English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

A recent surge in the discovery of new ultrafaint dwarf satellites of theMilky Way has inspired the idea of searching for faint satellites, $10^3\,\mathrm{M_{\odot}} < M_* < 10^6\, \mathrm{M_{\odot}}$, around less massivefield galaxies in the Local Group. Such satellites would be subject to weakerenvironmental influences than Milky Way satellites, and could lead to newinsights on low mass galaxy formation. In this paper, we predict the number ofluminous satellites expected around field dwarf galaxies by applying severalabundance matching models and a reionization model to the dark-matter only\textit{Caterpillar} simulation suite. For three of the four abundance matchingmodels used, we find a $>99\%$ chance that at least one satellite with stellarmass $M_*> 10^5\, \mathrm{M_{\odot}}$ exists around the combined five LocalGroup field dwarf galaxies with the largest stellar mass. When consideringsatellites with $M_*> 10^4\, \mathrm{M_{\odot}}$, we predict a combined $5-25$satellites for the five largest field dwarfs, and $10-50$ for the whole LocalGroup field dwarf population. Because of the relatively small number ofpredicted dwarfs, and their extended spatial distribution, a large fractioneach Local Group dwarf's virial volume will need to be surveyed to guaranteediscoveries. We compute the predicted number of satellites in a given field ofview of specific Local Group galaxies, as a function of minimum satelliteluminosity, and explicitly obtain such values for the Solitary Local dwarfssurvey. Uncertainties in abundance matching and reionization models are large,implying that comprehensive searches could lead to refinements of both models.

An observer's guide to the (Local Group) dwarf galaxies: predictions for their own dwarf satellite populations