Journal
ASTROPHYSICAL JOURNAL
Volume 892, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab781c
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Funding
- National Science Foundation (NSF) [1615105, 1615109, 1653300]
- NASA under ADAP grants [NNX16AF48G, NNX17AF39G]
- NASA under ATP grant [NNX17AG26G]
- Programme National Physique et Chimie du Milieu Interstellaire (PCMI) of CNRS/INSU
- INC/INP
- CEA
- CNES
- Programme National Cosmology et Galaxies (PNCG) of CNRS/INSU
- INP
- IN2P3
- Natural Sciences and Engineering Research Council of Canada (NSERC) [RGPIN-2017-03987]
- European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme [694343]
- Deutsche Forschungsgemeinschaft (DFG) through an Emmy Noether Research Group [KR4801/1-1]
- DFG Sachbeihilfe [KR4801/2-1]
- European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG [714907, 726384]
- Deutsche Forschungsgemeinschaft (DFG
- German Research Foundation) [138713538-SFB 881]
- Heidelberg cluster of excellence - German Excellence Strategy [EXC 2181390900948]
- Spanish funding grant (MINECO/FEDER) [AYA2016-79006-P]
- Spanish funding grant (MCIU/AEI/FEDER) [PGC2018-094671B-I00]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1615105, 1653300, 1615109] Funding Source: National Science Foundation
- NASA [905462, NNX16AF48G] Funding Source: Federal RePORTER
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We compare the observed turbulent pressure in molecular gas, P-turb, to the required pressure for the interstellar gas to stay in equilibrium in the gravitational potential of a galaxy, P-DE. To do this, we combine arcsecond resolution CO data from PHANGS-ALMA with multiwavelength data that trace the atomic gas, stellar structure, and star formation rate (SFR) for 28 nearby star-forming galaxies. We find that P-turb correlates with-but almost always exceeds-the estimated P-DE on kiloparsec scales. This indicates that the molecular gas is overpressurized relative to the large-scale environment. We show that this overpressurization can be explained by the clumpy nature of molecular gas; a revised estimate of P-DE on cloud scales, which accounts for molecular gas self-gravity, external gravity, and ambient pressure, agrees well with the observed P-turb in galaxy disks. We also find that molecular gas with cloud-scale in our sample is more likely to be self-gravitating, whereas gas at lower pressure it appears more influenced by ambient pressure and/or external gravity. Furthermore, we show that the ratio between P-turb and the observed SFR surface density, is compatible with stellar feedback-driven momentum injection in most cases, while a subset of the regions may show evidence of turbulence driven by additional sources. The correlation between P-DE in galaxy disks is consistent with the expectation from self-regulated star formation models. Finally, we confirm the empirical correlation between molecular-to-atomic gas ratio and kpc-scale P-DE reported in previous works.
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