A Herschel Space Observatory Spectral Line Survey of Local Luminous Infrared Galaxies from 194 to 671 Microns

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dc.contributor.authorLu, Nanyao
dc.contributor.authorZhao, Yinghe
dc.contributor.authorDiaz Santos, Tanio
dc.contributor.authorKevin Xu, C.
dc.contributor.authorGao, Yu
dc.contributor.authorArmus, Lee
dc.contributor.authorIsaak, Kate G.
dc.contributor.authorMazzarella, Joseph M.
dc.contributor.authorvan der Werf, Paul P.
dc.contributor.authorAppleton, Philip N.
dc.contributor.authorCharmandaris, Vassilis
dc.contributor.authorEvans, Aaron S.
dc.contributor.authorHowell, Justin
dc.contributor.authorIwasawa, Kazushi
dc.contributor.authorLeech, Jamie
dc.contributor.authorLord, Steven
dc.contributor.authorPetric, Andreea O.
dc.contributor.authorPrivon, George C.
dc.contributor.authorSanders, David B.
dc.contributor.authorSchulz, Bernhard
dc.contributor.authorSurace, Jason A.
dc.date.accessioned2024-01-10T12:37:29Z
dc.date.available2024-01-10T12:37:29Z
dc.date.issued2017
dc.description.abstractWe describe a Herschel Space Observatory 194-671 mu m spectroscopic survey of a sample of 121 local luminous infrared galaxies and report the fluxes of the CO J to J-1 rotational transitions for 4 <= J <= 13, the [N II] 205 mu m line, the [C I] lines at 609 and 370 mu m, as well as additional and usually fainter lines. The CO spectral line energy distributions (SLEDs) presented here are consistent with our earlier work, which was based on a smaller sample, that calls for two distinct molecular gas components in general: (i) a cold component, which emits CO lines primarily at J less than or similar to 4 and likely represents the same gas phase traced by CO (1-0), and (ii) a warm component, which dominates over the mid-J regime (4 < J less than or similar to 10) and is intimately related to current star formation. We present evidence that the CO line emission associated with an active galactic nucleus is significant only at J > 10. The flux ratios of the two [C I] lines imply modest excitation temperatures of 15-30 K; the [C I] 370 mu m line scales more linearly in flux with CO (4-3) than with CO (7-6). These findings suggest that the [C I] emission is predominantly associated with the gas component defined in (i) above. Our analysis of the stacked spectra in different far-infrared (FIR) color bins reveals an evolution of the SLED of the rotational transitions of H2O vapor as a function of the FIR color in a direction consistent with infrared photon pumping.
dc.description.funderNASA
dc.description.funderNatural Science Foundation of China (NSFC)
dc.description.funderCAS
dc.description.funderALMA-CONICYT project
dc.description.funderFONDECYT
dc.description.funderEU FP7 Grant
dc.description.funderSpanish MINECO
dc.description.funderICCUB (Unidad deExcelencia "Maria de Maeztu")
dc.description.funderNational Aeronautics and Space Administration
dc.description.funderICREA
dc.fechaingreso.objetodigital2024-05-30
dc.format.extent34 páginas
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4365/aa6476
dc.identifier.eissn1538-4365
dc.identifier.issn0067-0049
dc.identifier.urihttps://doi.org/10.3847/1538-4365/aa6476
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/76858
dc.identifier.wosidWOS:000400578000001
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 SUPPLEMENT SERIES
dc.rightsacceso restringido
dc.subjectgalaxies: active
dc.subjectgalaxies: ISM
dc.subjectgalaxies: star formation
dc.subjectinfrared: galaxies
dc.subjectISM: molecules
dc.subjectsubmillimeter: galaxies
dc.subjectACTIVE GALACTIC NUCLEUS
dc.subjectEXTREME STAR-FORMATION
dc.subjectWARM MOLECULAR GAS
dc.subjectHIGH-J CO
dc.subjectATOMIC CARBON
dc.subjectHYDROGEN-FLUORIDE
dc.subjectNGC 4418
dc.subjectARP 220
dc.subjectSUBMILLIMETER EMISSION
dc.subjectMIDINFRARED PROPERTIES
dc.titleA Herschel Space Observatory Spectral Line Survey of Local Luminous Infrared Galaxies from 194 to 671 Microns
dc.typeartículo
dc.volumen230
sipa.codpersvinculados1031484
sipa.indexWOS
sipa.indexScopus
sipa.trazabilidadCarga SIPA;09-01-2024
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