Curriculum Vitaes

Yoshitaka Saito

  (斎藤 芳隆)

Profile Information

Affiliation
Associate Professor, Institute of Space and Astronautical Science, Department of Interdisciplinary Space Science, Japan Aerospace Exploration Agency
Degree
(BLANK)(The University of Tokyo)
(BLANK)(The University of Tokyo)

J-GLOBAL ID
200901068528199528
researchmap Member ID
1000227990

科学観測用気球の開発とそれを用いた科学観測を行っています。気球には到達できる高さ、飛翔時間の制限がありますが、それを大きく打ち破る気球が誕生しつつあります。気球の研究を進め、気球の可能性を広げ、様々な科学観測実験で利用できるようにしたいと考えています。

 修士過程では、所属する研究室で開発が進められていた天体硬X線検出器を用いた気球実験に携わりました。博士過程ではそれを将来のX線天文衛星搭載用に発展させると共に、X線天文衛星「あすか」による回転駆動型パルサーの観測を行い、エネルギー放射機構の研究を進めました。

 その後、宇宙研気球グループに奉職し、高エネルギー宇宙物理に関する観測実験を継続すると共に、気球本体、搭載機器、地上系といった気球実験システム全般の開発と運用に従事するようになりました。気球の飛翔実験実施にあたっては受信班として、気球と地上間のデータ伝送の確立を担っています。

 気球本体の開発として最初に手掛けたのは、薄い皮膜を開発し、それを用いた気球を開発することで、飛翔高度を向上させる研究でした。3.4 um厚のフィルムを開発し、2002年にはそのフィルムを用いた気球により30年ぶりに世界最高気球高度記録を更新しています。さらにより薄いフィルムの開発を進め、2013年には2.8 um厚のフィルムにより、再度の記録更新に成功しました。

 この研究と並行して進めているのがスーパープレッシャー気球の開発です。これは、気球を密閉して加圧することで、夜間の浮力の低下を防ぎ、長時間の飛翔を可能にする気球です。2000年代は気球皮膜自体の開発や、ロープと皮膜を組み合わせることで構造強度を向上させたLobed-pumpkin型やその展開性能を改善した俵型の気球の開発を進めました。2010年には皮膜に菱形の目の網をかぶせることで軽い構造で高い耐圧性能が得られることを見出し、以後、この型の気球の開発を進めております。スーパープレッシャー気球の実現には、軽い構造で十分な耐圧性能と気密性能を持たせることが大切です。2019年には体積6,400 m3の気球の地上試験(地上試験としては世界最大級です)を実施し、十分な安全率をもって、高度27 kmに70 kgのペイロードを長時間飛翔させることができる耐圧性能を有することを確認しました。2020年には体積2,000 m3の気球の飛翔試験を実施したのですが、放球直後からガス漏れが発生するという不具合が発生しました。放球時に網が叩いたことで皮膜が衝撃破壊を起こしたもので、これを防ぐべく、2020~2023年にかけて、準静的に気球を立ち上げて放球する新しい方法を開発し、その実証試験まで完了しました。2024年には、この放球方法により、再度、体積2,000 m3の気球の飛翔試験を実施する計画です。また、皮膜を多層化することで10日以上の飛翔が可能となる気密性能が得られること、耐圧性能は3,000 Paを超えることを体積180 m3の小型気球の地上試験で実証しました。2022年には、この型の気球を用いて、南極域での大気重力波観測が実施され、2024年には改良を加えた気球での実験を計画しています。

満膨張になった体積6,400 m3の気球

 このように、気球の研究は進んでいるのですが、一方で、気球を用いた科学観測実験の方は開店休業状態であり、これが実施できていないことには忸怩たる思いがあります。残念ながら、現状の我が国の気球実験システムでは、気球の飛翔期間が数10時間に限られてしまうため、得られる光子数が乏しく、実施したい高エネルギー天体の研究が困難なのです。むろん、この制限の元で科学的な成果をあげることも不可能ではありませんが、自分が我が国で唯一、大気球の飛翔機会を提供している研究所に所属し、我々以外に気球の研究を進めているグループが存在しない現状を考えると、気球を用いた実験を実施するよりも、気球の研究を推進し、自らの実験を可能にすると共に、みなさまに利用していただける気球が提供できるようにすることこそが責務、と感じております。

 長時間飛翔が可能な気球は世界的にも黎明期にあり、我が国ではその技術は未獲得です。大型気球は開発コストが嵩むため、小型気球からの開発となるのですが、技術的には小型の方が困難です。これは、気球重量が表面積に比例しているのに対し、浮力は体積に比例することが一因で、もう一つには気球皮膜の欠陥数は表面積に比例するのに対し、ガス漏れの許容量は気球体積に比例するためです。上にも記載しましたが、我々は耐圧性能、気密性能、それぞれの向上手段を見出しており、これらを用いて科学観測に利用できる気球を開発し、小型気球による科学観測を開始したいと考えています。 


