15.17
23.10
23.08
18.77
23.54
17.63
20.51
21.82
18.67
18.45
17.39
22.19
16.77
16.34
16.07
24.75
21.28
17.49
16.34
20.92
15.08
24.67
20.49
16.05
17.45:
17.42
23.36
17.56
25.55
15.19
20.12
17.88
20.27
17.30
22.52
18.84
20.75
16.80
18.17
16.99
18.98
17.69
−0.36
0.89
0.93
0.86
−1.00
−0.49
−0.82
0.08
−1.00
0.55
1.00
−0.82
0.17
0.93
0.76
0.52
0.08
0.86
0.58
1.00
0.11
0.82
−0.40
0.86
0.38
−1.00
−1.00
0.97
−1.00
−1.00
0.93
0.84
−0.06
1.00
0.4
0.0
18.5
98.5
0.0
60.5
0.0
51.5
12.5
14.5
22.1
13.1
80.4
5.5
43.4
6.1
0.0
130.1
7.6
48.4
9.4
41.6
0.0
3.1
4.7
4.3
20.9
76.8
0.0
2.8
−0.73
35.6
0.97
0.96
0.25
0.89
0.98
2.1
0.0
13.9
11.8
1.1
Sp.-V/AQuan/1999/10/11:11:34
Page 560
560 / 22
S TAR C LUSTERS
Table 22.4. (Continued.)
(1)
Cluster
NGC6256
Pal 15
NGC6266(M62)
NGC6273(M19)
NGC6284
NGC6287
NGC6293
NGC6304
NGC6316
NGC6341(M92)
NGC6325
NGC6333(M9)
NGC6342
NGC6356
NGC6355
NGC6352
Terzan 2(HP 3)
NGC6366
Terzan 4(HP 4)
HP 1(BH 229)
NGC6362
Liller 1
NGC6380(Ton 1)
Terzan 1(HP 2)
Ton 2(Pismis 26)
NGC6388
NGC6402(M14)
NGC6401
NGC6397
Pal 6
NGC6426
Djorg 1
Terzan 5(Terzan 11)
NGC6440
NGC6441
Terzan 6(HP 5)
NGC6453
UKS 1
NGC6496
Terzan 9
Djorg 2(E456-SC38)
NGC6517
Terzan 10
NGC6522
NGC6535
NGC6528
NGC6539
NGC6540(Djorg 3)
NGC6544
NGC6541
NGC6553
NGC6558
IC1276(Pal 7)
Terzan 12
NGC6569
NGC6584
(2)
RA
(h m s)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
b
VH B
Red.
[Fe/H]
ST
vr
16 59 32.6
17 00 02.4
17 01 12.6
17 02 37.7
17 04 28.8
17 05 09.4
17 10 10.4
17 14 32.5
17 16 37.4
17 17 07.3
17 17 59.2
17 19 11.8
17 21 10.2
17 23 35.0
17 23 58.6
17 25 29.2
17 27 33.4
17 27 44.3
17 30 38.9
17 31 05.2
17 31 54.8
17 33 24.5
17 34 28.0
17 35 47.8
17 36 10.5
17 36 17.0
17 37 36.1
17 38 36.9
17 40 41.3
17 43 42.2
17 44 54.7
17 47 28.3
17 48 04.9
17 48 52.6
17 50 12.9
17 50 46.4
17 50 51.8
17 54 27.2
17 59 02.0
18 01 38.8
18 01 49.1
18 01 50.6
18 02 57.4
18 03 34.1
18 03 50.7
18 04 49.6
18 04 49.8
18 06 08.6
18 07 20.6
18 08 02.2
18 09 15.6
18 10 18.4
18 10 44.2
18 12 15.8
18 13 38.9
18 18 37.7
−37 07 17
−00 32 31
−30 06 44
−26 16 05
−24 45 53
−22 42 29
−26 34 54
−29 27 44
−28 08 24
+43 08 11
−23 45 57
−18 30 59
−19 35 14
−17 48 47
−26 21 13
−48 25 22
−30 48 08
−05 04 36
−31 35 44
−29 58 54
−67 02 53
−33 23 20
−39 04 09
−30 28 11
−38 33 12
−44 44 06
−03 14 45
