Fahrion, K.; Lyubenova, M.; Hilker, M.; van de Ven, G.; Falcón-Barroso, J.; Leaman, R.; Martín-Navarro, I.; Bittner, A.; Coccato, L.; Corsini, E. M.; Gadotti, D. A.; Iodice, E.; McDermid, R. M.; Pinna, F.; Sarzi, M.; Viaene, S.; de Zeeuw, P. T.; Zhu, L.
Astronomy and Astrophysics
Globular clusters (GCs) are found ubiquitously in massive galaxies and due to their old ages, they are regarded as fossil records of galaxy evolution. Spectroscopic studies of GC systems are often limited to the outskirts of galaxies, where GCs stand out against the galaxy background and serve as bright tracers of galaxy assembly. In this work, we use the capabilities of the Multi Unit Explorer Spectrograph (MUSE) to extract a spectroscopic sample of 722 GCs in the inner regions (≲3 Reff) of 32 galaxies in the Fornax cluster. These galaxies were observed as part of the Fornax 3D project, a MUSE survey that targets early and late-type galaxies within the virial radius of Fornax. After accounting for the galaxy background in the GC spectra, we extracted line-of-sight velocities and determined metallicities of a sub-sample of 238 GCs. We found signatures of rotation within GC systems, and comparing the GC kinematics and that of the stellar body shows that the GCs trace the spheroid of the galaxies. While the red GCs prove to closely follow the metallicity profile of the host galaxy, the blue GCs show a large spread of metallicities but they are generally more metal-poor than the host.
The globular cluster catalogue (full Table A.1) is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/637/A26
Based on observations collected at the ESO Paranal La Silla Observatory, Chile, Prog. 296.B-5054(A).
Traces of Galaxy Formation: Stellar populations, Dynamics and Morphology
We are a large, diverse, and very active research group aiming to provide a comprehensive picture for the formation of galaxies in the Universe. Rooted in detailed stellar population analysis, we are constantly exploring and developing new tools and ideas to understand how galaxies came to be what we now observe.