Foreground and background dust in star cluster directions
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/10183/98104 |
Resumo: | This paper compares reddening values E(B-V) derived from the stellar content of 103 old open clusters and 147 globular clusters of the Milky Way with those derived from DIRBE/IRAS 100 μm dust emission in the same directions. Star clusters at |b| > 20º show comparable reddening values between the two methods, in agreement with the fact that most of them are located beyond the disk dust layer. For very low galactic latitude lines of sight, differences occur in the sense that DIRBE/IRAS reddening values can be substantially larger, suggesting effects due to the depth distribution of the dust. The differences appear to arise from dust in the background of the clusters consistent with a dust layer where important extinction occurs up to distances from the Plane of ≈ 300 pc. For 3% of the sample a significant background dust contribution might be explained by higher dust clouds. We find evidence that the MilkyWay dust lane and higher dust clouds are similar to those of several edge-on spiral galaxies recently studied in detail by means of CCD imaging. |
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Dutra, Carlos MaximilianoBica, Eduardo Luiz Damiani2014-07-18T02:04:41Z20000004-6361http://hdl.handle.net/10183/98104000274946This paper compares reddening values E(B-V) derived from the stellar content of 103 old open clusters and 147 globular clusters of the Milky Way with those derived from DIRBE/IRAS 100 μm dust emission in the same directions. Star clusters at |b| > 20º show comparable reddening values between the two methods, in agreement with the fact that most of them are located beyond the disk dust layer. For very low galactic latitude lines of sight, differences occur in the sense that DIRBE/IRAS reddening values can be substantially larger, suggesting effects due to the depth distribution of the dust. The differences appear to arise from dust in the background of the clusters consistent with a dust layer where important extinction occurs up to distances from the Plane of ≈ 300 pc. For 3% of the sample a significant background dust contribution might be explained by higher dust clouds. We find evidence that the MilkyWay dust lane and higher dust clouds are similar to those of several edge-on spiral galaxies recently studied in detail by means of CCD imaging.application/pdfengAstronomy and astrophysics. New York. Vol. 359, no. 1 (July 2000), 347-363GalaxiaPoeira cosmicaMateria interestelarAglomerados estelaresGalaxy: globular clusters: general – –Galaxy: open clusters and associations: generalISM: dust, extinctionForeground and background dust in star cluster directionsEstrangeiroinfo: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:UFRGSTEXT000274946.pdf.txt000274946.pdf.txtExtracted Texttext/plain65194http://www.lume.ufrgs.br/bitstream/10183/98104/2/000274946.pdf.txtc66ed1a898293e46f300ce23b6d44225MD52ORIGINAL000274946.pdf000274946.pdfTexto completo (inglês)application/pdf256926http://www.lume.ufrgs.br/bitstream/10183/98104/1/000274946.pdfbb9722f285b28b14afb3367fb3e9e898MD51THUMBNAIL000274946.pdf.jpg000274946.pdf.jpgGenerated Thumbnailimage/jpeg2012http://www.lume.ufrgs.br/bitstream/10183/98104/3/000274946.pdf.jpg87d651113f309d08ae97ca132cf27bb0MD5310183/981042024-04-13 06:44:58.778461oai:www.lume.ufrgs.br:10183/98104Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-04-13T09:44:58Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Foreground and background dust in star cluster directions |
title |
Foreground and background dust in star cluster directions |
spellingShingle |
Foreground and background dust in star cluster directions Dutra, Carlos Maximiliano Galaxia Poeira cosmica Materia interestelar Aglomerados estelares Galaxy: globular clusters: general – – Galaxy: open clusters and associations: general ISM: dust, extinction |
title_short |
Foreground and background dust in star cluster directions |
title_full |
Foreground and background dust in star cluster directions |
title_fullStr |
Foreground and background dust in star cluster directions |
title_full_unstemmed |
Foreground and background dust in star cluster directions |
title_sort |
Foreground and background dust in star cluster directions |
author |
Dutra, Carlos Maximiliano |
author_facet |
Dutra, Carlos Maximiliano Bica, Eduardo Luiz Damiani |
author_role |
author |
author2 |
Bica, Eduardo Luiz Damiani |
author2_role |
author |
dc.contributor.author.fl_str_mv |
Dutra, Carlos Maximiliano Bica, Eduardo Luiz Damiani |
dc.subject.por.fl_str_mv |
Galaxia Poeira cosmica Materia interestelar Aglomerados estelares |
topic |
Galaxia Poeira cosmica Materia interestelar Aglomerados estelares Galaxy: globular clusters: general – – Galaxy: open clusters and associations: general ISM: dust, extinction |
dc.subject.eng.fl_str_mv |
Galaxy: globular clusters: general – – Galaxy: open clusters and associations: general ISM: dust, extinction |
description |
This paper compares reddening values E(B-V) derived from the stellar content of 103 old open clusters and 147 globular clusters of the Milky Way with those derived from DIRBE/IRAS 100 μm dust emission in the same directions. Star clusters at |b| > 20º show comparable reddening values between the two methods, in agreement with the fact that most of them are located beyond the disk dust layer. For very low galactic latitude lines of sight, differences occur in the sense that DIRBE/IRAS reddening values can be substantially larger, suggesting effects due to the depth distribution of the dust. The differences appear to arise from dust in the background of the clusters consistent with a dust layer where important extinction occurs up to distances from the Plane of ≈ 300 pc. For 3% of the sample a significant background dust contribution might be explained by higher dust clouds. We find evidence that the MilkyWay dust lane and higher dust clouds are similar to those of several edge-on spiral galaxies recently studied in detail by means of CCD imaging. |
publishDate |
2000 |
dc.date.issued.fl_str_mv |
2000 |
dc.date.accessioned.fl_str_mv |
2014-07-18T02:04:41Z |
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/10183/98104 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-6361 |
dc.identifier.nrb.pt_BR.fl_str_mv |
000274946 |
identifier_str_mv |
0004-6361 000274946 |
url |
http://hdl.handle.net/10183/98104 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and astrophysics. New York. Vol. 359, no. 1 (July 2000), 347-363 |
dc.rights.driver.fl_str_mv |
info:eu-repo/semantics/openAccess |
eu_rights_str_mv |
openAccess |
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application/pdf |
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