GAS KINEMATICS ON GIANT MOLECULAR CLOUD SCALES IN M51 WITH PAWS: CLOUD STABILIZATION THROUGH DYNAMICAL PRESSURE

We use the high spatial and spectral resolution of the PAWS CO(1-0) survey of the inner 9 kpc of the iconic spiral galaxy M51 to examine the effects of gas streaming motions on the star-forming properties of individual giant molecular clouds (GMCs). We compare our view of gas flows in M51-which aris...

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Bibliographic Details
Published in:The Astrophysical journal 2013-12, Vol.779 (1), p.1-22
Main Authors: Meidt, Sharon E, Schinnerer, Eva, Garcia-Burillo, Santiago, Hughes, Annie, Colombo, Dario, Pety, Jerome, Dobbs, Clare L, Schuster, Karl F, Kramer, Carsten, Leroy, Adam K, DUMAS, GALLE, Thompson, Todd A
Format: Article
Language:English
Subjects:
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CARBON MONOXIDE
Clouds
COMPARATIVE EVALUATIONS
Cosmology and Extra-Galactic Astrophysics
EMISSION
GALAXIES
GAS FLOW
Gravitation
GRAVITATIONAL INSTABILITY
MASS
Molecular clouds
Physics
RESOLUTION
Sciences of the Universe
STABILIZATION
Star formation
STARS
Surface pressure
SURFACES
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Summary:We use the high spatial and spectral resolution of the PAWS CO(1-0) survey of the inner 9 kpc of the iconic spiral galaxy M51 to examine the effects of gas streaming motions on the star-forming properties of individual giant molecular clouds (GMCs). We compare our view of gas flows in M51-which arise due to departures from axisymmetty in the gravitational potential (i.e., the nuclear bar and spiral arms)-with the global pattern of star formation as traced by H alpha and 24 mu m emission. We find that the dynamical environment of GMCs strongly affects their ability to form stars, in the sense that GMCs situated in regions with large streaming motions can be stabilized, while similarly massive GMCs in regions without streaming go on to efficiently form stars. We argue that this is the result of reduced surface pressure felt by clouds embedded in an ambient medium undergoing large streaming motions, which prevent collapse.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/779/1/45