−23 54 32
−53 40 25
−26 13 21
+03 10 13
−33 03 56
−24 48 45
−20 21 34
−37 03 04
−31 16 31
−34 35 55
−24 08 43
−44 15 54
−26 50 23
−27 49 33
−08 57 32
−26 04 00
−30 02 02
−00 17 49
−30 03 21
−07 35 09
−27 45 55
−24 59 51
−43 42 20
−25 54 28
−31 45 49
−07 12 27
−22 44 31
−31 49 35
−52 12 54
347.8
18.9
353.6
356.9
358.3
0.1
357.6
355.8
357.2
68.3
1.0
5.5
4.9
6.7
359.6
341.4
356.3
18.4
356.0
357.4
325.6
354.8
350.2
357.6
350.8
345.6
21.3
3.5
338.2
2.1
28.1
356.7
3.8
7.7
353.5
358.6
355.7
5.1
348.0
3.6
2.8
19.2
4.4
1.0
27.2
1.1
20.8
3.3
5.8
349.3
5.2
0.2
21.8
8.4
0.5
342.1
3.3
24.3
7.3
9.4
9.9
11.0
7.8
5.4
5.8
34.9
8.0
10.7
9.7
10.2
5.4
−7.2
2.3
16.0
1.3
2.1
−17.6
−0.2
−3.4
1.0
−3.4
−6.7
14.8
4.0
−12.0
1.8
16.2
−2.5
1.7
3.8
−5.0
−2.2
−3.9
0.8
−10.0
−2.0
−2.5
6.8
−1.9
−3.9
10.4
−4.2
6.8
−3.3
−2.2
−11.2
−3.0
−6.0
5.7
−2.1
−6.7
−16.4
18.20:
20.00
16.30
16.40:
17.30
17.00
16.50
16.25
17.78
15.10
18.30
16.30
16.90
17.50
17.20
15.13
20.10
15.65
0.84
0.40
0.47
0.37
0.28
0.59
0.39
0.52
0.55
0.02
0.89
0.36
0.44
0.29
0.75
0.21
1.42
0.69
20.10:
15.34
25.23:
1.50
0.09
2.95
1.38
1.64
0.91
0.38
0.60
0.85
0.18
1.53
0.35
1.70
1.87
1.09
0.45
2.04
0.61
2.93
0.13
1.75
1.00
1.08
2.60
0.50
0.32
0.62
1.00
0.60
0.74
0.12
0.84
0.42
0.92
1.57
0.56
0.11
−0.70
−1.90
−1.29
−1.68
−1.32
−2.05
−1.92
−0.59
−0.55
−2.33
−1.17
−1.78
−0.65
−0.50
−1.50
−0.70
−0.25
−0.82
−0.94
−0.43
−1.06
+0.22
19.95
18.20:
17.25
17.20
17.70
12.87
19.70:
18.00:
20.80:
20.20:
18.70:
17.10
21.44
17.70:
24.14:
16.47
20.58:
19.50:
19.10
23.42:
16.40
15.73
17.10
18.33
15.30:
14.90:
15.30
16.60
16.70
18.40:
17.10:
16.53
F9:
F7
F9
F5
F3
G3
G2
F2
G0
F5/6
G3/4
G3
G0
G4
G3
−0.35
−0.60
−1.39
−1.12
−1.91
−0.10
−2.20
−0.29
−0.34
−0.53
−0.65
−1.53
−1.20
−0.64
−1.00
69
−68
129
30
−208
−99
−105
71
−120
3
229
81
27
−177
−115
109
−122
−50
53
−13
52
35
G2
F4
F9
F4
G1:
G4
G2
F8
81
−111
−65
19
201
−162
−94
−79
18
126
−84
G4
−98
59
F8
−40
−1.37
−0.70
−1.52
−1.80
−0.17
−0.66
−1.00
−1.56
−1.83
−0.25
−1.44
F7/8
G0
G3
G4:
−9
−215
165
−46
F9
F6
G4
F7
−17
−154
−24
−144
−0.86
−1.49
G1:
F6
−28
223
Sp.-V/AQuan/1999/10/11:11:34
Page 561
22.2 G LOBULAR C LUSTERS IN THE M ILKY WAY / 561
Table 22.4. (Continued.)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
(18)
(19)
(20)
(21)
(22)
(23)
Cluster
DM
RGC
V
MV
Col.
