Pith. sign in

REVIEW 3 major objections 5 minor 86 references

An emerging baryon cycle in a galaxy 500 million years after the Big Bang

T0 review · 3 major / 5 minor · reviewed 2026-08-11 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Gz9p3, a merging galaxy 500 million years after the Big Bang, is caught in the act of establishing a self-regulating baryon cycle, with the first direct electron-density measurement of a high-redshift cool outflow.

desk verdict A genuinely new high-z outflow density measurement that deserves referee time, but the headline number rests on an unresolved C II/C II* blend the paper should demonstrate, not just prefer. read the letter →

arxiv 2608.09813 v1 pith:YZTRNTDQ submitted 2026-08-10 astro-ph.GA

Shengzhe Wang , Xin Wang , Hang Zhou , Zhijie Qu , Zhaozhou Li , Yuxuan Pang , Qianqiao Zhou , Shouyi Wang
show 12 more authors
Yangyao Chen Yuguang Chen Karl Glazebrook Glenn G. Kacprzak Nicha Leethochawalit Houjun Mo Themiya Nanayakkara Huiyuan Wang Weida Hu Xunda Sun Chao-Wei Tsai Hu Zhan
This is my paper · ORCID
classification astro-ph.GA
keywords high-redshiftgalaxiesgalacticoutflowsmass-loadingfactorfine-structureabsorptionelectrondensityfeedback-freestarburstbaryoncycleJWSTspectroscopy
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper argues that Gz9p3, a merging galaxy seen 500 million years after the Big Bang, is caught at the moment stellar feedback begins to regulate galaxy growth. By measuring the electron density of the cool outflowing gas directly from fine-structure absorption lines, the authors obtain a mass-loading factor of $\eta = 12.3^{+21.7}_{-9.9}$, among the highest measured for galaxies of similar mass and far above what emission-line methods would infer. The outflow speed is below the escape velocity of the host halo, so the expelled, metal-enriched gas is likely to remain bound and be recycled through the circumgalactic medium. The timing, an intense starburst 10-20 Myr before observation followed by strong feedback now, matches the delayed onset of feedback predicted by feedback-free starburst models. If this picture holds, it shows that self-regulated baryon cycling was already in place during the epoch of reionization.

What carries the argument

The load-bearing object is the fine-structure absorption diagnostic: the relative strengths of the resonance transitions CII $\lambda1334$ and SiII $\lambda1260$ versus their excited fine-structure lines CII$^*$ $\lambda1335$ and SiII$^*$ $\lambda\lambda1265,1533$ depend on the collisional excitation balance, which is set by the electron density. The authors compute the level-population ratios as functions of $n_e$ at $T_e=10^4$ K using an atomic database, then fit all four lines jointly with a six-parameter MCMC model that treats the covering fraction as free. The measured density then converts the absorption-line column into a mass flux via $\dot M_{\rm out} = \mu_H m_p n_H v_{\rm out} C_f A$, with the hydrogen density inferred from $n_e$ under full ionization, deliberately minimizing the inferred loading. This replaces the usual assumption-laden thin-shell or emission-line prescriptions; for comparison, the conventional [OIII]-based approach with an assumed $n_e=380$ cm$^{-3}$ gives $\eta=0.13$, nearly two orders of magnitude lower.

What would settle it

A higher-resolution spectrum (resolving power above about 4000) that separates CII $\lambda1334$ from CII$^*$ $\lambda1335$, which differ by roughly 264 km/s, would settle the question: if the excess absorption then tracks the other low-ionization lines rather than the fine-structure wavelength, the inferred density and the derived mass-loading factor collapse.

Watch

Extended reading notes

Core claim

Gz9p3 at $z=9.311$ exhibits a multiphase outflow: saturated SiII and SiIV absorption with covering fractions $C_{f,\rm LIS}>0.6$ and $C_{f,\rm HIS}>0.8$, both blueshifted by roughly 150-200 km/s, plus a broad [OIII] emission component consistent with a bipolar geometry. The central discovery is the joint modeling of CII, CII$^*$, SiII, and SiII$^*$ absorption, which yields $\log(n_e/{\rm cm^{-3}})=1.22^{+0.44}_{-0.71}$ (about 17 cm$^{-3}$) for the cool outflowing gas. Combined with the H$\beta$-based star-formation rate and the measured covering fraction, this gives an ionized mass-loading factor of $\eta = 12.3^{+21.7}_{-9.9}$. Because the density is measured rather than assumed, this estimate does not require an assumed outflow radius, opening angle, or dynamical time, and the authors argue it is a conservative lower limit for the ionized phase alone. Spatially resolved damped Ly$\alpha$ fits show a neutral-gas reservoir of $\log(N_{\rm HI}/{\rm cm^{-2}})\simeq 21.6$-$22.1$ extending along the merger-driven tidal tail, while the cool outflow velocity stays below the estimated escape velocity of about 350-650 km/s, so the baryons are redistributed rather than lost.

Load-bearing premise

The entire electron-density measurement rests on reading the excess absorption near CII $\lambda1334$ as fine-structure CII$^*$ rather than as a separate, carbon-rich velocity component; at the spectral resolution of about $R=1000$ the two interpretations cannot be cleanly separated, and the authors state they consider the fine-structure reading more likely rather than prove it.

Editorial extensions

If this is right

  • If Gz9p3 is representative, feedback that can regulate star formation was already operating about 500 million years after the Big Bang, earlier than most previous outflow measurements assumed.
  • Measured outflow densities can differ from commonly assumed values by orders of magnitude, so existing emission-line-based estimates of $\eta$ at high redshift may be systematically too low.
  • The finding supports a key untested prediction of feedback-free starburst models: a brief transition from unregulated burst to feedback-regulated cycling, with characteristic burst efficiencies $\epsilon \simeq 0.17$-$0.28$ in the adopted wind framework.
  • Because the cool outflow remains bound, much of the metal-enriched gas stays in the circumgalactic medium and can fuel later star formation, making mergers and feedback part of a single recycling cycle rather than one-way mass loss.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The same fine-structure pair method could be applied to other ultra-deep rest-frame UV spectra at $z>6$; if similar CII/CII$^*$ and SiII/SiII$^*$ pairs are detected, a whole class of absorption-line outflow measurements could be converted from assumption-dependent to density-calibrated.
  • The authors adopt fully ionized hydrogen, which minimizes the inferred hydrogen density; if a substantial neutral fraction coexists in the same cool phase, the true mass loading could be even higher than the reported $\eta$.
  • The contrast between the measured outflow density near 17 cm$^{-3}$ and the systemic ISM density near 225 cm$^{-3}$ suggests the cool outflowing gas is far more diffuse than the ambient medium, pointing to a probe for tracing how feedback redistributes gas.
  • If the recycling picture holds, one would expect Gz9p3 and similar post-burst galaxies to show later star-formation episodes in the tidally redistributed neutral gas, visible as spatially offset young stellar populations in deeper imaging.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper presents JWST/NIRSpec observations of Gz9p3, a merging galaxy at z=9.311, and reports two main results: (i) a spatially resolved DLA analysis of four sightlines indicating an enhanced neutral-gas reservoir along the tidal tail, and (ii) a multiphase outflow with a directly measured electron density of the cool phase, log(n_e/cm^-3)=1.22(+0.44,-0.71), inferred from a joint fit to CII, CII*, SiII, and SiII* absorption. From this density and the Hβ-based SFR, the authors derive a mass-loading factor eta=12.3(+21.7,-9.9), and they interpret the combination of a recent starburst and high present-day mass loading as evidence for delayed onset of feedback in a feedback-free starburst (FFB) framework. The paper also reports a moderate [OIII] emission-line outflow component and argues that the cool outflow is likely bound to the halo, so the baryons remain available for recycling.

