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Globular clusters are some of the oldest stellar systems in the Universe. They are believed to be formed in the earliest stages of galaxy formation and/or in extreme merger-driven star formation episodes. For individual galaxies, the number of GCs is so strongly correlated with halo mass that GC counts can be used as a proxy halo mass measurement, making them some of the best dynamical tracers of galaxies.
Globular clusters are some of the oldest stellar systems in the Universe. They are believed to be formed in the earliest stages of galaxy formation and/or in extreme merger-driven star formation episodes. For individual galaxies, the number of GCs is so strongly correlated with halo mass that GC counts can be used as a proxy halo mass measurement, making them some of the best dynamical tracers of galaxies.
The large-scale structure of GCs in the NGC 1052 group
The large-scale structure of GCs in the NGC 1052 group
Prompted by the many controversial claims involving the NGC 1052 group, including that it hosts two dark matter-free galaxies with overluminous and monochromatic globular cluster (GC) systems, we mapped out the large-scale structure (LSS) of GCs over the entire group. We found that the GC distribution in the group does not strongly support any formation scenario in particular. It favours, none the less, scenarios relying on galaxy-galaxy interactions and on the coeval formation of GCs around the DM-free dwarf galaxies. These may include the recently proposed bullet-dwarf formation, as well as high-redshift tidal dwarf galaxy models. More details in Buzzo et al. 2023.
A new method to find and characterise GCs
A new method to find and characterise GCs
We have recently developed and demonstrated a reliable and efficient means for GC pre-selection (Buzzo et al. 2022a), using a combination of resolution, proper motion, and SED shape.
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