GA-NIFS: high prevalence of dusty and metal-enriched outflows in massive and luminous star-forming galaxies at $z\sim3-9$

A. Bunker; B. Rodr\'iguez Del Pino; C. Marconcini; E. Bertola; E. Parlanti; F. D'Eugenio; G. C. Jones; G. Cresci; G. Venturi; H. \"Ubler

REVIEW 3 major objections 5 minor 4 cited by

This paper claims that the ionized outflows driven by intense star formation in the most massive galaxies at z~3–9 are common but inefficient: they move at speeds below the escape velocity, carry typical mass-loading factors below one, and

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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2026-08-03 11:27 UTC pith:Y57MRIT7

load-bearing objection The observational core — first IFU census of dusty, metal-enriched outflows in massive z=3–9 galaxies — is solid and worth publishing; the 'inefficient feedback' conclusion, however, is hostage to an adopted outflow electron density that could flip η above unity if wrong. the 3 major comments →

arxiv 2601.06255 v2 pith:Y57MRIT7 submitted 2026-01-09 astro-ph.GA

GA-NIFS: high prevalence of dusty and metal-enriched outflows in massive and luminous star-forming galaxies at zsim3-9

B. Rodr\'iguez Del Pino , S. Arribas , M. Perna , I. Lamperti , A. Bunker , S. Carniani , S. Charlot , F. D'Eugenio

show 11 more authors

R. Maiolino H. \"Ubler E. Bertola T. B\"oker G. Cresci G. C. Jones C. Marconcini E. Parlanti J. Scholtz G. Venturi S. Zamora

This is my paper

classification astro-ph.GA

keywords galactic outflowsstellar feedbackhigh-redshift galaxiesJWSTintegral field spectroscopymass-loading factorgas metallicitydust attenuation

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 asks whether the violent star formation in the most massive galaxies of the early Universe (redshifts 3 to 9) powers outflows that actually stop star formation and expel gas into intergalactic space. Using JWST's integral-field spectroscopy, the authors resolve the kinematics of the ionized gas in 40 galaxy regions within 15 complex systems and find a broad outflow component in 14 of them. Compared with the host interstellar medium, this outflowing gas is on average more heavily dust-attenuated (by about 0.6 magnitudes) and more metal-enriched (by about 0.13 dex), but it is usually moving slower than the escape velocity and its mass-loss rate is typically no higher than the star-formation rate. The conclusion is that in this mass and redshift regime, ionized ejective feedback is inefficient; the winds stir and enrich the galaxy's own gas rather than powering the galaxy-wide quenching and circumgalactic enrichment that some models assume. This matters because it identifies the mass and time regime where stellar feedback may not be the dominant mechanism that regulates early massive galaxies.

Core claim

The central discovery is that spatially resolved ionized outflows in massive, luminous star-forming galaxies at z~3–9 are common (35% of regions) yet dynamically and energetically modest. The outflowing gas shows enhanced dust attenuation (A_V about 0.59 mag higher) and oxygen abundance (about 0.13 dex higher) than the systemic gas, which the authors take as direct evidence that the broad component is a genuine outflow rather than a merger artifact. Outflow velocities range from 170 to 600 km/s with dispersions 130–340 km/s, and in all but one case the outflow velocity remains below the estimated escape velocity. Mass-loading factors, computed from dust-corrected [OIII] luminosities and spat

What carries the argument

The central object is the broad kinematic component: a second Gaussian component in the [OIII]5007 and Hα line profiles, selected when a Bayesian information criterion favors two components, the broad component has signal-to-noise above 3, and its velocity dispersion exceeds 100–140 km/s. Its properties (dust attenuation from Balmer decrements, oxygen abundance from R3/N2 indicators, velocity, and spatial extent from resolved maps) are compared with the narrow systemic component. The quantitative workhorse is the mass-loading factor η = Ṁ_out/SFR, with Ṁ_out = M_out v_out/r_out; the outflow mass M_out is obtained from the dust-corrected broad [OIII] luminosity divided by metallicity and elec

Load-bearing premise

The conclusions hinge on the adopted electron density of the outflow: it is measured for only a few sources, and for the remaining nine outflows the paper assumes a common value of 500 cm^-3; because the computed outflow mass (and hence the mass-loading factor) is inversely proportional to this density, a true density closer to 100 cm^-3 would raise most η values above unity and overturn the 'inefficient feedback' conclusion.

