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Luis Fernando Lanz Oca DEPARTAMENTO DE FISICA´ MODERNA INSTITUTO DE FISICA´ DE CANTABRIA UNIVERSIDAD DE CANTABRIA CSIC-UC DETECCION´ DE FUENTES EXTRAGALACTICAS´ EN MAPAS DE LA RADIACION´ DEL FONDO COSMICO´ DE MICROONDAS MEDIANTE TECNICAS´ MULTIFRECUENCIALES Memoria presentada para optar al t´ıtulo de Doctor otorgado por la Universidad de Cantabria por Luis Fernando Lanz Oca Programa de Doctorado de Ciencias, Tecnolog´ıa y Computacion´ Curso 2015/2016 Declaracion´ de Autor´ıa Diego Herranz Munoz˜ , Doctor en Ciencias F´ısicas y profesor titular de la Universidad de Cantabria, y Marcos Lopez-Caniego´ Alcarria, Doctor en Ciencias F´ısicas y cient´ıfico en Aurora Technologies para la Agencia Espacial Europea, CERTIFICAN que la presente memoria Deteccion´ de fuentes extragalacticas´ en mapas de la radiacion´ del fondo cosmico´ de microondas mediante tecnicas´ multifrecuenciales ha sido realizada por Luis Fernando Lanz Oca bajo nuestra direccion´ en el Instituto de F´ısica de Cantabria, para optar al t´ıtulo de Doctor por la Universidad de Cantabria. Consideramos que esta memoria contiene aportaciones cient´ıficas suficientemente relevantes como para constituir la Tesis Doctoral del interesado. En Santander, a 25 de enero de 2016, Diego Herranz Munoz˜ Marcos Lopez-Caniego´ Alcarria A Vega. ¿Anudas tu´ los lazos de las Pleyades´ o desatas las cuerdas del Orion?´ ¿Haces salir las H´ıadas a su tiempo y gu´ıas a la Osa y sus cachorros? ¿Conoces las leyes de los cielos? ¿Regulas su dominio sobre la tierra? Job 38,31-33 Agradecimientos La tesis que tienes entre las manos ha sido el fruto de muchos (mas´ de los esperados) anos,˜ y no hubiera sido posible sin la inestimable ayuda de muchas personas. Pero para ser justos, el primer ≪gra- cias≫ se lo he de dar a Jose´ Luis Sanz, que me ofrecio´ al entrar en una de sus clases de Relatividad General y Cosmolog´ıa hacer la tesis en su grupo con el entonces profesor de las practicas´ (y futuro director de esta tesis) Diego Herranz. Podr´ıa decirse que ese momento fue la superficie de last scat- tering de mi doctorado. Por supuesto, mil gracias a mis directores, el ya nombrado Diego y Marcos Lopez-Caniego´ (el root), especialmente por estas ultimas´ semanas y meses donde les he bombardeado con las sucesivas versiones de la tesis y los plazos de entrega. Sin sus consejos y sus directrices esta tesis no hubiera sido posible. Por supuesto, tambien´ tengo que agradecer al resto del grupo su cercan´ıa y disponibilidad siempre que ha sido necesario: Kike, Belen´ B., Chema, Patri, Patxi, Pier Paolo, Marina, Diego M., Franceso, etc. Y muy en particular a mis sucesivos companeros˜ de despacho, cuyo aporte, seguramente mas´ vital que laboral, ha sido mas´ importante que cualquier paper que hubiera podido publicar. Desde los primeros, como Jacobo y Andres´ y su ≪sutil≫ diplomacia, hasta las maquinaciones de Marcos (no te perdonare´ jamas´ lo del Diplomacy, Marcos, JAMAS).´ Tambien´ a Raquel, la gallega mas´ americana (o al reves,´ no recuerdo) y su ayuda con mi ingles;´ a Biuse, cuyo buen humor es contagioso; a Raul,´ por ser buen companero˜ de viaje y de conversaciones (y solo he pasado lo mas´ facil,´ chorbo); a Airam, pro- longacion´ de las ecuaciones en el mundo real y hacerme descubrir, junto a Raul´ y Biuse, las maravillas culinarias del Emilio’s. Y a David, nuestro ironman particular, por no ponerse l´ımites (el Soplao te espera, chaval). Tambien´ es justo mencionar a otras personas con las que he compartido otros momentos extra- IFCA, como el futbol´ junto a Gervasio, Esteban, Jordi, Nuria,´ Richard, Federico, Diego T., Carlos, Dani, etc; el rol junto a Anuar, Nacho, Judit, Rosa, Belen´ H., Angel,´ etc; el poker´ junto a Diego P. oInaki˜ entre otros; y alguno mas´ que seguramente se me escape (Lander, Joserra, etc). He tenido la oportunidad de descubrir a gente muy buena que no solo trabaja bien, sino con la que pasarselo´ bien. A Joaqu´ın, Laura, Gianfranco y Marcella por su hospitalidad en mis estancias en Trieste y Padua. Y para terminar (tienes toda una tesis que leer), reconocer aqu´ı a las personas que no me han pasado ni un codigo´ pero que han sido los pilares de todo este trabajo. Para empezar, mis padres, a los que no solo tengo que (debo) agradecer todo lo que me han dado, sino reconocerselo.´ A mis hermanos, por su apoyo. A mi tocayo, por estar ah´ı aunque no nos veamos mucho; la gente de Vista Alegre, por llevar un VII mundo nuevo en sus corazones. A mis cunaos˜ , en particular a Cova y Jorge, y las laurisilvas. A Yoli, por la paciencia de estos ultimos´ tiempos (no habra´ una segunda tesis, jeje) y por su comprension.