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REVIEW 3 major objections 6 minor 3 cited by

This paper establishes that the MACS0647-JD system at z=10.17 is a pre-coalescence merger in which turbulent, metal-poor gas between the two stellar clumps drives the current starburst.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-02 19:59 UTC pith:DQ2PQWUB

load-bearing objection First z>10 resolved ISM study with a clever Hβ recovery, but the merger narrative rests on a sub-PSF centroid offset that needs more work. the 3 major comments →

arxiv 2603.00232 v3 pith:DQ2PQWUB submitted 2026-02-27 astro-ph.GA

GA-NIFS: Dissecting The Alchemised: JWST reveals turbulent metal-poor gas fuelling a co-spatial starburst in a complex system at z=10.17

Robert G. Pascalau , Francesco D'Eugenio , Roberto Maiolino , Qiao Duan , Yuki Isobe , Santiago Arribas , Andrew J. Bunker , St\'ephane Charlot
show 20 more authors
Michele Perna Bruno Rodriguez Del Pino Hannah Ubler Elena Bertola Torsten Boker Stefano Carniani Dan Coe Giovanni Cresci Mirko Curti Tiger Y.Y. Hsiao Lucy R. Ivey Gareth C. Jones Isabella Lamperti Eleonora Parlanti Jan Scholtz Sandro Tacchella Lorenzo Ulivi Giacomo Venturi Joris Witstok Sandra Zamora
This is my paper
classification astro-ph.GA
keywords high-redshift galaxiesJWSTNIRSpec/IFUgas-phase metallicitystarburstgalaxy mergersMACS0647-JDturbulent ISM
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper tries to establish that MACS0647-JD1, a gravitationally lensed galaxy seen when the Universe was about 460 million years old, is not a single rotating disc but a system of two stellar clumps caught in the early stages of a merger. Using JWST's NIRSpec integral-field spectroscopy, the authors map gas-phase metallicity, electron temperature, velocity dispersion, and star-formation burstiness on sub-kiloparsec scales. They find that the two clumps have markedly different oxygen abundances, that the brightest Hydrogen-gamma emission is offset 150 pc from the stellar continuum, and that the most intense recent star formation sits exactly where the gas is most turbulent and metal-poor. If correct, this gives the first spatially resolved picture of how metal-poor gas inflows and gravitational interactions trigger starbursts in the earliest galaxies, directly supporting the theoretical scenario in which feedback removes metals and fresh accretion fuels bursts.

Core claim

The central claim is that MACS0647-JD1 consists of two stellar components with distinct enrichment histories — the more massive south-east clump at 12+log(O/H)=7.89 and the less massive north-west clump at 7.47 — separated by only ~300 pc in the source plane. The H-gamma line-emission centroid is offset by ~0.1 arcsec (150 pc) from the stellar continuum, which coincides with the main component. Spaxel-by-spaxel maps show the region between the clumps holds the most turbulent gas (FWHM up to ~300 km/s), the lowest metallicities, and the highest star-formation burstiness, while the more massive clump is comparatively quiescent. The authors interpret this as evidence that recently accreted, dyn

What carries the argument

A PSF-matched NIRSpec/IFU data-cube with spaxel-scale spectral fitting; an extended wavelength calibration that recovers H-beta beyond the nominal G395M range; direct electron-temperature metallicities from the [OIII]4363 auroral line; a strong-line photoionisation grid; and spaxel-by-spaxel SED-derived star-formation histories. The load-bearing observable is the spatial offset between line-emission and stellar-continuum centroids, combined with co-spatial maps of metallicity, velocity dispersion, and burstiness that tie the turbulent metal-poor gas to the local starburst.

Load-bearing premise

The ~0.1 arcsec offset between the H-gamma line-emission centroid and the stellar continuum centroid is a real displacement and not a NIRSpec/IFU calibration artifact; the PSF FWHM is 0.22 arcsec, the astrometric re-alignment is a 0.19 arcsec correction, and slice-geometry systematics can create spurious velocity patterns.

