Dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback
We investigate the impact of ram pressure stripping due to the intracluster medium (ICM) on star-forming disk galaxies with a multiphase interstellar medium maintained by strong stellar feedback. We carry out radiation-hydrodynamic simulations of an isolated disk galaxy embedded in a 1011 M ⊙ dark m...
| Main Authors: | , , , , , |
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| Format: | Journal article |
| Language: | English |
| Published: |
IOP Science
2020
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| _version_ | 1797053947111800832 |
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| author | Lee, J Kimm, T Katz, H Rosdahl, J Devriendt, J Slyz, A |
| author_facet | Lee, J Kimm, T Katz, H Rosdahl, J Devriendt, J Slyz, A |
| author_sort | Lee, J |
| collection | OXFORD |
| description | We investigate the impact of ram pressure stripping due to the intracluster medium (ICM) on star-forming disk galaxies with a multiphase interstellar medium maintained by strong stellar feedback. We carry out radiation-hydrodynamic simulations of an isolated disk galaxy embedded in a 1011 M ⊙ dark matter halo with various ICM winds mimicking the cluster outskirts (moderate) and the central environment (strong). We find that both star formation quenching and triggering occur in ram pressure–stripped galaxies, depending on the strength of the winds. H i and H2 in the outer galactic disk are significantly stripped in the presence of moderate winds, whereas turbulent pressure provides support against ram pressure in the central region, where star formation is active. Moderate ICM winds facilitate gas collapse, increasing the total star formation rates by ~40% when the wind is oriented face-on or by ~80% when it is edge-on. In contrast, strong winds rapidly blow away neutral and molecular hydrogen gas from the galaxy, suppressing star formation by a factor of 2 within ~200 Myr. Dense gas clumps with n H gsim 10 M ⊙ pc−2 are easily identified in extraplanar regions, but no significant young stellar populations are found in such clumps. In our attempts to enhance radiative cooling by adopting a colder ICM of T = 106 K, only a few additional stars are formed in the tail region, even if the amount of newly cooled gas increases by an order of magnitude. |
| first_indexed | 2024-03-06T18:50:43Z |
| format | Journal article |
| id | oxford-uuid:101f108f-d4ed-4106-b6e0-91b3ae418f8d |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T18:50:43Z |
| publishDate | 2020 |
| publisher | IOP Science |
| record_format | dspace |
| spelling | oxford-uuid:101f108f-d4ed-4106-b6e0-91b3ae418f8d2022-03-26T09:54:49ZDual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedbackJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:101f108f-d4ed-4106-b6e0-91b3ae418f8dEnglishSymplectic ElementsIOP Science2020Lee, JKimm, TKatz, HRosdahl, JDevriendt, JSlyz, AWe investigate the impact of ram pressure stripping due to the intracluster medium (ICM) on star-forming disk galaxies with a multiphase interstellar medium maintained by strong stellar feedback. We carry out radiation-hydrodynamic simulations of an isolated disk galaxy embedded in a 1011 M ⊙ dark matter halo with various ICM winds mimicking the cluster outskirts (moderate) and the central environment (strong). We find that both star formation quenching and triggering occur in ram pressure–stripped galaxies, depending on the strength of the winds. H i and H2 in the outer galactic disk are significantly stripped in the presence of moderate winds, whereas turbulent pressure provides support against ram pressure in the central region, where star formation is active. Moderate ICM winds facilitate gas collapse, increasing the total star formation rates by ~40% when the wind is oriented face-on or by ~80% when it is edge-on. In contrast, strong winds rapidly blow away neutral and molecular hydrogen gas from the galaxy, suppressing star formation by a factor of 2 within ~200 Myr. Dense gas clumps with n H gsim 10 M ⊙ pc−2 are easily identified in extraplanar regions, but no significant young stellar populations are found in such clumps. In our attempts to enhance radiative cooling by adopting a colder ICM of T = 106 K, only a few additional stars are formed in the tail region, even if the amount of newly cooled gas increases by an order of magnitude. |
| spellingShingle | Lee, J Kimm, T Katz, H Rosdahl, J Devriendt, J Slyz, A Dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback |
| title | Dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback |
| title_full | Dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback |
| title_fullStr | Dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback |
| title_full_unstemmed | Dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback |
| title_short | Dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback |
| title_sort | dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback |
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