Updated on 2022/06/28

写真b

 
ZEIDLER, Simon
 
*Items subject to periodic update by Rikkyo University (The rest are reprinted from information registered on researchmap.)
Affiliation*
College of Science Department of Physics
Title*
Assistant Professor
Degree
Ph.D. ( 7 2013   Friedrich-Schiller-University Jena )
Research Interests
  • Interferometry

  • Spectroscopy

  • Gravitation

  • Material Science

  • Optics

  • Gravitational Waves

  • Campus Career*
    • 4 2020 - Present 
      College of Science   Department of Physics   Assistant Professor
    Profile

    I am a physicist, specialized in optics, data analysis, and material science who is working in the field of experimental gravitation research

     

    Research Areas

    • Natural Science / Semiconductors, optical properties of condensed matter and atomic physics  / Optical Property Characterization of Solids

    • Natural Science / Theoretical studies related to particle-, nuclear-, cosmic ray and astro-physics  / Gravitational Wave Detector Science

    Research History

    • 4 2020 - Present 
      Rikkyo University   College of Science Department of Physics   Assistant Professor

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    • 6 2019 - 3 2020 
      National Astronomical Observatory of Japan   Gravitational Wave Project Office   Senior Specialist

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    • 6 2014 - 5 2019 
      National Astronomical Observatory of Japan   Gravitational Wave Project Office   Project Research Fellow

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    • 2 2010 - 10 2013 
      Friedrich-Schiller University Jena   Astrophysical Institute   Research Associate

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    • 9 2009 - 1 2010 
      Friedrich-Schiller University Jena   Astrophysical Institute   Research Assistant

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    Education

    • 2 2010 - 7 2013 
      Friedrich-Schiller University Jena   Physical-Astronomical Department   Ph.D.

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      Country: Germany

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    • 10 2003 - 1 2009 
      Friedrich-Schiller University Jena   Physical-Astronomical Department   Physics Diploma (Master)

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    • 9 1993 - 7 2002 
      Gymnasium Egeln   High-School

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    Papers

    • Overview of KAGRA: Calibration, detector characterization, physical environmental monitors, and the geophysics interferometer

      T Akutsu, M Ando, K Arai, Y Arai, S Araki, A Araya, N Aritomi, H Asada, Y Aso, S Bae, Y Bae, L Baiotti, R Bajpai, M A Barton, K Cannon, Z Cao, E Capocasa, M Chan, C Chen, K Chen, Y Chen, C -Y Chiang, H Chu, Y -K Chu, S Eguchi, Y Enomoto, R Flaminio, Y Fujii, Y Fujikawa, M Fukunaga, M Fukushima, D Gao, G Ge, S Ha, A Hagiwara, S Haino, W -B Han, K Hasegawa, K Hattori, H Hayakawa, K Hayama, Y Himemoto, Y Hiranuma, N Hirata, E Hirose, Z Hong, B Hsieh, G -Z Huang, H -Y Huang, P Huang, Y -C Huang, Y Huang, D C Y Hui, S Ide, B Ikenoue, S Imam, K Inayoshi, Y Inoue, K Ioka, K Ito, Y Itoh, K Izumi, C Jeon, H -B Jin, K Jung, P Jung, K Kaihotsu, T Kajita, M Kakizaki, M Kamiizumi, N K, a, G Kang, K Kawaguchi, N Kawai, T Kawasaki, C Kim, J Kim, J C Kim, W S Kim, Y -M Kim, N Kimura, N Kita, H Kitazawa, Y Kojima, K Kokeyama, K Komori, A K H Kong, K Kotake, C Kozakai, R Kozu, R Kumar, J Kume, C Kuo, H -S Kuo, Y Kuromiya, S Kuroyanagi, K Kusayanagi, K Kwak, H K Lee, H W Lee, R Lee, M Leonardi, K L Li, L C -C Lin, C -Y Lin, F -K Lin, F -L Lin, H L Lin, G C Liu, L -W Luo, E Majorana, M Marchio, Y Michimura, N Mio, O Miyakawa, A Miyamoto, Y Miyazaki, K Miyo, S Miyoki, Y Mori, S Morisaki, Y Moriwaki, K Nagano, S Nagano, K Nakamura, H Nakano, M Nakano, R Nakashima, Y Nakayama, T Narikawa, L Naticchioni, R Negishi, L Nguyen Quynh, W -T Ni, A Nishizawa, S Nozaki, Y Obuchi, W Ogaki, J J Oh, K Oh, S H Oh, M Ohashi, N Ohishi, M Ohkawa, H Ohta, Y Okutani, K Okutomi, K Oohara, C Ooi, S Oshino, S Otabe, K Pan, H Pang, A Parisi, J Park, F E Pe{\~{n } }a Arellano, I Pinto, N Sago, S Saito, Y Saito, K Sakai, Y Sakai, Y Sakuno, S Sato, T Sato, T Sawada, T Sekiguchi, Y Sekiguchi, L Shao, S Shibagaki, R Shimizu, T Shimoda, K Shimode, H Shinkai, T Shishido, A Shoda, K Somiya, E J Son, H Sotani, R Sugimoto, J Suresh, T Suzuki, T Suzuki, H Tagoshi, H Takahashi, R Takahashi, A Takamori, S Takano, H Takeda, M Takeda, H Tanaka, K Tanaka, K Tanaka, T Tanaka, T Tanaka, S Tanioka, E N Tapia San Martin, S Telada, T Tomaru, Y Tomigami, T Tomura, F Travasso, L Trozzo, T Tsang, J -S Tsao, K Tsubono, S Tsuchida, T Tsutsui, T Tsuzuki, D Tuyenbayev, N Uchikata, T Uchiyama, A Ueda, T Uehara, K Ueno, G Ueshima, F Uraguchi, T Ushiba, M H P M van Putten, H Vocca, J Wang, T Washimi, C Wu, H Wu, S Wu, W -R Xu, T Yamada, K Yamamoto, K Yamamoto, T Yamamoto, K Yamashita, R Yamazaki, Y Yang, K Yokogawa, J Yokoyama, T Yokozawa, T Yoshioka, H Yuzurihara, S Zeidler, M Zhan, H Zhang, Y Zhao, Z -H Zhu

      Progress of Theoretical and Experimental Physics2021 ( 5 )   18 5 2021

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:Oxford University Press ({OUP})  

      <jats:title>Abstract</jats:title>
      <jats:p>KAGRA is a newly built gravitational wave observatory, a laser interferometer with a 3 km arm length, located at Kamioka, Gifu, Japan. In this series of articles we present an overview of the baseline KAGRA, for which we finished installing the designed configuration in 2019. This article describes the method of calibration (CAL) used for reconstructing gravitational wave signals from the detector outputs, as well as the characterization of the detector (DET). We also review the physical environmental monitoring (PEM) system and the geophysics interferometer (GIF). Both are used for characterizing and evaluating the data quality of the gravitational wave channel. They play important roles in utilizing the detector output for gravitational wave searches. These characterization investigations will be even more important in the near future, once gravitational wave detection has been achieved, and in using KAGRA in the gravitational wave astronomy era.</jats:p>

      DOI: 10.1093/ptep/ptab018

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    • Overview of KAGRA: KAGRA science

      T Akutsu, M Ando, K Arai, Y Arai, S Araki, A Araya, N Aritomi, H Asada, Y Aso, S Bae, Y Bae, L Baiotti, R Bajpai, M A Barton, K Cannon, Z Cao, E Capocasa, M Chan, C Chen, K Chen, Y Chen, C -Y Chiang, H Chu, Y -K Chu, S Eguchi, Y Enomoto, R Flaminio, Y Fujii, F Fujikawa, M Fukunaga, M Fukushima, D Gao, G Ge, S Ha, A Hagiwara, S Haino, W -B Han, K Hasegawa, K Hattori, H Hayakawa, K Hayama, Y Himemoto, Y Hiranuma, N Hirata, E Hirose, Z Hong, B H Hsieh, C -Z Huang, H -Y Huang, P Huang, Y Huang, Y -C Huang, D C Y Hui, S Ide, B Ikenoue, S Imam, K Inayoshi, Y Inoue, K Ioka, K Ito, Y Itoh, K Izumi, C Jeon, H -B Jin, K Jung, P Jung, K Kaihotsu, T Kajita, M Kakizaki, M Kamiizumi, N K, a, G Kang, K Kashiyama, K Kawaguchi, N Kawai, T Kawasaki, C Kim, J Kim, J C Kim, W S Kim, Y -M Kim, N Kimura, N Kita, H Kitazawa, Y Kojima, K Kokeyama, K Komori, A K H Kong, K Kotake, C Kozakai, R Kozu, R Kumar, J Kume, C Kuo, H -S Kuo, Y Kuromiya, S Kuroyanagi, K Kusayanagi, K Kwak, H K Lee, H W Lee, R Lee, M Leonardi, K L Li, T G F Li, C -Y Lin, F -K Lin, F -L Lin, H L Lin, L C -C Lin, G C Liu, L -W Luo, E Majorana, M Marchio, Y Michimura, N Mio, O Miyakawa, A Miyamoto, Y Miyazaki, K Miyo, S Miyoki, Y Mori, S Morisaki, Y Moriwaki, K Nagano, S Nagano, K Nakamura, H Nakano, M Nakano, R Nakashima, Y Nakayama, T Narikawa, L Naticchioni, R Negishi, L Nguyen Quynh, W -T Ni, A Nishizawa, S Nozaki, Y Obuchi, W Ogaki, J J Oh, K Oh, S H Oh, M Ohashi, N Ohishi, M Ohkawa, H Ohta, Y Okutani, K Okutomi, K Oohara, C P Ooi, S Oshino, S Otabe, K Pan, H Pang, A Parisi, J Park, F E Pe na Arellano, I Pinto, N Sago, S Saito, Y Saito, K Sakai, Y Sakai, Y Sakuno, S Sato, T Sato, T Sawada, T Sekiguchi, Y Sekiguchi, L Shao, S Shibagaki, R Shimizu, T Shimoda, K Shimode, H Shinkai, T Shishido, A Shoda, K Somiya, E J Son, H Sotani, R Sugimoto, J Suresh, T Suzuki, T Suzuki, H Tagoshi, H Takahashi, R Takahashi, A Takamori, S Takano, H Takeda, M Takeda, H Tanaka, K Tanaka, K Tanaka, T Tanaka, T Tanaka, S Tanioka, E N Tapia San Martin, S Telada, T Tomaru, Y Tomigami, T Tomura, F Travasso, L Trozzo, T Tsang, J -S Tsao, K Tsubono, S Tsuchida, D Tsuna, T Tsutsui, T Tsuzuki, D Tuyenbayev, N Uchikata, T Uchiyama, A Ueda, T Uehara, K Ueno, G Ueshima, F Uraguchi, T Ushiba, M H P M van Putten, H Vocca, J Wang, T Washimi, C Wu, H Wu, S Wu, W -R Xu, T Yamada, K Yamamoto, K Yamamoto, T Yamamoto, K Yamashita, R Yamazaki, Y Yang, K Yokogawa, J Yokoyama, T Yokozawa, T Yoshioka, H Yuzurihara, S Zeidler, M Zhan, H Zhang, Y Zhao, Z -H Zhu