What would settle it

Re-observing MACS0647-JD1 at a position angle rotated by 90 degrees, or with an independent astrometric calibration, would settle the question: if the H-gamma centroid offset and the apparent velocity gradient vanish or shrink below ~0.02 arcsec, the merger-driven starburst interpretation collapses. Alternatively, a deep ALMA/NOEMA detection of cold gas showing ordered rotation rather than disturbed kinematics would argue for a disc.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

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If this is right

  • Early galaxies at z>10 can be spatially resolved with JWST IFU, revealing that their ISM is not uniformly enriched but contains metal-poor gas pockets that track recent star formation.
  • A metallicity contrast of 0.4 dex over ~300 pc is hard to produce by in-situ clump formation in a single disc, favouring mergers or external gas accretion as the trigger of early starbursts.
  • The co-spatiality of high velocity dispersion, low metallicity, and high burstiness suggests that turbulence in the early ISM is powered by gravitational interactions and inflows rather than only by stellar feedback.
  • Recovering H-beta beyond the nominal NIRSpec G395M range is feasible and yields flux-calibration uncertainties below ~15%, extending the usable wavelength coverage for z>10 spectroscopy.
  • If the merger interpretation holds, MACS0647-JD1 offers a local-scale laboratory for the feedback-inflow cycle thought to regulate bursty star formation before Cosmic Noon.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The method of using emission-line-to-continuum centroid offsets as a merger/starburst diagnostic could be applied to other JWST IFU targets; the real test will be whether re-observations at a rotated position angle reproduce the same offset.
  • The apparent anti-correlation between FWHM and the O3Hg line ratio, if confirmed at lower redshift, implies that high-dispersion spaxels are preferentially ionised by harder radiation fields — a selection effect that could bias integrated metallicity measurements in turbulent galaxies.
  • A direct extension of this work is to measure the cold gas content of the same system; if the rough gas-mass estimate (log M_gas/M_sun ~ 8.2) is confirmed, the system is gas-dominated, meaning the next starburst could be even stronger once the inflowing gas reaches the clumps.
  • The tentative AGN-like signatures in the south-west region, which the authors disfavour, could be tested by deeper auroral-line or X-ray observations; if AGN contribution is present, the strong-line metallicities in that region would be biased.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. This paper presents NIRSpec/IFU G395M observations of the gravitationally lensed z=10.17 system MACS0647-JD1. The authors perform spaxel-by-spaxel and aperture-averaged emission-line fitting, recover H-beta beyond the nominal G395M wavelength range, derive direct-Te and strong-line gas-phase metallicities, and fit SEDs with prospector to map stellar mass and star-formation burstiness. They report two stellar components with different metallicities (SE clump 12+log(O/H)=7.89±0.11; NW clump 7.47±0.14, direct method), a ~0.1 arcsec (150 pc) offset between the H-gamma emission centroid and the F444W stellar continuum centroid, and spatially correlated turbulent, metal-poor gas in the north-east region. They interpret these as evidence for a merger-driven starburst with infalling low-metallicity gas. The paper includes extensive cross-checks: direct and strong-line abundances agree, H-beta-based and H-gamma-based abundances agree, the MIRI-based H-beta flux is consistent, and bootstrap resampling retains only the FWHM-O3Hg anti-correlation.

Significance. The work is potentially important: it is the first spatially resolved ISM study at z>10, provides the highest-redshift NIRSpec direct-Te metallicity, and demonstrates a technically challenging H-beta recovery beyond the nominal grating range. The internal consistency checks are a strength, and the paper is generally careful in acknowledging systematics (e.g., Appendix C). However, the central physical narrative—a merger-driven starburst between two clumps—rests heavily on the 0.1 arcsec line/continuum centroid offset, which is sub-PSF and comparable to known NIRSpec/IFU calibration uncertainties. The velocity-field evidence is explicitly inconclusive. If the offset is not real, the merger interpretation loses its strongest spatial argument, although the metallicity asymmetry and burstiness maps remain interesting. The manuscript merits major revision to either robustly establish the offset or soften the causal claims.

