Publication: Espectroscopía en el infrarrojo lejano para la región OMC-2 : optimización del procesado de datos y análisis físico
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2016-02-10
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Universidad Complutense de Madrid
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Abstract
Esta tesis presenta el trabajo realizado con el fin de conocer mejor la región OMC-2, que se encuentra en el complejo de formación estelar Orion A de la Galaxia, a través de los datos tomados con el satélite Herschel. Los datos de este trabajo pertenecen al programa HOPS (Herschel Orion Protostar Survey), un programa clave de tiempo abierto tomado con el satélite Herschel, liderado por el Dr. T. S. Megeath. El objetivo de este programa es responder a las cuestiones clave que conciernen a la formación estelar de estrellas de baja masa y de masa intermedia. Para este estudio, la región de Orión es un lugar óptimo por su proximidad 420 pc, (Menten et al. 2007) y la variedad de entornos en las que nacen estrellas en ella. El programa de observación de HOPS tomó imagenes y espectros con los instrumentos PACS y SPIRE, para objetos clasificados como protoestrellas por el satélite Spitzer. De ellas, 298 fueron observadas con la cámara PACS en las bandas 70 y 160 m, mientras que para 36 protoestrellas se tomaron espectros en el rango espectral 50-210 m , también con el instrumento PACS. Para dos de estos targets se tomaron mapas espectroscópicos de SPIRE de alta cobertura. La combinación de fotometría de campo profundo, espectroscopía de amplio rango espectral y mapas espectrales hacen de este programa un legado único para el estudio de la formación estelar. La estrategia observacional para las observaciones espectroscópicas de PACS han sido un compromiso entre la eficiencia observacional y el retorno científico. Un subconjunto de 4 objetos de la muestra espectroscópica de HOPS/PACS fue observada en modo mapa en el rango 55-210 m , entre las que se incluye la región OMC-2 tratada en esta tesis.
This PhD thesis presents the work performed to better understand the OMC-2 region, in the Orion A complex star-forming region in the Galaxy, by using the Herschel satellite data. We have contributed to the optimisation and calibration of the data processing required for the scientific analysis of the data. The data of this work belongs to the HOPS programme (Herschel Orion Protostar Survey), a Herschel Open Time Key Programe lead by Dr. T. S. Megeath. The objective of the program is to answer to key questions concerning low and intermediate-mass star formation. The Orion region is an optimal place for this study due to its proximity 420 pc, (Menten et al. 2007) and its variety of environments where stars form. The HOPS observing programme performed imaging and spectroscopy with the PACS and SPIRE instruments for Spitzer identified protostars. 298 protostars were imaged with the PACS camera at 70 and at 160 m bands and 36 protostars in full range spectroscopy from 50-210 m with the PACS instrument. For two of these targets, SPIRE spectrometer mapping observations with full sampling were performed. The combination of deep photometry, full range spectroscopy and spectral imaging makes the programme an unique legacy for star formation studies. The optimised observing strategy for the HOPS PACS spectroscopic sample was a trade o between observing e ciency and science return. A subset of 4 objects of the PACS spectroscopy sample has been observed in mapping mode for the range 55-210 m , included the OMC-2 region. The first challenge in this PhD was the optimisation of the standard spectroscopy data processing pipeline for the HOPS data collected by the PACS instrument. These data correspond to two smaller areas in the OMC-2 region, collected with di erent observing modes. The OMC-2 FIR 3 have been observed as an oversample raster, providing Nyquist sample spectral maps of the target, and FIR 4 was observed as a single pointing mode. A significant amount of this work consists of finding the optimal method for combining and processing both regions and both type of observations in a single and homogenous way to facilitate the analysis of the region as a whole, to be able to characterise the morphology and interactions among components. We applied simulations of hybrid data combining pointing information from the spacecraft with simulated flux distribution which allows to optimise parameters for the selection and parametrisation of the reconstruction techniques.
This PhD thesis presents the work performed to better understand the OMC-2 region, in the Orion A complex star-forming region in the Galaxy, by using the Herschel satellite data. We have contributed to the optimisation and calibration of the data processing required for the scientific analysis of the data. The data of this work belongs to the HOPS programme (Herschel Orion Protostar Survey), a Herschel Open Time Key Programe lead by Dr. T. S. Megeath. The objective of the program is to answer to key questions concerning low and intermediate-mass star formation. The Orion region is an optimal place for this study due to its proximity 420 pc, (Menten et al. 2007) and its variety of environments where stars form. The HOPS observing programme performed imaging and spectroscopy with the PACS and SPIRE instruments for Spitzer identified protostars. 298 protostars were imaged with the PACS camera at 70 and at 160 m bands and 36 protostars in full range spectroscopy from 50-210 m with the PACS instrument. For two of these targets, SPIRE spectrometer mapping observations with full sampling were performed. The combination of deep photometry, full range spectroscopy and spectral imaging makes the programme an unique legacy for star formation studies. The optimised observing strategy for the HOPS PACS spectroscopic sample was a trade o between observing e ciency and science return. A subset of 4 objects of the PACS spectroscopy sample has been observed in mapping mode for the range 55-210 m , included the OMC-2 region. The first challenge in this PhD was the optimisation of the standard spectroscopy data processing pipeline for the HOPS data collected by the PACS instrument. These data correspond to two smaller areas in the OMC-2 region, collected with di erent observing modes. The OMC-2 FIR 3 have been observed as an oversample raster, providing Nyquist sample spectral maps of the target, and FIR 4 was observed as a single pointing mode. A significant amount of this work consists of finding the optimal method for combining and processing both regions and both type of observations in a single and homogenous way to facilitate the analysis of the region as a whole, to be able to characterise the morphology and interactions among components. We applied simulations of hybrid data combining pointing information from the spacecraft with simulated flux distribution which allows to optimise parameters for the selection and parametrisation of the reconstruction techniques.
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Tesis inédita de la Universidad Complutense de Madrid, Facultad de Ciencias Físicas, leída el 18-12-2015