      Progress of Theoretical and Experimental Physics2021 ( 5 )   18 5 2021

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:Oxford University Press ({OUP})  

      <jats:title>Abstract</jats:title>
      <jats:p>KAGRA is a newly build gravitational wave observatory, a laser interferometer with 3 km arm length, located in Kamioka, Gifu, Japan. In this paper, one of a series of articles featuring KAGRA, we discuss the science targets of KAGRA projects, considering not only the baseline KAGRA (current design) but also its future upgrade candidates (KAGRA+) for the near to middle term ($\sim$5 years).</jats:p>

      DOI: 10.1093/ptep/ptaa120

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      Other Link: http://academic.oup.com/ptep/article-pdf/2021/5/05A103/37953064/ptaa120.pdf

    • Overview of KAGRA: Detector design and construction history

      T Akutsu, M Ando, K Arai, Y Arai, S Araki, A Araya, N Aritomi, Y Aso, S Bae, Y Bae, L Baiotti, R Bajpai, M A Barton, K Cannon, E Capocasa, M Chan, C Chen, K Chen, Y Chen, H Chu, Y -K Chu, S Eguchi, Y Enomoto, R Flaminio, Y Fujii, M Fukunaga, M Fukushima, G Ge, A Hagiwara, S Haino, K Hasegawa, H Hayakawa, K Hayama, Y Himemoto, Y Hiranuma, N Hirata, E Hirose, Z Hong, B H Hsieh, C -Z Huang, P Huang, Y Huang, B Ikenoue, S Imam, K Inayoshi, Y Inoue, K Ioka, Y Itoh, K Izumi, K Jung, P Jung, T Kajita, M Kamiizumi, N K, a, G Kang, K Kawaguchi, N Kawai, T Kawasaki, C Kim, J C Kim, W S Kim, Y -M Kim, N Kimura, N Kita, H Kitazawa, Y Kojima, K Kokeyama, K Komori, A K H Kong, K Kotake, C Kozakai, R Kozu, R Kumar, J Kume, C Kuo, H -S Kuo, S Kuroyanagi, K Kusayanagi, K Kwak, H K Lee, H W Lee, R Lee, M Leonardi, L C -C Lin, C -Y Lin, F -L Lin, G C Liu, L -W Luo, M Marchio, Y Michimura, N Mio, O Miyakawa, A Miyamoto, Y Miyazaki, K Miyo, S Miyoki, S Morisaki, Y Moriwaki, K Nagano, S Nagano, K Nakamura, H Nakano, M Nakano, R Nakashima, T Narikawa, R Negishi, W -T Ni, A Nishizawa, Y Obuchi, W Ogaki, J J Oh, S H Oh, M Ohashi, N Ohishi, M Ohkawa, K Okutomi, K Oohara, C P Ooi, S Oshino, K Pan, H Pang, J Park, F E Pe{\~{n } }a Arellano, I Pinto, N Sago, S Saito, Y Saito, K Sakai, Y Sakai, Y Sakuno, S Sato, T Sato, T Sawada, T Sekiguchi, Y Sekiguchi, S Shibagaki, R Shimizu, T Shimoda, K Shimode, H Shinkai, T Shishido, A Shoda, K Somiya, E J Son, H Sotani, R Sugimoto, T Suzuki, T Suzuki, H Tagoshi, H Takahashi, R Takahashi, A Takamori, S Takano, H Takeda, M Takeda, H Tanaka, K Tanaka, K Tanaka, T Tanaka, T Tanaka, S Tanioka, E N Tapia San Martin, S Telada, T Tomaru, Y Tomigami, T Tomura, F Travasso, L Trozzo, T Tsang, K Tsubono, S Tsuchida, T Tsuzuki, D Tuyenbayev, N Uchikata, T Uchiyama, A Ueda, T Uehara, K Ueno, G Ueshima, F Uraguchi, T Ushiba, M H P M van Putten, H Vocca, J Wang, C Wu, H Wu, S Wu, W- R Xu, T Yamada, K Yamamoto, K Yamamoto, T Yamamoto, K Yokogawa, J Yokoyama, T Yokozawa, T Yoshioka, H Yuzurihara, S Zeidler, Y Zhao, Z -H Zhu

      Progress of Theoretical and Experimental Physics2021 ( 5 )   18 5 2021

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:Oxford University Press ({OUP})  

      <jats:title>Abstract</jats:title>
      <jats:p>KAGRA is a newly built gravitational-wave telescope, a laser interferometer comprising arms with a length of 3 km, located in Kamioka, Gifu, Japan. KAGRA was constructed under the ground and it is operated using cryogenic mirrors that help in reducing the seismic and thermal noise. Both technologies are expected to provide directions for the future of gravitational-wave telescopes. In 2019, KAGRA finished all installations with the designed configuration, which we call the baseline KAGRA. For this occasion, we present an overview of the baseline KAGRA from various viewpoints in a series of articles. In this article, we introduce the design configurations of KAGRA with its historical background.</jats:p>

      DOI: 10.1093/ptep/ptaa125

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    • Cryogenic suspension design for a kilometer-scale gravitational-wave detector

      Takafumi Ushiba, Tomotada Akutsu, Sakae Araki, Rishabh Bajpai, Dan Chen, Kieran Craig, Yutaro Enomoto, Ayako Hagiwara, Sadakazu Haino, Yuki Inoue, Kiwamu Izumi, Nobuhiro Kimura, Rahul Kumar, Yuta Michimura, Shinji Miyoki, Iwao Murakami, Yoshikazu Namai, Masayuki Nakano, Masatake Ohashi, Koki Okutomi, Takaharu Shishido, Ayaka Shoda, Kentaro Somiya, Toshikazu Suzuki, Suguru Takada, Masahiro Takahashi, Ryutaro Takahashi, Shinichi Terashima, Takayuki Tomaru, Flavio Travasso, Ayako Ueda, Helios Vocca, Tomohiro Yamada, Kazuhiro Yamamoto, Simon Zeidler

      Classical and Quantum Gravity38 ( 8 ) 085013 - 085013   22 4 2021

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      Publishing type:Research paper (scientific journal)   Publisher:{IOP} Publishing  

      DOI: 10.1088/1361-6382/abe9f3

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      Other Link: https://iopscience.iop.org/article/10.1088/1361-6382/abe9f3/pdf

    • Radiative Cooling of the Thermally Isolated System in KAGRA Gravitational Wave Telescope

      T. Akutsu, M. Ando, K. Arai, Y. Arai, S. Araki, A. Araya, N. Aritomi, Y. Aso, S.-W. Bae, Y.-B. Bae, L. Baiotti, R. Bajpai, M. A. Barton, K. Cannon, E. Capocasa, M.-L. Chan, C.-S. Chen, K.-H. Chen, Y.-R. Chen, H.-Y. Chu, Y.-K. Chu, S. Eguchi, Y. Enomoto, R. Flaminio, Y. Fujii, M. Fukunaga, M. Fukushima, G.-G. Ge, A. Hagiwara, S. Haino, K. Hasegawa, H. Hayakawa, K. Hayama, Y. Himemoto, Y. Hiranuma, N. Hirata, E. Hirose, Z. Hong, B.-H. Hsieh, G.-Z. Huang, P.-W. Huang, Y.-J. Huang, B. Ikenoue, S. Imam, K. Inayoshi, Y. Inoue, K. Ioka, Y. Itoh, K. Izumi, K. Jung, P. Jung, T. Kajita, M. Kamiizumi, N. Kanda, G.-W. Kang, K. Kawaguchi, N. Kawai, T. Kawasaki, C. Kim, J. Kim, W. Kim, Y.-M. Kim, N. Kimura, N. Kita, H. Kitazawa, Y. Kojima, K. Kokeyama, K. Komori, A. K. H. Kong, K. Kotake, C. Kozakai, R. Kozu, R. Kumar, J. Kume, C.-M. Kuo, H.-S. Kuo, S. Kuroyanagi, K. Kusayanagi, K. Kwak, H.-K. Lee, H.-W. Lee, R.-K. Lee, M. Leonardi, C.-Y. Lin, F.-L. Lin, L. C.-C. Lin, G.-C. Liu, L.-W. Luo, M. Marchio, Y. Michimura, N. Mio, O. Miyakawa, A. Miyamoto, Y. Miyazaki, K. Miyo, S. Miyoki, S. Morisaki, Y. Moriwaki, K. Nagano, S. Nagano, K. Nakamura, H. Nakano, M. Nakano, R. Nakashima, T. Narikawa, R. Negishi, W.-T. Ni, A. Nishizawa, Y. Obuchi, W. Ogaki, J. J. Oh, S.-H. Oh, M. Ohashi, N. Ohishi, M. Ohkawa, K. Okutomi, K. Oohara, C.-P. Ooi, S. Oshino, K.-C. Pan, H.-F. Pang, J. Park, F. E. Peiia Arellano, I. Pinto, N. Sago, S. Saito, Y. Saito, K. Sakai, Y. Sakai, Y. Sakuno, S. Sato, T. Sato, T. Sawada, T. Sekiguchi, Y. Sekiguchi, S. Shibagaki, R. Shimizu, T. Shimoda, K. Shimode, H. Shinkai, T. Shishido, A. Shoda, K. Somiya, E. J. Son, H. Sotani, R. Sugimoto, T. Suzuki, T. Suzuki, H. Tagoshi, H. Takahashi, R. Takahashi, A. Takamori, S. Takano, H. Takeda, M. Takeda, H. Tanaka, K. Tanaka, K. Tanaka, T. Tanaka, T. Tanaka, S. Tanioka, E. N. Tapia San Martin, S. Telada, T. Tomaru, Y. Tomigami, T. Tomura, F. Travasso, L. Trozzo, T. T. L. Tsang, K. Tsubono, S. Tsuchida, T. Tsuzuki, D. Tuyenbayev, N. Uchikata, T. Uchiyama, A. Ueda, T. Uehara, K. Ueno, G. Ueshima, F. Uraguchi, T. Ushiba, M. H. P. M. van Putten, H. Vocca, J. Wang, C.-M. Wu, H.-C. Wu, S.-R. Wu, W.-R. Xu, T. Yamada, K. Yamamoto, K. Yamamoto, T. Yamamoto, K. Yokogawa, J. Yokoyama, T. Yokozawa, T. Yoshioka, H. Yuzurihara, S. Zeidler, Y. Zhao, Z.-H. Zhu

