We performed a spectroscopic study of the 1809 keV gamma-ray line from ^ { 26 } Al decay in the Galaxy using the SPI imaging spectrometer with its high-resolution Ge detector camera on the INTEGRAL observatory .
We analyzed observations of the first two mission years , fitting spectra from all 7130 telescope pointings in narrow energy bins to models of instrumental background and the ^ { 26 } Al sky .
Instrumental background is estimated from independent tracers of cosmic-ray activation .
The shape of the ^ { 26 } Al signal is compared to the instrumental response to extract the width of the celestial line.We detect the ^ { 26 } Al line at \simeq 16 \sigma significance .
The line is broadened only slightly , if at all ; we constrain the width to be below 2.8 keV ( FWHM , 2 \sigma ) .
The average Doppler velocities of ^ { 26 } Al at the time of its decay in the interstellar medium ( \tau \sim 1.04 My ) therefore are probably around 100 km s ^ { -1 } , in agreement with expectations from Galactic rotation and interstellar turbulence .
The flux ( 3.3 ( \pm 0.4 ) 10 ^ { -4 } ph cm ^ { -2 } s ^ { -1 } rad ^ { -1 } ) and spatial distribution of the emission are found consistent with previous observations .
The derived amount of ^ { 26 } Al in the Galaxy is 2.8 ( \pm 0.8 ) M _ { \odot } .