High-Mass Star-Forming Regions in the G333 Cloud Indra Bains
& the DQS team Slide 2 A B C D E Slide 3 Source A CO channel
maps 12 CO contours, 13 CO greyscale Slide 4 * MSX source H2O maser
OH maser HII region 1.2 mm source IRAS error ellipse Absorption
features Self-absorbed 12 CO 13 CO CS SiO A Slide 5 Source C
molecular outflow 12 CO CS * MSX source H2O maser OH maser star
CH3OH maser 1.2 mm source IRAS error ellipse CS Slide 6 Source D
molecular outflow * MSX source OH maser 1.2 mm source IRAS error
ellipse 12 CO CS Slide 7 Outflow analysis T 13 > 5 , T 12 > 5
, T 12 /T 13 > 1: T 12 /T 13 = 1-e 13 /1-e 13 12 = 13 = 45 12 =
15-130 Calculate Tex ( 12 CO); N 12 assuming all levels thermalised
etc T 13 > 5 , T 12 > 5 , T 12 /T 13 5 , T 12 < 5 : N 13
in optically thin limit, Tex=7.5 K T 12 > 5 , T 13 < 5 , (eg
wings, larger spatial offsets) 12 = 15, calculate Tex( 12 CO), N 12
M(x,y,v) = m mol N H2 V(x,y,v) N H2 = XN CO d=3.6 kpc Slide 8
Outflow properties Source C: M out = 5.5e3 Mo (M 1.2mm = 7.2e3 Mo
Mookerjea et al 2004) Source D: M out = 2.1e3 Mo (M 1.2mm = 5.5e3
Mo) KE ~ 10^49 erg Slide 9 ATCA observations Freq (MHz) typical
beam (``x``) mode 1384 14.10 x 8.90 c 2368 8.37 x 5.22 c 4800 4.37
x 2.23 c 8640 2.36 x 1.22 c 22369 0.83 x 0.58 RRL + c 89209 2.16 x
1.75 HCO + + c Slide 10 Source C radio continuum 1384 MHz 2368 MHz
4800 MHz 8640 MHz Slide 11 Source C SED = 1.2 22 GHz89 GHz Slide 12
Source C properties 3 mm dust mass lower limit 6.6e3 Mo (T d = 40
K), 1.4e4 Mo (T d = 20 K) c.f. 1.2 mm mass 4.6e3 Mo (T d = 40 K;
Mookerjea et al 2004) 22 GHz deconvolved size 0.02 pc Assuming
22GHz
