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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| Hauptverfasser: | , , , , , , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2024 September
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| In: |
The astronomical journal
Year: 2024, Jahrgang: 168, Heft: 3, Pages: 1-15 |
| ISSN: | 1538-3881 |
| DOI: | 10.3847/1538-3881/ad597a |
| Online-Zugang: | 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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| Verfasserangaben: | 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 |
| Zusammenfassung: | 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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| Beschreibung: | Online veröffentlicht am 13. August 2024 Gesehen am 26.05.2025 |
| Beschreibung: | Online Resource |
| ISSN: | 1538-3881 |
| DOI: | 10.3847/1538-3881/ad597a |