Papers

 305
  • KASAHARA Katsuaki, MOCHIZUKI Eiko, TORII Shoji, TATEYAMA Nobuhito, TAMURA Tadahisa, YOSHIDA Kenji, OHUCHI Tatsumi, NISHIMURA Jun, YAMAGAMI Takamasa, SAITO Yoshitaka, MURAKAMI Hiroyuki, KOBAYASHI Tadashi, KOMORI Yoshiko, HONDA Morihiro, MIDORIKAWA Shoichi, YUDA Toshinori
    宇宙科学研究所報告 特集, 41(41) 65-72, Feb, 2001  Peer-reviewed
    We have performed a series of observation of atmospheric gamma rays to determine the absolute flux of neutrinos in relation to presence of the neutrino oscillations which have been claimed by the Super-Kamiokande experiment. The observations were carried out with the BETS instrument which was improved for the gamma-ray detection by adding the trigger system. In 2000, we obtained reliable data by using an optimized trigger system. The gamma-ray fluxes at balloon altitudes were compared with the expected ones by Monte-Carlo simulations using different nuclear interaction models. The best-fit model for the gamma-ray flux is proposed for the calculation of the absolute neutrino flux.
  • NAMIKI Michiyoshi, MATSUZAKA Yukihiko, TORIUMI Michihiko, UCHIDA Yuubu, HIRAYAMA Shoji, KOMATSU Toshiro, HONDA Hideyuki, IZUTSU Naoki, SAITO Yoshitaka, OHTA Shigeo, YAMAGAMI Takamasa, HIROSAWA Haruto, MATSUMOTO Toshio, KODAMA Kosuke, HONMA Youji
    宇宙科学研究所報告 特集, 41(41) 25-34, Feb, 2001  Peer-reviewed
    The sanriku Balloon Center (SBC) which belongs to the Institute of Space and Astronautical Science was built in 1971. The launching field of SBC was 140 m in length and 20 m in width. In Japan, the balloon launching method used since 1971 is a kind of static launching method. To launch larger balloons, we have developed a "semi-dynamic" launching method and extended the launching field by 20 m and developed a new launcher in 1998. This new launcher is different from the one used in the dynamic launching method. It is fixed to the ground creating freedom of rotation around the vertical axis. In addition, it is also possible for the launcher to lift a payload up to 5 m height from the ground. We have successfully launched the first test balloon by using this new launching method on September 6, 1999. Utilizing this new launching machine, it has now become possible even in Japan to launch a balloon with a volume of 1,000,000 m^3 and a total lift of 2 tons.
  • Y Saito, N Kawai, A Rots, T Kamae, S Shibata
    NEW CENTURY OF X-RAY ASTRONOMY, 251 404-405, 2001  Peer-reviewed
    We performed 82 ksec observation of the millisecond pulsar PSR B1821-24, the brightest in the X-ray band among the species. It shows a double peaked pulse profile, with peak widths of 80 and 170 musec in FWHM, respectively. The sharper peak coincides approximately with one of the two radio peaks as reported before. The shape of the pulse profile does not depend on energy in 2 to 20 keV band and shows no variation during the observation. The energy spectra of the both peaks are represented by a hard power-law with photon index of 1.1 and no apparent difference in the spectra is found.
  • K. Yoshida, S. Torii, N. Tateyama, T. Tamura, T. Ouchi, T. Kashiwagi, K. Hibino, J. Nishimura, T. Yamagami, Y. Saito, H. Murakami, T. Kobayashi, Y. Komori, K. Kasahara, T. Yuda, M. Ohnishi, M. Shibata, F. Makino
    Advances in Space Research, 27(4) 681-686, 2001  Peer-reviewed
    The CALET (CALorimetric Electron Telescope) instrument is proposed for the observation of TeV electrons at the Japanese Experiment Module Exposure Facility (JEM/EF) on the ISS, which is composed of an imaging calorimeter with scintillating fibers and lead plates, and a total absorption calorimeter with BGO logs. Since TeV electrons could reach only from the nearby sources within a distance less than 1 kpc, we can expect that the energy spectrum has a structural component and the arrival directions show an anisotropy. Therefore, we should be able to localize and identify the nearby cosmic-ray sources by the TeV electron observation. We report the status of development of the CALET instrument, which has a capability to observe electrons up to 10 TeV and a proton rejection power of ~ 10 6 . We expect to observe ~ 10 3 events over 1 TeV during the 3 years observation. By using the excellent imaging capability of the CALET, gamma-rays over the GeV region and the nuclear components up to 10 15 eV might also be observed. © 2001 COSPAR. Published by Elsevier Science Ltd. All rights reserved.
  • S. Torii, T. Tamura, N. Tateyama, K. Yoshida, T. Ouchi, J. Nishimura, T. Yamagami, Y. Saito, H. Murakami, T. Kobayashi, Y. Komori, K. Kasahara, T. Yuda
    Advances in Space Research, 27(4) 675-680, 2001  Peer-reviewed
    New measurements of the electron flux from 10 to 100 GeV were carried out with the BETS (balloon-borne electron telescope with scintillating fibers) instrument. The detector is an imaging calorimeter consisting of scintillating-fiber belts of 36 layers (each 280 mm wide) and the 8 plates of lead (each 5mm thick). Rejection of the background protons was performed at an efficiency of ~ 2000 using the shower imaging capability with high granulation. The observed electron flux around a few 10 GeV is consistent with the recent results reported by the HEAT group. Comparing the flux with theoretical expectations from a diffusion model, the best fit is obtained for the model of a diffusion coefficient of 2 × 10 28 (E/GeV) 0.3 cm 2 /sec for the SN rate of once per 30 years in the Galaxy. © 2001 COSPAR. Published by Elsevier Science Ltd. All rights reserved.
