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Detection-And-Characterization-Of UNIVERSIDAD DE CHILE FACULTAD DE CIENCIAS FÍSICAS Y MATEMÁTICAS DEPARTAMENTO DE ASTRONOMÍA DETECTION AND CHARACTERIZATION OF SINGLE AND DOUBLE STELLAR/PLANETARY SYSTEMS TESIS PARA OPTAR AL GRADO DE DOCTORA EN CIENCIAS, MENCIÓN ASTRONOMÍA MARITZA GABRIELA SOTO VÁSQUEZ PROFESOR GUÍA: JAMES STEWART JENKINS MIEMBROS DE LA COMISIÓN: GUILLEM ANGLADA-ESCUDÉ RICARDO RODRIGO MUÑOZ VIDAL PATRICIO MICHEL ROJO RUBKE Este trabajo ha sido parcialmente financiado por CONICYT-PCHA/Doctorado Nacional/2014-21141037 SANTIAGO DE CHILE 2018 RESUMEN DE LA MEMORIA PARA OPTAR AL TÍTULO DE DOCTORA EN CIENCIAS, MENCIÓN ASTRONOMÍA POR: MARITZA GABRIELA SOTO VÁSQUEZ FECHA: 20 DE JUNIO, 2018 PROF. GUÍA: JAMES STEWART JENKINS DETECTION AND CHARACTERIZATION OF SINGLE AND DOUBLE STELLAR/PLANETARY SYSTEMS El crecimiento exponencial del número de exoplanetas descubiertos en los últimos años ha derivado en un mayor entendimiento de los planetas en la galaxia, de los cuales la Tierra es miembro; pero aún nos queda un gran camino por delante. El propósito de esta tesis es descubrir y confirmar nuevos planetas orbitando estrellas enanas y gigantes, además de desarrollar técnicas para extraer la mayor cantidad de información posible de las estrellas, permitiendo así una mayor compresión de los sistemas planetarios en estudio. Primero, analizamos datos crudos tomados con FEROS de las estrellas HD 11977, HD 47536, HD 110014, y HD122430, todas con al menos un planeta descubierto. Confirmamos la existencia de los planetas orbitando a HD 11977, HD 47536 y HD 110012, pero con parámetros orbitales distintos a los publicados. Además, no encontramos evidencia que respaldara la existencia del segundo planeta orbitando a HD 47536, ni que hubiese planetas alrededor de HD 122430 y HD 70573. Finalmente, reportamos el descubrimiento de un segundo planeta orbitanto a HD 110014, con una masa mínima de 3.1 MJupy periodo orbital de 130 días. Luego, usando datos fotométricos de la campaña 11 y 12 de la misión K2, junto con mediciones de velocidad radial tomados con los espectrógrafos HARPS, FEROS, y Coralie, reportamos el descubrimiento de dos planetas Jupiter calientes orbitando a dos estrellas enanas. Encontramos +0:10 +0:13 +0:07 +0:15 que K2-237 b y K2-238 b tienen masas de 1:36−0:10 y 0:86−0:12 MJup, radio de 1:63−0:08 y 1:30−0:14 RJup, y orbitan a sus estrellas con órbitas de 1.28 y 3.2 días, respectivamente. El gran tamaño de K2-237 b nos lleva a concluir que corresponde a un Jupiter caliente altamente inflado, mientras que el radio de K2-238 b es consistente con modelos teóricos. K2-237 b representa un excelente laboratorio para estudios de atmósferas planetarias. Finalmente, desarrollamos una herramiento que permite el cálculo automático de parámetros es- telares para grandes cantidades de estrellas, usando espectros echelle de alta resolución. SPECIES mide anchos equivalentes para un gran número de líneas de fierro y los usa para resolver la ecuación de transferencia radiativa asumiento equilibrio termodinámico local para obtener los párametros at- mosféricos. Estos valores son usados para obtener la abundancia de 11 elementos químicos en las atmósferas estelares. La velocidad de rotación y de macroturbulencia son obtenidos usando fór- mulas calibradas a la temperatura estelar, y perfiles de línea sintéticos que igualen a los perfiles medidos para cinco líneas de absorción. SPECIES obtiene la masa, radio y edad interpolando en isocronas MIST, usando el método Bayesiano. Luego de una serie de pruebas encontramos que los parámetros que obtiene SPECIES son congruentes con los de la literatura. También deriva- mos relaciones analíticas que describen las correlaciones entre los parámetros, e implementamos nuevos métodos para trabajar con estas correlaciones en la obtención de las incertezas asociadas a cada medición. i ii RESUMEN DE LA MEMORIA PARA OPTAR AL TÍTULO DE DOCTORA EN CIENCIAS, MENCIÓN ASTRONOMÍA POR: MARITZA GABRIELA SOTO VÁSQUEZ FECHA: 20 DE JUNIO, 2018 PROF. GUÍA: JAMES STEWART JENKINS DETECTION AND CHARACTERIZATION OF SINGLE AND DOUBLE STELLAR/PLANETARY SYSTEMS The exponential growth of the exoplanet detection frequency in the past years has led to a great improvement in our understanding of the population of planets in the galaxy; of which the Earth is one, yet we are still very much at the beginning of a long road ahead. The aim of this thesis work is to discover and confirm new planetary candidates orbiting dwarf and giant stars, as well as to develop techniques to extract as much information from the host-star as possible, allowing a deeper understanding of the planetary system under study. We first reanalyzed raw FEROS data for the stars HD 11977, HD 47536, HD 70573, HD 110014 and HD 122430, all of which were claimed to have at least one planetary