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dc.contributor.authorMulroy, Sarah L.
dc.contributor.authorMcGee, Sean L.
dc.contributor.authorGillman, Steven
dc.contributor.authorSmith, Graham P.
dc.contributor.authorHaines, Chris P.
dc.contributor.authorDémoclès, Jessica
dc.contributor.authorOkabe, Nobuhiro
dc.contributor.authorEgami, Eiichi
dc.date.accessioned2017-11-03T21:29:30Z
dc.date.available2017-11-03T21:29:30Z
dc.date.issued2017-12
dc.identifier.citationGalaxy cluster luminosities and colours, and their dependence on cluster mass and merger state 2017, 472 (3):3246 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stx2108
dc.identifier.urihttp://hdl.handle.net/10150/625963
dc.description.abstractWe 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.
dc.description.sponsorshipSTFC Postgraduate Studentshipen
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttp://academic.oup.com/mnras/article/472/3/3246/4085639/Galaxy-cluster-luminosities-and-colours-and-theiren
dc.rights© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.en
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectgravitational lensing: weaken
dc.subjectgalaxies: clusters: generalen
dc.subjectcosmology: observationsen
dc.titleGalaxy cluster luminosities and colours, and their dependence on cluster mass and merger stateen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
dc.description.collectioninformationThis 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.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-06-19T05:56:04Z
html.description.abstractWe 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.


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