The GeV Emission in the Field of the Star-forming Region W30 Revisited

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.