We report the first successful ALMA followup observations of a secure z gt 10 JWSTselected galaxy by robustly detecting 6.6sigma the OIII88mu m line in JADESGSz140 hereafter GSz14. The ALMA detection yields a spectroscopic redshift of z14.1793pm0.0007 and increases the precision on the prior redshift measurement of z14.320.200.08 from NIRSpec by gtrsim180times. Moreover the redshift is consistent with that previously determined from a tentative detection 3.6sigma of CIII19071909 z14.178pm0.013 solidifying the redshift determination via multiple line detections. We measure a line luminosity of LmathrmOIII88  2.1 pm 0.5times108Lodot placing GSz14 at the lower end but within the scatter of the local LmathrmOIII88star formation rate relation. No dust continuum from GSz14 is detected suggesting an upper limit on the dusttostellar mass ratio of lt 2 times 103 consistent with dust production from supernovae with a yield yd lt 0.3Modot. Combining a previous JWSTMIRI photometric measurement of the OIIIlambdalambda49595007mathrmmathringA and Hbeta lines with Cloudy models we find GSz14 to be surprisingly metalenriched Zsim0.05  0.2Zodot a mere 300mathrmMyr after the Big Bang. The detection of a bright oxygen line in GSz14 thus reinforces the notion that galaxies in the early Universe undergo rapid evolution.
['Astrophysics - Astrophysics of Galaxies']
Detection of OIII88mum in JADESGSz140 at z14.1793
{'Detection of [OIII] 88 µm in JADES-GS-z14-0 at z=14.1793': "Sander Schouws, 1 Rychard J. Bouwens, 1 Katherine Ormerod, 2 Renske Smit, 2 Hiddo Algera, 3, 4 Laura Sommovigo, 5 Jacqueline Hodge, 1 Andrea Ferrara, 6 Pascal A. Oesch, 7, 8, 9 Lucie E. Rowland, 1 Ivana van Leeuwen, 1 Mauro Stefanon, 1 Thomas Herard-Demanche, 1 Yoshinobu Fudamoto, 10 Huub Rottgering, 1 and Paul van der Werf 1  \n1 Leiden Observatory, Leiden University, NL-2300 RA Leiden, Netherlands  \n2 Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, United Kingdom 3 Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan 4 National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo, Japan  \n5 Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA  \n6 Scuola Normale Superiore, Piazza dei Cavalieri 7, 50126 Pisa, Italy  \n7 Departement d'Astronomie, Universit'e de Gen'eeve, 51 Ch. des Maillettes, CH-1290 Versoix, Switzerland  \n8 Cosmic Dawn Center (DAWN), Copenhagen, Denmark  \n9 Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200 Copenhagen N, Denmark  \n10 Center for Frontier Science, Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522, Japan", 'ABSTRACT': 'We report the first successful ALMA follow-up observations of a secure z > 10 JWST-selected galaxy, by robustly detecting (6 . 6 σ ) the [OIII] 88 µm line in JADES-GS-z14-0 (hereafter GS-z14). The ALMA detection yields a spectroscopic redshift of z = 14 . 1793 ± 0 . 0007, and increases the precision on the prior redshift measurement of z = 14 . 32 +0 . 08 -0 . 20 from NIRSpec by ≳ 180 × . Moreover, the redshift is consistent with that previously determined from a tentative detection (3 . 6 σ ) of CIII] 1907 , 1909 ( z = 14 . 178 ± 0 . 013), solidifying the redshift determination via multiple line detections. We measure a line luminosity of L [OIII]88 = (2 . 1 ± 0 . 5) × 10 8 L ⊙ , placing GS-z14 at the lower end, but within the scatter of, the local L [OIII]88 -star formation rate relation. No dust continuum from GS-z14 is detected, suggesting an upper limit on the dust-to-stellar mass ratio of < 2 × 10 -3 , consistent with dust production from supernovae with a yield y d < 0 . 3 M ⊙ . Combining a previous JWST/MIRI photometric measurement of the [OIII] λλ 4959,5007 ˚ A and H β lines with Cloudy models, we find GS-z14 to be surprisingly metal-enriched ( Z ∼ 0 . 05 -0 . 2 Z ⊙ ) a mere 300 Myr after the Big Bang. The detection of a bright oxygen line in GS-z14 thus reinforces the notion that galaxies in the early Universe undergo rapid evolution.', '1. INTRODUCTION': 'The discovery and spectroscopic confirmation of galaxies at z > 10 has recently become possible due to the groundbreaking capabilities offered by the James Webb Space Telescope ( JWST ) (e.g. Curtis-Lake et al. 2023; Robertson et al. 2023; Bunker et al. 2023; Carniani et al. 2024; Finkelstein et al. 2024; Zavala et al. 2024). In particular JADES-GS-z14-0 (hereafter GS-z14) was recently spectroscopically confirmed to be the most distant known galaxy at z spec = 14 . 32 +0 . 08 -0 . 20 , less than 300 Myr after the Big Bang (Carniani et al. 2024). Notably GS-z14 is also very luminous with M UV = -20 . 