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Introduction

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Dark Energy and the Formation of the Large Scale Structure of the Universe

Part of the book series: Springer Theses ((Springer Theses))

Abstract

I feel particularly lucky to have been working on my Ph.D. at such an exciting time for cosmology. With the fantastic results of the Planck mission [1], our picture of the Universe and its history has become much clearer.

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Notes

  1. 1.

    A brief introduction to the theory of inflation will be presented in Sect. 4.1.

  2. 2.

    In the rest of this thesis, unless specified, we take \(c=1\).

  3. 3.

    This results from the invariance of the matter action under coordinate transformations, as we will see later in Sect. 2.5.3.

  4. 4.

    1 parsec (pc)\(=3.1 \times 10^{16} \text {m}=3.3\) lightyears (ly).

  5. 5.

    Note that by definition of a cosmological constant, it does not have perturbations: \(\delta _\Lambda =0\).

  6. 6.

    According to Planck [22], CDM represents \(\sim {85}\,\%\) of the matter content.

  7. 7.

    This assumes the validity of the equivalence principle. This is no longer true otherwise, see [36, 37].

  8. 8.

    For simplicity, I will assume a flat spatial metric.

  9. 9.

    I am thankful to Emmanuel Schaan for a great explanation of CMB lensing.

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  1. Jet Propulsion Laboratory, Pasadena, CA, USA

    Jérôme Gleyzes

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Gleyzes, J. (2016). Introduction. In: Dark Energy and the Formation of the Large Scale Structure of the Universe. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-41210-8_1

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