Magnetized H i superbubbles in the Small Magellanic Cloud revealed by the POSSUM pilot survey
Article Swipe
S Lyla Jung
,
Amit Seta
,
J. Price
,
N. M. McClure‐Griffiths
,
J. D. Livingston
,
B. M. Gaensler
,
Yik Ki
,
Mehrnoosh Tahani
,
C. S. Anderson
,
Christoph Federrath
,
Cameron L. Van Eck
,
D. A. Leahy
,
S. P. O’Sullivan
,
Jennifer West
,
G. Heald
,
Takuya Akahori
·
YOU?
·
· 2024
· Open Access
·
· DOI: https://doi.org/10.1093/mnras/stae2245
YOU?
·
· 2024
· Open Access
·
· DOI: https://doi.org/10.1093/mnras/stae2245
Neutral hydrogen (H i) bubbles and shells are common in the interstellar medium (ISM). Studying their properties provides insight into the characteristics of the local ISM as well as the galaxy in which the bubbles reside. We report the detection of magnetic fields associated with superbubbles in the nearby irregular galaxy, the Small Magellanic Cloud (SMC). Using the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) pilot survey, we obtain a high-density grid ($\approx 25 \, \rm sources\, deg^{-2}$) of Faraday rotation measure (RM) from polarized sources behind the SMC. This provides a sufficiently large number of RM measurements to study the magnetic properties of three of the largest H i shells previously identified in the SMC. The RM profiles as a function of distance from the shell centre show characteristic patterns at angular scales comparable to the shell size. We demonstrate that this can be explained by magnetohydrodynamic simulation models of bubbles expanding in magnetized environments. From the observations, we estimate the line-of-sight magnetic field strength at the edges of the shells is enhanced by $\sim 1\, \rm \mu G$ with respect to their centres. This is an order of magnitude larger than the field strength in the ambient medium ($\sim 0.1\, \rm \mu G$) estimated based on the expansion velocity of the shells. This paper highlights the power of densely mapped RM grids in studying the magnetic properties of galactic substructures beyond the Milky Way.
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- Type
- article
- Language
- en
- Landing Page
- https://doi.org/10.1093/mnras/stae2245
- OA Status
- gold
- Cited By
- 1
- References
- 84
- Related Works
- 10
- OpenAlex ID
- https://openalex.org/W4402909135
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- DOI
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https://doi.org/10.1093/mnras/stae2245Digital Object Identifier
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Magnetized H
i superbubbles in the Small Magellanic Cloud revealed by the POSSUM pilot surveyWork title - Type
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articleOpenAlex work type
- Language
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enPrimary language
- Publication year
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2024Year of publication
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2024-09-27Full publication date if available
- Authors
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S Lyla Jung, Amit Seta, J. Price, N. M. McClure‐Griffiths, J. D. Livingston, B. M. Gaensler, Yik Ki, Mehrnoosh Tahani, C. S. Anderson, Christoph Federrath, Cameron L. Van Eck, D. A. Leahy, S. P. O’Sullivan, Jennifer West, G. Heald, Takuya AkahoriList of authors in order
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https://doi.org/10.1093/mnras/stae2245Publisher landing page
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YesWhether a free full text is available
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goldOpen access status per OpenAlex
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https://doi.org/10.1093/mnras/stae2245Direct OA link when available
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Physics, Astrophysics, Large Magellanic Cloud, Astronomy, Small Magellanic Cloud, Cloud computing, Stars, Operating system, Computer scienceTop concepts (fields/topics) attached by OpenAlex
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1Total citation count in OpenAlex
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2025: 1Per-year citation counts (last 5 years)
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10Other works algorithmically related by OpenAlex
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| abstract_inverted_index.densely | 222 |
| abstract_inverted_index.galaxy, | 51 |
| abstract_inverted_index.insight | 19 |
| abstract_inverted_index.largest | 109 |
| abstract_inverted_index.measure | 83 |
| abstract_inverted_index.reside. | 36 |
| abstract_inverted_index.respect | 183 |
| abstract_inverted_index.shells. | 215 |
| abstract_inverted_index.sources | 87 |
| abstract_inverted_index.survey, | 68 |
| abstract_inverted_index.(POSSUM) | 66 |
| abstract_inverted_index.ABSTRACT | 0 |
| abstract_inverted_index.Studying | 15 |
| abstract_inverted_index.centres. | 186 |
| abstract_inverted_index.distance | 125 |
| abstract_inverted_index.enhanced | 175 |
| abstract_inverted_index.estimate | 162 |
| abstract_inverted_index.function | 123 |
| abstract_inverted_index.galactic | 232 |
| abstract_inverted_index.hydrogen | 2 |
| abstract_inverted_index.magnetic | 42, 103, 165, 229 |
| abstract_inverted_index.patterns | 132 |
| abstract_inverted_index.profiles | 120 |
| abstract_inverted_index.provides | 18, 92 |
| abstract_inverted_index.rotation | 82 |
| abstract_inverted_index.strength | 167, 197 |
| abstract_inverted_index.studying | 227 |
| abstract_inverted_index.velocity | 212 |
| abstract_inverted_index.($\approx | 74 |
| abstract_inverted_index.Magnetism | 65 |
| abstract_inverted_index.detection | 40 |
| abstract_inverted_index.estimated | 207 |
| abstract_inverted_index.expanding | 154 |
| abstract_inverted_index.expansion | 211 |
| abstract_inverted_index.explained | 147 |
| abstract_inverted_index.irregular | 50 |
| abstract_inverted_index.magnitude | 192 |
| abstract_inverted_index.polarized | 86 |
| abstract_inverted_index.sources\, | 78 |
| abstract_inverted_index.Magellanic | 54 |
| abstract_inverted_index.associated | 44 |
| abstract_inverted_index.comparable | 136 |
| abstract_inverted_index.deg^{-2}$) | 79 |
| abstract_inverted_index.highlights | 218 |
| abstract_inverted_index.identified | 114 |
| abstract_inverted_index.magnetized | 156 |
| abstract_inverted_index.previously | 113 |
| abstract_inverted_index.properties | 17, 104, 230 |
| abstract_inverted_index.simulation | 150 |
| abstract_inverted_index.demonstrate | 142 |
| abstract_inverted_index.Polarisation | 59 |
| abstract_inverted_index.Universe’s | 64 |
| abstract_inverted_index.high-density | 72 |
| abstract_inverted_index.interstellar | 12 |
| abstract_inverted_index.measurements | 99 |
| abstract_inverted_index.sufficiently | 94 |
| abstract_inverted_index.superbubbles | 46 |
| abstract_inverted_index.environments. | 157 |
| abstract_inverted_index.line-of-sight | 164 |
| abstract_inverted_index.observations, | 160 |
| abstract_inverted_index.substructures | 233 |
| abstract_inverted_index.characteristic | 131 |
| abstract_inverted_index.characteristics | 22 |
| abstract_inverted_index.magnetohydrodynamic | 149 |
| cited_by_percentile_year.max | 95 |
| cited_by_percentile_year.min | 91 |
| countries_distinct_count | 7 |
| institutions_distinct_count | 16 |
| citation_normalized_percentile.value | 0.70322871 |
| citation_normalized_percentile.is_in_top_1_percent | False |
| citation_normalized_percentile.is_in_top_10_percent | False |