major comments (3)
  1. [Section 2.4 / 5.1.1 / Appendix A] The claim that the H-gamma (and [NeIII]) emission centroid is offset by ~0.1'' from the stellar continuum centroid is load-bearing for the merger-driven starburst interpretation (Section 5.1.1; first bullet of Section 6). The offset is two 0.05'' spaxels, while the PSF FWHM is 0.22'' and the astrometric re-alignment itself is 0.19''. Appendix A reports that ~1-spaxel centroid shifts between emission-line maps are expected from filter transmission and NIRSpec/IFU calibration imperfections and dismisses them as 'not worrying'; it does not demonstrate that a 2-spaxel shift is above the systematic floor for an extended source. The cited Beck (2025) 0.02'' residual applies to point sources, and Appendix C shows that slice-geometry systematics can create spurious spatial/kinematic patterns. To support the offset, the authors should quantify the systematic centroid uncertainty for this specific
  2. [Section 5.1.5 / Appendix C] The kinematic evidence does not discriminate between a merger and a rotating disc. The paper states in Appendix C that it is 'not able to fully rule out the hypothesis that this kinematic pattern might be real', and that a rotating disc is a possible interpretation. The slit-width model reproduces a substantial fraction (44 vs 114 km/s, 5th-95th percentile) of the observed gradient, and Beck (2025) reports artificial shifts of ~1.6 spectral pixels for G395M, similar to the observed gradient. Therefore the merger conclusion cannot rest on kinematics; it rests on the centroid offset and the metallicity contrast. If the offset is confirmed, the merger story is supported, but as written the discussion in Section 5.1.5 overstates the case.
  3. [Section 5.1.4 / Fig. 13] The burstiness map SFR_Hgamma/SFR100 is based on the same H-gamma line fluxes used to define the line centroid. If the line centroid is biased by the systematic offset discussed in Major Comment 1, the NE burstiness enhancement could be partly a spatial artifact. The SFR10/SFR100 map is a more independent tracer, but it is derived from prospector fits with a flexible non-parametric SFH and may suffer from degeneracies. The authors should show that the NE enhancement persists when the line-flux map is re-centered on the continuum centroid, or when only continuum-derived SFR10 is used. This is necessary to support the conclusion that the starburst is genuinely located in the metal-poor, turbulent region between the clumps.
minor comments (6)
  1. [Figure D2 caption] The panel labelled 'Spectro-photometric fit for the SE clump' in Figure D2 actually shows the NW clump results; the caption should be corrected.
  2. [Section 3.2] The noise re-scaling factor is a free parameter. Please state explicitly whether the reported uncertainties include this re-scaling in the final covariance, and whether the re-scaling is applied consistently to spaxel and aperture spectra.
  3. [Eq. (5)] Define the units of L_Hgamma explicitly (erg/s) and clarify the origin of the -40.5 constant and the -0.3 dex correction (Kennicutt & Evans 2012 with the Reddy et al. 2022 / Shapley et al. 2023 adjustment). Without these details the reader cannot reproduce the SFR scale.
  4. [Section 4.3] For the four spaxels with below-case-B Balmer ratios, setting A_V,cont = 0 is an ad hoc assumption. The paper acknowledges this, but a systematic uncertainty or a prior-based marginalization would better reflect the resulting metallicity uncertainty.
  5. [Abstract / Section 5.1.1] The phrase 'co-spatial starburst' is ambiguous: the starburst region (NE) is spatially offset from the two stellar components. Please define what is meant by 'co-spatial' (presumably co-spatial with the turbulent metal-poor gas, not with the stellar continuum).
  6. [Section 2.2] The sentence on background subtraction using 'H-gamma and [NeIII] 3869 to obtain the source mask' is unclear. Specify how these lines define the mask and whether continuum-only regions were used for background estimation.

