Deep Chandra Monitoring Observations of NGC 4649: II. Wide-Field Hubble Space Telescope Imaging of the Globular Clusters

TL;DR

This study uses Hubble Space Telescope imaging to analyze globular clusters in NGC 4649, revealing metallicity gradients, size differences, and candidate ultra-compact dwarfs, providing insights into their properties and origins.

Contribution

It provides detailed photometry, size estimates, and identification of ultra-compact dwarf candidates in NGC 4649, expanding understanding of globular cluster systems in elliptical galaxies.

Findings

Metal-poor GCs show a negative metallicity gradient with radius.

Metal-poor GCs are larger than metal-rich GCs at large distances.

Approximately 20 ultra-compact dwarf candidates identified.

Abstract

We present g and z photometry and size estimates for globular clusters (GCs) in the massive Virgo elliptical NGC 4649 (M60) using a five-pointing Hubble Space Telescope/Advanced Camera for Surveys mosaic. The metal-poor GCs show a monotonic negative metallicity gradient of (-0.43 +/- 0.10) dex per dex in radius over the full radial range of the data, out to ~ 24 kpc. There is evidence for substantial color substructure among the metal-rich GCs. The metal-poor GCs have typical sizes ~ 0.4 pc larger than the metal-rich GCs out to large galactocentric distances (~> 20 kpc), favoring an intrinsic explanation for the size difference rather than projection effects. There is no clear relation between half-light radius and galactocentric distance beyond ~ 15 kpc, suggesting that the sizes of GCs are not generically set by tidal limitation. Finally, we identify ~ 20 candidate ultra-compact dwarfs that extend down to surprisingly faint absolute magnitudes (M_z ~ -8.5), and may bridge the gap between this class and "extended clusters" in the Local Group. Three of the brighter candidates have published radial velocities and can be confirmed as bona fide ultra-compact dwarfs; follow-up spectroscopy will determine the nature of the remainder of the candidates.