      Journal of Physics: Conference Series1857 ( 1 ) 012002 - 012002   1 4 2021

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      Publishing type:Research paper (scientific journal)   Publisher:IOP Publishing  

      DOI: 10.1088/1742-6596/1857/1/012002

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      Other Link: https://iopscience.iop.org/article/10.1088/1742-6596/1857/1/012002/pdf

    • Vibration isolation systems for the beam splitter and signal recycling mirrors of the KAGRA gravitational wave detector

      Akutsu, T., Ando, M., Arai, K., Arai, Y., Araki, S., Araya, A., Aritomi, N., Asada, H., Aso, Y., Bae, S., Bae, Y., Baiotti, L., Bajpai, R., Barton, M.A., Cannon, K., Cao, Z., Capocasa, E., Chan, M., Chen, C., Chen, K., Chen, Y., Chiang, C.-Y., Chu, H., Chu, Y.-K., Eguchi, S., Enomoto, Y., Flaminio, R., Fujii, Y., Fujikawa, Y., Fukunaga, M., Fukushima, M., Gao, D., Ge, G., Ha, S., Hagiwara, A., Haino, S., Han, W.-B., Hasegawa, K., Hatoya, R., Hattori, K., Hayakawa, H., Hayama, K., Himemoto, Y., Hiranuma, Y., Hirata, N., Hirose, E., Hong, Z., Hsieh, B., Huang, G.-Z., Huang, H.-Y., Huang, P., Huang, Y.-C., Huang, Y., Hui, D.C.Y., Ide, S., Ikenoue, B., Imam, S., Inayoshi, K., Inoue, Y., Ioka, K., Ito, K., Itoh, Y., Izumi, K., Jeon, C., Jin, H.-B., Jung, K., Jung, P., Kaihotsu, K., Kajita, T., Kakizaki, M., Kamiizumi, M., Kanda, N., Kang, G., Kawaguchi, K., Kawai, N., Kawasaki, T., Kim, C., Kim, J., Kim, J.C., Kim, W.S., Kim, Y.-M., Kimura, N., Kita, N., Kitazawa, H., Kojima, Y., Kokeyama, K., Komori, K., Kong, A.K.H., Kotake, K., Kozakai, C., Kozu, R., Kumar, R., Kume, J., Kuo, C., Kuo, H.-S., Kuromiya, Y., Kuroyanagi, S., Kusayanagi, K., Kwak, K., Lee, H.K., Lee, H.W., Lee, R., Leonardi, M., Li, K.L., Lin, L.C.-C., Lin, C.-Y., Lin, F.-K., Lin, F.-L., Lin, H.L., Liu, G.C., Luo, L.-W., Majorana, E., Marchio, M., Michimura, Y., Mio, N., Miyakawa, O., Miyamoto, A., Miyazaki, Y., Miyo, K., Miyoki, S., Mori, Y., Morisaki, S., Moriwaki, Y., Nagano, K., Nagano, S., Nakamura, K., Nakano, H., Nakano, M., Nakashima, R., Nakayama, Y., Narikawa, T., Naticchioni, L., Negishi, R., Nguyen Quynh, L., Ni, W.-T., Nishizawa, A., Nozaki, S., Obuchi, Y., Ogaki, W., Oh, J.J., Oh, K., Oh, S.H., Ohashi, M., Ohishi, N., Ohkawa, M., Ohta, H., Okutani, Y., Okutomi, K., Oohara, K., Ooi, C., Oshino, S., Otabe, S., Pan, K., Pang, H., Parisi, A., Park, J., Pea Arellano, F.E., Pinto, I., Sago, N., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sakuno, Y., Sato, S., Sato, T., Sawada, T., Sekiguchi, T., Sekiguchi, Y., Shao, L., Shibagaki, S., Shimizu, R., Shimoda, T., Shimode, K., Shinkai, H., Shishido, T., Shoda, A., Somiya, K., Son, E.J., Sotani, H., Sugimoto, R., Suresh, J., Suzuki, T., Suzuki, T., Tagoshi, H., Takahashi, H., Takahashi, R., Takamori, A., Takano, S., Takeda, H., Takeda, M., Tanaka, H., Tanaka, K., Tanaka, K., Tanaka, T., Tanaka, T., Tanioka, S., Tapia San Martin, E.N., Telada, S., Tomaru, T., Tomigami, Y., Tomura, T., Travasso, F., Trozzo, L., Tsang, T., Tsao, J.-S., Tsubono, K., Tsuchida, S., Tsutsui, T., Tsuzuki, T., Tuyenbayev, D., Uchikata, N., Uchiyama, T., Ueda, A., Uehara, T., Ueno, K., Ueshima, G., Uraguchi, F., Ushiba, T., Van Putten, M.H.P.M., Vocca, H., Wang, J., Washimi, T., Wu, C., Wu, H., Wu, S., Xu, W.-R., Yamada, T., Yamamoto, K., Yamamoto, K., Yamamoto, T., Yamashita, K., Yamazaki, R., Yang, Y., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoshioka, T., Yuzurihara, H., Zeidler, S., Zhan, M., Zhang, H., Zhao, Y., Zhu, Z.-H.

      Classical and Quantum Gravity38 ( 6 ) 065011 - 065011   2021

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      Publishing type:Research paper (scientific journal)   Publisher:IOP Publishing  

      DOI: 10.1088/1361-6382/abd922

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    • Application of independent component analysis to the iKAGRA data Peer-reviewed

      Akutsu, T., Akutsu, T., Ando, M., Ando, M., Ando, M., Arai, K., Arai, Y., Araki, S., Araya, A., Aritomi, N., Asada, H., Asada, H., Aso, Y., Aso, Y., Atsuta, S., Awai, K., Bae, S., Bae, Y., Baiotti, L., Bajpai, R., Barton, M.A., Cannon, K., Capocasa, E., Chan, M., Chen, C., Chen, C., Chen, K., Chen, Y., Chu, H., Chu, Y.-K., Craig, K., Creus, W., Doi, K., Eda, K., Eguchi, S., Enomoto, Y., Flaminio, R., Flaminio, R., Fujii, Y., Fujimoto, M.-K., Fukunaga, M., Fukushima, M., Furuhata, T., Ge, G., Hagiwara, A., Hagiwara, A., Haino, S., Hasegawa, K., Hashino, K., Hayakawa, H., Hayama, K., Himemoto, Y., Hiranuma, Y., Hirata, N., Hirobayashi, S., Hirose, E., Hong, Z., Hsieh, B.H., Huang, G.-Z., Huang, P., Huang, Y., Ikenoue, B., Imam, S., Inayoshi, K., Inoue, Y., Ioka, K., Itoh, Y., Itoh, Y., Izumi, K., Jung, K., Jung, P., Kaji, T., Kajita, T., Kakizaki, M., Kamiizumi, M., Kanbara, S., Kanda, N., Kanda, N., Kanemura, S., Kaneyama, M., Kang, G., Kasuya, J., Kataoka, Y., Kawaguchi, K., Kawai, N., Kawamura, S., Kawasaki, T., Kim, C., Kim, J.C., Kim, W.S., Kim, Y.-M., Kimura, N., Kinugawa, T., Kirii, S., Kita, N., Kitaoka, Y., Kitazawa, H., Kojima, Y., Kokeyama, K., Komori, K., Kong, A.K.H., Kotake, K., Kozakai, C., Kozu, R., Kumar, R., Kume, J., Kume, J., Kuo, C., Kuo, H.-S., Kuroyanagi, S., Kusayanagi, K., Kwak, K., Lee, H.K., Lee, H.M., Lee, H.M., Lee, H.W., Lee, R., Leonardi, M., Lin, C., Lin, C.-Y., Lin, F.-L., Liu, G.C., Liu, Y., Luo, L., Majorana, E., Mano, S., Marchio, M., Matsui, T., Matsushima, F., Michimura, Y., Mio, N., Miyakawa, O., Miyamoto, A., Miyamoto, T., Miyazaki, Y., Miyo, K., Miyoki, S., Morii, W., Morisaki, S., Moriwaki, Y., Morozumi, T., Musha, M., Nagano, K., Nagano, S., Nakamura, K., Nakamura, T., Nakano, H., Nakano, M., Nakano, M., Nakao, K., Nakashima, R., Narikawa, T., Naticchioni, L., Negishi, R., Quynh, L.N., Ni, W.-T., Ni, W.-T., Ni, W.-T., Nishizawa, A., Obuchi, Y., Ochi, T., Ogaki, W., Oh, J.J., Oh, S.H., Ohashi, M., Ohishi, N., Ohkawa, M., Okutomi, K., Oohara, K., Ooi, C.P., Oshino, S., Pan, K., Pang, H., Park, J., Arellano, F.E.P., Pinto, I., Sago, N., Saijo, M., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sakai, Y., Sakuno, Y., Sasaki, M., Sasaki, Y., Sato, S., Sato, T., Sawada, T., Sekiguchi, T., Sekiguchi, Y., Seto, N., Shibagaki, S., Shibata, M., Shibata, M., Shimizu, R., Shimoda, T., Shimode, K., Shinkai, H., Shishido, T., Shoda, A., Somiya, K., Son, E.J., Sotani, H., Suemasa, A., Sugimoto, R., Suzuki, T., Suzuki, T., Tagoshi, H., Takahashi, H., Takahashi, R., Takamori, A., Takano, S., Takeda, H., Takeda, M., Tanaka, H., Tanaka, K., Tanaka, K., Tanaka, T., Tanaka, T., Tanioka, S., Tanioka, S., Martin, E.N.T.S., Tatsumi, D., Telada, S., Tomaru, T., Tomigami, Y., Tomura, T., Travasso, F., Travasso, F., Trozzo, L., Tsang, T., Tsubono, K., Tsuchida, S., Tsuzuki, T., Tuyenbayev, D., Uchikata, N., Uchiyama, T., Ueda, A., Uehara, T., Uehara, T., Ueki, S., Ueno, K., Ueshima, G., Uraguchi, F., Ushiba, T., Van Putten, M.H.P.M., Vocca, H., Wada, S., Wakamatsu, T., Wang, J., Wu, C., Wu, H., Wu, S., Xu, W.-R., Yamada, T., Yamamoto, A., Yamamoto, K., Yamamoto, K., Yamamoto, S., Yamamoto, T., Yokogawa, K., Yokoyama, J., Yokoyama, J., Yokozawa, T., Yoon, T.H., Yoshioka, T., Yuzurihara, H., Zeidler, S., Zhao, Y., Zhu, Z.-H.

