Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831
Autor(a) principal: | |
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Data de Publicação: | 2002 |
Outros Autores: | , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/206297 |
Resumo: | We present the analysis of a deep colour-magnitude diagram (CMD) of NGC 1831, a rich star cluster in the LMC. The data were obtained with HST/WFPC2 in the F555W (~V) and F814W (~I) filters, reaching m555~25. We discuss and apply a method of correcting the CMD for sampling incompleteness and field star contamination. Efficient use of the CMD data was made by means of direct comparisons of the observed to model CMDs. The model CMDs are built by an algorithm that generates artificial stars from a single stellar population, characterized by an age, a metallicity, a distance, a reddening value, a present day mass function and a fraction of unresolved binaries. Photometric uncertainties are empirically determined from the data and incorporated into the models as well. Statistical techniques are presented and applied as an objective method to assess the compatibility between the model and data CMDs. By modelling the CMD of the central region in NGC 1831 we infer a metallicity Z=0.012, 8.75≤log(τ/yr)≤ 8.80, 18.54 ≤ (m− M)0 ≤ 18.68 and 0.00≤ E(B−V) ≤ 0.03. For the position dependent PDMF slope (α = −dlogΦ(M)/dlogM), we clearly observe the effect of mass segregation in the system: for projected distances R≤30 arcsec, α=1.7, whereas 2.2≤α≤2.5 in the outer regions of NGC1831. |
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Kerber, Leandro de OliveiraSantiago, Basilio XavierCastro, RodrigoValls-Gabaud, D.2020-02-28T04:05:46Z20020004-6361http://hdl.handle.net/10183/206297000330644We present the analysis of a deep colour-magnitude diagram (CMD) of NGC 1831, a rich star cluster in the LMC. The data were obtained with HST/WFPC2 in the F555W (~V) and F814W (~I) filters, reaching m555~25. We discuss and apply a method of correcting the CMD for sampling incompleteness and field star contamination. Efficient use of the CMD data was made by means of direct comparisons of the observed to model CMDs. The model CMDs are built by an algorithm that generates artificial stars from a single stellar population, characterized by an age, a metallicity, a distance, a reddening value, a present day mass function and a fraction of unresolved binaries. Photometric uncertainties are empirically determined from the data and incorporated into the models as well. Statistical techniques are presented and applied as an objective method to assess the compatibility between the model and data CMDs. By modelling the CMD of the central region in NGC 1831 we infer a metallicity Z=0.012, 8.75≤log(τ/yr)≤ 8.80, 18.54 ≤ (m− M)0 ≤ 18.68 and 0.00≤ E(B−V) ≤ 0.03. For the position dependent PDMF slope (α = −dlogΦ(M)/dlogM), we clearly observe the effect of mass segregation in the system: for projected distances R≤30 arcsec, α=1.7, whereas 2.2≤α≤2.5 in the outer regions of NGC1831.application/pdfengAstronomy and astrophysics. Les Ulis. Vol. 390, no. 1 (July 2002), p. 121-132Grande Nuvem de MagalhãesAglomerados estelaresFotometria estelarGalaxies: star clustersMagellanic CloudGlobular clusters: individual: NGC 1831Stars: statisticsAnalysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831Estrangeiroinfo: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:UFRGSTEXT000330644.pdf.txt000330644.pdf.txtExtracted Texttext/plain53574http://www.lume.ufrgs.br/bitstream/10183/206297/2/000330644.pdf.txt66a23242b78eb15b979510d60946786eMD52ORIGINAL000330644.pdfTexto completo (inglês)application/pdf611617http://www.lume.ufrgs.br/bitstream/10183/206297/1/000330644.pdf25a2bff6c707032dd0b602f313109c26MD5110183/2062972023-07-05 03:47:16.835949oai:www.lume.ufrgs.br:10183/206297Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-07-05T06:47:16Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831 |
title |
Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831 |
spellingShingle |
Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831 Kerber, Leandro de Oliveira Grande Nuvem de Magalhães Aglomerados estelares Fotometria estelar Galaxies: star clusters Magellanic Cloud Globular clusters: individual: NGC 1831 Stars: statistics |
title_short |
Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831 |
title_full |
Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831 |
title_fullStr |
Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831 |
title_full_unstemmed |
Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831 |
title_sort |
Analysis of colour-magnitude diagrams of rich LMC clusters : NGC 1831 |
author |
Kerber, Leandro de Oliveira |
author_facet |
Kerber, Leandro de Oliveira Santiago, Basilio Xavier Castro, Rodrigo Valls-Gabaud, D. |
author_role |
author |
author2 |
Santiago, Basilio Xavier Castro, Rodrigo Valls-Gabaud, D. |
author2_role |
author author author |
dc.contributor.author.fl_str_mv |
Kerber, Leandro de Oliveira Santiago, Basilio Xavier Castro, Rodrigo Valls-Gabaud, D. |
dc.subject.por.fl_str_mv |
Grande Nuvem de Magalhães Aglomerados estelares Fotometria estelar |
topic |
Grande Nuvem de Magalhães Aglomerados estelares Fotometria estelar Galaxies: star clusters Magellanic Cloud Globular clusters: individual: NGC 1831 Stars: statistics |
dc.subject.eng.fl_str_mv |
Galaxies: star clusters Magellanic Cloud Globular clusters: individual: NGC 1831 Stars: statistics |
description |
We present the analysis of a deep colour-magnitude diagram (CMD) of NGC 1831, a rich star cluster in the LMC. The data were obtained with HST/WFPC2 in the F555W (~V) and F814W (~I) filters, reaching m555~25. We discuss and apply a method of correcting the CMD for sampling incompleteness and field star contamination. Efficient use of the CMD data was made by means of direct comparisons of the observed to model CMDs. The model CMDs are built by an algorithm that generates artificial stars from a single stellar population, characterized by an age, a metallicity, a distance, a reddening value, a present day mass function and a fraction of unresolved binaries. Photometric uncertainties are empirically determined from the data and incorporated into the models as well. Statistical techniques are presented and applied as an objective method to assess the compatibility between the model and data CMDs. By modelling the CMD of the central region in NGC 1831 we infer a metallicity Z=0.012, 8.75≤log(τ/yr)≤ 8.80, 18.54 ≤ (m− M)0 ≤ 18.68 and 0.00≤ E(B−V) ≤ 0.03. For the position dependent PDMF slope (α = −dlogΦ(M)/dlogM), we clearly observe the effect of mass segregation in the system: for projected distances R≤30 arcsec, α=1.7, whereas 2.2≤α≤2.5 in the outer regions of NGC1831. |
publishDate |
2002 |
dc.date.issued.fl_str_mv |
2002 |
dc.date.accessioned.fl_str_mv |
2020-02-28T04:05:46Z |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
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article |
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publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/206297 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-6361 |
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000330644 |
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0004-6361 000330644 |
url |
http://hdl.handle.net/10183/206297 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
Astronomy and astrophysics. Les Ulis. Vol. 390, no. 1 (July 2002), p. 121-132 |
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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UFRGS |
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Repositório Institucional da UFRGS |
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Repositório Institucional da UFRGS |
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http://www.lume.ufrgs.br/bitstream/10183/206297/2/000330644.pdf.txt http://www.lume.ufrgs.br/bitstream/10183/206297/1/000330644.pdf |
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