Source Confusion from Neutron Star Binaries in Ground-Based Gravitational Wave Detectors is Minimal
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arXiv
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| Natura: | Preprint |
| Pubblicazione: |
2024
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| _version_ | 1866909164756795392 |
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| author | Johnson, Aaron D. Chatziioannou, Katerina Farr, Will M. |
| author_facet | Johnson, Aaron D. Chatziioannou, Katerina Farr, Will M. |
| contents | Upgrades beyond the current second generation of ground-based gravitational wave detectors will allow them to observe tens of thousands neutron star and black hole binaries. Given the typical minute-to-hour duration of neutron star signals in the detector frequency band, a number of them will overlap in the time-frequency plane resulting in a nonzero cross-correlation. We examine source confusion arising from overlapping signals whose time-frequency tracks cross. Adopting the median observed merger rate of $100$ Gpc$^{-3}$yr$^{-1}$, each neutron star binary signal overlaps with an average of 42(4)[0.5] other signals when observed from 2(5)[10] Hz. The vast majority of overlaps occur at low frequencies where the inspiral evolution is slow: 91% of time-frequency overlaps occur in band below 5 Hz. The combined effect of overlapping signals does not satisfy the central limit theorem and source confusion cannot be treated as stationary, Gaussian noise: on average 0.91(0.17)[0.05] signals are present in a single adaptive time-frequency bin centered at 2(5)[10] Hz. We quantify source confusion under a realistic neutron star binary population and find that parameter uncertainty typically increases by less than 1% unless there are overlapping signals whose detector-frame chirp mass difference is $\lesssim 0.01 M_{\odot}$ and the overlap frequency is $\gtrsim$ 40 Hz. Out of $1\times10^6$ simulated signals, 0.14% fall within this region of detector-frame chirp mass differences, but their overlap frequencies are typically lower than 40 Hz. Source confusion for ground-based detectors, where events overlap instantaneously is significantly milder than the equivalent LISA problem, where many classes of events overlap for the lifetime of the mission. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2402_06836 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Source Confusion from Neutron Star Binaries in Ground-Based Gravitational Wave Detectors is Minimal Johnson, Aaron D. Chatziioannou, Katerina Farr, Will M. General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena Instrumentation and Methods for Astrophysics Upgrades beyond the current second generation of ground-based gravitational wave detectors will allow them to observe tens of thousands neutron star and black hole binaries. Given the typical minute-to-hour duration of neutron star signals in the detector frequency band, a number of them will overlap in the time-frequency plane resulting in a nonzero cross-correlation. We examine source confusion arising from overlapping signals whose time-frequency tracks cross. Adopting the median observed merger rate of $100$ Gpc$^{-3}$yr$^{-1}$, each neutron star binary signal overlaps with an average of 42(4)[0.5] other signals when observed from 2(5)[10] Hz. The vast majority of overlaps occur at low frequencies where the inspiral evolution is slow: 91% of time-frequency overlaps occur in band below 5 Hz. The combined effect of overlapping signals does not satisfy the central limit theorem and source confusion cannot be treated as stationary, Gaussian noise: on average 0.91(0.17)[0.05] signals are present in a single adaptive time-frequency bin centered at 2(5)[10] Hz. We quantify source confusion under a realistic neutron star binary population and find that parameter uncertainty typically increases by less than 1% unless there are overlapping signals whose detector-frame chirp mass difference is $\lesssim 0.01 M_{\odot}$ and the overlap frequency is $\gtrsim$ 40 Hz. Out of $1\times10^6$ simulated signals, 0.14% fall within this region of detector-frame chirp mass differences, but their overlap frequencies are typically lower than 40 Hz. Source confusion for ground-based detectors, where events overlap instantaneously is significantly milder than the equivalent LISA problem, where many classes of events overlap for the lifetime of the mission. |
| title | Source Confusion from Neutron Star Binaries in Ground-Based Gravitational Wave Detectors is Minimal |
| topic | General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2402.06836 |