Abstract
Abstract We present a detailed study of the γ-ray emission from the direction of the star-forming region W30 based on a decade of the Fermi Large Area Telescope data in the 0.3–300 GeV photon energy range. The morphological and spectral analyses allow us to resolve the γ-ray emission into two extended structures from different origins. One of them mostly overlaps with the supernova remnant (SNR) G8.7−0.1 and has a soft spectrum that resembles the spectra of other middle-aged SNRs interacting with molecular clouds. The other shows remarkable spatial and spectral consistency with the TeV emission from HESS J1804−216, and its spectrum could be naturally explained by inverse Compton scattering of electrons like a number of TeV γ-ray emitting pulsar wind nebulae. Thus we attribute this source to the nebula around the pulsar PSR J1803−2137.
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