G&M to Challenge Poolbeg with Light Fiction

The SOFIA Massive (SOMA) Star Formation Survey. II. High Luminosity Protostars

“…Conversely, a Class I methanol maser was detected by Walsh et al (2007) 3 due east of G305B, and they are generally only found in outflows. Walsh et al (2001) observed the 6.7 GHz methanol maser site G305A in the MIR (10.5 µm and 20 µm) and found that G305A is not associated with any MIR source. G305A is out of the field of our Gemini images.…”

“…The brightest MIR source appears to be associated with the methanol masers of G305B, but does not possess detectable radio continuum emission (below a 4σ detection limit of 0.9 mJy beam −1 (beam ∼ 1.5 ) at 8.6 GHz in Phillips et al 1998, and a 3σ detection limit of 0.09 mJy at 18 GHz in Walsh et al 2007). Walsh et al (2007) found no HC 3 N, NH 3 , OCS, or water at the position of G305B and proposed that it has evolved enough to the point that it has already had time to clear out its surrounding molecular material. By contrast, Boley et al (2013) proposed G305B is a massive protostar in a pre-UCHII-region stage.…”

“…We could corroborate the outflow cavity hypothesis if we had evidence of an outflow and knew its angle. Walsh et al (2006) did image the area in commonly used outflow tracers 13 CO and HCO + , and presented the data as integrated emission maps. However, the emission appears to peak on G305A and extends at larger scales in a direction parallel to the dark lane orientation, tracing the location of the extended 1.2 mm continuum emission (rather than an outflow).…”

“…However, the emission appears to peak on G305A and extends at larger scales in a direction parallel to the dark lane orientation, tracing the location of the extended 1.2 mm continuum emission (rather than an outflow). However, if the hypothesis of Walsh et al (2007) is correct, i.e., that due to low chemical abundance this source is more evolved and has cleared much of its surrounding molecular material, then the source may have passed the stage where it would exhibit an active outflow. Conversely, a Class I methanol maser was detected by Walsh et al (2007) 3 due east of G305B, and they are generally only found in outflows.…”

“…However, if the hypothesis of Walsh et al (2007) is correct, i.e., that due to low chemical abundance this source is more evolved and has cleared much of its surrounding molecular material, then the source may have passed the stage where it would exhibit an active outflow. Conversely, a Class I methanol maser was detected by Walsh et al (2007) 3 due east of G305B, and they are generally only found in outflows. Walsh et al (2001) observed the 6.7 GHz methanol maser site G305A in the MIR (10.5 µm and 20 µm) and found that G305A is not associated with any MIR source.…”