What would settle it

Measure the [OII] or [SII] doublet ratio in the broad outflow component of a few of these galaxies to obtain a direct electron density; if typical densities are ~100 cm^-3 instead of ~500 cm^-3, the mass-loading factors exceed one, contradicting the central claim. Alternatively, deep observations of neutral or molecular outflow tracers (such as [CII]) in these systems that show most of the outflowing mass is in non-ionized phases would indicate that the ionized phase underestimates the true ejective feedback.

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

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If this is right

Ionized outflows in massive z≈3–9 starbursts do not by themselves quench star formation: mass-loading factors η≤1 in the majority of cases.
These winds are likely redistributing dust and metals inside the halo rather than expelling them to the circumgalactic medium, as v_out/vesc<1 in all but one case.
The high metal content of the broad component rules out a pristine infall or merger-driven origin for the broad emission, strengthening the outflow interpretation.
Outflow speed correlates with star-formation rate across a wider mass range than previously probed, with a slope similar to that of local ultra-luminous infrared galaxies.
Detectability of outflows rises with stellar mass and SFR; previous lower-mass samples gave conflicting incidence and η values partly because of resolution and selection criteria.

Where Pith is reading between the lines

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

If the true electron density of the outflowing gas is lower than the assumed ~500 cm^-3 (or the measured systemic densities), the mass-loading factors would scale upward proportionally; direct density measurements of the broad component are the single measurement most likely to alter the paper's central conclusion.
The ionized phase may be only a tracer; if neutral and molecular outflows (e.g., traced by [CII] at these redshifts) carry substantially more mass, the total ejective feedback could still be efficient even though the ionized phase is not.
The near-identical slope of the v_out–SFR relation between these early galaxies and local ULIRGs suggests a redshift-independent empirical scaling for starburst-driven winds that could be used as a simple sub-grid feedback recipe in simulations.
The bound, metal-enriched winds imply that heavy elements should remain inside the halo potential, which is testable by searching for extended metal-line halos around these same galaxies at larger radii.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

The observational core — first IFU census of dusty, metal-enriched outflows in massive z=3–9 galaxies — is solid and worth publishing; the 'inefficient feedback' conclusion, however, is hostage to an adopted outflow electron density that could flip η above unity if wrong.

read the letter

Quick take: this is the first spatially resolved IFU census of ionized outflows at the massive, luminous end of z=3–9, and it delivers a genuinely new result: the broad components are, on average, dustier (A_V ~0.59 mag) and more metal-rich (0.13 dex) than the host ISM. That is a clean, useful measurement, and it also argues against the broad emission being just merger turbulence. The v_out–SFR correlation combining their sample with Carniani+, Xu+, and Ivey+ is a nice consolidation. The paper is careful about spectral fitting, aperture corrections, AGN exclusion, and it flags its own subjective calls (candidate outflows HZ10_E and B14 are excluded from the global averages).

The soft spot is not the spectroscopy; it is the extrapolation from outflow luminosity to mass-loading factor. Eq. 2 has M_out ∝ n_out⁻¹, and for 9 of 14 outflows they adopt n_out=500 cm⁻³ without measuring the broad-component density. The [OII]/[SII] doublets are blended or low S/N. If the true outflow density is ~100 cm⁻³ — plausible if the outflowing gas has expanded — η scales up by a factor of five, and the 'η≤1 in 9/14' headline flips to a majority above unity. Their sensitivity test at 380 cm⁻³ only shifts η by 30%; it does not bracket the lower-density regime. The same lever propagates into the mass outflow rate. The escape-velocity comparison rests on M_dyn=2×M_star, another adopted number, though that one is conservative in the direction they state.

