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 derive the stellar-to-halo mass relation (SHMR), namely $f_\star\proptoM_\star/M_{\rm h}$ versus $M_\star$ and $M_{\rm h}$, for early-type galaxiesfrom their near-IR luminosities (for $M_\star$) and the position-velocitydistributions of their globular cluster systems (for $M_{\rm h}$). Ourindividual estimates of $M_{\rm h}$ are based on fitting a dynamical model witha distribution function expressed in terms of action-angle variables andimposing a prior on $M_{\rm h}$ from the concentration-mass relation in thestandard $\Lambda$CDM cosmology. We find that the SHMR for early-type galaxiesdeclines with mass beyond a peak at $M_\star\sim 5\times 10^{10}M_\odot$ and$M_{\rm h}\sim 10^{12}M_\odot$ (near the mass of the Milky Way). This result isconsistent with the standard SHMR derived by abundance matching for the generalpopulation of galaxies, and with previous, less robust derivations of the SHMRfor early types. However, it contrasts sharply with the monotonically risingSHMR for late types derived from extended HI rotation curves and the same$\Lambda$CDM prior on $M_{\rm h}$ as we adopt for early types. The SHMR formassive galaxies varies more or less continuously, from rising to falling, withdecreasing disc fraction and decreasing Hubble type. We also show that thedifferent SHMRs for late and early types are consistent with the similarscaling relations between their stellar velocities and masses (Tully-Fisher andFaber-Jackson relations). Differences in the relations between the stellar andhalo virial velocities account for the similarity of the scaling relations. Weargue that all these empirical findings are natural consequences of a picturein which galactic discs are built mainly by smooth and gradual inflow,regulated by feedback from young stars, while galactic spheroids are built by acooperation between merging, black-hole fuelling, and feedback from AGNs.

Dynamical evidence for a morphology-dependent relation between the stellar and halo masses of galaxies