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Implicaciones Cosmológicas De Las DEPARTAMENTO DE F´ISICAMODERNA INSTITUTODEF´ISICA DE CANTABRIA UNIVERSIDAD DE CANTABRIA IFCA (UC-CSIC) IMPLICACIONES COSMOLOGICAS´ DE LAS ANISOTROP´IAS DE TEMPERATURA Y POLARIZACION´ DE LA RFCM Y LA ESTRUCTURA A GRAN ESCALA DEL UNIVERSO Memoria presentada para optar al t´ıtulo de Doctor otorgado por la Universidad de Cantabria por Ra´ul Fern´andez Cobos Declaraci´on de Autor´ıa Patricio Vielva Mart´ınez, Doctor en Ciencias F´ısicas y Profesor Contratado Doctor de la Universidad de Cantabria y Enrique Mart´ınez Gonz´alez, Doctor en Ciencias F´ısicas y Profesor de Investigaci´on del Consejo Superior de Investigaciones Cient´ıficas, CERTIFICAN que la presente memoria Implicaciones cosmol´ogicas de las anisotrop´ıas de temperatura y polarizaci´on de la RFCM y la estructura a gran escala del universo ha sido realizada por Ra´ul Fern´andez Cobos bajo nuestra direcci´on 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 rele- vantes como para constituir la Tesis Doctoral del interesado. En Santander, a 19 de septiembre de 2014, Patricio Vielva Mart´ınez Enrique Mart´ınez Gonz´alez A mis padres. Creo que seremos inmortales, que sembraremos las estrellas y viviremos eternamente en la carne de nuestros hijos. Ray Bradbury. Agradecimientos La realizaci´on de esta tesis doctoral ha servido de excusa para llevar a cabo un proyecto mucho m´as amplio, que se ha saldado con unos a˜nos de impagable crecimiento personal y del que estas p´aginas constituyen solo la peque˜na parte tangible. Quisiera reservar unas l´ıneas a todas las personas y organismos que han hecho posible esta tarea. Empezando —como no podr´ıa ser de otro modo— por los in- condicionales, mis padres, que han estado apoy´andome desde el principio y en todo momento, y han sabido relativizar mis accesos catastrofistas. Sin olvidar que esto viene de mucho antes, a saber, de un D´ıa del Libro y una historia geol´ogica de la Tierra para ni˜nos. No alcanzan a imaginar el valor de la confianza que depositan en m´ı. Sin ´animo de frivolizar, y porque la ciencia —y las personas que la cultivan— no se mantiene del aire, creo necesario agradecer la financiaci´on recibida a cargo del Programa Junta de Ampliaci´on de Estudios (JAE) del Consejo Superior de Investiga- ciones Cient´ıficas, subvencionado por el Fondo Social Europeo, que ha posibilitado mi independencia durante el periodo de investigaci´on, as´ıcomo la realizaci´on de varias estancias en otros centros. Me gustar´ıa resaltar la inestimable labor de mis directores de tesis, que me han visto medrar desde aquella primera vez que los visit´econ veintid´os a˜nos, y su tenacidad por que aprenda el oficio: Patricio Vielva, accesible desde el primer d´ıa y con una paciencia infinita; y Enrique Mart´ınez, cuya cotidianidad transmite su pasi´on por hacer ciencia. Tambi´en merecen un espacio los investigadores que me acogieron durante mis es- tancias breves de doctorado en Tenerife y Roma: Jos´eAlberto Rubi˜no, por su tiempo y dedicaci´on; Ricardo G´enova, siempre tan dispuesto a echar una mano; y Amedeo Balbi, por su buena disposici´on. As´ıcomo las personas que volvieron m´as amena mi estad´ıa: Carlos L´opez, por su visi´on de la vida y su amistad; y Marina Migliaccio, que vel´opor mis ´animos en Tor Vergata. Y tambi´en el personal del Observatorio del Teide, por no dejarme ceder ante la locura durante mis liminales subidas de dieciocho d´ıas. Quisiera agradecer adem´as a Luigi Toffolatti y a Bel´en Barreiro, quienes fueron mis padrinos en Santander y me brindaron la oportunidad de empezar todo esto. Y, por supuesto, trasladar aqu´ıel apoyo recibido por el resto del grupo de Cosmolog´ıa VII Observacional e Instrumentaci´on del Instituto de F´ısica de Cantabria. Mi percepci´on de esta etapa ser´ıa completamente distinta de excluir el buen am- biente de convivencia que ha reinado en el despacho. Son responsables mis compa˜neros a lo largo de todo este periplo: Andr´es Curto, la ´unica persona capaz de lograr que la Salamanca rural sea Macondo, me ense˜n´oque si algo corre como un pato y grazna como un pato, probablemente sea un pato; Luis Lanz, camarada de viajes con el que habr´e de contar ma˜nana, porque ambos sabemos que solo hemos pasado lo m´as f´acil; Raquel Fraga, non-cosmological yankee style, a quien admiro por su obstinaci´on en perseguir sue˜nos; David Ortiz, que a menudo aporta una nota cabal a la sinfon´ıa ca´otica que habita entre las mesas; Airam Marcos, cuya curiosidad por lo que le rodea raya en lo patol´ogico y por eso nos entendemos tan bien; Biuse Casaponsa, confidente con un sexto sentido a quien no cambiar´ıa ni por mil gigapeutas; y Nuria Castell´o, cuya falta de per´ıfrasis solo se ve superada por su coraje. Que el mundo recuerde esta peque˜na burbuja de paliques y debates. Tambi´en me gustar´ıa hacer una menci´on especial al buen hacer de Mar´ıa Saro, autora del dibujo de portada. VIII