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From Local Velocities to Microwave Background | | S. Zaroubi
; N. Sugiyama
; J. Silk
; Y. Hoffman
; A. Dekel
; | | Date: |
17 Oct 1996 | | Subject: | astro-ph | | Affiliation: | UCB), N. Sugiyama (Kyoto), J. Silk (UCB), Y. Hoffman (HU), and A. Dekel (UCB, HU | | Abstract: | The mass density field as extracted from peculiar velocities in our cosmological neighborhood is mapped back in time to the CMB in two ways. First, the density power spectrum ($P_k$) is translated into a temperature angular power spectrum of sub-degree resolution ($C_l$) and compared to observations. Second, the local density field is translated into a temperature map in a patch on the last-scattering surface of a distant observer. A likelihood analysis of the Mark III peculiar velocity data have constrained the range of parameters for $P_k$ within the family of COBE-normalized CDM models (Zaroubi et al 1996), favoring a slight tilt in the initial spectrum, $n<1$. The corresponding range of $C_l$’s is plotted against current observations, indicating that the CMB data can tighten the constraints further: only models with ``small’’ tilt ($nsim 0.9$) and ``high’’ baryonic content ($Omega_b sim 0.1$) could survive the two data sets simultaneously. The local mass density field that has been recovered from the velocities via a Wiener method is convolved with a Boltzmann calculation to recover $10’$ resolution temperature maps as viewed from different directions. The extent of the CMB patch and the amplitude of fluctuations depend on the choice of cosmological parameters, e.g., the local $100hmpc$ sphere corresponds to $90’$ to $30’$ at the CMB for $Omega$ between 1 and 0 respectively. The phases of the temperature map are correlated with those of the density field, contrary to the contribution of the Sachs-Wolfe effect alone. This correlation suggests the possibility of an inverse reconstruction of the underlying density field from CMB data with interesting theoretical implications. | | Source: | arXiv, astro-ph/9610132 | | Services: | Forum | Review | PDF | Favorites | |
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