Global environmental effects versus galaxy interactions

We explore properties of close galaxy pairs and merging systems selected from the Sloan Digital Sky Survey Data Release 4 in different environments with the aim to assess the relative importance of the role of interactions over global environmental processes. For this purpose, we perform a comparati...

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Detalles Bibliográficos
Publicado: 2009
Materias:
Galaxies: evolution
Galaxies: general
Galaxies: interactions
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v399_n3_p1157_Perez
http://hdl.handle.net/20.500.12110/paper_00358711_v399_n3_p1157_Perez
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00358711_v399_n3_p1157_Perez
record_format dspace
spelling paper:paper_00358711_v399_n3_p1157_Perez2023-06-08T15:01:28Z Global environmental effects versus galaxy interactions Galaxies: evolution Galaxies: general Galaxies: interactions We explore properties of close galaxy pairs and merging systems selected from the Sloan Digital Sky Survey Data Release 4 in different environments with the aim to assess the relative importance of the role of interactions over global environmental processes. For this purpose, we perform a comparative study of galaxies with and without close companions as a function of local density and host halo mass, carefully removing sources of possible biases. We find that at low- and high-local-density environments, colours and concentration indices of close galaxy pairs are very similar to those of isolated galaxies. At intermediate densities, we detect significant differences, indicating that close pairs could have experienced a more rapid transition on to the red sequence than isolated galaxies. The presence of a correlation between concentration index and colours indicates that the physical mechanism responsible for the colour transformation also operates in the transformation of the luminous matter distribution. At fixed local densities, we find a dependence of the red galaxy fraction on dark matter halo mass for galaxies with or without a close companion. This suggests the action of host halo mass related effects. Regardless of dark matter halo mass, we show that the percentage of red galaxies in close pairs and in the control sample are comparable at low- and high-local-density environments. However, at intermediate local densities, the gap in the red fraction between close pairs and the control galaxies increases from ∼10 per cent in low-mass haloes up to ∼50 per cent in the most massive ones. Interestingly, we also detect that 50 per cent of merging systems populate the intermediate local environments, with a large fraction of them being extremely red and bulge dominated. Our findings suggest that in intermediate-density environments galaxies are efficiently pre-processed by close encounters and mergers before entering higher local density regions. © 2009 RAS. 2009 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v399_n3_p1157_Perez http://hdl.handle.net/20.500.12110/paper_00358711_v399_n3_p1157_Perez
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Galaxies: evolution
Galaxies: general
Galaxies: interactions
spellingShingle Galaxies: evolution
Galaxies: general
Galaxies: interactions
Global environmental effects versus galaxy interactions
topic_facet Galaxies: evolution
Galaxies: general
Galaxies: interactions
description We explore properties of close galaxy pairs and merging systems selected from the Sloan Digital Sky Survey Data Release 4 in different environments with the aim to assess the relative importance of the role of interactions over global environmental processes. For this purpose, we perform a comparative study of galaxies with and without close companions as a function of local density and host halo mass, carefully removing sources of possible biases. We find that at low- and high-local-density environments, colours and concentration indices of close galaxy pairs are very similar to those of isolated galaxies. At intermediate densities, we detect significant differences, indicating that close pairs could have experienced a more rapid transition on to the red sequence than isolated galaxies. The presence of a correlation between concentration index and colours indicates that the physical mechanism responsible for the colour transformation also operates in the transformation of the luminous matter distribution. At fixed local densities, we find a dependence of the red galaxy fraction on dark matter halo mass for galaxies with or without a close companion. This suggests the action of host halo mass related effects. Regardless of dark matter halo mass, we show that the percentage of red galaxies in close pairs and in the control sample are comparable at low- and high-local-density environments. However, at intermediate local densities, the gap in the red fraction between close pairs and the control galaxies increases from ∼10 per cent in low-mass haloes up to ∼50 per cent in the most massive ones. Interestingly, we also detect that 50 per cent of merging systems populate the intermediate local environments, with a large fraction of them being extremely red and bulge dominated. Our findings suggest that in intermediate-density environments galaxies are efficiently pre-processed by close encounters and mergers before entering higher local density regions. © 2009 RAS.
title Global environmental effects versus galaxy interactions
title_short Global environmental effects versus galaxy interactions
title_full Global environmental effects versus galaxy interactions
title_fullStr Global environmental effects versus galaxy interactions
title_full_unstemmed Global environmental effects versus galaxy interactions
title_sort global environmental effects versus galaxy interactions
publishDate 2009
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00358711_v399_n3_p1157_Perez
http://hdl.handle.net/20.500.12110/paper_00358711_v399_n3_p1157_Perez
_version_ 1768543599442526208

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