Little is known about the mass-metallicity relation in galaxies at cosmic dawn, z = 5 − 15. This paper uses the FirstLight database of cosmological simulations to predict the mass-metallicity relation at z = 5 − 8. There is weak evolution of the metallicity with redshift at a fixed stellar mass. This is mostly driven by the weak evolution of the gas fraction at these high redshifts. Emission lines ratios, such as [OIII]λ5007/Hβ, are relatively good tracers of metallicity and stellar mass with an abrupt decrease of the line luminosities at low metallicities and low masses driven by the low metal abundances at these early times.

Context. Determining when the first galaxies formed remains an outstanding goal of modern observational astronomy. Theory and current stellar population models imply that the first galaxies formed at least at z = 14 − 15. But to date, only one galaxy at z > 13 (GS-z13-0) has been spectroscopically confirmed. Aims. The galaxy ‘HD1’ was recently proposed to be a z ∼ 13.27 galaxy based on its potential Lyman break and tentative [O III] 88 μm detection with ALMA. We hereby aim to test this scenario with new ALMA Band 4 observations of what would be the [C II] 158 μm emission if HD1 is at z ∼ 13.27. Methods. We carefully analyse the new ALMA Band 4 observations and re-analyse the existing ALMA Band 6 data on the source to determine the proposed redshift. Results. We find a tentative 4σ feature in the Band 4 data that is spatially offset by 1.​​″7 and spectrally offset by 190 km s−1 from the previously reported 3.8σ ‘[O III] 88 μm’ feature. Through various statistical tests, we demonstrate that these tentative features are fully consistent with both being random noise features. Conclusions. We conclude that we are more likely to be recovering noise features than both [O III] 88 μm and [C II] 158 μm emission from a source at z ∼ 13.27. Although we find no credible evidence of a z ∼ 13.27 galaxy, we cannot entirely rule out this scenario. Non-detections are also possible for a z ∼ 13 source with a low interstellar gas-phase metallicity or ionisation parameter and/or high gas density. Moreover, the new continuum and line upper limits provide no strong evidence for or against a lower-redshift scenario. Determining where and exactly what type of galaxy HD1 is, will now likely require JWST/NIRSpec spectroscopy.

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