Determining star formation rates for infrared galaxies

We 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:...

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Detalles Bibliográficos
Autores: Rieke, G. H., Alonso Herrero, A., Weiner, B. J., Pérez González, Pablo Guillermo, Blaylock, M., Donley, J. L., Marcillac, D.
Tipo de recurso: artículo
Fecha de publicación:2009
País:España
Institución:Universidad Complutense de Madrid (UCM)
Repositorio:Docta Complutense
Idioma:inglés
OAI Identifier:oai:docta.ucm.es:20.500.14352/45119
Acceso en línea:https://hdl.handle.net/20.500.14352/45119
Access Level:acceso abierto
Palabra clave:52
Initial mass function
Spitzer-space-telescope
Multiband imaging photometer
Active galactic nuclei
Submillimeter galaxies
Nearby galaxies
Forming galaxies
H-alpha
Radio correlation
Spiral galaxies
Astrofísica
Astronomía (Física)
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oai_identifier_str oai:docta.ucm.es:20.500.14352/45119
network_acronym_str ES
network_name_str España
repository_id_str
spelling Determining star formation rates for infrared galaxiesRieke, G. H.Alonso Herrero, A.Weiner, B. J.Pérez González, Pablo GuillermoBlaylock, M.Donley, J. L.Marcillac, D.52Initial mass functionSpitzer-space-telescopeMultiband imaging photometerActive galactic nucleiSubmillimeter galaxiesNearby galaxiesForming galaxiesH-alphaRadio correlationSpiral galaxiesAstrofísicaAstronomía (Física)We 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.American Astronomical SocietyUniversidad Complutense de Madrid20092009-02-1020092009-02-10journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/45119reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/451192026-06-02T12:44:21Z
dc.title.none.fl_str_mv Determining star formation rates for infrared galaxies
title Determining star formation rates for infrared galaxies
spellingShingle Determining star formation rates for infrared galaxies
Rieke, G. H.
52
Initial mass function
Spitzer-space-telescope
Multiband imaging photometer
Active galactic nuclei
Submillimeter galaxies
Nearby galaxies
Forming galaxies
H-alpha
Radio correlation
Spiral galaxies
Astrofísica
Astronomía (Física)
title_short Determining star formation rates for infrared galaxies
title_full Determining star formation rates for infrared galaxies
title_fullStr Determining star formation rates for infrared galaxies
title_full_unstemmed Determining star formation rates for infrared galaxies
title_sort Determining star formation rates for infrared galaxies
dc.creator.none.fl_str_mv Rieke, G. H.
Alonso Herrero, A.
Weiner, B. J.
Pérez González, Pablo Guillermo
Blaylock, M.
Donley, J. L.
Marcillac, D.
author Rieke, G. H.
author_facet Rieke, G. H.
Alonso Herrero, A.
Weiner, B. J.
Pérez González, Pablo Guillermo
Blaylock, M.
Donley, J. L.
Marcillac, D.
author_role author
author2 Alonso Herrero, A.
Weiner, B. J.
Pérez González, Pablo Guillermo
Blaylock, M.
Donley, J. L.
Marcillac, D.
author2_role author
author
author
author
author
author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 52
Initial mass function
Spitzer-space-telescope
Multiband imaging photometer
Active galactic nuclei
Submillimeter galaxies
Nearby galaxies
Forming galaxies
H-alpha
Radio correlation
Spiral galaxies
Astrofísica
Astronomía (Física)
topic 52
Initial mass function
Spitzer-space-telescope
Multiband imaging photometer
Active galactic nuclei
Submillimeter galaxies
Nearby galaxies
Forming galaxies
H-alpha
Radio correlation
Spiral galaxies
Astrofísica
Astronomía (Física)
description We 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.
publishDate 2009
dc.date.none.fl_str_mv 2009
2009-02-10
2009
2009-02-10
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/20.500.14352/45119
url https://hdl.handle.net/20.500.14352/45119
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv American Astronomical Society
publisher.none.fl_str_mv American Astronomical Society
dc.source.none.fl_str_mv reponame:Docta Complutense
instname:Universidad Complutense de Madrid (UCM)
instname_str Universidad Complutense de Madrid (UCM)
reponame_str Docta Complutense
collection Docta Complutense
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869418223059861504
score 15,300724

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