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Tracing Lyα and LyC Escape in Galaxies with Mg II Emission

  • Authors: Xinfeng Xu, Alaina Henry, Timothy Heckman, John Chisholm, Gábor Worseck, Max Gronke, Anne Jaskot, Stephan R. McCandliss, Sophia R. Flury, Mauro Giavalisco, Zhiyuan Ji, Ricardo O. Amorín, Danielle A. Berg, Sanchayeeta Borthakur, Nicolas Bouche, Cody Carr, Dawn K. Erb, Harry Ferguson, Thibault Garel, Matthew Hayes, Kirill Makan, Rui Marques-Chaves, Michael Rutkowski, Göran Östlin, Marc Rafelski, Alberto Saldana-Lopez, Claudia Scarlata, Daniel Schaerer, Maxime Trebitsch, Christy Tremonti, Anne Verhamme, Bingjie Wang

Xinfeng Xu et al 2022 The Astrophysical Journal 933 .

  • Provider: AAS Journals

Caption: Figure 7.

Physical structure of a photoionized cloud at the transition between H I and H II zones. Simulations are done using CLOUDY, and the adopted parameters are provided in Section 3.2.1. The position of the hydrogen Strömgren radius is indicated by the vertical black dashed line. The x-axis is the total hydrogen column density (N H). Top: comparison between N H and the ion population for certain elements in the y-axis, e.g., n(O III) = the number of O III ions/total oxygen ions in all states. The approximated regions for the two limiting cases of density and ionization bounds are indicated by the two arrows separately. Bottom: accumulated N ion for H I, O II, O III, and Mg II. For the curve of log(N(H I)), we scale it down by 4.0 dex to include it in the figure. The horizontal orange line represents N(H I) = 17.0 cm−2, where the cloud becomes optically thick to ionizing photons (see discussion in Section 3.2.1).

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