Veronika Dornan
@dornanv.bsky.social
🔭 Post-doctoral research associate at The University of Edinburgh studying extragalactic globular star clusters (she/her)
dornanv.github.io/
dornanv.github.io/
In addition, that correlation was driven by the *red* GCs specifically, the blue GCs didn't have the same correlation. Since red GCs tend to be formed in massive galaxies and blue GCs in smaller satellites, this result is likely driven by a few major galaxy mergers rather than many minor mergers.
June 2, 2025 at 2:27 PM
In addition, that correlation was driven by the *red* GCs specifically, the blue GCs didn't have the same correlation. Since red GCs tend to be formed in massive galaxies and blue GCs in smaller satellites, this result is likely driven by a few major galaxy mergers rather than many minor mergers.
When comparing the steepness of those GC system profiles to where the galaxies sit on the GC system mass - total galaxy mass relation we found that the steepness of those GC system profiles correlated to how offset their host galaxies were on that relation.
June 2, 2025 at 2:27 PM
When comparing the steepness of those GC system profiles to where the galaxies sit on the GC system mass - total galaxy mass relation we found that the steepness of those GC system profiles correlated to how offset their host galaxies were on that relation.
For 16 of these galaxies we had colour information and could determine the profiles for the red and blue GCs separately. As expected, the red GCs tend to have steeper profiles and the blue GCs tend to have shallower profiles.
June 2, 2025 at 2:27 PM
For 16 of these galaxies we had colour information and could determine the profiles for the red and blue GCs separately. As expected, the red GCs tend to have steeper profiles and the blue GCs tend to have shallower profiles.
We determined the globular cluster (GC) radial density profiles for 27 brightest cluster galaxies (BCGs) from Hubble photometry. These are massive systems, hosting 1,000s to 10,000s of GCs!
June 2, 2025 at 2:27 PM
We determined the globular cluster (GC) radial density profiles for 27 brightest cluster galaxies (BCGs) from Hubble photometry. These are massive systems, hosting 1,000s to 10,000s of GCs!