      Progress of Theoretical and Experimental Physics2020 ( 5 )   2020

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      Publishing type:Research paper (scientific journal)   Publisher:Oxford University Press (OUP)  

      <title>Abstract</title>
      We apply independent component analysis (ICA) to real data from a gravitational wave detector for the first time. Specifically, we use the iKAGRA data taken in April 2016, and calculate the correlations between the gravitational wave strain channel and 35 physical environmental channels. Using a couple of seismic channels which are found to be strongly correlated with the strain, we perform ICA. Injecting a sinusoidal continuous signal in the strain channel, we find that ICA recovers correct parameters with enhanced signal-to-noise ratio, which demonstrates the usefulness of this method. Among the two implementations of ICA used here, we find the correlation method yields the optimal results for the case of environmental noise acting on the strain channel linearly.

      DOI: 10.1093/ptep/ptaa056

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

      Akutsu, T., Ando, M., Arai, K., Arai, K., Arai, Y., Araki, S., Araya, A., Aritomi, N., Aso, Y., Bae, S., Bae, Y., Baiotti, L., Bajpai, R., Barton, M.A., Cannon, K., Capocasa, E., Chan, M., Chen, C.S., Chen, K., Chen, Y., Chu, H., Chu, Y.-K., Doi, K., Eguchi, S., Enomoto, Y., Flaminio, R., Fujii, Y., Fukunaga, M., Fukushima, M., Ge, G.-G., Hagiwara, A., Haino, S., Hasegawa, K., Hayakawa, H., Hayama, K., Himemoto, Y., Hiranuma, Y., Hirata, N., Hirose, E., Hong, Z., Hsieh, B.H., Huang, G.-Z., Huang, P.-W., Huang, Y., Ikenoue, B., Imam, S., Inayoshi, K., Inoue, Y., Ioka, K., Itoh, Y., Izumi, K., Jung, K., Jung, P., Kajita, T., Kamiizumi, M., Kanbara, S., Kanda, N., Kang, G., Kawaguchi, K., Kawai, N., Kawasaki, T., Kim, C., Kim, J.C., Kim, W.S., Kim, Y.-M., Kimura, N., Kita, N., Kitazawa, H., Kojima, Y., Kokeyama, K., Komori, K., Kong, A.K.H., Kotake, K., Kozakai, C., Kozu, R., Kumar, R., Kume, J., Kuo, C., Kuo, H.-S., Kuroyanagi, S., Kusayanagi, K., Kwak, K., Lee, H.K., Lee, H.W., Lee, R., Leonardi, M., Lin, L.C.-C., Lin, C.-Y., Lin, F.-L., Liu, G.C., Luo, L.-W., Marchio, M., Michimura, Y., Mio, N., Miyakawa, O., Miyamoto, A., Miyazaki, Y., Miyo, K., Miyoki, S., Morisaki, S., Moriwaki, Y., Musha, M., Nagano, K., Nagano, S., Nakamura, K., Nakano, H., Nakano, M., Nakashima, R., Narikawa, T., Negishi, R., Ni, W.-T., Nishizawa, A., Obuchi, Y., Ogaki, W., Oh, J.J., Oh, S.H., Ohashi, M., Ohishi, N., Ohkawa, M., Ohmae, N., Okutomi, K., Oohara, K., Ooi, C.P., Oshino, S., Pan, K.-C., Pang, H., Park, J., Peña Arellano, F.E., Pinto, I., Sago, N., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sakuno, Y., Sato, S., Sato, T., Sawada, T., Sekiguchi, T., Sekiguchi, Y., Shibagaki, S., Shimizu, R., Shimoda, T., Shimode, K., Shinkai, H., Shishido, T., Shoda, A., Somiya, K., Son, E.J., Sotani, H., Sugimoto, R., Suzuki, T., Suzuki, T., Tagoshi, H., Takahashi, H., Takahashi, R., Takamori, A., Takano, S., Takeda, H., Takeda, M., Tanaka, H., Tanaka, K., Tanaka, K., Tanaka, T., Tanaka, T., Tanioka, S., Tapia San Martin, E.N., Tatsumi, D., Telada, S., Tomaru, T., Tomigami, Y., Tomura, T., Travasso, F., Trozzo, L., Tsang, T., Tsubono, K., Tsuchida, S., Tsuzuki, T., Tuyenbayev, D., Uchikata, N., Uchiyama, T., Ueda, A., Uehara, T., Ueno, K., Ueshima, G., Uraguchi, F., Ushiba, T., van Putten, M.H.P.M., Vocca, H., Wang, J., Wu, C., Wu, H., Wu, S., Xu, W.-R., Yamada, T., Yamamoto, K., Yamamoto, K., Yamamoto, T., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoshioka, T., Yuzurihara, H., Zeidler, S., Zhao, Y., Zhu, Z.-H.

      Classical and Quantum Gravity37 ( 3 ) 035004 - 035004   2020

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:IOP PUBLISHING LTD  

      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.

      DOI: 10.1088/1361-6382/ab5c95

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    • KAGRA: 2.5 generation interferometric gravitational wave detector Peer-reviewed

      Akutsu, T., Ando, M., Arai, K., Arai, Y., Araki, S., Araya, A., Aritomi, N., Asada, H., Aso, Y., Atsuta, S., Awai, K., Bae, S., Baiotti, L., Barton, M.A., Cannon, K., Capocasa, E., Chen, C.-S., Chiu, T.-W., Cho, K., Chu, Y.-K., Craig, K., Creus, W., Doi, K., Eda, K., Enomoto, Y., Flaminio, R., Fujii, Y., Fujimoto, M.-K., Fukunaga, M., Fukushima, M., Furuhata, T., Haino, S., Hasegawa, K., Hashino, K., Hayama, K., Hirobayashi, S., Hirose, E., Hsieh, B.H., Huang, C.-Z., Ikenoue, B., Inoue, Y., Ioka, K., Itoh, Y., Izumi, K., Kaji, T., Kajita, T., Kakizaki, M., Kamiizumi, M., Kanbara, S., Kanda, N., Kanemura, S., Kaneyama, M., Kang, G., Kasuya, J., Kataoka, Y., Kawai, N., Kawamura, S., Kawasaki, T., Kim, C., Kim, J., Kim, J.C., Kim, W.S., Kim, Y.-M., Kimura, N., Kinugawa, T., Kirii, S., Kitaoka, Y., Kitazawa, H., Kojima, Y., Kokeyama, K., Komori, K., Kong, A.K.H., Kotake, K., Kozu, R., Kumar, R., Kuo, H.-S., Kuroyanagi, S., Lee, H.K., Lee, H.M., Lee, H.W., Leonardi, M., Lin, C.-Y., Lin, F.-L., Liu, G.C., Liu, Y., Majorana, E., Mano, S., Marchio, M., Matsui, T., Matsushima, F., Michimura, Y., Mio, N., Miyakawa, O., Miyamoto, A., Miyamoto, T., Miyo, K., Miyoki, S., Morii, W., Morisaki, S., Moriwaki, Y., Morozumi, T., Musha, M., Nagano, K., Nagano, S., Nakamura, K., Nakamura, T., Nakano, H., Nakano, M., Nakao, K., Narikawa, T., Naticchioni, L., Quynh, L.N., Ni, W.-T., Nishizawa, A., Obuchi, Y., Ochi, T., Oh, J.J., Oh, S.H., Ohashi, M., Ohishi, N., Ohkawa, M., Okutomi, K., Ono, K., Oohara, K., Ooi, C.P., Pan, S.-S., Park, J., Arellano, F.E.P., Pinto, I., Sago, N., Saijo, M., Saitou, S., Saito, Y., Sakai, K., Sakai, Y., Sakai, Y., Sasai, M., Sasaki, M., Sasaki, Y., Sato, S., Sato, N., Sato, T., Sekiguchi, Y., Seto, N., Shibata, M., Shimoda, T., Shinkai, H., Shishido, T., Shoda, A., Somiya, K., Son, E.J., Suemasa, A., Suzuki, T., Suzuki, T., Tagoshi, H., Tahara, H., Takahashi, H., Takahashi, R., Takamori, A., Takeda, H., Tanaka, H., Tanaka, K., Tanaka, T., Tanioka, S., Martin, E.N.T.S., Tatsumi, D., Tomaru, T., Tomura, T., Travasso, F., Tsubono, K., Tsuchida, S., Uchikata, N., Uchiyama, T., Uehara, T., Ueki, S., Ueno, K., Uraguchi, F., Ushiba, T., van Putten, M.H.P.M., Vocca, H., Wada, S., Wakamatsu, T., Watanabe, Y., Xu, W.-R., Yamada, T., Yamamoto, A., Yamamoto, K., Yamamoto, K., Yamamoto, S., Yamamoto, T., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoon, T.H., Yoshioka, T., Yuzurihara, H., Zeidler, S., Zhu, Z.-H.

