The calibration of monochromatic far-infrared star formation rate indicators
Spitzer data at 24, 70, and 160 μm and ground-based Hα images are analyzed for a sample of 189 nearby star-forming and starburst galaxies to investigate whether reliable star formation rate (SFR) indicators can be defined using the monochromatic infrared dust emission centered at 70 and 160 μm. We c...
| Autor: | |
|---|---|
| Formato: | artículo |
| Fecha de publicación: | 2010 |
| País: | España |
| Recursos: | Universidad Complutense de Madrid (UCM) |
| Repositorio: | Docta Complutense |
| Idioma: | inglés |
| OAI Identifier: | oai:docta.ucm.es:20.500.14352/44885 |
| Acesso em linha: | https://hdl.handle.net/20.500.14352/44885 |
| Access Level: | acceso abierto |
| Palavra-chave: | 52 Initial mass function Diffuse ionized medium Aromatic-hydrocarbon emission Nearby spiral galaxies Compact dwarf galaxies Digital sky survey H II regions Starburst galaxies Forming galaxies Local universe Astrofísica Astronomía (Física) |
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The calibration of monochromatic far-infrared star formation rate indicatorsGil De Paz, Armando52Initial mass functionDiffuse ionized mediumAromatic-hydrocarbon emissionNearby spiral galaxiesCompact dwarf galaxiesDigital sky surveyH II regionsStarburst galaxiesForming galaxiesLocal universeAstrofísicaAstronomía (Física)Spitzer data at 24, 70, and 160 μm and ground-based Hα images are analyzed for a sample of 189 nearby star-forming and starburst galaxies to investigate whether reliable star formation rate (SFR) indicators can be defined using the monochromatic infrared dust emission centered at 70 and 160 μm. We compare recently published recipes for SFR measures using combinations of the 24 μm and observed Hα luminosities with those using 24 μm luminosity alone. From these comparisons, we derive a reference SFR indicator for use in our analysis. Linear correlations between SFR and the 70 μm and 160 μm luminosity are found for L(70)≳ 1.4 × 10^42 erg s^–1 and L(160) ≳ 2 × 10^42 erg s^–1, corresponding to SFR gsim 0.1-0.3 M_☉ yr–1, and calibrations of SFRs based on L(70) and L(160) are proposed. Below those two luminosity limits, the relation between SFR and 70 μm (160 μm) luminosity is nonlinear and SFR calibrations become problematic. A more important limitation is the dispersion of the data around the mean trend, which increases for increasing wavelength. The scatter of the 70 μm (160 μm) data around the mean is about 25% (factor ~2) larger than the scatter of the 24 μm data. We interpret this increasing dispersion as an effect of the increasing contribution to the infrared emission of dust heated by stellar populations not associated with the current star formation. Thus, the 70 (160) μm luminosity can be reliably used to trace SFRs in large galaxy samples, but will be of limited utility for individual objects, with the exception of infrared-dominated galaxies. The nonlinear relation between SFR and the 70 and 160 μm emission at faint galaxy luminosities suggests a variety of mechanisms affecting the infrared emission for decreasing luminosity, such as increasing transparency of the interstellar medium, decreasing effective dust temperature, and decreasing filling factor of star-forming regions across the galaxy. In all cases, the calibrations hold for galaxies with oxygen abundance higher than roughly 12 +log(O/H) ~ 8.1. At lower metallicity, the infrared luminosity no longer reliably traces the SFR because galaxies are less dusty and more transparent.American Astronomical SocietyUniversidad Complutense de Madrid20102010-05-1020102010-05-10journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/44885reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/448852026-06-02T12:44:21Z |
| dc.title.none.fl_str_mv |
The calibration of monochromatic far-infrared star formation rate indicators |
| title |
The calibration of monochromatic far-infrared star formation rate indicators |
| spellingShingle |
