Anomalous anisotropic cross-correlations between WMAP CMB maps and SDSS galaxy distribution and implications on the dark flow scenario

TL;DR

This study investigates the potential dark flow signal in CMB-galaxy cross correlations, finding anisotropic components but no conclusive evidence for dark flow, suggesting alternative explanations or very high velocities.

Contribution

First attempt to search for dark flow via weighted CMB-galaxy cross correlation, revealing anisotropic signals inconsistent with dark flow expectations.

Findings

Detected statistically anisotropic components in CMB-galaxy correlation.

Observed directional dependence deviates from dark flow model predictions.

If caused by dark flow, the implied velocity exceeds 6000 km/s.

Abstract

We search for the dark flow induced diffuse kinetic Sunyaev Zel'dovich (kSZ) effect through CMB-galaxy cross correlation. Such angular correlation is anisotropic, with a unique $cos(theta_DF)$ angular dependence and hence can be distinguished from other components. Here, $theta_DF$ is the angle between the opposite dark flow direction and the direction of the sky where the correlation is measured. We analyze the KIAS-VAGC galaxy catalog of SDSS-DR7 and the WMAP seven-year temperature maps, applying an unbiased optimal weighting scheme to eliminate any statistically isotropic components and to enhance the dark flow detection signal. Non-zero weighted cross correlations are detected at 3.5 sigma for the redshift bin z<0.1 and at 3 sigma for the bin 0.1<z<0.2, implying the existence of statistically anisotropic components in CMB. However, further analysis does not support the dark flow explanation. The observed directional dependence deviates from the $\propto cos(theta_DF)$ relation expected, and hence can not be explained by the presence of a single dark flow, and if the observed cross correlation is generated by the dark flow induced kSZ effect, the velocity would be too high (> 6000 km/s). We report this work as the first attempt to search for dark flow through weighted CMB-galaxy cross correlation and to draw the attention on the sources of the detected anomalous CMB-galaxy cross correlation.