So the direct measurements — incidence, kinematics, dust, metallicity — are a solid advance and should survive. The interpretive layer ('ejective feedback is inefficient in massive high-z galaxies') is conditional on density and dynamical-mass assumptions that are not yet measured. The authors are transparent about this, but the abstract states the strong conclusion without the caveat.

Who is this for? People working on high-z feedback and the baryon cycle; it will be a standard reference for the massive end. It deserves a serious referee: the sample is unique, the analysis is mostly careful, and the density issue can be addressed with density-sensitive line measurements or at least an honest bracketing of η. I'd send it out.

Referee Report

3 major / 5 minor

Summary. The paper presents a search for and characterization of ionized outflows in 40 galaxies/regions belonging to 15 star-forming systems at z~3–9, using JWST/NIRSpec IFU data from GA-NIFS. Broad kinematic components are identified in 14/40 regions (≈35% incidence). From two-component spectral fits, the authors report that the broad (outflow) component is on average more dust-attenuated (ΔA_V≈0.59 mag) and more metal-enriched (Δ12+log(O/H)≈0.13 dex) than the narrow (ISM) component. They compute mass-loading factors η=Ṁ_out/SFR using a conical outflow model and the Carniani et al. (2024) formulation for M_out, finding η≤1 in most outflows (10/14 excluding candidates; the abstract says 9/14), and compare v_out with an estimated escape velocity, concluding that most outflows remain bound and that ejective feedback is inefficient in massive, luminous high-z star-forming galaxies.

Significance. If the main result holds, this is a valuable benchmark: it is one of the first large, spatially resolved NIRSpec IFU studies of ionized outflows at z>3 in the high-mass regime (log M*/M⊙≈9.5–11), complementing earlier MOS/WFSS studies of lower-mass galaxies. The paper’s strengths include a homogeneous reduction and MCMC spectral modeling with tied kinematics, direct Balmer-decrement and metallicity measurements for the broad component in a subset, careful discussion of AGN exclusion, and an explicit comparison with previous samples that reveals a significant v_out–SFR correlation. The main limitation is that the central η-based conclusion is inversely proportional to an unmeasured outflow electron density; a realistic lower n_out would flip the headline. The paper is transparent about this and other assumptions, but the conclusions currently overstate the robustness of the 'inefficient ejective feedback' claim.

major comments (3)

[§7.2.1, Eq. (2)] The mass-loading factor and hence the central claim of inefficient ejective feedback scale as η ∝ M_out ∝ n_out^{-1}. For 9 of 14 outflows the broad-component electron density is not measured and a common n_out=500 cm^-3 is adopted; [OII] and [SII] doublets are blended or low-S/N. If the true outflow density is ~100 cm^-3, as is plausible for expanded outflowing gas, η increases by a factor ~5 and most of the 14 outflows would have η>1. The sensitivity test with n_e=380 cm^-3 only raises η by ~30% and does not bracket this regime. I request an explicit sensitivity analysis over n_out≈100–1000 cm^-3 (or a stacked measurement of broad-component density-sensitive doublets), and conclusions that clearly state this dependence. This is load-bearing because it directly affects the 'η≤1 in 9/14' summary.
[§5 and §7.2.2] The outflow sample is defined by the presence of a broad component with σ_broad>100 km/s (or a single component with σ>140 km/s) in [OIII]/Hα. The claim that the broad component is metal-enriched and therefore truly an outflow is not an independent test, because the same broad component is used both to define the outflow and to measure Z_broad and A_V,broad. Merger-induced turbulence can also produce broad, high-σ emission, and the selection in merging systems is explicitly subjective (Sec. 5, Appendix B.10). To make the outflow identification load-bearing for the incidence (14/40) and metal-enrichment results, the authors should provide robustness tests (e.g., varying the σ threshold, alternative region definitions, excluding all merger/tidal systems) and, if possible, an independent kinematic or spatial criterion for outflow nature.
[§6.2.1, Table 2, §7.1] The quoted incidence (≈35%) and average outflow dust/metal enhancements are computed after subjective choices of outflow apertures and after excluding two candidate outflows (HZ10_E and B14). The regions range from nearly the whole broad-emission extension to small nuclear circular apertures in mergers. No uncertainty is propagated from these region definitions into the average A_V, Z, r_out, or η. Since the paper’s headline comparison with previous works and its 'dusty and metal-enriched outflows' claim depend on these choices, a robustness analysis (e.g., including the candidates, using a flux-weighted size, or alternative region boundaries) is needed to demonstrate that the averages and the incidence are stable.