companion. We confirmed the existence of the planets around HD 11977, HD 47536 and HD 110014, but with different orbital parameters than those previously published. In addition, we found no evidence of the second planet candidate around HD 47536, nor any companions orbiting HD 122430 and HD 70573, and therefore we helped debias de population statistics for giant stars. Finally, we report the discovery of a second planet around HD 110014, with a minimum mass of 3.1 MJup and a orbital period of 130 d. Next, using photometric data from Campaigns 11 and 12 of the K2 mission, along with radial velocity measurements from the HARPS, FEROS, and Coralie spectrographs, we report the discov- ery of two hot Jupiters orbiting two dwarf stars. We find that K2-237 b and K2-238 b have masses +0:10 +0:13 +0:07 +0:15 of 1:36−0:10 and 0:86−0:12 MJup, radii of 1:63−0:08 and 1:30−0:14 RJup, and are orbiting their host stars in 2.18 and 3.2 day orbits, respectively. The large radius of K2-237 b leads us to conclude that this corresponds to a highly inflated hot Jupiter-type planet, while the radius of K2-238 b is consis- tent with theoretical models. K2-237 b represents an excellent laboratory for planetary atmosphere studies. Finally, we develop a tool that allows the automated calculation of stellar parameters for a large number of stars, using high-resolution echelle spectra. SPECIES measures the equivalent widths of many iron lines and uses them to solve the radiative transfer equation assuming local thermodynamic equilibrium to obtain the atmospheric parameters. These values are used to derive the abundance of an additional 11 important chemical elements in the stellar photosphere. Rotation and macroturbulent velocity are obtained using temperature calibrators and synthetic line profiles to match the observed spectra of five absorption lines. SPECIES derives the mass, radius, and age, by interpolating in a grid of MIST isochrones, using a Bayesian approach. After thorough testing we found that SPECIES obtains bulk parameters that are in good agreement with those in the literature. We also obtained analytic relations to describe the correlations between different parameters, and we implemented new methods to better handle these correlations, providing a better description of the uncertainties associated with the measurements. iii iv Agradecimientos Hay muchas personas que me ayudaron a completar este trabajo de Tesis, y no podré mencionarlos a todos en esta página. Primero, debo agradecer a mi profesor guía. James, creo que fuiste el mejor guía que me pudo haber tocado. Siempre me trataste como una igual, y eso me dio la confianza de hablarte de cualquier tema, de poder ir a tu oficina y preguntarte lo que fuese, sin importar lo básico o simple que fuese esa duda. A pesar de que siempre me empujabas a seguir trabajando, nunca me sentí presionada, y sabía que podía trabajar a mi propio ritmo. Bajo tu guía siento que me fui convirtiendo poco a poco en una investigadora más independiente. Fuiste un muy buen amigo en todo este proceso, desde el primer día, y no habría podido terminar este trabajo sin tu apoyo ni guía. I also want to thank Didier Queloz, for being a great advisor during my time in Cambridge. Even though you always had so much work to do, you still found the time to talk with me, and take interest in my research. I really thank all your support. Quiero también agradecer a mi familia por todo el apoyo que siempre me dieron. Por nunca dudar de esta carrera que decidí seguir, y por apoyarme desde el primer momento que mostré interés en la astronomía. Por siempre mostrarse orgullosos de mis logros, y emocionarse cada vez que aparecía mi cara en algún lado. También una mención muy importante a todas mis mascotas, que siempre quieren pasar tiempo conmigo, yo también quiero pasar todo mi tiempo con ellos. Finalmente, quiero agradecer a todas las personas que hicieron mi paso por Calán una experi- encia muy divertida. A todas las personas que pasaron por mi oficina: la Paula S, Paula L., Srini, Jose, Elise, Matías S., Coni, y Bica. Ustedes hacían el ir a Calán algo no terrible, porque siempre sabía que me iban a hacer reir, y que siempre podía contarles a ustedes lo que fuese que me pasara. Cada vez que me sentía frustrada o aburrida de todo, ustedes me levantaban el ánimo. La oficina ’Pequeños Placeres’ es de verdad la mejor de Calán, donde todo pasa, y la más divertida de estar. Aunque a veces se tornaba difícil trabajar porque todos estábamos hablando, no lo cambiaría por nada. Una mención especial al Matías D, que siempre entendió mi frustración con Calán y la inves- tigación, junto con otras cosas. I must also thank my very dear friends Irina and Lucinda. You two, along with Penny and the cats, made my months in Cambridge some of the best ones I’ve ever had.
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