High energy observation of the Galactic center region 511 keV and Al-26 lines with HEXAGONE

Details High energy observation of the Galactic center region 511 keV and Al-26 lines with HEXAGONE High energy observation of the Galactic center region 511 keV and Al-26 lines with HEXAGONE

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26as...97..185d&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 97, no. 1, p. 185-187.

Astronomy and Astrophysics

Astronomy

12

Aluminum 26, Galactic Nuclei, Gamma Ray Astronomy, Milky Way Galaxy, Astronomical Spectroscopy, Balloon-Borne Instruments, Positron Annihilation

Scientific paper

Results of the observation of the annihilation and Al-26 lines in the direction of the Galactic center during the HEXAGONE May 1989 balloon flight are presented. The observed profile and the intensity of the 511 keV line are compared with the theoretical models developed by Guessoum et al. (1991). On the assumption of a Gaussian profile with a constant step function, a flux of the annihilation line of (9.54 +/- 2.29) x 10 exp -4 ph/sq cm s is derived. It is shown that a warm medium (about 8000 K) is the best candidate to explain the annihilation of the positrons from the diffuse component of the 511 keV. In the case of Al-26, a model-dependent analysis is performed, taking into account the full response of the present detection system, together with distribution models proposed for the origin of the Al-26. Assuming a point source at the Galactic center, the flux is 1.9 x 10 exp -4 ph/sq cm s at 90 percent confidence level, and 4.6 x 10 exp -4 ph/sq cm s for a COS B-type distribution.

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