Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)

R X Adhikari; T Akutsu; M Ando; A Araya; N Aritomi; H Asada; Y Aso; S Bae; Y Bae; R Bajpai; S W Ballmer; K Cannon; Z Cao; E Capocasa; M Chan; C Chen; D Chen; K Chen; Y Chen; C-Y Chiang; Y-K Chu; J C Driggers; S E Dwyer; A Effler; S Eguchi; M Eisenmann; Y Enomoto; R Flaminio; H K Fong; V V Frolov; Y Fujikawa; Y Fujimoto; M Fukushima; D Gao; G-G Ge; S Ha; I P W Hadiputrawan; S Haino; W-B Han; K Hasegawa; K Hattori; H Hayakawa; K Hayama; Y Himemoto; N Hirata; C Hirose; T-C Ho; B-H Hsieh; H-F Hsieh; C Hsiung; H-Y Huang; P Huang; Y-C Huang; Y-J Huang; D C Y Hui; S Ide; B Ikenoue; K Inayoshi; Y Inoue; Y Itoh; K Izumi; C Jeon; H-B Jin; K Jung; P Jung; K Kaihotsu; T Kajita; M Kakizaki; M Kamiizumi; N Kanda; T Kato; K Kawabe; C Kim; Y-M Kim; N Kimura; Y Kobayashi; K Kohri; K Kokeyama; A K H Kong; N Koyama; C Kozakai; J Kume; Y Kuromiya; S Kuroyanagi; K Kwak; E Lee; H W Lee; R Lee; M Leonardi; K L Li; P Li; L C-C Lin; C-Y Lin; E T Lin; F-K Lin; F-L Lin; H L Lin; L-W Luo; M Ma’arif; E Majorana; Y Michimura; N Mio; O Miyakawa; K Miyo; S Miyoki; Y Mori; S Morisaki; N Morisue; Y Moriwaki; A Mullavey; K Nagano; H Nakano; Y Nakayama; T Narikawa; L Naticchioni; L Nguyen Quynh; W-T Ni; T Nishimoto; A Nishizawa; S Nozaki; Y Obayashi; Y Obuchi; W Ogaki; J J Oh; K Oh; M Ohashi; T Ohashi; M Ohkawa; H Ohta; Y Okutani; K Oohara; S Oshino; S Otabe; K-C Pan; A Parisi; J Park; F E Peña Arellano; S Saha; Y Saito; K Sakai; Y Sekiguchi; L Shao; Y Shikano; H Shimizu; R Shimizu; K Shimode; H Shinkai; T Shishido; A Shoda; K Somiya; I Song; R Sugimoto; J Suresh; H Tagoshi; H Takahashi; R Takahashi; H Takeda; M Takeda; M Tamaki; K Tanaka; S Tanioka; A Taruya; T Tomaru; T Tomura; L Trozzo; T Tsang; J-S Tsao; S Tsuchida; T Tsutsui; T Tsuzuki; D Tuyenbayev; N Uchikata; T Uchiyama; T Uehara; K Ueno; G Ueshima; F Uraguchi; T Ushiba; M H P M van Putten; J Wang; T Washimi; C Wu; H Wu; K Yamamoto; R Yamazaki; Y Yang; S-W Yeh; J Yokoyama; T Yokozawa; T Yoshioka; H Yuzurihara; S Zeidler; M Zhan; H Zhang; Y Zhao; Z-H Zhu

doi:10.1093/ptep/ptac093

Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)

