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

We use N-body simulations to study the tidal evolution of globular clusters(GCs) in dwarf spheroidal (dSph) galaxies. Our models adopt a cosmologicallymotivated scenario in which the dSph is approximated by a static NFW halo witha triaxial shape. For a large set of orbits and projection angles we examinethe spatial and velocity distribution of stellar debris deposited during thecomplete disruption of stellar clusters. Our simulations show that such debrisappears as shells, isolated clumps and elongated over-densities at low surfacebrightness (>26 mag/arcsec^2), reminiscent of substructure observed in severalMW dSphs. Such features arise from the triaxiality of the galaxy potential anddo not dissolve in time. Stellar over-densities reported in several MW dSphsmay thus be the telltale evidence of dark matter haloes being triaxial inshape.  We explore a number of kinematic signatures that would help to validate (orfalsify) this scenario. The mean angular momentum of the cluster debrisassociated with box and resonant orbits, which are absent in sphericalpotentials, is null. As a result, we show that the line-of-sight velocitydistribution may exhibit a characteristic "double-peak" depending on theoriention of the viewing angle with respect to the progenitor's orbital plane.Kinematic surveys of dSphs may help to detect and identify substructuresassociated with the disruption of stellar clusters, as well as to address theshape of the dark matter haloes in which dSphs are embedded.

Are stellar over-densities in dwarf galaxies the "smoking gun" of triaxial dark matter haloes?