  • S Torii, K Sakurai, T Shirai, T Taira, T Tamura, N Tateyama, K Yoshida, T Yamagami, E Kamioka, Y Saito, H Murakami, T Kobayashi, Y Komori, K Kasahara, T Yuda, J Nishimura
    SUN AND SIMILAR STARS/COSMIC RAY SPECTRA AND COMPOSITION, 26(11) 1867-1870, 2001  Peer-reviewed
    The TeV electrons observed in the solar system are considered to be produced in the sources within 1 kpc in distance and in period for the past 100,000 years. The supernova remnants as a candidate of the electron sources are, therefore, very limited in number as Monogem, Loop 1, Geminga and Vela. It is expected that the few sources cause a structural component in the energy spectrum and an anisotropy in the arrival directions. Our calculations show that the direct effects of these nearby sources can be detected by a yearly observation with a detector having a geometrical factor of 0.5 m(2) sr, We will present a future plan proposed for the observation of TeV electrons at the Japanese Experiment Module (JEM) in ISS. (C) 2001 COSPAR. Published by Elsevier Science Ltd. All rights reserved.
  • S Torii, T Tamura, N Tateyama, K Yoshida, T Yamagami, E Kamioka, Y Saito, H Murakami, T Kobayashi, Y Komori, K Kasahara, T Yuda, J Nishimura
    SUN AND SIMILAR STARS/COSMIC RAY SPECTRA AND COMPOSITION, 26(11) 1823-1826, 2001  Peer-reviewed
    The BETS (balloon-borne electron telescope with scintillating fibers) instrument has been developed for high-altitude balloon Rights to observe the cosmic ray electrons with energies of 10 GeV to several 100 GeV. The detector is a Lead/SciFi sampling calorimeter consisting of 36 SciFi belts (each 280 mm wide) and 8 lead plates (each 5 mm thick). The electron identification is performed by triggering the electro-magnetic showers on board and by analyzing the three-dimensional shower images by an intensified CCD camera. It is demonstrated in the Right data in 1995 and 1997 that a reliable identification of the electron component against the proton background is achieved up to a few 100 GeV. The performance of detector was tested by the CERN-SPS electron beams in 1996 and with the proton beams in 1997. The obtained energy spectrum is consistent with the recent observation by HEAT, although our result still has a little room for improvement. The energy spectrum from 10 GeV to 1000 GeV which is obtained by combining these data and the emulsion chamber data ( Nishimura et al. 1997)suggests that the diffusion constant is about 1 X 10(28) (E/GeV)(0.3) cm(2)/sec in the energy range between 10 GeV and 1000 GeV. A hump in the energy spectrum is observed around several hundred GeV, which is expected from a nearby source. (C) 2001 COSPAR. Published by Elsevier Science Ltd. All rights reserved.
  • 大気球シンポジウム集録, 2001  
  • S Torii, T Tamura, N Tateyama, K Yoshida, Y Ouchi, T Yamagami, Y Saito, H Murakami, T Kobayashi, Y Komori, K Kasahara, T Yuda, J Nishimura
    NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT, 452(1-2) 81-93, Sep, 2000  Peer-reviewed
    We describe a new detector system developed for high-altitude balloon flights to observe the cosmic-ray electrons above 10 GeV, The Balloon borne Electron Telescope with Scintillating (BETS) fibers instrument is an imaging calorimeter which is capable of selecting electrons against the large background of protons. The calorimeter is composed of a sandwich of scintillating optical-fiber belts and lead plates with a combination of three plastic scintillators for shower trigger. The total thickness of lead is 40 mm ( similar to 7.1 r.l.) and the number of fiber belts is nine. In each belt, alternating layers are oriented in orthogonal (x and y) directions. Two sets of an intensified CCD camera are adopted for read-out of the scintillating fibers in the x and y direction, respectively. The accelerator beam tests were carried out to study the performance of detector for electrons in 1996 and for protons in 1997 at CERN-SPS. The instrument was successfully flown aboard high-altitude balloon in 1997 and 1998. It is demonstrated by the flight data that a reliable identification of the electron component has been achieved in 10-100 GeV and the energy spectrum has been obtained. (C) 2000 Elsevier Science B.V. All rights reserved.
  • T Furusho, NY Yamasaki, T Ohashi, Y Saito, W Voges
    PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, 52(4) 677-684, Aug, 2000  Peer-reviewed
    An ASCA observation of a region containing a Class 0 protostar IRAS 20386 + 6751 in the Lynds 1157 dark cloud, has been carried out. The protostar was not detected, and the 95% upper limit to the luminosity depends on the assumed N-H: L-X(0.5-10 keV) < 1.1 x 10(31) erg s(-1) for N-H = 1 x 10(23) cm(-2). A Class I protostar in Lynds 1152, IRAS 20353 + 6742, in the same field was also undetected with an upper limit about three-times as much as the Lynds 1157 level. Besides these non detections, nine new X-ray sources were detected and a spectral analysis was performed for 4 sources. One object (AX J2038 + 6801) shows a hard spectrum with a temperature of kT similar to 8 keV or a power-law photon index of similar to 2.0 and absorbed with N-H similar to 2 x 10(22) cm(-2). Another fainter one (AX J2036 + 6800) has a soft spectrum with most of the emission falling below 2 keV. We examine the possible nature of these new X-ray sources based on their spectral properties.
  • TORII Shoji, YAMAGAMI Takamasa, MURAKAMI Hiroyuki, TAMURA Tadahisa, YOSHIDA Kenji, TATEYAMA Nobuhito, OUCHI Tatsumi, SAITO Yoshitaka, KOBAYASHI Tadashi, KOMORI Yoshiko, KASAHARA Katsuaki, YUDA Toshinori, NISHIMURA Jun
