Linking the structural properties of galaxies and their star formation histories with STAGES
We study the links between star formation history and structure for a large mass-selected galaxy sample at 0.05 ≤ zphot ≤ 0.30. The galaxies inhabit a very broad range of environments, from cluster cores to the field. Using Hubble Space Telescope (HST) images, we quantify their structure following H...
| Main Authors: | , , , , , , , |
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| Format: | Article |
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Oxford University Press
2016
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| Online Access: | https://eprints.nottingham.ac.uk/42045/ |
| _version_ | 1848796405204779008 |
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| author | Hoyos, Carlos Aragón-Salamanca, Alfonso Gray, Meghan E. Wolf, Christian Maltby, David T. Bell, Eric F. Böhm, Asmus Jogee, Shardha |
| author_facet | Hoyos, Carlos Aragón-Salamanca, Alfonso Gray, Meghan E. Wolf, Christian Maltby, David T. Bell, Eric F. Böhm, Asmus Jogee, Shardha |
| author_sort | Hoyos, Carlos |
| building | Nottingham Research Data Repository |
| collection | Online Access |
| description | We study the links between star formation history and structure for a large mass-selected galaxy sample at 0.05 ≤ zphot ≤ 0.30. The galaxies inhabit a very broad range of environments, from cluster cores to the field. Using Hubble Space Telescope (HST) images, we quantify their structure following Hoyos et al., and divide them into disturbed and undisturbed. We also visually identify mergers. Additionally, we provide a quantitative measure of the degree of disturbance for each galaxy (‘roughness’). The majority of elliptical and lenticular galaxies have relaxed structure, showing no signs of ongoing star formation. Structurally disturbed galaxies, which tend to avoid the lowest density regions, have higher star formation activity and younger stellar populations than undisturbed systems. Cluster spirals with reduced/quenched star formation have somewhat less disturbed morphologies than spirals with ‘normal’ star formation activity, suggesting that these ‘passive’ spirals have started their morphological transformation into S0s. Visually identified mergers and galaxies not identified as mergers but with similar roughness have similar specific star formation rates and stellar ages. The degree of enhanced star formation is thus linked to the degree of structural disturbance, regardless of whether it is caused by major mergers or not. This suggests that merging galaxies are not special in terms of their higher-than-normal star formation activity. Any physical process that produces ‘roughness’, or regions of enhanced luminosity density, will increase the star formation activity in a galaxy with similar efficiency. An alternative explanation is that star formation episodes increase the galaxies’ roughness similarly, regardless of whether they are merger induced or not. |
| first_indexed | 2025-11-14T19:47:27Z |
| format | Article |
| id | nottingham-42045 |
| institution | University of Nottingham Malaysia Campus |
| institution_category | Local University |
| last_indexed | 2025-11-14T19:47:27Z |
| publishDate | 2016 |
| publisher | Oxford University Press |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | nottingham-420452020-05-04T17:24:42Z https://eprints.nottingham.ac.uk/42045/ Linking the structural properties of galaxies and their star formation histories with STAGES Hoyos, Carlos Aragón-Salamanca, Alfonso Gray, Meghan E. Wolf, Christian Maltby, David T. Bell, Eric F. Böhm, Asmus Jogee, Shardha We study the links between star formation history and structure for a large mass-selected galaxy sample at 0.05 ≤ zphot ≤ 0.30. The galaxies inhabit a very broad range of environments, from cluster cores to the field. Using Hubble Space Telescope (HST) images, we quantify their structure following Hoyos et al., and divide them into disturbed and undisturbed. We also visually identify mergers. Additionally, we provide a quantitative measure of the degree of disturbance for each galaxy (‘roughness’). The majority of elliptical and lenticular galaxies have relaxed structure, showing no signs of ongoing star formation. Structurally disturbed galaxies, which tend to avoid the lowest density regions, have higher star formation activity and younger stellar populations than undisturbed systems. Cluster spirals with reduced/quenched star formation have somewhat less disturbed morphologies than spirals with ‘normal’ star formation activity, suggesting that these ‘passive’ spirals have started their morphological transformation into S0s. Visually identified mergers and galaxies not identified as mergers but with similar roughness have similar specific star formation rates and stellar ages. The degree of enhanced star formation is thus linked to the degree of structural disturbance, regardless of whether it is caused by major mergers or not. This suggests that merging galaxies are not special in terms of their higher-than-normal star formation activity. Any physical process that produces ‘roughness’, or regions of enhanced luminosity density, will increase the star formation activity in a galaxy with similar efficiency. An alternative explanation is that star formation episodes increase the galaxies’ roughness similarly, regardless of whether they are merger induced or not. Oxford University Press 2016-01-01 Article PeerReviewed Hoyos, Carlos, Aragón-Salamanca, Alfonso, Gray, Meghan E., Wolf, Christian, Maltby, David T., Bell, Eric F., Böhm, Asmus and Jogee, Shardha (2016) Linking the structural properties of galaxies and their star formation histories with STAGES. Monthly Notices of the Royal Astronomical Society, 455 (1). pp. 295-307. ISSN 1365-2966 galaxies: clusters: individual: Abell 901 Abell 902 galaxies: evolution galaxies: formation galaxies: peculiar galaxies: structure https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stv2321 doi:10.1093/mnras/stv2321 doi:10.1093/mnras/stv2321 |
| spellingShingle | galaxies: clusters: individual: Abell 901 Abell 902 galaxies: evolution galaxies: formation galaxies: peculiar galaxies: structure Hoyos, Carlos Aragón-Salamanca, Alfonso Gray, Meghan E. Wolf, Christian Maltby, David T. Bell, Eric F. Böhm, Asmus Jogee, Shardha Linking the structural properties of galaxies and their star formation histories with STAGES |
| title | Linking the structural properties of galaxies and their star formation histories with STAGES |
| title_full | Linking the structural properties of galaxies and their star formation histories with STAGES |
| title_fullStr | Linking the structural properties of galaxies and their star formation histories with STAGES |
| title_full_unstemmed | Linking the structural properties of galaxies and their star formation histories with STAGES |
| title_short | Linking the structural properties of galaxies and their star formation histories with STAGES |
| title_sort | linking the structural properties of galaxies and their star formation histories with stages |
| topic | galaxies: clusters: individual: Abell 901 Abell 902 galaxies: evolution galaxies: formation galaxies: peculiar galaxies: structure |
| url | https://eprints.nottingham.ac.uk/42045/ https://eprints.nottingham.ac.uk/42045/ https://eprints.nottingham.ac.uk/42045/ |