rh
rc
c
log t
µV
HBR
SRR
14.74
18.14
14.10
14.59
15.70
14.58
14.68
13.76
15.19
14.77
14.50
14.54
14.67
15.70
14.18
13.62
14.75
12.67
14.27
2.0
35.8
1.9
1.4
6.1
1.6
1.3
2.5
3.1
1.6
9.4
1.7
1.7
6.2
1.4
3.5
1.1
5.1
5.0
8.0
0.5
2.3
11.29
14.00
6.45
6.77
8.83
9.35
8.22
8.22
8.43
10.33
6.44
7.72
9.66
8.25
9.14
7.96
14.29
9.20
7.73
16.00
11.59
16.77
11.31
15.90
6.72
12.24
7.59
9.45
5.73
11.55
11.01
13.60
13.85
9.20
7.15
10.08
13.85
17.29
8.54
16.00
9.90
10.23
14.90
8.27
10.47
9.60
9.33
9.30
7.77
6.30
8.06
9.26
10.34
15.63
8.55
8.27
−6.05
−5.38
−9.11
−8.97
−7.73
−7.06
−7.66
−7.15
−8.46
−7.20
−8.13
−7.94
−6.37
−8.35
−7.36
−6.31
−4.86
−5.61
−6.82
1.69
0.85
1.21
1.23
1.25
0.78
0.75
0.91
1.41
0.71
0.94
1.09
0.95
0.88
0.74
0.87
2.00
1.52
2.63
2.18
0.02
1.21
0.18
0.43
0.07
0.26
0.05
0.21
0.17
0.03
0.23
0.58
0.05
0.23
0.05
0.83
0.03
1.83
1.32
2.50c
0.60
1.70c:
1.53
2.50c
1.60
2.50c
1.80
1.55
2.50c
1.81
1.15
2.50c
1.54
2.50c
1.10
2.50c
0.92
1.10
8.41
17.89
24.87
15.35
16.82
16.65
18.33
16.18:
17.34
17.40
17.56
15.58
17.40
17.44:
17.09
18.05:
18.42:
21.58
21.24
19.19
1.00
0.28
0.0
19.8
0.5
3.2
3.0
3.4
0.0
3.10
0.45
0.75
3.82
0.67
1.08
1.29
1.91
2.33
1.06
0.96
1.26
0.83
0.58
0.64
0.37
0.44
0.86
1.87
0.78
0.83
0.62
0.03
0.06
0.34
0.04
0.12
0.54
0.83
0.25
0.05
0.66
0.26
0.50
0.18
0.13
0.11
0.07
0.05
0.15
1.05
0.03
0.33
0.06
2.50c
2.30c:
1.55c:
2.50c
1.70
1.30
1.60
1.69
2.50c
1.10
1.70
1.50
1.74
1.70
1.85
2.50c
2.50c
2.10c:
0.70
2.50c
1.50
1.82
9.49
1.04
0.77
0.43
1.67
0.24
1.77
1.19
1.55
1.61
2.35
0.84
1.33
0.80
0.05
0.42
0.09
0.54
0.03
0.05
0.30
0.55
0.03
1.08
0.83
0.37
0.59
2.50c
1.30
2.29
1.60
2.50c
1.63c:
2.00c:
1.17
2.50c
1.29
0.57
1.27
1.20
8.25
8.05
7.73
8.38
NGC6256
Pal 15
NGC6266
NGC6273
NGC6284
NGC6287
NGC6293
NGC6304
NGC6316
NGC6325
NGC6341
NGC6333
NGC6342
NGC6356
NGC6355
NGC6352
Terzan 2
NGC6366
NGC6362
Terzan 4
HP 1
Liller 1
NGC6380
Terzan 1
NGC6388
Ton 2
NGC6402
NGC6401
NGC6397
Pal 6
NGC6426
Djorg 1
Terzan 5
NGC6440
NGC6441
NGC6453
Terzan 6
UKS 1
NGC6496
Terzan 9
Djorg 2
NGC6517
Terzan 10
NGC6522
NGC6535
NGC6528
NGC6539
NGC6540
NGC6544
NGC6541
NGC6553
NGC6558
IC1276
Terzan 12
NGC6569
NGC6584
14.54
15.04
13.94
15.19
14.58
14.62
14.29
11.69
13.98
16.36
14.73
13.46
14.39
14.81
15.12
14.25
14.30
15.19
14.36
15.60
15.03
14.50
14.15
14.10
14.21
14.36
12.64
11.92
14.29
13.05
14.69
14.75
1.9
3.9
1.4
3.7
1.1
6.1
1.8
12.6
3.1
3.1
1.2
1.7
2.7
1.0
1.0
3.9
0.8
5.2
3.8
0.7
1.3
3.9
1.2
3.0
4.6
5.6
2.2
4.0
1.1
3.4
14.54
15.49
0.9
6.1
1.19
1.03
0.99
1.20
0.96
1.31
1.39
1.66
0.63
0.97
1.26
1.13
1.48
1.06
1.44
0.85
−7.60
−7.42
2.01
−3.12
−9.65
−5.16
−8.89
−7.47
−6.52
−7.17
−6.43
−6.40
−5.41
−8.57
−9.06
−6.93
−6.72
−6.09
−7.06
−3.78
−8.80
−8.14
−7.66
−7.43
−4.62
−6.53
−8.13
−5.20
−6.44
−8.37
−7.59
−6.73
−7.26
−7.72
−7.56
1.17
1.25
1.58
0.73
2.83
1.02
2.77
1.97
1.27
1.31
0.98
1.75
1.21
0.94
1.53
1.83
1.46
0.76
1.73
1.11
1.76
1.34
0.76
8.55
9.28
8.54