    宇宙科学研究所報告 特集, 40(40) 77-83, Mar, 2000  Peer-reviewed
    We report new measurements of the electron flux from 10 GeV to 100 GeV observed with the BETS (Balloon-Borne Electron Telescope with Scintillating fibers) instrument. The detector is an imaging calorimeter consisting of ∿10,000 scintillating fibers and 7.1 r.l. thick lead. Rejection power of the background protons by the imaging capability of showers was proved to be 2,500. The balloon observations were carried out in 1997 and 1998 at Sanriku in Japan. Comparing the present results with previous ones, we discuss the diffusion characteristics of electrons in the Galaxy and the solor modulation effects.
  • SAITO Yoshitaka, OHTA Shigeo, TORIUMI Michihiko, NAMIKI Michiyoshi, MATSUZAKA Yukihiko, YAMAGAMI Takamasa, YOKOTA Rikio, ICHIMURA Koji, KOBAYASHI Tsutomu, NOZAWA Satoshi, MATSUSHIMA Kiyoho
    宇宙科学研究所報告 特集, 40(40) 1-17, Mar, 2000  Peer-reviewed
    The ISAS balloon group has been engaged in the development of a high altitude balloon. We have just succeeded in developing a new thin film with thickness of 3.4μm and confirmed that the film is able to be heat-sealed with protection tapes covering both side without loosing any original strength against tension. We have also decreased the weight of the protection tape by 1/4. Using the super thin film with the protection tape, we made a balloon with a volume of 1,000m^3. The balloon was launched on Sep. 1,1999 and reached a highest altitude of 37.1km successfully. This experiment is epoch making for the development of large plastic balloons with super thin films.
  • Y Matsuzaka, T Yamagami, M Namiki, M Toriumi, S Ohta, F Makino, H Hirosawa
    SCIENTIFIC BALLOONING, 26(9) 1365-1368, 2000  Peer-reviewed
    The development of high altitude balloons will enrich many areas of scientific observation. A high altitude balloon fabricated using improved technology with thin Winzen polyethylene films has been flown in the upper atmosphere. A light weight balloon carrying small instruments can reach an altitude higher than 40 km. In contrast to sounding rockets, the balloon-borne experiment provides a unique opportunity to stay at a high altitude for more than a few hours at low cost. We have developed methods for fabricating large balloons for scientific observation and have also established a new belt sealer and successful launching system. In January 27, 1997, a thin-film balloon with a volume of 120,000 m(3), carrying a payload of 11.8 kg, reached an altitude of 50.2 km which is the highest balloon altitude ever in Japan. This shows that a thin-film balloon is suitable for high altitude observations and can fill the gap between satellite and conventional balloon altitudes. (C) 2000 COSPAR. Published by Elsevier Science Ltd.
  • Advances in Space Research, 26(9) 1353-1356, 2000  Peer-reviewed
  • Saito Yoshitaka, Matsuzaka Yukihiko, Miyahara Yasuaki, Ohnishi Akira, Yamagami Takamasa, Yokota Rikio, Kobayashi Tadashi, Nishimura Jun
    Advances in Polar Upper Atmosphere Research, 14 163-171, 2000  Peer-reviewed
    Large plastic balloon play an important role for scientific observations at high altitude in the field of astrophysics and geophysics. In these observations, it has been well recognized that the long duration balloon flights are indispensable for precise observations. For a normal zero pressure balloon, we need to drop ballast to keep a level altitude during day and night to prevent from altitude excursions. This is due to the temperature change of lifting gas, and the duration of the balloon is limited when all the ballast on board the balloon has been exhausted. In this paper, we discuss a possibility of minimizing the temperature variation of the lifting gas using specific balloon films with suitable optical properties and show the optical properties of some test films for this purpose.
  • S Torii, N Tateyama, T Tamura, T Ouchi, K Kashiwagi, K Yoshida, K Hibino, Y Yamagami, Y Saito, H Murakami, T Kobayashi, Y Komori, K Kasahara, T Yuda, M Ohnishi, M Shibata, F Makino, J Nishimura
    SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM, PTS 1 AND 2, 504 187-192, 2000  
    The CALET instrument is proposed for the Japanese Experiment Module/ Exposure Facility (JEM/EF) on International Space Station (ISS) to resolve the long-term puzzles in high-energy cosmic-ray physics. The ISS gives us a unique opportunity to carry out the measurements of cosmic ray electrons with a relatively heavy and large detector, and for the long exposure. The instrument will be composed of an imaging calorimeter with scintillating fibers and a total absorption calorimeter for detecting the electrons up to 10,000 GeV. The origin of high-energy electrons and the diffusion characteristics in the Galaxy will be revealed by measuring the energy spectrum of electrons and the anisotropy of arrival directions. By the excellent capability of the CALET, both of the gamma-rays over GeV and nucleus component up to 10(15)eV might be investigated as additional possibilities of the observation.
  • M Takahashi, S Shibata, K Torii, Y Saito, N Kawai, M Hirayama, T Dotani, S Gunji, H Sakurai
    PULSAR ASTRONOMY - 2000 AND BEYOND: IAU COLLOQUIUM 177, 202 353-354, 2000  
