Searching for gaseous giant planets around debris disks
Fecha
2022
Autores
Profesor Guía
Formato del documento
Thesis
ORCID Autor
Título de la revista
ISSN de la revista
Título del volumen
Editor
Universidad de Valparaíso
Ubicación
ISBN
ISSN
item.page.issne
item.page.doiurl
Facultad
Departamento o Escuela
Intituto de Física y Astronomía
Determinador
Recolector
Especie
Nota general
Doctorado en Astrofísica. Universidad de Valparaíso. 2022.
Resumen
The past decades have clearly demonstrated that planet formation is an efficient process and that it can lead to a vast variety of planetary systems. Since then, understanding how to form this enormous population of extrasolar planets has been an important question for modern astrophysics. It has been possible to formalize different theories of planetary formation trying to explain the populations of planets that we observe. Direct imaging has provided important hints that help to confront and challenge these theories from the characterization of planets as well as their detectability. Despite the significant advances in technological terms (new instruments and techniques have been developed in recent years), and the great relevance of several discoveries (e.g., PDS70), direct imaging still has great challenges that must be faced.
In this thesis, we first provide some context on what we know about planetary formation and detection techniques, with an emphasis on direct imaging and its challenges in Chapter 1. We then investigate how to improve direct imaging data reductions and which are the main sources of improvement, when using the NaCo instrument. To do this, we developed a pipeline called CenteR within the ISPY consortium, to investigate the effects of centering and frame selection in sequences of thousands of frames. Our new reduction strategy and the main conclusions are presented in Chapter 2. In addition, we focused on searching for giant planets using the SPHERE instrument. Our sample was built based on hints of possible planet-disc interactions. Such interactions, complemented with information about the location of the disk from SED analysis, the proper motion anomaly, and recent planet-disk interaction models, provided us with important constraints on the presence of possible planets. Chapter 3 shows the target selection, the treatment carried out on the data, and the main conclusions of the analysis of our sample and our non-detections of planets. In Chapter 4 we present a brief conclusion on the work of this thesis and in Chapter 5 the future perspective on this work in the context of new instruments and archival data.
Descripción
Lugar de Publicación
Valparaíso
Auspiciador
Palabras clave
PLANETAS EXTRASOLARES DETECCION
Licencia
Atribución-NoComercial-CompartirIgual 3.0 Chile (CC BY-NC-SA 3.0 CL)