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Determining star formation rates for infrared galaxies

dc.contributor.authorRieke, G. H.
dc.contributor.authorAlonso Herrero, A.
dc.contributor.authorWeiner, B. J.
dc.contributor.authorPérez González, Pablo Guillermo
dc.contributor.authorBlaylock, M.
dc.contributor.authorDonley, J. L.
dc.contributor.authorMarcillac, D.
dc.date.accessioned2023-06-20T04:16:38Z
dc.date.available2023-06-20T04:16:38Z
dc.date.issued2009-02-10
dc.description© 2009 The American Astronomical Society. All rights reserved. We are grateful for helpful discussions with Phil Appleton, Chad Engelbracht, and Robert Kennicutt. We also thank Daniela Calzetti for providing the Paα measurements, Jennifer Sierchio for resampling the LIRG and ULIRG SEDs onto a common wavelength scale, Eckhard Sturm for providing the PACS response curves, and Alistair Glasse for providing MIRI response curves. We also thank the FIDEL team, led by Mark Dickinson, for the data presented in Figures 17 and 18. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. This research has used the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory under contract with NASA. It also makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. Support for this work was provided by NASA through JPL/Caltech contract 1255094 and by NAG5-12318 from NASA/Goddard to the University of Arizona. Funding for the DEEP2 survey has been provided by NSF grants AST95- 09298, AST-0071048, AST-0071198, AST-0507428, and AST- 0507483 as well as NASA LTSA grant NNG04GC89G. P. G. Pérez González acknowledges support from the grants PNAYA ´ 2006–02358 and PNAYA 2006–15698–C02–02 and from the Ramón y Cajal Program, financed by the Spanish Government and the European Union.
dc.description.abstractWe show that measures of star formation rates (SFRs) for infrared galaxies using either single-band 24 μm or extinction-corrected Paα luminosities are consistent in the total infrared luminosity = L(TIR) ~ 10^10 L_☉ range. MIPS 24 μm photometry can yield SFRs accurately from this luminosity upward: SFR(M_☉ yr^–1) = 7.8 × 10^–10 L(24 μm, L_☉) from L(TIR) = 5× 10^9 L_☉ to 10^11 L_☉ and SFR = 7.8 × 10^–10 L(24 μm, L_☉)(7.76 × 10^–11 L(24))^0.048 for higher L(TIR). For galaxies with L(TIR) ≥ 10^10 L_☉, these new expressions should provide SFRs to within 0.2 dex. For L(TIR) ≥ 10^11 L_☉, we find that the SFR of infrared galaxies is significantly underestimated using extinction-corrected Paα (and presumably using any other optical or near-infrared recombination lines). As a part of this work, we constructed spectral energy distribution templates for eleven luminous and ultraluminous purely star forming infrared galaxies and over the spectral range 0.4 μm to 30 cm. We use these templates and the SINGS data to construct average templates from 5 μm to 30 cm for infrared galaxies with L(TIR) = 5× 10^9 to 10^13 L_☉. All of these templates are made available online.
dc.description.departmentDepto. de Física de la Tierra y Astrofísica
dc.description.facultyFac. de Ciencias Físicas
dc.description.refereedTRUE
dc.description.sponsorshipMinisterio de Economía y Competitividad (MINECO)
dc.description.sponsorshipNational Aeronautics and Space Administration (NASA)
dc.description.sponsorshipNational Science Foundation (NSF)
dc.description.sponsorshipNASA/Goddard to the University of Arizona
dc.description.sponsorshipLabelled Transition Systems Analyser ( LTSA), NASA
dc.description.sponsorshipUnión Europea (UE)
dc.description.sponsorshipAyudas para contratos Ramón y Cajal (RYC), MINECO
dc.description.statuspub
dc.eprint.idhttps://eprints.ucm.es/id/eprint/38660
dc.identifier.doi10.1088/0004-637X/692/1/556
dc.identifier.issn0004-637X
dc.identifier.officialurlhttp://dx.doi.org/10.1088/0004-637X/692/1/556
dc.identifier.relatedurlhttp://iopscience.iop.org/
dc.identifier.urihttps://hdl.handle.net/20.500.14352/45119
dc.issue.number1
dc.journal.titleAstrophysical journal
dc.language.isoeng
dc.page.final573
dc.page.initial556
dc.publisherAmerican Astronomical Society
dc.relation.projectID1255094
dc.relation.projectIDNAG5-12318
dc.relation.projectIDAST95- 09298
dc.relation.projectIDAST-0071048
dc.relation.projectIDAST-0071198
dc.relation.projectIDAST-0507428
dc.relation.projectIDAST- 0507483
dc.relation.projectIDNNG04GC89
dc.relation.projectIDPNAYA 2006–02358
dc.relation.projectIDPNAYA 2006–15698–C02–02
dc.rights.accessRightsopen access
dc.subject.cdu52
dc.subject.keywordInitial mass function
dc.subject.keywordSpitzer-space-telescope
dc.subject.keywordMultiband imaging photometer
dc.subject.keywordActive galactic nuclei
dc.subject.keywordSubmillimeter galaxies
dc.subject.keywordNearby galaxies
dc.subject.keywordForming galaxies
dc.subject.keywordH-alpha
dc.subject.keywordRadio correlation
dc.subject.keywordSpiral galaxies
dc.subject.ucmAstrofísica
dc.subject.ucmAstronomía (Física)
dc.titleDetermining star formation rates for infrared galaxies
dc.typejournal article
dc.volume.number692
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