2015MNRAS.453.2082D

Studies of the diffuse Galactic radio emission are interesting both for better understanding the physical conditions in our Galaxy and for minimizing the contamination in cosmological measurements. Motivated by this, we present Cosmic Background Imager 31 GHz observations of the Galactic regions NGC 6357, NGC 6334, W51 and W40 at ∼ 4.5 arcmin resolution and conduct an investigation of the spectral emission process in the regions at 4.5 arcmin and 1° resolution. We find that most of the emission in the regions is due to optically thin free-free. For two sub-regions of NGC 6334 and for a sub-region of W51 though, at 4.5 arcmin resolution and at 31 GHz we detect less emission than expected from extrapolation of radio data at lower frequencies assuming a spectral index of -0.12 for optically thin free-free emission, at 3.3σ, 3.7σ and 6.5σ, respectively. We also detect excess emission in a sub-region of NCG 6334 at 6.4σ, after ruling out any possible contribution from ultra-compact Hii regions. At 1° resolution, we detect a spinning dust component in the spectral energy distribution of W40 that accounts for 18±7 percent of the total flux density in the region at the peak frequency of 37 GHz. Comparison with 100µm data indicates an average dust emissivity for the sub-regions of 0.5±4.4µK(MJy/sr)-1. Finally, we translate the excess emission in the regions to an anomalous microwave emission (AME) emissivity relative to the optical depth at 250µm. We find that this form of emissivity is independent of the AME significance and has a value somewhere in the order of 10⁴ Jy.