R X Adhikari, T Akutsu, M Ando, A Araya, N Aritomi, H Asada, Y Aso, S Bae, Y Bae, R Bajpai, S W Ballmer, K Cannon, Z Cao, E Capocasa, M Chan, C Chen, D Chen, K Chen, Y Chen, C-Y ChiangY-K Chu, J C Driggers, S E Dwyer, A Effler, S Eguchi, M Eisenmann, Y Enomoto, R Flaminio, H K Fong, V V Frolov, Y Fujikawa, Y Fujimoto, M Fukushima, D Gao, G-G Ge, S Ha, I P W Hadiputrawan, S Haino, W-B Han, K Hasegawa, K Hattori, H Hayakawa, K Hayama, Y Himemoto, N Hirata, C Hirose, T-C Ho, B-H Hsieh, H-F Hsieh, C Hsiung, H-Y Huang, P Huang, Y-C Huang, Y-J Huang, D C Y Hui, S Ide, B Ikenoue, K Inayoshi, Y Inoue, Y Itoh, K Izumi, C Jeon, H-B Jin, K Jung, P Jung, K Kaihotsu, T Kajita, M Kakizaki, M Kamiizumi, N Kanda, T Kato, K Kawabe, C Kim, Y-M Kim, N Kimura, Y Kobayashi, K Kohri, K Kokeyama, A K H Kong, N Koyama, C Kozakai, J Kume, Y Kuromiya, S Kuroyanagi, K Kwak, E Lee, H W Lee, R Lee, M Leonardi, K L Li, P Li, L C-C Lin, C-Y Lin, E T Lin, F-K Lin, F-L Lin, H L Lin, L-W Luo, M Ma’arif, E Majorana, Y Michimura, N Mio, O Miyakawa, K Miyo, S Miyoki, Y Mori, S Morisaki, N Morisue, Y Moriwaki, A Mullavey, K Nagano, H Nakano, Y Nakayama, T Narikawa, L Naticchioni, L Nguyen Quynh, W-T Ni, T Nishimoto, A Nishizawa, S Nozaki, Y Obayashi, Y Obuchi, W Ogaki, J J Oh, K Oh, M Ohashi, T Ohashi, M Ohkawa, H Ohta, Y Okutani, K Oohara, S Oshino, S Otabe, K-C Pan, A Parisi, J Park, F E Peña Arellano, S Saha, Y Saito, K Sakai, Y Sekiguchi, L Shao, Y Shikano, H Shimizu, R Shimizu, K Shimode, H Shinkai, T Shishido, A Shoda, K Somiya, I Song, R Sugimoto, J Suresh, H Tagoshi, H Takahashi, R Takahashi, H Takeda, M Takeda, M Tamaki, K Tanaka, S Tanioka, A Taruya, T Tomaru, T Tomura, L Trozzo, T Tsang, J-S Tsao, S Tsuchida, T Tsutsui, T Tsuzuki, D Tuyenbayev, N Uchikata, T Uchiyama, T Uehara, K Ueno, G Ueshima, F Uraguchi, T Ushiba, M H P M van Putten, J Wang, T Washimi, C Wu, H Wu, K Yamamoto, R Yamazaki, Y Yang, S-W Yeh, J Yokoyama, T Yokozawa, T Yoshioka, H Yuzurihara, S Zeidler, M Zhan, H Zhang, Y Zhao, Z-H Zhu

物理学科

研究成果: ジャーナルへの寄稿 › 学術論文 › 査読

9 被引用数 (Scopus)

抄録

Abstract KAGRA, the kilometer-scale underground gravitational-wave detector, is located at Kamioka, Japan. In April 2020, an astrophysics observation was performed at the KAGRA detector in combination with the GEO 600 detector; this observation operation is called O3GK. The optical configuration in O3GK is based on a power-recycled Fabry–Pérot–Michelson interferometer; all the mirrors were set at room temperature. The duty factor of the operation was approximately 53%, and the displacement sensitivity was approximately 1 × 10−18 ${\rm m}/\sqrt{\rm {Hz } }$ at 250 Hz. The binary-neutron-star (BNS) inspiral range was about 0.6 Mpc. The contributions of various noise sources to the sensitivity of O3GK were investigated to understand how the observation range could be improved; this study is called a “noise budget”. According to our noise budget, the measured sensitivity could be approximated by adding up the effect of each noise. The sensitivity was dominated by noise from the sensors used for local controls of the vibration isolation systems, acoustic noise, shot noise, and laser frequency noise. Further, other noise sources that did not limit the sensitivity were investigated. This paper provides a detailed account of the KAGRA detector in O3GK, including interferometer configuration, status, and noise budget. In addition, strategies for future sensitivity improvements, such as hardware upgrades, are discussed.

寄稿の翻訳タイトル	Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)
本文言語	英語
論文番号	10A101
ジャーナル	Progress of Theoretical and Experimental Physics
巻	2023
号	10
DOI	https://doi.org/10.1093/ptep/ptac093
出版ステータス	出版済み - 2023/10

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10.1093/ptep/ptac093ライセンス: 指定なし

引用スタイル

Adhikari, R. X., Akutsu, T., Ando, M., Araya, A., Aritomi, N., Asada, H., Aso, Y., Bae, S., Bae, Y., Bajpai, R., Ballmer, S. W., Cannon, K., Cao, Z., Capocasa, E., Chan, M., Chen, C., Chen, D., Chen, K., Chen, Y., ... Zhu, Z.-H. (2023). Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK). Progress of Theoretical and Experimental Physics, 2023(10), 記事 10A101. https://doi.org/10.1093/ptep/ptac093

