Proposal by the new members from Toyama university Fusakazu Matsushima and Yukinori Ono University of Toyama, Japan KAGRA face to face meeting,, Kashiwa, Feb. 14, 2013

in this talk 1. Overview University of Toyama History with KAGRA Members of colaboration: 4 groups 2. Inroduction to each group Laser: Matsushima et al. Signal analysis: Hirobayashi et al. Theory: Kakizaki Sapphire Mirror: Ono et al.

University of Toyama Faculty Science 82 staffs Engineering112 staffs Humanities Human Development Economics Art and Design Pharmacy Medicine many centers total903 staffs

1.Overview Ｌｏｃａｔｉｏｎ ｏｆ Ｔｏｙａｍａ Kamioka Toyama Tokyo Nagoya Kamioka – Toyama St. about 30km (about 40min. driving on Root 41) from city border: only few km

Root 41 : called as “Nobel road” Toyama Osawano Kamioka Takayama Nagoya 90km Root 41 K.Tanaka (chem.) S. Tonegawa (med.) M. Koshiba (phys.) H. Shirakawa (chem.) R. Noyori (chem.) O. Shimomura (chem.) M. Kobayashi (phys.) T. Masukawa (phys.) & more !

History of Toyama university and KAGRA about 10 years ago CLIO member (Prof. Ohashi et al) had a lecture. Students (Nagano, Hayakawa,..) work in this field Jan. KAGRA member (Prof. Kawamura et al.) had lectures July “Univ. of Toyama and KAGRA Group Joint workshop”. Campus mailing list “toyama-kagra” starts.

Univ. of Toyama and KAGRA Group Joint workshop July 7, 2012 in Toyama Many staffs in the faculties of science and engineering have much interest in KAGRA project.

2012 Sept. About 50 students of the physics department visited Kamioka Oct. Demonstration of interferometer in Campus Festival. President of Toyama Univ. visited Kamioka fiscal year Course lecture in the physics dept. by Prof. Kawamura

Four groups are now preparing 1. Laser: 4 members Fusakazu Matsushima (P), Yoshiki Moriwaki (P) Kaori Kobayashi (AP), Katsunari Enomoto (AP) collaborator: M1 students: 2, M2 students: 2 2. Signal analysis: 1 member Shigeki Hirobayashi (P) collaborator: M1 student: 1, M2 student: 1 3. Theory: 1 member Mitsuru Kakizaki (A) 4. Sapphire Mirror: 2 members Yukinori Ono (P), Tadahiro Hori (A) (P:professor, AS:associate professor, A: assistant professor)

Matsushima, Moriwaki, Kobayashi, Enomoto (Microwave Laboratory, Laser Physics Laboratory) Daily work: Control of motion of molecules → ultracold molecule → precise spectroscopy → fundamental physics → electric dipole moment of electron time evolution of fundamental constants Spectroscopy of interstellar molecules Collaboration with KAGRA: 2012 Dec.: Discussion with Prof. Terada and Prof. Kawamura → 2013 Collaboration title: "R&D for the intensity stabilization of the laser system in KAGRA" To obtain more concrete information on I/O system: → planning to visit LIGO Hanford in this March (with the budget by president of Univ. Toyama) 1: Laser Input/Output system

Organization: Shigeki Hirobayashi (University of Toyama) Collaborators: Seiji Kawamura (Tokyo) Hideyuki Tagoshi (Osaka) Gravitational Wave Detection Using Non-Harmonic Analysis 2. Signal Analysis

Background Signal processing – Audio and speech signals – Images – Signals used in medical engineering Optical coherence tomography Invention – New frequency analysis method Non-harmonic analysis (NHA) Gravitational Wave Detection Using Non-Harmonic Analysis

Advantages of NHA 1 We compared the accuracy of frequency analysis achieved by two approaches. MethodAccuracy DFT 1 order of magnitude NHA 10 or more orders of magnitude The square error of each estimated parameter. Better axail resolution can be expected when NHA is used. The accuracy of DFT analysis is relatively low when the objective signal is not a multiple of the fundamental frequency. Gravitational Wave Detection Using Non-Harmonic Analysis

15 Advantages of NHA (contd.) 3 NHA DFT Spectral components smaller than the sidelobe can be extracted independently. 2 Waveform 1 Original spectrum NHA

High Coherence Source Probe Arm  c/ ⊿ L t ➔ f FFT OCT signal zz Δλ ⊿L1⊿L1 ⊿L2⊿L2 Scan Depth Reference Arm Fixed mirror Coupler Sample 16 OCT Image Based on NHA (a) DFT （ FFT ） (b) NHA OCT cross-sectional images of onion skin.

Motivation Visualization of a gravitational wave Separation of gravitational waves from noise Time-Frequency Distribution Gravitational Wave Detection Using Non-Harmonic Analysis

3. Theory M. Kakizaki (Theoretical Physics Laboratory) Collaborate as a member of Prof. Kanda's Group 2013 thema "Study for KAGRA data analysis and research for its system"

Ｃｈａｒａｃｔｅｒｉｚａｔｉｏ ｎ ｏｆ s ａｐｐｈｉｒｅ ｍｉ ｒｒｏｒ ｆｏｒ ＫＡＧＲＡ ｕｓｉｎｇ ｅｌｅｃｔｒｏｎ ｓｐｉｎ ｒｅｓｏｎａｎｃｅ Yukinori Ono University of Toyama

Laser MC1 MC2 MC3 PRMPR2 PR3 BS SR3 SR2 SRM ITMX ITMY ETMX ETMY MT1 MT2  37cm  10cm Core optics of KAGRA Mirrors for Main cavities Initial: Silica Final: Sapphire 20

Mirror for KAGRA 温度を下げると物質の性質が変わる。 常温（ 300K ）で使用される鏡の材料 （合成石英）が利用できない。 光学的に透明な単結晶が望ましい。 酸化アルミニウム（ Al 2 O 3 ) Single crystal with diameter 25 ㎝, thickness 10 ㎝ and Mass 20kg. Optical property fluctuation Sapphire 21

Requirements for Sapphire Sapphire C-axis mirrors (  25cm x t15cm). –Current:  22cm 、 t15cm Absorption Cofficient: < 20 ppm/cm –Current ppm/cm? 22

AA AC P NameAbsorption [ppm/cm] 10 Samples from CSI have been measured Sapphire: Preliminary results

Purpose of this project Clarifying the origin by ESR ESR: Electron spin resonance Detecting unpaired spins > →Sensitive to impurity and defects in single crystal 24

Electron Spin Resonance X-band (Bruker) 3 – 300 K Cryostat (Oxford)

Signal A Signal B Signal C I p-p Preliminary results

Collaborators Dr. Masahiro Hori, University of Toyama Prof. Norikatsu Mio, The university of Tokyo Prof. Seiji Kawamura, The university of Tokyo Mr. Nobuhiro Fukumoto ， The university of Tokyo