The calibration of monochromatic far-infrared star formation rate indicators Gil De Paz, Armando 52 Initial mass function Diffuse ionized medium Aromatic-hydrocarbon emission Nearby spiral galaxies Compact dwarf galaxies Digital sky survey H II regions Starburst galaxies Forming galaxies Local universe Astrofísica Astronomía (Física) |
| title_short |
The calibration of monochromatic far-infrared star formation rate indicators |
| title_full |
The calibration of monochromatic far-infrared star formation rate indicators |
| title_fullStr |
The calibration of monochromatic far-infrared star formation rate indicators |
| title_full_unstemmed |
The calibration of monochromatic far-infrared star formation rate indicators |
| title_sort |
The calibration of monochromatic far-infrared star formation rate indicators |
| dc.creator.none.fl_str_mv |
Gil De Paz, Armando |
| author |
Gil De Paz, Armando |
| author_facet |
Gil De Paz, Armando |
| author_role |
author |
| dc.contributor.none.fl_str_mv |
Universidad Complutense de Madrid |
| dc.subject.none.fl_str_mv |
52 Initial mass function Diffuse ionized medium Aromatic-hydrocarbon emission Nearby spiral galaxies Compact dwarf galaxies Digital sky survey H II regions Starburst galaxies Forming galaxies Local universe Astrofísica Astronomía (Física) |
| topic |
52 Initial mass function Diffuse ionized medium Aromatic-hydrocarbon emission Nearby spiral galaxies Compact dwarf galaxies Digital sky survey H II regions Starburst galaxies Forming galaxies Local universe Astrofísica Astronomía (Física) |
| description |
Spitzer data at 24, 70, and 160 μm and ground-based Hα images are analyzed for a sample of 189 nearby star-forming and starburst galaxies to investigate whether reliable star formation rate (SFR) indicators can be defined using the monochromatic infrared dust emission centered at 70 and 160 μm. We compare recently published recipes for SFR measures using combinations of the 24 μm and observed Hα luminosities with those using 24 μm luminosity alone. From these comparisons, we derive a reference SFR indicator for use in our analysis. Linear correlations between SFR and the 70 μm and 160 μm luminosity are found for L(70)≳ 1.4 × 10^42 erg s^–1 and L(160) ≳ 2 × 10^42 erg s^–1, corresponding to SFR gsim 0.1-0.3 M_☉ yr–1, and calibrations of SFRs based on L(70) and L(160) are proposed. Below those two luminosity limits, the relation between SFR and 70 μm (160 μm) luminosity is nonlinear and SFR calibrations become problematic. A more important limitation is the dispersion of the data around the mean trend, which increases for increasing wavelength. The scatter of the 70 μm (160 μm) data around the mean is about 25% (factor ~2) larger than the scatter of the 24 μm data. We interpret this increasing dispersion as an effect of the increasing contribution to the infrared emission of dust heated by stellar populations not associated with the current star formation. Thus, the 70 (160) μm luminosity can be reliably used to trace SFRs in large galaxy samples, but will be of limited utility for individual objects, with the exception of infrared-dominated galaxies. The nonlinear relation between SFR and the 70 and 160 μm emission at faint galaxy luminosities suggests a variety of mechanisms affecting the infrared emission for decreasing luminosity, such as increasing transparency of the interstellar medium, decreasing effective dust temperature, and decreasing filling factor of star-forming regions across the galaxy. In all cases, the calibrations hold for galaxies with oxygen abundance higher than roughly 12 +log(O/H) ~ 8.1. At lower metallicity, the infrared luminosity no longer reliably traces the SFR because galaxies are less dusty and more transparent. |
| publishDate |
2010 |
| dc.date.none.fl_str_mv |
2010 2010-05-10 2010 2010-05-10 |
| 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/20.500.14352/44885 |
| url |
https://hdl.handle.net/20.500.14352/44885 |
| 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 |
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| repository.mail.fl_str_mv |
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1869416705442185216 |
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15,300719 |