Comparing advanced-era interferometric gravitational-wave detector network configurations: sky localization and source properties

TL;DR

This paper evaluates how adding detectors like Virgo and KAGRA to the gravitational-wave network improves sky localization and source parameter estimation, highlighting significant gains with increased sensitivity and network expansion.

Contribution

It provides a comprehensive Bayesian analysis of advanced detector network configurations, quantifying improvements in localization and parameter estimation for gravitational-wave sources.

Findings

Adding Virgo reduces sky-area by up to 95% at 40 Mpc.

KAGRA improves constraints starting from 10 Mpc.

Existing 20 Hz thresholds are sufficient for current sensitivity.

Abstract

The expansion and upgrade of the global network of ground-based gravitational wave detectors promises to improve our capacity to infer the sky-localization of transient sources, enabling more effective multi-messenger follow-ups. At the same time, the increase in the signal-to-noise ratio of detected events allows for more precise estimates of the source parameters. This study aims to assess the performance of advanced-era networks of ground-based detectors, focusing on the Hanford, Livingston, Virgo, and KAGRA instruments. We use full Bayesian parameter estimation procedures to predict the scientific potential of a network. Assuming a fixed LIGO configuration, we find that the addition of the Virgo detector is beneficial to the sky localization starting from a binary neutron star horizon distance of 20 Mpc and improves significantly from 40 Mpc onwards for both a single and double LIGO detector network, reducing the inferred mean sky-area by up to 95%. Similarly, the KAGRA detector tightens the constraints, starting from a sensitivity range of 10 Mpc. Looking at highly-spinning binary black holes, we find significant improvements with increasing sensitivity in constraining the intrinsic source parameters when adding Virgo to the two LIGO detectors. Finally, we also examine the impact of the low-frequency cut-off data on the signal-to-noise ratio. We find that existing 20 Hz thresholds are sufficient and propose a metric to monitor this to study detector performance. Our findings quantify how future enhancements in detector sensitivity and network configurations will improve the localization of gravitational wave sources and allow for more precise identification of their intrinsic properties.