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Cosmological Probes of Light Relics – Phd Thesis of Benjamin Wallisch

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Cosmological Probes of Light Relics – Phd Thesis of Benjamin Wallisch Cosmological Probes of Light Relics Benjamin Wallisch This dissertation is submitted for the degree of Doctor of Philosophy June 2018 Cosmological Probes of Light Relics Benjamin Wallisch One of the primary targets of current and especially future cosmological observations are light thermal relics of the hot big bang. Within the Standard Model of particle physics, an important thermal relic are cosmic neutrinos, while many interesting extensions of the Standard Model predict new light particles which are even more weakly coupled to ordinary matter and therefore hard to detect in terrestrial experiments. On the other hand, these elusive particles may be produced efficiently in the early universe and their gravitational influence could be detectable in cosmological observables. In this thesis, we describe how measurements of the cosmic microwave background (CMB) and the large-scale structure (LSS) of the universe can shed new light on the properties of neutrinos and on the possible existence of other light relics. These cosmological observations are remarkably sensitive to the amount of radiation in the early universe, partly because free-streaming species such as neutrinos imprint a small phase shift in the baryon acoustic oscillations (BAO) which we study in detail in the CMB and LSS power spectra. Building on this analytic understanding, we provide further evidence for the cosmic neutrino background by independently confirming its free-streaming nature in different, currently available datasets. In particular, we propose and establish a new analysis of the BAO spectrum beyond its use as a standard ruler, resulting in the first measurement of this imprint of neutrinos in the clustering of galaxies. Future cosmological surveys, such as the next generation of CMB experiments (CMB-S4), have the potential to measure the energy density of relativistic species at the sub-percent level and will therefore be capable of probing physics beyond the Standard Model. We demonstrate how this improvement in sensitivity can indeed be achieved and present an observational target which would allow the detection of any extra light particle that has ever been in thermal equilibrium. Interestingly, even the absence of a detection would result in new insights by providing constraints on the couplings to the Standard Model. As an example, we show that existing bounds on additional scalar particles, such as axions, may be surpassed by orders of magnitude. For my parents Declaration This dissertation is the result of my own work and includes nothing which is the outcome of work done in collaboration except as declared below and specified in the text. Following the tendency of modern research in theoretical physics, most of the material discussed in this dissertation is the result of collaborative research. In particular, Chapters 4 and 6, and Appendices A, C and D are based on work done in collaboration with Daniel Baumann and Daniel Green, published in [1, 2], Chapter 5 and Appendix B are the result of the research done in collaboration with Daniel Baumann, Daniel Green and Joel Meyers, published in [3], and Chapter 7 is mostly based on the work done in collaboration with Daniel Baumann, Florian Beutler, Raphael Flauger, Daniel Green, Anže Slosar, Mariana Vargas-Magaña and Christophe Yèche, published in [4]. I have made major contributions to the above, both in terms of results and writing. All figures presented in this dissertation were produced or adapted by myself. I hereby declare that my dissertation on Cosmological Probes of Light Relics is not substantially the same as any that I have submitted or is being concurrently submitted for a degree, diploma or other qualification at the University of Cambridge, any other University or similar institution. I further state that no substantial part of my dissertation has already been submitted or is being concurrently submitted for any such degree, diploma or other qualification at the University of Cambridge, any other University or similar institution. Benjamin Wallisch June 2018 vii Acknowledgements First and foremost, I wish to express my sincere gratitude to my supervisor Daniel Baumann for his phenomenal guidance, tireless effort and unwavering support. His enthusiasm and passion for physics continue to amaze me and are truly contagious. He is a remarkable mentor with endless patience and dedication. I cannot thank him enough for all his contributions at many different levels to this work and beyond. Second, I am most grateful to Daniel Green who was my other main collaborator and has essentially become a second supervisor in a number of ways. I could always count on his help and support, and the fact that