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Membres permanents : H J de Vega

Collaborateurs : N G Sanchez (Observatoire de Paris), D. Boyanovsky (U Pittsburgh), C. Destri (U Milano-Bicocca), F J Cao (U C Madrid).

Les travaux de l’équipe de Cosmologie portent sur la Théorie de l’Univers Primordial Confrontée aux Observations

It is known since several years that our Universe is described by the STANDARD or concordance model of the Universe.

The Universe started 13.7 Gyr ago by an accelereted stage of expansion : the INFLATIONARY era. In this short stage ( 10^-34 sec) the universe magnified by a factor 10^28 . Two succesive stages of deccelerated expansion followed inflation : the radiation dominated and the matter dominated eras. Since 5 Gyr the Universe is dominated by dark energy.

The Standard model of the Univers provides the only consistent explanation of the broad set of precise and independent astronomical observations available today over a wide range of scales. Namely : WMAP data and previous CMB data, Light Elements Abundances, Large Scale Structures Observations Supernova Luminosity/Distance Relations (Acceleration of the Universe expansion), Gravitational Lensing Observations, Lyman alpha Forest Observations, Hubble Constant Measurements, etc.

Our universe is formed today by 72 % of dark energy, 28 % of matter (84 % of which is dark) and 0.005 % of radiation.

Our research programme includes :

• 1) The theory of Inflation as an effective field theory in the Ginsburg-Landau spirit.

• 2) Contrasting the effective theory of Inflation with observations (cosmic microwave background anisotropies and large scale structure data) using Monte Carlo Markov Chains Analysis of the data. Predictions on primordial gravitons from the theory of Inflation.

• 3) The fast-roll initial stage of inflation and the theoretical explanation of the CMB quadrupole suppression by the fast-roll inflationary stage.

• 4) Deciphering the nature of dark matter from theory and observations. Kinetic theory in cosmology : Boltzmann equations. Data from galaxies and N-body numerical simulations.

• 5) Quantum (loop) corrections in the effective theory of Inflation. Explicit calculations of one-loop corrections in terms of the cosmological observables and trace anomalies.
  
  

Recent publications :

C. Destri, H. J. de Vega, N. G. Sanchez, The CMB Quadrupole depression produced by early fast-roll inflation : MCMC analysis of WMAP and SDSS data, arXiv:0804.2387.
http://arxiv.org/abs/0804.2387

D. Boyanovsky, H. J. de Vega, N. Sanchez, Constraints on dark matter particles from theory, galaxy observations and N-body simulations. Phys. Rev. \bf D 77, 043518 (2008), arXiv:0710.5180.
http://arxiv.org/abs/0710.5180

C. Destri, H. J. de Vega, N. G. Sanchez, MCMC analysis of WMAP3 data points to broken symmetry inflaton potentials and provides a lower bound on the tensor to scalar ratio, Phys. Rev. \bf D77, 043509 (2008), astro-ph/0703417.
http://arxiv.org/abs/astro-ph/0703417

D. Boyanovsky, H. J. de Vega, C. M. Ho, N. G. Sanchez, New Inflation vs. Chaotic Inflation, Higher Degree Potentials and the Reconstruction Program in light of WMAP3, Phys. Rev. \bf D75, 123504 (2007), astro-ph/0702627.
http://arxiv.org/abs/astro-ph/070262

D. Boyanovsky, H. J. de Vega, N. Sanchez, Clarifying Inflation Models : Slow-roll as an expansion in $ 1/N_efolds $ and No Fine Tuning. Phys. Rev. \bf D 73, 023008 (2006), astro-ph/0507595.
http://arxiv.org/abs/astro-ph/0507595

D. Boyanovsky, H. J. de Vega, N. Sanchez, Quantum corrections to slow roll inflation and new scaling of superhorizon fluctuations. Nucl. Phys. \bf B 747, 25 (2006), astro-ph/0503669.
http://arxiv.org/abs/astro-ph/0503669

D. Boyanovsky, H. J. de Vega, N. Sanchez, Quantum corrections to the inflaton potential and the power spectra from superhorizon modes and trace anomalies Phys. Rev. \bf D 72, 103006 (2005), astro-ph/0507596.
http://arxiv.org/abs/astro-ph/0507596

D. Boyanovsky, H. J. de Vega, D. J. Schwarz, Phase transitions in the early and the present Universe Ann. Rev. Nucl. Part. Sci. \bf 56, 441-500, (2006), hep-ph/0602002.
http://arxiv.org/abs/hep-ph/0602002