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Massive Star Formation in the Large Scale Structure of the Galaxy

Massive Star Formation in the Large Scale Structure of the Galaxy. David Eden Astrophysics Research Institute Liverpool John Moores University. l =30. Clump Formation Efficiency & Clump Mass Function.

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Massive Star Formation in the Large Scale Structure of the Galaxy

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  1. Massive Star Formation in the Large Scale Structure of the Galaxy David Eden Astrophysics Research Institute Liverpool John Moores University

  2. l=30

  3. Clump Formation Efficiency & Clump Mass Function Studies have shown that the clump mass function, CMF, mimics the stellar IMF (Simpson et al., 2008) and further studies are required to determine whether there is a direct mapping of the CMF to the IMF. In a similar fashion the clump formation efficiency, CFE, is analogous to the star formation efficiency in that it traces the mass of gas in dense clumps compared to the mass in the host molecular cloud.

  4. Data • BOLOCAM Galactic Plane Survey (BGPS): 1.1mm • Galactic Ring Survey (GRS) 13CO J=1-0 • JCMT HARP 13CO J=3-2

  5. Procedure The GRS cloud distance catalogue (Roman-Duval et al., 2009) and the GRS column density catalogue (Rathborne et al, 2009) were combined to give masses of the clouds within the field. The spectra at the positions of BGPS sources, as identified from the catalogue in Rosolowsky et al. (2010) were extracted and the peak velocity as well as it’s position in latitude and longitude were cross-referenced with the GRS catalogues, allowing a distance to be assigned to the source.

  6. Clump Mass Functions

  7. Clump Formation Efficiency

  8. Conclusions • The higher mass clumps are found towards the W43 star-forming complex but consistent slopes to the high-mass end of the CMF found at the tangent and away from it. • The CFE increases towards the tangent of the Galactic bar and the Scutum arm. Future Work • Assignment of all Bolocam sources to GRS clouds using the HARP 3-2 data. • The HARP data will allow temperatures and optical depths to be calculated for the entire field as both 13CO3-2 and 1-0 data is now available. • Analysis of how the CFE varies across the W43 star-forming complex to investigate it as a function of proximity to possible triggering sites.

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