our many discussions were enlightening and insightful. His imagination, excitement and approach to physics are an inspiration. It has been a true privilege and great pleasure to work with and learn from both Daniels throughout my PhD. Thanks are also due to my other collaborators, Florian Beutler, James Fergusson, Raphael Flauger, Helge Gruetjen, Joel Meyers, Paul Shellard, Anže Slosar, Mariana Vargas-Magaña and Christophe Yèche, for their valuable input, amazing ideas and enriching discussions. Working with this great group of cosmologists has helped me to understand many different aspects of our field. Furthermore, I thank my departmental colleagues in both Cambridge and Amsterdam, especially Valentin Assassi, Matteo Biagetti, Horng Sheng Chia, Garrett Goon, Hayden Lee, Guilherme Pimentel and John Stout, for numerous conversations and providing such a friendly and stimulating environment. Special thanks go to my Cambridge officemates Chandrima Ganguly and Will Cook. I am thankful to my friends and fellow students in Heidelberg, Cambridge, Amsterdam and elsewhere for spending countless fun and enriching moments together, for their understanding when I have neglected them, and for sharing numerous adventures. Finally, I want to thank my brother. More than anyone else, I however owe my deepest gratitude to my parents for their continuous and unconditional support in so many ways. I would not be where I am now without them. ix Acknowledgements I acknowledge support by a Cambridge European Scholarship of the Cambridge Trust, by the Department of Applied Mathematics and Theoretical Physics, by a Research Studentship Award of the Cambridge Philosophical Society, from a Starting Grant of the European Research Council (ERC STG Grant 279617), by an STFC Studentship, by Trinity Hall and by a Visiting PhD Fellowship of the Delta-ITP consortium, a program of the Netherlands Organisation for Scientific Research (NWO) that is funded by the Dutch Ministry of Education, Cultureand Science (OCW). I am also grateful to the CERN theory group, the Institute for Theoretical Physics at the University of Heidelberg and, in particular, the Institute of Physics at the University of Amsterdam for their hospitality. This work uses observations obtained by the Planck satellite (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA and Canada. This research is also partly based on observations obtained by the Sloan Digital Sky Survey III (SDSS-III, http://www.sdss3.org/). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the U.S. Department of Energy Office of Science. Parts of this work were undertaken onthe COSMOS Shared Memory System at DAMTP (University of Cambridge), operated on behalf of the STFC DiRAC HPC Facility. This equipment is funded by BIS National E-Infrastructure Capital Grant ST/J005673/1 and STFC Grants ST/H008586/1, ST/K00333X/1. Some analyses also used resources of the HPC cluster Atócatl at IA-UNAM, Mexico, and of the National Energy Research Scientific Computing Center, which is supported by the Office of Science oftheU.S. Department of Energy under Contract No. DE-AC02-05CH11231. The results presented in this thesis made use of CAMB [5], CLASS [6], CosmoMC/GetDist [7], FORM [8], IPython [9], MontePython [10], and the Python packages Astropy [11], emcee [12], Matplotlib [13], nbodykit [14] and NumPy/SciPy [15]. x Contents 1 Introduction 1 2 Review of Modern Cosmology 7 2.1 Homogeneous Cosmology . 7 2.1.1 Geometry and Dynamics of the Universe . 8 2.1.2 Standard Model of Cosmology . 9 2.2 Thermal History . 11 2.2.1 Brief History of the Hot Big Bang . 12 2.2.2 In and Out of Equilibrium . 12 2.2.3 Cosmic Neutrino Background . 17 2.2.4 Cosmic Microwave Background . 18 2.3 Inhomogeneous Cosmology . 19 2.3.1 Structure Formation . 19 2.3.2 Cosmic Sound Waves . 22 2.4 Cosmological Observables . 26 2.4.1 CMB Anisotropies . 27 2.4.2 Large-Scale Structure . 34 2.4.3 Baryon Acoustic Oscillations . 37 3 Light Species in Cosmology and Particle Physics 39 3.1 The Power of Astrophysics and Cosmology . 40 3.2 Physics Beyond the Standard Model . 41 3.2.1 Standard Model of Particle Physics . 41 3.2.2 Motivations for New Physics . 42 3.2.3 Effective Field Theory of Light Species . 45 3.3 Neutrinos and Dark Radiation . 49 3.3.1 Effective Number of Relativistic Species . 49 3.3.2 Thermal History with Additional Species . 52 xi Contents 3.3.3 Current Constraints on EFT Parameters . 55 3.4 Cosmological Signatures of Light Relics . 57 3.4.1 Diffusion Damping . 57 3.4.2 Phase Shift . 59 3.4.3 Matter-Radiation Equality . 60 3.4.4 Light Element Abundances . 62 4 New Target for Cosmic Axion Searches 63 4.1 Novel Constraints on Light Relics . 64 4.2 Constraints on Axions . 65 4.2.1 Coupling to Photons . 66 4.2.2 Coupling to Gluons . 68 4.3 Constraints on Familons . 69 4.3.1 Freeze-Out . 70 4.3.2 Freeze-In . 71 4.4 Constraints on Majorons . 73 4.4.1 Freeze-Out .
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