GRIS Measurement of High Velocity Radioactive (26) AL in the Galactic Center Region

Details GRIS Measurement of High Velocity Radioactive (26) AL in the Galactic Center Region GRIS Measurement of High Velocity Radioactive (26) AL in the Galactic Center Region

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.9301t&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #93.01; Bulletin of the American Astronomical Society, Vol. 28, p.1396

Astronomy and Astrophysics

Astronomy

Scientific paper

The Gamma Ray Imaging Spectrometer (GRIS) balloon experiment observed the 1809 keV line from the Galactic center region on a flight from Alice Springs, Australia on 24 October 1995. This line results from the decay of radioactive (26) Al. GRIS is a high resolution spectrometer capable of measuring the line profile. It was flown in a new configuration with a 100x75(deg) FOV to measure the integrated emission from the central region of our galaxy. The observed flux of 4.8+/- 0.7x 10(-4) ph s(-1) cm(-2) rad(-1) is in good agreement with previous observations. Surprisingly, the observed width of the line was 5.4+/-1.4 keV, which is much larger than the expected width from Galactic rotation (<1.8 keV). The high dispersion velocity (>450 km s(-1) ) this width implies has important consequences. It clearly favors supernova and Wolf-Rayet models which produce the (26) Al at high velocity over AGB star models that do not. The fact that the (26) Al has not come to rest in the interstellar medium after 10(6) years is very hard to square with our current understanding of the production and propogation of (26) Al in the interstellar medium.

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