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Dynamical Equilibrium in the Molecular ISM in 28 Nearby Star-Forming Galaxies | | Jiayi Sun
; Adam K. Leroy
; Eve C. Ostriker
; Annie Hughes
; Erik Rosolowsky
; Andreas Schruba
; Eva Schinnerer
; Guillermo A. Blanc
; Christopher Faesi
; J. M. Diederik Kruijssen
; Sharon Meidt
; Dyas Utomo
; Frank Bigiel
; Alberto D. Bolatto
; Mélanie Chevance
; I-Da Chiang
; Daniel Dale
; Eric Emsellem
; Simon C. O. Glover
; Kathryn Grasha
; Jonathan Henshaw
; Cinthya N. Herrera
; Maria Jesus Jimenez-Donaire
; Janice C. Lee
; Jérôme Pety
; Miguel Querejeta
; Toshiki Saito
; Karin Sandstrom
; Antonio Usero
; | | Date: |
20 Feb 2020 | | Abstract: | We compare the observed turbulent pressure in molecular gas,
$P_mathrm{turb}$, to the required pressure for the interstellar gas to stay in
equilibrium in the gravitational potential of a galaxy, $P_mathrm{DE}$. To do
this, we combine arcsecond resolution CO data from PHANGS-ALMA with
multi-wavelength data that traces the atomic gas, stellar structure, and star
formation rate (SFR) for 28 nearby star-forming galaxies. We find that
$P_mathrm{turb}$ correlates with, but almost always exceeds the estimated
$P_mathrm{DE}$ on kiloparsec scales. This indicates that the molecular gas is
over-pressurized relative to the large-scale environment. We show that this
over-pressurization can be explained by the clumpy nature of molecular gas; a
revised estimate of $P_mathrm{DE}$ on cloud scales, which accounts for
molecular gas self-gravity, external gravity, and ambient pressure, agrees well
with the observed $P_mathrm{turb}$ in galaxy disks. We also find that
molecular gas with cloud-scale
${P_mathrm{turb}}approx{P_mathrm{DE}}gtrsim{10^5,k_mathrm{B},mathrm{K,cm^{-3}}}$
in our sample is more likely to be self-gravitating, whereas gas at lower
pressure appears more influenced by ambient pressure and/or external gravity.
Furthermore, we show that the ratio between $P_mathrm{turb}$ and the observed
SFR surface density, $Sigma_mathrm{SFR}$, 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 $Sigma_mathrm{SFR}$ and kpc-scale $P_mathrm{DE}$ 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 $P_mathrm{DE}$ reported in previous works. | | Source: | arXiv, 2002.8964 | | Services: | Forum | Review | PDF | Favorites | |
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