The cosmological bulk flow in QCDM model: (In)consistency with $\Lambda CDM$

Abstract

We study the bulk flow of the local universe using Type Ia supernova data by considering a class of cosmological model which is spatially flat,(FRW) space-times and contains cold dark matter and $Q$ component (QCDM models) of the fluid as a scalar field, with self interactions determined by a potential $V(Q)=V_{0}Exp(-\lambda Q)$ evolving in Universe. We use different cumulative redshift slices of the Union 2 catalogue. A maximum-likelihood analysis of peculiar velocities confirms that at low redshift $0.015<z<0.1$, bulk flow is moving towards the $(l;b)=(302^o\pm 20^o;3^o\pm 10^o)$ direction with $v_{bulk}=240\pm 25km{s}^{-1}$ velocity. This direction is aligned with direction of (SSC) and agreement with a number previous studies at $(1-\sigma )$, however for high redshift $0.1<z<0.2$, we get $v_{bulk}=1000\pm 25km{s}^{-1}$ towards the $(l;b)=(254_{-14^o}^{+16^o};6_{-10^o}^{+7^o})$. This indicates that for low redshift our results are approximately consistent with the $\Lambda CDM$ model with the latest WMAP best fit cosmological parameters however for high redshift they are in disagreement of $\Lambda CDM$ and support the results of previous studies such as Kashlinsky et. al, which report the large bulk flow for the Universe. We can conclude that, in $QCDM$ model, at small scales, fluctuations of the dark energy are damped and do not enter in the evolution equation for the perturbations in the pressureless matter, while at very large scales $(\sim >100h^{-1}Mpc)$, they leaving an imprint on the microwave background anisotropy.

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