8.14
8.52
8.56
8.92
7.91
8.56
8.49
8.58
9.11
8.47
8.71
8.55
8.50
8.83
7.65
8.70
9.19
9.13
8.35
8.86
8.15
8.66
7.97
8.46
7.89
7.82
8.58
8.33
9.13
9.15
8.57
8.53
21.29
23.15:
19.96
25.09
14.55
22.16
18.41
18.67
15.65
21.58
20.37
23.10
20.33:
17.02
14.99
17.35
20.76
25.52
20.10
23.21
19.50
17.77
21.28
16.14:
20.22:
16.91
19.31
16.40
17.13:
15.58
18.15
17.08:
21.66
23.75
18.08
17.79
0.98
0.90
−1.00
−1.00
0.91
0.87
−1.00
−1.00
14.0
6.0
−1.00
−1.00
−0.97
−0.58
0.0
5.7
61.6
−1.00
0.0
0.0
0.7
0.65
0.98
−1.00
23.9
22.5
0.0
32.2
−1.00
−1.00
0.5
0.0
0.0
−1.00
0.0
0.71
1.00
−1.00
−1.00
5.3
0.0
0.0
0.0
1.00
1.00
−1.00
−0.15
0.0
0.9
6.1
1.2
8.2
40.8
Sp.-V/AQuan/1999/10/11:11:34
Page 562
562 / 22
S TAR C LUSTERS
Table 22.4. (Continued.)
(1)
Cluster
NGC6624
NGC6626(M28)
NGC6638
NGC6637(M69)
NGC6642
NGC6652
NGC6656(M22)
Pal 8
NGC6681(M70)
NGC6712
NGC6715(M54)
NGC6717(Pal 9)
NGC6723
NGC6749
NGC6752
NGC6760
NGC6779(M56)
Terzan 7
Pal 10
Arp 2
NGC6809(M55)
Terzan 8
Pal 11
NGC6838(M71)
NGC6864(M75)
NGC6934
NGC6981(M72)
NGC7006
NGC7078(M15)
NGC7089(M2)
NGC7099(M30)
Pal 12
Pal 13
NGC7492
22.3
(2)
RA
(h m s)
(3)
Dec.
(◦ )
(4)
(5)
(6)
(7)
(8)
(9)
(10)
b
VH B
Red.
[Fe/H]
ST
vr
18 23 40.5
18 24 32.9
18 30 56.2
18 31 23.2
18 31 54.3
18 35 45.7
18 36 24.2
18 41 29.9
18 43 12.7
18 53 04.3
18 55 03.3
18 55 06.2
18 59 33.2
19 05 15.3
19 10 51.8
19 11 12.1
19 16 35.5
19 17 43.7
19 18 02.1
19 28 44.1
19 39 59.4
19 41 45.0
19 45 14.4
19 53 46.1
20 06 04.8
20 34 11.6
20 53 27.9
21 01 29.5
21 29 58.3
21 33 29.3
21 40 22.0
21 46 38.8
23 06 44.4
23 08 26.7
−30 21 40
−24 52 12
−25 29 47
−32 20 53
−23 28 35
−32 59 25
−23 54 12
−19 49 33
−32 17 31
−08 42 22
−30 28 42
−22 42 03
−36 37 54
+01 54 03
−59 58 55
+01 01 50
+30 11 05
−34 39 27
+18 34 18
−30 21 14
−30 57 44
−34 00 01
−08 00 26
+18 46 42
−21 55 17
+07 24 15
−12 32 13
+16 11 15
+12 10 01
−00 49 23
−23 10 45
−21 15 03
+12 46 19
−15 36 41
2.8
7.8
7.9
1.7
9.8
1.5
9.9
14.1
2.9
25.4
5.6
12.9
0.1
36.2
336.5
36.1
62.7
3.4
52.4
8.5
8.8
5.8
31.8
56.7
20.3
52.1
35.2
63.8
65.0
53.4
27.2
30.5
87.1
53.4
−7.9
−5.6
−7.2
−10.3
−6.4
−11.4
−7.6
−6.8
−12.5
−4.3
−14.1
−10.9
−17.3
−2.2
−25.6
−3.9
8.3
−20.1
2.7
−20.8
−23.3
−24.6
−15.6
−4.6
−25.7
−18.9
−32.7
−19.4
−27.3
−35.8
−46.8
−47.7
−42.7
−63.5
16.11
15.70
16.50
15.85
16.30:
15.85
14.15
17.27
15.60
16.25
18.17
15.50
15.46
19.20:
13.70
17.50
16.16
17.76
19.50:
18.30
14.40
18.03
17.35
14.44
17.47
16.82
16.90
18.80
15.83
16.05
15.10
17.13
17.74
17.63
0.27
0.41
0.40
0.17
0.40
0.09
0.34
0.33
0.07
0.46
0.15
0.21
0.04
1.12
0.04
0.78
0.20
0.06
1.15
0.11
0.07
0.14
0.34
0.25
0.16
0.11
0.05
0.05
0.09
0.05
0.03
0.02
0.05
0.00
−0.42
−1.45
−0.99
−0.71
−1.35
−0.96
−1.64
−0.48
−1.51
−1.01
−1.59
−1.32
−1.12
G4/5
F8
G0
G2/3
F8
G3
F5
54
16
10
39
−57
−112
−149
−43
219
−108
142
2
−82
−1.61
−0.52
−1.94
−0.62
F4/5
G5
F5
−1.76
−1.81
−1.87
−0.39
−0.73
−1.32
−1.54
−1.54
−1.68
−2.22
−1.62
−2.12
−0.93
−1.79