Circularity Check

0 steps flagged

No significant circularity; the metallicity, stellar-population, and line-offset results rest on external calibrations and direct observations rather than on fitted inputs or self-citation.

full rationale

I walked the paper's derivation chain. Gas-phase metallicities are obtained from observed line ratios through external calibrations (Witstok et al. 2021; Gutkin et al. 2016) that are not fitted to this target, and the [OIII]5007 flux inferred from the Witstok relation is checked against the MIRI measurement of Hsiao et al. (2024b), so the agreement between the direct and strong-line methods is not purely by construction. Stellar masses and star-formation histories come from Prospector SED fits with stated priors, independent of the gas metallicity fits. The H-gamma/F444W centroid offset is an observational measurement; the merger/starburst narrative is an interpretation drawn from that offset plus the spatially resolved metallicity, FWHM, and burstiness maps, not a fitted parameter renamed as a prediction. Self-citations are to instrument-calibration and reduction methodology (PSF size, outlier rejection, slit-width effects) and are not load-bearing for the astrophysical conclusion in a circular way. The paper itself flags calibration limitations: Appendix A notes ~1-spaxel wavelength-dependent centroid drift 'caused by a combination of filter transmission effects and imperfect NIRSpec/IFU calibrations,' and Appendix C shows that slit-geometry systematics can produce artificial rotation patterns. These are acknowledged robustness concerns that could weaken the offset-based interpretation, but they do not make any derivation reduce to its own input. No equation is shown to be equivalent to the input by construction, and no fitted quantity is presented as a prediction. The only notable shared assumption is that both metallicity methods use the same Witstok et al. (2021) [OIII]5007 extrapolation; however, this is an external calibration with an external MIRI check, not a circular step.

Axiom & Free-Parameter Ledger

5 free parameters · 8 axioms · 0 invented entities

The central claim rests on standard JWST data reduction, direct-Te metallicity assumptions, a lensing model, an empirical extrapolation for [OIII]5007, and NIRSpec/IFU PSF/astrometry stability. The free parameters are calibration and SED-model parameters; there are no invented astrophysical entities. The most fragile input is the combination of the extrapolated [OIII]5007 relation and the sub-PSF centroid offset.

free parameters (5)
  • Per-spaxel noise rescaling factor = 1.9–2.5
    Free parameter in the emission-line fitting that rescales nominal flux uncertainties to match residual scatter; affects S/N thresholds and therefore which spaxels enter the metallicity and FWHM maps.
  • Prospector SED model parameters (log M*, SFR10, SFR100, Z*, tau2, tau1/tau2, ndust, Zgas, log U) = SE clump: log M*=7.77+/-0.09, log SFR10=0.04+/-0.07, log SFR100=0.26+/-0.09; NW clump: log M*=7.41+/-0.07, log SFR10=-0.
    Fitted to NIRCam photometry and NIRSpec spectroscopy with informative priors; these define the stellar masses, burstiness, and stellar metallicities reported in Table 1 and Appendix D.
  • A_V,cont = 0 for below-case-B Balmer spaxels = 0 mag (hand-set)
    Adopted for spaxels whose H-beta/H-gamma ratio falls below the case-B value, including four spaxels near the AGN-like south-west region; claimed effect on metallicity is <0.11 dex.
  • NIRSpec LSF pre-launch FWHM x 0.8 correction factor = 0.8
    Assumed from Shajib et al. 2025 to deconvolve intrinsic line widths; directly sets the gas FWHM map and the turbulence interpretation.
  • H-delta / H-zeta Gaussian prior = 2.46 +/- 0.3
    Prior used to deblend the H-zeta + HeI feature, centered on the case-B ratio with width set by flux-calibration uncertainties; small impact on the main results.
axioms (8)
  • standard math Flat LambdaCDM cosmology with H0=67.4 km/s/Mpc and Omega_m=0.315
    Used throughout for distances and physical scales; stated in Section 1.
  • domain assumption Lensing magnification mu=8+/-1 for MACS0647-JD1
    Taken from Chan et al. 2017; converts angular scales to source-plane kiloparsecs, SFRs, and gas masses.
  • domain assumption Witstok et al. (2021) Eq. (3) relation between [OIII]5007/[OII] and [NeIII]/[OII] holds at z=10.17
    Used to infer [OIII]5007, which is outside the NIRSpec G395M band; the relation is calibrated at z~0 and tested to z~9.5, but the z>10 application is an extrapolation.
  • domain assumption Case-B recombination ratios apply (H-beta/H-gamma=2.105, H-alpha/H-gamma=5.79, H-delta/H-zeta=2.46)
    Used for dust corrections, H-beta-based SFRs, and deblending; the paper explicitly sets some spaxels to zero attenuation when ratios fall below case-B.
  • domain assumption NIRSpec/IFU PSF is circular Gaussian with stpsf FWHM and residual astrometric/centroid systematics below 0.02 arcsec
    Justifies interpreting the 0.1 arcsec H-gamma versus continuum offset as astrophysical; the paper's own Appendix C shows slice-geometry effects can create artificial kinematic patterns.
  • domain assumption Oxygen exists only as O+ and O++; O3+ is negligible, so direct-Te abundances via PyNeb are valid
    Standard direct-method assumption, cited to Dors et al. 2020; used in Section 4.1 to convert [OII] and [OIII] line ratios to abundances.
  • domain assumption Star formation dominates the photoionization, with AGN and shocks disfavored
    Based on Mazzolari et al. 2024 diagnostics and shock modeling in Section 5.1.2; the paper acknowledges the south-west region is tentative and cannot be fully ruled out as AGN/shock-influenced.
  • domain assumption Gutkin et al. (2016) photoionization grid with C/O=0.72(C/O)_sun, xi_d=0.1, n_H=10^3 cm^-3, and 100 Msun IMF cutoff is appropriate for this system
    Used for strong-line metallicities in Section 4.5; grid choice is motivated by Hsiao et al. 2025 C/O measurement and high-redshift dust assumptions.