81 ± 0 . 16, which makes it the second most luminous z > 8 galaxy with a spectroscopic redshift; only GN-z11 (Oesch et al. 2016; Bunker et al. 2023) is more luminous by a factor ∼ 2 × .  \nMoreover, in contrast to other z > 10 galaxies, the rest-frame UV morphology of GS-z14 is extended and not highly concentrated. This implies that the luminosity is dominated by a spatially extended stellar population as opposed to an active galactic nucleus (AGN). The existence of objects like GS-z14 suggests a much more rapid build-up of galaxies in the very early universe than previously expected (Carniani et al. 2024). GS-z14 enables a unique opportunity to study this rapid build-up in detail (Ferrara 2024).  \nThe high luminosity of GS-z14 makes it an exceptional target for multi-wavelength follow-up observations capable of revealing its physical conditions. Here we present new observations of GS-z14 targeting the luminous [OIII] 88 µm far-infrared line with the the Atacama Large Millimeter/submillimeter Array (ALMA).  \nThe [OIII] 88-micron fine-structure line is one of the dominant coolants of the ISM. It originates from ionized gas in HII regions (Cormier et al. 2015), where ionizing radiation from young, massive stars has stripped electrons from oxygen atoms. Both semi-analytical models (Yang & Lidz 2020; Vallini et al. 2021, 2024) and radiative transfer post-processed large box (Moriwaki et al. 2018), cosmological zoom-in (Katz et al. 2017; Arata et al. 2020; Katz et al. 2022; Pallottini et al. 2022; Kohandel et al. 2023; Nakazato et al. 2023) hydrodynamical simulations have been employed to predict and interpret [OIII] 88 µm emission in high redshift sources. The consensus is that bright [OIII] 88 µm emission is generally associated with hard ionisation fields (Yang & Lidz 2020; Pallottini et al. 2022), high ionization parameters (Moriwaki et al. 2018; Arata et al. 2020; Vallini et al. 2024; Nakazato et al. 2023), and low metallicities (Katz et al. 2019; Vallini et al. 2024). These physical properties are likely to be ubiquitous in very actively star-forming galaxies at high redshifts, making this line the ideal target for ALMA follow-up observations of JWST-selected z > 10 galaxies.  \nIn the last two years, ALMA follow-up observations have been performed for several high-redshift galaxy candidates. GHZ2 (Castellano et al. 2022; Naidu et al. 2022; Donnan et al. 2022; Harikane et al. 2023; Bouwens et al. 2023), with a photometric redshift of z = 11 . 96 -12 . 42, was targeted with an ALMA Band 6 search for [OIII] 88 µm by Bakx et al. (2023), who determined a 5 σ upper limit of log( L [OIII] /L ⊙ ) < 1 . 7 × 10 8 (see also Popping 2023). GHZ2 was later spectroscopically confirmed at z = 12 . 34 (Castellano et al. 2024), with Zavala et al. (2024) estimating an SFR of 9 ± 3 M ⊙ yr -1 from the H α line. Following its spectroscopic confirmation, Zavala et al. (2024) re-examined the ALMA observations of GHZ2 presented in Bakx et al. (2023), but were not able to identify a plausible > 5 σ [OIII] 88 µm detection at the expected frequency.  \nAn ALMA line scan was also performed on GHZ1, with a photometric redshift of z ≈ 10 . 6 (Treu et al. 2023), SFR of 36 . 3 +54 . 5 -26 . 8 M ⊙ yr -1 and stellar mass log( M ⋆ /M ⊙ ) = 9 . 1 +0 . 3 -0 . 4 (Santini et al. 2023), yielding a marginal [OIII] 88 µm signal near its JWST position (Yoon et al. 2023) and an upper limit of L [OIII] < 2 . 2 × 10 8 L ⊙ . Another high-redshift candidate, HD1 at z = 13 . 3 (Harikane et al. 2023) was observed in ALMA Bands 4 and 6 targeting [CII] 158 µm and [OIII] 88 µm , respectively, but the lines were not detected (Kaasinen et al. 2023). HD1 was later shown to be a low-redshift interloper at z = 4 . 0 (Harikane et al. 2024). Finally, S5z17-1, identified in JWST ERO data, showed a potential 5.1 σ detection at 338.726 GHz, possibly corresponding  \nto [OIII] 52 µm at z = 16 (Fujimoto et al. 2023), suggesting an SFR < 120 M ⊙ yr -1 . However, the high-redshift nature of this galaxy has not been conclusively established.  \nOverall, these upper limits and non-detections indicate possible lower redshift solutions or insufficient sensitivity in the requested observations (Bakx et al. 2023; Furlanetto & Mirocha 2023; Kaasinen et al. 2023). However, the burstiness of SF in such high-redshift galaxies, as well as the impact of feedback processes on galaxy spectra and visibility, have also been suggested as physical motivations for the lack of ALMA detections at z > 10 (Nakazato et al. 2023; Kohandel et al. 2023).  \nThroughout this paper we assume a standard ΛCDM cosmology with H 0 = 70 km s -1 Mpc -1 , Ω m = 0 . 3 and Ω Λ = 0 . 7. Magnitudes are presented in the AB system (Oke & Gunn 1983). For star formation rates and stellar masses we adopt a Chabrier IMF (Chabrier 2003). Error-bars indicate the 68% confidence interval unless specified otherwise. All measured and derived physical quantities are corrected for gravitational lensing by a factor of 1.17 × (Carniani et al. 2024). Logarithms use base 10 unless specified otherwise.', '2.1. JWST': "GS-z14 was discovered in deep imaging of the GOODS-South field obtained by the JWST Advanced Deep Extragalactic Survey (JADES; Eisenstein et al. 2023a) and the First Reionization Epoch Spectroscopic COmplete Survey (FRESCO; Oesch et al. 2023). GSz14 was initially flagged as a likely low redshift interloper (Hainline et al. 2024; Williams et al. 2024) due to a nearby foreground galaxy at z = 3 . 475 with a separation of only 0.4' and due to its high luminosity. However, further analysis including additional medium-band observations favored a high redshift solution (Robertson et al. 2023).  \nDeep follow-up spectroscopy with NIRSpec presented in Carniani et al. (2024) shows a strong break at ∼ 1.85 µ m, consistent with a Lyman break at z ∼ 14. The profile of the Lyman break is sensitive to absorption of hydrogen along the line of sight, neutral gas in the galaxy and environment, velocity offsets, the presence of Lyman alpha emission and possible ionized bubbles. Accounting for these effects, Carniani et al. (2024) determined a spectroscopic redshift of z = 14.32 +0 . 08 -0 . 20 .  \nIn contrast to other z > 10 sources, the spectrum of GS-z14 does not contain strong rest-frame UV emission lines. Only CIII] λλ 1907,9 ˚ A is tentatively detected with a significance of 3.6 σ at z = 14 . 178 ± 0 . 013, consistent with the redshift obtained from the Lyman Break. Car-  \nFigure 1. Left Panel: The ALMA observations cover 98% of the redshift probability distribution derived from the Lyman break as observed by NIRSpec PRISM. We use two tunings with three spectral windows each, tuning 1 and 2 cover 83% and 15% of the probability distribution respectively. Right Panel: Flux constraints extracted at the position of GS-z14 ( blue histogram ) vs. frequency from the 2023.A.00037.S spectral scan observations. The grey contours indicate the 1 σ uncertainties. For context we show the expected redshift from the tentative CIII] 1907 , 1909 line from NIRSpec as well as the 5, 16, 50, 86 and 95th percentiles of the P(z) distribution. There is only one feature in the line scan that can be confidently identified as [OIII] 88 µm line emission and it occurs at a frequency of 223.528 ± 0.009 GHz.  \n<!-- image -->  \net al. (2024) discuss a number of mechanisms that could be responsible for the lack of strong emission lines in the rest-frame UV, ranging from a sudden quenching of the star formation, very low or high metallicities (Z < 0.05Z ⊙ or Z ∼ Z ⊙ ), a high escape fraction of ionizing photons and a difference in the dominant ionizing flux.  \nInterestingly, GS-z14 is also detected by MIRI in the F770W filter (Helton et al. 2024). This filter covers the rest-frame optical emission of GS-z14, corresponding to wavelengths of 4.4 to 5.7 µ m. This part of the spectrum contains the strong [OIII] λλ 4959,5007 ˚ A and H β emission lines, and indeed the observed flux is significantly stronger than observed in the adjacent F444W filter, implying a significant contribution from the emission lines (constituting about 1 / 3 of the total F770W flux).  \nSED fitting of GS-z14 performed by Helton et al. (2024) shows that the photometry is consistent with a stellar mass of log(M ∗ /M ⊙ )=8 . 7 +0 . 5 -0 . 4 . The models estimate that most of this stellar mass was formed relatively recently, with a mass-weighted age of ∼ 20 Myr. Helton et al. (2024) determine the current ( < 10 Myr) star formation rate of GS-z14 to be 25 +6 -5 M ⊙ yr -1 -consistent with the measurement of 22 ± 6 M ⊙ yr -1 from Carniani et al. (2024). Combined with the measured size of 260 ± 20 pc, this implies a high star formation rate surface density of ∼ 64 M ⊙ yr -1 pc -2 , comparable to intense starbursting galaxies in the local universe (Genzel et al. 2010). The UV slope β UV = -2 . 20 ± 0 . 07 indicates the presence of a moderate amount of dust in addition to the very young stellar population, with a visual extinction of A V =0.31 +0 . 14 -0 . 