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

Galaxy clusters have long been theorised to quench the star-formation oftheir members. This study uses integral-field unit observations from the$K$-band Multi-Object Spectrograph (KMOS) - Cluster Lensing And Supernovasurvey with Hubble (CLASH) survey (K-CLASH) to search for evidence of quenchingin massive galaxy clusters at redshifts $0.3<z<0.6$. We first constructmass-matched samples of exclusively star-forming cluster and field galaxies,then investigate the spatial extent of their H$\alpha$ emission and study theirinterstellar medium conditions using emission line ratios. The average ratio ofH$\alpha$ half-light radius to optical half-light radius($r_{\rm{e},\rm{H}\alpha}/r_{\rm{e},R_c}$) for all galaxies is $1.14\pm0.06$,showing that star formation is taking place throughout stellar discs at theseredshifts. However, on average, cluster galaxies have a smaller$r_{\rm{e},\rm{H}\alpha}/r_{\rm{e},R_c}$ ratio than field galaxies: $\langler_{\rm{e},\rm{H}\alpha}/r_{\rm{e},R_c}\rangle = 0.96\pm0.09$ compared to$1.22\pm0.08$ (smaller at a 98\% credibility level). These values areuncorrected for the wavelength difference between H$\alpha$ emission and$R_c$-band stellar light, but implementing such a correction only reinforcesour results. We also show that whilst the cluster and field samples followindistinguishable mass-metallicity (MZ) relations, the residuals around the MZrelation of cluster members correlate with cluster-centric distance; galaxiesresiding closer to the cluster centre tend to have enhanced metallicities(significant at the 2.6$\sigma$ level). Finally, in contrast to previousstudies, we find no significant differences in electron number density betweenthe cluster and field galaxies. We use simple chemical evolution models toconclude that the effects of disc strangulation and ram-pressure stripping canquantitatively explain our observations.

K-CLASH: Strangulation and Ram Pressure Stripping in Galaxy Cluster Members at 0.3 < z < 0.6