The Atmospheric Cherenkov Technique in Searches for Exploding Primordial Black Holes

Details The Atmospheric Cherenkov Technique in Searches for Exploding Primordial Black Holes The Atmospheric Cherenkov Technique in Searches for Exploding Primordial Black Holes

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981rspta.301..665d&link_type=abstract

Philosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences, Volume 301, Issue 1462,

Astronomy and Astrophysics

Astrophysics

Scientific paper

The Cherenkov technique has been used with a number of detectors, ranging from 1.5 m2 mirrors to the Central Receiver Test Facility of 8400 m2. Limits have been set to the flux of primordial black holes for various models of the evaporation process. Although detectable γ -ray line emission from various astrophysical sources has been predicted for over two decades, it is only recently that positive results have been obtained. The first unambiguous extraterrestrial lines were from the great solar flares of 2 and 4 August 1972, at 0.5, 2.2 and 4.4 MeV. Earlier reports from balloon observations of lines from the galactic centre and Cen A near 2.2, 4.4 and 6.13 MeV seem not to have been confirmed by more recent spacecraft observations. The 0.5 MeV line seems definitely to have been seen from the galactic centre region. Lines at various energies have also been detected from transient events and during cosmic γ -ray bursts. Earlier limits from balloons were at ca. 10-3 ph cm-2s-1; recent observations and limits are nearer 10-4 ph cm-2s-1. The Gamma-Ray Observatory to be launched in 1985 will carry an array of cooled Ge detectors whose sensitivity will be ca. 10-5 ph cm-2s-1.

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