07 (Carniani et al. 2024). Finally, the metallicity is poorly constrained owing to a lack of detected emission lines but is expected to be low (Z = 0.014 +0 . 052 -0 . 012 Z ⊙ ; Carniani et al. 2024).", '2.2. ALMA': "The ALMA Band 6 follow-up observations targeting the [OIII] 88 µm line were obtained as part of a Cycle 10 Director's Discretionary Time (DDT) program (#2023.A.00037.S, PI: Schouws). An observing set-up using two tunings with three spectral windows each was utilized to maximize the coverage of the redshift likelihood distribution derived from the spectroscopic Lyman break. This results in a continuous frequency coverage ranging from 218.70 GHZ to 229.45 GHz, corresponding to a redshift range of z = 13 . 79 to 14.51. We show in Figure 1 that the observing strategy covers 98% of the P(z).  \nThe observations for Tuning 2 were carried out between 15 and 16 August 2024 in good weather conditions (PWV=0.67mm), achieving the requested sensitivity in 2.8 hours. Tuning 1 was observed between 7 and 8 September 2024 for 2.8 hours in excellent conditions (PWV=0.30mm). Both tunings were observed with different array configurations due to scheduling constraints. Tuning 1 was observed in C-4 and Tuning 2 in C-5, with baselines of 15 -500 and 15 -919 m, respectively.  \nThe ALMA data were reduced and calibrated following the standard ALMA pipeline procedures with the Common Astronomy Software Applications (v6.5.4-9) ( Casa; Hunter et al. 2023). The resulting calibrated measurement sets were time-averaged in bins of 30 seconds to reduce the data-size, after carefully verifying that time-average smearing does not impact our results (e.g. Thompson et al. 2017).  \nImaging of the calibrated visibilities was performed with natural weighting using the tclean task in Casa , cleaning to a depth of 2 σ using automasking (Kepley et al. 2020). We use a pixel scale of 0.076 '' to properly  \nsample the synthesized beam, which has a FWHM of 1 . 08 '' × 0 . 80 '' at the frequency of the [OIII] 88 µm line.", '2.3. Line Search': "We perform a blind search for emission lines using an algorithm similar to the one used by B'ethermin et al. (2020) for the ALPINE survey and Schouws et al. in prep. for the REBELS survey. The algorithm loops over all channels and collapses moment maps over a range of 75 to 350 km s -1 in steps of 1 channel ( ∼ 10 km s -1 ). For each moment map, we identify the significant ( > 3 σ ) peaks and add the results to a large list of features. This list is then pruned by removing duplicates within 2 × FWHM and 1.5 × the beamsize. We also perform the search on the negative moment map, which is useful to characterize the noise properties. In Figure 1, we show a blind extraction of the ALMA spectrum at the location of GS-z14 using a 0.5' aperture.  \nThe most significant line candidate we extract within a 0.5' radius of the JWST position of GS-z14 is detected with a peak significance of 6.6 σ and separation of 0.12'. The candidate line is consistent with being spatially coincident with GS-z14 in the JWST/NIRCam observations given expected 0.18' positional uncertainties following from a 6.6 σ line detection and 1.08' beam. 1", '3.1. [OIII] 88 µm in GS-z14': "We have identified an emission line with a signal-tonoise of 6 . 6 σ within 0 . 12 '' of GS-z14 at 223.528 ± 0.009 GHz. This corresponds to [OIII] 88 µm at z = 14 . 1793 ± 0 . 0007, consistent with both the redshift derived from the Lyman break observed by JWST and also the tentative 3.6 σ detection of CIII] 1907 , 1909 at 2.89 µ m (Carniani et al. 2024). In particular, the consistency of our new redshift determination from [OIII] 88 µm with the earlier redshift estimate z = 14 . 178 ± 0 . 003 from the tentative CIII] 1907 , 1909 doublet (Carniani et al. 2024) greatly increases our confidence in the robustness of the current redshift determination given the availability of multiple line detections. We show the contours of the [OIII] 88 µm emission overlaid on the JWST F200W imaging and a S/N-optimized extraction of the spectrum in Figure 2.  \nWemeasure the integrated line flux using the momentzero map of the emission line, including all channels that fall within 2 × the FWHM of the line. The FWHM is determined in an iterative process; starting from an estimate of the FWHM we collapse a moment-zero map and extract a 1d spectrum, which is extracted by includ-  \nng all pixels with S/N > 3 σ on the moment-zero map. A new FWHM is then measured using this 1d spectrum by fitting a Gaussian. This new FWHM is then used to collapse a new moment-zero map for the next iteration. A stable FWHM is achieved in less than 10 steps (Schouws et al. 2022).  \nThe final FWHM we measure is 136 ± 31 km s -1 . Assuming that GS-z14 is dispersion-dominated and r [OIII] = r e = 260 pc, this implies a dynamical mass of (1.0 ± 0.5) × 10 9 M ⊙ (sin i ) 2 . At the current resolution we do not see evidence for a velocity gradient.  \nWe measure an integrated flux of 39 ± 10 Jy · km s -1 this corresponds to a [OIII] 88 µm luminosity of (2 . 1 ± 0 . 5) × 10 8 L ⊙ (Solomon et al. 1992) (after correction for lensing magnification; Carniani et al. 2024). This places GS-z14 a factor of ∼ 2 × below the local relation between L [OIII] and SFR for metal-poor dwarf galaxies from De Looze et al. (2014), albeit nearly within the scatter (Figure 3). The general consistency with the z = 0 relation for a galaxy a mere ∼ 300 Myr after the Big Bang suggests that GS-z14 has undergone rapid evolution, as discussed in detail in Section 4.1.", '3.2. Dust Continuum': 'We do not detect the dust continuum from GSz14, with a formal 90 µ m continuum limit of < 15 . 1 µ Jy beam -1 (3 σ ). We provide an upper limit on its dust mass given an assumed dust temperature of T d = 60K. This temperature is consistent with extrapolations from theoretical models (e.g., Liang et al. 2019; Sommovigo et al. 2022a) and observational trends (e.g., Schreiber et al. 2018; Witstok et al. 2023a) to z ≈ 14. Moreover, we follow Ferrara et al. (2024) by adopting the Weingartner & Draine (2001) dust model with κ 88 = 34 . 15 cm -2 g -1 at rest-frame 88 µ m and β IR = 2 . 03. This yields a (lensing-corrected) upper limit on the dust mass and infrared luminosity of log( M d /M ⊙ ) < 6 . 0 and log( L IR /L ⊙ ) < 11 . 1, respectively. The latter corresponds to an obscured SFR of SFR IR < 14 M ⊙ yr -1 which, combined with the unobscured SFR of GS-z14 inferred by Carniani et al. (2024), implies an obscured fraction of f obs < 0 . 66. Finally, using the stellar mass of GS-z14 inferred by Helton et al. (2024), we infer a dust-to-stellar mass ratio ξ d ≡ M d /M ⋆ < 2 . 4 × 10 -3 .  \nWhile the above estimates require the assumption of a dust temperature for GS-z14, we note that a lower (higher) temperature of T d = 50K ( T d = 80K) has < 0.4 dex impact on the estimated upper limit for the dust mass. In Section 4.2, we discuss this in further detail, focusing on the Attenuation Free Model by Ferrara et al. (2024) which self-consistently predicts a dust temperature for GS-z14 based on the observed V-band attenuation and the spatial extent of the dust.  \nFigure 3. The luminosity of [OIII] 88 µm in GS-z14 is consistent with the local relation for metal-poor dwarf galaxies found by De Looze et al. (2014). For context we also show the local relation for starburst galaxies (De Looze et al. 2014) as well as a compilation of z > 6 . 5 galaxies (Bakx et al. 2020; Carniani et al. 2020; Harikane et al. 2020; Akins et al. 2022; Witstok et al. 2022; Algera et al. 2024; Fujimoto et al. 2024). Even as early as z = 14 . 1793 ± 0 . 0007 and for high redshift galaxies in general, the relation for metal-poor dwarf galaxies seems to be a good fit (at SFR ≲ 100 M ⊙ yr -1 ).  \n<!-- image -->  \nFigure 2. Detection of [OIII] 88 µm in GS-z14 at z = 14 . 1793 ± 0 . 0007. Left Panel: Contours showing the [OIII] 88 µm emission (2, 3, 4 and 5 σ ) overlaid on the F200W imaging (Eisenstein et al. 2023a,b). The [OIII] 88 µm emission is detected at a peak significance of 6.6 σ in the collapsed data-cube. Right Panel: The spectrum of the [OIII] 88 µm line ( blue histogram ) extracted from the > 3 σ emission region in the moment-0 map. The red line shows the Gaussian fit used to measure the spectroscopic redshift and FWHM of the line. The grey shaded region indicates the 1 σ uncertainties.  \n<!-- image -->', '4.1. Constraints on the ISM of GS-z14': 'Luminosity ratios of emission lines are invaluable diagnostic tools to probe the conditions of the ISM in galaxies. Although the NIRSpec spectroscopy of GS-z14 does not show significant emission lines, its detection in the MIRI F770W band places a constraint on the combined [OIII] λλ 4959,5007 ˚ A+H β flux. Following Helton et al. (2024) we assume that the flux excess in F770W is 27.5 ± 5.6 nJy based on a flat underlying continuum emission.  \nThe [OIII] λ 5007 ˚ A luminosity (hereafter [OIII]) can subsequently be calculated based on an assumed [OIII]/H β ratio and be compared to the luminosity of OIII as measured by ALMA. We repeat this calculation 10 6 × , drawing random [OIII]/H β ratios from probability distribution from the SED fitting by Helton et al. (2024), where we combine the probability distributions from the three star formation history assumptions. In this process we also account for the uncertainty in the line luminosities from ALMA and JWST by drawing random values from a Gaussian error distribution.  \nThe resulting constraints on the [OIII]/[OIII] 88 µm versus [OIII]/H β line ratios are shown in Figure 4. For context we show a grid of ISM models for a large range of conditions based on Cloudy models (Ferland et al. 2017). The models consist of an HII region that smoothly transitions to a Photo Dissociation Region (PDR) until a fixed optical depth (A V =10) in a plane parallel geometry. For more details on the model we re-  \n<!-- image -->  \n/circledot  \nm  \nµ  \nI]88  \nI  \n[OI  \n/  \n˚  \nA  \nI]5007  \nI  \n[OI  \nlog  \n2  \n.  \n0  \n1  \n.  \n5  \n1  \n.  \n0  \n0  \n.  \n5  \n0  \n.  \n0  \nlog N=3.5  \nlog N=3.0  \nlog N=2.0  \nlog N=0.5  \nlog(U)=  \n-  \nFigure 4. The ALMA and MIRI observations constrain the emission line ratios of GS-z14 to the dark shaded region in the figure highlighted by the 1 and 2 σ contours. ISM modeling as shown by the coloured grid highlights the dependence on metallicity and density. This indicates that GS-z14 is consistent with a relatively high metallicity (Z > 0.1 Z ⊙ ) and moderate to low density log(N) < 3 . 0cm -3 . There is a further minor dependence on the ionization parameter that shifts and deforms the grid, but does not impact the conclusions. For context, SED fitting of GS-z14 finds log( U ) = -2 . 5 ± 0 . 5 (Helton et al. 2024).  \n<!-- image -->  \n-  \n3.0  \n-  \n0  \n.  \n5  \n0  \n.  \n0  \n0  \n.  \n5  \n1  \n.  \n0  \nlog [OIII]5007  \n˚  \nA  \n/ H  \nβ  \nfer to Witstok et al. (2022). We note that the ionization parameter of GS-z14 has been loosely constrained by Helton et al. (2024) to be log( U ion ) = -2 . 5 ± 0 . 5, and we therefore show two sets of Cloudy models bracketing this range, at a fixed log( U ion ) ∈ ( -3 . 0 , -2 . 0). We focus on the grid with an ionization parameter log( U ion ) = -2, as Kohandel et al. (2023) predict the most [OIII] 88 µm -luminous galaxies at z ≳ 10 have high ionization parameters.  \nWhile the uncertainties are substantial, given the existence of only a photometric detection of the [OIII] λλ 4959,5007 ˚ A line, the Witstok et al. (2022) models suggest a relatively high metallicity of Z ∼ 0 . 1 Z ⊙ , in combination with a moderate-to-low electron density (log N ≲ 10 2 . 5 ). This is on the low end of, albeit still consistent with, the distribution of electron densities found for z ≳ 5 galaxies, which typically show values of log( N ) ∼ 2 -3 (e.g., Isobe et al. 2023). However, for more accurate constraints on the ISM conditions of GSz14, direct spectroscopic detections of additional oxygen lines are crucial, for example through MIRI spectroscopy.  \nIntriguingly, the detection of [OIII] 88 µm at z = 14 . 1793 ± 0 . 0007 is consistent within 1 σ with the tentative detection of CIII] λλ 1907,9 ˚ A reported by Carniani et al. (2024) at z = 14 . 178 ± 0 . 013. Carniani et al. (2024) derive a CIII] λλ 1907,9 ˚ A rest-frame equivalent width (EW 0 ) of 8.0 ± 2.3 ˚ A, which is relatively high com-  \nEW 0 ([OIII]+H β ) of 370 +360 -130 ˚ A estimated by Helton et al. (2024), albeit consistent with the distribution found for galaxies at z ∼ 0 -4 (e.g. Maseda et al. 2017; Ravindranath et al. 2020; Tang et al. 2021), see Figure 5. The measured equivalent widths are in agreement with predictions from Cloudy at a metallicity of Z ∼ 0 . 05 -0 . 2 Z ⊙ , and with an ionization parameter of log( U ) ∼ -2 . 5, in agreement with Helton et al. (2024).  \nMoreover, Jones et al. (2020) derive a calibration for the oxygen abundance using the [OIII] 88 µm line and star-formation rate. Using their calibration we derive 12 + log O ++ / H + =7.66 +0 . 19 -0 . 21 ( ∼ 6-14% solar metallicity, using the solar abundance from Asplund et al. (2009)). In Figure 6 we use a Cloudy grid with a 1Myr old input stellar population to estimate the [OIII] 88 µm /SFR ratio as a function of ionisation parameter, for models with different metallicity and gas density. For modest gas density the measurements are consistent with 10% solar oxygen abundance, however, higher gas densities or older ages for the input stellar population will give higher metallicity estimates (up to solar metallicity).  \nThe detection of both carbon and oxygen lines thus reinforce the notion that GS-z14 is already moderately chemically enriched. Adopting a fiducial Z ∼ 0 . 