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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/1549
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dc.contributor.authorFernley, J.A.-
dc.contributor.authorBhavsar, S.P.-
dc.date.accessioned2006-11-30T07:27:09Z-
dc.date.available2006-11-30T07:27:09Z-
dc.date.issued1984-10-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 1984, Vol.210, p883-890en
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2289/1549-
dc.descriptionOpen Accessen
dc.description.abstractModel clusters selected from n-body simulations of clustering are used to evaluate the accuracy of virial methods in mass determination. Clusters having high virial masses due to contamination are identifiable by means of a chi-squared test which compares line-of-sight velocities with a normal distribution. For clusters with good chi-squared fits, the virial mass-to-actual mass ratio obtained indicates that a large degree of scatter inheres in the virial method. Atteention is given to mass-to-light ratio results for the Coma, A2151, and Hercules Supercluster formations. While the last of these is seriously contaminated, solar mass/solar luminosity ratios of 201 and 168 are derived for the other two. These ratios, however, are held to be uncertain by a factor of at least 3, and may therefore be due to 'massive halo' galaxies and intracluster gas.en
dc.format.extent8338 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherBlackwell Publishing for the Royal Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?1984MNRAS.210..883Fen
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984MNRAS.210..883F&link_type=ARTICLE&db_key=ASTen
dc.rights(1984) Royal Astronomical Societyen
dc.subjectASTRONOMICAL MODELS,en
dc.subjectGALACTIC CLUSTERS,en
dc.subjectVIRIAL THEOREM,en
dc.subjectBIG BANG COSMOLOGY,en
dc.subjectERROR ANALYSIS,en
dc.subjectMANY BODY PROBLEM,en
dc.subjectMASS DISTRIBUTION,ATIOS,en
dc.subjectMASS TO LIGHT RATIOSen
dc.titleThe virial masses of clusters of galaxies and the effects of contaminationen
dc.typeArticleen
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