Significance. If the electron-density measurement is correct, it is the first direct density constraint on a high-redshift galactic outflow and would substantially reduce one of the dominant uncertainties in outflow mass-loading estimates at the epoch of reionization. The paper is clearly written, makes transparent use of public JWST data, and explicitly acknowledges many of its assumptions. The spatially resolved DLA fitting is a constructive use of the prism data, and the CLASSY comparison provides a useful empirical sanity check of the fine-structure method. The significance is, however, conditional on the interpretation of the blended CII/CII* absorption feature, which is the load-bearing step for the central quantitative claims.

major comments (3)
  1. [Methods, 'Fine-structure absorption and electron density'] The electron-density measurement rests entirely on interpreting the excess absorption near CII 1334 as CII* 1335 rather than as an additional, carbon-rich velocity component. The paper states 'We consider the second interpretation more likely' but does not fit the alternative two-component CII model or compare evidences. At R~1000 the line separation is only ~264 km/s while the fitted b~85 km/s gives FWHM ~200 km/s, so the two interpretations are heavily blended; the qualitative arguments against a separate CII component (absence in SiII/OI/AlII, no redshifted counterpart) are not decisive, especially in a merger with known complex kinematics. The Supplementary Information states that G140H data from GLASS-JWST exist but were not used; these data could directly test the decomposition. This issue is load-bearing because if the excess is a separate CII component, the CII* column, n_e, and eta are unsupported.
  2. [Methods, 'FFB-model prediction and star-formation efficiency'; Eq. (8)] The claimed consistency with feedback-free starburst models is obtained by inverting Eq. (8), eta_app = (epsilon^{-1} - 0.8 - eta_h)/f_burst, using the observed eta together with f_burst=0.1 adopted from the same galaxy's SFH and eta_h=0.3 from M82. The resulting epsilon ~0.17-0.28 is therefore not an independent prediction but a solution forced through the observed eta; the agreement does not validate the FFB framework beyond showing that a solution exists. The paper should either present independent constraints on epsilon (e.g., from the SFH or from theoretical FFB calculations) or explicitly re-frame the result as a consistency check that inherits the model assumptions, and it should temper the abstract's claim that the observations are 'consistent with' FFB.
  3. [Fig. 3 and Methods, 'Outflow-rate calculation'] The 'bipolar+neutral' estimate multiplies the measured one-sided ionized eta by a factor of two for bipolar geometry and by another factor of two for an assumed equal neutral contribution, giving eta ~49, and this value is then used as the preferred comparison with simulation predictions. These two corrections are order-unity assumptions, not measurements, and the paper does not show how the comparison changes if they are relaxed. While the text labels the corrections as conservative, the main claim that Gz9p3 lies 1-2 orders of magnitude above TNG and FIRE predictions depends on these ad hoc factors; the paper should clearly separate the directly measured quantity from the corrected estimates and discuss the sensitivity of the conclusion to the adopted factors.
minor comments (5)
  1. [Supplementary Information, 'Additional details of the Voigt-profile fitting'] There is a typo: 'Supplementary Inforamtion' should be 'Supplementary Information'.
  2. [Methods, 'Outflow-rate calculation'] The text says the projected area A is taken as four-fifths of the slit area, but no justification or reference is given for this factor; the choice affects the absolute normalization of Mdot_out and eta.
  3. [Supplementary Information, 'Line-of-sight thickness of the low-ionization gas'] In Eq. (10) and the surrounding text, the symbols N_HI,out and N_DLA_HI are used without being explicitly defined in the main text; please define them at first use.
  4. [Abstract and Section 1] The acronym FFB is used in the abstract without being spelled out; define it at first use in the main text.
  5. [Fig. 3 caption] The caption states the dark-green shaded region is 'described in Methods', but the construction is only given in the Supplementary Information ('FFB mapping and momentum transfer'); please add a pointer to the correct location.

Circularity Check

1 steps flagged · score 4.0 of 10

Core n_e and mass-loading measurements are independent of the FFB framework, but the claimed FFB consistency is obtained by inverting the paper's own Eq. 8 and is therefore a self-consistency check rather than a model prediction.

  1. fitted input called prediction [Methods, 'FFB-model prediction and star-formation efficiency', Eqs. 7–8; main-text Fig. 3 discussion and 'Efficient feedback after a recent starburst' section]
    "For Gz9p3, Equation 8 is inverted directly: the observed loading constrains ε for the adopted f_burst and η_h, while M⋆ is used only to associate the solution with a halo mass. ... the FFB models with a star-formation efficiency (ε) ranging from 0.1 to 0.5 can reproduce the apparent outflow mass loading measured in Gz9p3"

    Equation 8 defines the apparent cool-phase loading as η_app = (ε^{-1} − 0.8 − η_h)/f_burst after adopting f_burst = 0.1 and η_h = 0.3. The paper then inverts this same equation to infer ε from the measured η_app. Therefore the green model region in Fig. 3 must contain the measured point whenever the inverted ε falls in the sampled 0.1–0.5 range; the agreement is a test of the adopted f_burst and η_h, not an independent FFB prediction. The paper partially acknowledges this ('a physically motivated constraint within the FFB framework rather than a unique determination'), but the main-text wording 'FFB models ... can reproduce' presents the inversion as independent support.

full rationale

The central quantitative derivation — electron density from CII/CII* and SiII/SiII* fine-structure ratios using CHIANTI atomic data, and the resulting mass-loading factor from Eq. 2 — is self-contained and does not reduce to its inputs. The density and η values would stand or fall on the spectral decomposition of the CII 1334/CII* 1335 blend, which is an interpretation/robustness issue, not a circularity in the paper's deductive chain. The DLA spatial gradient, escape-velocity comparison, and [OIII] decomposition are likewise independent analyses. The only substantive circular step is the FFB consistency argument: the model curve is generated from Eq. 8 and then Eq. 8 is inverted to infer ε from the observed η, so the 'reproduction' is guaranteed by construction within the sampled ε range. Because this circular step concerns a secondary interpretation and not the independent n_e/η measurement, a moderate score rather than a high one is appropriate.

