  We performed a spectroscopic study of the 1809 keV gamma-ray line from 26Al
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 26Al sky.
Instrumental background is estimated from independent tracers of cosmic-ray
activation. The shape of the 26Al signal is compared to the instrumental
response to extract the width of the celestial line. We detect the 26Al line at
\~16sigma 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 26Al at the time of its decay in the interstellar medium (decay
time~1.04 My) therefore are probably around 100 km/s, in agreement with
expectations from Galactic rotation and interstellar turbulence. The flux and
spatial distribution of the emission are found consistent with previous
observations. The derived amount of 26Al in the Galaxy is 2.8 (+/-0.8) M_solar.
