Advanced Statistical Methods for Astrophysical Probes of by Marisa Cristina March

By Marisa Cristina March

This thesis explores complicated Bayesian statistical equipment for extracting key info for cosmological version choice, parameter inference and forecasting from astrophysical observations. Bayesian version choice offers a degree of ways 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 carry an absolute instead of a relative degree of the way strong a version is. Supernovae style Ia have been the 1st astrophysical observations to point the past due time acceleration of the Universe - this paintings offers an in depth Bayesian Hierarchical version to deduce the cosmological parameters (in specific darkish strength) from observations of those supernovae kind Ia.

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5 Angular diameter distance, d A : a distant extended object of physical length, l, subtends an angle θ on the sky. Physical dimensions are shown in red; comoving distances and coordinates are shown in black; θ is the same in both comoving and physical dimensions The main problems which inflation sought to solve were the so-called flatness and horizon problems. The distribution of the photons released at recombination and observed today initially by Penzias and Wilson and later by space borne instruments such as COBE and WMAP, was seen to be inhomogeneous on small scales, but statistically homogeneous on large scales, θ 1◦ .

Although the scalar field model places a lower bound on w > −1, values for w below this are not ruled out observationally. Models which allow w < −1 are known as Phantom dark energy models, and they require more unorthodox Lagrangians, see for example [12, 13]. Once we have relaxed the condition that w(z) = −1, there is no special reason to constrain w(z) to be a fixed number, but it is also not clear what form w(z) should take. Several simple empirical parametrizations have been suggested for investigating a redshift dependent dark energy equation of state, the most common of these is the Chevalier-Polarski-Linder (CPL) formalism [14, 15].

The photon’s wavelength has been shifted towards the red end of the spectrum. 45) It is also useful to have an expression for the comoving distance from the observer out to the distant emitter, labeled χ (ae ) in Fig. 3. This comoving distance can be obtained from Eq. 41), but instead of integrating from the beginning of time to the present day, the limits need to be changed to find the the conformal time between the time of emission of the light pulse, te , z and time of its observation t0 , z = 0.

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