pith-pipeline@v1.3.0-alltime-deepseek · 42724 in / 15403 out tokens · 162965 ms · 2026-08-02T19:59:49.700348+00:00 · methodology

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Cite this review

Pith. "Pith review of GA-NIFS: Dissecting The Alchemised: JWST reveals turbulent metal-poor gas fuelling a co-spatial starburst in a complex system at $z=10.17$." pith.science (2026). https://pith.science/paper/DQ2PQWUB

@misc{pith2026260300232,
  author       = {Pith},
  title        = {Pith review of: GA-NIFS: Dissecting The Alchemised: JWST reveals turbulent metal-poor gas fuelling a co-spatial starburst in a complex system at $z=10.17$},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/DQ2PQWUB}},
  note         = {Machine review of arXiv:2603.00232}
}
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read the original abstract

Recent observations revealed that distant galaxies have bursty star formation histories, regulated by stellar or active galactic nuclei (AGN) feedback and gas inflows. According to theoretical models, feedback preferentially removes metal-rich gas, while subsequent starbursts are triggered by mergers and newly accreted gas that is generally less enriched than the galaxy's interstellar medium (ISM). Therefore, gas-phase metallicity provides key insights into the baryonic processes shaping early galaxies. We present the first NIRSpec/IFU study of spatially resolved ISM properties in the MACS0647-JD system ($z=10.17$). The system consists of two stellar components detected in NIRSpec/IFU and NIRCam photometry. The main component ($\log \left(M_{\ast}/M_{\odot}\right)=7.77 \pm0.09$; $12+\log\left(\rm O/H\right)=7.89 \pm 0.16$) is more massive and significantly more metal-rich compared to its companion ($\log \left(M_{\ast}/M_{\odot}\right)=7.42\pm0.07$; $12+\log\left(\rm O/H\right)=7.47 \pm 0.20$), suggesting an older stellar population and a prolonged chemical enrichment history. We find that the H$\gamma$ line emission centroid is spatially offset by $\sim 0.1^{\prime \prime}$ (150 pc in the source plane) from the stellar continuum centroid; the latter coincides with the location of the main stellar component. This offset provides possible evidence of a merger-driven starburst in this system. By comparing the spatial distributions of the metallicity, velocity dispersion, and the burstiness of star formation history, we infer the presence of turbulent, metal-poor gas outside the stellar components. %detected in both NIRSpec/IFU and NIRCam photometry. This metal-poor, dynamically unstable gas is likely responsible for the enhanced recent star formation in the north-east region of the system.

