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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

Stellar streams originating in disrupted dwarf galaxies and star clusters areobserved around the Milky Way and nearby galaxies. Such substructures are theimportant tracers that record how the host haloes have accreted progenitorgalaxies. Based on the cosmological context, we investigate the relationshipbetween structural properties of substructures such as length and thinness at$z=0$, and orbits of their progenitors. We model stellar components of a largesample of substructures around Milky Way-sized haloes by combiningsemi-analytic models with a high-resolution cosmological $N$-body simulation.Using the Particle Tagging method, we embed stellar components in progenitorhaloes and trace phase-space distributions of the substructures down to $z=0$.We find that the length and thinness of substructures vary smoothly as theredshift when the host haloes accrete their progenitors. For substructuresobserved like streams at $z=0$, a large part of the progenitors is accreted bytheir host haloes at redshift $0.5\lesssim z\lesssim 2.5$. Substructures withprogenitors out of this accretion redshift range are entirely or less disruptedby $z=0$ and cannot be observed as streams. We also find that the distributionsof length and thinness of substructures vary smoothly as pericenter andapocenter of the progenitors. Substructures observed like streams tend to havethe specific range of $10\ {\rm kpc} \lesssim r_{\rm peri}\lesssim100\ {\rmkpc}$ and $50\ {\rm kpc} \lesssim r_{\rm apo}\lesssim300\ {\rm kpc}$.

Statistical properties of substructures around Milky Way-sized haloes and their implications for the formation of stellar streams