Extended Data Fig. 4: Alternative balmer break fits to the spectra.
From: Spectroscopic confirmation of four metal-poor galaxies at z = 10.3–13.2
The fitted spectra if we force the observed spectral break to be interpreted as a Balmer break rather than a Lyman break. We see that the fits fail to reproduce the blue slopes red-ward of the spectral break, and in the cases of JADES-GS-z10-0 and JADES-GS-z11-0, flux in the fitted models blue-ward of the break is notably higher than the observed flux. Combined with the limits placed in Methods section 2 (and presented in Table 1), these fits show that the observed spectra are inconsistent with being Balmer breaks. The panels show the observed spectrum and 1σ standard error per pixel in red and light red respectively, and the median and 1σ range in fitted model spectra in blue.