@article{31bf6ee854264a3c914843ae81e98755,

title = "Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)",

abstract = "Abstract KAGRA, the kilometer-scale underground gravitational-wave detector, is located at Kamioka, Japan. In April 2020, an astrophysics observation was performed at the KAGRA detector in combination with the GEO 600 detector; this observation operation is called O3GK. The optical configuration in O3GK is based on a power-recycled Fabry–P{\'e}rot–Michelson interferometer; all the mirrors were set at room temperature. The duty factor of the operation was approximately 53%, and the displacement sensitivity was approximately 1 × 10−18 ${\rm m}/\sqrt{\rm {Hz } }$ at 250 Hz. The binary-neutron-star (BNS) inspiral range was about 0.6 Mpc. The contributions of various noise sources to the sensitivity of O3GK were investigated to understand how the observation range could be improved; this study is called a “noise budget”. According to our noise budget, the measured sensitivity could be approximated by adding up the effect of each noise. The sensitivity was dominated by noise from the sensors used for local controls of the vibration isolation systems, acoustic noise, shot noise, and laser frequency noise. Further, other noise sources that did not limit the sensitivity were investigated. This paper provides a detailed account of the KAGRA detector in O3GK, including interferometer configuration, status, and noise budget. In addition, strategies for future sensitivity improvements, such as hardware upgrades, are discussed.",

author = "Adhikari, {R X} and T Akutsu and M Ando and A Araya and N Aritomi and H Asada and Y Aso and S Bae and Y Bae and R Bajpai and Ballmer, {S W} and K Cannon and Z Cao and E Capocasa and M Chan and C Chen and D Chen and K Chen and Y Chen and C-Y Chiang and Y-K Chu and Driggers, {J C} and Dwyer, {S E} and A Effler and S Eguchi and M Eisenmann and Y Enomoto and R Flaminio and Fong, {H K} and Frolov, {V V} and Y Fujikawa and Y Fujimoto and M Fukushima and D Gao and G-G Ge and S Ha and Hadiputrawan, {I P W} and S Haino and W-B Han and K Hasegawa and K Hattori and H Hayakawa and K Hayama and Y Himemoto and N Hirata and C Hirose and T-C Ho and B-H Hsieh and H-F Hsieh and C Hsiung and H-Y Huang and P Huang and Y-C Huang and Y-J Huang and Hui, {D C Y} and S Ide and B Ikenoue and K Inayoshi and Y Inoue and Y Itoh and K Izumi and C Jeon and H-B Jin and K Jung and P Jung and K Kaihotsu and T Kajita and M Kakizaki and M Kamiizumi and N Kanda and T Kato and K Kawabe and C Kim and Y-M Kim and N Kimura and Y Kobayashi and K Kohri and K Kokeyama and Kong, {A K H} and N Koyama and C Kozakai and J Kume and Y Kuromiya and S Kuroyanagi and K Kwak and E Lee and Lee, {H W} and R Lee and M Leonardi and Li, {K L} and P Li and Lin, {L C-C} and C-Y Lin and Lin, {E T} and F-K Lin and F-L Lin and Lin, {H L} and L-W Luo and M Ma{\textquoteright}arif and E Majorana and Y Michimura and N Mio and O Miyakawa and K Miyo and S Miyoki and Y Mori and S Morisaki and N Morisue and Y Moriwaki and A Mullavey and K Nagano and H Nakano and Y Nakayama and T Narikawa and L Naticchioni and Quynh, {L Nguyen} and W-T Ni and T Nishimoto and A Nishizawa and S Nozaki and Y Obayashi and Y Obuchi and W Ogaki and Oh, {J J} and K Oh and M Ohashi and T Ohashi and M Ohkawa and H Ohta and Y Okutani and K Oohara and S Oshino and S Otabe and K-C Pan and A Parisi and J Park and Arellano, {F E Pe{\~n}a} and S Saha and Y Saito and K Sakai and Y Sekiguchi and L Shao and Y Shikano and H Shimizu and R Shimizu and K Shimode and H Shinkai and T Shishido and A Shoda and K Somiya and I Song and R Sugimoto and J Suresh and H Tagoshi and H Takahashi and R Takahashi and H Takeda and M Takeda and M Tamaki and K Tanaka and S Tanioka and A Taruya and T Tomaru and T Tomura and L Trozzo and T Tsang and J-S Tsao and S Tsuchida and T Tsutsui and T Tsuzuki and D Tuyenbayev and N Uchikata and T Uchiyama and T Uehara and K Ueno and G Ueshima and F Uraguchi and T Ushiba and van Putten, {M H P M} and J Wang and T Washimi and C Wu and H Wu and K Yamamoto and R Yamazaki and Y Yang and S-W Yeh and J Yokoyama and T Yokozawa and T Yoshioka and H Yuzurihara and S Zeidler and M Zhan and H Zhang and Y Zhao and Z-H Zhu",

