Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental Noises
The DECi-hertz Interferometer Gravitational-Wave Observatory (DECIGO) is a space gravitational wave (GW) detector. DECIGO was originally designed to be sensitive enough to observe primordial GW background (PGW). However, due to the lowered upper limit of the PGW by the Planck observation, further im...
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| Format: | Article |
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MDPI AG
2022-02-01
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| Series: | Galaxies |
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| Online Access: | https://www.mdpi.com/2075-4434/10/1/25 |
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| author | Yuki Kawasaki Ryuma Shimizu Tomohiro Ishikawa Koji Nagano Shoki Iwaguchi Izumi Watanabe Bin Wu Shuichiro Yokoyama Seiji Kawamura |
| author_facet | Yuki Kawasaki Ryuma Shimizu Tomohiro Ishikawa Koji Nagano Shoki Iwaguchi Izumi Watanabe Bin Wu Shuichiro Yokoyama Seiji Kawamura |
| author_sort | Yuki Kawasaki |
| collection | DOAJ |
| description | The DECi-hertz Interferometer Gravitational-Wave Observatory (DECIGO) is a space gravitational wave (GW) detector. DECIGO was originally designed to be sensitive enough to observe primordial GW background (PGW). However, due to the lowered upper limit of the PGW by the Planck observation, further improvement of the target sensitivity of DECIGO is required. In the previous studies, DECIGO’s parameters were optimized to maximize the signal-to-noise ratio (SNR) of the PGW to quantum noise including the effect of diffraction loss. To simulate the SNR more realistically, we optimize DECIGO’s parameters considering the GWs from double white dwarfs (DWDs) and the thermal noise of test masses. We consider two cases of the cutoff frequency of GWs from DWDs. In addition, we consider two kinds of thermal noise: thermal noise in a residual gas and internal thermal noise. To investigate how the mirror geometry affects the sensitivity, we calculate it by changing the mirror mass, keeping the mirror thickness, and vice versa. As a result, we obtained the optimums for the parameters that maximize the SNR that depends on the mirror radius. This result shows that a thick mirror with a large radius gives a good SNR and enables us to optimize the design of DECIGO based on the feasibility study of the mirror size in the future. |
| first_indexed | 2024-03-09T21:55:11Z |
| format | Article |
| id | doaj.art-ddb840046df0448db30eb13186b2aae7 |
| institution | Directory Open Access Journal |
| issn | 2075-4434 |
| language | English |
| last_indexed | 2024-03-09T21:55:11Z |
| publishDate | 2022-02-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Galaxies |
| spelling | doaj.art-ddb840046df0448db30eb13186b2aae72023-11-23T20:00:33ZengMDPI AGGalaxies2075-44342022-02-011012510.3390/galaxies10010025Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental NoisesYuki Kawasaki0Ryuma Shimizu1Tomohiro Ishikawa2Koji Nagano3Shoki Iwaguchi4Izumi Watanabe5Bin Wu6Shuichiro Yokoyama7Seiji Kawamura8Department of Physics, Nagoya University, Nagoya 464-8602, JapanDepartment of Physics, Nagoya University, Nagoya 464-8602, JapanDepartment of Physics, Nagoya University, Nagoya 464-8602, JapanInstitute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara 252-5210, JapanDepartment of Physics, Nagoya University, Nagoya 464-8602, JapanDepartment of Physics, Nagoya University, Nagoya 464-8602, JapanDepartment of Physics, Nagoya University, Nagoya 464-8602, JapanThe Kobayashi-Masukawa Institute for the Origin of Particles and the Universe, Nagoya University, Nagoya 464-8602, JapanDepartment of Physics, Nagoya University, Nagoya 464-8602, JapanThe DECi-hertz Interferometer Gravitational-Wave Observatory (DECIGO) is a space gravitational wave (GW) detector. DECIGO was originally designed to be sensitive enough to observe primordial GW background (PGW). However, due to the lowered upper limit of the PGW by the Planck observation, further improvement of the target sensitivity of DECIGO is required. In the previous studies, DECIGO’s parameters were optimized to maximize the signal-to-noise ratio (SNR) of the PGW to quantum noise including the effect of diffraction loss. To simulate the SNR more realistically, we optimize DECIGO’s parameters considering the GWs from double white dwarfs (DWDs) and the thermal noise of test masses. We consider two cases of the cutoff frequency of GWs from DWDs. In addition, we consider two kinds of thermal noise: thermal noise in a residual gas and internal thermal noise. To investigate how the mirror geometry affects the sensitivity, we calculate it by changing the mirror mass, keeping the mirror thickness, and vice versa. As a result, we obtained the optimums for the parameters that maximize the SNR that depends on the mirror radius. This result shows that a thick mirror with a large radius gives a good SNR and enables us to optimize the design of DECIGO based on the feasibility study of the mirror size in the future.https://www.mdpi.com/2075-4434/10/1/25gravitational wavesDECIGOthermal noisequantum noisediffraction loss |
| spellingShingle | Yuki Kawasaki Ryuma Shimizu Tomohiro Ishikawa Koji Nagano Shoki Iwaguchi Izumi Watanabe Bin Wu Shuichiro Yokoyama Seiji Kawamura Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental Noises Galaxies gravitational waves DECIGO thermal noise quantum noise diffraction loss |
| title | Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental Noises |
| title_full | Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental Noises |
| title_fullStr | Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental Noises |
| title_full_unstemmed | Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental Noises |
| title_short | Optimization of Design Parameters for Gravitational Wave Detector DECIGO Including Fundamental Noises |
| title_sort | optimization of design parameters for gravitational wave detector decigo including fundamental noises |
| topic | gravitational waves DECIGO thermal noise quantum noise diffraction loss |
| url | https://www.mdpi.com/2075-4434/10/1/25 |
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