2004ApJ...614..158B


Query : 2004ApJ...614..158B

2004ApJ...614..158B - Astrophys. J., 614, 158-166 (2004/October-2)

Globular cluster and galaxy formation: M 31, the Milky Way, and implications for globular cluster systems of spiral galaxies.

BURSTEIN D., LI Y., FREEMAN K.C., NORRIS J.E., BESSELL M.S., BLAND-HAWTHORN J., GIBSON B.K., BEASLEY M.A., LEE H.-C., BARBUY B., HUCHRA J.P., BRODIE J.P. and FORBES D.A.

Abstract (from CDS):

We find that the globular cluster (GC) systems of the Milky Way and of our neighboring spiral galaxy, M31, comprise two distinct entities, differing in three respects. First, M31 has a set of young GCs, ranging in age from a few times 102 Myr to 5 Gyr old, as well as old GCs. No such very young GCs are known in the Milky Way. Second, we confirm that the oldest M31 GCs have much higher nitrogen abundances than do Galactic GCs at equivalent metallicities, while carbon abundances appear normal for the GCs in both galaxies. Third, Morrison and coworkers have shown that M31 has a subcomponent of GCs that follow closely the disk rotation curve of that galaxy. Such a GC system in our own Galaxy has yet to be found. The only plausible scenario for the existence of the young M31 GC comes from the hierarchical-clustering-merging (HCM) paradigm for galaxy formation. We infer that M31 has absorbed more of its contingent of dwarf systems in the recent past than has the Milky Way. This inference has three implications: First, all spiral galaxies could differ in their GC properties, depending on how many companions each galaxy has and when the parent galaxy absorbs them. In this spectrum of possibilities, apparently the Milky Way ties down one end, in which almost all of its GCs were absorbed 10-12 Gyr ago. Second, it suggests that young GCs are preferentially formed in the dwarf companions of parent galaxies and then absorbed by the parent galaxy during mergers. Third, the young GCs seen in tidally interacting galaxies might come from the dwarf companions of these galaxies, rather than be made anew in the tidal interaction. However, there is no ready explanation for the marked difference in nitrogen abundance for the stars in the old M31 GCs relative to those in the oldest Galactic GCs, especially the most metal-poor GCs in both galaxies. The predictions made by Li & Burstein regarding the origin of nitrogen abundance in GCs are consistent with what is found for the old M31 GCs compared to that for the two 5 Gyr old M31 GCs.

Abstract Copyright: ∼

Journal keyword(s): Galaxies: Evolution - Galaxies: Formation - Galaxies: Individual: Messier Number: M31 - Galaxies: Star Clusters - Galaxy: Globular Clusters: General

