GRIS Measurement of High Velocity ^26Al from the Galactic Center Region

Details GRIS Measurement of High Velocity ^26Al from the Galactic Center Region GRIS Measurement of High Velocity ^26Al from the Galactic Center Region

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aps..apr.a1206t&link_type=abstract

American Physical Society, APS/AAPT Joint Meeting, April 18-21, 1997, abstract #A12.06

Physics

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 25 October 1995. This line results from the decay of radioactive ^26Al. GRIS is a high resolution spectrometer capable of measuring the line profile. It was flown in a new configuration with a 100×75^circ FOV to measure the integrated emission from the central region of our galaxy. The observed flux of 4.8± 0.7× 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 ^26Al at high velocity over AGB star models that do not. The fact that the ^26Al has not come to rest in the interstellar medium after 10^6 years is very hard to square with our current understanding of the interstellar medium.

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