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1 NASA/GSFC 滞在帰朝報告 穀山渉 Building 34 ( 沼田さんの実験室が入っている )
2 Contents NASA/GSFC 訪問 沼田さんの実験 Fiber Laser Development for LISA Laser Development for Earth Science Missions My Activity Iodine Wavemeter Others Miscellaneous 重力波研究交流会, Feb. 5, 2010
3 NASA/GSFC 訪問 訪問 10/1~12/17 (11 週間 ), 12/6-8 Caltech 出張 NASA Goddard Space Flight Center Gravitational Astrophysics Lab 重力波研究交流会, Feb. 5, 2010
4 NASA/GSFC 訪問 NASA Goddard Space Flight Center 米国メリーランド州グリーンベルト 1959 年開設 サイエンスの拠点 ( 地球 惑星 太陽系 天文学 ) ポトマック河 ゴダード ダラス国際空港 ワシントン DC メリーランド州 バージニア州 10km 重力波研究交流会, Feb. 5, 2010
5 Iodine Wavemeter 12/7 に Caltech で開かれた LISA WG meeting に行ってきました WG 2: PD, Laser, Phasemeter, Telescope, Interferometry Frequency Stabilization WG 3: Proof Mass 関係? そのスライドを流用しながらお話しします 重力波研究交流会, Feb. 5, 2010
6 沼田さんの実験 Fiber Laser Development for LISA (50%) Laser Development for Planetary Science Missions (50%) 重力波研究交流会, Feb. 5, 2010
7 Beyond Einstein: From the Big Bang to Black Holes Fiber Laser Development Kenji Numata Department of Astronomy, University of Maryland, CRESST Gravitational Astrophysics Laboratory (Code 663), NASA/GSFC GSFC - JPL
8 1. Introduction Beyond Einstein: From the Big Bang to Black Holes NPRO (Non-planar ring oscillator) has been used traditionally. Compact crystal cavity gives high stability. LISA needs low noise laser. Black box in many cases E.g.) TESAT NPRO for LPF All fiber/waveguide solution Fiber laser/amplifier technologies matured rapidly Higher robustness, cleaner output No strong magnet Dec. 7, 2009 Kenji Numata 2
9 2. Experimental Setup Beyond Einstein: From the Big Bang to Black Holes Ring configuration adopted over linear configuration More flexible, no spatial hole-burning, etc. Single-mode selection by filters (50MHz FSR) Fiber Bragg Grating (FBG) 34GHz BW + Fiber Fabry-Perot (FFP) 85MHz BW All PM components: single polarization operation Fast axis has much larger insertion loss. Dec. 7, 2009 Kenji Numata 3
10 Setup photo Beyond Einstein: From the Big Bang to Black Holes Prototype on a breadboard Control electronics PZT FBG FFP Pump LD Phase modulator Dec. 7, 2009 Kenji Numata 4
11 3. Experimental Results Beyond Einstein: From the Big Bang to Black Holes Coarse tuning FBG temperature FFP voltage (separation) 0.25nm (66GHz) range +-10V/+-10degree Fine tuning Wavelength [nm] FBG: 35ºC FBG: 25ºC FBG:15ºC FFP volrage [V] 20 Voltage on phase modulator Effectively changes laser cavity length Flat frequency response At least up to 100kHz Wider BW than commercial lasers Amplitude [Hz/V] Frequency [Hz] Dec. 7, Kenji Numata Amplitude Phase Phase [deg]
12 Noise of fiber laser Beyond Einstein: From the Big Bang to Black Holes Frequency noise Intensity noise Frequency noise [Hz/rtHz] Frequency [Hz] Low frequency: comparable to (better than) NPRO High frequency: increased noise due to relaxation oscillation Stabilization experiments GSFC fiber laser Lightwave NPRO Relative intensity noise [/rthz] GSFC fiber laser Lightwave NPRO after fiber Lightwave NPRO before fiber Frequency [Hz] Frequency: Planned using iodine or cavity. Intensity: Done after Yb amplifier and satisfied LISA requirement at low frequency. Dec. 7, 2009 Kenji Numata 6
