Sensitivity of present and future detectors across the black-hole binary gravitational wave spectrum

TL;DR

This paper introduces gwent, a versatile tool for modeling the sensitivities of current and future gravitational wave detectors across the entire spectrum of black-hole binary signals, aiding in detector design and analysis.

Contribution

The paper presents gwent, a comprehensive framework for modeling detector sensitivities and black-hole binary signals across all mass scales and detector types, with adaptable and extendable features.

Findings

Sensitivity curves for PTAs, space-based, and ground-based detectors generated.

Framework can model signals from black-hole binaries with varying parameters.

Tool helps optimize detector design and signal detection strategies.

Abstract

Black-holes are known to span at least 9 orders of magnitude in mass: from the stellar-mass objects observed by the Laser Interferometer Gravitational-Wave Observatory Scientific Collaboration and Virgo Collaboration, to supermassive black-holes like the one observed by the Event Horizon Telescope at the heart of M87. Regardless of the mass scale, all of these objects are expected to form binaries and eventually emit observable gravitational radiation, with more massive objects emitting at ever lower gravitational-wave frequencies. We present the tool, gwent, for modelling the sensitivities of current and future generations of gravitational wave detectors across the entire gravitational-wave spectrum of coalescing black-hole binaries. We provide methods to generate sensitivity curves for pulsar timing arrays (PTAs) using a novel realistic PTA sensitivity curve generator, space-based interferometers using adaptive models that can represent a wide range of proposed detector designs, and ground-based interferometers using realistic noise models that can reproduce current, second, and third generation designs, as well as novel variations of the essential design parameters. To model the signal from black-hole binaries at any mass scale, we use phenomenological waveforms capable of modelling the inspiral, merger, and ringdown for sources with varying mass ratios and spins. Using this adaptable framework, we produce signal-to-noise ratios for the combination of any modelled parameter, associated with either the detector or the source. By allowing variation across each detector and source parameter, we can pinpoint the most important factors to determining the optimal performance for particular instrument designs. The adaptability of our detector and signal models can easily be extended to new detector designs and other models of gravitational wave signals.