minor comments (5)

[Abstract and §8] The abstract states 'η≤1, in 9 out of 14 the outflows' while the text and Table 2 (excluding HZ10_E and B14) indicate 10 of 14 outflows have η≤1. Please reconcile the count.
[Table 2 caption] The caption lists M_out as a column, but the table does not contain M_out. Either add the column or remove the mention.
[§6.2.3] Text reads 'down to 100 km^-1'; should be 'km/s'.
[§7.1] The sentence 'with our data is less challenging and subject to lower uncertainties' is grammatically incomplete; the intended meaning is likely that the identification is less challenging and has lower uncertainties.
[Appendix B.10 vs Table 2] Appendix B.10 says 'we do not consider the presence of a clear outflow in this system' for B14, yet Table 2 lists B14 as a candidate outflow with measured properties. Clarify this apparent inconsistency.

Circularity Check

0 steps flagged

No significant circularity: outflow properties are measured, not defined into existence; η and v_esc rest on stated assumptions, not fitted predictions.

full rationale

The paper's central quantities are direct spectral measurements (broad-component kinematics, Balmer decrements, line ratios) or model-dependent estimates whose assumptions are stated and tested rather than fitted to the target conclusions. The outflow sample is defined kinematically (two-component fits with σ_broad>100 km/s and spatial association with star formation), and the reported A_V and metallicity enhancements are measured on those components, not imposed by the selection; the paragraph in Sec. 5 using those enhancements to argue against a merger interpretation is a consistency check, not a derivation. The mass-loading factors follow Eqs. 1-2 with adopted n_out values (systemic or 500 cm^-3), and the paper explicitly quantifies the sensitivity to n_e (Sec. 7.2.1); this is an assumption, not a fitted input masquerading as a prediction. The escape-velocity comparison uses an assumed M_dyn=2 M_star (Sec. 7.2.2) from prior work, but this is a parameter assumption with stated direction, not a self-referential derivation. No equation in the paper reduces to its own input, and no load-bearing claim is forced by a self-citation chain. Therefore no significant circularity is found.

Axiom & Free-Parameter Ledger

5 free parameters · 5 axioms · 0 invented entities

The paper's headline conclusions (η≤1, no escape, dust/metal redistribution) are supported by direct line-ratio measurements for dust and metallicity, but the quantitative outflow rates depend on several adopted parameters (n_out, r_out, M_dyn/M_star) that are not independently measured. The ledger counts five hand-chosen parameters and five domain assumptions; none are fitted to force the conclusions, but they set the normalization of η and v_esc.

free parameters (5)

