The fundamental plane of early type galaxies in rich Abell clusters
The space defined by mass, radius and velocity dispersion for self-gravitating systems allows a dimension reduction called the Fundamental Plane (FP). These quantities are related through the Virial Theorem. Observationally, the slope of the FP is determined by the relationship between mass and lumi...
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| Tipo de recurso: | tesis de maestría |
| Estado: | Versión aceptada para publicación |
| Fecha de publicación: | 2010 |
| País: | México |
| Institución: | Instituto Nacional de Astrofísica, Óptica y Electrónica |
| Repositorio: | Repositorio Institucional del INAOE |
| Idioma: | inglés |
| OAI Identifier: | oai:inaoe.repositorioinstitucional.mx:1009/518 |
| Acceso en línea: | http://inaoe.repositorioinstitucional.mx/jspui/handle/1009/518 |
| Access Level: | acceso abierto |
| Palabra clave: | info:eu-repo/classification/Clusters de galaxias/Clusters of galaxies info:eu-repo/classification/Galaxias elípticas/Elliptical galaxies info:eu-repo/classification/Estructura galáctica/Galactic structure info:eu-repo/classification/cti/1 info:eu-repo/classification/cti/21 |
| Sumario: | The space defined by mass, radius and velocity dispersion for self-gravitating systems allows a dimension reduction called the Fundamental Plane (FP). These quantities are related through the Virial Theorem. Observationally, the slope of the FP is determined by the relationship between mass and luminosity, more precise the mass-to-light ratio (M/L). In this thesis, we have generated the FP for 6, 132 cluster galaxies as part of a comprehensive program to generate the FP for stellar systems, galaxies, groups, and galaxy clusters. We have also generated a control sample of 4, 423 field galaxies searching for environmental effects that could affect the FP for early-type galaxies. In this study, we have used photometric and spectra measurements from the Sloan Digital Sky Survey Data Release 7 (SDSS-DR7). We have developed an suit of scripts and programs to deal with data selection, cluster membership and galaxy velocity dispersion. We have measured the velocity dispersions of galaxies using two methods: the crosscorrelation method and the direct-line-profile fitting method. We have used the Petrosian radius as a non-parametric scale indicator. The Petrosian radius overcomes the uncertainties of surface brightness profile fitting. |
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