−1.51
F5
F9
F7/8
F6
F9
F4
G1
F9
F7/8
F7
F6
F3/4
F4
F3
−27
−27
−136
166
115
175
130
−68
−23
−189
−411
−289
−378
−107
−7
−184
28:
−28
−188
GLOBULAR CLUSTERS IN OTHER GALAXIES
Globular clusters can be found in all large galaxies and many small ones, although in quite different
numbers. The specific frequency S N [57, 58] is defined as the number of globular clusters per unit
galaxy luminosity; if NGC is the total cluster population and MVT the visual absolute magnitude of the
entire galaxy, then S N ≡ NGC 100.4(MV +15) . S N is listed in Table 22.5 for 73 galaxies within which old
halo globular-cluster populations have been found.
Typically, the “old” globular clusters (that is, objects with ages ∼ 10 Gyr or more) make up 0.1%–
1% of the total light of a galaxy. They are usually present in much larger numbers within elliptical
galaxies than in spiral or irregular galaxies, although even for a given type of galaxy there are large
differences in specific frequency that depend roughly—although not exclusively—on environment: E
galaxies in rich surroundings like the Virgo or Fornax clusters tend to contain more globular clusters
than otherwise-similar galaxies in the field or in small groups. Some very luminous cD-type galaxies,
like M87 in Virgo, contain extremely large populations of globular clusters (tens of thousands in one
galaxy), extending out into their halos to radial distances of 100 kpc and more.
T
Sp.-V/AQuan/1999/10/11:11:34
Page 563
22.3 G LOBULAR C LUSTERS IN OTHER G ALAXIES / 563
Table 22.4. (Continued.)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
(18)
(19)
(20)
(21)
(22)
(23)
Cluster
DM
RGC
V
MV
Col.
rh
rc
c
log t
µV
HBR
SRR
14.36
13.72
14.46
14.47
14.33
14.76
12.42
15.34
14.69
14.03
17.02
14.11
14.56
14.93
12.90
14.19
16.70
14.93
15.14
17.31
13.54
16.97
15.37
12.81
16.24
15.79
16.05
17.98
14.99
15.22
14.43
16.25
16.94
16.93
1.3
2.7
1.5
1.5
1.7
2.0
5.1
4.5
2.0
3.6
17.8
2.5
2.4
5.7
5.3
4.8
14.6
9.3
8.6
21.8
4.0
17.9
7.0
6.7
11.7
11.7
12.2
36.9
10.2
10.0
6.9
14.7
25.5
23.5
7.87
6.79
9.02
7.64
9.13
8.62
5.10
11.02
7.87
8.10
7.60
9.28
7.01
12.44
5.40
8.88
12.00
8.27
13.22
12.30
6.32
12.40
9.80
8.19
8.52
8.83
9.27
10.56
6.20
6.47
7.19
11.99
13.80
11.29
−7.32
−8.20
−6.68
−7.35
−6.44
−6.42
−8.38
−5.35
−7.03
−7.35
−9.89
−5.48
−7.67
−5.96
−7.62
−7.72
−4.88
−7.28
−5.48
−5.35
−7.44
−5.00
−6.63
−5.40
−8.21
−7.30
−6.94
−7.58
−9.07
−8.90
−7.33
−4.33
−3.30
−5.64
1.11
1.08
1.15
1.01
1.11
0.94
0.98
1.22
0.72
1.17
0.85
1.00
0.75
2.14
0.66
1.66
0.82
1.56
0.66
0.83
0.73
0.65
3.26
0.57
0.93
1.37
0.49
0.68
1.61
0.56
2.34
2.18
0.97
1.16
1.52
1.91
2.89
1.00
1.49
1.65
0.47
0.60
0.88
0.38
1.06
0.93
1.15
1.28
0.46
1.22
0.06
0.24
0.26
0.34
0.10
0.07
1.42
0.40
0.03
0.94
0.11
0.08
0.94
0.47
0.17
0.33
0.61
0.37
0.80
1.59
2.83
1.00
2.00
0.63
0.10
0.25
0.54
0.24
0.07
0.34
0.06
0.20
0.48
0.83
2.50c
1.67
1.40
1.39
1.99
1.80
1.31
1.53
2.50c