year = "2023",

month = oct,

doi = "10.1093/ptep/ptac093",

language = "英語",

volume = "2023",

journal = "Progress of Theoretical and Experimental Physics",

issn = "2050-3911",

publisher = "Oxford University Press",

number = "10",

}

Adhikari, RX, Akutsu, T, Ando, M, Araya, A, Aritomi, N, Asada, H, Aso, Y, Bae, S, Bae, Y, Bajpai, R, Ballmer, SW, Cannon, K, Cao, Z, Capocasa, E, Chan, M, Chen, C, Chen, D, Chen, K, Chen, Y, Chiang, C-Y, Chu, Y-K, Driggers, JC, Dwyer, SE, Effler, A, Eguchi, S, Eisenmann, M, Enomoto, Y, Flaminio, R, Fong, HK, Frolov, VV, Fujikawa, Y, Fujimoto, Y, Fukushima, M, Gao, D, Ge, G-G, Ha, S, Hadiputrawan, IPW, Haino, S, Han, W-B, Hasegawa, K, Hattori, K, Hayakawa, H, Hayama, K, Himemoto, Y, Hirata, N, Hirose, C, Ho, T-C, Hsieh, B-H, Hsieh, H-F, Hsiung, C, Huang, H-Y, Huang, P, Huang, Y-C, Huang, Y-J, Hui, DCY, Ide, S, Ikenoue, B, Inayoshi, K, Inoue, Y, Itoh, Y, Izumi, K, Jeon, C, Jin, H-B, Jung, K, Jung, P, Kaihotsu, K, Kajita, T, Kakizaki, M, Kamiizumi, M, Kanda, N, Kato, T, Kawabe, K, Kim, C, Kim, Y-M, Kimura, N, Kobayashi, Y, Kohri, K, Kokeyama, K, Kong, AKH, Koyama, N, Kozakai, C, Kume, J, Kuromiya, Y, Kuroyanagi, S, Kwak, K, Lee, E, Lee, HW, Lee, R, Leonardi, M, Li, KL, Li, P, Lin, LC-C, Lin, C-Y, Lin, ET, Lin, F-K, Lin, F-L, Lin, HL, Luo, L-W, Ma’arif, M, Majorana, E, Michimura, Y, Mio, N, Miyakawa, O, Miyo, K, Miyoki, S, Mori, Y, Morisaki, S, Morisue, N, Moriwaki, Y, Mullavey, A, Nagano, K, Nakano, H, Nakayama, Y, Narikawa, T, Naticchioni, L, Quynh, LN, Ni, W-T, Nishimoto, T, Nishizawa, A, Nozaki, S, Obayashi, Y, Obuchi, Y, Ogaki, W, Oh, JJ, Oh, K, Ohashi, M, Ohashi, T, Ohkawa, M, Ohta, H, Okutani, Y, Oohara, K, Oshino, S, Otabe, S, Pan, K-C, Parisi, A, Park, J, Arellano, FEP, Saha, S, Saito, Y, Sakai, K, Sekiguchi, Y, Shao, L, Shikano, Y, Shimizu, H, Shimizu, R, Shimode, K, Shinkai, H, Shishido, T, Shoda, A, Somiya, K, Song, I, Sugimoto, R, Suresh, J, Tagoshi, H, Takahashi, H, Takahashi, R, Takeda, H, Takeda, M, Tamaki, M, Tanaka, K, Tanioka, S, Taruya, A, Tomaru, T, Tomura, T, Trozzo, L, Tsang, T, Tsao, J-S, Tsuchida, S, Tsutsui, T, Tsuzuki, T, Tuyenbayev, D, Uchikata, N, Uchiyama, T, Uehara, T, Ueno, K, Ueshima, G, Uraguchi, F, Ushiba, T, van Putten, MHPM, Wang, J, Washimi, T, Wu, C, Wu, H, Yamamoto, K, Yamazaki, R, Yang, Y, Yeh, S-W, Yokoyama, J, Yokozawa, T, Yoshioka, T, Yuzurihara, H, Zeidler, S, Zhan, M, Zhang, H, Zhao, Y & Zhu, Z-H 2023, 'Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)', Progress of Theoretical and Experimental Physics, vol. 2023, no. 10, 10A101. https://doi.org/10.1093/ptep/ptac093

