Role of Magnetic Fields in Ram Pressure Stripped Galaxies
Ram-pressure stripping is a crucial evolutionary driver for cluster galaxies and jellyfish galaxies characterized by very extended tails of stripped gas, and they are the most striking examples of it in action. Recently, those extended tails are found to show ongoing star formation, raising the ques...
| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | English |
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MDPI AG
2021-12-01
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| Series: | Galaxies |
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| Online Access: | https://www.mdpi.com/2075-4434/9/4/116 |
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| author | Ancla Müller Alessandro Ignesti Bianca Poggianti Alessia Moretti Mpati Ramatsoku Ralf-Jürgen Dettmar |
| author_facet | Ancla Müller Alessandro Ignesti Bianca Poggianti Alessia Moretti Mpati Ramatsoku Ralf-Jürgen Dettmar |
| author_sort | Ancla Müller |
| collection | DOAJ |
| description | Ram-pressure stripping is a crucial evolutionary driver for cluster galaxies and jellyfish galaxies characterized by very extended tails of stripped gas, and they are the most striking examples of it in action. Recently, those extended tails are found to show ongoing star formation, raising the question of how the stripped, cold gas can survive long enough to form new stars outside the stellar disk. In this study, we summarize the most recent results achieved within the GASP collaboration to provide a holistic explanation for this phenomenon. We focus on two textbook examples of jellyfish galaxies, JO206 and JW100, for which, via multi-wavelength observations from radio to X-ray and numerical simulations, we have explored the different gas phases (neutral, molecular, diffuse-ionized, and hot). Based on additional multi-phase gas studies, we now propose a scenario of stripped tail evolution including all phases that are driven by a magnetic draping sheath, where the intracluster turbulent magnetized plasma condenses onto the galaxy disk and tail and produces a magnetized interface that protects the stripped galaxy tail gas from evaporation. In such a scenario, the accreted environmental plasma can cool down and eventually join the tail gas, hence providing additional gas to form stars. The implications of our findings can shed light on the more general scenario of draping, condensation, and cooling of hot gas surrounding cold clouds that is fundamental in many astrophysical phenomena. |
| first_indexed | 2024-03-10T04:04:11Z |
| format | Article |
| id | doaj.art-43ae8ed3636a45529e633f12bbcaa945 |
| institution | Directory Open Access Journal |
| issn | 2075-4434 |
| language | English |
| last_indexed | 2024-03-10T04:04:11Z |
| publishDate | 2021-12-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Galaxies |
| spelling | doaj.art-43ae8ed3636a45529e633f12bbcaa9452023-11-23T08:26:26ZengMDPI AGGalaxies2075-44342021-12-019411610.3390/galaxies9040116Role of Magnetic Fields in Ram Pressure Stripped GalaxiesAncla Müller0Alessandro Ignesti1Bianca Poggianti2Alessia Moretti3Mpati Ramatsoku4Ralf-Jürgen Dettmar5Faculty of Physics and Astronomy, Astronomical Institute, Ruhr University Bochum, Universitätsstr. 150, 44801 Bochum, GermanyINAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I35122 Padova, ItalyINAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I35122 Padova, ItalyINAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I35122 Padova, ItalyDepartment of Physics & Electronics, Rhodes University, Makhanda 6139, South AfricaFaculty of Physics and Astronomy, Astronomical Institute, Ruhr University Bochum, Universitätsstr. 150, 44801 Bochum, GermanyRam-pressure stripping is a crucial evolutionary driver for cluster galaxies and jellyfish galaxies characterized by very extended tails of stripped gas, and they are the most striking examples of it in action. Recently, those extended tails are found to show ongoing star formation, raising the question of how the stripped, cold gas can survive long enough to form new stars outside the stellar disk. In this study, we summarize the most recent results achieved within the GASP collaboration to provide a holistic explanation for this phenomenon. We focus on two textbook examples of jellyfish galaxies, JO206 and JW100, for which, via multi-wavelength observations from radio to X-ray and numerical simulations, we have explored the different gas phases (neutral, molecular, diffuse-ionized, and hot). Based on additional multi-phase gas studies, we now propose a scenario of stripped tail evolution including all phases that are driven by a magnetic draping sheath, where the intracluster turbulent magnetized plasma condenses onto the galaxy disk and tail and produces a magnetized interface that protects the stripped galaxy tail gas from evaporation. In such a scenario, the accreted environmental plasma can cool down and eventually join the tail gas, hence providing additional gas to form stars. The implications of our findings can shed light on the more general scenario of draping, condensation, and cooling of hot gas surrounding cold clouds that is fundamental in many astrophysical phenomena.https://www.mdpi.com/2075-4434/9/4/116galaxies: magnetic fieldsgalaxies: evolutiongalaxies: ISMradio continuum: galaxiespolarization |
| spellingShingle | Ancla Müller Alessandro Ignesti Bianca Poggianti Alessia Moretti Mpati Ramatsoku Ralf-Jürgen Dettmar Role of Magnetic Fields in Ram Pressure Stripped Galaxies Galaxies galaxies: magnetic fields galaxies: evolution galaxies: ISM radio continuum: galaxies polarization |
| title | Role of Magnetic Fields in Ram Pressure Stripped Galaxies |
| title_full | Role of Magnetic Fields in Ram Pressure Stripped Galaxies |
| title_fullStr | Role of Magnetic Fields in Ram Pressure Stripped Galaxies |
| title_full_unstemmed | Role of Magnetic Fields in Ram Pressure Stripped Galaxies |
| title_short | Role of Magnetic Fields in Ram Pressure Stripped Galaxies |
| title_sort | role of magnetic fields in ram pressure stripped galaxies |
| topic | galaxies: magnetic fields galaxies: evolution galaxies: ISM radio continuum: galaxies polarization |
| url | https://www.mdpi.com/2075-4434/9/4/116 |
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