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 present a detailed investigation of the cluster stellar mass-to-light(M*/L) ratio and cumulative stellar masses, derived on a galaxy-by-galaxybasis, for 12 massive (M500 ~ 10^14 - 10^15 Msun), nearby clusters withavailable optical imaging data from the Sloan Digital Sky Survey Data Release10 and X-ray data from the Chandra X-ray Observatory. Our method involves astatistical cluster membership using both photometric and spectroscopicredshifts when available to maximize completeness whilst minimizingcontamination effects. We show that different methods of estimating the stellarmass-to-light ratio from observed photometry result in systematic discrepanciesin the total stellar masses and average mass-to-light ratios of clustergalaxies. Nonetheless, all conversion methodologies point to a lack ofcorrelation between M*/Li and total cluster mass, even though low-mass groupscontain relatively more blue galaxies. We also find no statisticallysignificant correlation between M*/Li and the fraction of blue galaxies. Forthe mass range covered by our sample, the assumption of a Chabrier IMF yieldsan integrated M*/Li = 1.7 +/- 0.2 Msun/Lsun, a lower value than used in mostsimilar studies, though consistent with the study of low-mass galaxy groups byLeauthaud et al. (2012). A light (diet) Salpeter IMF would imply a ~60%increase in M*/Li.

Revised Mass-to-Light Ratios For Nearby Galaxy Groups and Clusters