Observational Cosmology With Semi-Relativistic Stars

TL;DR

This paper explores the potential of detecting semi-relativistic stars ejected by galaxy mergers, which could serve as new cosmological probes and indicators of black hole binary activity.

Contribution

It estimates the density of high-velocity stars in the universe and discusses their detectability and potential applications in testing fundamental physics and identifying gravitational wave sources.

Findings

Estimated the density of stars moving faster than 0.1c and 0.5c.

Proposed detection methods using upcoming telescopes.

Suggested applications in testing cosmological principles and gravitational wave astronomy.

Abstract

Galaxy mergers lead to the formation of massive black hole binaries which can accelerate background stars close to the speed of light. We estimate the comoving density of ejected stars with a peculiar velocity in excess of $0.1c$ or $0.5c$ to be $\sim 10^{10}$ and $10^5$ Gpc$^{-3}$ respectively, in the present-day Universe. Semi-relativistic giant stars will be detectable with forthcoming telescopes out to a distance of a few Mpc, where their proper motion, radial velocity, and age, can be spectroscopically measured. In difference from traditional cosmological messengers, such as photons, neutrinos, or cosmic-rays, these stars shine and so their trajectories need not be directed at the observer for them to be detected. Tracing the stars to their parent galaxies as a function of speed and age will provide a novel test of the equivalence principle and the standard cosmological parameters. Semi-relativistic stars could also flag black hole binaries as gravitational wave sources for the future eLISA observatory.