Outflow electron density n_out = 500 cm^-3 (9 galaxies); systemic n_e for 5
Used in Eq. 2 to convert [OIII] luminosity to outflow mass; η ∝ n_out^-1, so the 'η≤1' conclusion depends on this. §7.2.1.
Outflow radius r_out = 0.5-1.7 kpc; 0.25-0.3'' aperture for mergers
Measured from circularized regions where possible, but for mergers a fixed small circular aperture is assumed, not measured; Mdot = M_out v/r, so η ∝ 1/r. §6.2.1.
Dynamical-to-stellar mass ratio M_dyn/M_star = 2
Determines v_esc for the 'no escape' conclusion; for compact/rotating systems the paper notes M_dyn could be larger, but it does not explore smaller values. §7.2.2.
Outflow selection thresholds = σ_broad>100 km/s; single σ>140 km/s
Hand-chosen criteria define which regions are called outflows; the 35% incidence and the resulting outflow sample depend on these thresholds. §5.
A_V,broad for 4 galaxies = A_V,broad = A_V,narrow
HFLS3_g1, COS3018, B14, MACSJ0416-Y1 lack broad Balmer detections; assumed same attenuation as host for luminosity correction in Eq. 2. §7.2.1.

axioms (5)

domain assumption A broad, high-σ emission-line component traces a galactic outflow
The entire outflow identification rests on this; mergers and tidal interactions can also broaden lines. The authors use metallicity enhancement as supporting evidence, but measure it on the same component (§5).
domain assumption Calzetti attenuation law and Case B ratios (Hα/Hβ=2.86) apply at z=3-9
Used for dust corrections and SFR calibration; if the dust law or recombination ratios differ at high z, A_V and SFR shift. §3.1, §4.2.
domain assumption BPT and Mazzolari diagnostics reliably separate SF from AGN at high z
Used to exclude AGN; low-metallicity AGN can mimic SF in the NII diagram, as the paper notes in §4.1.
domain assumption Constant mass-outflow-rate conical outflow model (Lutz 2020)
Mdot = M_out v_out / r_out; if the geometry or time-dependence differs, η changes. §7.2.1.
domain assumption SFR calibration of Clarke et al. (2024) with Z*=0.004 is valid for these galaxies
Converts Hα luminosity to SFR; adopted metallicity affects SFR and hence the mass-loading factor η. §4.2.

reviewed 2026-08-03 · how reviews work

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Cite this review

Pith. "Pith review of GA-NIFS: high prevalence of dusty and metal-enriched outflows in massive and luminous star-forming galaxies at $z\sim3-9$." pith.science (2026). https://pith.science/paper/Y57MRIT7

@misc{pith2026260106255,
  author       = {Pith},
  title        = {Pith review of: GA-NIFS: high prevalence of dusty and metal-enriched outflows in massive and luminous star-forming galaxies at $z\sim3-9$},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/Y57MRIT7}},
  note         = {Machine review of arXiv:2601.06255}
}

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read the original abstract

We present a search for and characterization of ionized outflows in 15 star-forming systems at $z\sim3-9$ with no evidence of Active Galactic Nuclei (AGN), observed with JWST/NIRSpec IFU as part of the GA-NIFS program. The targets often show satellites and complex substructure, from which we isolate 40 galaxies/regions. The sample probes the high-mass end of the galaxy population, with most sources having log$_{10}$~(M$_\star$/M$_\odot$)=$9.5-11$, extending previous studies on high-z star formation driven outflows that mainly focused on lower-mass galaxies. Using the [OIII]5007 and H$\alpha$ emission lines, we identify broad kinematic components consistent with galactic outflows in 14 galaxies/regions. We find that the outflowing gas is more dust attenuated (by $A_{\rm V}$$\sim0.59$ mag on average) and metal-enriched (0.13 dex) than the interstellar medium (ISM) of the host galaxies, but its velocities are insufficient to escape the galaxies and reach the circumgalactic medium, suggesting that outflows mainly redistribute dust and metals around their hosts. The outflows identified in this study display velocity dispersions within $\sigma_{\rm out}=130-340$~km~s$^{-1}$ and outflow velocities $v_{\rm out}=170-600$~km~s$^{-1}$, and, when combined with less luminous and less massive star-forming galaxies from previous works, reveal a statistically significant correlation between $v_{\rm out}$ and star formation rate (SFR). The typically low mass-loading factors ($\eta=\dot{M}_{\rm out}/SFR$$\leq1$, in 9 out of 14 the outflows) indicate that these outflows do not strongly suppress star formation. Overall, our results suggest that ejective feedback via ionized outflows is inefficient in massive, luminous star-forming galaxies within the first 2 Gyr of the Universe.