      Nature Astronomy3 ( 1 ) 35 - 40   2019

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:NATURE PUBLISHING GROUP  

      The recent detections of gravitational waves (GWs) reported by the LIGO and Virgo collaborations have made a significant impact on physics and astronomy. A global network of GW detectors will play a key role in uncovering the unknown nature of the sources in coordinated observations with astronomical telescopes and detectors. Here we introduce KAGRA, a new GW detector with two 3 km baseline arms arranged in an 'L' shape. KAGRA's design is similar to the second generations of Advanced LIGO and Advanced Virgo, but it will be operating at cryogenic temperatures with sapphire mirrors. This low-temperature feature is advantageous for improving the sensitivity around 100 Hz and is considered to be an important feature for the third-generation GW detector concept (for example, the Einstein Telescope of Europe or the Cosmic Explorer of the United States). Hence, KAGRA is often called a 2.5-generation GW detector based on laser interferometry. KAGRA's first observation run is scheduled in late 2019, aiming to join the third observation run of the advanced LIGO-Virgo network. When operating along with the existing GW detectors, KAGRA will be helpful in locating GW sources more accurately and determining the source parameters with higher precision, providing information for follow-up observations of GW trigger candidates.

      DOI: 10.1038/s41550-018-0658-y

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    • Vibration isolation system with a compact damping system for power recycling mirrors of KAGRA Peer-reviewed

      Akiyama, Y., Akutsu, T., Ando, M., Arai, K., Arai, Y., Araki, S., Araya, A., Aritomi, N., Asada, H., Aso, Y., Bae, S., Baiotti, L., Barton, M.A., Cannon, K., Capocasa, E., Chen, C.-S., Chiu, T.-W., Cho, K., Chu, Y.-K., Craig, K., Dattilo, V., Doi, K., Enomoto, Y., Flaminio, R., Fujii, Y., Fujimoto, M.-K., Fukunaga, M., Fukushima, M., Furuhata, T., Haino, S., Hasegawa, K., Hashimoto, Y., Hashino, K., Hayama, K., Hirayama, T., Hirose, E., Hsieh, B.H., Huang, C.-Z., Ikenoue, B., Inoue, Y., Ioka, K., Itoh, Y., Izumi, K., Kaji, T., Kajita, T., Kakizaki, M., Kamiizumi, M., Kanbara, S., Kanda, N., Kanemura, S., Kang, G., Kasuya, J., Kawai, N., Kawasaki, T., Kim, C., Kim, W.S., Kim, J., Kim, J.C., Kimura, N., Kirii, S., Kitaoka, Y., Kitazawa, H., Kojima, Y., Kokeyama, K., Komori, K., Kong, A., Kotake, K., Kozu, R., Kumar, R., Kuo, H.-S., Kuroki, S., Kuroyanagi, S., Lee, H.K., Lee, H.M., Lee, H.W., Leonardi, M., Lin, C.-Y., Lin, F.-L., Liu, G.C., Marchio, M., Matsui, T., Michimura, Y., Mio, N., Miyakawa, O., Miyamoto, A., Miyoki, S., Morii, W., Morisaki, S., Moriwaki, Y., Musha, M., Nagano, S., Nagano, K., Nakamura, K., Nakamura, T., Nakano, H., Nakano, M., Narikawa, T., Nguyen Quynh, L., Ni, W.-T., Nishizawa, A., Obuchi, Y., Oh, J., Oh, S.H., Ohashi, M., Ohishi, N., Ohkawa, M., Okutomi, K., Ono, K., Oohara, K., Ooi, C.P., Pan, S.-S., Paoletti, F., Park, J., Passaquieti, R., Pena Arellano, F.E., Sago, N., Saito, S., Saito, Y., Sakai, K., Sakai, Y., Sasai, M., Sato, S., Sato, T., Sekiguchi, T., Sekiguchi, Y., Shibata, M., Shimoda, T., Shinkai, H., Shishido, T., Shoda, A., Someya, N., Somiya, K., Son, E.J., Suemasa, A., Suzuki, T., Suzuki, T., Tagoshi, H., Tahara, H., Takahashi, H., Takahashi, R., Takeda, H., Tanaka, H., Tanaka, K., Tanaka, T., Tanioka, S., Tapia San Martin, E.N., Tomaru, T., Tomura, T., Travasso, F., Tsubono, K., Tsuchida, S., Uchikata, N., Uchiyama, T., Uehara, T., Ueno, K., Uraguchi, F., Ushiba, T., Van Putten, M.H.P.M., Vocca, H., Wakamatsu, T., Watanabe, Y., Xu, W.-R., Yamada, T., Yamamoto, K., Yamamoto, K., Yamamoto, S., Yamamoto, T., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoshioka, T., Yuzurihara, H., Zeidler, S., Zhu, Z.-H.

      Classical and Quantum Gravity36 ( 9 ) 095015 - 095015   2019

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      Publishing type:Research paper (scientific journal)   Publisher:IOP Publishing  

      DOI: 10.1088/1361-6382/ab0fcb

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    • Measuring scattering light distributions on high-absorptive surfaces for stray-light reduction in gravitational-wave detectors Peer-reviewed

      Zeidler, S., Akutsu, T., Torii, Y., Aso, Y.

      Optics Express27 ( 12 )   2019

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      Language:English   Publishing type:Research paper (scientific journal)  

      DOI: 10.1364/OE.27.016890

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    • First cryogenic test operation of underground km-scale gravitational-wave observatory KAGRA Peer-reviewed

      Akutsu, T., Ando, M., Arai, K., Arai, Y., Araki, S., Araya, A., Aritomi, N., Asada, H., Aso, Y., Atsuta, S., Awai, K., Bae, S., Baiotti, L., Barton, M.A., Cannon, K., Capocasa, E., Chen, C.-S., Chiu, T.-W., Cho, K., Chu, Y.-K., Craig, K., Creus, W., Doi, K., Eda, K., Enomoto, Y., Flaminio, R., Fujii, Y., Fujimoto, M.-K., Fukunaga, M., Fukushima, M., Furuhata, T., Hagiwara, A., Haino, S., Hasegawa, K., Hashino, K., Hayama, K., Hirobayashi, S., Hirose, E., Hsieh, B.H., Huang, C.-Z., Ikenoue, B., Inoue, Y., Ioka, K., Itoh, Y., Izumi, K., Kaji, T., Kajita, T., Kakizaki, M., Kamiizumi, M., Kanbara, S., Kanda, N., Kanemura, S., Kaneyama, M., Kang, G., Kasuya, J., Kataoka, Y., Kawai, N., Kawamura, S., Kawasaki, T., Kim, C., Kim, J., Kim, J.C., Kim, W.S., Kim, Y.-M., Kimura, N., Kinugawa, T., Kirii, S., Kitaoka, Y., Kitazawa, H., Kojima, Y., Kokeyama, K., Komori, K., Kong, A.K.H., Kotake, K., Kozu, R., Kumar, R., Kuo, H.-S., Kuroyanagi, S., Lee, H.K., Lee, H.M., Lee, H.W., Leonardi, M., Lin, C.-Y., Lin, F.-L., Liu, G.C., Liu, Y., Majorana, E., Mano, S., Marchio, M., Matsui, T., Matsushima, F., Michimura, Y., Mio, N., Miyakawa, O., Miyamoto, A., Miyamoto, T., Miyo, K., Miyoki, S., Morii, W., Morisaki, S., Moriwaki, Y., Morozumi, T., Murakami, I., Musha, M., Nagano, K., Nagano, S., Nakamura, K., Nakamura, T., Nakano, H., Nakano, M., Nakao, K., Namai, Y., Narikawa, T., Naticchioni, L., Nguyen Quynh, L., Ni, W.-T., Nishizawa, A., Obuchi, Y., Ochi, T., Oh, J.J., Oh, S.H., Ohashi, M., Ohishi, N., Ohkawa, M., Okutomi, K., Ono, K., Oohara, K., Ooi, C.P., Pan, S.-S., Park, J., Pena Arellano, F.E., Pinto, I., Sago, N., Saijo, M., Saito, Y., Saitou, S., Sakai, K., Sakai, Y., Sakai, Y., Sasai, M., Sasaki, M., Sasaki, Y., Sato, N., Sato, S., Sato, T., Sekiguchi, Y., Seto, N., Shibata, M., Shimoda, T., Shinkai, H., Shishido, T., Shoda, A., Somiya, K., Son, E.J., Suemasa, A., Suzuki, T., Suzuki, T., Tagoshi, H., Tahara, H., Takahashi, H., Takahashi, R., Takamori, A., Takeda, H., Tanaka, H., Tanaka, K., Tanaka, T., Tanioka, S., Tapia San Martin, E.N., Tatsumi, D., Terashima, S., Tomaru, T., Tomura, T., Travasso, F., Tsubono, K., Tsuchida, S., Uchikata, N., Uchiyama, T., Ueda, A., Uehara, T., Ueki, S., Ueno, K., Uraguchi, F., Ushiba, T., Van Putten, M.H.P.M., Vocca, H., Wada, S., Wakamatsu, T., Watanabe, Y., Xu, W.-R., Yamada, T., Yamamoto, A., Yamamoto, K., Yamamoto, K., Yamamoto, S., Yamamoto, T., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoon, T.H., Yoshioka, T., Yuzurihara, H., Zeidler, S., Zhu, Z.-H.

