Study of McLeish's interacting object
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/10183/108230 |
Resumo: | We discuss the morphology, kinematics, and physical conditions of the emitting gas of the interacting system IRAS 20048—6621. We present as well numerical simulations of this interacting system, discovered by David McLeish in 1946. The main galaxy (McL A) is an edge-on spiral galaxy with highly distorted NW side. On this side is also located McL B, the perturber galaxy. We determined a distance of 151 Mpc (h=0.75) and a diameter of 70 kpc for McL A. It presents a bright nucleus with broad red emission lines (‹FWHM› ≈ 500 km s-ˡ). McL A has far-IR color indexes closely comparable to NGC 3628, one the few nearby edge-on galaxies which is a bright infrared emitter. Nevertheless, McL A is more luminous (in these bands) than any of the edge-on galaxies in the sample of bright infrared galaxies of Young et al. (1988). The two sides of McL A rotation curve are remarkably dierent. The N-body model that best reproduces McL A kinematical and morphological data (Kuijken & Dubinski 1995) gives a total mass 7x1011 Mʘ for McL A. Numerical simulations with the TREESPH code closely reproduce the morphology and radial velocity observations. The best scenario for this system is that of a prograde encounter between McL A and B, with McL B's orbit 35º tilted with respect to the spiral disk of McL A and a perigalactic distance of 17.6 kpc. The derived mass ratio is McL B/McL A≈1/26. In the last 5x108 yr the perturber has crossed the main galaxy disk twice, in between it crossed the perigalacticon. According to our simulations, the emitting gas present in McL B has not been stripped out from the McL A disk, so that leads us to conclude that McL B is an irregular or small spiral galaxy. |
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Díaz, Rubén JoaquínRodrigues, IrapuanDottori, Horacio AlbertoCarranza, Gustavo Jose2014-12-13T02:17:57Z20000004-6256http://hdl.handle.net/10183/108230000275517We discuss the morphology, kinematics, and physical conditions of the emitting gas of the interacting system IRAS 20048—6621. We present as well numerical simulations of this interacting system, discovered by David McLeish in 1946. The main galaxy (McL A) is an edge-on spiral galaxy with highly distorted NW side. On this side is also located McL B, the perturber galaxy. We determined a distance of 151 Mpc (h=0.75) and a diameter of 70 kpc for McL A. It presents a bright nucleus with broad red emission lines (‹FWHM› ≈ 500 km s-ˡ). McL A has far-IR color indexes closely comparable to NGC 3628, one the few nearby edge-on galaxies which is a bright infrared emitter. Nevertheless, McL A is more luminous (in these bands) than any of the edge-on galaxies in the sample of bright infrared galaxies of Young et al. (1988). The two sides of McL A rotation curve are remarkably dierent. The N-body model that best reproduces McL A kinematical and morphological data (Kuijken & Dubinski 1995) gives a total mass 7x1011 Mʘ for McL A. Numerical simulations with the TREESPH code closely reproduce the morphology and radial velocity observations. The best scenario for this system is that of a prograde encounter between McL A and B, with McL B's orbit 35º tilted with respect to the spiral disk of McL A and a perigalactic distance of 17.6 kpc. The derived mass ratio is McL B/McL A≈1/26. In the last 5x108 yr the perturber has crossed the main galaxy disk twice, in between it crossed the perigalacticon. According to our simulations, the emitting gas present in McL B has not been stripped out from the McL A disk, so that leads us to conclude that McL B is an irregular or small spiral galaxy.application/pdfengThe Astronomical journal. Chicago. Vol. 119, no. 1, (Jan. 2000), p. 111-118Galáxias ativasFotometria astronômicaEspectros astronômicosNucleo galaticoGaláxiasAstronomia infravermelhaGalaxies : binaryGalaxies : individual (McLeish's object)Galaxies : interactionsGalaxies : kinematics and dynamicsGalaxies : nucleiGalaxies : peculiarStudy of McLeish's interacting objectEstrangeiroinfo: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:UFRGSORIGINAL000275517.pdf000275517.pdfTexto completo (inglês)application/pdf629798http://www.lume.ufrgs.br/bitstream/10183/108230/1/000275517.pdf6fd720c1d2c30163360ecbaa655f56ecMD51TEXT000275517.pdf.txt000275517.pdf.txtExtracted Texttext/plain30726http://www.lume.ufrgs.br/bitstream/10183/108230/2/000275517.pdf.txta3ab868f506d56e20051ff8796975d1aMD52THUMBNAIL000275517.pdf.jpg000275517.pdf.jpgGenerated Thumbnailimage/jpeg2270http://www.lume.ufrgs.br/bitstream/10183/108230/3/000275517.pdf.jpga12bccc99b262356e8800f01452323c0MD5310183/1082302018-10-22 09:01:19.128oai:www.lume.ufrgs.br:10183/108230Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2018-10-22T12:01:19Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Study of McLeish's interacting object |
