Cosmic flux of low energy gamma rays

Damle, S. V.; Daniel, R. R.; Joseph, George; Lavakare, P. J.

doi:10.1007/bf00653335

Cited by 14 publications

(6 citation statements)

References 11 publications

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“…These measurements were carried out with a 3-inch x 3-inch Na I (Tl) detector with a plastic scintillator shield and flown by balloons. A power law with spectral index ofl.8±0.2was found to be consistent with all the measurements of the diffuse cosmic flux in the 10 keV to 1 MeV range (Damle et al 1971) As a follow-up to the balloon program in gamma-ray astronomy, an Indo-Soviet joint mission for gamma-ray astronomy has been approved and is due for launch in 1993. The gamma-ray telescope consists of a multilayer drift chamber with a time-offlight system to define and accept gamma-rays entering from the front aperture, and a total energy spectrometer consisting of Na I (Tl) detectors locatedbelow the drift chamber.…”

supporting

confidence: 79%

Space Astronomy in India

Agrawal¹

1991

Publ. Astron. Soc. Aust.

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Astronomical observations from space-borne instruments are carried out in India in the areas of infrared, X-ray and gamma-ray astronomy. This paper briefly describes the facilities available in India for conducting experiments in space astronomy using balloons, rockets and satellites. It briefly reviews the important results obtained by Indian astronomers from observations made in India with the balloon, rocket and satellite experiments. The present status of research in different disciplines of space astronomy is discussed.

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supporting

confidence: 79%

Space Astronomy in India

Agrawal¹

1991

Publ. Astron. Soc. Aust.

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“…Correcting for the atmospheric background using a power law extrapolation of their growth curves, Daniel et al obtain a cosmic spectrum which is shown in Figure 11 along with other experimental points. It is clear that now they do not subscribe to the flattening around 1 MeV and are consistent with the upper Daniel et al (1972), if all the counting rate at float altitude is attributed to the cosmic component (Daniel et al, 1971).…”

Section: Energy E (Mev)mentioning

confidence: 55%

“…! Further a comparison of their count rate with that of (also shown in this figure), obtained with essentially a similar detector but at a latitude of 40° N, shows a large (a factor of 3) latitude effect and hence the presence of a large atmospheric background 5 Growth curves and extrapolations for atmospheric background used byDamle et al (1971) for two different energies.…”

mentioning

confidence: 61%

“…limits of Golenetskii et al (1971). The difference between the result of Damle et al (1971) and Daniel et al (1972) is an important lesson. These two detectors differ only in the extent that Damle et al had tried to make a better anti-coincidence shield by making it thicker and ended up having a lot more background.…”

Section: Energy E (Mev)mentioning

confidence: 87%

“…The consistent behaviour of the growth curve is indicated by the solid curves at small depths. If this is correct, as is likely in DAMLE et al (1971) o>-" 360-630 keV-5 10 50 100 ATMOSPHERIC DEPTH (g. cm" 2 ) Fig. 2.…”

Section: Work At Energies Below 1 Mevmentioning

confidence: 91%

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Diffuse Background of Energetic X-Rays

Yashpal

1973

Symp. - Int. Astron. Union

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The experimental situation in regard to the extra-galactic diffuse background of photons of energy above 30 keV is critically reviewed in the light of discussions at this Symposium.There seems to be some doubt about the spectral break at 40 keV. There is an indication of a small bump around 2 MeV and of a shoulder around 20 MeV. The spectrum below 1 MeV (down to 30 keV) can perhaps be represented as 25 (E/1 keV)–2.1. This spectrum also gives, roughly, the OSO III upper limit at 100 MeV, though it lies well below the two bumps mentioned above. A good deal of the discussion centres on the problem of backgrounds in different types of experiments to measure the diffuse X- and γ-ray fluxes.

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Die diffuse kosmische Gammastrahlung

Schönfelder

1975

Fortschr. Phys.

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Detektoren im Niederenergie-GammabereichDie gingigsten Detektoren in diesem Energiebereich sind einfache Szintillationskristalle, die zumeist aus einem Material mit hohem 8-Wert bestehen; iiblich sind NaJ(T1) oder CsJ(T1)-Kristalle. Der Kristall wird von einem dunnen Antikoinzidenzjoch aus Plastikszintillator umgeben, urn geladene Teilchen von der Registrierung auszuschlielien. Bild 2 Antikoinzidenz joch K"""iW' Na ' J "7Il -1 Bild 2. Scheinabild eines omnidirektional empfindlichen Szintillationsdetektors zeigt die MeSanordnung in einem Schemabild. Die Gammaquanten werden in dem Szintillationskristall iibe:r den Compton-und (oder) den Photoeffekt nachgewiesen, und der dabei erlittene Enei-gieverlust wird mit einem Photomultiplier gemessen. Solche Detektoren sind omnidirektional empfindlich, so da13 man keine Auskunft uber die Richtungsverteilung der Gammastrahlung erhalt. Zwar waren richtungsenipfindliche Messungen an der diffusen kosmischen Gammastrahlung sehr wiinschenswertwegen der Frage nach dem Grad der Isotropie der Strahlung. Es zeigt sich jedoch, daB sich niit diesen einfachen Szintillsitionsdetektoren im Gammabereich keine Richtungsmessungen durchfuhren lassen, auch wenn die Detektoren mit einer sehr dicken Abschirmung um-I* 4 V. SCHONFELDER geben werden. Wegen der kleinen Wirkungsquerschnitte von Comptoneffekt und Photoeffekt ist es nicht moglich, die Abschirmung so dick zu machen, daB die Strahlung vollig absorbiert wird. Dies moge in Bild 3 an Hand eines Beispieles veranschaulicht werden. Dort ist das Winkelansprechvermogen eines kleinen Szintillationskristalls aufgetragen, der sich im Inneren in der Mitte eines dicken CsJ-Kristalls (Lange 22 em, 0 14 cm) befindet. Ein Loch in der Abschirmung dient als Kollimatorspalt mit einein Offnungswinkel von etwa & 30". Die CsJ-Abschirmung ist in Antikoinzidenz zum Detektor geschaltet.

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Cosmic flux of low energy gamma rays

Cited by 14 publications

References 11 publications

Space Astronomy in India

Space Astronomy in India

Diffuse Background of Energetic X-Rays

Die diffuse kosmische Gammastrahlung

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