Bulk flows from galaxy luminosities: application to 2MASS redshift survey and forecast for next-generation datasets

TL;DR

This paper introduces a luminosity-based method for measuring cosmological bulk flows from large galaxy surveys, avoiding distance indicators and galaxy bias issues, and demonstrates its application to current and future datasets like 2MASS and EUCLID.

Contribution

The paper presents a novel, simple method for bulk flow measurement that is independent of distance indicators and galaxy bias, applicable to large photometric surveys.

Findings

Consistent bulk flow measurement with previous Tully-Fisher results.

Forecasts for constraining bulk flows at higher redshifts with upcoming surveys.

Potential to test dark energy and structure formation theories.

Abstract

We present a simple method for measuring cosmological bulk flows from large redshift surveys, based on the apparent dimming or brightening of galaxies due to their peculiar motion. It is aimed at estimating bulk flows of cosmological volumes containing large numbers of galaxies. Constraints on the bulk flow are obtained by minimizing systematic variations in galaxy luminosities with respect to a reference luminosity function measured from the whole survey. This method offers two advantages over more popular bulk flow estimators: it is independent of error-prone distance indicators and of the poorly-known galaxy bias. We apply the method to the 2MASS redshift survey (2MRS) to measure the local bulk flows of spherical shells centered on the Milky Way (MW). The result is consistent with that obtained by Nusser and Davis (2011) using the SFI++ catalogue of Tully-Fisher distance indicators. We also make an assessment of the ability of the method to constrain bulk flows at larger redshifts ($z=0.1-0.5$) from next generation datasets. As a case study we consider the planned EUCLID survey. Using this method we will be able to measure a bulk motion of $ \sim 200 \kms$ of $10^6$ galaxies with photometric redshifts, at the $3\sigma$ level for both $z\sim 0.15$ and $z\sim 0.5$. Thus the method will allow us to put strong constraints on dark energy models as well as alternative theories for structure formation.