    We report the first detection of the pulsed X-ray emission from the fastest millisecond pulsar known PSR B1937+21 (P =1.558msec) with ASCA. The pulsar is detected as a point source above similar to 1.7keV, with no nebulosity indicated. The source flux in the energy band 2-10keV is found to be f = 4.3 x 10(-13)erg s(-1) cm(-2), which corresponds to the luminosity of L-x = 4 pi D(2)f approximate to 6.6 x 10(32)(D/3.6kpc)(2) erg s(-1), where D is the distance, and correspond to approximate to 6 x 10(-4) of the rotation power of the pulsar. The pulsation is found at the period predicted by the radio ephemerides with very narrow primary peaks, the width of which is about 1/16 phase approximate to 100 mu s near the time resolution limit (61 mu s) of the observation. The pulsed luminosity within the primary peak (1/16 phase interval) is found to be f(p) = 4.0 x 10(-12)erg s(-1) cm(-2) Although there may be a secondary peak, its statistical significance is too low to identify. Spectra of the whole source region and the primary peak are fitted by power law models to give photon indices of about unity for both.
  • T Oka, N Kawai, T Naito, T Horiuchi, M Namiki, Y Saito, RW Romani, T Kifune
    ASTROPHYSICAL JOURNAL, 526(2) 764-771, Dec, 1999  Peer-reviewed
    CO J = 1-0 mapping observations of the dark nebula Lynds 227, which is possibly associated with the unidentified EGRET source 2EG J1811-2339, are presented. We detected a large amount of molecular gas along Lynds 227 with a total mass of (1-2) x 10(4) M-circle dot surrounding an X-ray synchrotron nebula, which was detected by the ASCA within the error circle of 2EG J1811-2339. Molecular gas along Lynds 227 shows spatial anticorrelation with the X-ray synchrotron nebula, suggesting that the synchrotron nebula is interacting with the Lynds 227 cloud. We propose a gamma-ray emission mechanism for 2EG J1811-2339: high-energy electrons are injected from a rotation-powered pulsar and further accelerated in shock waves generated by the interaction with ambient matter. The high-energy electrons move into the molecular cloud at the Lynds 227 and collide with dense interstellar matter to yield high-energy gamma-ray photons, mainly through relativistic bremsstrahlung.
  • K Torii, H Tsunemi, T Dotani, K Mitsuda, N Kawai, K Kinugasa, Y Saito, S Shibata
    ASTROPHYSICAL JOURNAL, 523(1) L69-L72, Sep, 1999  Peer-reviewed
    We report here the first measurement of the spin-down rate of the 65 ms X-ray pulsar within the supernova remnant G11.2-0.3. The period derivative is measured to be (P)over dot = (4.40(-0.04)(+0.03)) x 10(-14) s s(-1) using the Advanced Satellite for Cosmology and Astrophysics and BeppoSAX. From the pulsar period and its derivative, the corresponding surface magnetic field (B = 1.7 +/- 10(12) G) and the characteristic age [P/(2(P)over dot) = 2.4 x 10(4) yr] are derived. The physical association of the pulsar and supernova remnant with the historical record of A.D. 386 is discussed in the context of the measured (P)over dot. If the pulsar was formed during the historical event, the initial pulse period should have been relatively slow (P-0 similar or equal to 62 ms). This initial period is more than a factor of 3 larger than that of a small number of prototypical objects, suggesting a diversity of initial periods for newly formed neutron stars.
  • Sakurai, I, N Kawai, H Negoro, K Torii, Y Saito, S Shibata
    ASTRONOMISCHE NACHRICHTEN, 320(4-5) 339-339, 1999  Peer-reviewed
    We report results for the X-ray spectrum of a millisecond pulsar, PSR J2124-3358 observed with ASCA. This pulsar is an isolated 4.9 ms pulsar (Bailes et al 1997). Its X-ray pulsation was detected with ROSAT HRI in the 0.1- 2.4 keV band(Becker & Trumper 1998). The pulse profile was broad, and there is an indication of a secondary peak. Due to the lack of spectral information, the nature of the S-ray emission was unclear. An ASCA observation of this pulsar was carried out in May 1998, and provided the X-ray spectrum in the energy band from 0.5 to 10.0 keV. Due to poor statistics, the X-ray pulsation was not confirmed by ASCA.
  • K Torii, H Tsunemi, T Dotani, K Mitsuda, N Kawai, K Kinugasa, Y Saito, S Shibata
    ASTRONOMISCHE NACHRICHTEN, 320(4-5) 343-343, 1999  Peer-reviewed
  • M Takahashi, S Shibata, S Gunji, H Sakurai, K Torii, Y Saito, N Kawai, T Dotani, M Hirayama
    ASTRONOMISCHE NACHRICHTEN, 320(4-5) 340-340, 1999  Peer-reviewed
  • N Kawai, Y Saito
    ASTROPHYSICAL LETTERS & COMMUNICATIONS, 38(1-6) 1-8, 1999  Peer-reviewed
    The non-thermal magnetospheric X-ray emission from rotation-powered pulsars can be studied best in the energy band above 2 keV where the contamination by the thermal component is less significant than in the soft X-ray band. With the recent advances in the high sensitivity X-ray observations, X-ray pulsations are found from more pulsars including several millisecond pulsars. We review the recent progress in the X-ray observations of the millisecond pulsars, and show that the emission properties have strong correlation with the magnetic field strength at the light cylinder.
  • S Torii, N Tateyama, T Tamura, T Ouchi, K Kashiwagi, K Yoshida, K Hibino, T Yamagami, Y Saito, H Murakmai, T Kobayashi, Y Komori, K Kasahara, T Yuda, M Ohnishi, M Shibata, J Nishimura
    SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - 1999, PTS ONE AND TWO, 458 127-132, 1999  Peer-reviewed