´ Y a la enana, por hacerme olvidar todos los malos momentos con su sonrisa. Aunque no pueda leer aun´ estas palabras, espero que cuando pueda hacerlo sea tan feliz como lo soy yo con ella. VIII DEPARTAMENTO DE FISICA´ MODERNA INSTITUTO DE FISICA´ DE CANTABRIA UNIVERSIDAD DE CANTABRIA CSIC-UC DETECTION OF EXTRAGALACTIC SOURCES IN COSMIC MICROWAVE BACKGROUND MAPS WITH MULTIFREQUENCY TECHNIQUES A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics by Luis Fernando Lanz Prologue The observation and the analysis of the Cosmic Microwave Background (CMB) radiation is a crucial task to understand the early Universe and its properties. The last observations of this radiation (and its subsequent analysis) have allowed to know with more accuracy the age of the Universe (about 13.8 billion of years), the percentages of the composition of the Universe ( 4.9% of baryonic matter, ∼ 26.8% of dark matter and the remaining 68.3% of dark energy) and other cosmological parameters ∼ ∼ (Planck Collaboration et al., 2015e). When observing the sky at the microwave frequency range, we can see a combination of different components, e.g., Galactic and extragalactic diffuse and compact emission, and instrumental noise, besides the CMB itself. In order to study and characterise, any, or all, of these component, it is important to develop techniques that separate them from the observational mixture we detect with our instruments. In the case of the extragalactic objects, that appear most of times like point sources due to their distance from us and the relatively poor angular resolution of the experiments, linear filters are suitable devices to detect them. Besides, their detection is not only interesting to remove them from the CMB data, but also to study the point sources themselves. In the literature there are many examples where filters have been successfully used to detect point sources. Until the advent of experiments like WMAP and Planck, there was a lack of information about extragalactic compact sources in the frequency range 20-1000 GHz, gap that has been recently started to be covered with those experiments. Linear filters have been widely applied in these experiments, showing their efficiency. The literature also shows that most of times the techniques used has been single-frequency, i.e., filters deal with only one frequency each time. These single-frequency tech- niques, according to the latter results, have shown to be near the limit of their performance and capac- ity. While we wait for future higher resolution experiments we can develop new tools that improve the detection of fainter sources, tools that can be used in the future with the higher resolution experiments as well. To achieve this goal, in this Thesis I will introduce a multifrequency linear filtering method. The use of two or more channels in a simultaneous way allow us to take into account more available information that is ignored in the single-frequency methods. In the case of this Thesis, the additional information used will be the cross-power spectrum of the noise, spatial information of the point sources (like the fact that one source is located in the same point in the sky at two different frequencies) and the parametrisation of the spectral behaviour of the point sources like a power law. The multifrequency XI linear filter to be presented in this Thesis uses all this information in a natural way. Its performance is compared with the matched filter applying both techniques (the single- and the multi-frequency) in a set of realistic simulations of the Planck sky, showing the results in the Chapter 3. Accuracy in the recovered flux density and spectral index, percentages of spurious and real detections, etc, are better in general with the multifrequency method than with the matched filter. Once the efficiency and power of the multifrequency method has been tested, it will be applied to real data, in particular the channels V and W (61 and 94 GHz, respectively) in the WMAP 7-year data. After some considerations (in particular the antenna beams) that must be taken into account respect to the Planck case mentioned in the previous paragraph, and explained more in detail in the Chapter 4, the multifilter tool obtains, in a totally blind search, a number of 119 5σ extragalactic objects at both channels simultaneously, to be compared with the 22 detections at 94 GHz in a non-blind search with the WMAP 3-year data (Lopez-Caniego´ et al., 2007). XII XIV Contents 1 INTRODUCTION 1 1.1 The ΛCDM Model and the Cosmic Microwave Background . 1 1.2 CMBanisotropies..................................... 10 1.2.1 Primary anisotropies . 10 1.2.2 Secondary anisotropies . 12 1.2.3 Polarisation of the CMB . 13 1.3 Galactic contamination . 15 1.3.1 Synchrotron emission . 15 1.3.2 Free-free emission . 19 1.3.3 Thermaldust ................................... 19 1.3.4 Spinningdust................................... 20 1.3.5 COemission ................................... 20 1.4 Extragalactic components .
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