Molecular Gas Properties on Cloud Scales across the Local Star-forming Galaxy Population
Author
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Sun, Jiayi
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Leroy, Adam K.
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Schinnerer, Eva
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Hughes, Annie
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Rosolowsky, Erik
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Querejeta, Miguel
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Schruba, Andreas
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Liu, Daizhong
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Saito, Toshiki
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Herrera, Cinthya N.
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Faesi, Christopher
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Usero, Antonio
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Pety, Jérôme
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Kruijssen, J. M. Diederik
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Ostriker, Eve C.
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Bigiel, Frank
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Blanc Mendiberri, Guillermo
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Bolatto, Alberto D.
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Boquien, Médéric
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Chevance, Mélanie
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Dale, Daniel A.
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Deger, Sinan
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Emsellem, Eric
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Glover, Simon C.O.
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Grasha, Kathryn
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Groves, Brent
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Henshaw, Jonathan
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Jiménez Donaire, María J.
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Kim, Jenny J.
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Klessen, Ralf S.
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Kreckel, Kathryn
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Lee, Janice C.
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Meidt, Sharon
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Sandstrom, Karin
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Sardone, Amy E.
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Utomo, Dyas
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Williams, Thomas G.
Admission date
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2021-07-24T21:48:27Z
Available date
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2021-07-24T21:48:27Z
Publication date
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2020
Cita de ítem
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The Astrophysical Journal Letters, 901:L8 (12pp), 2020 September 20
es_ES
Identifier
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10.3847/2041-8213/abb3be
Identifier
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https://repositorio.uchile.cl/handle/2250/180670
Abstract
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Using the PHANGS-ALMA CO(2-1) survey, we characterize molecular gas properties on similar to 100 pc scales across 102,778 independent sightlines in 70 nearby galaxies. This yields the best synthetic view of molecular gas properties on cloud scales across the local star-forming galaxy population obtained to date. Consistent with previous studies, we observe a wide range of molecular gas surface densities (3.4 dex), velocity dispersions (1.7 dex), and turbulent pressures (6.5 dex) across the galaxies in our sample. Under simplifying assumptions about subresolution gas structure, the inferred virial parameters suggest that the kinetic energy of the molecular gas typically exceeds its self-gravitational binding energy at similar to 100 pc scales by a modest factor (1.3 on average). We find that the cloud-scale surface density, velocity dispersion, and turbulent pressure (1) increase toward the inner parts of galaxies, (2) are exceptionally high in the centers of barred galaxies (where the gas also appears less gravitationally bound), and (3) are moderately higher in spiral arms than in inter-arm regions. The galaxy-wide averages of these gas properties also correlate with the integrated stellar mass, star formation rate, and offset from the star-forming main sequence of the host galaxies. These correlations persist even when we exclude regions with extraordinary gas properties in galaxy centers, which contribute significantly to the inter-galaxy variations. Our results provide key empirical constraints on the physical link between molecular cloud populations and their galactic environment.
es_ES
Patrocinador
dc.description.sponsorship
National Science Foundation (NSF)
1615105
1615109
1653300
National Aeronautics and Space Administration (NASA) under ADAP
NNX16AF48G
NNX17AF39G
European Research Council (ERC)
694343
Natural Sciences and Engineering Research Council of Canada (NSERC)
RGPIN-2017-03987
MINECO/FEDER
AYA2016-79006-P
MCIU/AEI/FEDER
PGC2018-094671-B-I00
German Research Foundation (DFG)
KR4801/1-1
German Research Foundation (DFG)
KR4801/2-1
European Research Council (ERC)
714907
European Unions Horizon 2020 research and innovation program
726384/EMPIRE
German Research Foundation (DFG)
138713538
Heidelberg Cluster of Excellence STRUCTURES
EXC-2181/1 -390900948
European Research Council via the ERC Synergy Grant ECOGAL
855130
European Research Council via the ERC Advanced Grant STARLIGHT
339177
German Research Foundation (DFG)
KR4598/2-1
National Science Foundation (NSF)
AST-1903834