Search for TeV gamma ray emission from PSR 1957 + 20

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Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...232l...5a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 232, no. 1, June 1990, p. L5-L8.

Astronomy and Astrophysics

Astronomy

4

Eclipsing Binary Stars, Gamma Ray Astronomy, Gamma Rays, Pulsars, Stellar Radiation, Cerenkov Radiation, Gamma Ray Telescopes

Scientific paper

The recently discovered eclipsing millisecond binary pulsar PSR 1957 + 20 was observed in order to detect emission of gamma rays in the TeV energy range during April-May 1989 using the atmospheric Cerenkov telescope at Pachmarhi, India. No significant emission of TeV gamma-rays, either pulsed or steady, was seen in any orbital phase interval. Three sigma upper limits for the steady emission of gamma-rays of energy greater than 4.3 TeV during orbital phase intervals corresponding to the eclipse and the Lagrange points L4 and L5 are given as 4.1 x 10 to the -11th, 1.9 x 10 to the -10th, and 1.8 x 10 to the -10th, gamma/sq cm per sec, respectively. A time-averaged three sigma upper limit of 1.4 x 10 to the -11th, gamma/sq cm per sec is placed on pulsed emission of gamma-rays at the same energies, with a periodicity of that of the pulsar.

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