Multiple mechanisms quench passive spiral galaxies
We examine the properties of a sample of 35 nearby passive spiral galaxies in order to determine their dominant quenching mechanism(s). All five low-mass (M⋆ < 1 × 1010 M⊙) passive spiral galaxies are located in the rich Virgo cluster. This is in contrast to low-mass spiral galaxies with star for...
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Oxford University Press
2018
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| Online Access: | https://eprints.nottingham.ac.uk/50495/ |
| _version_ | 1848798265577832448 |
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| author | Fraser-McKelvie, Amelia Brown, Michael J. I. Pimbblet, Kevin Dolley, Tim Bonne, Nicolas J. |
| author_facet | Fraser-McKelvie, Amelia Brown, Michael J. I. Pimbblet, Kevin Dolley, Tim Bonne, Nicolas J. |
| author_sort | Fraser-McKelvie, Amelia |
| building | Nottingham Research Data Repository |
| collection | Online Access |
| description | We examine the properties of a sample of 35 nearby passive spiral galaxies in order to determine their dominant quenching mechanism(s). All five low-mass (M⋆ < 1 × 1010 M⊙) passive spiral galaxies are located in the rich Virgo cluster. This is in contrast to low-mass spiral galaxies with star formation, which inhabit a range of environments. We postulate that cluster-scale gas stripping and heating mechanisms operating only in rich clusters are required to quench low-mass passive spirals, and ram-pressure stripping and strangulation are obvious candidates. For higher mass passive spirals, while trends are present, the story is less clear. The passive spiral bar fraction is high: 74 ± 15 per cent, compared with 36 ± 5 per cent for a mass, redshift and T-type matched comparison sample of star-forming spiral galaxies. The high mass passive spirals occur mostly, but not exclusively, in groups, and can be central or satellite galaxies. The passive spiral group fraction of 74 ± 15 per cent is similar to that of the comparison sample of star-forming galaxies at 61 ± 7 per cent. We find evidence for both quenching via internal structure and environment in our passive spiral sample, though some galaxies have evidence of neither. From this, we conclude no one mechanism is responsible for quenching star formation in passive spiral galaxies – rather, a mixture of mechanisms is required to produce the passive spiral distribution we see today. |
| first_indexed | 2025-11-14T20:17:02Z |
| format | Article |
| id | nottingham-50495 |
| institution | University of Nottingham Malaysia Campus |
| institution_category | Local University |
| last_indexed | 2025-11-14T20:17:02Z |
| publishDate | 2018 |
| publisher | Oxford University Press |
| recordtype | eprints |
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| spelling | nottingham-504952020-05-04T19:33:27Z https://eprints.nottingham.ac.uk/50495/ Multiple mechanisms quench passive spiral galaxies Fraser-McKelvie, Amelia Brown, Michael J. I. Pimbblet, Kevin Dolley, Tim Bonne, Nicolas J. We examine the properties of a sample of 35 nearby passive spiral galaxies in order to determine their dominant quenching mechanism(s). All five low-mass (M⋆ < 1 × 1010 M⊙) passive spiral galaxies are located in the rich Virgo cluster. This is in contrast to low-mass spiral galaxies with star formation, which inhabit a range of environments. We postulate that cluster-scale gas stripping and heating mechanisms operating only in rich clusters are required to quench low-mass passive spirals, and ram-pressure stripping and strangulation are obvious candidates. For higher mass passive spirals, while trends are present, the story is less clear. The passive spiral bar fraction is high: 74 ± 15 per cent, compared with 36 ± 5 per cent for a mass, redshift and T-type matched comparison sample of star-forming spiral galaxies. The high mass passive spirals occur mostly, but not exclusively, in groups, and can be central or satellite galaxies. The passive spiral group fraction of 74 ± 15 per cent is similar to that of the comparison sample of star-forming galaxies at 61 ± 7 per cent. We find evidence for both quenching via internal structure and environment in our passive spiral sample, though some galaxies have evidence of neither. From this, we conclude no one mechanism is responsible for quenching star formation in passive spiral galaxies – rather, a mixture of mechanisms is required to produce the passive spiral distribution we see today. Oxford University Press 2018-02-21 Article PeerReviewed Fraser-McKelvie, Amelia, Brown, Michael J. I., Pimbblet, Kevin, Dolley, Tim and Bonne, Nicolas J. (2018) Multiple mechanisms quench passive spiral galaxies. Monthly Notices of the Royal Astronomical Society, 474 (2). pp. 1909-1921. ISSN 1365-2966 galaxies: evolution galaxies: general galaxies: spiral galaxies: stellar content https://academic.oup.com/mnras/article/474/2/1909/4582902 doi:10.1093/mnras/stx2823 doi:10.1093/mnras/stx2823 |
| spellingShingle | galaxies: evolution galaxies: general galaxies: spiral galaxies: stellar content Fraser-McKelvie, Amelia Brown, Michael J. I. Pimbblet, Kevin Dolley, Tim Bonne, Nicolas J. Multiple mechanisms quench passive spiral galaxies |
| title | Multiple mechanisms quench passive spiral galaxies |
| title_full | Multiple mechanisms quench passive spiral galaxies |
| title_fullStr | Multiple mechanisms quench passive spiral galaxies |
| title_full_unstemmed | Multiple mechanisms quench passive spiral galaxies |
| title_short | Multiple mechanisms quench passive spiral galaxies |
| title_sort | multiple mechanisms quench passive spiral galaxies |
| topic | galaxies: evolution galaxies: general galaxies: spiral galaxies: stellar content |
| url | https://eprints.nottingham.ac.uk/50495/ https://eprints.nottingham.ac.uk/50495/ https://eprints.nottingham.ac.uk/50495/ |