PIRSA:12010134 Scientific Series Cosmology

DOI10.48660/12010134

Series: Cosmology and Gravitation

Ma, Y. (2012). Cosmology on Large and Small Cosmic Scales. Perimeter Institute. https://pirsa.org/12010134

Ma, Yin-Zhe. Cosmology on Large and Small Cosmic Scales. Perimeter Institute, Jan. 31, 2012, https://pirsa.org/12010134 

@misc{ pirsa_PIRSA:12010134,
  doi = {10.48660/12010134},
  url = {https://pirsa.org/12010134},
  author = {Ma, Yin-Zhe},
  keywords = {Cosmology},
  language = {en},
  title = {Cosmology on Large and Small Cosmic Scales},
  publisher = {Perimeter Institute},
  year = {2012},
  month = {jan},
  note = {PIRSA:12010134 see, \url{https://pirsa.org}}
}

Abstract

In this talk, I am going to test the concordance cosmology in three different cosmic scales. (1) On the super-horizon scale, “Copi etal. (2009)” have been arguing that the lack of large angular correlations of the CMB temperature field provides strong evidence against the standard, statistically isotropic, LCDM cosmology. I am going to argue that the “ad-hoc” discrepancy is due to the sub-optimal estimator of the low-l multipoles, and a posteriori statistics, which exaggerates the statistical significance. (2) LCDM model also predict the existence of primordial gravitational wave, for which B-mode polarization will be a powerful tool to distinguish different models of the early Universe; (3) On Galactic scales, “Watkins et al. (2008)” shows that the very large bulk flow prefers a very large density fluctuation, which seems to contradict to the LCDM model. We provide a physical explanation for this big bulk flow, based on the assumption that CMB frame does not coincide with matter rest frame, resulting in the tilted Universe. We show that the ‘tilted Universe’ could well explain the bulk flow phenomena and more importantly, the constraints for this tilted Universe can lead to the constraint on the number of e-folds of inflation; (4) In addition, cosmic Mach Number from peculiar velocity catalog may provide a powerful test of the growth of the structure.

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