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 investigate the stellar and dynamical mass profiles in the centres of 25brightest cluster galaxies (BCGs) at redshifts of 0.05 $\leq z \leq$ 0.30. Ourspectroscopy enables us to robustly measure the Gauss-Hermite higher ordervelocity moments $h_{3}$ and $h_{4}$, which we compare to measurements formassive early-type galaxies, and central group galaxies. We measure positivecentral values for $h_{4}$ for all the BCGs. We derive the stellarmass-to-light ratio ($\Upsilon_{\star \rm DYN}$), and velocity anisotropy($\beta$) based on a Multi-Gaussian Expansion (MGE) and axisymmetric JeansAnisotropic Methods (JAM, cylindrically- and spherically-aligned). Weexplicitly include a dark matter halo mass component, which is constrained byweak gravitational lensing measurements for these clusters. We find a strongcorrelation between anisotropy and velocity dispersion profile slope, withrising velocity dispersion profiles corresponding to tangential anisotropy anddecreasing velocity dispersion profiles corresponding to radial anisotropy. Therising velocity dispersion profiles can also indicate a significantcontribution from the intracluster light (ICL) to the total light (inprojection) in the centre of the galaxy. For a small number of BCGs with risingvelocity dispersion profiles, a variable stellar mass-to-light ratio can alsoaccount for the profile shape, instead of tangential anisotropy or asignificant ICL contribution. We note that, for some BCGs, a variable$\beta_{z}(r)$ (from radial to tangential anisotropy) can improve the model fitto the observed kinematic profiles. The observed diversity in these propertiesillustrates that BCGs are not the homogeneous class of objects they are oftenassumed to be.

Dynamical masses of brightest cluster galaxies I: stellar velocity anisotropy and mass-to-light ratios