Kunio Takagishi

Publications (5)0 Total impact

• Source

  Available from: Michel Boër

  Article: HETE-2 Observations of the X-Ray Flash XRF 040916

  Makoto Arimoto, Nobuyuki Kawai, Atsumasa Yoshida, Toru Tamagawa, Yuji Shirasaki, Motoko Suzuki, Masaru Matsuoka, Jun'ichi Kotoku, Rie Sato, Takashi Shimokawabe, [......], Timothy Q. Donaghy, Donald Q. Lamb, Edward E. Fenimore, Mark Galassi, Michel Boer, Jean-Pascal Dezalay, Jean-Francios Olive, Joao Braga, Ravi Manchanda, Graziella Pizzichini
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  ABSTRACT: A long X-ray flash was detected and localized by the instruments aboard the High Energy Transient Explorer II (HETE-2) at 00:03:30 UT on 2004 September 16. The position was reported to the GRB Coordinates Network (GCN) approximately 2 hours after the burst. This burst consists of two peaks separated by 200 s, with durations of 110 s and 60 s. We have analyzed the energy spectra of the 1st and 2nd peaks observed with the Wide Field X-Ray Monitor (WXM) and the French Gamma Telescope (FREGATE). We discuss the origin of the 2nd peak in terms of flux variabilities and timescales. We find that it is most likely part of the prompt emission, and is explained by the long-acting engine model. This feature is similar to some bright X-ray flares detected in the early afterglow phase of bursts observed by the Swift satellite.
  04/2007;
• Source

  Available from: Eiji Nakagawa

  Article: An Optically Dark GRB Observed by HETE-2: GRB 051022

  Yujin E. Nakagawa, Atsumasa Yoshida, Satoshi Sugita, Kaoru Tanaka, Nobuyuki Ishikawa, Toru Tamagawa, Motoko Suzuki, Yuji Shirasaki, Nobuyuki Kawai, Masaru Matsuoka, [......], J. Garret Jernigan, Takanori Sakamoto, Jean-Francois Olive, Michel Boer, Edward E. Fenimore, Mark Galassi, Stanford E. Woosley, Makoto Yamauchi, Kunio Takagishi, Isamu Hatsukade
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  ABSTRACT: GRB 051022 was detected at 13:07:58 on 22 October 2005 by HETE-2. The location of GRB 051022 was determined immediately by the flight localization system. This burst contains multiple pulses and has a rather long duration of about 190 seconds. The detections of candidate X-ray and radio afterglows were reported, whereas no optical afterglow was found. The optical spectroscopic observations of the host galaxy revealed the redshift z = 0.8. Using the data derived by HETE-2 observation of the prompt emission, we found the absorption N_H = 8.8 -2.9/+3.1 x 10^22 cm^-2 and the visual extinction A_V = 49 -16/+17 mag in the host galaxy. If this is the case, no detection of any optical transient would be quite reasonable. The absorption derived by the Swift XRT observations of the afterglow is fully consistent with those obtained from the early HETE-2 observation of the prompt emission. Our analysis implies an interpretation that the absorbing medium could be outside external shock at R ~ 10^16 cm, which may be a dusty molecular cloud.
  06/2006;
• Article: SPIE's 1996 International Symposium on Optical Science, Engineering, and Instrumentation

  Fuyuki Tokanai, Masaru Matsuoka, Nobuyuki Kawai, Atsumasa Yoshida, Makoto Yamauchi, Kunio Takagishi, Isamu Hatsukade, Edward E. Fenimore, Mark C. Galassi, Jean J. M. in't Zand, Ian A. Bond, Kohji Morimoto, Hiroshi Nakamura
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  ABSTRACT: The wide-field x-ray monitor (WXM) is one of the three scientific instruents onboard high energy transient experiment (HETE) satellite, which was launched in 1996. The primary objective of HETE is to carry out the first multi- wavelength study of gamma-ray bursts with UV, x-ray, and gamma-ray instruments mounted on a single, compact spacecraft. WXM has been designed to undertake comprehensive x-ray spectra observations and quickly determine small error boxes of GRB locations within a large field of view of about 1.5 steradian. It is based on the principle of coded aperture imaging. It has four identical one-dimensional position sensitive proportional counters (PSPCs), one pair in each of two orthogonal directions. Each PSPC is filled with 1.4 atm Xe (97%) and CO2 (3%), equipped with three resistive carbon anodes of 10 micrometer diameter, and sensitive to x-rays between 2 and 25 keV. It provides position resolution of about 1.0 mm (FWHM), and energy resolution of about 17% (FWHM) at 8 keV.© (1996) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.
  10/1996;
• Article: HETE2衛星と連携したフォローアップ観測によるγ線バーストの研究

  誠 山内, 邦夫 高岸, 勇 廿日出, 英之 松澤, Makoto Yamauchi, Kunio Takagishi, Isamu Hatsukade, Hideyuki Matsuzawa, マコト ヤマウチ, クニオ タカギシ, イサム ハツカデ, ヒデユキ マツザワ
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  ABSTRACT: 平成13年度～平成16年度 科学研究費補助金 (基盤研究(C)(2)) 研究成果報告書 論文別刷 Lamb, D. Q., Ricker, G. R., Atteia, J. -., Barraud, G., Boër, M., Braga, J., et al. (2004). Scientific highlights of the HETE-2 mission. Nuclear Physics B - Proceedings Supplements, 132, 279-288 10.1016/j.nuclphysbps.2004.04.049
• Article: 衛星と地上観測機関の連携によるガンマ線バーストの研究

  誠 山内, 邦夫 高岸, 勇 廿日出, 篤正 吉田, Makoto Yamauchi, Kunio Takagishi, Isamu Hatsukade, Atsumasa Yoshida, マコト ヤマウチ, クニオ タカギシ, イサム ハツカデ, アツマサ ヨシダ
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  ABSTRACT: 平成9年度～平成12年度 科学研究費補助金 (基盤研究(C)(2)) 研究成果報告書