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Small-scale Intensity Mapping: Extended Lyα, Hα, and Continuum Emission as a Probe of Halo Star Formation in High-redshift Galaxies

  • Authors: Lluís Mas-Ribas, Mark Dijkstra, Joseph F. Hennawi, Michele Trenti, Rieko Momose, and Masami Ouchi

2017 The Astrophysical Journal 841 19.

  • Provider: AAS Journals

Caption: Figure 4.

Left panel: radial UV surface brightness profiles with physical distance from the central galaxy for the fiducial (solid gray line) and the power-law (dashed line) models, reduced by a factor of three and two, respectively, to better fit the data. Magenta and cyan dots, line, and bars denote the data as in Figure 2. Right panel: predicted Lyα surface brightness profiles for the two models in the left panel assuming different population-averaged Lyα EW (rest frame). The profiles with ﹩\langle \mathrm{EW}\rangle \sim 80\,\mathring{\rm{A}} ﹩ correspond to the “best-fit” profiles in the left panel assuming the same escape fraction for Lyα and UV.

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