By Marisa Cristina March
This thesis explores complicated Bayesian statistical equipment for extracting key details for cosmological version choice, parameter inference and forecasting from astrophysical observations. Bayesian version choice offers a degree of the way reliable types in a suite are relative to one another - yet what if the easiest version is lacking and never integrated within the set? Bayesian Doubt is an strategy which addresses this challenge and seeks to convey an absolute instead of a relative degree of ways strong a version is. Supernovae style Ia have been the 1st astrophysical observations to point the overdue time acceleration of the Universe - this paintings provides a close Bayesian Hierarchical version to deduce the cosmological parameters (in specific darkish power) from observations of those supernovae variety Ia.
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Additional info for Advanced Statistical Methods for Astrophysical Probes of Cosmology
Peacock, J. , White, S. D. , Frenk, C. , Pearce, F. , Thomas, P. , and Couchman, H. M. : 2003, MNRAS 341, 1311 27. Blake, C. : 2003, ApJ 594, 665 28. Eisenstein, D. , Hogg, D. , Blanton, M. , Nichol, R. , Anderson, S. , Castander, F. , Frieman, J. , Gunn, J. , Hendry, J. , Knapp, G. , Lupton, R. , Mckay, T. , Munn, J. , Richmond, M. , Schneider, D. , Strauss, M. , Szalay, A. , Tucker, D. , and York, D. : 2005, ApJ 633, 560 Chapter 3 Dark Energy and Apparent Late Time Acceleration Astrophysical observations suggest that the expansion of the Universe is accelerating.
The idea is to use the spacing of these acoustic peaks as a ‘standard ruler’ for probing the expansion history of the universe Eq. 89), in order to obtain the photon distribution at the time of recombination (η ). However, there is also an analytic approach, aspects of which we will briefly highlight here as it gives a physical insight into the physics of the early universe, and the resulting spacing of the CMB peaks. Hu and Sugiyama  developed an analytical method for obtaining the photon density and velocity distribution: From Eq.
The location of the peaks of the baryon acoustic oscillations in the matter power spectrum are directly related to the size of the sound horizon at recombination. 110) where A is an amplitude fitting parameter and Pref is a smooth reference power spectrum with no baryons. Crucially, k A is given by k A = 2π rs where rs is the sound horizon at recombination given by Eq. 96). The idea is that the co-moving separation of the acoustic peaks or acoustic oscillations in Fourier space act as a cosmological standard ruler.
Advanced Statistical Methods for Astrophysical Probes of Cosmology by Marisa Cristina March