Description of source "G351.24+0.67" from Voronkov et al. (2014)

This is another source from the NGC 6334 complex (source IV, which is also known as source A; see e.g. Mun˜oz et al. 2007; Hashimoto et al. 2008). The class I methanol masers are clustered around the 6.7-GHz maser, which does not appear to be associated with any mid-infrared source (Fig. 1; Caswell et al. 2010). The class II maser site 351.242+0.670 (or 351.243+0.671) is discussed extensively by Caswell & Phillips (2008). It is notable for its strong water maser which is dominated by a blueshifted outflow extending more than 100 km s−1 from the systemic velocity. Caswell & Phillips (2008) noted the non-detection of OH, with upper limit 0.4 Jy. Breen et al. (2010b) summarize additional data on nearby water masers, one associated with the infrared source located to the south of the 6.7-GHz maser and another associated with an extended H II region located in the eastern part of Fig. 1. It is worth noting that the class I masers at C are seen projected on to the edge of this H II region and may be associated with the ionization shock and, therefore, unrelated to the YSO traced by the 6.7-GHz maser. Although the strongest 44-GHz emission feature of B was fitted within the noise (by the sum of Gaussian components shown in Table 3), the red wing is systematically underestimated at the velocities greater than −3.2 km s−1.