Instrument description and performance of the Imaging Gamma-Ray Telescope COMPTEL aboard the Compton Gamma-Ray Observatory

Schöenfelder, V.; Aarts, H.; Bennett, K.; Boer, H. de; Clear, J.; Collmar, W.; Connors, A.; Deerenberg, A. J. M.; Diehl, R.; Dordrecht, A. von; Herder, J. W. den; Hermsen, W.; Kippen, M.; Kuiper, L.; Lichti, G.; Lockwood, J. A.; Macri, J.; McConnell, Mark L.; Morris, D.; Much, R.; Ryan, J.; Simpson, G. A.; Snelling, M.; Stacy, G.; Steinle, H.; Strong, A. W.; Swanenburg, B. N.; Taylor, B. G.; Vries, C. P. de; Winkler, C.

doi:10.1086/191794

Cited by 492 publications

(253 citation statements)

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“…G1). ACT utilizes advances in the Compton imaging technique pioneered by COMPTEL [99]. COMPTEL employed a design with two widely separated (1.6 m) scintillator detector arrays, with moderate 2-D position resolution (~1 cm 2 ) and energy resolution (#E/E~10%).…”

Section: G Science Instrumentation Scientific Approachmentioning

confidence: 99%

The Advanced Compton Telescope mission

Boggs¹,

Kurfess²,

Ryan³

et al. 2006

New Astronomy Reviews

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Section: G Science Instrumentation Scientific Approachmentioning

confidence: 99%

The Advanced Compton Telescope mission

Boggs¹,

Kurfess²,

Ryan³

et al. 2006

New Astronomy Reviews

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“…The pioneering balloone-borne experiments ( 1976) and the COMPTEL [114] and OSSE [59] instruments aboard the Compton Observatory (1991-2000; [34]) provided a first sky survey and identified several prominent gamma-ray lines, thus confirming expectations from theory. The INTEGRAL mission [146] deepened the exploration of the nuclear-radiation sky since 2002.…”

Section: Discussionmentioning

confidence: 54%

“…CGRO had two gamma-ray spectroscopy instruments on board, the COMP-TEL Compton telescope [114], and the OSSE Spectrometer [59]; both featured a modest spectral resolution of order 10% (FWHM). This is inadequate for any gamma-ray spectroscopy in the sense of identifying new lines or constraining kinematics of source regions through line shape measurements, as we now know from high-resolution instruments based on semiconductor detectors, such as IN-TEGRAL's SPI spectrometer which provide resolutions of 0.1% .…”

Section: Telescopes For Cosmic Gamma-raysmentioning

confidence: 99%

Cosmic Gamma-Ray Spectroscopy

Diehl

2013

Astronomical Review

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Penetrating gamma-rays require complex instrumentation for astronomical spectroscopy measurements of gamma-rays from cosmic sources. Multiple-interaction detectors in space combined with sophisticated postprocessing of detector events on ground have lead to a spectroscopy performance which is now capable to provide new astrophysical insights. Spectral signatures in the MeV regime originate from transitions in the nuclei of atoms (rather than in their electron shell). Nuclear transitions are stimulated by either radioactive decays or high-energy nuclear collisions such as with cosmic rays. Gamma-ray lines have been detected from radioactive isotopes produced in nuclear burning inside stars and supernovae, and from energetic-particle interactions in solar flares. Radioactive-decay gamma-rays from 56 Ni directly reflect the source of supernova light. 44 Ti is produced in core-collapse supernova interiors, and the paucity of corresponding 44 Ti gamma-ray line sources reflects the variety of dynamical conditions herein. 26 Al and 60 Fe are dispersed in interstellar space from massive-star nucleosynthesis over millions of years. Gamma-rays from their decay are measured in detail by gamma-ray telescopes, astrophysical interpretations reach from massive-star interiors to dynamical processes in the interstellar medium. Nuclear de-excitation gamma-ray lines have been found in solar-flare events, and convey information about energetic-particle production in these events, and their interaction in the solar atmosphere. The annihilation of positrons leads to another type of cosmic gamma-ray source. The characteristic annihilation gamma-rays at 511 keV have been measured long ago in solar flares, and now throughout the interstellar medium of our Milky Way galaxy. But now a puzzle has appeared, as a surprising predominance of the central bulge region was determined. This requires either new positron sources or transport processes not yet known to us. In this paper we discuss instrumentation and data processing for cosmic gamma-ray spectroscopy, and the astrophysical issues and insights from these measurements.

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“…The photopeak efficiencies and the background rates that went into the calculation of the line sensitivities in Table 1. 2.3 × 10 −2 − 6.5 × 10 −2 1.0 × 10 −3 847 3.4 × 10 −2 4.2 × 10 −3 − 8.6 × 10 −3 2.6 × 10 −4 847 (3% FWHM) 5.2 × 10 −1 8.0 × 10 −2 − 1.6 × 10 −1 2.1 × 10 −3 (Schönfelder et al 1993). Any need for off-source observations is therefore obviated, and the total effective observation time t tot can be spent pointing at the source.…”

Section: Max-tgrs Max-nctseg Max-nctcomptmentioning

confidence: 99%

Monte Carlo study of detector concepts for the MAX Laue lens gamma-ray telescope

Weidenspointner¹,

Wunderer²,

Barrière³

et al. 2006

Focusing Telescopes in Nuclear Astrophysics

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Abstract. MAX is a proposed Laue lens gamma-ray telescope taking advantage of Bragg diffraction in crystals to concentrate incident photons onto a distant detector. The Laue lens and the detector are carried by two separate satellites flying in formation. Significant effort is being devoted to studying different types of crystals that may be suitable for focusing gamma rays in two 100 keV wide energy bands centered on two lines which constitute the prime astrophysical interest of the MAX mission: the 511 keV positron annihilation line, and the broadened 847 keV line from the decay of 56 Co copiously produced in Type Ia supernovae. However, to optimize the performance of MAX, it is also necessary to optimize the detector used to collect the source photons concentrated by the lens. We address this need by applying proven Monte Carlo and event reconstruction packages to predict the performance of MAX for three different Ge detector concepts: a standard coaxial detector, a stack of segmented detectors, and a Compton camera consisting of a stack of strip detectors. Each of these exhibits distinct advantages and disadvantages regarding fundamental instrumental characteristics such as detection efficiency or background rejection, which ultimately determine achievable sensitivities. We conclude that the Compton camera is the most promising detector for MAX in particular, and for Laue lens gamma-ray telecopes in general.

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Instrument description and performance of the Imaging Gamma-Ray Telescope COMPTEL aboard the Compton Gamma-Ray Observatory

Cited by 492 publications

References 0 publications

The Advanced Compton Telescope mission

The Advanced Compton Telescope mission

Cosmic Gamma-Ray Spectroscopy

Monte Carlo study of detector concepts for the MAX Laue lens gamma-ray telescope

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