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16 papers · 2 filters
Finding the dispersing siblings of young open clusters. Dynamical traceback simulations using Gaia DR3
Eero Vaher, David Hobbs, Paul McMillan +1
Context. Stars tend to form in clusters, but many escape their birth clusters very early. Identifying the escaped members of clusters can inform us about the dissolution of star cl…
From particles to orbits: precise dark matter density profiles using dynamical information
Claudia Muni, Andrew Pontzen, Jason L. Sanders +3
We introduce a new method to calculate dark matter halo density profiles from simulations. Each particle is 'smeared' over its orbit to obtain a dynamical profile that is averaged…
Multiple stellar population mass loss in massive Galactic globular clusters
Elena Lacchin, Alessandra Mastrobuono-Battisti, Francesco Calura +4
The degree of mass loss, i.e. the fraction of stars lost by globular clusters, and specifically by their different populations, is still poorly understood. Many scenarios of the fo…
The galactic acceleration scale is imprinted on globular cluster systems of early-type galaxies of most masses and on red and blue globular cluster subpopulations
Michal Bílek, Michael Hilker, Florent Renaud +3
Context. Globular clusters (GCs) carry information about the formation histories and gravitational fields of their host galaxies. Bílek et al. (2019, BSR19 hereafter) reported that…
Measuring the physical imprints of gas flows in galaxies I: Accretion rate histories
A. Camps-Fariña, P. Sánchez-Blázquez, S. Roca-Fàbrega +1
Galaxies are expected to accrete pristine gas from their surroundings to sustain their star formation over cosmic timescales. Its lower abundance affects the metallicity of the ISM…
Pre-supernova feedback sets the star cluster mass function to a power law and reduces the cluster formation efficiency
Eric P. Andersson, Mordecai-Mark Mac Low, Oscar Agertz +2
The star cluster initial mass function is observed to have an inverse power law exponent around 2, yet there is no consensus on what determines this distribution, and why some vari…