DEPARTAMENTO DE F´ISICAMODERNA INSTITUTODEF´ISICA DE CANTABRIA UNIVERSIDAD DE CANTABRIA IFCA (UC-CSIC) COSMOLOGICAL IMPLICATIONS FROM THE CMB TEMPERATURE AND POLARISATION ANISOTROPIES AND THE LARGE-SCALE STRUCTURE OF THE UNIVERSE A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics by Ra´ul Fern´andez Cobos Abbreviations used in the text ACT Atacama Cosmology Telescope AGN Active galactic nuclei AME Anomalous microwave emission APOGEE Apache Point Observatory Galactic Evolution Experiment BAO Baryon acoustic oscillations BICEP Background Imaging of Cosmic Extragalactic Polarization BipoSH Bipolar Spherical Harmonic BOOMERanG Balloon Observations Of Millimetric Extragalactic Radiation ANd Geophysics BOSS Baryon Oscillation Spectroscopic Survey CAPMAP Cosmic Anisotropy Polarization MAPer CBI Cosmic Background Imager CENSORS Combined EIS-NVSS Survey Of Radio Sources CfA Center for Astrophysics CL Confidence level CMB Cosmic microwave background COBE COsmic Background Explorer COSMOSOMAS COSMOlogical Structures On Medium Angular Scales CPL Chevallier-Polarski-Linder CS Cold Spot C-BASS C-Band All Sky Survey DA Differencing Assembly DASI Degree Angular Scale Interferometer DES Dark Energy Survey DMR Differential Microwave Radiometer EBEX E and B EXperiment EIS ESOImagingSurvey ESA European Space Agency ESO European Southern Observatory FIRAS Far-InfraRed Absolute Spectrophotometer FLRW Friedmann-Lemaˆıtre-Robertson-Walker XI FWHM Full width at half maximum GUT Grand Unification Theories HEALPix Hierarchical Equal Area isoLatitude Pixelization HEAO High Energy Astronomy Observatory HFI High-Frequency Instrument HST Hubble Space Telescope HW HEALPix wavelet IAU International Astronomical Union ICA Independent component analysis ILC Internal linear combination ISW Integrated Sachs-Wolfe J-PAS Javalambre-Physics of the Accelerated Universe Astrophysi- cal Survey LAMBDA Legacy Archive for Microwave Background Data Analysis LCRS LasCampanasRedshiftSurvey LFI Low-Frequency Instrument LSS Large-scale structure MARVELS Multi-object Apache Point Observatory Radial Velocity Ex- oplanet Large-area Survey MCMC Markov chain Monte Carlo MEM Maximum Entropy Method MITC Multi-resolution Internal Template Cleaning NILC Needlet-based Internal Linear Combination NRAO National Radio Astronomy Observatory NVSS NRAO VLA Sky Survey N-pdf N-point probability density function QUaD QUEST at DASI QUEST Q and U Extragalactic Sub-mm Telescope QUIET Q/UImagingExperimenT QUIJOTE Q-U-I JOint TEnerife RFCM Radiaci´on de fondo c´osmico de microondas SDSS Sloan Digital Sky Survey SEGUE Sloan Extension for Galactic Understanding and Exploration SEVEM Spectral estimation via Expectation-Maximization SMHW Spherical Mexican Hat wavelet XII SMICA Spectral matching of independent component analysis SPT South Pole Telescope SZ Sunyaev-Zel’dovich VLA Very Large Array WISE Wide-field Infrared Survey Explorer WMAP Wilkinson Microwave Anisotropy Probe 2dFGS Two-degree-Field Galaxy Survey 2MASS Two Micron All Sky Survey 6dFGS Six-degree-Field Galaxy Survey ΛCDM Lambda Cold Dark Matter XIII Prologue Both the cosmic microwave background (CMB) observations and the galaxy sur- veys have confirmed the main outlines of the standard cosmological model with an un- precedented accuracy. In light of the recent results from the European Space Agency (ESA) Planck satellite (Planck Collaboration I, 2013), the observed universe seems to be well described by the main outlines of this scenario. The six-parameter ΛCDM model, with a spatially-flat geometry and a power-law spectrum of adiabatic scalar perturbations, has passed the test with the most precise cosmological data measured so far. However, there are still several open issues which should be explored in greater depth, because they could hide the key to new and exciting discoveries. On the one hand, the values of some of the cosmological parameters of the model estimated by using CMB data seem to be in tension with some measurements provided by other as- trophysical data sets. For instance, the low value of the Hubble constant found by the Planck Collaboration could be deviated from the estimations obtained with Hubble Space Telescope (HST) observations of Cepheid variables or galaxy clusters traced by the Sunyaev-Zel’dovich effect and X-ray measurements (see Planck Collaboration XVI, 2013, and references therein). The value of the root mean square of the matter fluc- −1 tuations in 8 h Mpc spheres at the present time in linear theory, σ8, obtained from observations of galaxy clusters is also shifted around 3σ with respect to the estimation supplied by the Planck Collaboration. On the other hand, along with a deficit of low-ℓ power, a series of large-scale anomalies in the distribution of the CMB temperature anisotropies, first detected by WMAP, have been confirmed with a high confidence level (Planck Collaboration XXIII, 2013).
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