Electron density distribution in H ii regions in IC 10

• Verfasst von: Polles, Fiorella L. [VerfasserIn]
• Verfasst von: Fadda, Dario [VerfasserIn]
• Verfasst von: Vacca, William D. [VerfasserIn]
• Verfasst von: Abel, Nicholas P. [VerfasserIn]
• Verfasst von: Chevance, Mélanie [VerfasserIn]
• Verfasst von: Fischer, Christian [VerfasserIn]
• Verfasst von: Jackson, James M. [VerfasserIn]
• Verfasst von: Lebouteiller, Vianney [VerfasserIn]
• Verfasst von: Madden, Suzanne [VerfasserIn]
• Verfasst von: Ramambason, Lise [VerfasserIn]
• Titel: Electron density distribution in H ii regions in IC 10
• Verf.angabe: 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
• E-Jahr: 2024
• Jahr: 2024 September
• Umfang: 15 S.
• Illustrationen: Illustrationen
• Fussnoten: Online veröffentlicht am 13. August 2024 ; Gesehen am 26.05.2025
• Titel Quelle: Enthalten in: The astronomical journal
• Ort Quelle: Washington, DC : AAS Publishing, American Astronomical Society, 1998
• Jahr Quelle: 2024
• Band/Heft Quelle: 168(2024), 3 vom: Sept., Artikel-ID 117, Seite 1-15
• ISSN Quelle: 1538-3881
• DOI: doi:10.3847/1538-3881/ad597a
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1926591445

Abstract

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.