Inhomogeneities in the Microwave Background Radiation Interpreted within the Framework of the Quasi–Steady State Cosmology

Abstract

We calculate the expected angular power spectrum of the temperature fluctuations in the microwave background radiation (MBR) generated in the quasi-steady state cosmology (QSSC). The paper begins with a brief description of how the background is produced and thermalized in the QSSC. We then discuss within the framework of a simple model, the likely sources of fluctuations in the background due to astrophysical and cosmological causes. Power spectrum peaks at l ≈ 6 − 10, 180 − 220 and 600 − 900 are shown to be related in this cosmology respectively to curvature effects at the last minimum of the scale factor, clusters and groups of galaxies. The effect of clusters is shown to be related to their distribution in space as indicated by a toy model of structure formation in the QSSC. We derive and parameterize the angular power spectrum using six parameters related to the sources of temperature fluctuations at three characteristic scales. We are able to obtain a satisfactory fit to the observational band power estimates of MBR temperature fluctuation spectrum. Moreover, the values of 'best fit' parameters are consistent with the range of expected values.

Interpretations of the Accelerating Universe

“…In a separate paper (Narlikar et al 2002) devoted to the spectrum and fluctuations of the microwave background radiation (MBR) in the QSSC, we have shown that the MBR anisotropy from rich clusters can be revealed by a peak in the power spectrum around , while smaller peaks are l p 200 revealed in the range from groups of galaxies and l ∼ 600-900 perhaps weaker peaks at from individual galaxies or l տ 3000 compact groups.…”

Cosmological dynamics of a phantom field

“…In adherence to the Perfect Cosmological Principle, a creation field (C-field) was for the first time introduced [39] to reconcile with homogeneous density by creation of new matter in the voids caused by the expansion of the universe. It was further refined and reformulated in the Hoyle and Narlikar theory of gravitation [40], see Refs [41,42,43,44] for details of the C-field cosmology. The C-field appeared on the right hand side of the Einstein equation.…”

Cosmology and cosmogony in a cyclic universe

“…It has also been demonstrated that inhomogeneities on the observed scale result from the thermalized radiation from clusters, groups of galaxies etc. thermalized at the minimum of the last oscillation (Narlikar et al, 2003). By using a toy model for these sources, it has been shown that the resulting angular power spectrum has a satisfactory fit to the data compiled by Podariu et al (2001) for the band power spectrum of the CMBR temperature inhomogeneities.…”

“…This set of parameters has been used in recent papers on the QSSC (Narlikar, et al 2002(Narlikar, et al , 2003. For this model the ratio of maximum to minimum scale factor in any oscillation is around 9.6.…”

“…The resultant inhomogeneity of the CMBR thus arises from a superposition of random spots of three characteristic sizes corresponding to the three effects -the curvature effects at the last minimum of the the scale factor, clusters, and groups of galaxies. This is given by a 7 -parameter model of the angular power spectrum (for more details, see Narlikar et al, 2003):…”