Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation
Autor(a) principal: | |
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Data de Publicação: | 1996 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/108779 |
Resumo: | The spatial distributions of SWB I [10<~t(Myr)30]<~ and SWB II [30<~t(Myr)<~70] LMC clusters are analyzed using the enlarged sample of integrated V BV photometry of star clusters and associations published by Bica et ai. in 1996. The differences in the clusters' spatial distributions are interpreted as dating back from their formation epoch and as being caused by a perturbation in the gaseous disk generated by the LMC stellar bar. The two SWB distributions present noncoincident bar or barlike struc tures with a position angle difference of ≈22° ± 2°, which, together with the age difference between the groups, leads to a perturbation propagation velocity of 13.7 ± 2 km s-ˡ kpc-ˡ, which suggests bar induced star formation effects bn the disk. Differences are also observed in the outer parts of the SWB I and SWB II spatial distributions. A spatial Fourier analysis reveals the predominance of m = 1 and m = 2 components in both cases. The spatial distribution of clusters younger than 10 Myr (SWB O) is also studied. The patterns measured by the Fourier analysis for the SWB O clusters resemble the gas distribution in the potential of disk models with an off-center bar. The H I kinematics is also evidence of the presence of the perturbation in the LMC disk. Although some evidence of locally induced star formation effects is found, our analysis indicates that globally triggered star formation effects induced by the potential play an important role in organizing the overall patterns and the toei of Shapley's Constellations. |
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Dottori, Horacio AlbertoBica, Eduardo Luiz DamianiClaria Olmedo, Juan JosePuerari, Ivanio2015-01-07T02:10:56Z19960004-637Xhttp://hdl.handle.net/10183/108779000148842The spatial distributions of SWB I [10<~t(Myr)30]<~ and SWB II [30<~t(Myr)<~70] LMC clusters are analyzed using the enlarged sample of integrated V BV photometry of star clusters and associations published by Bica et ai. in 1996. The differences in the clusters' spatial distributions are interpreted as dating back from their formation epoch and as being caused by a perturbation in the gaseous disk generated by the LMC stellar bar. The two SWB distributions present noncoincident bar or barlike struc tures with a position angle difference of ≈22° ± 2°, which, together with the age difference between the groups, leads to a perturbation propagation velocity of 13.7 ± 2 km s-ˡ kpc-ˡ, which suggests bar induced star formation effects bn the disk. Differences are also observed in the outer parts of the SWB I and SWB II spatial distributions. A spatial Fourier analysis reveals the predominance of m = 1 and m = 2 components in both cases. The spatial distribution of clusters younger than 10 Myr (SWB O) is also studied. The patterns measured by the Fourier analysis for the SWB O clusters resemble the gas distribution in the potential of disk models with an off-center bar. The H I kinematics is also evidence of the presence of the perturbation in the LMC disk. Although some evidence of locally induced star formation effects is found, our analysis indicates that globally triggered star formation effects induced by the potential play an important role in organizing the overall patterns and the toei of Shapley's Constellations.application/pdfengThe astrophysical journal. Chicago. Vol. 461, no. 2, pt. 1 (Apr. 1996), p. 742-749Aglomerados estelaresDinamica estelarGrande Nuvem de MagalhãesGalaxies: kinematics and dynamicsGalaxies: structureMagellanic CloudsOpen clusters and associations: generalSpatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubationEstrangeiroinfo: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:UFRGSORIGINAL000148842.pdf000148842.pdfTexto completo (inglês)application/pdf1144510http://www.lume.ufrgs.br/bitstream/10183/108779/1/000148842.pdf50f1855d73eb523969a25e70a4a4a6a4MD51TEXT000148842.pdf.txt000148842.pdf.txtExtracted Texttext/plain176http://www.lume.ufrgs.br/bitstream/10183/108779/2/000148842.pdf.txt8c4575b5ff7ba8677bfb60d55698b6bcMD52THUMBNAIL000148842.pdf.jpg000148842.pdf.jpgGenerated Thumbnailimage/jpeg2146http://www.lume.ufrgs.br/bitstream/10183/108779/3/000148842.pdf.jpg6403a48d15c9109f96558748ffbe2f5bMD5310183/1087792024-04-14 06:45:49.097679oai:www.lume.ufrgs.br:10183/108779Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2024-04-14T09:45:49Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation |
title |
Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation |
spellingShingle |
Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation Dottori, Horacio Alberto Aglomerados estelares Dinamica estelar Grande Nuvem de Magalhães Galaxies: kinematics and dynamics Galaxies: structure Magellanic Clouds Open clusters and associations: general |
title_short |
Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation |
title_full |
Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation |
title_fullStr |
Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation |
title_full_unstemmed |
Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation |
title_sort |
Spatial distributions of young Large Magellanic Cloud clusters and tracers of a bar pertubation |
author |
Dottori, Horacio Alberto |
author_facet |
Dottori, Horacio Alberto Bica, Eduardo Luiz Damiani Claria Olmedo, Juan Jose Puerari, Ivanio |
author_role |
author |
author2 |
Bica, Eduardo Luiz Damiani Claria Olmedo, Juan Jose Puerari, Ivanio |
author2_role |
author author author |
dc.contributor.author.fl_str_mv |
Dottori, Horacio Alberto Bica, Eduardo Luiz Damiani Claria Olmedo, Juan Jose Puerari, Ivanio |
dc.subject.por.fl_str_mv |
Aglomerados estelares Dinamica estelar Grande Nuvem de Magalhães |
topic |
Aglomerados estelares Dinamica estelar Grande Nuvem de Magalhães Galaxies: kinematics and dynamics Galaxies: structure Magellanic Clouds Open clusters and associations: general |
dc.subject.eng.fl_str_mv |
Galaxies: kinematics and dynamics Galaxies: structure Magellanic Clouds Open clusters and associations: general |
description |
The spatial distributions of SWB I [10<~t(Myr)30]<~ and SWB II [30<~t(Myr)<~70] LMC clusters are analyzed using the enlarged sample of integrated V BV photometry of star clusters and associations published by Bica et ai. in 1996. The differences in the clusters' spatial distributions are interpreted as dating back from their formation epoch and as being caused by a perturbation in the gaseous disk generated by the LMC stellar bar. The two SWB distributions present noncoincident bar or barlike struc tures with a position angle difference of ≈22° ± 2°, which, together with the age difference between the groups, leads to a perturbation propagation velocity of 13.7 ± 2 km s-ˡ kpc-ˡ, which suggests bar induced star formation effects bn the disk. Differences are also observed in the outer parts of the SWB I and SWB II spatial distributions. A spatial Fourier analysis reveals the predominance of m = 1 and m = 2 components in both cases. The spatial distribution of clusters younger than 10 Myr (SWB O) is also studied. The patterns measured by the Fourier analysis for the SWB O clusters resemble the gas distribution in the potential of disk models with an off-center bar. The H I kinematics is also evidence of the presence of the perturbation in the LMC disk. Although some evidence of locally induced star formation effects is found, our analysis indicates that globally triggered star formation effects induced by the potential play an important role in organizing the overall patterns and the toei of Shapley's Constellations. |
publishDate |
1996 |
dc.date.issued.fl_str_mv |
1996 |
dc.date.accessioned.fl_str_mv |
2015-01-07T02:10:56Z |
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 |
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publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/108779 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
dc.identifier.nrb.pt_BR.fl_str_mv |
000148842 |
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0004-637X 000148842 |
url |
http://hdl.handle.net/10183/108779 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Chicago. Vol. 461, no. 2, pt. 1 (Apr. 1996), p. 742-749 |
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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