05 -0 . 2 Z ⊙ in combination with the stellar mass from Helton et al. (2024), GS-z14 falls onto the high-redshift massmetallicity relation, which has been mapped out to z ∼  \n1  \n.  \n0  \nσ  \n3  \nσ  \n1  \nσ  \n2  \n/circledot  \n10, and appears to show only mild evolution beyond z ≳ 3 (e.g., Curti et al. 2024).  \n1 Figure 5. The rest-frame equivalent width of CIII] λλ 1907,9 ˚ A as a function of EW 0 ([OIII]+H β ) (Carniani et al. 2024; Helton et al. 2024). GS-z14-0 is broadly consistent with measurements from the literature at z = 1 -3 (grey, purple and orange points; Maseda et al. 2017; Ravindranath et al. 2020; Tang et al. 2021).  \n<!-- image -->  \n0  \n1 Figure 6. Cloudy modelling of the [OIII] 88 µm /SFR as a function of ionisation parameter for a range of metallicities and densities ∼ 50-100 cm -3 . Our model gives a lower limit on the metallicity of ∼ 10% Z ⊙ , with higher gas densities and older ages preferring higher metallicity estimates.  \n<!-- image -->', '4.2. Constraints on Dust Formation Processes': 'The build-up of dust in galaxies is a complex process involving multiple mechanisms of dust production and destruction, operating on different timescales.  \nSupernova explosions (SNe) produce dust quickly, on timescales similar to the lifecycle of massive stars ( ∼ 10 Myr), whilst Asymptotic Giant Branch (AGB) stars contribute to dust production on significantly longer timescales ( ∼ 300 Myr, Schneider & Maiolino 2024). The contribution from grain growth in the ISM depends on the physical conditions, but is expected to be subdominant at extremely high redshifts and low gas-phase metallicities (Ferrara et al. 2016; Dayal et al. 2022; Witstok et al. 2023a; Markov et al. 2024).  \nAt lower redshifts it is difficult to disentangle the impact of different contributions (e.g., De Looze et al. 2020; Galliano et al. 2021), but GS-z14 has formed sufficiently early in cosmic history that dust production through SNe is likely the dominant formation process. This makes GS-z14 an ideal test-bed for dust formation models in the early universe.  \nThe efficiency of dust production from SNe can be inferred by measuring the dust-to-stellar mass ratio ( ξ d ). This parameter is hard to interpret as it depends on both the expected number of SNe per unit of formed stellar mass ( ν ), which in turn depends on the assumed Initial Mass Function (IMF), and on the net dust yield per SN event ( y d ), ξ d = y d × ν . In local SN remnants y d values varying in the wide range from 0.01 to 1.1 M ⊙ have been directly measured (Milisavljevic et al. 2024). Such values are broadly in agreement with most indirect high-z measurements based on dust-to-stellar mass ratios (Sommovigo et al. 2022a,b).  \nUtilizing the continuum non-detection of GS-z14, we can attempt to place an upper limit on y d . Following Michaglyph[suppress]lowski (2015) and adopting a Salpeter IMF, the limit of ξ d < 2 × 10 -3 suggests a yield of y d < 0 . 3 M ⊙ / SN. This is consistent with a commonly adopted yield of y d ∼ 0 . 1/SN (e.g., Sommovigo et al. 2022a; Dayal et al. 2022). If we rely on such a value for y d ∼ 0 . 1/SN and assume that dust follows a similar spatial distribution as the stellar component, GS-z14 should be largely obscured (A V ∼ 9.5, see also Ferrara et al. 2024) and would not have been detected with JWST. However, the JWST data only reveal a relatively low visual extinction of A V =0.31, implying a much (1 dex) lower dust mass of 5 × 10 4 M ⊙ and ξ d < 10 -4 (Ferrara et al. 2024).  \nClearly, SNe (and later on growth in the ISM) do produce tangible amounts of dust, as less than 500 Myr later, at z ≈ 7, dust appears widespread (Inami et al. 2022; Schouws et al. 2023; Witstok et al. 2023a; Algera et al. 2023) - both puzzlingly high dust-to-stellar mass ratios ( M d /M ⋆ ∼ 0 . 01; Algera et al. 2024) and fully dust-obscured sources (Fudamoto et al. 2021) are observed at this epoch. In addition, features of the at-  \nion curve associated with the carbonaceous dust grains produced by SNe are observed at z ∼ 6 . 7 (Witstok et al. 2023b).  \nThe discrepancy between what is observed by JWST versus what is expected based on dust production from past SNe can be resolved by assuming that the majority of the dust has been removed from star-forming regions by radiation pressure-driven outflows. Such a scenario had been suggested in the Attenuation Free Model (AFM) presented in Ferrara et al. (2024).  \nIn their fiducial model, Ferrara et al. (2024) suggest the dust in GS-z14 to have a typical extent of 1 . 