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Proceedings Paper

MeV gamma-ray observation with a well-defined point spread function based on electron tracking
Author(s): A. Takada; T. Tanimori; H. Kubo; T. Mizumoto; Y. Mizumura; S. Komura; T. Kishimoto; T. Takemura; K. Yoshikawa; Y. Nakamasu; Y. Matsuoka; M. Oda; S. Miyamoto; S. Sonoda; D. Tomono; K. Miuchi; S. Kurosawa; T. Sawano
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Paper Abstract

The field of MeV gamma-ray astronomy has not opened up until recently owing to imaging difficulties. Compton telescopes and coded-aperture imaging cameras are used as conventional MeV gamma-ray telescopes; however their observations are obstructed by huge background, leading to uncertainty of the point spread function (PSF). Conventional MeV gamma-ray telescopes imaging utilize optimizing algorithms such as the ML-EM method, making it difficult to define the correct PSF, which is the uncertainty of a gamma-ray image on the celestial sphere. Recently, we have defined and evaluated the PSF of an electron-tracking Compton camera (ETCC) and a conventional Compton telescope, and thereby obtained an important result: The PSF strongly depends on the precision of the recoil direction of electron (scatter plane deviation, SPD) and is not equal to the angular resolution measure (ARM). Now, we are constructing a 30 cm-cubic ETCC for a second balloon experiment, Sub-MeV gamma ray Imaging Loaded-on-balloon Experiment: SMILE-II. The current ETCC has an effective area of ~1 cm2 at 300 keV, a PSF of ~10° at FWHM for 662 keV, and a large field of view of ~3 sr. We will upgrade this ETCC to have an effective area of several cm2 and a PSF of ~5° using a CF4-based gas. Using the upgraded ETCC, our observation plan for SMILE-II is to map of the electron-positron annihilation line and the 1.8 MeV line from 26Al. In this paper, we will report on the current performance of the ETCC and on our observation plan.

Paper Details

Date Published: 18 July 2016
PDF: 10 pages
Proc. SPIE 9905, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray, 99052M (18 July 2016); doi: 10.1117/12.2232171
Show Author Affiliations
A. Takada, Kyoto Univ. (Japan)
T. Tanimori, Kyoto Univ. (Japan)
H. Kubo, Kyoto Univ. (Japan)
T. Mizumoto, Kyoto Univ. (Japan)
Y. Mizumura, Kyoto Univ. (Japan)
S. Komura, Kyoto Univ. (Japan)
T. Kishimoto, Kyoto Univ. (Japan)
T. Takemura, Kyoto Univ. (Japan)
K. Yoshikawa, Kyoto Univ. (Japan)
Y. Nakamasu, Kyoto Univ. (Japan)
Y. Matsuoka, Kyoto Univ. (Japan)
M. Oda, Kyoto Univ. (Japan)
S. Miyamoto, Kyoto Univ. (Japan)
S. Sonoda, Kyoto Univ. (Japan)
D. Tomono, Kyoto Univ. (Japan)
K. Miuchi, Kobe Univ. (Japan)
S. Kurosawa, Tohoku Univ. (Japan)
T. Sawano, Kanazawa Univ. (Japan)

Published in SPIE Proceedings Vol. 9905:
Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray
Jan-Willem A. den Herder; Tadayuki Takahashi; Marshall Bautz, Editor(s)

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