Figures

Figures reproduced from arXiv: 2603.00232 by Andrew J. Bunker, Bruno Rodriguez Del Pino, Dan Coe, Elena Bertola, Eleonora Parlanti, Francesco D'Eugenio, Gareth C. Jones, Giacomo Venturi, Giovanni Cresci, Hannah Ubler, Isabella Lamperti, Jan Scholtz, Joris Witstok, Lorenzo Ulivi, Lucy R. Ivey, Michele Perna, Mirko Curti, Qiao Duan, Robert G. Pascalau, Roberto Maiolino, Sandra Zamora, Sandro Tacchella, Santiago Arribas, Stefano Carniani, St\'ephane Charlot, Tiger Y.Y. Hsiao, Torsten Boker, Yuki Isobe.

Figure 2
Figure 2. Figure 2: The top panels show the astrometric alignment between the ICRS coordinates of the NIRSpec/IFU synthetic F444W image (Fig. 2a) and the original NIRCam F444W photometry (Fig. 2b). In Fig. 2a, we overlay con￾tours from the normalised NIRCam imaging data at 0.3, 0.5, 0.7, and 0.9 times the peak flux (defined by the stellar continuum centroid). We also highlight the brightest spaxels in the two clumps in the sy… view at source ↗
Figure 3
Figure 3. Figure 3: In Fig. 3a we display the raw and smoothed spectra from the circular aperture discussed in the main text in Section 3.2, together with the extrap￾olation towards longer wavelengths, outside the nominal wavelength range, but where the detector is still sensitive enough for us to extract meaningful data. Fig. 3b illustrates the variation of the derived flux calibration factor 𝑓cal across the wavelength range… view at source ↗
Figure 4
Figure 4. Figure 4: Fig. 4a shows the observed integrated aperture spectrum in the rest-frame wavelength range between 3600 Å and 4700 Å, highlighting the key emission lines discussed in the main text, including the [O ii] doublet and blended features. Fig. 4b represents a zoom-in over the spectral wavelength range 4800 Å < 𝜆rest < 4900 Å, which, for 𝑧 = 10.17, is redder than the nominal wavelength coverage of NIRSpec/G395M (… view at source ↗
Figure 5
Figure 5. Figure 5: Top panels: maps of the diagnostic ratios O3Hg and Ne3O2 (allow￾ing only spaxels with S/N > 3 for each emission line involved). The bottom panels show the spaxel-by-spaxel maps of gas-phase metallicity (Fig. 5c; showing only the spaxels with S/N > 3 for [O iii] 𝜆4363, H𝛾 and inferred [O iii] 𝜆5007) and the intrinsic, de-convolved gas FWHM (Fig. 5d; we only show spaxels with a S/N > 5 detection of H𝛾). The … view at source ↗
Figure 6
Figure 6. Figure 6: Fig. 6a illustrates the position of individual spaxels on the O3Hg vs Ne3O2 diagnostic diagram from Mazzolari et al. (2024). The dashed demarcation line separates regimes that are fully dominated by AGN photoionisation (AGN only) from regions in which both AGN and/or star formation may have similar contributions. Squares are individual spaxels, colour coded by the FWHM from the single Gaussian component fi… view at source ↗
Figure 7
Figure 7. Figure 7: This figure shows the map of the electron temperature of the [O iii] emitting gas in the central region of the system. We only show spaxels with S/N > 3 for the auroral [O iii] 𝜆4363 line. The white ‘+’ and ‘×’ crosses mark the centroids of stellar continuum and H𝛾 line emission, respectively. outside the nominal range of G395M grating. As an alternative we use the Ne3O2 which closely tracks O32 and it has… view at source ↗
Figure 8
Figure 8. Figure 8: This figure shows the R3-Ne3O2 photoionisation grid (with varying metallicity and ionisation parameter) of SFGs from Gutkin et al. (2016) based on CLOUDY models (Ferland et al. 2013, 2017). The choice of the grid is motivated in the main text of Section 4.5. Individual spaxels (with S/N > 5 on [Ne iii] 𝜆3869, [O ii] 𝜆3726, 3729 and H𝛽 lines) are plotted as dark-cyan small squares and their median uncertain… view at source ↗
Figure 10
Figure 10. Figure 10: In this figure, we illustrate the various shock models that we overlaid on the Mazzolari et al. (2024) diagnostic diagram, in order to compare with our data-points. Individual spaxels are marked with grey squares (with the pink error bars showing their median uncertainties), whereas the blue symbols have similar meanings to Fig. 6a: the diamond represent the full-aperture, the star is the SE clump and the… view at source ↗
Figure 11
Figure 11. Figure 11: This figure shows the variation of gas velocity dispersion (FWHM) as a function of O3Hg line ratio (Fig. 11a), electron temperature (Fig. 11b) or gas-phase metallicity calculated using the direct method (Fig. 11c). As before, we only show the spaxels with S/N[O iii]𝜆4363 > 3, but we also show the values corresponding to the SE and NW clump and for the full-aperture spectra. We display the individual and t… view at source ↗
Figure 12
Figure 12. Figure 12: This figure shows the calculated gas-phase metallicities (using both the direct-𝑇e and the strong-line methods) and the uncertainties for the spectra of the four apertures identified in Fig. 2b. For each aperture and method, violin plots illustrate the metallicities of spaxels within the said aperture. Darker-shade violins show the kernel density estimate (KDE) of median metallicities, while lighter-shade… view at source ↗
Figure 13
Figure 13. Figure 13: In this figure, we display the spatially resolved star formation burstiness in MACS0647-JD1 system. The burstiness probes the recent versus prolonged star formation activity in our target, and is defined in two alternative ways: SFRH𝛾/SFR100 (Fig. 13a) and SFR10/SFR100 (Fig. 13b). The magenta rectangles are the apertures corresponding to the two clumps (SE and NW, as identified from NIRCam F444W imaging; … view at source ↗

