The dust content and opacity of actively star-forming galaxies
Autor(a) principal: | |
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Data de Publicação: | 2000 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/108886 |
Resumo: | We present far-infrared (FIR) photometry at 150 and 205 μm of eight low-redshift starburst galaxies obtained with the Infrared Space Observatory (ISO) ISOPHOT. Five of the eight galaxies are detected in both wave bands, and these data are used, in conjunction with IRAS archival photometry, to model the dust emission at λ>~40 μm. The FIR spectral energy distributions (SEDs) are best Ðtted by a combination of two modiÐed Planck functions, with T ~ 40−55 K (warm dust) and T ~ 20−23 K (cool dust) and with a dust emissivity index Є=2. The cool dust can be a major contributor to the FIR emission of starburst galaxies, representing up to 60% of the total flux. This component is heated not only by the general interstellar radiation field, but also by the starburst itself. The cool dust mass is up to ~150 times larger than the warm dust mass, bringing the gas-to-dust ratios of the starbursts in our sample close to Milky Way values, once rescaled for the appropriate metallicity. The ratio between the total dust FIR emission in the range 1−1000 μm and the IRAS FIR emission in the range 40~120 μm is ~1.75, with small variations from galaxy to galaxy. This ratio is about 40% larger than previously inferred from data at millimeter wavelengths. Although the galaxies in our sample are generally classified as "UV bright", for four of them the UV energy emerging shortward of 0.2 μm is less than 15% of the FIR energy. On average, about 30% of the bolometric flux is coming out in the UV−to−near-IR wavelength range; the rest is emitted in the FIR. Energy balance calculations show that the FIR emission predicted by the dust reddening of the UV−to−near-IR stellar emission is within a factor of ~2 of the observed value in individual galaxies and within 20% when averaged over a large sample. If our sample of local starbursts is representative of high-redshift (z>~1), UV-bright, star-forming galaxies, these galaxies' FIR emission will be generally undetected in submillimeter surveys, unless (1) their bolometric luminosity is comparable to or larger than that of ultraluminous FIR galaxies and (2) their FIR SED contains a cool dust component. |
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Calzetti, DanielaArmus, LeeBohlin, Ralph C.Kinney, Anne LouiseKoornneef, JanStorchi-Bergmann, Thaisa2015-01-13T02:14:41Z20000004-637Xhttp://hdl.handle.net/10183/108886000274860We present far-infrared (FIR) photometry at 150 and 205 μm of eight low-redshift starburst galaxies obtained with the Infrared Space Observatory (ISO) ISOPHOT. Five of the eight galaxies are detected in both wave bands, and these data are used, in conjunction with IRAS archival photometry, to model the dust emission at λ>~40 μm. The FIR spectral energy distributions (SEDs) are best Ðtted by a combination of two modiÐed Planck functions, with T ~ 40−55 K (warm dust) and T ~ 20−23 K (cool dust) and with a dust emissivity index Є=2. The cool dust can be a major contributor to the FIR emission of starburst galaxies, representing up to 60% of the total flux. This component is heated not only by the general interstellar radiation field, but also by the starburst itself. The cool dust mass is up to ~150 times larger than the warm dust mass, bringing the gas-to-dust ratios of the starbursts in our sample close to Milky Way values, once rescaled for the appropriate metallicity. The ratio between the total dust FIR emission in the range 1−1000 μm and the IRAS FIR emission in the range 40~120 μm is ~1.75, with small variations from galaxy to galaxy. This ratio is about 40% larger than previously inferred from data at millimeter wavelengths. Although the galaxies in our sample are generally classified as "UV bright", for four of them the UV energy emerging shortward of 0.2 μm is less than 15% of the FIR energy. On average, about 30% of the bolometric flux is coming out in the UV−to−near-IR wavelength range; the rest is emitted in the FIR. Energy balance calculations show that the FIR emission predicted by the dust reddening of the UV−to−near-IR stellar emission is within a factor of ~2 of the observed value in individual galaxies and within 20% when averaged over a large sample. If our sample of local starbursts is representative of high-redshift (z>~1), UV-bright, star-forming galaxies, these galaxies' FIR emission will be generally undetected in submillimeter surveys, unless (1) their bolometric luminosity is comparable to or larger than that of ultraluminous FIR galaxies and (2) their FIR SED contains a cool dust component.application/pdfengThe Astrophysical journal. Chicago. Vol. 533, no. 2 pt. 1 (Apr. 2000), p. 682-695Poeira cosmicaOpacidade estelarGaláxias ativasExplosoes de estrelasFotometriaMateria interestelarAstronomia submilimétricaGalaxies : starburstInfrared : galaxiesInfrared : ISM: continuumISM: dust, extinctionThe dust content and opacity of actively star-forming galaxiesEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL000274860.pdf000274860.pdfTexto completo (inglês)application/pdf205718http://www.lume.ufrgs.br/bitstream/10183/108886/1/000274860.pdf268ff34000eb2b0a8c9ee5f346641bedMD51TEXT000274860.pdf.txt000274860.pdf.txtExtracted Texttext/plain80606http://www.lume.ufrgs.br/bitstream/10183/108886/2/000274860.pdf.txt72ebafae5f11c5de36837f24c5a2646fMD52THUMBNAIL000274860.pdf.jpg000274860.pdf.jpgGenerated Thumbnailimage/jpeg2145http://www.lume.ufrgs.br/bitstream/10183/108886/3/000274860.pdf.jpg93f2453a153d796cf5c77fe3c7dc891dMD5310183/1088862018-10-23 08:37:31.576oai:www.lume.ufrgs.br:10183/108886Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2018-10-23T11:37:31Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
