ATLASGAL - star forming efficiencies and the Galactic star formation rate
dc.contributor | Centre for Astrophysics and Planetary Science, University of Kent, Canterbury CT2 7NH, UK; Max Planck Institute for Astronomy, Konigstuhl 17, D-69117 Heidelberg, Germany | |
dc.contributor | Centre for Astrophysics and Planetary Science, University of Kent, Canterbury CT2 7NH, UK | |
dc.contributor | Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK | |
dc.contributor | School of Physics and Astronomy, Cardiff University, Queen's Buildings, The Parade, Cardiff CF24 3AA, UK | |
dc.contributor | Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DB, UK | |
dc.contributor | School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT UK | |
dc.contributor.author | Wells, M. R. A. | |
dc.contributor.author | Urquhart, J. S. | |
dc.contributor.author | Moore, T. J. T. | |
dc.contributor.author | Browning, K. E. | |
dc.contributor.author | Ragan, S. E. | |
dc.contributor.author | Rigby, A. J. | |
dc.contributor.author | Eden, D. J. | |
dc.contributor.author | Thompson, M. A. | |
dc.date.accessioned | 2024-02-01T17:11:20Z | |
dc.date.available | 2024-02-01T17:11:20Z | |
dc.date.issued | 2022-11-01T00:00:00Z | |
dc.identifier.doi | 10.1093/mnras/stac2420 | |
dc.identifier.doi | 10.48550/arXiv.2208.11121 | |
dc.identifier.other | 2022arXiv220811121W | |
dc.identifier.other | astro-ph.GA | |
dc.identifier.other | 2022arXiv220811121W | |
dc.identifier.other | 2022MNRAS.516.4245W | |
dc.identifier.other | 10.1093/mnras/stac2420 | |
dc.identifier.other | 10.48550/arXiv.2208.11121 | |
dc.identifier.other | arXiv:2208.11121 | |
dc.identifier.other | - | |
dc.identifier.other | 0000-0002-1605-8050 | |
dc.identifier.other | 0000-0003-4164-5588 | |
dc.identifier.other | 0000-0002-3351-2200 | |
dc.identifier.other | 0000-0002-5881-3229 | |
dc.identifier.uri | http://hdl.handle.net/20.500.14302/1402 | |
dc.description.abstract | The 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.publisher | Monthly Notices of the Royal Astronomical Society | |
dc.title | ATLASGAL - star forming efficiencies and the Galactic star formation rate | |
dc.type | article | |
dc.source.journal | MNRAS | |
dc.source.journal | MNRAS.516 | |
dc.source.volume | 516 | |
refterms.dateFOA | 2024-02-01T17:11:20Z | |
dc.identifier.bibcode | 2022MNRAS.516.4245W |