The Giant Molecular Cloud associated with RCW 106

Mookerjea, B.; Krämer, C.; Nielbock, M.; Nyman, L.-Å.

doi:10.1051/0004-6361:20040365

Cited by 69 publications

(169 citation statements)

References 37 publications

(61 reference statements)

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“…From observations with the VLT MIR VISIR camera, Grave et al (2014) found indications that this region consists of two main luminous sources (O4V and O5V) which account for at least half of the luminosity from this region. As well as being proximate to the Hii region G333.6-0.22, this molecular outflow source is also associated with MSX and 1.2-mm dust sources (Mookerjea et al 2004) and masers of H 2 O and OH (Batchelor et al 1980;Caswell 1998).…”

Section: G333 Outflow/infall Sourcesmentioning

confidence: 87%

“…Typical outflow masses are 10 to 40 M⊙in each lobe, compared to core masses of order Table 10. IR source fluxes in Jy measured with MSX, IRAS, TIFR balloon-borne telescope (Karnik et al 2001) and SEST/SIMBA (Mookerjea et al 2004). The second row for G333.6-0.2 is for fluxes taken within a 3 ′ aperture.…”

Section: Discussionmentioning

confidence: 99%

“…The G333.6-0.2 molecular outflow is associated with the most massive of the three HMSFRs and harbours a young OB cluster (e.g. Fujiyoshi et al 2006), with a dust mass of 1.6 × 10 4 M⊙ (Mookerjea et al 2004). The IRAS source closest to G333.6-0.2, IRAS 16183-4958, is one of the most luminous far-infrared (FIR) sources in the sky.…”

Section: G333 Outflow/infall Sourcesmentioning

confidence: 99%

“…The Mopra beam is 36 arcseconds at 3-mm wavelengths. The references are: (a) Mookerjea et al (2004); (b) Becklin et al (1973); (c) Murphy et al (2010); (d) Figuerêdo et al (2005); (e) Breen et al (2007); (f) Caswell (1998); (g) Caswell et al (1995). Ladd et al (2005) and the beam efficiencies used are as listed there.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

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Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

Wiles

Redman

et al. 2015

Mon. Not. R. Astron. Soc.

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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 arcseconds) of IRAS sources, 1.2-mm dust clumps, various masing species and radio continuum-detected Hii 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 to 40 M ⊙ in each lobe, with core masses of order 10 3 M ⊙ . outflow size scales are a few tenth of a parsec, timescales are of several ×10 4 years, mass loss rates a few ×10 −4 M ⊙ /yr. We also find the cores are turbulent and highly supersonic.

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Section: G333 Outflow/infall Sourcesmentioning

confidence: 87%

Section: Discussionmentioning

confidence: 99%

Section: G333 Outflow/infall Sourcesmentioning

confidence: 99%

Section: Observations and Data Reductionmentioning

confidence: 99%

See 2 more Smart Citations

Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

Wiles

Redman

et al. 2015

Mon. Not. R. Astron. Soc.

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“…In many works, it is assumed that (sub)millimeter clumps/clouds would have a common temperature (e.g., Mookerjea et al 2004;Kirk et al 2006;López et al 2011). This is a logical assumption in the case of isolated clouds, athough it is not valid for regions like Gum 31, where different parts of the nebula are affected by different levels of radiation.…”

Section: Identification Of Dust Clumps At 870 μMmentioning

confidence: 99%

870μm continuum observations of the bubble-shaped nebula Gum 31

Duronea

Vasquez

Gómez

et al. 2015

A&A

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Aims. We present here a study of the cold dust in the close environs of the ring nebula Gum 31. We aim at deriving the physical properties of the molecular gas and dust associated with the nebula, and investigating its correlation with the star formation in the region, which was probably triggered by the expansion of the ionization front against its environment. Methods. We make use of 870 μm emission data obtained with the Large APEX Bolometer Camera (LABOCA) to map the dust emission. The 870 μm emission provides an excellent probe of mass and density of dense molecular clouds. The obtained LABOCA image was compared to archival infrared, radio continuum, and optical images. Results. The 870 μm emission follows the 8 μm (Spitzer), 250 μm, and 500 μm (Herschel) emission distributions showing the classical morphology of a two-dimensional projection of a spherical shell. We use the 870 μm and 250 μm images to identify 60 dust clumps in the collected layers of molecular gas using the Gaussclumps algorithm. The clumps have effective deconvolved radii between 0.16 pc and 1.35 pc, masses between 70 M and 2800 M , and volume densities between 1.1 × 10 3 cm −3 and ∼2.04× 10 5 cm −3 . The total mass of the clumps is ∼37 600 M . The dust temperature of the clumps is in the range from 21 K to 32 K, while inside the Hii region it reaches ∼40 K. The clump mass distribution for the sample is fitted by a power law dN/dlog(M/M ) ∝ M −α , with α = 0.93± 0.28. The slope differs from those obtained for the stellar IMF in the solar neighborhood, suggesting that the clumps are not direct progenitors of single stars/protostars. The mass-radius relationship for the 41 clumps detected in the 870 μm emission shows that only 37% of them lie in or above the high-mass star formation threshold. Most of this 37% have candidate YSOs projected inside their limits. A comparison of the dynamical age of the Hii region with the fragmentation time, allowed us to conclude that the collect-and-collapse mechanism may be important for the star formation at the edge of Gum 31, although other processes may be acting simultaneously. The position of the identified young stellar objects in the region is also a strong indicator that the collect-and-collapse process is acting.

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