A new measurement of the bulk flow of X-ray luminous clusters of galaxies

TL;DR

This paper measures large-scale galaxy cluster bulk flows using WMAP data and an expanded X-ray catalog, finding consistent flow velocities up to 800 Mpc and emphasizing the importance of luminous clusters for accurate measurements.

Contribution

It introduces an improved method for measuring bulk flows via the kinematic SZ effect with a larger cluster catalog and refined error analysis, extending measurements to larger scales.

Findings

Bulk flow consistent with constant velocity up to 800 Mpc.

Higher luminosity clusters yield larger dipole signals.

Flow significance peaks around 500 Mpc.

Abstract

We present new measurements of the large-scale bulk flows of galaxy clusters based on 5-year WMAP data and a significantly expanded X-ray cluster catalogue. Our method probes the flow via measurements of the kinematic Sunyaev-Zeldovich (SZ) effect produced by the hot gas in moving clusters. It computes the dipole in the cosmic microwave background (CMB) data at cluster pixels, which preserves the SZ component while integrating down other contributions. Our improved catalog of over 1,000 clusters enables us to further investigate possible systematic effects and, thanks to a higher median cluster redshift, allows us to measure the bulk flow to larger scales. We present a corrected error treatment and demonstrate that the more X-ray luminous clusters, while fewer in number, have much larger optical depth, resulting in a higher dipole and thus a more accurate flow measurement. This results in the observed correlation of the dipole derived at the aperture of zero monopole with the monopole measured over the cluster central regions. This correlation is expected if the dipole is produced by the SZ effect and cannot be caused by unidentified systematics (or primary cosmic microwave background anisotropies). We measure that the flow is consistent with approximately constant velocity out to at least 800 Mpc. The significance of the measured signal peaks around 500 Mpc, most likely because the contribution from more distant clusters becomes progressively more diluted by the WMAP beam. We can, however, at present not rule out that these more distant clusters simply contribute less to the overall motion.