Molecular line mapping of the giant molecular cloud associated with RCW 106 – II. Column density and dynamical state of the clumps

Wong, Tony; Ladd, E. F.; Brisbin, D.; Burton, M. G.; Bains, Indra; Cunningham, M. R.; Lo, Nadia; Jones, P. A.; Thomas, Kristen; Longmore, Steven N.; Vigan, A.; Mookerjea, B.; Krämer, C.; Fukui, Y.; Kawamura, Akiko

doi:10.1111/j.1365-2966.2008.13107.x

Cited by 64 publications

(100 citation statements)

References 56 publications

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“…This is somewhat smaller than the ratio determined in the G333 molecular cloud of ß6 by Wong et al (2008), or indeed the abundance ratio of 7.4 adopted by the same authors; however, our determination of the ratio is not sufficiently precise to test whether this amounts to a real difference. We note that only one clear (but weak) detection is seen at positive velocities in the data set.…”

Section: O and Positive Velocitiescontrasting

confidence: 40%

The Mopra Southern Galactic Plane CO Survey

Burton

Braiding

Glueck

et al. 2013

Publ. Astron. Soc. Aust.

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We present the first results from a new carbon monoxide (CO) survey of the southern Galactic plane being conducted with the Mopra radio telescope in Australia. The 12 CO, 13 CO, and C 18 O J = 1-0 lines are being mapped over the l = 305 • -345 • , b = ±0.5 • portion of the fourth quadrant of the Galaxy, at 35 arcsec spatial and 0.1 km s −1 spectral resolution. The survey is being undertaken with two principal science objectives: (i) to determine where and how molecular clouds are forming in the Galaxy and (ii) to probe the connection between molecular clouds and the 'missing' gas inferred from gamma-ray observations. We describe the motivation for the survey, the instrumentation and observing techniques being applied, and the data reduction and analysis methodology. In this paper, we present the data from the first degree surveyed, l = 323 • -324 • , b = ±0.5 • . We compare the data to the previous CO survey of this region and present metrics quantifying the performance being achieved; the rms sensitivity per 0.1 km s −1 velocity channel is ß1.5 K for 12 CO and ß0.7 K for the other lines. We also present some results from the region surveyed, including line fluxes, column densities, molecular masses, 12 CO/ 13 CO line ratios, and 12 CO optical depths. We also examine how these quantities vary as a function of distance from the Sun when averaged over the 1 square degree survey area. Approximately 2 × 10 6 M of molecular gas is found along the G323 sightline, with an average H 2 number density of n H 2 ∼ 1 cm −3 within the Solar circle. The CO data cubes will be made publicly available as they are published.

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Section: O and Positive Velocitiescontrasting

confidence: 40%

The Mopra Southern Galactic Plane CO Survey

Burton

Braiding

Glueck

et al. 2013

Publ. Astron. Soc. Aust.

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“…The determination of PDFs from molecular line data was attempted by Goodman et al (2009) andWong et al (2008), but it turned out to be problematic when these lines become optically thick and thus do not correctly reflect the molecular cloud spatial and density structure. In addition, uncertainties in the abundance can complicate conversion into H 2 column density.…”

Section: Column Density Histogram -Pdfmentioning

confidence: 99%

Large scale IRAM 30 m CO-observations in the giant molecular cloud complex W43

Carlhoff

Luong

Schilke

et al. 2013

A&A

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We aim to fully describe the distribution and location of dense molecular clouds in the giant molecular cloud complex W43. It was previously identified as one of the most massive star-forming regions in our Galaxy. To trace the moderately dense molecular clouds in the W43 region, we initiated W43-HERO, a large program using the IRAM 30 m telescope, which covers a wide dynamic range of scales from 0.3 to 140 pc. We obtained on-the-fly-maps in 13 CO (2-1) and C 18 O (2-1) with a high spectral resolution of 0.1 km s −1 and a spatial resolution of 12 . These maps cover an area of ∼1.5 square degrees and include the two main clouds of W43 and the lower density gas surrounding them. A comparison to Galactic models and previous distance calculations confirms the location of W43 near the tangential point of the Scutum arm at approximately 6 kpc from the Sun. The resulting intensity cubes of the observed region are separated into subcubes, which are centered on single clouds and then analyzed in detail. The optical depth, excitation temperature, and H 2 column density maps are derived out of the 13 CO and C 18 O data. These results are then compared to those derived from Herschel dust maps. The mass of a typical cloud is several 10 4 M while the total mass in the dense molecular gas (>10 2 cm −3 ) in W43 is found to be ∼1.9 × 10 6 M . Probability distribution functions obtained from column density maps derived from molecular line data and Herschel imaging show a log-normal distribution for low column densities and a power-law tail for high densities. A flatter slope for the molecular line data probability distribution function may imply that those selectively show the gravitationally collapsing gas.

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“…The molecular line data presented here are comprised of data from our Mopra G333 multi-molecular lines mapping (Bains et al 2006;Wong et al 2008;Lo et al 2009) as well as 12 CO maps of the individual sources. For a more detailed description of the observing procedure and data reduction steps, we refer the reader to the references mentioned immediately above.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…To provide benchmarking observational constraints for the role of turbulence in giant molecular clouds, a multimolecular line mapping of the G333 Giant Molecular Cloud (GMC) with the Mopra and Nanten2 telescopes has been undertaken (see Bains et al 2006;Wong et al 2008;Lo et al 2007Lo et al , 2009Lo et al , 2011. In collecting data for this project, we have serendipitously detected signatures of outflow and infall in three of the brighter molecular features in the GMC, which we have designated G333.6-0.2, G333.1-0.4 and G332.8-0.5.…”

Section: Introductionmentioning

confidence: 99%

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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Molecular line mapping of the giant molecular cloud associated with RCW 106 – II. Column density and dynamical state of the clumps

Cited by 64 publications

References 56 publications

The Mopra Southern Galactic Plane CO Survey

The Mopra Southern Galactic Plane CO Survey

Large scale IRAM 30 m CO-observations in the giant molecular cloud complex W43

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

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