Galaxy cluster luminosities and colours, and their dependence on cluster mass and merger state
Author
Mulroy, Sarah L.McGee, Sean L.
Gillman, Steven
Smith, Graham P.
Haines, Chris P.
Démoclès, Jessica
Okabe, Nobuhiro
Egami, Eiichi
Affiliation
Univ Arizona, Steward ObservIssue Date
2017-12
Metadata
Show full item recordPublisher
OXFORD UNIV PRESSCitation
Galaxy cluster luminosities and colours, and their dependence on cluster mass and merger state 2017, 472 (3):3246 Monthly Notices of the Royal Astronomical SocietyRights
© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We study a sample of 19 galaxy clusters in the redshift range 0.15 < z < 0.30 with highly complete spectroscopic membership catalogues (to K < K*(z) + 1.5) from the Arizona Cluster Redshift Survey, individual weak-lensing masses and near-infrared data from the Local Cluster Substructure Survey, and optical photometry from the Sloan Digital Sky Survey. We fit the scaling relations between total cluster luminosity in each of six bandpasses (grizJK) and cluster mass, finding cluster luminosity to be a promising mass proxy with low intrinsic scatter sigma ln (L|M) of only similar to 10-20 per cent for all relations. At fixed overdensity radius, the intercept increases with wavelength, consistent with an old stellar population. The scatter and slope are consistent across all wavelengths, suggesting that cluster colour is not a function of mass. Comparing colour with indicators of the level of disturbance in the cluster, we find a narrower variety in the cluster colours of 'disturbed' clusters than of 'undisturbed' clusters. This trend is more pronounced with indicators sensitive to the initial stages of a cluster merger, e.g. the Dressler Schectman statistic. We interpret this as possible evidence that the total cluster star formation rate is 'standardized' in mergers, perhaps through a process such as a system-wide shock in the intracluster medium.ISSN
0035-87111365-2966
Version
Final published versionSponsors
STFC Postgraduate StudentshipAdditional Links
http://academic.oup.com/mnras/article/472/3/3246/4085639/Galaxy-cluster-luminosities-and-colours-and-theirae974a485f413a2113503eed53cd6c53
10.1093/mnras/stx2108