Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud
Autor(a) principal: | |
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Data de Publicação: | 2005 |
Outros Autores: | , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/98771 |
Resumo: | We present in this study flux-calibrated integrated spectra in the range (3600–6800) Å for 18 concentrated SMC clusters. Cluster reddening values were estimated by interpolation between the extinction maps of Burstein & Heiles (1982, AJ, 87, 1165) and Schlegel et al. (1998, ApJ, 500, 525). The cluster parameters were derived from the template matching procedure by comparing the line strengths and continuum distribution of the cluster spectra with those of template cluster spectra with known parameters and from the equivalent width (EW) method. In this case, new calibrations were used together with diagnostic diagrams involving the sum of EWs of selected spectral lines. A very good agreement between ages derived from both methods was found. The final cluster ages obtained from the weighted average of values taken from the literature and the present measured ones range from 15 Mr (e.g. L 51) to 7 Gyr (K3). Metal abundances have been derived for only 5 clusters from the present sample, while metallicity values directly averaged from published values for other 4 clusters have been adopted. Combining the present cluster sample with 19 additional SMC clusters whose ages and metal abundances were put onto a homogeneous scale, we analyse the age and metallicity distributions in order to explore the SMC star formation history and its spatial extent. By considering the distances of the clusters from the SMC centre instead of their projections onto the right ascension and declination axes, the present age-position relation suggests that the SMC inner disk could have been related to a cluster formation episode which reached the peak ~2.5 Gyr ago. Evidence for an age gradient in the inner SMC disk is also presented. |
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Piatti, Andres E.Santos Junior, Joao Francisco Coelho dosClaria Olmedo, Juan JoseBica, Eduardo Luiz DamianiAhumada, Andrea VeronicaParisi, M. C.2014-07-26T02:09:20Z20050004-6361http://hdl.handle.net/10183/98771000536672We present in this study flux-calibrated integrated spectra in the range (3600–6800) Å for 18 concentrated SMC clusters. Cluster reddening values were estimated by interpolation between the extinction maps of Burstein & Heiles (1982, AJ, 87, 1165) and Schlegel et al. (1998, ApJ, 500, 525). The cluster parameters were derived from the template matching procedure by comparing the line strengths and continuum distribution of the cluster spectra with those of template cluster spectra with known parameters and from the equivalent width (EW) method. In this case, new calibrations were used together with diagnostic diagrams involving the sum of EWs of selected spectral lines. A very good agreement between ages derived from both methods was found. The final cluster ages obtained from the weighted average of values taken from the literature and the present measured ones range from 15 Mr (e.g. L 51) to 7 Gyr (K3). Metal abundances have been derived for only 5 clusters from the present sample, while metallicity values directly averaged from published values for other 4 clusters have been adopted. Combining the present cluster sample with 19 additional SMC clusters whose ages and metal abundances were put onto a homogeneous scale, we analyse the age and metallicity distributions in order to explore the SMC star formation history and its spatial extent. By considering the distances of the clusters from the SMC centre instead of their projections onto the right ascension and declination axes, the present age-position relation suggests that the SMC inner disk could have been related to a cluster formation episode which reached the peak ~2.5 Gyr ago. Evidence for an age gradient in the inner SMC disk is also presented.application/pdfengAstronomy and astrophysics. Les Ulis. Vol. 440, no. 1 (Sept. 2005), p. 111-120GalaxiaEspectros estelaresGalaxies: star clustersTechniques: spectroscopicMagellanic CloudsIntegrated spectral analysis of 18 concentrated star clusters in the Small Magellanic CloudEstrangeiroinfo: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:UFRGSORIGINAL000536672.pdf000536672.pdfTexto completo (inglês)application/pdf1058474http://www.lume.ufrgs.br/bitstream/10183/98771/1/000536672.pdfc52ccc053bb9bf914cfd255698c98390MD51TEXT000536672.pdf.txt000536672.pdf.txtExtracted Texttext/plain58253http://www.lume.ufrgs.br/bitstream/10183/98771/2/000536672.pdf.txt9018243de8409a45fa761018136618a1MD52THUMBNAIL000536672.pdf.jpg000536672.pdf.jpgGenerated Thumbnailimage/jpeg2019http://www.lume.ufrgs.br/bitstream/10183/98771/3/000536672.pdf.jpg53c70437f4adeac91e103490d2a98c3dMD5310183/987712024-04-12 06:19:55.747571oai:www.lume.ufrgs.br:10183/98771Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-04-12T09:19:55Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud |
title |
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud |
spellingShingle |
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud Piatti, Andres E. Galaxia Espectros estelares Galaxies: star clusters Techniques: spectroscopic Magellanic Clouds |
title_short |
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud |
title_full |
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud |
title_fullStr |
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud |
title_full_unstemmed |
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud |
title_sort |
Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud |
author |
Piatti, Andres E. |
author_facet |
Piatti, Andres E. Santos Junior, Joao Francisco Coelho dos Claria Olmedo, Juan Jose Bica, Eduardo Luiz Damiani Ahumada, Andrea Veronica Parisi, M. C. |
author_role |
author |
author2 |
Santos Junior, Joao Francisco Coelho dos Claria Olmedo, Juan Jose Bica, Eduardo Luiz Damiani Ahumada, Andrea Veronica Parisi, M. C. |
author2_role |
author author author author author |
dc.contributor.author.fl_str_mv |
Piatti, Andres E. Santos Junior, Joao Francisco Coelho dos Claria Olmedo, Juan Jose Bica, Eduardo Luiz Damiani Ahumada, Andrea Veronica Parisi, M. C. |
dc.subject.por.fl_str_mv |
Galaxia Espectros estelares |
topic |
Galaxia Espectros estelares Galaxies: star clusters Techniques: spectroscopic Magellanic Clouds |
dc.subject.eng.fl_str_mv |
Galaxies: star clusters Techniques: spectroscopic Magellanic Clouds |
description |
We present in this study flux-calibrated integrated spectra in the range (3600–6800) Å for 18 concentrated SMC clusters. Cluster reddening values were estimated by interpolation between the extinction maps of Burstein & Heiles (1982, AJ, 87, 1165) and Schlegel et al. (1998, ApJ, 500, 525). The cluster parameters were derived from the template matching procedure by comparing the line strengths and continuum distribution of the cluster spectra with those of template cluster spectra with known parameters and from the equivalent width (EW) method. In this case, new calibrations were used together with diagnostic diagrams involving the sum of EWs of selected spectral lines. A very good agreement between ages derived from both methods was found. The final cluster ages obtained from the weighted average of values taken from the literature and the present measured ones range from 15 Mr (e.g. L 51) to 7 Gyr (K3). Metal abundances have been derived for only 5 clusters from the present sample, while metallicity values directly averaged from published values for other 4 clusters have been adopted. Combining the present cluster sample with 19 additional SMC clusters whose ages and metal abundances were put onto a homogeneous scale, we analyse the age and metallicity distributions in order to explore the SMC star formation history and its spatial extent. By considering the distances of the clusters from the SMC centre instead of their projections onto the right ascension and declination axes, the present age-position relation suggests that the SMC inner disk could have been related to a cluster formation episode which reached the peak ~2.5 Gyr ago. Evidence for an age gradient in the inner SMC disk is also presented. |
publishDate |
2005 |
dc.date.issued.fl_str_mv |
2005 |
dc.date.accessioned.fl_str_mv |
2014-07-26T02:09:20Z |
dc.type.driver.fl_str_mv |
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http://hdl.handle.net/10183/98771 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and astrophysics. Les Ulis. Vol. 440, no. 1 (Sept. 2005), p. 111-120 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
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