      Classical and Quantum Gravity36 ( 16 ) 165008 - 165008   2019

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      Publishing type:Research paper (scientific journal)   Publisher:IOP Publishing  

      DOI: 10.1088/1361-6382/ab28a9

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    • Construction of KAGRA: An underground gravitational-wave observatory Peer-reviewed

      Akutsu, T., Ando, M., Araki, S., Araya, A., Arima, T., Aritomi, N., Asada, H., Aso, Y., Atsuta, S., Awai, K., Baiotti, L., Barton, M.A., Chen, D., Cho, K., Craig, K., DeSalvo, R., Doi, K., Eda, K., Enomoto, Y., Flaminio, R., Fujibayashi, S., Fujii, Y., Fujimoto, M.-K., Fukushima, M., Furuhata, T., Hagiwara, A., Haino, S., Harita, S., Hasegawa, K., Hasegawa, M., Hashino, K., Hayama, K., Hirata, N., Hirose, E., Ikenoue, B., Inoue, Y., Ioka, K., Ishizaki, H., Itoh, Y., Jia, D., Kagawa, T., Kaji, T., Kajita, T., Kakizaki, M., Kakuhata, H., Kamiizumi, M., Kanbara, S., Kanda, N., Kanemura, S., Kaneyama, M., Kasuya, J., Kataoka, Y., Kawaguchi, K., Kawai, N., Kawamura, S., Kawazoe, F., Kim, C., Kim, J., Kim, J.C., Kim, W., Kimura, N., Kitaoka, Y., Kobayashi, K., Kojima, Y., Kokeyama, K., Komori, K., Kotake, K., Kubo, K., Kumar, R., Kume, T., Kuroda, K., Kuwahara, Y., Lee, H.-K., Lee, H.-W., Lin, C.-Y., Liu, Y., Majorana, E., Mano, S., Marchio, M., Matsui, T., Matsumoto, N., Matsushima, F., Michimura, Y., Mio, N., Miyakawa, O., Miyake, K., Miyamoto, A., Miyamoto, T., Miyo, K., Miyoki, S., Morii, W., Morisaki, S., Moriwaki, Y., Muraki, Y., Murakoshi, M., Musha, M., Nagano, K., Nagano, S., Nakamura, K., Nakamura, T., Nakano, H., Nakano, M., Nakano, M., Nakao, H., Nakao, K., Narikawa, T., Ni, W.-T., Nonomura, T., Obuchi, Y., Oh, J.J., Oh, S.-H., Ohashi, M., Ohishi, N., Ohkawa, M., Ohmae, N., Okino, K., Okutomi, K., Ono, K., Ono, Y., Oohara, K., Ota, S., Park, J., Peña Arellano, F.E., Pinto, I.M., Principe, M., Sago, N., Saijo, M., Saito, T., Saito, Y., Saitou, S., Sakai, K., Sakakibara, Y., Sasaki, Y., Sato, S., Sato, T., Sato, Y., Sekiguchi, T., Sekiguchi, Y., Shibata, M., Shiga, K., Shikano, Y., Shimoda, T., Shinkai, H., Shoda, A., Someya, N., Somiya, K., Son, E.J., Starecki, T., Suemasa, A., Sugimoto, Y., Susa, Y., Suwabe, H., Suzuki, T., Tachibana, Y., Tagoshi, H., Takada, S., Takahashi, H., Takahashi, R., Takamori, A., Takeda, H., Tanaka, H., Tanaka, K., Tanaka, T., Tatsumi, D., Telada, S., Tomaru, T., Tsubono, K., Tsuchida, S., Tsukada, L., Tsuzuki, T., Uchikata, N., Uchiyama, T., Uehara, T., Ueki, S., Ueno, K., Uraguchi, F., Ushiba, T., Van Putten, M.H.P.M., Wada, S., Wakamatsu, T., Yaginuma, T., Yamamoto, K., Yamamoto, S., Yamamoto, T., Yano, K., Yokoyama, J., Yokozawa, T., Yoon, T.H., Yuzurihara, H., Zeidler, S., Zhao, Y., Zheng, L., Agatsuma, K., Akiyama, Y., Arai, N., Asano, M., Bertolini, A., Fujisawa, M., Goetz, R., Guscott, J., Hashimoto, Y., Hayashida, Y., Hennes, E., Hirai, K., Hirayama, T., Ishitsuka, H., Kato, J., Khalaidovski, A., Koike, S., Kumeta, A., Miener, T., Morioka, M., Mueller, C.L., Narita, T., Oda, Y., Ogawa, T., Sekiguchi, T., Tamura, H., Tanner, D.B., Tokoku, C., Toritani, M., Utsuki, T., Uyeshima, M., Van Den Brand, J.F.J., Van Heijningen, J.V., Yamaguchi, S., Yanagida, A.

      Progress of Theoretical and Experimental Physics2018 ( 1 )   2018

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      Language:English   Publishing type:Research paper (scientific journal)  

      DOI: 10.1093/ptep/ptx180

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    • Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA International journal

      Abbott, B.P., Abbott, R., Abbott, T.D., Abernathy, M.R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R.X., Adya, V.B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O.D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Allen, B., Allocca, A., Altin, P.A., Ananyeva, A., Anderson, S.B., Anderson, W.G., Ando, M., Appert, S., Arai, K., Araya, A., Araya, M.C., Areeda, J.S., Arnaud, N., Arun, K.G., Asada, H., Ascenzi, S., Ashton, G., Aso, Y., Ast, M., Aston, S.M., Astone, P., Atsuta, S., Aufmuth, P., Aulbert, C., Avila-Alvarez, A., Awai, K., Babak, S., Bacon, P., Bader, M.K.M., Baiotti, L., Baker, P.T., Baldaccini, F., Ballardin, G., Ballmer, S.W., Barayoga, J.C., Barclay, S.E., Barish, B.C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M.A., Bartos, I., Bassiri, R., Basti, A., Batch, J.C., Baune, C., Bavigadda, V., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Belgin, M., Bell, 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D’Antonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C.F., Dattilo, V., Dave, I., Davier, M., Davies, G.S., Davis, D., Daw, E.J., Day, B., Day, R., De, S., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dergachev, V., De Rosa, R., DeRosa, R.T., DeSalvo, R., Devine, R.C., Dhurandhar, S., Díaz, M.C., Fiore, L.D., Giovanni, M.D., Girolamo, T.D., Lieto, A.D., Pace, S.D., Palma, I.D., Virgilio, A.D., Doctor, Z., Doi, K., Dolique, V., Donovan, F., Dooley, K.L., Doravari, S., Dorrington, I., Douglas, R., Dovale Álvarez, M., Downes, T.P., Drago, M., Drever, R.W.P., Driggers, J.C., Du, Z., Ducrot, M., Dwyer, S.E., Eda, K., Edo, T.B., Edwards, M.C., Effler, A., Eggenstein, H.-B., Ehrens, P., Eichholz, J., Eikenberry, S.S., Eisenstein, R.A., Essick, R.C., Etienne, Z., Etzel, T., Evans, M., Evans, T.M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W.M., Fauchon-Jones, 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Kakizaki, M., Kalaghatgi, C.V., Kalogera, V., Kamiizumi, M., Kanda, N., Kandhasamy, S., Kanemura, S., Kaneyama, M., Kang, G., Kanner, J.B., Karki, S., Karvinen, K.S., Kasprzack, M., Kataoka, Y., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawai, N., Kawamura, S., Kéfélian, F., Keitel, D., Kelley, D.B., Kennedy, R., Key, J.S., Khalili, F.Y., Khan, I., Khan, S., Khan, Z., Khazanov, E.A., Kijbunchoo, N., Kim, C., Kim, H., Kim, J.C., Kim, J., Kim, W., Kim, Y.-M., Kimbrell, S.J., Kimura, N., King, E.J., King, P.J., Kirchhoff, R., Kissel, J.S., Klein, B., Kleybolte, L., Klimenko, S., Koch, P., Koehlenbeck, S.M., Kojima, Y., Kokeyama, K., Koley, S., Komori, K., Kondrashov, V., Kontos, A., Korobko, M., Korth, W.Z., Kotake, K., Kowalska, I., Kozak, D.B., Krämer, C., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, R., Kuo, L., Kuroda, K., Kutynia, A., Kuwahara, Y., Lackey, B.D., Landry, M., Lang, R.N., Lange, J., Lantz, B., Lanza, R.K., 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      Living Reviews in Relativity21 ( 1 ) 3 - 3   2018

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      Language:English   Publishing type:Research paper (scientific journal)  

      We present possible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next decade, with the intention of providing information to the astronomy community to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals, and study the capability of the network to determine the sky location of the source. We report our findings for gravitational-wave transients, with particular focus on gravitational-wave signals from the inspiral of binary neutron star systems, which are the most promising targets for multi-messenger astronomy. The ability to localize the sources of the detected signals depends on the geographical distribution of the detectors and their relative sensitivity, and [Formula: see text] credible regions can be as large as thousands of square degrees when only two sensitive detectors are operational. Determining the sky position of a significant fraction of detected signals to areas of 5-[Formula: see text] requires at least three detectors of sensitivity within a factor of [Formula: see text] of each other and with a broad frequency bandwidth. When all detectors, including KAGRA and the third LIGO detector in India, reach design sensitivity, a significant fraction of gravitational-wave signals will be localized to a few square degrees by gravitational-wave observations alone.

      DOI: 10.1007/s41114-018-0012-9

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    • Absorption and scattering by interstellar dust in the silicon K-edge of GX 5-1 Peer-reviewed

      Zeegers, S.T., Costantini, E., De Vries, C.P., Tielens, A.G.G.M., Chihara, H., De Groot, F., Mutschke, H., Waters, L.B.F.M., Zeidler, S.

      Astronomy and Astrophysics599   2017

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:EDP SCIENCES S A  

      Context. We study the absorption and scattering of X-ray radiation by interstellar dust particles, which allows us to access the physical and chemical properties of dust. The interstellar dust composition is not well understood, especially on the densest sight lines of the Galactic plane. X-rays provide a powerful tool in this study.
      Aims. We present newly acquired laboratory measurements of silicate compounds taken at the Soleil synchrotron facility in Paris using the Lucia beamline. The dust absorption profiles resulting from this campaign were used in this pilot study to model the absorption by interstellar dust along the line of sight of the low-mass X-ray binary GX 5-1.
      Methods. The measured laboratory cross-sections were adapted for astrophysical data analysis and the resulting extinction profiles of the Si K-edge were implemented in the SPEX spectral fitting program. We derive the properties of the interstellar dust along the line of sight by fitting the Si K-edge seen in absorption in the spectrum of GX 5-1.
      Results. We measured the hydrogen column density towards GX 5-1 to be 3.40 +/- 0 : 1 x 10(22) cm(-2). The best fit of the silicon edge in the spectrum of GX 5-1 is obtained by a mixture of olivine and pyroxene. In this study, our modeling is limited to Si absorption by silicates with different Mg:Fe ratios. We obtained an abundance of silicon in dust of 4.0 +/- 0.3 x 10(-5) per H atom and a lower limit for total abundance, considering both gas and dust of &gt;4.4 x 10(-5) per H atom, which leads to a gas to dust ratio of &gt;0.22. Furthermore, an enhanced scattering feature in the Si K-edge may suggest the presence of large particles along the line of sight.