The dust content and opacity of actively star-forming galaxies |
title |
The dust content and opacity of actively star-forming galaxies |
spellingShingle |
The dust content and opacity of actively star-forming galaxies Calzetti, Daniela Poeira cosmica Opacidade estelar Galáxias ativas Explosoes de estrelas Fotometria Materia interestelar Astronomia submilimétrica Galaxies : starburst Infrared : galaxies Infrared : ISM: continuum ISM: dust, extinction |
title_short |
The dust content and opacity of actively star-forming galaxies |
title_full |
The dust content and opacity of actively star-forming galaxies |
title_fullStr |
The dust content and opacity of actively star-forming galaxies |
title_full_unstemmed |
The dust content and opacity of actively star-forming galaxies |
title_sort |
The dust content and opacity of actively star-forming galaxies |
author |
Calzetti, Daniela |
author_facet |
Calzetti, Daniela Armus, Lee Bohlin, Ralph C. Kinney, Anne Louise Koornneef, Jan Storchi-Bergmann, Thaisa |
author_role |
author |
author2 |
Armus, Lee Bohlin, Ralph C. Kinney, Anne Louise Koornneef, Jan Storchi-Bergmann, Thaisa |
author2_role |
author author author author author |
dc.contributor.author.fl_str_mv |
Calzetti, Daniela Armus, Lee Bohlin, Ralph C. Kinney, Anne Louise Koornneef, Jan Storchi-Bergmann, Thaisa |
dc.subject.por.fl_str_mv |
Poeira cosmica Opacidade estelar Galáxias ativas Explosoes de estrelas Fotometria Materia interestelar Astronomia submilimétrica |
topic |
Poeira cosmica Opacidade estelar Galáxias ativas Explosoes de estrelas Fotometria Materia interestelar Astronomia submilimétrica Galaxies : starburst Infrared : galaxies Infrared : ISM: continuum ISM: dust, extinction |
dc.subject.eng.fl_str_mv |
Galaxies : starburst Infrared : galaxies Infrared : ISM: continuum ISM: dust, extinction |
description |
We present far-infrared (FIR) photometry at 150 and 205 μm of eight low-redshift starburst galaxies obtained with the Infrared Space Observatory (ISO) ISOPHOT. Five of the eight galaxies are detected in both wave bands, and these data are used, in conjunction with IRAS archival photometry, to model the dust emission at λ>~40 μm. The FIR spectral energy distributions (SEDs) are best Ðtted by a combination of two modiÐed Planck functions, with T ~ 40−55 K (warm dust) and T ~ 20−23 K (cool dust) and with a dust emissivity index Є=2. The cool dust can be a major contributor to the FIR emission of starburst galaxies, representing up to 60% of the total flux. This component is heated not only by the general interstellar radiation field, but also by the starburst itself. The cool dust mass is up to ~150 times larger than the warm dust mass, bringing the gas-to-dust ratios of the starbursts in our sample close to Milky Way values, once rescaled for the appropriate metallicity. The ratio between the total dust FIR emission in the range 1−1000 μm and the IRAS FIR emission in the range 40~120 μm is ~1.75, with small variations from galaxy to galaxy. This ratio is about 40% larger than previously inferred from data at millimeter wavelengths. Although the galaxies in our sample are generally classified as "UV bright", for four of them the UV energy emerging shortward of 0.2 μm is less than 15% of the FIR energy. On average, about 30% of the bolometric flux is coming out in the UV−to−near-IR wavelength range; the rest is emitted in the FIR. Energy balance calculations show that the FIR emission predicted by the dust reddening of the UV−to−near-IR stellar emission is within a factor of ~2 of the observed value in individual galaxies and within 20% when averaged over a large sample. If our sample of local starbursts is representative of high-redshift (z>~1), UV-bright, star-forming galaxies, these galaxies' FIR emission will be generally undetected in submillimeter surveys, unless (1) their bolometric luminosity is comparable to or larger than that of ultraluminous FIR galaxies and (2) their FIR SED contains a cool dust component. |
publishDate |
2000 |
dc.date.issued.fl_str_mv |
2000 |
dc.date.accessioned.fl_str_mv |
2015-01-13T02:14:41Z |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/108886 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
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000274860 |
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http://hdl.handle.net/10183/108886 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The Astrophysical journal. Chicago. Vol. 533, no. 2 pt. 1 (Apr. 2000), p. 682-695 |
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openAccess |
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