Recovering the Physical Properties of Molecular Gas in Galaxies from CO SLED Modeling

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dc.contributor.authorKamenetzky, J.
dc.contributor.authorPrivon, G. C.
dc.contributor.authorNarayanan, D.
dc.date.accessioned2024-01-10T14:21:32Z
dc.date.available2024-01-10T14:21:32Z
dc.date.issued2018
dc.description.abstractModeling of the spectral line energy distribution (SLED) of the CO molecule can reveal the physical conditions (temperature and density) of molecular gas in Galactic clouds and other galaxies. Recently, the Herschel Space Observatory and ALMA have offered, for the first time, a comprehensive view of the rotational J = 4-3 through J = 13-12 lines, which arise from a complex, diverse range of physical conditions that must be simplified to one, two, or three components when modeled. Here we investigate the recoverability of physical conditions from SLEDs produced by galaxy evolution simulations containing a large dynamical range in physical properties. These simulated SLEDs were generally fit well by one component of gas whose properties largely resemble or slightly underestimate the luminosity-weighted properties of the simulations when clumping due to nonthermal velocity dispersion is taken into account. If only modeling the first three rotational lines, the median values of the marginalized parameter distributions better represent the luminosity-weighted properties of the simulations, but the uncertainties in the fitted parameters are nearly an order of magnitude, compared to approximately 0.2 dex in the "best-case" scenario of a fully sampled SLED through J= 10-9. This study demonstrates that while common CO SLED modeling techniques cannot reveal the underlying complexities of the molecular gas, they can distinguish bulk luminosity-weighted properties that vary with star formation surface densities and galaxy evolution, if a sufficient number of lines are detected and modeled.
dc.description.funderNational Science Foundation
dc.description.funderFONDECYT Postdoctoral Fellowship
dc.description.funderUniversity of Florida
dc.description.funderNASA
dc.description.funderNSF
dc.description.funderDanish National Research Foundation
dc.fechaingreso.objetodigital2024-05-30
dc.format.extent11 páginas
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/aab3e2
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/aab3e2
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/79696
dc.identifier.wosidWOS:000432456000009
dc.information.autorucFísica; Privon GC ;S/I;1031484
dc.issue.numero1
dc.language.isoen
dc.nota.accesoContenido parcial
dc.publisherIOP PUBLISHING LTD
dc.revistaASTROPHYSICAL JOURNAL
dc.rightsacceso restringido
dc.subjectgalaxies: ISM
dc.subjectISM: molecules
dc.subjectsubmillimeter: ISM
dc.subjectPARTICLE HYDRODYNAMICS SIMULATIONS
dc.subjectLINE ENERGY-DISTRIBUTIONS
dc.subjectCO-H2 CONVERSION FACTOR
dc.subjectSTAR-FORMING GALAXIES
dc.subjectLUMINOUS GALAXIES
dc.subjectFORMATION LAW
dc.subjectHIGH-REDSHIFT
dc.subjectCLOUDS
dc.subjectTRANSITION
dc.subjectDENSITY
dc.titleRecovering the Physical Properties of Molecular Gas in Galaxies from CO SLED Modeling
dc.typeartículo
dc.volumen859
sipa.codpersvinculados1031484
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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