0.90
1.84
2.07c:
1.05
0.75
2.50c
1.59
1.08
1.37
1.56
0.90
0.76
0.60
0.69
1.15
1.88
1.53
1.23
1.42
2.50c
1.80
2.50c
1.94
0.66
1.00
8.50
8.78
8.02
8.69
8.25
8.50
8.86
9.02
8.40
8.64
9.03
8.14
8.94
15.42
16.08
17.27
16.83
16.68
16.31
17.32
19.83
15.28
18.65
14.82
16.48
17.92
21.54:
15.20
18.79
20.65
18.06
22.03
24.21
19.13
22.82
20.33
19.22
15.55
17.26
18.90
18.50
14.21
15.92
15.28
20.59:
23.36:
21.33
−1.00
0.90
−0.30
−1.00
1.2
6.8
42.6
0.0
−1.00
0.91
−1.00
0.93
−0.64
0.87
0.0
8.0
NGC6624
NGC6626
NGC6638
NGC6637
NGC6642
NGC6652
NGC6656
Pal 8
NGC6681
NGC6712
NGC6715
NGC6717
NGC6723
NGC6749
NGC6752
NGC6760
Terzan 7
NGC6779
Pal 10
Arp 2
NGC6809
Terzan 8
Pal 11
NGC6838
NGC6864
NGC6934
NGC6981
NGC7006
NGC7078
NGC7089
NGC7099
Pal 12
Pal 13
NGC7492
0.86
0.86
0.72
1.27
1.09
0.87
0.77
0.72
0.75
0.68
0.66
0.60
1.07
0.72
0.42
8.65
8.80
8.70
9.46
8.89
9.06
8.10
8.72
8.64
8.93
8.97
9.01
9.05
8.55
9.11
−0.08
3.1
13.8
8.0
6.4
24.7
1.00
−1.00
−1.00
0.98
0.0
0.0
0.0
2.5
0.86
0.87
0.0
10.5
−1.00
−0.42
0.28
0.17
−0.28
0.67
0.96
0.89
−1.00
−0.20
0.81
0.0
0.0
6.2
60.2
63.8
63.4
26.3
4.7
11.7
0.0
191.8
16.6
Note
a A colon after a number indicates that it is very uncertain.
Measurements of cluster radial velocities, spectroscopic abundance properties, and spatial distributions help to constrain the dynamical and chemical evolution of the early formation stages of large
galaxies [57].
Most of the more remote galaxies in this table have no other published information on their globular
clusters except for total numbers (S N values). However, many of the nearby ones have multicolor
photometry or even spectroscopic data available, and the sources cited should be consulted for these
data. The material in this table is based on the literature survey given in [57], updated to 1996 and
recalculated where necessary. The fiducial distance to the Virgo cluster, which provides a fundamental
basis of comparison for several other galaxies in the list, is adopted here to be (m − M)V = 31.0.
Changes to distances for some individual galaxies with more recent measurements have also been
incorporated.
Column (1) gives the NGC number or name of the galaxy. The first 11 galaxies listed are members
of the Local Group and are referred to by their most common names. The galaxies outside the Local
Group are listed in order of right ascension.
Sp.-V/AQuan/1999/10/11:11:34
Page 564
564 / 22
S TAR C LUSTERS
Column (2) gives the group or cluster (if any) of which the galaxy is a member.
Column (3) gives the Hubble type of the galaxy (elliptical E, spiral S, irregular I).
Column (4) shows the radial velocity of the cluster, or (if the galaxy is isolated or very nearby) the
individual radial velocity of the galaxy.
Column (5) shows the apparent visual distance modulus (H0 = 75 km s−1 Mpc−1 for galaxies
more distant than Virgo, or individual distance calibrations for nearby ones).