Assumptions & free parameters 9 free parameters · 6 assumptions · 0 invented entities

The core measurement of n_e and eta is largely self-contained and does not invoke new physical entities. The interpretive FFB analysis, however, depends on several adopted parameters (f_burst, eta_h, halo mass, correction factors) and on the assumed CII* decomposition, so the ledger is dominated by modeling assumptions rather than by new postulates.

free parameters (9)
  • T_e (electron temperature of cool outflow) = 10^4 K (fiducial)
    Assumed for the CHIANTI collisional excitation balance; varying to 1.5x10^4 and 2x10^4 K shifts log n_e by +0.09 and +0.20 dex, smaller than the statistical uncertainty.
  • f_burst (ratio of current to burst SFR) = 0.1
    Adopted from the reconstructed SFH of Chen et al. 2026; in Eq. 8 it scales the apparent cool-phase loading by 1/f_burst and directly sets the inferred epsilon.
  • eta_h (hot-phase mass loading) = 0.3
    Adopted from Strickland and Heckman (2009) for M82; splits the FFB wind into hot and cool phases and shifts the inferred epsilon.
  • Halo mass range = log M_h/Msun = 10.8 to 11.5, fiducial 11.0
    Not directly measured; derived from abundance matching and clustering. Sets the escape-velocity range and the FFB domain in Fig. 3.
  • x_HII (ionized fraction of outflow hydrogen) = 1 (fiducial)
    Chosen to minimize the inferred total hydrogen density and hence give a conservative lower limit on the mass outflow rate.
  • A (projected outflow area) = 0.8 x MSA slit area
    Adopted from the multi-band imaging morphology; directly multiplies Mdot. Not derived from a fit and has no assigned uncertainty.
  • N_HI per sightline (DLA columns) = log N_HI/cm^-2 about 21.6 to 22.1
    Fitted in the joint DLA model. The absolute scale is degenerate with the IGM parameters, so the spatial gradient is the robust output, not the normalization.
  • x_HI and R_ion (IGM damping-wing parameters) = x_HI = 0.38 (+0.09 -0.08), R_ion = 0.12 (+0.12 -0.08) Mpc
    Fitted with uniform priors and shared across the four sightlines; they partially set the absolute N_HI scale.
  • Bipolar and neutral correction factors = 2x (bipolar) and 2x (neutral mass equal to ionized)
    Ad hoc multipliers applied to the one-sided ionized eta for the simulation comparison. No uncertainties are assigned, and the neutral fraction is not measured.
assumptions (6)
  • domain assumption The excess absorption near CII 1334 is primarily CII* 1335 rather than an additional CII velocity component
    Methods, 'Fine-structure absorption and electron density'. Load-bearing for the n_e measurement; the alternative is argued unlikely but cannot be ruled out at R~1000.
  • domain assumption Photoionization with log U greater than -3 sets the outflow radius upper limit
    Methods, 'Physical scale of the outflows'. Guides R less than 5 kpc; if the HIS gas is shock-dominated, the limit does not apply.
  • domain assumption Uniform-flow model with gas crossing the projected continuum-emitting area
    Methods, Eq. 2. Assumes the measured density and velocity are representative of all gas crossing 4/5 of the slit area; clumping would reduce the true mass flux.
  • standard math Case B recombination and Kennicutt H-alpha SFR calibration with Chabrier IMF
    Converts H-beta luminosity to SFR; adopted from Chen et al. 2026 with negligible dust attenuation.
  • domain assumption Truncated isothermal sphere for the escape-velocity estimate
    Methods, Eq. 6. Neglects the baryonic potential, which would raise v_esc, and depends on the adopted halo mass range.
  • domain assumption M_star approximately f_b * epsilon * M_h mapping for the FFB display
    Methods, 'FFB mapping and momentum transfer'. Used to place the model region in the (M*, eta) plane; not needed for the central measurement.

how reviews work

0 comments
Cite this review

Pith. "Pith review of An emerging baryon cycle in a galaxy 500 million years after the Big Bang." pith.science (2026). https://pith.science/paper/YZTRNTDQ

@misc{pith2026260809813,
  author       = {Pith},
  title        = {Pith review of: An emerging baryon cycle in a galaxy 500 million years after the Big Bang},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YZTRNTDQ}},
  note         = {Machine review of arXiv:2608.09813}
}
abstract

The emergence of stellar feedback as a regulator of galaxy growth marks a fundamental transition in cosmic history. At early times, rapid gas accretion and collapse may induce intense star formation before feedback becomes effective, producing feedback-free starbursts. When and how such bursts subsequently develop into self-regulated baryon cycles remain observationally unknown. Here we show that Gz9p3, a merging galaxy at $z=9.311$, is caught in this transition only 500 million years after the Big Bang. Deep JWST spectroscopy reveals a substantial neutral-gas reservoir along its merger-driven tidal structure and a multiphase outflow. Fine-structure absorption provides the first direct measurement of the electron density of the cool outflowing gas at high redshift ($\approx\,17\,{\rm cm^{-3}}$), yielding a mass-loading factor among the highest yet measured for galaxies of comparable stellar mass. The emergence of such efficient feedback after an intense burst is consistent with the delayed onset of feedback expected in feedback-free starburst models. The cool outflowing gas is unlikely to escape the host halo, implying that much of this metal-enriched material may remain available for future recycling through the circumgalactic medium. Gz9p3 therefore provides an early view of a baryon cycle being established through the interplay of merger-driven gas redistribution, bursty star formation and stellar feedback, suggesting that feedback-regulated recycling was already shaping galaxy growth during the epoch of reionization.

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

86 extracted references · 22 canonical work pages

  1. [1]

    Tumlinson, J., Peeples, M.S., Werk, J.K.: The Circumgalactic Medium. Ann. Rev. Astron. Astrophys.55(1), 389–432 (2017) https://doi.org/10.1146/ annurev-astro-091916-055240 arXiv:1709.09180 [astro-ph.GA]

    arXiv 2017

  2. [2]

    Dekel, A., Sarkar, K.C., Birnboim, Y., Mandelker, N., Li, Z.: Efficient formation of massive galaxies at cosmic dawn by feedback-free starbursts. Mon. Not. Roy. Astron. Soc.523(3), 3201–3218 (2023) https://doi.org/10.1093/mnras/stad1557 arXiv:2303.04827 [astro-ph.GA] 9

    arXiv 2023

  3. [3]

    Li, Z., Dekel, A., Sarkar, K.C., Aung, H., Giavalisco, M., Mandelker, N., Tac- chella, S.: Feedback-free starbursts at cosmic dawn: Observable predictions for JWST. Astron. Astrophys.690, 108 (2024) https://doi.org/10.1051/0004-6361/ 202348727 arXiv:2311.14662 [astro-ph.GA]

    arXiv 2024

  4. [4]