    By using the JEM (Japanese Experiment Module) facility on ISS, we are planning to carry out a precise measurement of the flux and energy spectrum of cosmic-ray electrons of 10 GeV to several TeV. Since the electrons over several 100 GeV could be contributed only from the nearby sources within a distance less than 1 kpc, it is expected in the high energy region that the energy spectrum has a structural component and the distribution of the arrival directions presents anisotropy. By helping to localize and identify the nearest cosmic ray sources, these data should help to resolve the long-term puzzle. The instrument used for the observation is a kind of scintilating-fiber/lead imaging calorimeter that has been used for the balloon observations. We are developing an improved detector having a geometrical factor of 0.5 m(2)sr and a higher rejection power against the background protons ( greater than or equal to 10(4)). It is expected to observe nearly 500 electrons over 1 TeV during the one-year observation.
  • Oka T, Kawai N, Naito T, Horiuchi T, Namiki M, Saito Y, Romani R. W, Kifune T
    Astronomische Nachrichten, 320(4-5) 327, 1999  
  • Kokubun M, Fukazawa Y, Idesawa E, Kataoka J, Kamae T, Matsuzaki K, Mizuno T, Saito Y, Takahashi T, Takizawa K, Tashiro M, Tamura T, Yoshida A
    IEEE Nuclear Science Symposium and Medical Imaging Conference, 1 227-232, 1999  Peer-reviewed
    ASTRO-E Hard X-ray Detector (HXD) is characterized by well-type phoswich counters in a compound-eye configuration which reduce the X-ray and non X-ray background to lower level than any other past hard X-ray missions. When operating in Low Earth Orbit, the expected background of the HXD is an order of 10-5[counts/s/keV/cm2], mainly caused from the radioactivity induced within the detector materials by nuclear interactions with geomagnetically trapped protons. Results are presented from measurements of induced radioactivity in two phoswich scintillators, GSO and BGO, irradiated by mono-energetic protons at an accelerator facility. Radiation transport computer codes are used to build the detector response functions against emissions from decays of spallation products. Based on the comparison of experimental and simulation results, the activation background level of HXD in the orbit is estimated.
  • 大気球シンポジウム集録, 73, 1999  
  • 中性子星の誕生と進化研究会集録, 127, 1999  
  • 超高エネルギー天体研究会集録, 85, 1999  
  • M. Kokubun, Y. Fukazawa, E. Idesawa, J. Kataoka, T. Kamae, K. Matsuzaki, T. Mizuno, Y. Saito, T. Takahashi, K. Takizawa, M. Tashiro, T. Tamura, A. Yoshida
    IEEE Transactions on Nuclear Science, 46(3) 371-376, 1999  
    ASTRO-E Hard X-ray Detector (HXD) is characterized by well-type phoswich counters[1] in a compound-eye configuration which reduce the detector background to lower level than any other past hard X-ray mission. When operating in Low Earth Orbit, the expected background of the HXD is an order of 10 -5 counts/s/kcV/cm 2, mainly caused from the radioactivity induced within the detector materials by geomagnetically trapped protons. Results are presented from measurements of induced radioactivity in two phoswich scintillators, GSO (Gd 2SiO 5:Ce 0.5% mol) and BGO (Bi 4Ge 3O 12), irradiated by mono-energetic protons at an accelerator facility. Radiation transport computer codes are used to build the detector response functions for emissions from decays of spallation products. Based on the comparison between experimental and simulation results, the activation background level of HXD in the orbit is estimated. © 1999 IEEE.
  • Y Saito, E Mochizuki, T Yamagami, N Kawai
    ASTRONOMISCHE NACHRICHTEN, 320(4-5) 329-329, 1999  
  • Yoshitaka Saito, Takamasa Yamagami, Jun Nishimura
    Advances in Polar Upper Atmosphere Research, 13 182-190, 1999  Peer-reviewedLead author
    For long duration balloon flights, when the balloon is outside the tele-command range, it is necessary to control the altitude automatically since the temperature of the lifting gas decreases at sunset. Here, we propose a new method referring to the inner pressure at the nadir of a balloon. The inner pressure is approximately proportional to the amount of descent from the level altitude and to the atmospheric pressure at the level altitude. This method has advantages in its simplic- ity and does not require prior information of the level altitude.
  • AH Rots, K Jahoda, DJ Macomb, N Kawai, Y Saito, VM Kaspi, AG Lyne, RN Manchester, DC Backer, AL Somer, D Marsden, RE Rothschild
    ASTROPHYSICAL JOURNAL, 501(2) 749-757, Jul, 1998  Peer-reviewed
    Observations with the Rossi X-Ray Timing Explorer and the Jodrell Bank, Parkes, and Green Bank telescopes have enabled us to determine the time delay between radio and X-ray pulses in the two isolated pulsars B1821-24 and B1509-58. For the former we find that the narrow X-ray and radio pulse components are close to being coincident in time, with the radio peak leading by 0.02 period (60 +/- 20 mu s), while the wide X-ray pulse component lags the last of the two wider radio components by about 0.08 period. For the latter pulsar we find, using the standard value for the dispersion measure, that the X-ray pulse lags the radio by about 0.27 period, with no evidence for any energy dependence in the range 2-100 keV. However, uncertainties in the history of the dispersion measure for this pulsar make a comparison to previous results difficult. It is clear that there are no perceptible variations in either the lag or the dispersion measure at timescales of a year or less.
  • JP Finley, R Srinivasan, Y Saito, M Hiriyama, T Kamae, K Yoshida
    ASTROPHYSICAL JOURNAL, 493(2) 884-890, Feb, 1998  Peer-reviewed