Simbad objects: 43

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Number of rows : 43
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 NAME Mayall II GlC 00 32 46.5323801712 +39 34 40.504803060   14.564 13.807 13.208 12.684 ~ 400 1
2 Bol 311 GlC 00 39 33.7263390600 +40 31 14.621665512 16.338 16.209 15.362 14.803 14.39 ~ 82 0
3 Bol 315 GlC 00 39 48.570 +40 31 30.45 16.304 16.581 16.090 15.755 15.298 ~ 54 1
4 Bol 1 GlC 00 39 51.0040400976 +40 58 10.711050528 18.783 18.261 17.156 16.455 15.712 ~ 41 0
5 Bol 321 GlC 00 40 15.38 +40 27 45.9 17.913 18.068 17.615 17.316 16.834 ~ 29 1
6 Bol 19 GlC 00 40 52.5299628912 +41 18 53.489147724 16.360 15.940 14.98 14.310 13.740 ~ 55 0
7 Bol 338 GlC 00 40 58.871 +40 35 47.41 15.123 15.034 14.168 13.621 13.27 ~ 76 0
8 M31GC J004112+410532 GlC 00 41 12.24 +41 05 28.8 19.022 18.776 18.149 17.692 16.947 ~ 28 1
9 Bol 29 GlC 00 41 17.8243331280 +41 00 22.868949204 18.297 17.725 16.713 16.069 15.380 ~ 54 0
10 Bol 347 GlC 00 42 22.8912032352 +41 54 27.462341268 17.380 17.230 16.500 15.970 15.490 ~ 37 0
11 M 31 AGN 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 13622 1
12 Bol 158 GlC 00 43 14.3953843272 +41 07 21.141017796 15.900 15.560 14.65 14.150 13.550 ~ 119 1
13 Bol 171 GlC 00 43 25.6003962624 +41 15 37.095704604 16.795 16.192 15.217 14.635 14.07 ~ 75 0
14 Bol 179 GlC 00 43 31.1069226792 +41 18 14.612214636 16.449 16.162 15.316 14.800 14.43 ~ 55 0
15 Bol 193 GlC 00 43 45.4998657576 +41 36 57.605146668 16.746 16.097 15.193 14.565 14.18 ~ 89 0
16 Bol 210 GlC 00 44 02.78 +41 14 24.5 18.14 18.09 17.57 17.21 16.20 ~ 34 1
17 Bol 216 GlC 00 44 08.78 +41 37 55.8 17.543 17.556 17.168 16.899 16.548 ~ 41 1
18 Bol 218 GlC 00 44 14.3248282920 +41 19 19.371822456 15.875 15.559 14.682 14.230 13.74 ~ 74 0
19 Bol 223 GlC 00 44 27.0341393160 +41 34 37.019012916 17.919 17.958 17.680 17.467 17.164 ~ 36 1
20 Bol 225 GlC 00 44 29.5618369896 +41 21 35.714596284 15.50 15.000 14.220 13.679 13.02 ~ 136 0
21 Bol 232 GlC 00 44 40.2313035720 +41 15 00.510653016 16.463 16.357 15.586 15.096 14.67 ~ 66 0
22 Bol 238 GlC 00 45 14.69 +41 19 37.0 17.552 17.164 16.329 15.732 15.156 ~ 42 0
23 Bol 484 GlC 00 45 53.8935132696 +41 47 36.718439172 18.822 18.690 18.10 17.893 17.483 ~ 28 1
24 Bol 380 GlC 00 46 06.2106491840 +42 00 53.127933100 17.461 17.282 16.829 16.573 16.114 ~ 34 1
25 Bol 386 GlC 00 46 27.0143614272 +42 01 52.743069552 16.554 16.355 15.541 14.997 14.435 ~ 93 0
26 Bol 400 GlC 00 48 01.4397192000 +42 25 32.946728520 17.337 17.096 16.377 15.873 15.300 ~ 36 0
27 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 12317 1
28 NGC 1754 Cl* 04 54 18.080 -70 26 32.58   12.32 11.57     ~ 96 0
29 NGC 1795 Cl* 04 59 46.940 -69 48 08.06   13.15 12.42     ~ 49 0
30 BD+52 913 WD* 05 05 30.6180977592 +52 49 51.919301604 10.25 11.44 11.69 11.93 12.108 DA.8 1153 0
31 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 19090 0
32 M 53 GlC 13 12 55.25 +18 10 05.4     7.79     ~ 907 0
33 M 3 GlC 13 42 11.62 +28 22 38.2     6.39     ~ 2593 0
34 M 5 GlC 15 18 33.22 +02 04 51.7     5.95     ~ 2095 0
35 BD+33 2642 pA* 15 51 59.8854348048 +32 56 54.329485272 9.806 10.61 10.73 10.884 10.961 O7p 456 0
36 EGGR 327 WD* 16 27 53.4891141091 +09 12 16.023524499 16.008 16.475 16.117 15.899 15.683 DA6.9 105 0
37 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2291 0
38 M 92 GlC 17 17 07.39 +43 08 09.4     6.52     ~ 2240 0
39 M 71 GlC 19 53 46.49 +18 46 45.1           ~ 1190 0
40 M 15 GlC 21 29 58.33 +12 10 01.2           ~ 3274 0
41 M 2 GlC 21 33 27.02 -00 49 23.7     6.25     ~ 1114 1
42 BD+28 4211 HS* 21 51 11.0221915656 +28 51 50.367627468 8.922 10.25 10.58 10.656 10.831 sdO2VIIIHe5 837 0
43 Feige 110 HS* 23 19 58.3996844256 -05 09 56.171142864 10.360 11.45 11.50 11.970 12.145 sdO8VIIIHe5 673 1

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