Toward a Measurement of the Transverse Peculiar Velocity of Galaxy Pairs

TL;DR

This paper uses galaxy pair proper motions to measure transverse peculiar velocities, providing a model-independent way to test large-scale structure and cosmological parameters, with future Gaia data expected to enhance these measurements.

Contribution

It introduces a method to constrain transverse peculiar velocities using proper motions without relying on precise distance measurements, advancing cosmological tests.

Findings

Placed limits on galaxy pair proper motions at < 1500 Mpc

Confirmed large-scale expansion consistent with Hubble flow

Predicted Gaia will detect mass distribution on < 25 Mpc scales

Abstract

The transverse peculiar velocities caused by the mass distribution of large-scale structure provide a test of the theoretical matter power spectrum and the cosmological parameters that contribute to its shape. Typically, the matter density distribution of the nearby Universe is measured through redshift or line-of-sight peculiar velocity surveys. However, both methods require model-dependent distance measures to place the galaxies or to differentiate peculiar velocity from the Hubble expansion. In this paper, we use the correlated proper motions of galaxy pairs from the VLBA Extragalactic Proper Motion Catalog to place limits on the transverse peculiar velocity of galaxy pairs with comoving separations <1500 Mpc without a reliance on precise distance measurements. The relative proper motions of galaxy pairs across the line of sight can be directly translated into relative peculiar velocities because no proper motion will occur in a homogeneous expansion. We place a 3 sigma limit on the relative proper motion of pairs with comoving separations < 100 Mpc of -17.4 microas/yr < thetadot / sin theta < 19.8 microas/yr. We also confirm that large-separation objects (> 200 Mpc) are consistent with pure Hubble expansion to within ~ 5.3 microas/yr (1 sigma). Finally, we predict that Gaia end-of-mission proper motions will be able to significantly detect the mass distribution of large-scale structure on length scales < 25 Mpc. This future detection will allow a test of the shape of the theoretical mass power spectrum without a reliance on precise distance measurements.