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| Natura: | Preprint |
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2019
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| Accesso online: | https://arxiv.org/abs/1911.09745 |
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| _version_ | 1866913712839852032 |
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| author | Mingarelli, Chiara M. F. Taylor, Stephen R. Sathyaprakash, B. S. Farr, Will M. |
| author_facet | Mingarelli, Chiara M. F. Taylor, Stephen R. Sathyaprakash, B. S. Farr, Will M. |
| contents | In this paper we provide a comprehensive derivation of the energy density in the stochastic gravitational-wave background $Ω_\mathrm{gw}(f)$, and show how this quantity is measured in ground-based detectors such as Laser Interferometer Gravitational-Wave Observatory (LIGO), space-based Laser Interferometer Space Antenna (LISA), and Pulsar Timing Arrays. By definition $Ω_\mathrm{gw}(f) \propto S_h(f)$ -- the power spectral density (PSD) of the Fourier modes of the gravitational-wave background. However, this is often confused with the PSD of the strain signal, which we call $S_\mathrm{gw}(f)$, and is a detector-dependent quantity. This has led to confusing definitions of $Ω_\mathrm{gw}(f)$ in the literature which differ by factors of up to 5 when written in a detector-dependent way. In addition to clarifying this confusion, formulas presented in this paper facilitate easy comparison of results from different detector groups, and how to convert from one measure of the strength of the background (or an upper limit) to another. Our codes are public and on GitHub. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_1911_09745 |
| institution | arXiv |
| publishDate | 2019 |
| record_format | arxiv |
| spellingShingle | Understanding $Ω_\mathrm{gw}(f)$ in Gravitational Wave Experiments Mingarelli, Chiara M. F. Taylor, Stephen R. Sathyaprakash, B. S. Farr, Will M. General Relativity and Quantum Cosmology Cosmology and Nongalactic Astrophysics In this paper we provide a comprehensive derivation of the energy density in the stochastic gravitational-wave background $Ω_\mathrm{gw}(f)$, and show how this quantity is measured in ground-based detectors such as Laser Interferometer Gravitational-Wave Observatory (LIGO), space-based Laser Interferometer Space Antenna (LISA), and Pulsar Timing Arrays. By definition $Ω_\mathrm{gw}(f) \propto S_h(f)$ -- the power spectral density (PSD) of the Fourier modes of the gravitational-wave background. However, this is often confused with the PSD of the strain signal, which we call $S_\mathrm{gw}(f)$, and is a detector-dependent quantity. This has led to confusing definitions of $Ω_\mathrm{gw}(f)$ in the literature which differ by factors of up to 5 when written in a detector-dependent way. In addition to clarifying this confusion, formulas presented in this paper facilitate easy comparison of results from different detector groups, and how to convert from one measure of the strength of the background (or an upper limit) to another. Our codes are public and on GitHub. |
| title | Understanding $Ω_\mathrm{gw}(f)$ in Gravitational Wave Experiments |
| topic | General Relativity and Quantum Cosmology Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/1911.09745 |