Three observational differences for binary black holes detections with second and third generation gravitational-wave detectors

Abstract

Advanced gravitational-wave observatories, such as LIGO and Virgo, will detect hundreds of gravitational waves emitted by binary black holes in the next few years. The collection of detected sources is expected to have certain properties. It is expected that a selection bias will exist toward higher mass systems, that most events will be oriented with their angular momentum pointing to or away from Earth, and that quiet events will be much more numerous than loud events. In this paper we show how all these assumptions are only true for existing detectors and do not have any universality. Using an network of proposed third-generation gravitational wave detectors, we show how each of these assumptions must be revised and we discuss several consequences on the characterization of the sources.

Version matching paper accepted by PRD Rapid Communications

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Cited by in corpus (2)

• Frequency-Dependent Responses in 3rd Generation Gravitational-Wave Detectors
• Host galaxy identification for binary black hole mergers with long baseline gravitational wave detectors