title |
Study of McLeish's interacting object |
spellingShingle |
Study of McLeish's interacting object Díaz, Rubén Joaquín Galáxias ativas Fotometria astronômica Espectros astronômicos Nucleo galatico Galáxias Astronomia infravermelha Galaxies : binary Galaxies : individual (McLeish's object) Galaxies : interactions Galaxies : kinematics and dynamics Galaxies : nuclei Galaxies : peculiar |
title_short |
Study of McLeish's interacting object |
title_full |
Study of McLeish's interacting object |
title_fullStr |
Study of McLeish's interacting object |
title_full_unstemmed |
Study of McLeish's interacting object |
title_sort |
Study of McLeish's interacting object |
author |
Díaz, Rubén Joaquín |
author_facet |
Díaz, Rubén Joaquín Rodrigues, Irapuan Dottori, Horacio Alberto Carranza, Gustavo Jose |
author_role |
author |
author2 |
Rodrigues, Irapuan Dottori, Horacio Alberto Carranza, Gustavo Jose |
author2_role |
author author author |
dc.contributor.author.fl_str_mv |
Díaz, Rubén Joaquín Rodrigues, Irapuan Dottori, Horacio Alberto Carranza, Gustavo Jose |
dc.subject.por.fl_str_mv |
Galáxias ativas Fotometria astronômica Espectros astronômicos Nucleo galatico Galáxias Astronomia infravermelha |
topic |
Galáxias ativas Fotometria astronômica Espectros astronômicos Nucleo galatico Galáxias Astronomia infravermelha Galaxies : binary Galaxies : individual (McLeish's object) Galaxies : interactions Galaxies : kinematics and dynamics Galaxies : nuclei Galaxies : peculiar |
dc.subject.eng.fl_str_mv |
Galaxies : binary Galaxies : individual (McLeish's object) Galaxies : interactions Galaxies : kinematics and dynamics Galaxies : nuclei Galaxies : peculiar |
description |
We discuss the morphology, kinematics, and physical conditions of the emitting gas of the interacting system IRAS 20048—6621. We present as well numerical simulations of this interacting system, discovered by David McLeish in 1946. The main galaxy (McL A) is an edge-on spiral galaxy with highly distorted NW side. On this side is also located McL B, the perturber galaxy. We determined a distance of 151 Mpc (h=0.75) and a diameter of 70 kpc for McL A. It presents a bright nucleus with broad red emission lines (‹FWHM› ≈ 500 km s-ˡ). McL A has far-IR color indexes closely comparable to NGC 3628, one the few nearby edge-on galaxies which is a bright infrared emitter. Nevertheless, McL A is more luminous (in these bands) than any of the edge-on galaxies in the sample of bright infrared galaxies of Young et al. (1988). The two sides of McL A rotation curve are remarkably dierent. The N-body model that best reproduces McL A kinematical and morphological data (Kuijken & Dubinski 1995) gives a total mass 7x1011 Mʘ for McL A. Numerical simulations with the TREESPH code closely reproduce the morphology and radial velocity observations. The best scenario for this system is that of a prograde encounter between McL A and B, with McL B's orbit 35º tilted with respect to the spiral disk of McL A and a perigalactic distance of 17.6 kpc. The derived mass ratio is McL B/McL A≈1/26. In the last 5x108 yr the perturber has crossed the main galaxy disk twice, in between it crossed the perigalacticon. According to our simulations, the emitting gas present in McL B has not been stripped out from the McL A disk, so that leads us to conclude that McL B is an irregular or small spiral galaxy. |
publishDate |
2000 |
dc.date.issued.fl_str_mv |
2000 |
dc.date.accessioned.fl_str_mv |
2014-12-13T02:17:57Z |
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Estrangeiro info:eu-repo/semantics/article |
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article |
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publishedVersion |
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http://hdl.handle.net/10183/108230 |
dc.language.iso.fl_str_mv |
eng |
language |
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dc.relation.ispartof.pt_BR.fl_str_mv |
The Astronomical journal. Chicago. Vol. 119, no. 1, (Jan. 2000), p. 111-118 |
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openAccess |
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