    A massive interacting galaxy 510 million years after the Big Bang

    Boyett, K., Trenti, M., Leethochawalit, N., Calabr´ o, A., Metha, B., Roberts- Borsani, G., Dalmasso, N., Yang, L., Santini, P., Treu, T., Jones, T., Henry, A., Mason, C.A., Morishita, T., Nanayakkara, T., Roy, N., Wang, X., Fontana, A., Merlin, E., Castellano, M., Paris, D., Bradaˇ c, M., Malkan, M., Marchesini, D., Mascia, S., Glazebrook, K., Pentericci...

    work page Pith review arXiv 2024

  5. [5]

    The Open Journal of Astrophysics9, 56033 (2026) https://doi.org/10.33232/001c.156033 arXiv:2505.11263 [astro-ph.GA]

    Naidu, R.P., Oesch, P.A., Brammer, G., Weibel, A., Li, Y., Matthee, J., Chisolm, J., Pollock, C.L., Heintz, K.E., Johnson, B.D., Shen, X., Hviding, R.E., Leja, J., Tacchella, S., Ganguly, A., Witten, C., Atek, H., Belli, S., Bose, S., Bouwens, R., Dayal, P., Decarli, R., de Graaff, A., Fudamoto, Y., Giovinazzo, E., Greene, J.E., Illingworth, G., Inoue, A....

    arXiv 2026

  6. [6]

    Astrophys

    Harikane, Y., Ouchi, M., Oguri, M., Ono, Y., Nakajima, K., Isobe, Y., Umeda, H., Mawatari, K., Zhang, Y.: A Comprehensive Study of Galaxies at z 9-16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch. Astrophys. J., Suppl. Ser. 265(1), 5 (2023) https://doi.org/10.3847/1538-4365/a...

    arXiv 2023

  7. [7]

    Donnan, C.T., McLeod, D.J., Dunlop, J.S., McLure, R.J., Carnall, A.C., Begley, R., Cullen, F., Hamadouche, M.L., Bowler, R.A.A., Magee, D., McCracken, H.J., Milvang-Jensen, B., Moneti, A., Targett, T.: The evolution of the galaxy UV luminosity function at redshifts z = 8 - 15 from deep JWST and ground-based near-infrared imaging. Mon. Not. Roy. Astron. So...

    arXiv 2023

  8. [8]

    Astrophys

    Finkelstein, S.L., Leung, G.C.K., Bagley, M.B., Dickinson, M., Ferguson, H.C., Papovich, C., Akins, H.B., Arrabal Haro, P., Dav´ e, R., Dekel, A., Kartaltepe, J.S., Kocevski, D.D., Koekemoer, A.M., Pirzkal, N., Somerville, R.S., Yung, L.Y.A., Amor ´ ın, R.O., Backhaus, B.E., Behroozi, P., Bisigello, L., Bromm, V., Casey, C.M., Ch´ avez Ortiz, ´O.A., Cheng...

    arXiv 2024

Show all 86 references
  1. [9]

    Sun, G., Faucher-Gigu` ere, C.-A., Hayward, C.C., Shen, X.: Seen and unseen: bursty star formation and its implications for observations of high-redshift galax- ies with JWST. Mon. Not. Roy. Astron. Soc.526(2), 2665–2672 (2023) https: //doi.org/10.1093/mnras/stad2902 arXiv:230...

    2023 arXiv

  2. [10]

    Astrophys

    Leitherer, C., Schaerer, D., Goldader, J.D., Delgado, R.M.G., Robert, C., Kune, D.F., de Mello, D.F., Devost, D., Heckman, T.M.: Starburst99: Synthesis Models for Galaxies with Active Star Formation. Astrophys. J., Suppl. Ser.123(1), 3–40 (1999) https://doi.org/10.1086/313233 ...

    1999 arXiv

  3. [11]

    Hopkins, P.F., Quataert, E., Murray, N.: Stellar feedback in galaxies and the origin of galaxy-scale winds. Mon. Not. Roy. Astron. Soc.421(4), 3522–3537 (2012) https://doi.org/10.1111/j.1365-2966.2012.20593.x arXiv:1110.4638 [astro- ph.CO]

    2012

  4. [12]

    Chevance, M., Kruijssen, J.M.D., Hygate, A.P.S., Schruba, A., Longmore, S.N., Groves, B., Henshaw, J.D., Herrera, C.N., Hughes, A., Jeffreson, S.M.R., Lang, P., Leroy, A.K., Meidt, S.E., Pety, J., Razza, A., Rosolowsky, E., Schinnerer, E., Bigiel, F., Blanc, G.A., Emsellem, E....

    2020 arXiv

  5. [13]

    Eldridge, J.J., Stanway, E.R.: New Insights into the Evolution of Mas- sive Stars and Their Effects on Our Understanding of Early Galaxies. Ann. Rev. Astron. Astrophys.60, 455–494 (2022) https://doi.org/10.1146/ annurev-astro-052920-100646 arXiv:2202.01413 [astro-ph.GA]

    2022 arXiv

  6. [14]

    Astrophys

    Heckman, T.M., Armus, L., Miley, G.K.: On the Nature and Implications of Starburst-driven Galactic Superwinds. Astrophys. J., Suppl. Ser.74, 833 (1990) https://doi.org/10.1086/191522

    1990 doi

  7. [15]

    Veilleux, S., Cecil, G., Bland-Hawthorn, J.: Galactic Winds. Ann. Rev. Astron. Astrophys.43(1), 769–826 (2005) https://doi.org/10.1146/annurev.astro.43. 072103.150610 arXiv:astro-ph/0504435 [astro-ph]

    2005 arXiv

  8. [16]

    Astrophys

    Steidel, C.C., Erb, D.K., Shapley, A.E., Pettini, M., Reddy, N., Bogosavljevi´ c, 11 M., Rudie, G.C., Rakic, O.: The Structure and Kinematics of the Circumgalactic Medium from Far-ultraviolet Spectra of z ˜= 2-3 Galaxies. Astrophys. J.717(1), 289–322 (2010) https://doi.org/10....

    2010 arXiv

  9. [17]

    Galaxies6(4), 138 (2018) https://doi.org/10.3390/ galaxies6040138 arXiv:1812.05184 [astro-ph.GA]

    Rupke, D.S.N.: A Review of Recent Observations of Galactic Winds Driven by Star Formation. Galaxies6(4), 138 (2018) https://doi.org/10.3390/ galaxies6040138 arXiv:1812.05184 [astro-ph.GA]

    2018 arXiv

  10. [18]

    Astrophys

    Rudie, G.C., Steidel, C.C., Pettini, M., Trainor, R.F., Strom, A.L., Hummels, C.B., Reddy, N.A., Shapley, A.E.: Column Density, Kinematics, and Thermal State of Metal-bearing Gas within the Virial Radius of z∼2 Star-forming Galax- ies in the Keck Baryonic Structure Survey. Ast...

    2019 arXiv

  11. [19]

    Astrophys

    Cooper, R.A., Caputi, K.I., Iani, E., Rinaldi, P., Desprez, G., Navarro-Carrera, R.: High-velocity Outflows in [O III] Emitters at 2.5 ¡ z ¡ 9 from JWST NIRSpec Medium-resolution Spectroscopy. Astrophys. J.994(1), 102 (2025) https://doi. org/10.3847/1538-4357/ae0580 arXiv:2502...