      DOI: 10.1051/0004-6361/201628507

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    • Calculation method for light scattering caused by multilayer coated mirrors in gravitational wave detectors Peer-reviewed

      Zeidler, S., Akutsu, T., Torii, Y., Hirose, E., Aso, Y., Flaminio, R.

      Optics Express25 ( 5 ) 4741 - 4760   2017

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OPTICAL SOC AMER  

      Scattered light in inteferometric gravitational wave detectors needs to be reduced so that it will not harm the actual signals coming from a gravitational wave. In this paper, we report on the application of the theory of light scattering from mirrors in interferometric detectors having multilayer coatings on their surfaces and compared the results with single-surface scattering theories, which are traditionally used in the field of gravitational wave detectors. For the first time in this field, we have calculated the scattering distributions of the power-recycling, the signal-recycling, and the beam-splitter mirrors in KAGRA (a cryogenic interferometric gravitational wave detector currently under construction in the Kamioka mine in Japan) by using models of their multilayer coatings. Furthermore, we have performed simulations to show the differences between multilayer scattering and single-surface scattering models in the back-scattering of mechanical structures close to the mirrors and the impact on the sensitivity of the KAGRA detector. We show that the back-scattering by using those coatings can be larger by up to almost two orders of magnitude and they also give rise to additional scattering features that should be taken into account for all optical applications in gravitational wave detectors. (C) 2017 Optical Society of America

      DOI: 10.1364/OE.25.004741

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    • Prospects for Observing and Localizing Gravitational-Wave Transients with Advanced LIGO and Advanced Virgo Peer-reviewed

      Simon Zeidler

      Living Reviews in Relativity   12 2016

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      Language:English   Publishing type:Research paper (scientific journal)  

      DOI: 10.1007/lrr-2016-1

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    • Vacuum and cryogenic compatible black surface for large optical baffles in advanced gravitational-wave telescopes Peer-reviewed

      Tomotada Akutsu, Yoshio Saito, Yusuke Sakakibara, Yoshihiro Sato, Yoshito Niwa, Nobuhiro Kimura, Toshikazu Suzuki, Kazuhiro Yamamoto, Chihiro Tokoku, Shigeaki Koike, Dan Chen, Simon Zeidler, Kouichi Ikeyama, Yusuke Ariyama

      OPTICAL MATERIALS EXPRESS6 ( 5 ) 1613 - 1626   5 2016

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:OPTICAL SOC AMER  

      This paper reports on the optical properties, outgassing rate, and cryogenic performance of surface finishing we have adopted for large optical baffles absorbing stray light in KAGRA, an advanced interferometer for detecting gravitational waves. The surface finishing is based on an electroless nickel-phosphorus-tungsten (NiPW) plating, applicable to large surface area up to similar to 800 mm in diameter, and achieves less than 3% total reflectance against a light beam at 1064 nm with a reasonable scattering distribution similar to 0.05/sr. The outgassing rate from the black coating meets our requirements of 3 x 10 Pa-7.m(3) s (1)m (2). The black coating can tolerate low temperature down to 12 K, and can be installed close to cold mirrors indispensable for the future interferometers. (C) 2016 Optical Society of America

      DOI: 10.1364/OME.6.001613

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    • Temperature-dependent infrared optical constants of olivine and enstatite Peer-reviewed

      S. Zeidler, H. Mutschke, Th Posch

      Astrophysical Journal798 ( 2 )   10 1 2015

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:Institute of Physics Publishing  

      Since the Infrared Space Observatory (ISO) mission, it has become clear that dust in circumstellar disks and outflows consists partly of crystalline silicates of pyroxene and olivine type. An exact mineralogical analysis of the dust infrared emission spectra relies on laboratory spectra, which, however, have been mostly measured at room temperature so far. Given that infrared spectral features depend on the thermal excitation of the crystal's vibrational modes, laboratory spectra measured at various (low and high) temperatures, corresponding to the thermal conditions at different distances from the star, can improve the accuracy of such analyses considerably. We have measured the complex refractive index in a temperature range of 10-973 K for one mineral of each of those types of silicate, i.e., for an olivine and an enstatite of typical (terrestrial) composition. Thus, our data extend the temperature range of previous data to higher values and the compositional range to higher iron contents. We analyze the temperature dependence of oscillator frequencies and damping parameters governing the spectral characteristics of the bands and calculate absorption cross-sectional spectra that can be compared with astronomical emission spectra. We demonstrate the usefulness of our new data by comparing spectra calculated for a 100 K dust temperature with the ISO SWS spectrum of IRAS 09425-6040.

      DOI: 10.1088/0004-637X/798/2/125

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    • Mg-Al Oxides and the Remarkable Temperature Dependence of their 13 mu m and 32 mu m Emission Bands Peer-reviewed

      S. Zeidler, H. Mutschke, Th Posch

      WHY GALAXIES CARE ABOUT AGB STARS III: A CLOSER LOOK IN SPACE AND TIME497   409 - 410   2015

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher:ASTRONOMICAL SOC PACIFIC  

      We present the temperature-dependent (10-928 K) infrared spectra of corundum and spinel, two refractory solids which occur in the stellar outflows of oxygen-rich AGB stars. From our measurements, we were able to calculate the temperature dependent optical constants by oscillator fits. These new data are useful to further constrain the still poorly understood features of oxide dust around AGB stars, especially the 13 mu m and 32 mu m emission bands. For the latter, spinel continues to be the most promising carrier.

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    • IR Optical Constants of Olivine and Enstatite from 10 K to 928 K Peer-reviewed

      S. Zeidler, H. Mutschke, Th Posch

      WHY GALAXIES CARE ABOUT AGB STARS III: A CLOSER LOOK IN SPACE AND TIME497   407 - 408   2015

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher:ASTRONOMICAL SOC PACIFIC  

      Infrared emission spectra of dust produced by AGB stars are influenced by the temperature of the dust. However, optical data for dust at high temperatures, which can be used for comparison, are rare. Here, we present some results of reflection measurements on olivine and enstatite crystals (two abundant components in circumstellar dust) and subsequent calculations of the complex index of refraction.

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    • TEMPERATURE-DEPENDENT INFRARED OPTICAL CONSTANTS OF OLIVINE AND ENSTATITE Peer-reviewed

      S. Zeidler, H. Mutschke, Th. Posch

      ASTROPHYSICAL JOURNAL798 ( 2 )   1 2015

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:IOP PUBLISHING LTD  

      Since the Infrared Space Observatory (ISO) mission, it has become clear that dust in circumstellar disks and outflows consists partly of crystalline silicates of pyroxene and olivine type. An exact mineralogical analysis of the dust infrared emission spectra relies on laboratory spectra, which, however, have been mostly measured at room temperature so far. Given that infrared spectral features depend on the thermal excitation of the crystal's vibrational modes, laboratory spectra measured at various (low and high) temperatures, corresponding to the thermal conditions at different distances from the star, can improve the accuracy of such analyses considerably. We have measured the complex refractive index in a temperature range of 10-973 K for one mineral of each of those types of silicate, i.e., for an olivine and an enstatite of typical (terrestrial) composition. Thus, our data extend the temperature range of previous data to higher values and the compositional range to higher iron contents. We analyze the temperature dependence of oscillator frequencies and damping parameters governing the spectral characteristics of the bands and calculate absorption cross-sectional spectra that can be compared with astronomical emission spectra. We demonstrate the usefulness of our new data by comparing spectra calculated for a 100 K dust temperature with the ISO SWS spectrum of IRAS 09425-6040.

      DOI: 10.1088/0004-637X/798/2/125

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    • Optical constants of refractory oxides at high temperatures Peer-reviewed

      Astronomy & Astrophysics   5 2013

    • HIGH-TEMPERATURE OPTICAL CONSTANTS OF DUST ANALOGUES FOR THE SOLAR NEBULA Peer-reviewed

      S. Zeidler

      ECLA: EUROPEAN CONFERENCE ON LABORATORY ASTROPHYSICS58   409 - 413   2013

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher:E D P SCIENCES  

      The dust in protoplanetary disks is influenced by many different processes. Among others, heating processes are the most important ones: they change not only the physical and chemical properties of dust particles, but also their emission spectra. In order to compare observed infrared spectra of young stellar systems with laboratory data of hot (up to 655 degrees C) circumstellar dust analogues, we investigate materials, which are important constituents of dust in protoplanetary disks. We calculated the optical constants by means of a simple Lorentzian oscillator fit and applied them to simulations of small-particle emission spectra in order to compare our results with real astronomical spectra of AGB-stars and protoplanetary disks.

      DOI: 10.1051/eas/1258070

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    • Far-infrared continuum absorption of olivine at low temperatures Peer-reviewed

      H. Mutschke, S. Zeidler, H. Chihara

      Earth, Planets and Space65 ( 10 ) 1139 - 1143   2013

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher:Springer Berlin  

      The far-infrared continuum opacity of cold dust is an important quantity for the study of debris disks in planetary systems and of protoplanetary disks. Olivine is considered the most abundant crystalline dust species in such environments. We present spectroscopic absorption measurements on olivine plates of the order of a millimeter thickness at wavelengths between 60 and 400 μm for temperatures down to 10 K. Our data reveal a strong temperature dependence of the continuum absorption coefficient, i.e. more than an order of magnitude decrease at 100 μm for 10 K compared to room temperature. The absolute values are generally much lower than those measured with olivine powders embedded into polyethylene pellets, even if the difference between plate and powder samples is taken into account by theoretical models. In contrast to this, the room temperature data are in relatively good agreement with simulations using optical constants determined from reflection measurements. At low temperatures, the absorption coefficient of olivine was measurable with sufficient accuracy only up to 90 μm for 10 K and up to 110 μm for 100 K. These data reveal a drastic change in the spectral slope (from β ∼ 2.0 to β &gt
      5.0) for the continuum underlying the 69-μm band, which is not predicted by the low-temperature optical constants determined for forsterite. © The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS)
      .

