An arm length stabilization system for KAGRA and future gravitational-wave detectors

被引：15

作者：

Akutsu, T. ^{[1
,2
]}

Ando, M. ^{[1
,3
,4
]}

Arai, K. ^{[5
,6
]}

Arai, Y. ^{[6
]}

Araki, S. ^{[7
]}

Araya, A. ^{[8
]}

Aritomi, N. ^{[3
]}

Aso, Y. ^{[9
,10
]}

Bae, S. ^{[11
]}

Bae, Y. ^{[12
]}

Baiotti, L. ^{[13
]}

Bajpai, R. ^{[14
]}

Barton, M. A. ^{[1
]}

Cannon, K. ^{[4
]}

Capocasa, E. ^{[1
]}

Chan, M. ^{[15
]}

Chen, C. S. ^{[16
]}

Chen, K. ^{[19
]}

Chen, Y. ^{[17
,18
]}

Chu, H. ^{[19
]}

Chu, Y-K ^{[20
]}

Doi, K. ^{[21
]}

Eguchi, S. ^{[15
]}

Enomoto, Y. ^{[3
]}

Flaminio, R. ^{[1
,22
]}

Fujii, Y. ^{[23
]}

Fukunaga, M. ^{[6
]}

Fukushima, M. ^{[1
]}

Ge, G-G ^{[24
]}

Hagiwara, A. ^{[6
,25
]}

Haino, S. ^{[20
]}

Hasegawa, K. ^{[6
]}

Hayakawa, H. ^{[26
]}

Hayama, K. ^{[15
]}

Himemoto, Y. ^{[27
]}

Hiranuma, Y. ^{[28
]}

Hirata, N. ^{[1
]}

Hirose, E. ^{[6
]}

Hong, Z. ^{[29
]}

Hsieh, B. H. ^{[30
]}

Huang, G-Z ^{[29
]}

Huang, P-W ^{[24
]}

Huang, Y. ^{[20
]}

Ikenoue, B. ^{[1
]}

Imam, S. ^{[29
]}

Inayoshi, K. ^{[31
]}

Inoue, Y. ^{[19
]}

Ioka, K. ^{[32
]}

Itoh, Y. ^{[33
,34
]}

Izumi, K. ^{[35
]}

机构：

[1] Natl Astron Observ Japan, Gravitat Wave Project Off, Mitaka, Tokyo 1818588, Japan

[2] Natl Astron Observ Japan, Adv Technol Ctr, Mitaka, Tokyo 1818588, Japan

[3] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan

[4] Univ Tokyo, Res Ctr Early Universe RESCEU, Bunkyo Ku, Tokyo 1130033, Japan

[5] CALTECH, Pasadena, CA 91125 USA

[6] Univ Tokyo, KAGRA Observ, ICRR, Kashiwa, Chiba 2778582, Japan

[7] High Energy Accelerator Res Org KEK, Accelerator Lab, Tsukuba, Ibaraki 3050801, Japan

[8] Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan

[9] Natl Astron Observ Japan, Kamioka Branch, Kamioka Cho, Hida City, Gifu 5061205, Japan

[10] Grad Univ Adv Studies, SOKENDAI, Mitaka, Tokyo 1818588, Japan

[11] Korea Inst Sci & Technol Informat, Daejeon 34141, South Korea

[12] Natl Inst Math Sci, Daejeon 34047, South Korea

[13] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan

[14] Grad Univ Adv Studies, SOKENDAI, Sch High Energy Accelerator Sci, Tsukuba, Ibaraki 3050801, Japan

[15] Fukuoka Univ, Dept Appl Phys, Fukuoka, Fukuoka 8140180, Japan

[16] Tamkang Univ, Dept Phys, New Taipei 25137, Taiwan

[17] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan

[18] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan

[19] Natl Cent Univ, Ctr High Energy & High Field Phys, Dept Phys, Taoyuan 32001, Taiwan

[20] Acad Sinica, Inst Phys, Taipei 11529, Taiwan

[21] Univ Toyama, Dept Phys, Toyama, Toyama 9308555, Japan

[22] Univ Savoie Mt Blanc, Univ Grenoble Alpes, LAPP, CNRS IN2P3, F-74941 Annecy, France