    2025 arXiv

  12. [20]

    Astrophys

    Xu, X., Henry, A., Heckman, T., Carr, C., Strom, A.L., Jones, T., Berg, D.A., Chisholm, J., Erb, D., James, B.L., Jaskot, A., Martin, C.L., Mingozzi, M., Senchyna, P., Roy, N., Scarlata, C., Stark, D.P.: Shining a Light on the Con- nections between Galactic Outflows Seen in Ab...

    2025 arXiv

  13. [21]

    Carniani, S., Venturi, G., Parlanti, E., de Graaff, A., Maiolino, R., Arribas, S., Bonaventura, N., Boyett, K., Bunker, A.J., Cameron, A.J., Charlot, S., Cheval- lard, J., Curti, M., Curtis-Lake, E., Eisenstein, D.J., Giardino, G., Hausen, R., Kumari, N., Maseda, M.V., Nelson,...

    2024 arXiv

  14. [22]

    arXiv e-prints, 2606–08782 (2026) https://doi.org/10.48550/arXiv.2606.08782 arXiv:2606.08782 [astro-ph.GA]

    Nakane, M., Ouchi, M.: JWST Absorption-Line Analysis of UV-Bright Galaxies atz= 7.2−10.6: Early Chemical Enrichment Traced by C, O, Mg, Al, Si, and Fe. arXiv e-prints, 2606–08782 (2026) https://doi.org/10.48550/arXiv.2606.08782 arXiv:2606.08782 [astro-ph.GA]

    2026 doi arXiv

  15. [23]

    arXiv e-prints, 2604–21516 (2026) https://doi.org/10.48550/arXiv.2604.21516 arXiv:2604.21516 [astro-ph.GA] 12

    Chen, Z., Stark, D.P., Mason, C.A., Plat, A., Gelli, V., Senchyna, P., Keerthi Vasan G., C., Endsley, R., Tang, M., Topping, M.W., Whitler, L.: SPURS: Bursty Star Formation in an Extremely Luminous Weak Emission Line Galaxy atz= 9.3. arXiv e-prints, 2604–21516 (2026) https://d...

    2026 doi arXiv

  16. [24]

    Astrophys

    Du, X., Shapley, A.E., Reddy, N.A., Jones, T., Stark, D.P., Steidel, C.C., Strom, A.L., Rudie, G.C., Erb, D.K., Ellis, R.S., Pettini, M.: The Redshift Evo- lution of Rest-UV Spectroscopic Properties in Lyman-break Galaxies at z∼ 2-4. Astrophys. J.860(1), 75 (2018) https://doi....

    2018 arXiv

  17. [25]

    Brazzini, M., D’Odorico, V., Bischetti, M., Feruglio, C., Cupani, G., Becker, G., Tripodi, R.: Multi-phase investigation of outflows in the circumgalactic and inter- stellar media of luminous quasars at z∼5. Astron. Astrophys.698, 145 (2025) https://doi.org/10.1051/0004-6361/2...

    2025 arXiv

  18. [26]

    Astrophys

    Kraemer, S.B., Crenshaw, D.M., Gabel, J.R.: STIS Echelle Observations of the Intrinsic UV Absorption in the Seyfert 1 Galaxy NGC 3783. Astrophys. J.557(1), 30–38 (2001) https://doi.org/10.1086/321619 arXiv:astro-ph/0104303 [astro-ph]

    2001 arXiv

  19. [27]

    Rickard, M.J., Hainich, R., Hamann, W.-R., Oskinova, L.M., Prinja, R.K., Ramachandran, V., Pauli, D., Todt, H., Sander, A.A.C., Shenar, T., Chu, Y.-H., Gallagher, J.S.: Stellar wind properties of the nearly complete sample of O stars in the low metallicity young star cluster N...

    2022 arXiv

  20. [28]

    Chen, H.-Z., Li, Z., Dekel, A., Yao, Z., Mandelker, N., Kang, X.: Feedback-free star formation in clusters within a galaxy simulated at high resolution in cosmic dawn. Mon. Not. Roy. Astron. Soc.550(2), 1214 (2026) https://doi.org/10.1093/ mnras/stag1214 arXiv:2606.12605 [astro-ph.GA]

    2026 arXiv

  21. [29]

    Fluetsch, A., Maiolino, R., Carniani, S., Marconi, A., Cicone, C., Bourne, M.A., Costa, T., Fabian, A.C., Ishibashi, W., Venturi, G.: Cold molecular outflows in the local Universe and their feedback effect on galaxies. Mon. Not. Roy. Astron. Soc.483(4), 4586–4614 (2019) https:...

    2019 arXiv

  22. [30]

    Fluetsch, A., Maiolino, R., Carniani, S., Arribas, S., Belfiore, F., Bellocchi, E., Cazzoli, S., Cicone, C., Cresci, G., Fabian, A.C., Gallagher, R., Ishibashi, W., Mannucci, F., Marconi, A., Perna, M., Sturm, E., Venturi, G.: Properties of the multiphase outflows in local (ul...

    2021 arXiv

  23. [31]

    Davies, R.L., Belli, S., Park, M., Mendel, J.T., Johnson, B.D., Conroy, C., Ben- ton, C., Bugiani, L., Emami, R., Leja, J., Li, Y., Maheson, G., Mathews, E.P., Naidu, R.P., Nelson, E.J., Tacchella, S., Terrazas, B.A., Weinberger, R.: JWST reveals widespread AGN-driven neutral ...

    2024 arXiv

  24. [32]

    Nelson, D., Pillepich, A., Springel, V., Pakmor, R., Weinberger, R., Genel, S., Torrey, P., Vogelsberger, M., Marinacci, F., Hernquist, L.: First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feed- back. Mon. Not. Roy. Astron. Soc.490...

    2019 arXiv

  25. [33]

    Pandya, V., Fielding, D.B., Angl´ es-Alc´ azar, D., Somerville, R.S., Bryan, G.L., Hayward, C.C., Stern, J., Kim, C.-G., Quataert, E., Forbes, J.C., Faucher- Gigu` ere, C.-A., Feldmann, R., Hafen, Z., Hopkins, P.F., Kereˇ s, D., Murray, N., Wetzel, A.: Characterizing mass, mom...

