TY - JOUR
T1 - Dense Gas, Dynamical Equilibrium Pressure, and Star Formation in Nearby Star-forming Galaxies
AU - Gallagher, Molly J.
AU - Leroy, Adam K.
AU - Bigiel, Frank
AU - Cormier, Diane
AU - Jiménez-Donaire, María J.
AU - Ostriker, Eve Charis
AU - Usero, Antonio
AU - Bolatto, Alberto D.
AU - García-Burillo, Santiago
AU - Hughes, Annie
AU - Kepley, Amanda A.
AU - Krumholz, Mark
AU - Meidt, Sharon E.
AU - Meier, David S.
AU - Murphy, Eric J.
AU - Pety, Jérôme
AU - Rosolowsky, Erik
AU - Schinnerer, Eva
AU - Schruba, Andreas
AU - Walter, Fabian
N1 - Publisher Copyright:
© 2018. The American Astronomical Society. All rights reserved..
PY - 2018/5/10
Y1 - 2018/5/10
N2 - We use new ALMA observations to investigate the connection between dense gas fraction, star formation rate (SFR), and local environment across the inner region of four local galaxies showing a wide range of molecular gas depletion times. We map HCN (1-0), HCO+ (1-0), CS (2-1), 13CO (1-0), and C18O (1-0) across the inner few kiloparsecs of each target. We combine these data with short-spacing information from the IRAM large program EMPIRE, archival CO maps, tracers of stellar structure and recent star formation, and recent HCN surveys by Bigiel et al. and Usero et al. We test the degree to which changes in the dense gas fraction drive changes in the SFR. (tracing the dense gas fraction) correlates strongly with I CO (tracing molecular gas surface density), stellar surface density, and dynamical equilibrium pressure, P DE. Therefore, becomes very low and HCN becomes very faint at large galactocentric radii, where ratios as low as become common. The apparent ability of dense gas to form stars, (where Σdense is traced by the HCN intensity and the star formation rate is traced by a combination of Hα and 24 μm emission), also depends on environment. decreases in regions of high gas surface density, high stellar surface density, and high P DE. Statistically, these correlations between environment and both and are stronger than that between apparent dense gas fraction () and the apparent molecular gas star formation efficiency . We show that these results are not specific to HCN.
AB - We use new ALMA observations to investigate the connection between dense gas fraction, star formation rate (SFR), and local environment across the inner region of four local galaxies showing a wide range of molecular gas depletion times. We map HCN (1-0), HCO+ (1-0), CS (2-1), 13CO (1-0), and C18O (1-0) across the inner few kiloparsecs of each target. We combine these data with short-spacing information from the IRAM large program EMPIRE, archival CO maps, tracers of stellar structure and recent star formation, and recent HCN surveys by Bigiel et al. and Usero et al. We test the degree to which changes in the dense gas fraction drive changes in the SFR. (tracing the dense gas fraction) correlates strongly with I CO (tracing molecular gas surface density), stellar surface density, and dynamical equilibrium pressure, P DE. Therefore, becomes very low and HCN becomes very faint at large galactocentric radii, where ratios as low as become common. The apparent ability of dense gas to form stars, (where Σdense is traced by the HCN intensity and the star formation rate is traced by a combination of Hα and 24 μm emission), also depends on environment. decreases in regions of high gas surface density, high stellar surface density, and high P DE. Statistically, these correlations between environment and both and are stronger than that between apparent dense gas fraction () and the apparent molecular gas star formation efficiency . We show that these results are not specific to HCN.
KW - galaxies: ISM
KW - galaxies: star formation
KW - radio lines: ISM
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U2 - 10.3847/1538-4357/aabad8
DO - 10.3847/1538-4357/aabad8
M3 - Article
AN - SCOPUS:85047213012
SN - 0004-637X
VL - 858
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 90
ER -