Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects
Autor(a) principal: | |
---|---|
Data de Publicação: | 1994 |
Outros Autores: | , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/108842 |
Resumo: | Spectral distributions from the UV to the near-IR of a sample of 44 star-forming galaxies are used to calculate the metallicity (0/H), star-formation rate (SFR) and age of the starbursts. The oxygen abundance covers the range 8.3 < 0/H < 9.4, and nitrogen (N) is found to be mostly a product of secondary nucleosynthesis for 0/H > 8.4. Dueto its secondary origin, N/0 ratios up to ≈4 times the solar value can be obtained for metal rich starbursts. The SFR ranges from 0.01 to 100 M 0 yr-ˡ. The lower metallicity galaxies seem to be experiencing ao instantaneous burst of star formation, with ages ranging from under 5 x 10 6 to 10 7 yr. The highest metallicity galaxies are most probably experiencing a continuous burst. Correlations between the calculated quantities and severa! spectral features are investigated. We found a highly significant correlation between the equivalent width W(C IV λ1550)−a stellar (absorption) feature−and the oxygen abundance of the emitting gas (0/H). Thus we show for the first time that the stellar metallicity is well correlated with the gas metallicity in star-bursting galaxies. The equivalent width W(Si IV λ1400) and the emission line ratio [N II] λλ6548,84/Hα also correlate well with 0/H, and all three features can be used as metallicity indicators for star-forming galaxies. The continuum color between λ1400 and λ3500 [C(14-35)] is shown to correlate with 0/H, although it is better correlated with E(B- V). It was not possible to disentangle the metallicity from the reddening effect in C(14-35). We estimate that the reddening affecting the UV continuum is about half the one derived from the Balmer decrement of the emitting gas. The SFR correlates well with the galaxy luminosity and there is no dependence of the continuum color on the SFR. The higher metallicities are only found in the more luminous galaxies, while low metallicities are found over the whole luminosity interval (-16 < M8 < -23, H0 =50 km s-ˡ Mpc-ˡ) covered by the sample. |
id |
UFRGS-2_ad564ebc08d600f4b6c02eeeaec42797 |
---|---|
oai_identifier_str |
oai:www.lume.ufrgs.br:10183/108842 |
network_acronym_str |
UFRGS-2 |
network_name_str |
Repositório Institucional da UFRGS |
repository_id_str |
|
spelling |
Storchi-Bergmann, ThaisaCalzetti, DanielaKinney, Anne Louise2015-01-08T02:13:09Z19940004-637Xhttp://hdl.handle.net/10183/108842000254243Spectral distributions from the UV to the near-IR of a sample of 44 star-forming galaxies are used to calculate the metallicity (0/H), star-formation rate (SFR) and age of the starbursts. The oxygen abundance covers the range 8.3 < 0/H < 9.4, and nitrogen (N) is found to be mostly a product of secondary nucleosynthesis for 0/H > 8.4. Dueto its secondary origin, N/0 ratios up to ≈4 times the solar value can be obtained for metal rich starbursts. The SFR ranges from 0.01 to 100 M 0 yr-ˡ. The lower metallicity galaxies seem to be experiencing ao instantaneous burst of star formation, with ages ranging from under 5 x 10 6 to 10 7 yr. The highest metallicity galaxies are most probably experiencing a continuous burst. Correlations between the calculated quantities and severa! spectral features are investigated. We found a highly significant correlation between the equivalent width W(C IV λ1550)−a stellar (absorption) feature−and the oxygen abundance of the emitting gas (0/H). Thus we show for the first time that the stellar metallicity is well correlated with the gas metallicity in star-bursting galaxies. The equivalent width W(Si IV λ1400) and the emission line ratio [N II] λλ6548,84/Hα also correlate well with 0/H, and all three features can be used as metallicity indicators for star-forming galaxies. The continuum color between λ1400 and λ3500 [C(14-35)] is shown to correlate with 0/H, although it is better correlated with E(B- V). It was not possible to disentangle the metallicity from the reddening effect in C(14-35). We estimate that the reddening affecting the UV continuum is about half the one derived from the Balmer decrement of the emitting gas. The SFR correlates well with the galaxy luminosity and there is no dependence of the continuum color on the SFR. The higher metallicities are only found in the more luminous galaxies, while low metallicities are found over the whole luminosity interval (-16 < M8 < -23, H0 =50 km s-ˡ Mpc-ˡ) covered by the sample.application/pdfengThe astrophysical journal. Chicago. Vol. 429, no. 2, pt. 1 (July 1994), p. 572-581Astrofisica extragalaticaMetalicidadeFormacao de estrelasGaláxiasEvolucao galaticaEspectros astronômicosExplosoes de estrelasGalaxies: abundancesGalaxies: evolutionGalaxies: photometryGalaxies: starburstUltraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effectsEstrangeiroinfo: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:UFRGSORIGINAL000254243.pdf000254243.pdfTexto completo (inglês)application/pdf204897http://www.lume.ufrgs.br/bitstream/10183/108842/1/000254243.pdfa94f061ef9797af1284febed54340887MD51TEXT000254243.pdf.txt000254243.pdf.txtExtracted Texttext/plain220http://www.lume.ufrgs.br/bitstream/10183/108842/2/000254243.pdf.txt728e29fe7d7fb65807355614fc16afa7MD52THUMBNAIL000254243.pdf.jpg000254243.pdf.jpgGenerated Thumbnailimage/jpeg2168http://www.lume.ufrgs.br/bitstream/10183/108842/3/000254243.pdf.jpg1a40e48a50541b273634277694702b12MD5310183/1088422018-10-23 08:35:12.651oai:www.lume.ufrgs.br:10183/108842Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2018-10-23T11:35:12Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects |
title |
Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects |
spellingShingle |
Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects Storchi-Bergmann, Thaisa Astrofisica extragalatica Metalicidade Formacao de estrelas Galáxias Evolucao galatica Espectros astronômicos Explosoes de estrelas Galaxies: abundances Galaxies: evolution Galaxies: photometry Galaxies: starburst |
title_short |
Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects |
title_full |
Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects |
title_fullStr |
Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects |
title_full_unstemmed |
Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects |
title_sort |
Ultraviolet to near-infrared spectral distributions of star-forming galaxies : metallicity and age effects |
author |
Storchi-Bergmann, Thaisa |
author_facet |
Storchi-Bergmann, Thaisa Calzetti, Daniela Kinney, Anne Louise |
author_role |
author |
author2 |
Calzetti, Daniela Kinney, Anne Louise |
author2_role |
author author |
dc.contributor.author.fl_str_mv |
Storchi-Bergmann, Thaisa Calzetti, Daniela Kinney, Anne Louise |
dc.subject.por.fl_str_mv |
Astrofisica extragalatica Metalicidade Formacao de estrelas Galáxias Evolucao galatica Espectros astronômicos Explosoes de estrelas |
topic |
Astrofisica extragalatica Metalicidade Formacao de estrelas Galáxias Evolucao galatica Espectros astronômicos Explosoes de estrelas Galaxies: abundances Galaxies: evolution Galaxies: photometry Galaxies: starburst |
dc.subject.eng.fl_str_mv |
Galaxies: abundances Galaxies: evolution Galaxies: photometry Galaxies: starburst |
description |
Spectral distributions from the UV to the near-IR of a sample of 44 star-forming galaxies are used to calculate the metallicity (0/H), star-formation rate (SFR) and age of the starbursts. The oxygen abundance covers the range 8.3 < 0/H < 9.4, and nitrogen (N) is found to be mostly a product of secondary nucleosynthesis for 0/H > 8.4. Dueto its secondary origin, N/0 ratios up to ≈4 times the solar value can be obtained for metal rich starbursts. The SFR ranges from 0.01 to 100 M 0 yr-ˡ. The lower metallicity galaxies seem to be experiencing ao instantaneous burst of star formation, with ages ranging from under 5 x 10 6 to 10 7 yr. The highest metallicity galaxies are most probably experiencing a continuous burst. Correlations between the calculated quantities and severa! spectral features are investigated. We found a highly significant correlation between the equivalent width W(C IV λ1550)−a stellar (absorption) feature−and the oxygen abundance of the emitting gas (0/H). Thus we show for the first time that the stellar metallicity is well correlated with the gas metallicity in star-bursting galaxies. The equivalent width W(Si IV λ1400) and the emission line ratio [N II] λλ6548,84/Hα also correlate well with 0/H, and all three features can be used as metallicity indicators for star-forming galaxies. The continuum color between λ1400 and λ3500 [C(14-35)] is shown to correlate with 0/H, although it is better correlated with E(B- V). It was not possible to disentangle the metallicity from the reddening effect in C(14-35). We estimate that the reddening affecting the UV continuum is about half the one derived from the Balmer decrement of the emitting gas. The SFR correlates well with the galaxy luminosity and there is no dependence of the continuum color on the SFR. The higher metallicities are only found in the more luminous galaxies, while low metallicities are found over the whole luminosity interval (-16 < M8 < -23, H0 =50 km s-ˡ Mpc-ˡ) covered by the sample. |
publishDate |
1994 |
dc.date.issued.fl_str_mv |
1994 |
dc.date.accessioned.fl_str_mv |
2015-01-08T02:13:09Z |
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/10183/108842 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
dc.identifier.nrb.pt_BR.fl_str_mv |
000254243 |
identifier_str_mv |
0004-637X 000254243 |
url |
http://hdl.handle.net/10183/108842 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Chicago. Vol. 429, no. 2, pt. 1 (July 1994), p. 572-581 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
dc.format.none.fl_str_mv |
application/pdf |
dc.source.none.fl_str_mv |
reponame:Repositório Institucional da UFRGS instname:Universidade Federal do Rio Grande do Sul (UFRGS) instacron:UFRGS |
instname_str |
Universidade Federal do Rio Grande do Sul (UFRGS) |
instacron_str |
UFRGS |
institution |
UFRGS |
reponame_str |
Repositório Institucional da UFRGS |
collection |
Repositório Institucional da UFRGS |
bitstream.url.fl_str_mv |
http://www.lume.ufrgs.br/bitstream/10183/108842/1/000254243.pdf http://www.lume.ufrgs.br/bitstream/10183/108842/2/000254243.pdf.txt http://www.lume.ufrgs.br/bitstream/10183/108842/3/000254243.pdf.jpg |
bitstream.checksum.fl_str_mv |
a94f061ef9797af1284febed54340887 728e29fe7d7fb65807355614fc16afa7 1a40e48a50541b273634277694702b12 |
bitstream.checksumAlgorithm.fl_str_mv |
MD5 MD5 MD5 |
repository.name.fl_str_mv |
Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS) |
repository.mail.fl_str_mv |
|
_version_ |
1801224862123950080 |