Measuring the Hubble constant: Gravitational wave observations meet galaxy clustering

TL;DR

This paper proposes a novel method to measure the Hubble constant by correlating gravitational wave binary black hole distances with galaxy clustering data, achieving around 8% accuracy with current detectors and better with future ones.

Contribution

The authors introduce a new approach combining gravitational wave data and galaxy catalogs to estimate $H_0$ without electromagnetic counterparts, improving measurement precision.

Findings

Current detectors can measure $H_0$ to about 8% accuracy with 25 binaries.

Third-generation detectors like ET can constrain $H_0$ to about 7% with 25 observations.

Method also applicable to estimate other cosmological parameters.

Abstract

We show how the distances to binary black holes measured in gravitational wave observations with ground-based interferometers can be used to constrain the redshift-distance relation and, thereby, measure the Hubble constant ($H_0$). Gravitational wave observations of stellar-mass binary black holes are not expected to be accompanied by any electro-magnetic event that may help in accessing their redshifts. We address this deficiency by using an optical catalog to get the distribution of galaxies in redshift. Assuming that the clustering of the binaries is correlated with that of the galaxies, we propose using that correlation to measure $H_0$. We show that employing this method on simulated data obtained for second-generation networks comprising at least three detectors, e.g., advanced LIGO - advanced VIRGO network, one can measure $H_0$ with an accuracy of $\sim$8% with detection of a reference population of 25 binaries, each with black holes of mass 10$M_\odot$. As expected, with third-generation detectors like the Einstein telescope (ET), which will measure distances much more accurately and to greater depths, one can obtain better estimates for $H_0$. Specifically, we show that with 25 observations, ET can constrain $H_0$ to an accuracy of $\sim$7%. This method can also be used to estimate other cosmological parameters like the matter density $\Omega_m$ and the dark energy equation of state.