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 ($\tau_{\rm Dep}^{\rm m...
Gespeichert in:
| Hauptverfasser: | , , , |
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| Dokumenttyp: | Article (Journal) Kapitel/Artikel |
| Sprache: | Englisch |
| Veröffentlicht: |
2017
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| In: |
Arxiv
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| Online-Zugang: | Verlag, kostenfrei, Volltext: http://arxiv.org/abs/1706.08540
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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 |
| Zusammenfassung: | 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 ($\tau_{\rm Dep}^{\rm mol}$), the star formation efficiency per free fall time ($\epsilon_{\rm ff}$), and the mass-weighted cloud-scale (40 pc) properties of the molecular gas: surface density, $\Sigma$, line width, $\sigma$, and |
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| Beschreibung: | Gesehen am 18.10.2017 |
| Beschreibung: | Online Resource |