TY - JOUR

T1 - Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)

AU - Adhikari, R X

AU - Akutsu, T

AU - Ando, M

AU - Araya, A

AU - Aritomi, N

AU - Asada, H

AU - Aso, Y

AU - Bae, S

AU - Bae, Y

AU - Bajpai, R

AU - Ballmer, S W

AU - Cannon, K

AU - Cao, Z

AU - Capocasa, E

AU - Chan, M

AU - Chen, C

AU - Chen, D

AU - Chen, K

AU - Chen, Y

AU - Chiang, C-Y

AU - Chu, Y-K

AU - Driggers, J C

AU - Dwyer, S E

AU - Effler, A

AU - Eguchi, S

AU - Eisenmann, M

AU - Enomoto, Y

AU - Flaminio, R

AU - Fong, H K

AU - Frolov, V V

AU - Fujikawa, Y

AU - Fujimoto, Y

AU - Fukushima, M

AU - Gao, D

AU - Ge, G-G

AU - Ha, S

AU - Hadiputrawan, I P W

AU - Haino, S

AU - Han, W-B

AU - Hasegawa, K

AU - Hattori, K

AU - Hayakawa, H

AU - Hayama, K

AU - Himemoto, Y

AU - Hirata, N

AU - Hirose, C

AU - Ho, T-C

AU - Hsieh, B-H

AU - Hsieh, H-F

AU - Hsiung, C

AU - Huang, H-Y

AU - Huang, P

AU - Huang, Y-C

AU - Huang, Y-J

AU - Hui, D C Y

AU - Ide, S

AU - Ikenoue, B

AU - Inayoshi, K

AU - Inoue, Y

AU - Itoh, Y

AU - Izumi, K

AU - Jeon, C

AU - Jin, H-B

AU - Jung, K

AU - Jung, P

AU - Kaihotsu, K

AU - Kajita, T

AU - Kakizaki, M

AU - Kamiizumi, M

AU - Kanda, N

AU - Kato, T

AU - Kawabe, K

AU - Kim, C

AU - Kim, Y-M

AU - Kimura, N

AU - Kobayashi, Y

AU - Kohri, K

AU - Kokeyama, K

AU - Kong, A K H

AU - Koyama, N

AU - Kozakai, C

AU - Kume, J

AU - Kuromiya, Y

AU - Kuroyanagi, S

AU - Kwak, K

AU - Lee, E

AU - Lee, H W

AU - Lee, R

AU - Leonardi, M

AU - Li, K L

AU - Li, P

AU - Lin, L C-C

AU - Lin, C-Y

AU - Lin, E T

AU - Lin, F-K

AU - Lin, F-L

AU - Lin, H L

AU - Luo, L-W

AU - Ma’arif, M

AU - Majorana, E

AU - Michimura, Y

AU - Mio, N

AU - Miyakawa, O

AU - Miyo, K

AU - Miyoki, S

AU - Mori, Y

AU - Morisaki, S

AU - Morisue, N

AU - Moriwaki, Y

AU - Mullavey, A

AU - Nagano, K

AU - Nakano, H

AU - Nakayama, Y

AU - Narikawa, T

AU - Naticchioni, L

AU - Quynh, L Nguyen

AU - Ni, W-T

AU - Nishimoto, T

AU - Nishizawa, A

AU - Nozaki, S

AU - Obayashi, Y

AU - Obuchi, Y

AU - Ogaki, W

AU - Oh, J J

AU - Oh, K

AU - Ohashi, M

AU - Ohashi, T

AU - Ohkawa, M

AU - Ohta, H

AU - Okutani, Y

AU - Oohara, K

AU - Oshino, S

AU - Otabe, S

AU - Pan, K-C

AU - Parisi, A

AU - Park, J

AU - Arellano, F E Peña

AU - Saha, S

AU - Saito, Y

AU - Sakai, K

AU - Sekiguchi, Y

AU - Shao, L

AU - Shikano, Y

AU - Shimizu, H

AU - Shimizu, R

AU - Shimode, K

AU - Shinkai, H

AU - Shishido, T

AU - Shoda, A

AU - Somiya, K

AU - Song, I

AU - Sugimoto, R

AU - Suresh, J

AU - Tagoshi, H

AU - Takahashi, H

AU - Takahashi, R

AU - Takeda, H

AU - Takeda, M

AU - Tamaki, M

AU - Tanaka, K

AU - Tanioka, S

AU - Taruya, A

AU - Tomaru, T

AU - Tomura, T

AU - Trozzo, L

AU - Tsang, T

AU - Tsao, J-S

AU - Tsuchida, S

AU - Tsutsui, T

AU - Tsuzuki, T

AU - Tuyenbayev, D

AU - Uchikata, N

AU - Uchiyama, T

AU - Uehara, T

AU - Ueno, K

AU - Ueshima, G

AU - Uraguchi, F

AU - Ushiba, T

AU - van Putten, M H P M

AU - Wang, J

AU - Washimi, T

AU - Wu, C

AU - Wu, H

AU - Yamamoto, K

AU - Yamazaki, R

AU - Yang, Y

AU - Yeh, S-W

AU - Yokoyama, J

AU - Yokozawa, T

AU - Yoshioka, T

AU - Yuzurihara, H

AU - Zeidler, S

AU - Zhan, M

AU - Zhang, H

AU - Zhao, Y

AU - Zhu, Z-H

PY - 2023/10

