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10 51 erg less: the Galactic H II region OA 184

Aims. The identification of the object OA 184 as a Galactic Supernova Remnant (SNR) is re-examined, and evidence to the contrary is presented. The aim is to show definitively that OA 184 is actually a Galactic H ii region, and to estimate some physical parameters for the nebula (e.g. temperature, density, and magnetic field in the ionized shell). Methods. To determine the broad spectral properties of OA 184 a multiwavelength approach is used, with historical and new radio data, and existing X-ray and IR data on OA 184 considered. Radio continuum 408 and 1420 MHz Canadian Galactic Plane Survey (CGPS) data, Effelsberg 2695 MHz data, and new Urumqi 5 GHz radio observations in Stokes I, Q ,a ndU are presented. As well, we present CGPS H i line data, and eight radio recombination lines (RRL, H103-110α) observed for this study with the Green Bank Telescope. Results. An integrated radio spectrum of index α = −0.14 to −0.2 (S (Jy) ∝ ν α ) is determined from four radio frequencies. RRL emission appears at vLSR = −25. 8k m s −1 and at the intensity predicted for free-free thermal emission. Q and U maps at λ 6c m show OA 184 as a depolarizing source, affecting a background filament of polarized non-thermal Galactic emission. An H ii shell of thickness less than 0.2 ◦ is indicated by this depolarization. CGPS ∼1-arcminute resolution H i line maps are presented, and the systemic velocity of the ISM immediately surrounding OA 184 is −26.8 km s −1 . The distance of OA 184 is 2.2 ± 0.4 kpc, obtained from a new distance method based on a Galactic H i modelling procedure. A simple model as a shell of ionized hydrogen 4 pc thick is considered, and the RRL observations are used to estimate (under conditions of non-thermodynamic equilibrium) the electron +/− +/−