    2021 arXiv

  26. [34]

    Astrophys

    Heckman, T.M., Alexandroff, R.M., Borthakur, S., Overzier, R., Leitherer, C.: The Systematic Properties of the Warm Phase of Starburst-Driven Galactic Winds. Astrophys. J.809(2), 147 (2015) https://doi.org/10.1088/0004-637X/ 809/2/147 arXiv:1507.05622 [astro-ph.GA]

    2015 arXiv

  27. [35]

    Chisholm, J., Tremonti, C.A., Leitherer, C., Chen, Y.: The mass and momentum outflow rates of photoionized galactic outflows. Mon. Not. Roy. Astron. Soc.469(4), 4831–4849 (2017) https://doi.org/10.1093/mnras/stx1164 arXiv:1702.07351 [astro-ph.GA]

    2017 arXiv

  28. [36]

    The Properties of Starburst- driven Warm Ionized Outflows

    Xu, X., Heckman, T., Henry, A., Berg, D.A., Chisholm, J., James, B.L., Martin, C.L., Stark, D.P., Aloisi, A., Amor ´ ın, R.O., Arellano-C´ ordova, K.Z., Bordoloi, R., Charlot, S., Chen, Z., Hayes, M., Mingozzi, M., Sugahara, Y., Kewley, L.J., Ouchi, M., Scarlata, C., Steidel, ...

    2022 arXiv

  29. [37]

    van der Hulst, J.M.: The kinematics and distribution of neutral hydrogen in the interacting galaxy pair NGC 4038/39. Astron. Astrophys.71, 131–140 (1979)

    1979

  30. [38]

    Nature372(6506), 530–532 (1994) https://doi.org/ 10.1038/372530a0

    Yun, M.S., Ho, P.T.P., Lo, K.Y.: A high-resolution image of atomic hydrogen in the M81 group of galaxies. Nature372(6506), 530–532 (1994) https://doi.org/ 10.1038/372530a0

    1994 doi

  31. [39]

    Hibbard, J.E., van Gorkom, J.H.: HI, HII, and R-Band Observations of a Galac- tic Merger Sequence. Astron. J111, 655 (1996) https://doi.org/10.1086/117815 arXiv:astro-ph/9512035 [astro-ph]

    1996 arXiv

  32. [40]

    The Antennae

    Hibbard, J.E., van der Hulst, J.M., Barnes, J.E., Rich, R.M.: High-Resolution H I Mapping of NGC 4038/39 (“The Antennae”) and Its Tidal Dwarf Galaxy Candidates. Astron. J122(6), 2969–2992 (2001) https://doi.org/10.1086/324102 arXiv:astro-ph/0110581 [astro-ph] 14

    2001 arXiv

  33. [41]

    Ancillary data and additional JWST observations

    Duc, P.-A., Renaud, F.: Tides in Colliding Galaxies. In: Souchay, J., Mathis, S., Tokieda, T. (eds.) Lecture Notes in Physics, Berlin Springer Verlag vol. 861, p. 327 (2013). https://doi.org/10.1007/978-3-642-32961-6 9 15 Methods Observations and data reduction Gz9p3 is locate...

    2013 doi

  34. [42]

    arXiv e-prints, 2604–03563 (2026) https://doi.org/10.48550/arXiv.2604.03563 arXiv:2604.03563 [astro-ph.GA]

    Tang, M., Stark, D.P., Mason, C.A., Chen, Z., Katz, H., Gronke, M., Furtak, L.J., Chang, S.-J., Matthee, J., Whitler, L., Zitrin, A., Endsley, R., Gelli, V., Roy- chowdhury, T., Senchyna, P., Topping, M.W., Zhang, M.: SPURS: Evidence for Clumpy Neutral Envelopes and Ionized IG...

    2026 doi arXiv

  35. [43]

    Astrophys

    Bezanson, R., Labbe, I., Whitaker, K.E., Leja, J., Price, S.H., Franx, M., Bram- mer, G., Marchesini, D., Zitrin, A., Wang, B., Weaver, J.R., Furtak, L.J., Atek, H., Coe, D., Cutler, S.E., Dayal, P., van Dokkum, P., Feldmann, R., F¨ orster Schreiber, N.M., Fujimoto, S., Geha, ...

    2024 arXiv

  36. [44]

    https://doi.org/10.5281/zenodo

    Brammer, G.: msaexp: NIRSpec Analyis Tools. https://doi.org/10.5281/zenodo. 7299500 . https://github.com/gbrammer/msaexp

    doi

  37. [45]

    Astronomy and Astrophysics Supplement Series125, 149–173 (1997) https://doi.org/10.1051/aas:1997368

    Dere, K.P., Landi, E., Mason, H.E., Monsignori Fossi, B.C., Young, P.R.: CHI- ANTI - an atomic database for emission lines. Astronomy and Astrophysics Supplement Series125, 149–173 (1997) https://doi.org/10.1051/aas:1997368

    1997 doi

  38. [46]

    Del Zanna, G., Dere, K.P., Young, P.R., Landi, E.: CHIANTI—An Atomic Database for Emission Lines. XVI. Version 10, Further Extensions. Astrophys. J. 909(1), 38 (2021) https://doi.org/10.3847/1538-4357/abd8ce arXiv:2011.05211 [physics.atom-ph]

    2021 arXiv

  39. [47]

    Dere, K.P., Del Zanna, G., Young, P.R., Landi, E.: CHIANTI-An Atomic Database for Emission Lines. XVII. Version 10.1: Revised Ionization and Recom- bination Rates and Other Updates. Astrophys. J., Suppl. Ser.268(2), 52 (2023) https://doi.org/10.3847/1538-4365/acec79 arXiv:2305...

    2023 arXiv

  40. [48]

    Mao, H., Li, J.-T., Yu, X., Qu, Z., Liu, W., Ji, L.: Probing the He II Reionization ERa via Absorbing C IV Historical Yield (HIERACHY). IV. A Complex Red- shifted Absorption System Intrinsic to Quasar. Astrophys. J.994(1), 18 (2025) https://doi.org/10.3847/1538-4357/ae0a0f arX...

    2025

  41. [49]

    Astrophys

    Gazagnes, S., Mauerhofer, V., Berg, D.A., Blaizot, J., Verhamme, A., Garel, T., Erb, D.K., Arellano-C´ ordova, K.Z., Brinchmann, J., Chisholm, J., Hayes, M., Henry, A., James, B.L., Jaskot, A., Jurlin, N., Martin, C.L., Maseda, M., Scar- lata, C., Skillman, E.D., Wilkins, S.M....

    2023 arXiv

  42. [50]

    Xu, X., Heckman, T., Henry, A., Berg, D.A., Chisholm, J., James, B.L., Mar- tin, C.L., Stark, D.P., Hayes, M., Arellano-C´ ordova, K.Z., Carr, C., Huberty, M., Mingozzi, M., Scarlata, C., Sugahara, Y.: CLASSY. VI. The Density, Struc- ture, and Size of Absorption-line Outflows ...

