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

We present a study of the evolution of brightest cluster galaxies (BCGs) in asample of clusters at $0.05 \leq z<0.35$ from the SDSS and WISE with halomasses in the range $6 \times 10^{13}M_\odot$ (massive groups) -$10^{15.5}M_\odot$ (Coma-like clusters). We analyse optical and infraredcolours and stellar masses of BCGs as a function of the mass of their hosthaloes. We find that BCGs are mostly red and quiescent galaxies and that aminority ($\sim 9$\%) of them are star-forming. We find that the optical $g-r$colours are consistent with those of red sequence galaxies at the sameredshifts; however, we detect the presence of a tail of blue and mostlystar-forming BCGs preferentially located in low-mass clusters and groups.Although the blue tail is dominated by star-forming galaxies, we find thatstar-forming BCGs may also have red $g-r$ colours, indicating dust-enshroudedstar formation. The fraction of star-forming BCGs increases with redshift anddecreases with cluster mass and BCG stellar mass. We find that cool-coreclusters host both star-forming and quiescent BCGs; however, non cool-coreclusters are dominated by quiescent BCGs. Star formation appears thus as theresult of processes that depend on stellar mass, cluster mass and cooling stateof the intra-cluster medium. Our results suggest no significant stellar massgrowth at $z<0.35$, supporting the notion that BCGs had accreted most of theirmass by $z = 0.35$. Overall we find a low (1\%) AGN fraction detected at IRwavelengths.

monthly notices of the royal astronomical society

The Evolution of Brightest Cluster Galaxies in the Nearby Universe I:  Colours and Stellar Masses from the Sloan Digital Sky Survey and Wide  Infrared Survey Explorer