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Caption: Figure 9.
NIRCam galaxy counts in the JWIDF and the El Gordo noncluster module (orange and brown filled circles, respectively). Each row of three panels shows one wavelength as indicated in the panels. (a) (Left panels): differential galaxy counts in 0.5 mag bins. Open diamonds show a combination of previous ground-based, HST, and Spitzer/WISE counts (Driver et al. 2016a; Koushan et al. 2021) with different surveys shown in different colors as indicated in the legends. The green lines represent the hierarchical-model predictions for the 0.9–4.5 μm galaxy counts of Yung et al. (2022). When broadband filters in different instruments are similar but not identical, small corrections for effective wavelength differences may be needed (Robotham et al. 2020; Koushan et al. 2021, see Appendix B.2 here). (b) (Middle panels): energy counts after dividing the left panels by a 0.40 dex mag−1 slope. Units used are described in Section 4 and Koushan et al. (2021). Triangles without error bars indicate bins having only a single object. The brightest bins of the PEARLS counts at 18 ≲ AB ≲ 20 mag show cosmic variance (Sections 2 and 4.5), but do not weigh into the IGL fits, which at these flux levels are dominated by the faint end of the brighter surveys. PEARLS counts beyond the respective 80% completeness limits (as derived in Table 1 from a best-fit power-law extrapolation) are plotted as lightly shaded points, and are not included in the spline extrapolations to estimate the total IGL. (c) (Right panels): integral of the middle panels normalized to 100% of the IGL energy received.
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© 2022. The Author(s). Published by the American Astronomical Society.
