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dc.contributorCentre for Astrophysics and Planetary Science, University of Kent, Canterbury CT2 7NH, UK; Max Planck Institute for Astronomy, Konigstuhl 17, D-69117 Heidelberg, Germany
dc.contributorCentre for Astrophysics and Planetary Science, University of Kent, Canterbury CT2 7NH, UK
dc.contributorAstrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK
dc.contributorSchool of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK
dc.contributorArmagh Observatory and Planetarium, College Hill, Armagh BT61 9DB, UK
dc.contributorSchool of Physics and Astronomy, University of Leeds, Leeds LS2 9JT UK
dc.contributor.authorWells, M. R. A.
dc.contributor.authorUrquhart, J. S.
dc.contributor.authorMoore, T. J. T.
dc.contributor.authorBrowning, K. E.
dc.contributor.authorRagan, S. E.
dc.contributor.authorRigby, A. J.
dc.contributor.authorEden, D. J.
dc.contributor.authorThompson, M. A.
dc.date.accessioned2024-02-01T17:11:20Z
dc.date.available2024-02-01T17:11:20Z
dc.date.issued2022-11-01T00:00:00Z
dc.identifier.doi10.1093/mnras/stac2420
dc.identifier.doi10.48550/arXiv.2208.11121
dc.identifier.other2022arXiv220811121W
dc.identifier.otherastro-ph.GA
dc.identifier.other2022arXiv220811121W
dc.identifier.other2022MNRAS.516.4245W
dc.identifier.other10.1093/mnras/stac2420
dc.identifier.other10.48550/arXiv.2208.11121
dc.identifier.otherarXiv:2208.11121
dc.identifier.other-
dc.identifier.other0000-0002-1605-8050
dc.identifier.other0000-0003-4164-5588
dc.identifier.other0000-0002-3351-2200
dc.identifier.other0000-0002-5881-3229
dc.identifier.urihttp://hdl.handle.net/20.500.14302/1402
dc.description.abstractThe ATLASGAL survey has characterized the properties of approximately 1000 embedded H II regions and found an empirical relationship between the clump mass and bolometric luminosity that covers 3-4 orders of magnitude. Comparing this relation with simulated clusters drawn from an initial mass function and using different star formation efficiencies we find that a single value is unable to fit the observed luminosity to mass (L/M) relation. We have used a Monte Carlo simulation to generate 200 000 clusters using the L/M-ratio as a constraint to investigate how the star formation efficiency changes as a function of clump mass. This has revealed that the star formation efficiency decreases with increasing clump mass with a value of 0.2 for clumps with masses of a few hundred solar masses and dropping to 0.08 for clumps with masses of a few thousand solar masses. We find good agreement between our results and star formation efficiencies determined from counts of embedded objects in nearby molecular clouds. Using the star formation efficiency relationship and the infrared excess time for embedded star formation of 2 ± 1 Myr we estimate the Galactic star formation rate to be approximately 0.9 ± 0.45 M<SUB>⊙</SUB> yr<SUP>-1</SUP>, which is in good agreement with previously reported values. This model has the advantage of providing a direct means of determining the star formation rate and avoids the difficulties encountered in converting infrared luminosities to stellar mass that affect previous galactic and extragalactic studies.
dc.publisherMonthly Notices of the Royal Astronomical Society
dc.titleATLASGAL - star forming efficiencies and the Galactic star formation rate
dc.typearticle
dc.source.journalMNRAS
dc.source.journalMNRAS.516
dc.source.volume516
refterms.dateFOA2024-02-01T17:11:20Z
dc.identifier.bibcode2022MNRAS.516.4245W


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