4 kpc, as a more compact size would be inconsistent with the visual extinction measured by JWST. We note that, given the resolution of our data, dust of this extent would not be resolved across multiple ALMA beams. Combined with a fiducial yield of 0 . 1 M ⊙ /SN, the AFM predicts a continuum flux density for GS-z14 of F 88 = 14 . 9 µ Jy. This is just below the sensitivity limit of our observations, which yield an upper limit of F 88 < 15 . 1 µ Jy beam -1 . As such, a conclusive investigation of the dust content of GS-z14, as well as further testing of the AFM model predictions, requires deeper and high-resolution ALMA continuum observations.  \nTable 1. Properties of GS-z14  \nNotes: M UV from Carniani et al. (2024); stellar mass and SFR from Helton et al. (2024). Values have been corrected for a lensing magnification of 1.17 × (Carniani et al. 2024).', '5. SUMMARY': 'We report the robust detection of a 6.6 σ [OIII] 88 µm line of JADES-GS-z14-0 at 223.528 ± 0.009 GHz, providing us with a precise spectroscopic redshift measurement of z = 14 . 1793 ± 0 . 0007. This represents a substantial jump in redshift over the previous highredshift [OIII] 88 µm -detection from MACS1149-JD1 at z = 9 . 1096 (Hashimoto et al. 2018). The [OIII] 88 µm line  \nwas identified using data from an ALMA Cycle-10 DDT program (2023.A.00037.S, PI: Schouws) providing a spectral scan from 218.70 to 229.45 GHz (10.75 GHz baseline), covering the redshift range z=13.79 to 14.51. The precision of the current redshift measurement represents ≳ 180 × gain over the prior redshift measurement of z = 14 . 32 +0 . 08 -0 . 20 from NIRSpec.  \nThe redshift we find for the source is consistent with the redshift Carniani et al. (2024) derive ( z = 14 . 178 ± 0 . 013) based on their tentative 3.6 σ detection of CIII] 1907 , 1909 doublet at 2.89 µ m, providing strong evidence the earlier line detection is real. As such, we now have multiple line detections of GS-z14-0, CIII] 1907 , 1909 (3.6 σ ) with JWST and [OIII] 88 µm (6.6 σ ) with ALMA, providing rather definitive evidence for the robustness of the redshift determination of GS-z14-0. Of note, the detection of [OIII] 88 µm with ALMA was achieved with less integration time (2.8 hours) than was required for the 3.6 σ tentative detection of CIII] 1907 , 1909 with JWST (9.3 hours), providing a rather dramatic illustration of the discovery potential of ALMA.  \nWe find no detection of the dust continuum from JADES-GS-z14-0 based on the DDT observations, with a < 3 σ upper limit of < 15.1 µ Jy beam -1 . This suggests a low dust content of M d /M ⋆ < 2 . 4 × 10 -3 , consistent with supernova dust production yields y d < 0 . 3 M ⊙ /SN.  \nCombining a previous JWST/MIRI photometric measurement of the [OIII] λλ 4959,5007 ˚ A and H β lines with Cloudy models, we find GS-z14 to be surprisingly metal-enriched ( Z ∼ 0 . 05-0.2 Z ⊙ ) a mere 300 Myr after the Big Bang, with moderate to low density log( N ) < 3 . 0 cm -3 .  \nThanks to the precise spectroscopic redshift measurement and [OIII] 88 µm line detection we now have for GS14-0 using just 2.8 hours, it is clear that additional follow-up of GS-z14-0 with ALMA would be highly fruitful and should include (1) higher spatial resolution observations of [OIII] 88 µm to improve constraints on dynamical masses and state of GS-z14-0 and deeper constraints on the dust continuum, (2) observations of the [CII] 158 µm line in band 4, lying just 0.2 GHz above the low-frequency boundary, to better probe the ionization parameter U and build-up of metals, and (3) JWST/MIRI observations of [OIII] λλ 4959,5007 ˚ A and H β to place tighter constraints on the electron density and metallicity of GS-z14-0.', 'ACKNOWLEDGMENTS': 'This paper makes use of the following ALMA data: ADS/JAO.ALMA 2023.A.00037.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We are greatly appreciative to our ALMA program coordinator Violette Impellizzeri for support with our ALMA program and Allegro, the European ALMA Regional Center node in the Netherlands. We are grateful to Joris Witstok for providing the Cloudy models from Witstok et al. (2022) for the analysis conducted in this paper. This work was supported by NAOJ ALMA Scientific Research Grant Code 2021-19A (HA).', 'REFERENCES': "Akins, H. B., Fujimoto, S., Finlator, K., et al. 2022, ApJ, 934, 64, doi: 10.3847/1538-4357/ac795b Algera, H. S. B., Inami, H., Oesch, P. A., et al. 2023, MNRAS, 518, 6142, doi: 10.1093/mnras/stac3195 Algera, H. S. 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