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Star formation mechanisms in luminous compact blue galaxies. Integral field spectroscopy study of local LCBGs (Mecanismo de formación estelar en galaxias luminosas compactas azules. Estudio espectroscópico de campo integral de galaxias luminosas compactas azules locales)

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2012-09-21
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Las galaxias luminosas compactas azules (LCBGs) son galaxias starburst, el extremo más brillante de la nube azul. A z = 1 eran muy abundantes y responsables de una buena parte de la formación de estelar de aquella época. Mientras que en el universo local son mucho menos numerosas, siendo la población que más ha cambiado desde entonces. En este trabajo se analizan 3 LCBGs locales con la técnica de espectroscopía bidimensional en el rango espectral visible y se estudian las propiedades del gas en emisión. A partir de los espectros reducidos y corregidos de extinción estelar, generamos mapas de flujos de líneas de emisión así como de otras propiedades físicas (extinción, mecanismo de excitación y metalicidad del gas, tasa de formación estelar...). Al mismo tiempo seleccionamos diferentes regiones para llevar a cabo un análisis más detallado determinando la extinción, mecanismo de excitación y metalicidad del gas, la tasa de formación estelar así como el número de estrellas Wolf-Rayet. A la vista de todas las propiedades derivadas en este trabajo se concluye que bajo el nombre de LCBGs se encuentra una categoría muy heterogénea, resultado de una casuística muy amplia pero con unas propiedades observacionales bien definidas. MRK538 es una gran espiral con formación estelar espoleada por una interacción con NGC7714. Mientras que UCM2250+2427 es también un espiral que sin necesidad de ninguna interacción (en el presente) tiene una alta tasa de formación estelar en las estructuras de su disco en rotación. En cambio para UCM1648+2855 no hemos identificado ningún mecanismo como el principal responsable de la formación estelar siendo por tanto el objeto de mayor interés en este trabajo. [ABSTRACT] Luminous Compact Blue Galaxies (LCBGs) are starburst galaxies, the most bright ones in the blue cloud. At z = 1 they were very numerous and responsible for a large proportion of the star formation at that time. Whilst in the local universe they are less common, being the population that have changed the most ever since. This work analyses 3 local LCBGs with the bidimensional spectroscopy technique in the optical spectral range and studies the properties of the gas in emission. Based on the reduced and extinction-corrected spectra, we generate maps of emission line uxes as well as other physical properties (gas extinction, excitation mechanism and metallicity, star formation rate...). While different regions are selected to carry out a more detailed analysis on them, by determining the gas extinction, excitation mechanism and metallicity, star formation rate and the number of Wolf-Rayet stars. In the light of all the properties and uxes measured it is therefore concluded that under the name of LCBGs there is a very heterogeneous category, as a result of the various casuistry, but with well-defined observational parameters. MRK538 is a large spiral with the star formation triggered by the interaction with NGC7714. Whereas UCM2250+2427 is also a large spiral that has a high star formation rate in the rotating-disc structures with no need for any interaction (in the present) to explain the observed values. However for UCM1648+2855 we have not identified any mechanism responsible for the star formation, being this object the most interesting one in this work.
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Máster Interuniversitario en Astrofísica. Facultad Ciencias Físicas. Curso 2011-2012
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