The mass-density field as extracted from peculiar velocities in our cosmological neighborhood is mapped back in time to the cosmic microwave background (CMB) in two ways. First, the density power spectrum (Pk) is translated into a temperature angular power spectrum of subdegree resolution (Cl) 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 catalog of peculiar velocities have constrained the range of parameters for Pk within the family of COBE-normalized cold dark matter (CDM) models, favoring a slight tilt in the initial spectrum, n < 1. The corresponding range of Cl is plotted against current observations, indicating that the CMB data can tighten the constraints further: only models with small tilt (n ∼ 0.9) and high baryonic content (Ωb ∼ 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 convovled 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 100 h-1 Mpc sphere corresponds to 90′-30′ at the CMB for Q 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.
|Number of pages||9|
|Issue number||2 PART I|
|State||Published - 1997|
- Cosmic microwave background
- Cosmology: observations dark matter
- Cosmology: theory
- Large-scale structure of universe