    The young "Vela"-like neutron star PSR B1706-44 was imaged by both the HRI aboard ROSAT and the solid-state imaging spectrometers and gas imaging spectrometers aboard ASCA during a 6 month period in late 1994 and early 1995. The broadband data set, extending over two decades in energy, allowed a detailed spatial, spectral, and temporal study to be conducted. PSR B1706-44 is found embedded in a compact synchrotron nebula of physical size similar to 0.32 pc and displays the morphology characteristic of the other young neutron stars in the 10(4)-10(5) yr age range. No pulsations at the radio period were detected in either the ROSAT or the ASCA data. The spectrum is well described by a power-law distribution, and the data are consistent with there being no spectral break from the radio through the soft X-ray band. The unpulsed TeV emission that has been observed from PSR B1706-44 can be reconciled with these observations if the TeV emission results from the up-scattering of background IR photons by the population of high-energy particles that produce the soft X-ray photons.
  • N Kawai, K Tamura, Y Saito
    SPACE BASED ASTRONOMY: ISO, AGN, RADIOPULSARS AND THE SUN, 21(1-2) 213-221, 1998  Peer-reviewed
    Results from the X-ray observations of pulsars with ASCA are presented. The surroundings of pulsars are investigated in detail taking advantage of ASCA's unique capabilities; high spectral resolution and a high throughput over a wide energy range from 0.4 keV to 10 keV. We detected diffuse emission sources in the vicinity of many pulsars, often with asymmetric structure. The high probability of finding such diffuse sources for many pulsars suggests that they exist universally for all the active pulsars, and that they are powered by the pulsars. The results of the ASCA observation of the two millisecond pulsars, PSR J0437-4715 and PSR B1821-24 are presented. They have very different characteristics. The energy spectrum of PSR J0437-4715 is best described by a blackbody with kT=0.27 keV. PSR B1821-24, on the contrary, has a hard X-ray spectra. A non-thermal sharp pulsed emission was detected. (C) 1998 COSPAR. Published by Elsevier Science Ltd.
  • 斎藤芳隆
    原子核研究, 42(6), 1998  
  • 大気球シンポジウム集録, 68, 1998  
  • R Danner, Kulkarni, SR, Y Saito, N Kawai
    NATURE, 388(6644) 751-753, Aug, 1997  
    Globular clusters, the most ancient stellar groups in our galaxy, are known to contain bright X-ray sources, faint X-ray sources and millisecond pulsars, The bright X-ray sources are neutron stars accreting matter from a companion star(1), and the millisecond pulsars are believed to be descendants of these sources(2). But the origin of the faint X-ray sources remains unclear Here we report satellite-based X-ray observations of the globular cluster M28 which reveal two faint X-ray sources; an extended source slightly offset from the centre of the duster, and a point source. The point source pulsates with the same period as a well-known(3,4) 3-millisecond pulsar in M28. The nature of the extended source is more puzzling, however, and its spatial and spectral properties permit a range of plausible models. We argue that this source is either a collection of low-luminosity accreting neutron-star binaries or a synchrotron nebula powered by a recent outburst of energy from an unknown source. Sensitive optical and X-ray observations should be able to distinguish between these two possibilities.
  • Y Saito, N Kawai, T Kamae, S Shibata, T Dotani, Kulkarni, SR
    ASTROPHYSICAL JOURNAL, 477(1) L37-L40, Mar, 1997  Peer-reviewedLead author
    We report the first clear detection of X-ray pulsation of magnetospheric origin from a millisecond pulsar, PSR B1821-24, with the Advanced Satellite for Cosmology and Astrophysics. The photon arrival time shows a periodicity of 3.05 ms period, as observed in the radio band. The observed X-ray pulse is double peaked. The pulses are characterized by a sharp temporal profile and hard power-law spectrum with a phase-averaged photon index of similar to 1.9. These two features are quite similar to the X-ray/y-ray pulses from the Crab pulsar and characteristic of the nonthermal emission from the magnetosphere of the neutron star, but contradictory to the thermal emission from its surface. Since this pulsar has physical parameters completely different from those of young pulsars, we expect these observations to provide significant constraints on models of pulsar magnetospheric emission, which have been developed mostly based on the observations of young pulsars.
  • 大気球シンポジウム集録, 1997  
  • Y Saito, N Kawai, T Kamae, S Shibata
    PROCEEDINGS OF THE FOURTH COMPTON SYMPOSIUM, PTS 1 AND 2, (410) 628-632, 1997  
    We observed 8 pulsars with high spin down flux and searched for pulsation in the X-ray band (0.6-10 keV) with ASCA. We detected X-ray emission from all pulsars, including new detection in the 2-10 keV band for 3 pulsars. We also found pulsed emission from 3 pulsars including the first detection of millisecond pulsar PSR B1821-24 [1]. The pulse of PSR B1821-24 has sharp double peaks similar to that of the Crab pulsar and power-law spectrum which strongly suggest the magnetospheric origin. We found an empirical relation between the pulsed luminosity L-X(pulse) and the rotation energy loss (E) over dot(rot) in the X-ray band among all X-ray pulsars observed with ASCA. The pulsed luminosity is consistent with the relation L-X(pulse) proportional to (E) over dot (3/2)(rot), while those Tor the pulsed emission in gamma-ray band L-gamma(pulse) is L-gamma(pulse) proportional to (E) over dot(rot)(1/2). It should he noted that the empirical relation in the X-ray band holds also for the millisecond pulsar PSR B1821-24, which suggests same pulse emission mechanism works for millisecond pulsars.
