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The Cygnus region harbours a huge complex of massive stars at a distance of1.0-2.0kpc from us. About 170 O stars are distributed over several OBassociations, among which the Cyg OB2 cluster is by far the largest with about100-120 O stars. As a consequence of their successive nuclear-burning episodes,these massive stars inject large quantities of radioactive nuclei into theinterstellar medium such as 26Al and 60Fe. The gamma-ray line signal from thelatter is a solid tracer of ongoing nucleosynthesis. We want to compare thedecay emission from the Cygnus region with predictions of recently improvedstellar models. As a first step, we establish observational constraints uponthe gamma-ray line emission from 26Al and 60Fe, with particular emphasis placedon separating the emission due to the Cygnus complex from the foreground andbackground mean Galactic contributions. We used the high-resolution gamma-rayspectrometer INTEGRAL/SPI to analyse the 26Al and 60Fe decay signal from theCygnus region. The weak gamma-ray line emissions at 1809 and 1173/1332keV havebeen characterised in terms of photometry, spectrometry, and source morphology.The 1809keV emission from Cygnus is centred on the position of the Cyg OB2cluster and has a typical size of 9 degrees or more. The total 1809keV fluxfrom the Cygnus region is (6.0 +/- 1.0) x10e-5 ph/cm2/s, but the flux reallyattributable to the Cygnus complex reduces to (3.9 +/- 1.1) x10e-5 ph/cm2/s.The 1809keV line centroid is agrees with expectations considering the directionand distance of the Cygnus complex, and the line width is consistent withtypical motions of the interstellar medium. No decay emission from 60Fe hasbeen observed from the Cygnus region and an upper limit of 1.6 x10e-5 ph/cm2/swas derived.

New estimates of the gamma-ray line emission of the Cygnus region from INTEGRAL/SPI observations