[23] Univ Tokyo, Dept Astron, Mitaka, Tokyo 1818588, Japan

[24] Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China

[25] High Energy Accelerator Res Org KEK, Appl Res Lab, Tsukuba, Ibaraki 3050801, Japan

[26] Univ Tokyo, KAGRA Observ, ICRR, Kamioka Cho, Hida City, Gifu 5061205, Japan

[27] Nihon Univ, Coll Ind Technol, Narashino, Chiba 2758575, Japan

[28] Niigata Univ, Grad Sch Sci & Technol, Nishi Ku, Niigata, Niigata 9502181, Japan

[29] Natl Taiwan Normal Univ, Dept Phys, Taipei 116, Taiwan

[30] Univ Tokyo, RCCN, ICRR, Kashiwa, Chiba 2778582, Japan

[31] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[32] Kyoto Univ, YITP, Sakyou Ku, Kyoto, Kyoto 6068502, Japan

[33] Osaka City Univ, Grad Sch Sci, Dept Phys, Sumiyoshi Ku, Osaka, Osaka 5588585, Japan

[34] Osaka City Univ, Nambu Yoichiro Inst Theoret & Expt Phys NITEP, Sumiyoshi Ku, Osaka, Osaka 5588585, Japan

[35] Inst Space & Astronaut Sci JAXA, Chuo Ku, Sagamihara, Kanagawa 2520222, Japan

[36] Ulsan Natl Inst Sci & Technol, Sch Nat Sci, Dept Phys, Ulsan 44919, South Korea

[37] Univ Tokyo, ICRR, Kashiwa, Chiba 2778582, Japan

[38] Tokyo Inst Technol, Grad Sch Sci & Technol, Meguro Ku, Tokyo 1528551, Japan

[39] Ewha Womans Univ, Dept Phys, Seoul 03760, South Korea

[40] Inje Univ, Dept Comp Simulat, Gimhae 50834, Gyeongsangnam D, South Korea

[41] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 9030213, Japan

[42] Univ Tokyo, RCCN, ICRR, Kamioka Cho, Hida City, Gifu 5061205, Japan

[43] Nagoya Univ, Inst Adv Res, Chikusa Ku, Furocho, Nagoya, Aichi 4648602, Japan

[44] Hanyang Univ, Dept Phys, Seoul 133791, South Korea

[45] Natl Appl Res Labs, Natl Ctr High Performance Comp, Hsinchu Sci Pk, Hsinchu 30076, Taiwan

[46] Univ Tokyo, Inst Photon Sci & Technol, Bunkyo Ku, Tokyo 1138656, Japan

[47] Univ Electrocommun, Inst Laser Sci, Chofu, Tokyo 1828585, Japan

[48] Natl Inst Informat & Commun Technol NICT, Appl Electromagnet Res Inst, Koganei, Tokyo 1848795, Japan

[49] Ryukoku Univ, Fac Law, Fushimi Ku, Kyoto, Kyoto 6128577, Japan

[50] Kyoto Univ, Dept Phys, Sakyou Ku, Kyoto, Kyoto 6068502, Japan

来源：

CLASSICAL AND QUANTUM GRAVITY | 2020年 / 37卷 / 03期

基金：

新加坡国家研究基金会;

关键词：

gravitational-wave detector; interferometer; multi-colour; FREQUENCY STABILIZATION; EXTRACTION; LOCK;

D O I：

10.1088/1361-6382/ab5c95

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Modern ground-based gravitational wave (GW) detectors require a complex interferometer configuration with multiple coupled optical cavities. Since achieving the resonances of the arm cavities is the most challenging among the lock acquisition processes, the scheme called arm length stabilization (ALS) had been employed for lock acquisition of the arm cavities. We designed a new type of the ALS, which is compatible with the interferometers having long arms like the next generation GW detectors. The features of the new ALS are that the control configuration is simpler than those of previous ones and that it is not necessary to lay optical fibers for the ALS along the kilometer-long arms of the detector. Along with simulations of its noise performance, an experimental test of the new ALS was performed utilizing a single arm cavity of KAGRA. This paper presents the first results of the test where we demonstrated that lock acquisition of the arm cavity was achieved using the new ALS. We also demonstrated that the root mean square of residual noise was measured to be 8.2 Hz in units of frequency, which is smaller than the linewidth of the arm cavity and thus low enough to lock the full interferometer of KAGRA in a repeatable and reliable manner.

引用

页数：19

共 34 条

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