Abstrakt
Due to their low surface brightness, dwarf galaxies are particularly susceptible to tidal forces. The expected degree of disturbance depends on the assumed gravity law and whether they have a dominant dark halo.
This makes dwarf galaxies useful for testing different gravity models. In this project, we use the Fornax Deep Survey (FDS) dwarf galaxy catalogue to compare the properties of dwarf galaxies in the Fornax Cluster with those predicted by the Lambda cold dark matter (Lambda CDM) standard model of cosmology and Milgromian dynamics (MOND).
We construct a test particle simulation of the Fornax system. We then use the Markov Chain Monte Carlo (MCMC) method to fit this to the FDS distribution of tidal susceptibility eta (half-mass radius divided by theoretical tidal radius), the fraction of dwarfs that visually appear disturbed as a function of eta, and the distribution of projected separation from the cluster centre.
This allows us to constrain the eta value at which dwarfs should get destroyed by tides. Accounting for an r'-band surface brightness limit of 27.8 magnitudes per square arcsec, the required stability threshold is eta(dest) = 0.25(-0.03)(+0.07) in Lambda CDM and 1.88(-0.53)(+0.85) in MOND.
The Lambda CDM value is in tension with previous N-body dwarf galaxy simulations, which indicate that eta(destr) approximate to 1. Our MOND N-body simulations indicate that eta(destr) = 1.70 +/- 0.30, which agrees well with our MCMC analysis of the FDS.
We therefore conclude that the observed deformations of dwarf galaxies in the Fornax Cluster and the lack of low surface brightness dwarfs towards its centre are incompatible with Lambda CDM expectations but well consistent with MOND.