Y1 - 2023/10

N2 - Abstract KAGRA, the kilometer-scale underground gravitational-wave detector, is located at Kamioka, Japan. In April 2020, an astrophysics observation was performed at the KAGRA detector in combination with the GEO 600 detector; this observation operation is called O3GK. The optical configuration in O3GK is based on a power-recycled Fabry–Pérot–Michelson interferometer; all the mirrors were set at room temperature. The duty factor of the operation was approximately 53%, and the displacement sensitivity was approximately 1 × 10−18 ${\rm m}/\sqrt{\rm {Hz } }$ at 250 Hz. The binary-neutron-star (BNS) inspiral range was about 0.6 Mpc. The contributions of various noise sources to the sensitivity of O3GK were investigated to understand how the observation range could be improved; this study is called a “noise budget”. According to our noise budget, the measured sensitivity could be approximated by adding up the effect of each noise. The sensitivity was dominated by noise from the sensors used for local controls of the vibration isolation systems, acoustic noise, shot noise, and laser frequency noise. Further, other noise sources that did not limit the sensitivity were investigated. This paper provides a detailed account of the KAGRA detector in O3GK, including interferometer configuration, status, and noise budget. In addition, strategies for future sensitivity improvements, such as hardware upgrades, are discussed.

AB - Abstract KAGRA, the kilometer-scale underground gravitational-wave detector, is located at Kamioka, Japan. In April 2020, an astrophysics observation was performed at the KAGRA detector in combination with the GEO 600 detector; this observation operation is called O3GK. The optical configuration in O3GK is based on a power-recycled Fabry–Pérot–Michelson interferometer; all the mirrors were set at room temperature. The duty factor of the operation was approximately 53%, and the displacement sensitivity was approximately 1 × 10−18 ${\rm m}/\sqrt{\rm {Hz } }$ at 250 Hz. The binary-neutron-star (BNS) inspiral range was about 0.6 Mpc. The contributions of various noise sources to the sensitivity of O3GK were investigated to understand how the observation range could be improved; this study is called a “noise budget”. According to our noise budget, the measured sensitivity could be approximated by adding up the effect of each noise. The sensitivity was dominated by noise from the sensors used for local controls of the vibration isolation systems, acoustic noise, shot noise, and laser frequency noise. Further, other noise sources that did not limit the sensitivity were investigated. This paper provides a detailed account of the KAGRA detector in O3GK, including interferometer configuration, status, and noise budget. In addition, strategies for future sensitivity improvements, such as hardware upgrades, are discussed.

U2 - 10.1093/ptep/ptac093

DO - 10.1093/ptep/ptac093

M3 - 学術論文

SN - 2050-3911

VL - 2023

JO - Progress of Theoretical and Experimental Physics

JF - Progress of Theoretical and Experimental Physics

IS - 10

M1 - 10A101

ER -

Performance of the KAGRA detector during the first joint observation with GEO 600 (O3GK)

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