    2023 arXiv

  43. [51]

    Astrophys

    Wang, B., Heckman, T.M., Zhu, G., Norman, C.A.: A Systematic Study of Galac- tic Outflows via Fluorescence Emission: Implications for Their Size and Structure. Astrophys. J.894(2), 149 (2020) https://doi.org/10.3847/1538-4357/ab88b4 arXiv:2004.06105 [astro-ph.GA]

    2020 arXiv

  44. [52]

    Luridiana, V., Morisset, C., Shaw, R.A.: PyNeb: a new tool for analyzing emission lines. I. Code description and validation of results. Astron. Astrophys.573, 42 (2015) https://doi.org/10.1051/0004-6361/201323152 arXiv:1410.6662 [astro- ph.IM]

    2015 arXiv

  45. [53]

    Chisholm, J., Tremonti, C.A., Leitherer, C., Chen, Y., Wofford, A.: Shin- ing a light on galactic outflows: photoionized outflows. Mon. Not. Roy. Astron. Soc.457(3), 3133–3161 (2016) https://doi.org/10.1093/mnras/stw178 arXiv:1601.05090 [astro-ph.GA]

    2016 arXiv

  46. [54]

    Jr.: Star Formation in Galaxies Along the Hubble Sequence

    Kennicutt, R.C. Jr.: Star Formation in Galaxies Along the Hubble Sequence. Ann. Rev. Astron. Astrophys.36, 189–232 (1998) https://doi.org/10.1146/annurev. astro.36.1.189 arXiv:astro-ph/9807187 [astro-ph]

    1998 arXiv

  47. [55]

    Chabrier, G.: Galactic Stellar and Substellar Initial Mass Function. Publ. Astron. Soc. Pac.115(809), 763–795 (2003) https://doi.org/10.1086/376392 arXiv:astro- ph/0304382 [astro-ph]

    2003

  48. [56]

    Behroozi, P., Wechsler, R.H., Hearin, A.P., Conroy, C.: UNIVERSEMACHINE: The correlation between galaxy growth and dark matter halo assembly from z = 0-10. Mon. Not. Roy. Astron. Soc.488(3), 3143–3194 (2019) https://doi.org/10. 1093/mnras/stz1182 arXiv:1806.07893 [astro-ph.GA]

    2019 arXiv

  49. [57]

    Harikane, Y., Ouchi, M., Ono, Y., Saito, S., Behroozi, P., More, S., Shimasaku, K., Toshikawa, J., Lin, Y.-T., Akiyama, M., Coupon, J., Komiyama, Y., Konno, A., Lin, S.-C., Miyazaki, S., Nishizawa, A.J., Shibuya, T., Silverman, J.: GOL- DRUSH. II. Clustering of galaxies at z∼4...

    2018 arXiv

  50. [58]

    arXiv e-prints, 2607–29589 (2026) https://doi.org/10.48550/arXiv.2607

    Aditya, K., Sarkar, K.C.: A Massive Galaxy at the Edge of Feedback-Free Effi- ciency. arXiv e-prints, 2607–29589 (2026) https://doi.org/10.48550/arXiv.2607. 29589 arXiv:2607.29589 [astro-ph.GA]

    2026 doi arXiv

  51. [59]

    Astrophys

    Bryan, G.L., Norman, M.L.: Statistical Properties of X-Ray Clusters: Analytic and Numerical Comparisons. Astrophys. J.495(1), 80–99 (1998) https://doi. org/10.1086/305262 arXiv:astro-ph/9710107 [astro-ph]

    1998 arXiv

  52. [60]

    Astrophys

    Martin, C.L.: Mapping Large-Scale Gaseous Outflows in Ultraluminous Galax- ies with Keck II ESI Spectra: Variations in Outflow Velocity with Galactic Mass. Astrophys. J.621(1), 227–245 (2005) https://doi.org/10.1086/427277 arXiv:astro-ph/0410247 [astro-ph]

    2005 arXiv

  53. [61]

    Astrophys

    Chisholm, J., Tremonti, C.A., Leitherer, C., Chen, Y., Wofford, A., Lundgren, B.: Scaling Relations Between Warm Galactic Outflows and Their Host Galaxies. Astrophys. J.811(2), 149 (2015) https://doi.org/10.1088/0004-637X/811/2/149 arXiv:1412.2139 [astro-ph.GA]

    2015 arXiv

  54. [62]

    Astrophys

    Strickland, D.K., Heckman, T.M.: Supernova Feedback Efficiency and Mass Loading in the Starburst and Galactic Superwind Exemplar M82. Astrophys. J.697(2), 2030–2056 (2009) https://doi.org/10.1088/0004-637X/697/2/2030 arXiv:0903.4175 [astro-ph.CO]

    2009 arXiv

  55. [63]

    Astro- phys

    Wakker, B.P., Savage, B.D., Fox, A.J., Benjamin, R.A., Shapiro, P.R.: Characterizing Transition Temperature Gas in the Galactic Corona. Astro- phys. J.749(2), 157 (2012) https://doi.org/10.1088/0004-637X/749/2/157 arXiv:1202.5973 [astro-ph.GA]

    2012 arXiv

  56. [64]

    Lehner, N., Howk, J.C.: Highly ionized plasma in the Large Magellanic Cloud: evidence for outflows and a possible galactic wind. Mon. Not. Roy. Astron. Soc.377(2), 687–704 (2007) https://doi.org/10.1111/j.1365-2966.2007.11631.x arXiv:astro-ph/0702427 [astro-ph]

    2007

  57. [65]

    Astrophys

    Shull, J.M., Stevans, M., Danforth, C., Penton, S.V., Lockman, F.J., Arav, N.: HST/COS Observations of Galactic High-velocity Clouds: Four Active Galactic Nucleus Sight Lines through Complex C. Astrophys. J.739(2), 105 (2011) https: //doi.org/10.1088/0004-637X/739/2/105 arXiv:...

    2011 arXiv

  58. [66]

    Lehner, N., Howk, J.C., Prochaska, J.X., Wolfe, A.M.: Probing feedback in proto- galaxies: multiphase gas in a DLA at z ˜2.4. Mon. Not. Roy. Astron. Soc.390(1), 2–20 (2008) https://doi.org/10.1111/j.1365-2966.2008.13692.x arXiv:0807.0930 [astro-ph]

    2008

  59. [67]

    Astrophys

    Nielsen, N.M., Kacprzak, G.G., Pointon, S.K., Murphy, M.T., Churchill, C.W., Dav´ e, R.: The CGM at Cosmic Noon with KCWI: Outflows from a Star-forming Galaxy at z = 2.071. Astrophys. J.904(2), 164 (2020) https://doi.org/10.3847/ 1538-4357/abc561 arXiv:2002.08516 [astro-ph.GA] 29

    2020 arXiv

  60. [68]

    Evidence for both circum- burst plasma and outflowing interstellar gas

    Fox, A.J., Ledoux, C., Vreeswijk, P.M., Smette, A., Jaunsen, A.O.: High-ion absorption in seven GRB host galaxies at z = 2-4. Evidence for both circum- burst plasma and outflowing interstellar gas. Astron. Astrophys.491(1), 189–207 (2008) https://doi.org/10.1051/0004-6361:2008...