13 4. Summary Beyond Einstein: From the Big Bang to Black Holes Fiber laser has significant advantages over traditional NPRO. Higher robustness, cleaner output, no strong magnet, etc. Now we can make single-mode, single-polarization laser. Fully custom-made laser possible No special gain fiber, standard components only Single-mode lasing achieved Comparable frequency/intensity noise to NPRO Wider frequency control bandwidth than NPRO Current activities Trying new configurations and filters to improve efficiency Starting component space qualifications Stabilization experiments Dec. 7, 2009 Kenji Numata 7
14 Laser Development for Planetary Science Missions OPAを用いた火星探査 Lidar 用レーザー光源 OPA (Optical Parametric Amplifier) : Seeded OPG nm (for CH4) と nm (for CO2) を生成 1064nm Q switch Laser (3ns, 300mW ave., 5kW peak, E pulse ~60μJ ) OPA Telescope で発射携帯電波塔に取り付けた反射板で見る 重力波研究交流会, Feb. 5, 2010
15 Laser Development for Planetary Science Missions (ASCENDS ミッションその他 ) での CO 2 観測用安定化レーザー光源 CO2 の nm 吸収線を観測し CO 2 濃度の 1ppm 単位での測定を目指す 安定化が必要 概念図 吸収線 FWHM~1.5GHz 時系列 Master Slave1 Slave2 Slave Lasers (Master に PhaseLock) 1μs 131μs Master Laser (CO 2 セルにロック ) 重力波研究交流会, Feb. 5, 2010
16 Laser Development for Planetary Science Missions 実験装置 現時点で 7 本のレーザー 重力波研究交流会, Feb. 5, 2010 CO2 セル : 結構大きい
17 My activity at Goddard Iodine Wavemeter LISA の現在のデザインでは キャビティを使った周波数安定化を行う その場合 2 機の S/C のレーザー間でビートを取るときに絶対周波数を知らないので 周波数を振ってサーチすることになる ヨウ素セルを用いて絶対周波数を知る装置 (Wavemeter) があるとリスク低減につながるのでうれしいのではないか 衛星に搭載することを考えて なるべくシンプルなセットアップで レーザーの PZT に変調もかけず ヨウ素吸収線を見るだけで絶対周波数を合わせる実験をした その結果 20MHz (LISA 搭載 PD の BW ) 以内に独立な 2 つのレーザーを追い込むことや オフセット周波数 4MHz の Phase Lock のデモンストレーションができた 重力波研究交流会, Feb. 5, 2010
18 Beyond Einstein: From the Big Bang to Black Holes Iodine Wavemeter Wataru Kokuyama Department of Physics, University of Tokyo (Visiting NASA/GSFC) Dec. 7, 2009 Kenji Numata 1
19 Background Beyond Einstein: From the Big Bang to Black Holes Iodine stabilization demonstration completed (~3 years ago) LISA pre stabilization requirement achieved Radiation test on doubling crystal, measurement of alignment sensitivity, etc. Involved bulk crystal in oven, modulations, cooler for cell, etc. Other use of iodine with simpler setup? Full setup RF EOM I 2 Cell Cooler Simplified setup EOM LF I 2 Cell Laser >~500mW Crystal in heater AOM Laser >~500mW Crystal in heater Cooler
20 Motivation Beyond Einstein: From the Big Bang to Black Holes Lock acquisition of the constellation is a challenge for LISA Lower risk for unknown unknowns of laser frequency acquisition Independent frequency reference on each spacecraft The simpler, the better. Iodine wavemeter Information on absolute laser frequency Onboard laser diagnostics Less sensitive to environmental disturbances Easier initial lock acquisition and robust onboard laser system We demonstrated ~10MHz accuracy and automatic phase lock with very simple setup
