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| Main Authors: | , , |
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| Format: | Preprint |
| Published: |
2025
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2505.19962 |
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| _version_ | 1866909623413374976 |
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| author | Singh, Neha Bulik, Tomasz Olejak, Aleksandra |
| author_facet | Singh, Neha Bulik, Tomasz Olejak, Aleksandra |
| contents | The Einstein Telescope (ET) is a proposed third-generation, wide-band gravitational wave (GW) detector which will have an improved detection sensitivity in low frequencies, leading to a longer observation time in the detection band and higher detection rate for binary neutron stars (BNSs). Despite the fact that ET will have a higher detection rate, a large fraction of BNSs will remain undetectable. We present a scheme to estimate accurate detection efficiency and to reconstruct the true merger rate density of the population of the BNSs, as a function of redshift. We show that with ET as a single instrumnet, for a population of BNSs with $R_{mer} \sim 100 (300)$ $\rm Gpc^{-3} yr^{-1}$ at $z\sim 0(2)$, we can reconstruct the merger rate density uptil $z \sim 2$ , with a relative error of $12\%$ at ($z \sim 2$), despite the loss in detection of the bulk of the BNS population. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_19962 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Estimating the binary neutron star merger rate density evolution with Einstein Telescope Singh, Neha Bulik, Tomasz Olejak, Aleksandra High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology The Einstein Telescope (ET) is a proposed third-generation, wide-band gravitational wave (GW) detector which will have an improved detection sensitivity in low frequencies, leading to a longer observation time in the detection band and higher detection rate for binary neutron stars (BNSs). Despite the fact that ET will have a higher detection rate, a large fraction of BNSs will remain undetectable. We present a scheme to estimate accurate detection efficiency and to reconstruct the true merger rate density of the population of the BNSs, as a function of redshift. We show that with ET as a single instrumnet, for a population of BNSs with $R_{mer} \sim 100 (300)$ $\rm Gpc^{-3} yr^{-1}$ at $z\sim 0(2)$, we can reconstruct the merger rate density uptil $z \sim 2$ , with a relative error of $12\%$ at ($z \sim 2$), despite the loss in detection of the bulk of the BNS population. |
| title | Estimating the binary neutron star merger rate density evolution with Einstein Telescope |
| topic | High Energy Astrophysical Phenomena General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2505.19962 |