High-Mass Star-Forming Regions in the G333 Cloud

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High-Mass Star-Forming Regions in the G333 Cloud

• Indra Bains the DQS team

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(No Transcript)
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Source A CO channel maps
12CO contours, 13CO greyscale
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A
Self-absorbed
12CO
13CO
Absorption features
CS
SiO
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Source C molecular outflow
12CO
CS
CS
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Source D molecular outflow
12CO
CS
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Outflow analysis

• T13 gt 5?, T12 gt 5?, T12/T13 gt 1
• T12/T13 1-e??13/1-e?13 ?12??13 ? 45
• ?12 15-130
• Calculate Tex (12CO) N12 assuming all levels
  thermalised etc
• T13 gt 5?, T12 gt 5?, T12/T13 lt 1 (eg line centres)
  or T13 gt 5?, T12 lt 5?
• N13 in optically thin limit, Tex7.5 K
• T12 gt 5?, T13 lt 5?, (eg wings, larger spatial
  offsets)
• ?12 15, calculate Tex(12CO), N12
• M(x,y,v) mmol NH2 V(x,y,v) NH2 XNCO d3.6
  kpc

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Outflow properties

• Source C Mout 5.5e3 Mo (M1.2mm 7.2e3 Mo
  Mookerjea et al 2004)
• Source D Mout 2.1e3 Mo (M1.2mm 5.5e3 Mo)
• KE 1049 erg

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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

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Source C radio continuum
1384 MHz
2368 MHz
4800 MHz
8640 MHz
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Source C SED
22 GHz
89 GHz
? 1.2
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Source C properties

• 3 mm dust mass lower limit 6.6e3 Mo (Td 40 K),
  1.4e4 Mo (Td 20 K)
• c.f. 1.2 mm mass 4.6e3 Mo (Td 40 K Mookerjea
  et al 2004)
• 22 GHz deconvolved size 0.02 pc
• Assuming ?22GHz ltlt 1 (lower limit)
• Ni 4.4e48 s-1 1 ZAMS O7 (Panagia 1973)
• EM 1.4e9 pc cm-6
• ne 2.4e5 cm-3
• Mion 0.03 Mo
• Assuming vexp cs 11.4 km s-1 t 1e3 yr
• UCHII region

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Source D radio continuum
2368 MHz
2368 MHz
4800 MHz
8640 MHz
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Source D SED
22GHz
89 GHz
?23681384 3.0 ?86404800 0.6
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Source D properties

• 3 mm dust mass lower limit 2.1e3 Mo (Td 40 K),
  4.4e3 Mo (Td 20 K)
• c.f. 1.2 mm mass 5.5e3 Mo (Td 40 K Mookerjea
  et al 2004)
• 22 GHz deconvolved size 0.03 pc
• Assuming ?22GHz ltlt 1 within resolution effects
• Ni 5.7e48 s-1 1 ZAMS O6.5 (Panagia 1973)
• EM 1.4e9 pc cm-6
• ne 2.1e5 cm-3
• Mion 0.1 Mo
• UCHII region

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Summary

• G333 cloud contains massive bipolar outflows with
  HII regions in the centre
• Line modelling
• NANTEN2 observations of higher J transitions
• ATCA HCO data
• Obtaining 2 more RRLs to solve for broadening
  terms, hence Te, ne etc in HII regions