Figures

Figures reproduced from arXiv: 2601.06255 by A. Bunker, B. Rodr\'iguez Del Pino, C. Marconcini, E. Bertola, E. Parlanti, F. D'Eugenio, G. C. Jones, G. Cresci, G. Venturi, H. \"Ubler, I. Lamperti, J. Scholtz, M. Perna, R. Maiolino, S. Arribas, S. Carniani, S. Charlot, S. Zamora, T. B\"oker.

**Figure 1.** Figure 1: Maps of integrated fluxes in [O iii] λ5007 for all the galaxy systems in our sample, with the exception of HFLS3_g1 for which we show integrated Hα fluxes. Orange apertures mark small regions at the peaks of emission of the different (sub-) systems to constrain the dominant ionization mechanisms (see [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗

**Figure 2.** Figure 2: Emission-line diagnostics for the galaxies in our sample obtained for the apertures highlighted in Figure [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗

**Figure 3.** Figure 3: Stellar mass vs total SFR for the individual star forming [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗

**Figure 4.** Figure 4: Velocity dispersion maps of the broad component ( [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗

**Figure 5.** Figure 5: Comparison of the nebular dust attenuation ( [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗

**Figure 6.** Figure 6: Kinematic properties of the outflows, σout, ∆V, Vout, compared to host properties, LHα (SFR), ΣL(Hα) (ΣSFR), M∗. Large symbols correspond to the outflows identified in our study, and are color-coded according to their redshifts, as in [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗

**Figure 7.** Figure 7: Mass loading factor (η) of the outflows in our sample as a function of S FRHα (LHα; left) and stellar mass, M⋆, of the host galaxy (right). Symbols are the same as in [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗

**Figure 8.** Figure 8: Ratio between the outflow velocity (vout) and the vesc as a function of S FRHα (LHα). In [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗

discussion (0)

Forward citations

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Reference graph

Works this paper leans on

6 extracted references · 1 linked inside Pith · cited by 4 Pith papers

[1]

2024, Astronomy and Astrophysics, 686, A85 Arribas, S., Colina, L., Bellocchi, E., Maiolino, R., & Villar-Martín, M

Álvarez-Márquez, J., Colina, L., Crespo Gómez, A., et al. 2024, Astronomy and Astrophysics, 686, A85 Arribas, S., Colina, L., Bellocchi, E., Maiolino, R., & Villar-Martín, M. 2014, Astronomy and Astrophysics, 568, A14 Article number, page 14 of 39 B. Rodríguez Del Pino et al.: GA-NIFS: Spatially-resolved outflows at 3<z<9 Arribas, S., Perna, M., Rodríguez...

Pith/arXiv arXiv 2024
[4]

(2024) already identified a spatially resolved ionized bi-conical outflow with an extension of∼3 kpc along the minor axis of the central galaxy of this system (see their Figure 6)

In their study, Lamperti et al. (2024) already identified a spatially resolved ionized bi-conical outflow with an extension of∼3 kpc along the minor axis of the central galaxy of this system (see their Figure 6). Similarly to their results, we find a region with enhanced velocity dispersion extending to the East and West from the central regions of 5001-C...

2024
[5]

To compute these losses, we start by generating a data cube containing the simulated PSF of the NIRSpec IFS mode using the STPSF3 Python package

we apply a correction for the light losses outside the adopted apertures caused by the NIRSpec PSF. To compute these losses, we start by generating a data cube containing the simulated PSF of the NIRSpec IFS mode using the STPSF3 Python package. At this stage we work with a data cube generated in the R100 mode, which allows to compute the losses across th...

