Electron density distribution in H ii regions in IC 10
We present the [O III] λ52 μm map of the dwarf galaxy IC 10 obtained with the Field-Imaging Far-Infrared Line Spectrometer on board the Stratospheric Observatory for Infrared Astronomy. We combine the [O III] λ52 μm map with Herschel and Spitzer observations to estimate the electron density distribu...
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| Main Authors: | , , , , , , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
2024 September
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| In: |
The astronomical journal
Year: 2024, Volume: 168, Issue: 3, Pages: 1-15 |
| ISSN: | 1538-3881 |
| DOI: | 10.3847/1538-3881/ad597a |
| Online Access: | Verlag, kostenfrei, Volltext: https://doi.org/10.3847/1538-3881/ad597a Verlag, kostenfrei, Volltext: https://dx.doi.org/10.3847/1538-3881/ad597a 
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| Author Notes: | Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, and Lise Ramambason |
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| 100 | 1 | |a Polles, Fiorella L. |e VerfasserIn |0 (DE-588)1180523857 |0 (DE-627)1067749853 |0 (DE-576)52019473X |4 aut | |
| 245 | 1 | 0 | |a Electron density distribution in H ii regions in IC 10 |c Fiorella L. Polles, Dario Fadda, William D. Vacca, Nicholas P. Abel, Mélanie Chevance, Christian Fischer, James M. Jackson, Vianney Lebouteiller, Suzanne Madden, and Lise Ramambason |
| 246 | 3 | 3 | |a Electron density distribution in H two regions in IC ten |
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| 520 | |a We present the [O III] λ52 μm map of the dwarf galaxy IC 10 obtained with the Field-Imaging Far-Infrared Line Spectrometer on board the Stratospheric Observatory for Infrared Astronomy. We combine the [O III] λ52 μm map with Herschel and Spitzer observations to estimate the electron density distribution of the brightest H ii regions of IC 10. We find that the line ratio [O III] λ88 μm/[O III] λ52 μm gives electron density (n e) values (n e [O III]) that cover a broad range, while the n e values obtained using the line ratio [S III] λ33 μm/[S III] λ18 μm (n e [S III]) are all similar within the uncertainties. n e [O III] is similar to n e [S III] for the M1, M2, and A1 regions, and it is higher than n e [S III] for the two regions, A2 and M1b, which are the brightest in the 24 μm continuum emission. These results suggest that for these regions, the two ions, O++ and S++, trace two different ionized gas components and that the properties of the ionized gas component traced by the O++ ion are more sensitive to the local physical conditions. In fact, while the gas layer traced by [S III] does not keep track of the characteristics of the radiation field, the n e [O III] correlates with the star formation rate, the dust temperature, and the 24 μm. Therefore, n e [O III] is an indicator of the evolutionary stage of the H ii region and the radiation field, with higher n e [O III] found in younger star-forming regions and in more energetic environments. | ||
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| 700 | 1 | |a Vacca, William D. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Abel, Nicholas P. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Chevance, Mélanie |e VerfasserIn |0 (DE-588)1141805553 |0 (DE-627)1000759342 |0 (DE-576)470814411 |4 aut | |
| 700 | 1 | |a Fischer, Christian |e VerfasserIn |4 aut | |
| 700 | 1 | |a Jackson, James M. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Lebouteiller, Vianney |e VerfasserIn |0 (DE-588)1205982906 |0 (DE-627)1691810630 |4 aut | |
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| 700 | 1 | |a Ramambason, Lise |e VerfasserIn |0 (DE-588)127952703X |0 (DE-627)1832659771 |4 aut | |
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