Globular Cluster and Galaxy formation: M31, The Milky Way, and Implications for Globular Cluster Systems of Spiral Galaxies

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 10 2 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.

[1]  Peter Nilson,et al.  Uppsala general catalogue of galaxies , 1973 .

[2]  W. Sargent,et al.  Search for globular clusters in M31. I - The disk and the minor axis , 1977 .

[3]  David Burstein,et al.  Old stellar populations. I. A spectroscopic comparison of galactic globular clusters, M 31 globular clusters, and elliptical galaxies. , 1984 .

[4]  J. Tomkin,et al.  Nitrogen abundances in disk and halo Dwarfs , 1984 .

[5]  W. Harris,et al.  Supergiant Molecular Clouds and the Formation of Globular Cluster Systems , 1994 .

[6]  M. Irwin,et al.  A dwarf satellite galaxy in Sagittarius , 1994, Nature.

[7]  T. Davidge,et al.  Absorption Line Gradients in the Blue and Near-Ultraviolet Spectra of Bright Elliptical Galaxies, and Implications for Studies of Intermediate Redshift Objects , 1994 .

[8]  B. Whitmore,et al.  Hubble space telescope observations of young star clusters in NGC-4038/4039, 'the antennae' galaxies , 1995 .

[9]  William E. Harris,et al.  A Catalog of Parameters for Globular Clusters in the Milky Way , 1996 .

[10]  G. Kauffmann,et al.  Galaxy formation and large scale bias , 1995, astro-ph/9512009.

[11]  Global Relationships Among the Physical Properties of Stellar Systems. , 1997, astro-ph/9707037.

[12]  David Burstein,et al.  Old Stellar Populations. VI. Absorption-Line Spectra of Galaxy Nuclei and Globular Clusters , 1997, astro-ph/9712258.

[13]  M. Rieke,et al.  Integrated Ultraviolet Spectra and Line Indices of M31 Globular Clusters and the Cores of Elliptical Galaxies , 1998 .

[14]  J. P. Huchra,et al.  Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant , 1998, astro-ph/9801080.

[15]  J. P. Huchra,et al.  M31 Globular Clusters: Colors and Metallicities* ** *** , 2000 .

[16]  Models for Old, Metal-poor Stars with Enhanced α-Element Abundances. III. Isochrones and Isochrone Population Functions , 2001, astro-ph/0102480.

[17]  Xu Zhou,et al.  Spectral Energy Distributions, Ages, and Metallicities of Star Clusters in M33 , 2001 .

[18]  TO APPEAR IN THE ASTROPHYSICAL JOURNAL LETTERS Preprint typeset using L ATEX style emulateapj v. 04/03/99 EVIDENCE FOR A SIGNIFICANT INTERMEDIATE-AGE POPULATION IN THE M31 HALO FROM , 2003 .

[19]  B. Behr.  Chemical Abundances and Rotation Velocities of Blue Horizontal-Branch Stars in Six Globular Clusters , 2003, astro-ph/0307178.

[20]  J. Rose,et al.  Analyzing Starbursts Using Magellanic Cloud Star Clusters as Simple Stellar Populations , 2003, astro-ph/0306358.

[21]  I. Ivans,et al.  A Globular Cluster Metallicity Scale Based on the Abundance of Feii , 2002, astro-ph/0305380.

[22]  D. Burstein,et al.  Nitrogen Overabundance: Globular Cluster and Halo Formation , 2003, astro-ph/0310441.

[23]  M31's Undisturbed Thin Disk of Globular Clusters , 2003, astro-ph/0307302.

[24]  E. Observatory,et al.  Abundance analysis of turn-off and early subgiant stars in the globular cluster 47 Tuc (NGC 104) , 2003, astro-ph/0311347.

[25]  THE GLOBULAR CLUSTER SYSTEM OF THE CANIS MAJOR DWARF GALAXY , 2004, astro-ph/0403136.

[26]  Judith G. Cohen,et al.  The Chemical Inhomogeneity of Faint M13 Stars: Carbon and Nitrogen Abundances , 2003, astro-ph/0312315.

[27]  Duncan A. Forbes,et al.  THE CHEMICAL PROPERTIES OF MILKY WAY AND M31 GLOBULAR CLUSTERS. I. A COMPARATIVE STUDY , 2004 .