2018
[6]

Jones et al

observations. Jones et al. (2025) identified the presence of a broad component associated to the integrated spectra of these structures (FW H M∼550−750 km/s), as well as an extended broad emission as traced by theW80 index over a region of about 4 kpc along the direction of the two main cores. They interpreted these features as due to tidal effects or the...

2025
[2019]

and [Cii] 157.7µm (Bakx et al. 2020). In a recent study using NIRCam/WFSS data, Ma et al. (2024) estimated highS FRs (∼165M ⊙yr−1), relatively large dust extinctionA V =0.92− 1.10 mag and very young stellar populations (<5 Myr). In our study, we identify a compact (r out =0.5 kpc) ionized outflow in a star-forming region at the East of the system, and σou...

2020
[2025]

have revealed three close merging galaxies/structures in the system, HZ4-N, HZ4-C, and HZ4-S, all within a projected distance of about 4 kpc. They detect and characterize ionized outflows in HZ4-C and found that it extends over regions of up to 4 kpc with velocity 4The FoV also includes GS-4923, but this galaxy has a photometric redshift of about 0.2 acco...

2021

This paper was first reviewed by deepseek-v4-flash on August 3, 2026.

[1] [1]

2024, Astronomy and Astrophysics, 686, A85 Arribas, S., Colina, L., Bellocchi, E., Maiolino, R., & Villar-Martín, M

Álvarez-Márquez, J., Colina, L., Crespo Gómez, A., et al. 2024, Astronomy and Astrophysics, 686, A85 Arribas, S., Colina, L., Bellocchi, E., Maiolino, R., & Villar-Martín, M. 2014, Astronomy and Astrophysics, 568, A14 Article number, page 14 of 39 B. Rodríguez Del Pino et al.: GA-NIFS: Spatially-resolved outflows at 3<z<9 Arribas, S., Perna, M., Rodríguez...

Pith/arXiv arXiv 2024

[2] [4]

(2024) already identified a spatially resolved ionized bi-conical outflow with an extension of∼3 kpc along the minor axis of the central galaxy of this system (see their Figure 6)

In their study, Lamperti et al. (2024) already identified a spatially resolved ionized bi-conical outflow with an extension of∼3 kpc along the minor axis of the central galaxy of this system (see their Figure 6). Similarly to their results, we find a region with enhanced velocity dispersion extending to the East and West from the central regions of 5001-C...

2024

[3] [5]

To compute these losses, we start by generating a data cube containing the simulated PSF of the NIRSpec IFS mode using the STPSF3 Python package

we apply a correction for the light losses outside the adopted apertures caused by the NIRSpec PSF. To compute these losses, we start by generating a data cube containing the simulated PSF of the NIRSpec IFS mode using the STPSF3 Python package. At this stage we work with a data cube generated in the R100 mode, which allows to compute the losses across th...

2018

[4] [6]

Jones et al

observations. Jones et al. (2025) identified the presence of a broad component associated to the integrated spectra of these structures (FW H M∼550−750 km/s), as well as an extended broad emission as traced by theW80 index over a region of about 4 kpc along the direction of the two main cores. They interpreted these features as due to tidal effects or the...

2025

[5] [2019]

and [Cii] 157.7µm (Bakx et al. 2020). In a recent study using NIRCam/WFSS data, Ma et al. (2024) estimated highS FRs (∼165M ⊙yr−1), relatively large dust extinctionA V =0.92− 1.10 mag and very young stellar populations (<5 Myr). In our study, we identify a compact (r out =0.5 kpc) ionized outflow in a star-forming region at the East of the system, and σou...

2020

[6] [2025]

have revealed three close merging galaxies/structures in the system, HZ4-N, HZ4-C, and HZ4-S, all within a projected distance of about 4 kpc. They detect and characterize ionized outflows in HZ4-C and found that it extends over regions of up to 4 kpc with velocity 4The FoV also includes GS-4923, but this galaxy has a photometric redshift of about 0.2 acco...

2021