  • T Takahashi, H Ezawa, Y Fukazawa, M Hirayama, E Idesawa, H Ikeda, Y Ishisaki, N Iyomoto, T Kamae, J Kataoka, H Kaneda, H Kubo, K Makishima, K Matsushita, K Matsuzaki, T Mizuno, T Murakami, K Nagata, S Nakamae, M Nomachi, H Obayashi, T Ohtsuka, H Ozawa, Y Saito, M Sugizaki, T Tamura, M Tashiro, N Tsuchida, K Tsukada, A Yoshida
    ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES, 120(4) C645-C648, Dec, 1996  Peer-reviewed
    The Hard X-ray Detector (HXD) is one of three instruments on the fifth Japanese X-ray astronomy satellite, ASTRO-E, scheduled for launch in 2000. The HXD consists of a 4x4 = 16 modular assembly of identical counters, each consisting of a combination of YAP(or GSO)/BGO well-type phoswich counters and silicon PIN diodes. The field of view of the detector for high energy photons is restricted to 4 degrees x 4 degrees by active collimators made of BGO and the fov for low energy photons is restricted to 0.5 degrees x 0.5 degrees by the fine passive collimators made of phosphor bronze. The detector is characterized by a low background reaching severalx10(-6) c/s/cm(2)/keV. Combined with the other two instruments for soft X-ray observations (0.5-12 keV), the ASTRO-E mission will cover the entire range of soft and hard X-rays with the highest sensitivity ever achieved. Furthermore, thick EGO counters which surround the 4x4 matrix of well-type phoswich counters act as a gamma-ray burst detector in the energy band of 100-2000 keV.
  • H Ezawa, M Hirayama, T Kamae, H Kubo, K Matsuzaki, K Nagata, Y Saito, H Ikeda, K Tsukada, Y Sano, K Shimizu, H Ozawa, T Takahashi, H Murakami
    1995 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE RECORD, VOLS 1-3, 224-228, 1996  Peer-reviewed
  • RIKEN Super Computing Prog. Rep., 2 1, 1996  
  • Procs. of X-ray Imaging and Spectroscopy of Cosmic Hot Plasmas, 403, 1996  
  • Procs. of X-ray Imaging and Spectroscopy of Cosmic Hot Plasmas, 503, 1996  
  • H KANEDA, M TASHIRO, Y IKEBE, Y ISHISAKI, H KUBO, K MAKISHIMA, T OHASHI, Y SAITO, H TABARA, T TAKAHASHI
    ASTROPHYSICAL JOURNAL, 453(1) L13-L16, Nov, 1995  Peer-reviewed
    Extended X-ray emission was detected with ASCA from the synchrotron double lobes of the radio galaxy Fornax A. This is thought to be the same emission as was detected with ROSAT. The excess X-rays exhibit very hard spectra, described by a power law of energy index 1.2 +/- 0.5. Since this index is consistent with the synchrotron. radio index of 0.9 +/- 0.2, the X-rays are thought to arise when the radio-emitting relativistic electrons make inverse-Compton scattering off the cosmic microwave photons. Comparison of the X-ray and radio fluxes yields the lobe magnetic field intensity of 2-4 mu G. The relativistic electrons in the lobes are inferred to have an energy density close to that of the magnetic fields.
  • Hidehiro Kaneda, Hajime Ezawa, Masaharu Hirayama, Tuneyoshi Kamae, Hidetoshi Kubo, Keiichi Matsuzaki, Kazuo Makishima, Takanori Ohtsuka, Yoshitaka Saito, Yutaro Sekimoto, Tadayuki Takahashi, Takayuki Tamura, Makoto Tashiro, Naohiko Tsuchida, Toshio Murakami, Mutsumi Sugizaki, Hirokazu Ikeda, Kiwamu Tsukada, Masaharu Nomachi, Shuichi Gunji, Satoshi Miyazaki, Tadahisa Tamura, Noriko Y. Yamasaki, Atsumasa Yoshida
    EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy VI, 2518 85-95, Sep 1, 1995  
    The ASTRO-E satellite is scheduled for launch in 2000 by the Institute of Space and Astronautical Science (ISAS). In this paper the design and performance of the hard x ray detector (HXD) developed for ASTRO-E are described. The HXD is a combination of YAP/BGO phoswich scintillators and silicon PIN diodes covering a wide energy band of 10 - 700 keV. The detector background is reduced down to several times 10 -6c/s/cm 2/keV, and the sensitivity of the HXD is more than one order of magnitude higher than any other past missions in the range of a few 10 keV to several 100 keV. Thus ASTRO-E HXD is expected to achieve an extreme high performance for detecting cosmic hard x rays and low-energy gamma rays. Astrophysics to be explored with the HXT are expected to be extremely widespread and rich.
  • SAITO Yoshitaka, EZAWA Hajime, KAMAE Tuneyoshi, KUBO Hidetoshi, SUZUKI Kiyoshi, SEKIMOTO Yutaro, TAKAHASHI Tadayuki, TANAKA Mitsuaki, HIRAYAMA Masaharu, MATSUZAKI Keiichi, YAJIMA Nobuyuki, YAMAGAMI Takamasa, AKIYAMA Hiromitsu, GUNJI Shuichi, TAMURA Tadahisa, NOMACHI Masaharu, MIYAZAKI Satoshi, MURAKAMI Hiroyuki, MORI Kunishiro, YAMASAKI Noriko, EDBERG Tim
    宇宙科学研究所報告. 特集, 32(32) 71-88, Mar, 1995  Peer-reviewed
    We have developed the azimuth control system utilizing a reaction wheel and a torsion relief motor for the hard X-ray/γ-ray detector Welcome-1 (mk2). In this paper, we describe the hardware characteristics and the performance obtained from the ground test and the flight data.
  • M TASHIRO, K MAKISHIMA, H EZAWA, Y FUKAWA, E IDESAWA, Y ISHISAKI, N IYOMOTO, T KAMAE, H KANEDA, K MATSUSHITA, K MATSUZAKI, Y SAITO, Y SEKIMOTO, T TAMURA, M HIRAYAMA, M ISHIDA, H KUBO, K OKADA, T TAKAHASHI, Y UEDA, K KIKUCHI, T OHASHI, NY YAMASAKI, Y KOHMURA, Y IKEBE, T MIHARA, T TSURU, K EBISAWA, S GUNJI
    EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY VI, 2518 2-12, 1995  Peer-reviewed

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    昼休みにも熱心に超小型スーパープレッシャー気球の飛翔制御の研究を行っています(ソフトテニスともいう)。いかに気球に上手に網(ネットではなく、ガット)をかぶせるが重要です。

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