Column (6) shows the absolute visual integrated magnitude of the galaxy.
Column (7) gives the total number of globular clusters estimated to be in the given galaxy (see [57]
for method of calculation).
Column (8) gives the specific frequency (number of globular clusters per unit galaxy luminosity)
as defined above.
Column (9) gives the reference source for the globular-cluster data.
Table 22.5. Cluster populations in other galaxies.a
(1)
NGC
(2)
Cluster
(3)
Type
(4)
V0
(5)
(m − M)V
Galaxy
LMCb
SMCb
Fornax
Sgr
147
185
205
221
M31
M33
55
253
524
720
1052
1275
1374
1379
1387
1399
1404
1549
1553
2403
3031
2683
3109
3115
3115DW1
3226
3311
3377
3379
3384
3557
3607
3842
Local
Local
Local
Local
Local
Local
Local
Local
Local
Local
Local
Sculptor
Sculptor
CfA13
T52-9
Cetus
Perseus
Fornax
Fornax
Fornax
Fornax
Fornax
Doradus
Doradus
M81
M81
Sbc
Smc
Imc
dE0c
dEc
dE5c
dE3c
dE5c
E2
Sb
Scd
Smc
Sc
S0
E5
E4
Ep/cD
E0
E0
S0
E1/cD
E1
E0
S0
Scd
Sab
Sb
Im
S0
dE1, Nc
E2
E0/cD
E5
E1
S0
E3
S0
E3
12
−30
−51
140
89
39
−1
35
−59
3
106
260
2 600
1 660
1 400
5 450
1 390
1 390
1 390
1 390
1 390
1 010
1 010
260
260
370
130
460
460
1 210
3 420
630
630
630
2 560
1 090
6 500
18.64
18.92
20.70
17.44
24.45
24.40
24.49
24.54
24.54
24.64
25.75
26.8
32.7
31.4
31.3:
34.9
31.0
31.0
31.0
31.0
31.0
30.7:
30.7:
27.64
27.8
29.75
26.35
30.2
30.2
31.0:
33.4
30.00
30.00
30.00
33.0
31.0:
34.7
CfA58
A1060
Leo
Leo
Leo
T31-10
CfA77
A1367
(6)
MVT
−21.3
−18.6
−16.9
−13.7
−13:
−15.0
−15.2
−16.5
−16.3
−21.7
−19.1
−19.0
−20.4
−22.1
−21.2
−20.8
−23.3
−19.7
−19.9
−20.2
−21.1
−20.7
−20.8
−21.2
−19.5
−21.2
−20.8
−17.3
−21.1
−17.7
−19.6
−22.3
−19.8
−20.7
−20.0
−22.6
−21.0
−23.1
(7)
NGC
(8)
SN
160 ± 20
15:
2±1
5±1
3±1
4±1
8±2
9±1
<3
350 ± 100
30:
2
22:
4430 ± 950
660 ± 190
600 ± 70
7750 ± 2520
440 ± 200
380 ± 100
385 ± 80
5340 ± 1780
950 ± 140
165 ± 60
600 ± 134
8:
210 ± 30
310 ± 100
20:
630 ± 150
59 ± 23
480 ± 170
12 400 ± 5000
210 ± 50
260 ± 140
110 ± 60
400 ± 300
1000 ± 700
14 000 ± 2500
0.5 ± 0.1
0.5:
0.4 ± 0.2
17 ± 7
19:
4.0 ± 1.0
6.5 ± 1.6
2.3 ± 0.3
< 0.8
0.7 ± 0.2
0.6:
> 0.1:
0.2 ± 0.1
6.4 ± 1.4
2.2 ± 0.9
3.0 ± 0.4
4.3 ± 1.4
5.7 ± 2.6
4.1 ± 1.1
3.3 ± 0.7
19 ± 6
4.3 ± 0.7
0.8 ± 0.3
2.0 ± 0.5
> 0.1:
0.7 ± 0.1
1.7 ± 0.5
2.4:
2.3 ± 0.5
4.9 ± 1.9
7.0 ± 2.4
15 ± 6
2.6 ± 0.6
1.3 ± 0.7
1.1 ± 0.5
0.4 ± 0.3
4.0 ± 2.8
7.7 ± 1.4
(9)
Reference
[1]
[1]
[1]
[2]
[3]
[1]
[1]
[1]
[1]
[1]
[1]
[1]
[1]
[1]
[4]
[1]
[5]
[1]
[1]
[1]
[6]
[7]
[1]
[1]
[1]
[8]
[1]
[1]
[1]
[9]
[1]
[10]
[1]
[1]
[1]
[1]
[1]
[11]
Sp.-V/AQuan/1999/10/11:11:34
Page 565
22.3 G LOBULAR C LUSTERS IN OTHER G ALAXIES / 565
Table 22.5. (Continued.)