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Reference graph

Works this paper leans on

4 extracted references · cited by 3 Pith papers

  1. [1]

    Abdurro’uf et al., 2024, ApJ, 973, 47 Agertz O., et al., 2020, MNRAS, 491, 1656 Alarie A., Morisset C., 2019, Rev. Mex. Astron. Astrofis., 55, 377 Allen M. G., Groves B. A., Dopita M. A., Sutherland R. S., Kewley L. J., 2008, ApJS, 178, 20 Álvarez-Márquez J., et al., 2025, A&A, 695, A250 Arellano-Córdova K. Z., et al., 2022, ApJ, 940, L23 Arribas S., et a...

    arXiv 2024

  2. [4]

    We also indicate the position angle of the aperture of these observations, PA=38.83 ◦, i.e

    Figure C2.This figure shows the spatially resolvedΔ𝑣(the velocity field) map derived from single-Gaussian component spaxel-by-spaxel spectral fits (Fig.C2a).WeonlyshowthespaxelswithasoliddetectionofH𝛾(S/N>5). We also indicate the position angle of the aperture of these observations, PA=38.83 ◦, i.e. the direction of the NIRSpec/IFU slices. The velocity gr...

    2025

  3. [2020]

    In particular, Isobe et al

    and, more recently, in high spectral resolu- tion IFU studies of high-redshift galaxies. In particular, Isobe et al. (2023a) demonstrated that a differential effective slit width across theIFUslicescanintroducespuriousvelocitygradientsalignedwith the instrumental geometry, thereby mimicking ordered rotation in emission-line velocity fields. While the geom...

    2016

  4. [2024]

    We can remark that, in contrast to the results based on the diagnosticO3Hg−Ne3O2(from Fig

    are illustrated: O3Hg-O32(top panels)and O3Hg-O33(bottom panels). We can remark that, in contrast to the results based on the diagnosticO3Hg−Ne3O2(from Fig. 6, showing the presence of a south-southwest AGN-dominated region), if we use eitherO3Hg−O32orO3Hg−O33diagnostics, we would observe that all regions of the MACS0647-JD1 system are either dominated by ...

    2026