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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Dwarf spheroidal (dSph) galaxies are considered the basic building blocks ofthe galaxy formation process in the LCDM (Lambda Cold Dark Matter) hierarchicalcosmological model. These galaxies are believed to be the most dark matter (DM)dominated systems known, have the lowest stellar content, and are poor in gas.Many theories attempt to explain the formation of dSph galaxies resorting tothe fact that these galaxies are mainly found orbiting large galaxies orinvoking other mechanisms of interactions. Here we show the full set ofsimulation as an extension of our fiducial model, where we study the formationof classical dSph galaxies in isolation by dissolving star clusters within theDM halo of the dwarf galaxy. In our parameter survey we adopt cored and cuspedDM halo profiles and consider different numbers of dissolving star clusters. Weinvestigate the dependency of observable quantities with different masses andscale-lengths of the DM halo and different star formation efficiencies (SFE).We find that our proposed scenario explains many features of the classical dSphgalaxies of the Milky Way, like their morphology and their dynamics. We seetrends how the surface brightness and the scale-length of the luminouscomponent vary with the parameters of our simulations. We also identify howirregularities in their shape, i.e. clumpiness and ellipticity vary in oursimulations. In velocity space, we identify the parameters leading to flatvelocity dispersions curves. We recognize kinematically cold substructures invelocity space, named fossil remnants and stemming from our unique initialconditions, which alter the expected results. These streaming motions areconsidered as a key feature for future observation with high resolution tovalidate our scenario.

A Possible Formation Scenario for Dwarf Spheroidal Galaxies - II: A Parameter Study