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JWST spectroscopy identifies two luminous galaxies at redshifts near 14

Carniani and collaborators used JWST/NIRSpec spectroscopy and NIRCam imaging to examine two early galaxy candidates. Both spectra show strong continuum breaks interpreted as Lyman-alpha breaks, yielding model-fitted redshifts near 14.32 and 13.90 in the first author preprint; the brighter object is spatially extended in the imaging. In a later ALMA follow-up, Schouws and colleagues detected a far-infrared oxygen line from the brighter source and obtained a more precise, consistent redshift.

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What is recorded here?

Carniani and collaborators used JWST/NIRSpec spectroscopy and NIRCam imaging to examine two early galaxy candidates. Both spectra show strong continuum breaks interpreted as Lyman-alpha breaks, yielding model-fitted redshifts near 14.32 and 13.90 in the first author preprint; the brighter object is spatially extended in the imaging. In a later ALMA follow-up, Schouws and colleagues detected a far-infrared oxygen line from the brighter source and obtained a more precise, consistent redshift.

Source-linked catalogue note. A detailed explanatory guide has not yet been prepared for this entry.

Scientific scope

The redshifts are fitted from the break shape with assumptions about neutral hydrogen absorption and possible emission. The 3.6-sigma candidate CIII] line for the brighter source was tentative in v1, not a secure line detection; a third target was not spectroscopically confirmed. A close foreground galaxy required contamination and lensing corrections. The inferred stellar mass, star-formation history and dust content depend on population and spectral models, and cosmological ages depend on adopted parameters. The first-preprint values and 2024-era comparison are not a claim of today’s distance record or a direct contradiction of cosmology. The separate ALMA paper reports an [O III] 88-micrometre line at 6.6 sigma and z = 14.1793 ± 0.0007, for JADES-GS-z14-0 only; its [O III] line is not the same as the earlier tentative 3.6-sigma C III] feature. The authors regard their consistency as supporting the earlier interpretation, but this does not by itself reproduce the earlier spectrum. Their dust continuum was not detected, and dust and metallicity inferences depend on temperature, lensing and emission models. The follow-up quotes two different uncertainties for the earlier tentative line (0.003 in its main text and 0.013 elsewhere); the prior source gives 0.013. Earlier and follow-up author groups are separately attributed.

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People and systems

Stefano Carniani; Kevin Hainline; Francesco D’Eugenio; Daniel J. Eisenstein; Peter Jakobsen; Joris Witstok; Benjamin D. Johnson; Jacopo Chevallard; Roberto Maiolino; Jakob M. Helton; Chris Willott; Brant Robertson; Stacey Alberts; Santiago Arribas; William M. Baker; Rachana Bhatawdekar; Kristan Boyett; Andrew J. Bunker; Alex J. Cameron; Phillip A. Cargile; Stéphane Charlot; Mirko Curti; Emma Curtis-Lake; Eiichi Egami; Giovanna Giardino; Kate Isaak; Zhiyuan Ji; Gareth C. Jones; Michael V. Maseda; Eleonora Parlanti; Tim Rawle; George Rieke; Marcia Rieke; Bruno Rodríguez Del Pino; Aayush Saxena; Jan Scholtz; Renske Smit; Fengwu Sun; Sandro Tacchella; Hannah Übler; Giacomo Venturi; Christina C. Williams; Christopher N. A. Willmer

These are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. An incomplete list is explicitly marked; same names are not automatically merged.

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English catalogue narrative

JWST spectroscopy identifies two luminous galaxies at redshifts near 14

Carniani and collaborators used JWST/NIRSpec spectroscopy and NIRCam imaging to examine two early galaxy candidates. Both spectra show strong continuum breaks interpreted as Lyman-alpha breaks, yielding model-fitted redshifts near 14.32 and 13.90 in the first author preprint; the brighter object is spatially extended in the imaging. In a later ALMA follow-up, Schouws and colleagues detected a far-infrared oxygen line from the brighter source and obtained a more precise, consistent redshift.

Scientific scope

The redshifts are fitted from the break shape with assumptions about neutral hydrogen absorption and possible emission. The 3.6-sigma candidate CIII] line for the brighter source was tentative in v1, not a secure line detection; a third target was not spectroscopically confirmed. A close foreground galaxy required contamination and lensing corrections. The inferred stellar mass, star-formation history and dust content depend on population and spectral models, and cosmological ages depend on adopted parameters. The first-preprint values and 2024-era comparison are not a claim of today’s distance record or a direct contradiction of cosmology. The separate ALMA paper reports an [O III] 88-micrometre line at 6.6 sigma and z = 14.1793 ± 0.0007, for JADES-GS-z14-0 only; its [O III] line is not the same as the earlier tentative 3.6-sigma C III] feature. The authors regard their consistency as supporting the earlier interpretation, but this does not by itself reproduce the earlier spectrum. Their dust continuum was not detected, and dust and metallicity inferences depend on temperature, lensing and emission models. The follow-up quotes two different uncertainties for the earlier tentative line (0.003 in its main text and 0.013 elsewhere); the prior source gives 0.013. Earlier and follow-up author groups are separately attributed.

Reading status

This is a source-linked WRS catalogue note. A full explanatory guide and independent scientific reconstruction have not been completed for this entry. Read the identified original work for its complete narrative and arguments.

People and systems

Stefano Carniani; Kevin Hainline; Francesco D’Eugenio; Daniel J. Eisenstein; Peter Jakobsen; Joris Witstok; Benjamin D. Johnson; Jacopo Chevallard; Roberto Maiolino; Jakob M. Helton; Chris Willott; Brant Robertson; Stacey Alberts; Santiago Arribas; William M. Baker; Rachana Bhatawdekar; Kristan Boyett; Andrew J. Bunker; Alex J. Cameron; Phillip A. Cargile; Stéphane Charlot; Mirko Curti; Emma Curtis-Lake; Eiichi Egami; Giovanna Giardino; Kate Isaak; Zhiyuan Ji; Gareth C. Jones; Michael V. Maseda; Eleonora Parlanti; Tim Rawle; George Rieke; Marcia Rieke; Bruno Rodríguez Del Pino; Aayush Saxena; Jan Scholtz; Renske Smit; Fengwu Sun; Sandro Tacchella; Hannah Übler; Giacomo Venturi; Christina C. Williams; Christopher N. A. Willmer

These are the listed authors of the cited contribution sources. Paper authorship does not quantify individual effort. An incomplete list is explicitly marked; same names are not automatically merged.

Original sources