ner_tags: O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software B-Software I-Software I-Software I-Software O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O B-CelestialObject I-CelestialObject O B-Citation O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O B-CelestialObject O O O O O O O O O O O O O O B-CelestialObject B-CelestialObject O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject O O O O B-CelestialObject O B-CelestialObject O O O O O O O B-CelestialObject O O O O O B-Wavelength O B-Wavelength O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O B-CelestialObject O O O O B-CelestialObject O O O O B-CelestialObject O O O O B-CelestialObject O O O O O B-CelestialObject O O O O O O O O O B-CelestialObject O O O O B-CelestialObject O O O O B-CelestialObject O O O O O B-CelestialObject O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O B-Wavelength I-Wavelength B-Observatory O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-CelestialObject O O O O O O O O B-Observatory O O O O O O O B-Wavelength I-Wavelength B-Telescope O O O O O O O O O O O B-Observatory O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O B-CelestialObject O O O B-CelestialObject O O O B-CelestialObject O O O B-CelestialObject O O O B-CelestialObject O O O B-CelestialObject O O O B-CelestialObject
tokens: and calibrated with the use of miriad (Sault, Teuben Wright 1995 ). miriad was also used to perform phase and target self-calibration as well as final imaging of each configuration. The images were then primary beam corrected and exported to casa (Common Astronomy Software Applications) for processing. The 6 km and 750 m images were analysed within casa to determine flux densities and ejecta dimensions. The final set of images created had varying resolutions. The 6 km pointing at 5.5 GHz had a beam size of 2.92 × 1.54 arcsec (PA −2.50°) and at 9 GHz, a beam size of 1.71 × 0.99 arcsec (PA 0.79°). Images created from the 750 m pointing had a beam size of 13.79 × 6.98 arcsec (PA 5.04°) at 5.5 GHz, and 6.98 × 4.44 arcsec (PA 6.28°) at 9 GHz. Calibration and imaging is still on-going for the 1.5 km pointings at both spectral windows. A full combination of all the data is underway, with results from the concatenated data set to be provided in a future work (Andrews, in preparation). In this letter we focus on the presence of asymmetric spatially extended emission associated with all but one of the cool super/hypergiants, seen in the 5.5 GHz observations at the 6 km pointing. Clark et al. ( 1998 ) previously identified a cometary nebula around the RSG Wd1-26, with D10 confirming similar nebulosity around a second RSG Wd1-20, and an elliptical structure around a third RSG, Wd1-237, as well as more compact but still extended emission around three of the YHGs, Wd1-4a, -12a, and -265. The greater sensitivity of our new observations reveals striking additional detail for these structures, while resolving the nebulae associated with the last RSG, Wd1-75 and two further YHGS, Wd1-16, and -32. This leaves only a single cluster YHG, Wd1-8, with no detection at any mm or radio frequency. In Fig. 1 we present 5.5 GHz maps of these six stars, while Fig. 2 presents an optical/radio montage indicating the nebulae location and orientation. Figure 1. Shown are images of the YHGs and RSGs and their associated extended emission, from the 5.5 GHz observations at 6 km. Sources are the YHGs Wd1-4a (top − left) , Wd1-12a (top − centre) , Wd1-265 (top − right) , Wd1-16a (middle − left) , and Wd1-32 (centre) . These images are followed by the RSGs, Wd1-20 (middle − right) , Wd1-26 (bottom − left) , Wd-237 (bottom − centre) , and Wd1-75 (bottom − right) . The colourscale shows the hypergiants from the 5.5 GHz observations at the 6 km pointing, with the overlaid contours from 100 GHz ALMA observations of the cluster with a resolution of 750 × 570 mas (Fenech et al. 2018 ). W265 was out of the field of view for ALMA, so is overlaid with contours of the 9 GHz ATCA observations from the 6 km pointing. The contour levels of the ALMA observations are −1, 1, 1.414, 2, 2.828, 4, 5.656, 8, 11.31, 16, 22.62, 32, 45.25, 64, and 90.50 × 3σ (σ = 52.4 Jy for Wd1-4a, 40.0 Jy for Wd1-12a, 24.3 Jy for Wd1-16a, 28.1 Jy for Wd1-32, 30.5 Jy for Wd1-20, 63.7 Jy for Wd1-26, 31.9 Jy for Wd1-237