Same as Fig. 5, except at the wavelengths longward of, but adjacent to the NISP bands, which are used for refinements in α_ν (e.g., Fig. 2 and Sect. 5). The JWST counts are filter-transformed to either ground-based VISTA filters or Spitzer filters at the long near-IR wavelengths (S. Tompkins, R. Windhorst, private communication). HRK reconstruction is shown at the wavelengths of 2.2, 3.6, and 4.5 μm.