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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

It has been observed that low redshift early-type galaxies can be separatedinto slow and fast rotators according to a proxy of specific stellar angularmomentum, $\lambda_{R_e}$. Detailed studies of a handful of nearby clustershave shown that slow rotators are generally found at the centres of clusterswhere the number density is highest, whereas the fast rotators trace the trendfollowed by early-type galaxies of increasing in number with local density. Inthis paper, we study the environmental distribution of slow and fast rotatorsusing the stellar kinematics of about 3900 galaxies from the Sloan Digital SkySurvey's Mapping Nearby Galaxies at Apache Point Observatory survey. Forgalaxies in groups closer than $z=0.08$ that are not observed with MaNGA butsatisfy the necessary conditions for slow rotators, we visually assignslow/fast rotator classifications to obtain a complete sample. Our finalcatalogue contains about 900 groups of five or more members. We observe thekinematic morphology-density (kT-$\Sigma$) relation for each group and find anincreasing fraction of massive slow rotators with increasing number density. Weprovide evidence suggesting that the observed lack of trends in angularmomentum with environment at fixed stellar mass is partly because the maximumdensity varies between clusters, and that the locations of massive slowrotators are strongly correlated with peak densities in galaxy groups andclusters. We conclude that the (projected) number density relative to thecluster peak is more fundamental than the absolute number density ininfluencing the abundance of slow rotators. We find that the kT-$\Sigma$relation does exist at fixed stellar mass, and we rule out the hypothesis thatthe kT-$\Sigma$ relation is a result of dynamical friction alone, insteadarguing that massive slow rotators grow hierarchically in tandem with theirhost clusters.

SDSS-IV MaNGA: New benchmark for the connection between stellar angular momentum and environment: a study of about 900 groups/clusters