      DOI: 10.5047/eps.2013.07.003

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    • Near-infrared absorption properties of oxygen-rich stardust analogs The influence of coloring metal ions Peer-reviewed

      S. Zeidler, T. Posch, H. Mutschke, H. Richter, O. Wehrhan

      ASTRONOMY & ASTROPHYSICS526   2 2011

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:EDP SCIENCES S A  

      Context. Several astrophysically relevant solid oxides and silicates have extremely small opacities in the visual and near-infrared in their pure forms. Datasets for the opacities and for the imaginary part k of their complex indices of refraction are hardly available in these wavelength ranges.
      Aims. We aimed at determining k for spinel, rutile, anatase, and olivine, especially in the near-infrared region. Our measurements were made with impurity-containing, natural, and synthetic stardust analogs.
      Methods. Two experimental methods were used: preparing small sections of natural minerals and synthesizing melt droplets under the electric arc furnace. In both cases, the aborption properties of the samples were measured by transmission spectroscopy.
      Results. For spinel (MgAl(2)O(4)), anatase, rutile (both TiO(2)), and olivine ((Mg,Fe)(2)SiO(4)), the optical constants have been extended to the visual and near-infrared. We highlight that the individual values of k(lambda) and the absorption cross section Q(abs)(lambda) depend strongly on the content in transition metals like iron. Based on our measurements, we infer that k values below 10(-5) are very rare in natural minerals including stardust grains, if they occur at all.
      Conclusions. Data for k and Q(abs)(lambda) are important for various physical properties of stardust grains such as temperature and radiation pressure. With increasing Q(abs)(lambda) due to impurities, the equilibrium temperature of small grains in circumstellar shells increases as well. We discuss why and to what extent this is the case.

      DOI: 10.1051/0004-6361/201015219

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    • Recent Results of Solid-State Spectroscopy Peer-reviewed

      Cornelia Jaeger, Thomas Posch, Harald Mutschke, Simon Zeidler, Akemi Tamanai, Bernard L. de Vries

      MOLECULAR UNIVERSE ( 280 ) 416 - 430   2011

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      Language:English   Publishing type:Research paper (international conference proceedings)   Publisher:CAMBRIDGE UNIV PRESS  

      Solid state spectroscopy continues to be an important source of information on the mineralogical composition and physical properties of dust grains both in space and on planetary surfaces. With only a few exceptions, artificially produced or natural terrestrial analog materials, rather than 'real' cosmic dust grains, are the subject of solid state astrophysics. The Jena laboratory has provided a large number of data sets characterizing the UV, optical and infrared properties of such cosmic dust analogs. The present paper highlights recent developments and results achieved in this context, focussing on 'non-standard conditions' such as very low temperatures, very high temperatures and very long wavelengths.

      DOI: 10.1017/S1743921311025166

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    • Far-infrared spectra of hydrous silicates at low temperatures Providing laboratory data for Herschel and ALMA Peer-reviewed

      H. Mutschke, S. Zeidler, Th. Posch, F. Kerschbaum, A. Baier, Th. Henning

      ASTRONOMY & ASTROPHYSICS492 ( 1 ) 117 - 125   12 2008

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      Language:English   Publishing type:Research paper (scientific journal)   Publisher:EDP SCIENCES S A  

      Context. Hydrous silicates occur in various cosmic environments, and are among the minerals with the most pronounced bands in the far infrared (FIR) spectral region. Given that Herschel and ALMA will open up new possibilities for astronomical FIR and sub-mm spectroscopy, data characterizing the dielectric properties of these materials at long wavelengths are desirable.
      Aims. We aimed at examining the FIR spectra of talc, picrolite, montmorillonite, and chamosite, which belong to four different groups of phyllosilicates. We tabulated positions and band widths of the FIR bands of these minerals depending on the dust temperature.
      Methods. By means of powder transmission spectroscopy, spectra of the examined materials were measured in the wavelength range 25-500 mu m at temperatures of 300, 200, 100, and 10K. Results. Room-temperature measurements yield the following results. For talc, a previously unknown band, centered at 98.5 mu m, was found, in addition to bands at 56.5 and 59.5 mu m. For montmorillonite, several bands at wavelengths &lt; 110 mu m were detected, including a band at 105 mu m with an FWHM of about 10 mu m. Picrolite shows a sharp 77 mu m FIR band. Chamosite is characterized by bands in the 72-92 mu m range, and a prominent band at 277 mu m. At decreasing temperature, most of the bands shift to shorter wavelengths.
      Conclusions. Examining a potential counterpart of the 105 mu m band in the spectra of HD 142527 and HD 100546, we find that the broad band in the spectra of these young stars-extending from 85 to 125 mu m-cannot be due to montmorillonite or any of the hydrous silicates we studied, since these materials have sharper bands in the FIR wavelength range than previously assumed, especially at low temperatures.

      DOI: 10.1051/0004-6361:200810312

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    Misc.

    • The status of KAGRA underground cryogenic gravitational wave telescope

      KAGRA Collaboration, T. Akutsu, M. Ando, A. Araya, N. Aritomi, H. Asada, Y. Aso, S. Atsuta, K. Awai, M. A. Barton, K. Cannon, K. Craig, W. Creus, K. Doi, K. Eda, Y. Enomoto, R. Flaminio, Y. Fujii, M. -K. Fujimoto, T. Furuhata, S. Haino, K. Hasegawa, K. Hashino, K. Hayama, S. Hirobayashi, E. Hirose, B. H. Hsieh, Y. Inoue, K. Ioka, Y. Itoh, T. Kaji, T. Kajita, M. Kakizaki, M. Kamiizumi, S. Kambara, N. Kanda, S. Kanemura, M. Kaneyama, G. Kang, J. Kasuya, Y. Kataoka, N. Kawai, S. Kawamura, C. Kim, H. Kim, J. Kim, Y. Kim, N. Kimura, T. Kinugawa, S. Kirii, Y. Kitaoka, Y. Kojima, K. Kokeyama, K. Komori, K. Kotake, R. Kumar, H. Lee, H. Lee, Y. Liu, N. Luca, E. Majorana, S. Mano, M. Marchio, T. Matsui, F. Matsushima, Y. Michimura, O. Miyakawa, T. Miyamoto, A. Miyamoto, K. Miyo, S. Miyoki, W. Morii, S. Morisaki, Y. Moriwaki, T. Morozumi, M. Musha, S. Nagano, K. Nagano, K. Nakamura, T. Nakamura, H. Nakano, M. Nakano, K. Nakao, T. Narikawa, L. Nguyen Quynh, W. -T. Ni, T. Ochi, J. Oh, S. Oh, M. Ohashi, N. Ohishi, M. Ohkawa, K. Okutomi, K. Oohara, F. E, Peña Alleano, I. Pinto, N. Sago, M. Saijo, Y. Saito, K. Sakai, Y. Sakai, Y. Sasaki, M. Sasaki, S. Sato, T. Sato, Y. Sekiguchi, N. Seto, M. Shibata, T. Shimoda, H. Shinkai, A. Shoda, K. Somiya, E. Son, A. Suemasa, T. Suzuki, T. Suzuki, H. Tagoshi, H. Takahashi, R. Takahashi, A. Takamori, H. Takeda, H. Tanaka, K. Tanaka, T. Tanaka, D. Tatsumi, T. Tomaru, T. Tomura, F. Travasso, K. Tsubono, S. Tsuchida, N. Uchikata, T. Uchiyama, T. Uehara, S. Ueki, K. Ueno, T. Ushiba, M. H, P. M. van Putten, H. Vocca, S. Wada, T. Wakamatsu, T. Yamada, S. Yamamoto, T. Yamamoto, K. Yamamoto, A. Yamamoto, J. Yokoyama, T. Yokozawa, T. H. Yoon, H. Yuzurihara, S. Zeidler, Z. -H. Zhu

          13 10 2017

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      Publishing type:Internal/External technical report, pre-print, etc.  

      KAGRA is a 3-km interferometric gravitational wave telescope located in the<br />
      Kamioka mine in Japan. It is the first km-class gravitational wave telescope<br />
      constructed underground to reduce seismic noise, and the first km-class<br />
      telescope to use cryogenic cooling of test masses to reduce thermal noise. The<br />
      construction of the infrastructure to house the interferometer in the tunnel,<br />
      and the initial phase operation of the interferometer with a simple 3-km<br />
      Michelson configuration have been completed. The first cryogenic operation is<br />
      expected in 2018, and the observing runs with a full interferometer are<br />
      expected in 2020s. The basic interferometer configuration and the current<br />
      status of KAGRA are described.

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    Teaching Experience

    • 4 2020 - Present 
      Physics Experiments 2 (Semiconductor) ( Rikkyo University )

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    • 4 2020 - Present 
      Basic Physics Experiments 1 ( Rikkyo University )

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    •  
      Experimental Physics ( Friedrich-Schiller University Jena )

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    Professional Memberships

    Research Projects

    • Novel Methods to Measure the Gravity Constant with the Aid of Laser-Interferometers

      Rikkyo University 

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      7 2020 - 7 2021

      Authorship:Principal investigator 

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    • High-Temperature Optical Constants of Dust Analogues for the Solar Nebula

      DFG - German Research Foundation  The First 1- Million Years of the Solar System 

      Simon Zeidler

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      1 2009 - 7 2013

      Authorship:Principal investigator  Grant type:Competitive

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    • Investigations on the Crystallization Behavior of Olivine Glasses

      JSPS - Japanese Society for the Promotion of Science  JSPS Summer Program 2009 

      Simon Zeidler

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      6 2009 - 8 2009

      Authorship:Principal investigator  Grant type:Competitive

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    • Far-Infrared Spectra of Hydrous Silicates at Low Temerature

      DFG - German Research Foundation  DFG Individual Grants Program 

      Simon Zeidler

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      2007 - 2008

      Authorship:Principal investigator  Grant type:Competitive

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