Gamma-Rays from 26Al radioactivity have become a tracer of massive stars in our Galaxy, as these shed nucleosynthesis products through Wolf-Rayet winds and supernovae. With a radioactive-decay time scale of 1 Myr, ejecta from many stars and supernovae are generally superimposed. Thus, 26Al gamma-rays reflect current nucleosynthesis from massive stars in our Galaxy, and is seen from regions distributed along the plane of the Galaxy and its spiral arms.
Early INTEGRAL / SPI high-resolution spectroscopy had exploited the global signal from the inner-Galaxy's bright ridge. The 26Al gamma-ray line (E = 1809 keV) had been found to be rather narrow and in agreement with a standard moderately-turbulent ISM around typical massive-star groups. Also, encouraged by 26Al line gamma-ray energy shifts from the inner Galaxy, which were recognized and compatible with large-scale Galactic rotation, the 26Al flux was interpreted as a global Galactic quantity. Using model yields and the standard IMF, it is converted into a measurement of the current core-collapse supernova rate in our Galaxy of 1.9±1.1 supernovae per century.
Now the exposure along the Galactic plane becomes sufficient for spatially-resolved spectroscopy in the 26Al line, the signal exceeds 5σ significance in 20-degree wide bins along the bright parts of the Galactic plane. The flux in the bright inner-Galaxy ridge is determined as 2.9±0.2 *10-4 ph cm-2 s-1rad-1, and a small (~1.3 ±0.2) asymmetry favoring the fourth quadrant is indicated. The systematic shifts of line centroids from large-scale Galactic rotation are now clearly established, their detailed comparisons with expected Doppler shifts from (uncertain and model-dependent) large-scale motions in the inner Galaxy with its bar are under investigation. The line appears to be narrow with ISM velocities within the 100-km s-1 range in all samples, except for a hint of increased velocity spread towards the Aquila region. The latitudinal scale height of 26Al gamma-rays is ~130 pc and significantly exceeds the thickness of the Galactic disk in molecular gas. For the Cygnus region, a sufficently-accurate stellar census has been derived in recent years. Employing the spatial resolution of the SPI gamma-ray telescope, the 26Al flux attributed to Cygnus complex of massive stars is discriminated against the large-scale Galactic-disk emission as 3.9 ±1.1 *10-5 ph cm-2 s-1, with the Cygnus OB2 association as dominating source. This allows for a more detailed consistency check of observed flux against nucleosynthesis models for massive stars and their supernovae.
W. Wang et al.: "Spectral and intensity variations of Galactic 26Al emission", A&A 496, 713 - 724 (2009)
P. Martin et al.: "The gamma-ray line emission of the Cygnus region from INTEGRAL/SPI observations", A&A (in press) (2009)
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