(1)
NGC
(2)
Cluster
(3)
Type
(4)
V0
3923
4073
4278
4565
4216
4340
4365
4374
4406
4472
4486
4494
4526
4552
4564
4569
4621
4636
4649
4697
4594
5018
5170
4874
4881
4889
5128
5629
5813
5846
UGC9799b
UGC9958b
6166
7768
7814
T22-4
MKW4
Coma I
Coma I
Virgo
Virgo
Virgo W
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo
Virgo SE
T11-0
T11-18
A1656
A1656
A1656
Centaurus
AWM3
CfA150
CfA150
A2052
A2107
A2199
A2666
E3
E1/cD
E1
Sb
Sb
SB0
E2
E1
E3
E2
E0/cD
E0
S0
E0
E6
Sab
E5
E0
E2
E6
Sa
E4p
Sb
E0
E0
E4
E0p
E/cD
E1
E0
E/cD
E/cD
E2/cD
E2/cD
Sab
1 590
6 090
910
1 210
1 080
1 080
1 080
1 080
1 080
1 080
1 080
1 290
1 080
1 080
1 080
1 080
1 080
1 080
1 080
1 080
840
2 800
1 350
6 950
6 950
6 950
320
4 600
1 810
1 810
10 440
12 630
9 080
7 950
1 110
(5)
(m − M)V
31.9
34.6
30.0
30.0
31.0
31.0
31.4
31.0
31.0
31.0
31.0
30.8
31.0
31.0
31.0
31.0
31.0
31.0
31.0
31.0
29.9
33.2:
31.7:
34.9
34.9
34.9
28.25
34.0
32.3
32.3
35.9
36.3
35.6
35.3
31.0
(6)
MVT
−22.1
−23.1
−19.8
−21.6
−21.7
−20.0
−21.8
−21.7
−21.8
−22.6
−22.4
−21.0
−21.4
−21.2
−20.1
−21.8
−21.2
−21.4
−22.2
−21.7
−22.3
−22.4
−21.2
−23.0
−21.6
−23.5
−22.0
−21.7
−21.6
−22.1
−23.4
−23.4
−23.6
−22.9
−21.0
(7)
NGC
(8)
SN
4300 ± 1000
8290 ± 460
1050 ± 120
180 ± 45
620 ± 310
775 ± 310
2500 ± 200
3040 ± 400
3350 ± 400
6300 ± 1900
13 000 ± 500
1400 ± 350
2700 ± 400
2400:
1000 ± 300
930 ± 300
1900 ± 400
3060 ± 270
5100 ± 160
2500 ± 600
1900 ± 620
800 ± 300
390 ± 140
22 600 ± 2700
390 ± 40
17 300 ± 3000
1700 ± 400
< 2000
3000 ± 750
3120 ± 1850
48 000 ± 16 000
27 000 ± 13 000
10 000 ± 5000
4050 ± 2600
500 ± 160
6.4 ± 1.5
4.8 ± 0.3
12.3 ± 1.4
0.4 ± 0.1
1.3 ± 0.7
8.0 ± 3.2
5.0 ± 0.4
6.6 ± 0.9
6.3 ± 0.8
5.6 ± 1.7
13.9 ± 0.5
5.4 ± 1.3
7.7 ± 1.2
8:
10.0 ± 3.0
1.8 ± 0.6
6.3 ± 1.2
8.4 ± 0.8
6.9 ± 0.2
5.0 ± 1.3
2.3 ± 0.7
0.9 ± 0.3
1.2 ± 0.4
14.3 ± 1.7
1.0 ± 0.1
6.9 ± 1.2
2.6 ± 0.6
<5
6.9 ± 1.7
4.5 ± 2.7
21 ± 7
12 ± 5.6
4±2
2.8 ± 1.8
2.6 ± 0.8
(9)
Reference
[12]
[13]
[1]
[14]
[1]
[1]
[15]
[1]
[1]
[1]
[16]
[14]
[1]
[17]
[1]
[1]
[1]
[18]
[1]
[1]
[19]
[20]
[1]
[21]
[22]
[21]
[1]
[13]
[23]
[1]
[24]
[24]
[1]
[24]
[25]
Notes
a A colon after a number indicates that it is very uncertain.
b LMC: Large Magellanic Clound. SMC: Small Magellanic Cloud. UGC: Uppsala Galaxy Catalog.
c Sm, Im: Magellanic-type spiral or irregular. dE: dwarf elliptical.
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