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| Main Authors: | , , , |
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| Format: | Preprint |
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2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2406.01742 |
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| _version_ | 1866914821766643712 |
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| author | Kim, Jin-Ah Chung, Haeun Vargas, Carlos J. Hamden, Erika |
| author_facet | Kim, Jin-Ah Chung, Haeun Vargas, Carlos J. Hamden, Erika |
| contents | We examined archival Far Ultraviolet Spectroscopic Explorer data to search for far-ultraviolet emission lines in the starburst galaxy M82. The observations were made in an outflow region that extends beyond the galactic disk. We found the O VI $λλ$ 1032, 1038 emission lines from the galaxy's southern outflow region. The O VI lines suggest that the outflowing warm-hot gas is undergoing radiative cooling. We measured a radial velocity of $\sim$420 km s$^{-1}$ from the O VI lines, which is faster than the velocity seen in H$α$ observations. The O VI $λ$1038 emission line seems to be blended with the C II $λ$1037 emission line, which has a radial velocity of $\sim$300 km s$^{-1}$, similar to what is observed in H$α$ observations. The outflow medium of M82 appears to be composed of gas in multiple phases with varying temperatures and kinematics. Future spectroscopic observations in high energy regimes covering a wider spatial area are necessary to understand better the properties of the warm-hot gas medium in the outflow. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2406_01742 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | UV Cooling via O VI Emission in the Superwind of M82 Observed with the Far Ultraviolet Spectroscopic Explorer (FUSE) Kim, Jin-Ah Chung, Haeun Vargas, Carlos J. Hamden, Erika Astrophysics of Galaxies We examined archival Far Ultraviolet Spectroscopic Explorer data to search for far-ultraviolet emission lines in the starburst galaxy M82. The observations were made in an outflow region that extends beyond the galactic disk. We found the O VI $λλ$ 1032, 1038 emission lines from the galaxy's southern outflow region. The O VI lines suggest that the outflowing warm-hot gas is undergoing radiative cooling. We measured a radial velocity of $\sim$420 km s$^{-1}$ from the O VI lines, which is faster than the velocity seen in H$α$ observations. The O VI $λ$1038 emission line seems to be blended with the C II $λ$1037 emission line, which has a radial velocity of $\sim$300 km s$^{-1}$, similar to what is observed in H$α$ observations. The outflow medium of M82 appears to be composed of gas in multiple phases with varying temperatures and kinematics. Future spectroscopic observations in high energy regimes covering a wider spatial area are necessary to understand better the properties of the warm-hot gas medium in the outflow. |
| title | UV Cooling via O VI Emission in the Superwind of M82 Observed with the Far Ultraviolet Spectroscopic Explorer (FUSE) |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2406.01742 |