Document Type

Article

Publication Date

January 2016

Publication Title

The Astrophysical Journal

Volume

824

Issue Number

1

DOI

10.3847/0004-637X/824/1/42

Keywords

galaxies: individual (M31), galaxies: star clusters: general, Local Group

Disciplines

Astrophysics and Astronomy | External Galaxies

Abstract

We carry out a joint spatial–kinematical–metallicity analysis of globular clusters (GCs) around the Andromeda Galaxy (M31), using a homogeneous, high-quality spectroscopic data set. In particular, we remove the contaminating young clusters that have plagued many previous analyses. We find that the clusters can be divided into three major metallicity groups based on their radial distributions: (1) an inner metal-rich group ([Fe/H] > -0.4); (2) a group with intermediate metallicity (with median [Fe/H] = −1); and (3) a metal-poor group, with [Fe/H] < -1.5. The metal-rich group has kinematics and spatial properties like those of the disk of M31, while the two more metal-poor groups show mild prograde rotation overall, with larger dispersions—in contrast to previous claims of stronger rotation. The metal-poor GCs are the least concentrated group; such clusters occur five times less frequently in the central bulge than do clusters of higher metallicity. Despite some well-known differences between the M31 and Milky Way GC systems, our revised analysis points to remarkable similarities in their chemodynamical properties, which could help elucidate the different formation stages of galaxies and their GCs. In particular, the M31 results motivate further exploration of a metal-rich GC formation mode in situ, within high-redshift, clumpy galactic disks.

Comments

This article was originally published in The Astrophysical Journal, volume 824, issue 1. © 2016. The American Astronomical Society. All rights reserved.
This article is also available online at the following link: https://doi.org/10.3847/0004-637X/824/1/42

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