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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: Polles, Fiorella L. (Author) , Fadda, Dario (Author) , Vacca, William D. (Author) , Abel, Nicholas P. (Author) , Chevance, Mélanie (Author) , Fischer, Christian (Author) , Jackson, James M. (Author) , Lebouteiller, Vianney (Author) , Madden, Suzanne (Author) , Ramambason, Lise (Author)
Format: Article (Journal)
Language:English
Published: 2024 September
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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Summary: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.
Item Description:Online veröffentlicht am 13. August 2024
Gesehen am 26.05.2025
Physical Description:Online Resource
ISSN:1538-3881
DOI:10.3847/1538-3881/ad597a

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