Description of source "G48.99-0.30" from Kang et al. (2015)

G40.28-0.22, G48.99-0.30

G40.28-0.22 and G48.99-0.30 are the strongest 44 GHz and 95 GHz maser sources in our sample, respectively (Table 3).

G40.28-0.22 has a peak ux density of 89.2 1.4 Jy at 44 GHz and 72.7 1.0 Jy at 95 GHz. This object is associated with a luminous (Lbol ; 2.1 105 Le) YSO, which might be a hypercompact H II region (Pandian et al. 2010). Water and 44 GHz methanol masers were newly detected, while 95 GHz methanol maser emission has been detected by Chen et al. (2011) with a peak ux density of 53.2 Jy at 72.8 km s1.

Urquhart et al. (2011) searched for water maser emission at this site, but did not detect any. G48.99-0.30 has a 44 GHz peak ux density of 93.2 1.2 Jy at 66.4 km s1and a 95 GHz peak ux density of 54.2 0.9 Jy at 66.5 km s1. Both class I methanol maser transitions are new detections, whereas the water maser emission has been detected by multiple surveys (see Table 1).

For instance, Codella et al. (1994) and Valdettaro et al. (2001) observed water maser emission of 7 Jy at 71.0 km s 1 and 8 Jy at 70.9 km s 1 , respectively. Urquhart et al. (2011) detected a peak ux density of 58.9 Jy at 65.3 km s1, which is similar to our detection of 62.4 0.8 Jy at 66.0 km s1.