21 Experimental Setup Beyond Einstein: From the Big Bang to Black Holes Laser 150mW Lightwave NPRO 2.5mW SHG I 2 Cell SHG I 2 Cell BS I 2 Cell Detector 60mm Iodine cell w/o cooler for pressure control Waveguide Detector fiber-coupled waveguide PPKTP For LISA, SHG w/o heater available No heater (for LISA), No cooler, No modulator
22 Method Beyond Einstein: From the Big Bang to Black Holes How to tune lasers Program written in LabView 1. Sweep laser frequency - All frequency range 2. Identify Doppler broadened line - Remove mode-hop regions Rough tuning 3. Tune laser to identified line (Rough tuning) 4. Sweep again on the peak and go to halfmax (Fine tuning) 10MHz accuracy achieved; Beatnote of two lasers is < 20MHz (LISA s Detector BW) FWHM~250MHz Fine tuning to harlmax
23 Results Beyond Einstein: From the Big Bang to Black Holes < 10MHz accuracy of absolute frequency 4MHz phase lock with two independentlytuned lasers 1st step: Sweep starts from frequency difference > 10GHz 2nd step: Identify peak automatically Tune Beatnote monitor Tune 4th step: fine tuning and lock 3rd step: rough tuning LISA s detector BW :20MHz <100MHz Sweep/Identify halfmax Phase lock acquired
24 Summary Beyond Einstein: From the Big Bang to Black Holes Iodine wavemeter offers significant advantages for LISA. Absolute frequency reference will simplify lock acquisition of spacecrafts. Risk reduction We demonstrated automatic 4MHz phase lock, laser diagnosis, and ~10MHz accuracy wavemeter with very simple configuration. No heater, No cooler, No modulator Fiber-coupled waveguide, small cell only The small package can be put on anywhere in spacecraft. Goddard に帰ってから追加実験 : IR:4mW (Green:1.6mW) でも OK!
25 前から見た写真 絶対周波数リファレンス ヨウ素セルセットアップ レーザー (2 台 ) 重力波研究交流会, Feb. 5, 2010
26 後ろから見た写真 レーザー (2 台 ) ヨウ素セルセットアップ 絶対周波数リファレンス Labveiw DAQ Box 重力波研究交流会, Feb. 5, 2010
27 その他ちょこっとやったこと (1) 沼田さんのところにあった ヨウ素周波数安定化装置を動かしてみた (2 台のビート ) 重力波研究交流会, Feb. 5, 2010 うーん
28 その他ちょこっとやったこと (2) 新しく買ったメタンセルの内圧を吸収率でキャリブレーションしてみた P=1.0 torr でフィッティング I 2 は吸収が強いから楽 弱い吸収線は大変ですね 重力波研究交流会, Feb. 5, 2010
29 引越し 沼田さんの実験室の引越し (11/13-14) 高い!? Before After セットアップをブレッドボード上に 引越し後 2 日くらいで実験開始 重力波研究交流会, Feb. 5, 2010
30 Miscellaneous メリーランドでの暮らし 観光 お金 &Visa 重力波研究交流会, Feb. 5, 2010
31 メリーランドでの暮らし 家 家から毎日車を運転して 通勤 : 8 時半 ~9 時半に来て 19 時半ごろ帰る 朝ごはん : 家 昼ごはん :Goddard のカフェテリア / 外 晩ごはん : 家 重力波研究交流会, Feb. 5, 2010
32 メリーランドでの暮らし Ms. Judith Hamburg の家の一室を間借りのような形 : キッチン リビング共同 バスルーム別 最大 3 人 重力波研究交流会, Feb. 5, 2010
33 観光 U.S. Capitol The White House アポロ 11 号の司令船 ( 本物 ) スミソニアン博物館 Bethesda でのお祭り 重力波研究交流会, Feb. 5, 2010
34 お金 &Visa 渡航 滞在でかかった費用 項目 費用 ( 円換算,2.5ヶ月) 旅費 105,000 家 ~ 195,000 ($800/m) レンタカー ~ 190,000 ($780/m) Caltech ~ 60,000 食費など ~ 100,000 計 ~ 650,000 借りていたレンタカー その他滞在関係の手続きについて J-1 ビザを取得 (NASAだから厳しくて必要だった? Caltechは必要なし?) DS-2019をNASAに発行してもらう 予約 大使館へ Visa 入手 携帯電話 銀行口座 ( バンカメ ) 開く Social Security Number を取得 重力波研究交流会, Feb. 5, 2010
35 おわり 重力波研究交流会, Feb. 5, 2010
36 重力波研究交流会, Feb. 5, 2010
37 重力波研究交流会, Feb. 5, 2010
38 重力波研究交流会, Feb. 5, 2010
39 重力波研究交流会, Feb. 5, 2010
40 重力波研究交流会, Feb. 5, 2010
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