TY - JOUR
T1 - Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud
AU - Lo, N.
AU - Wiles, B.
AU - Redman, M. P.
AU - Cunningham, M. R.
AU - Bains, I.
AU - Jones, P. A.
AU - Burton, M. G.
AU - Bronfman, L.
N1 - Publisher Copyright:
© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2015/11/1
Y1 - 2015/11/1
N2 - We present molecular line imaging observations of three massive molecular outflow sources, G333.6-0.2, G333.1-0.4, and G332.8-0.5, all of which also show evidence for infall, within the G333 giant molecular cloud (GMC). All three are within a beam size (36 arcsec) of IRAS sources, 1.2-mm dust clumps, various masing species, and radio continuum-detected H II regions and hence are associated with high-mass star formation. We present the molecular line data and derive the physical properties of the outflows including the mass, kinematics, and energetics and discuss the inferred characteristics of their driving sources. Outflow masses are of 10-40 M⊙ in each lobe, with core masses of the order of 103 M⊙. Outflow size scales are a few tenth of a parsec, time-scales are of several ×104 years, mass-loss rates a few ×10-4 M⊙ yr-1. We also find the cores are turbulent and highly supersonic.
AB - We present molecular line imaging observations of three massive molecular outflow sources, G333.6-0.2, G333.1-0.4, and G332.8-0.5, all of which also show evidence for infall, within the G333 giant molecular cloud (GMC). All three are within a beam size (36 arcsec) of IRAS sources, 1.2-mm dust clumps, various masing species, and radio continuum-detected H II regions and hence are associated with high-mass star formation. We present the molecular line data and derive the physical properties of the outflows including the mass, kinematics, and energetics and discuss the inferred characteristics of their driving sources. Outflow masses are of 10-40 M⊙ in each lobe, with core masses of the order of 103 M⊙. Outflow size scales are a few tenth of a parsec, time-scales are of several ×104 years, mass-loss rates a few ×10-4 M⊙ yr-1. We also find the cores are turbulent and highly supersonic.
KW - ISM: jets and outflows
KW - ISM: molecules
KW - Radio lines: ISM
KW - Stars: formation
KW - Stars: massive -HII regions
UR - http://www.scopus.com/inward/record.url?scp=84947782385&partnerID=8YFLogxK
U2 - 10.1093/mnras/stv1880
DO - 10.1093/mnras/stv1880
M3 - Article
SN - 0035-8711
VL - 453
SP - 3245
EP - 3256
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -