Integrated spectra of Milky Way globular clusters
Autor(a) principal: | |
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Data de Publicação: | 2019 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/204124 |
Resumo: | Integrated spectra of Milky Way globular clusters (GCs) are reproduced by computing synthetic spectra taking into account individual element abundances. Five clusters were selected from their location in the Galactic bulge, for which integrated spectra were available in the WiFeS Atlas of Galactic Globular Cluster Spectra project. Our aim is to further study the oldest GCs located in the Galactic bulge, with a metallicity in the range −1.6 < [Fe/H] < −0.7. We also include the halo cluster NGC 6752 for comparison purposes. We reproduce the full spectra in the range 4500–9000 Å available in these observed spectra, as well as individual lines of Na, Mg, Al, Si, Ca, Ti, Ba, and Eu. We report a list of lines that are suitable for abundance derivation, and by adopting these abundances, we are able to fit the damping parameters that define the wings of strong lines of well-known triplets of Mg i and Ca ii. Finally, the effect of multiple stellar populations through enhanced Na abundances is tested. |
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Moura, TatianaTrevisan, MarinaBarbuy, BeatrizRossi, Silvia2020-01-14T04:15:32Z20190004-637Xhttp://hdl.handle.net/10183/204124001108967Integrated spectra of Milky Way globular clusters (GCs) are reproduced by computing synthetic spectra taking into account individual element abundances. Five clusters were selected from their location in the Galactic bulge, for which integrated spectra were available in the WiFeS Atlas of Galactic Globular Cluster Spectra project. Our aim is to further study the oldest GCs located in the Galactic bulge, with a metallicity in the range −1.6 < [Fe/H] < −0.7. We also include the halo cluster NGC 6752 for comparison purposes. We reproduce the full spectra in the range 4500–9000 Å available in these observed spectra, as well as individual lines of Na, Mg, Al, Si, Ca, Ti, Ba, and Eu. We report a list of lines that are suitable for abundance derivation, and by adopting these abundances, we are able to fit the damping parameters that define the wings of strong lines of well-known triplets of Mg i and Ca ii. Finally, the effect of multiple stellar populations through enhanced Na abundances is tested.application/pdfengThe astrophysical journal. Bristol. Vol. 885, no. 1 (Nov. 2019), 28, 23 p.Aglomerados estelares globularesAtmosferas estelaresPopulacoes estelaresGalactic bulgeGlobular star clustersGalaxy abundancesStellar atmospheresStellar populationsIntegrated spectra of Milky Way globular clustersEstrangeiroinfo: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:UFRGSTEXT001108967.pdf.txt001108967.pdf.txtExtracted Texttext/plain49625http://www.lume.ufrgs.br/bitstream/10183/204124/2/001108967.pdf.txt6c05b655162f2b77b158ac27d2f31ebfMD52ORIGINAL001108967.pdfTexto completo (inglês)application/pdf2877931http://www.lume.ufrgs.br/bitstream/10183/204124/1/001108967.pdf58af5540104b9ca5811a59f84f2cc442MD5110183/2041242023-08-11 03:52:55.26363oai:www.lume.ufrgs.br:10183/204124Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-08-11T06:52:55Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Integrated spectra of Milky Way globular clusters |
title |
Integrated spectra of Milky Way globular clusters |
spellingShingle |
Integrated spectra of Milky Way globular clusters Moura, Tatiana Aglomerados estelares globulares Atmosferas estelares Populacoes estelares Galactic bulge Globular star clusters Galaxy abundances Stellar atmospheres Stellar populations |
title_short |
Integrated spectra of Milky Way globular clusters |
title_full |
Integrated spectra of Milky Way globular clusters |
title_fullStr |
Integrated spectra of Milky Way globular clusters |
title_full_unstemmed |
Integrated spectra of Milky Way globular clusters |
title_sort |
Integrated spectra of Milky Way globular clusters |
author |
Moura, Tatiana |
author_facet |
Moura, Tatiana Trevisan, Marina Barbuy, Beatriz Rossi, Silvia |
author_role |
author |
author2 |
Trevisan, Marina Barbuy, Beatriz Rossi, Silvia |
author2_role |
author author author |
dc.contributor.author.fl_str_mv |
Moura, Tatiana Trevisan, Marina Barbuy, Beatriz Rossi, Silvia |
dc.subject.por.fl_str_mv |
Aglomerados estelares globulares Atmosferas estelares Populacoes estelares |
topic |
Aglomerados estelares globulares Atmosferas estelares Populacoes estelares Galactic bulge Globular star clusters Galaxy abundances Stellar atmospheres Stellar populations |
dc.subject.eng.fl_str_mv |
Galactic bulge Globular star clusters Galaxy abundances Stellar atmospheres Stellar populations |
description |
Integrated spectra of Milky Way globular clusters (GCs) are reproduced by computing synthetic spectra taking into account individual element abundances. Five clusters were selected from their location in the Galactic bulge, for which integrated spectra were available in the WiFeS Atlas of Galactic Globular Cluster Spectra project. Our aim is to further study the oldest GCs located in the Galactic bulge, with a metallicity in the range −1.6 < [Fe/H] < −0.7. We also include the halo cluster NGC 6752 for comparison purposes. We reproduce the full spectra in the range 4500–9000 Å available in these observed spectra, as well as individual lines of Na, Mg, Al, Si, Ca, Ti, Ba, and Eu. We report a list of lines that are suitable for abundance derivation, and by adopting these abundances, we are able to fit the damping parameters that define the wings of strong lines of well-known triplets of Mg i and Ca ii. Finally, the effect of multiple stellar populations through enhanced Na abundances is tested. |
publishDate |
2019 |
dc.date.issued.fl_str_mv |
2019 |
dc.date.accessioned.fl_str_mv |
2020-01-14T04:15:32Z |
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/10183/204124 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
dc.identifier.nrb.pt_BR.fl_str_mv |
001108967 |
identifier_str_mv |
0004-637X 001108967 |
url |
http://hdl.handle.net/10183/204124 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Bristol. Vol. 885, no. 1 (Nov. 2019), 28, 23 p. |
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 |
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UFRGS |
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Repositório Institucional da UFRGS |
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Repositório Institucional da UFRGS |
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