Cloud-scale ISM structure and star formation in M51
We compare the structure of molecular gas at 40 pc resolution to the ability of gas to form stars across the disk of the spiral galaxy M51. We break the PAWS survey into 370 pc and 1.1 kpc resolution elements, and within each we estimate the molecular gas depletion time ( ##IMG## [http://ej.iop.org/...
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| Hauptverfasser: | , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2017 August 31
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| In: |
The astrophysical journal
Year: 2017, Jahrgang: 846, Heft: 1 |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/aa7fef |
| Online-Zugang: | Verlag, kostenfrei, Volltext: http://dx.doi.org/10.3847/1538-4357/aa7fef
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| Verfasserangaben: | Adam K. Leroy, Eva Schinnerer, Annie Hughes, J.M. Diederik Kruijssen, Sharon Meidt, Andreas Schruba, Jiayi Sun, Frank Bigiel, Gonzalo Aniano, Guillermo A. Blanc, Alberto Bolatto, Mélanie Chevance, Dario Colombo, Molly Gallagher, Santiago Garcia-Burillo, Carsten Kramer, Miguel Querejeta, Jerome Pety, Todd A. Thompson, and Antonio Usero |
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| 520 | |a We compare the structure of molecular gas at 40 pc resolution to the ability of gas to form stars across the disk of the spiral galaxy M51. We break the PAWS survey into 370 pc and 1.1 kpc resolution elements, and within each we estimate the molecular gas depletion time ( ##IMG## [http://ej.iop.org/images/0004-637X/846/1/71/apjaa7fefieqn1.gif] $\tau _\mathrmDep^\mathrmmol$ ), the star-formation efficiency per free-fall time ( ##IMG## [http://ej.iop.org/images/0004-637X/846/1/71/apjaa7fefieqn2.gif] $\epsilon _\mathrmff$ ), and the mass-weighted cloud-scale (40 pc) properties of the molecular gas: surface density, Σ, line width, σ , and ##IMG## [http://ej.iop.org/images/0004-637X/846/1/71/apjaa7fefieqn3.gif] | ||
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