Spatial Periodicity of Galaxy Number Counts, CMB Anisotropy, and SNIa Hubble Diagram Based on the Universe Accompanied by a Non-Minimally Coupled Scalar Field

TL;DR

This paper presents a cosmological model with a non-minimally coupled scalar field that explains galaxy distribution periodicity, CMB anisotropy, and supernova observations, introducing a novel potential form to control scalar field evolution.

Contribution

The paper introduces a new scalar field potential that enables a cosmological model to simultaneously fit galaxy periodicity, CMB anisotropy, and supernova data.

Findings

Model reproduces galaxy N-z relation picket-fence structure.

Model matches CMB temperature anisotropy observations.

Model aligns with Type Ia supernova Hubble diagram.

Abstract

We have succeeded in establishing a cosmological model with a non-minimally coupled scalar field $\phi$ that can account not only for the spatial periodicity or the {\it picket-fence structure} exhibited by the galaxy $N$-$z$ relation of the 2dF survey but also for the spatial power spectrum of the cosmic microwave background radiation (CMB) temperature anisotropy observed by the WMAP satellite. The Hubble diagram of our model also compares well with the observation of Type Ia supernovae. The scalar field of our model universe starts from an extremely small value at around the nucleosynthesis epoch, remains in that state for sufficiently long periods, allowing sufficient time for the CMB temperature anisotropy to form, and then starts to grow in magnitude at the redshift $z$ of $\sim 1$, followed by a damping oscillation which is required to reproduce the observed picket-fence structure of the $N$-$z$ relation. To realize such behavior of the scalar field, we have found it necessary to introduce a new form of potential $V(\phi)\propto \phi^2\exp(-q\phi^2)$, with $q$ being a constant. Through this parameter $q$, we can control the epoch at which the scalar field starts growing.