    2008 arXiv

  61. [69]

    Astrophys

    Heckman, T.M., Norman, C.A., Strickland, D.K., Sembach, K.R.: On the Physical Origin of O VI Absorption-Line Systems. Astrophys. J.577(2), 691–700 (2002) https://doi.org/10.1086/342232 arXiv:astro-ph/0205556 [astro-ph]

    2002 arXiv

  62. [70]

    Astrophys

    Gnat, O., Sternberg, A.: Time-dependent Ionization in Radiatively Cooling Gas. Astrophys. J., Suppl. Ser.168(2), 213–230 (2007) https://doi.org/10.1086/ 509786 arXiv:astro-ph/0608181 [astro-ph]

    2007 arXiv

  63. [71]

    Astrophys

    Borkowski, K.J., Balbus, S.A., Fristrom, C.C.: Radiative Magnetized Thermal Conduction Fronts. Astrophys. J.355, 501 (1990) https://doi.org/10.1086/ 168784

    1990

  64. [72]

    Astrophys

    Slavin, J.D., Shull, J.M., Begelman, M.C.: Turbulent Mixing Layers in the Inter- stellar Medium of Galaxies. Astrophys. J.407, 83 (1993) https://doi.org/10. 1086/172494

    1993

  65. [73]

    Dopita, M.A., Sutherland, R.S.: Spectral Signatures of Fast Shocks. I. Low- Density Model Grid. Astrophys. J., Suppl. Ser.102, 161 (1996) https://doi.org/ 10.1086/192255

    1996 doi

  66. [74]

    30" 45" 26'00

    Slavin, J.D., Cox, D.P.: Completing the Evolution of Supernova Remnants and Their Bubbles. Astrophys. J.392, 131 (1992) https://doi.org/10.1086/171412 30 Acknowledgments.This paper is dedicated to the memory of Prof. Avishai Dekel, whose foundational contributions to galaxy ev...

    1992 doi

  67. [75]

    NoT e-sensitive diagnostic line is detected

    and calculate the ionic abundances withPyNeb[52]. NoT e-sensitive diagnostic line is detected. In particular, the 3σupper limit on [OIII]λ4363 implies onlyT e ≲6×10 4 K and is too weak to constrain the abundance. We therefore adoptT e = 10,000 K as a fiducial assumption rather...

    2002

  68. [76]

    Astrophys

    Suess, K.A., Weaver, J.R., Price, S.H., Pan, R., Wang, B., Bezanson, R., Bram- mer, G., Cutler, S.E., Labb´ e, I., Leja, J., Williams, C.C., Whitaker, K.E., Atek, H., Dayal, P., de Graaff, A., Feldmann, R., Franx, M., Fudamoto, Y., Fuji- moto, S., Furtak, L.J., Goulding, A.D.,...

    2024 arXiv

  69. [77]

    arXiv e-prints, 2603–24893 (2026) https://doi.org/10.48550/arXiv.2603.24893 arXiv:2603.24893 [astro-ph.GA]

    Zou, F., Gallo, E., Zuo, Z., Hodges-Kluck, E., Nguyen, D.D., Roberts-Borsani, G., Madau, P., Pacucci, F., Seth, A.C., Treu, T.: Revisiting the Claim for a Direct- Collapse Black Hole in UHZ1 atz= 10.05. arXiv e-prints, 2603–24893 (2026) https://doi.org/10.48550/arXiv.2603.2489...

    2026 doi

  70. [78]

    Astrophys

    Evans, I.N., Evans, J.D., Mart ´ ınez-Galarza, J.R., Miller, J.B., Primini, F.A., Azadi, M., Burke, D.J., Civano, F.M., D’Abrusco, R., Fabbiano, G., Graessle, D.E., Grier, J.D., Houck, J.C., Lauer, J., McCollough, M.L., Nowak, M.A., Plummer, D.A., Rots, A.H., Siemiginowska, A....

    2024 arXiv

  71. [79]

    arXiv e-prints, 2604–22460 (2026) https://doi.org/10.48550/ arXiv.2604.22460 arXiv:2604.22460 [astro-ph.GA]

    Bik, A., ´Alvarez-M´ arquez, J., Crespo G´ omez, A., Colina, L., P´ erez-Gonz´ alez, P.G., ¨Ostlin, G., Blanco Prieto, C., Melinder, J., Langeroodi, D., Wright, G., Algera, H.S.B., Boogaard, L.A., Caputi, K., Gillman, S., Greve, T., Hjorth, J., Iani, E., Kendrew, S., Labiano O...

    2026 doi arXiv

  72. [80]

    Treu, T., Roberts-Borsani, G., Bradac, M., Brammer, G., Fontana, A., Henry, A., Mason, C., Morishita, T., Pentericci, L., Wang, X., Acebron, A., Bagley, M., Bergamini, P., Belfiori, D., Bonchi, A., Boyett, K., Boutsia, K., Calabr´ o, A., Caminha, G.B., Castellano, M., Dressler...

    2022

  73. [81]

    Astrophys

    Johnson, B.D., Leja, J., Conroy, C., Speagle, J.S.: Stellar Population Inference with Prospector. Astrophys. J., Suppl. Ser.254(2), 22 (2021) https://doi.org/ 10.3847/1538-4365/abef67 arXiv:2012.01426 [astro-ph.GA]

    2021 arXiv

  74. [82]

    arXiv e-prints, 2606–13078 (2026) https://doi.org/10.48550/arXiv

    Pollock, C.L., Heintz, K.E., Rusta, E., Watson, D., Salvadori, S., Witten, C., Witstok, J., Koutsouridou, I., Gelli, V., Oesch, P.A., Brammer, G.B., Saccardi, A., Ito, K., Gottumukkala, R., Bergholt, D., Brooksby, K.R., Terp, C., Valentino, F.: Chemical signatures from the fir...

    2026 doi arXiv

  75. [83]

    Astrophys

    Rix, S.A., Pettini, M., Leitherer, C., Bresolin, F., Kudritzki, R.-P., Steidel, C.C.: Spectral Modeling of Star-forming Regions in the Ultraviolet: Stellar Metallicity Diagnostics for High-Redshift Galaxies. Astrophys. J.615(1), 98–117 (2004) https://doi.org/10.1086/424031 arX...

    2004 arXiv

  76. [84]

    Morton, D.C.: Atomic Data for Resonance Absorption Lines. III. Wavelengths Longward of the Lyman Limit for the Elements Hydrogen to Gallium. Astrophys. J., Suppl. Ser.149(1), 205–238 (2003) https://doi.org/10.1086/377639

    2003 doi

  77. [85]

    Kewley, L.J., Geller, M.J., Jansen, R.A.: [O II] as a Star Formation Rate Indicator. Astron. J127(4), 2002–2030 (2004) https://doi.org/10.1086/382723 arXiv:astro-ph/0401172 [astro-ph]

    2004 arXiv

  78. [86]

    Carniani, S., Marconi, A., Maiolino, R., Balmaverde, B., Brusa, M., Cano-D ´ ıaz, M., Cicone, C., Comastri, A., Cresci, G., Fiore, F., Feruglio, C., La Franca, F., Mainieri, V., Mannucci, F., Nagao, T., Netzer, H., Piconcelli, E., Risaliti, G., Schneider, R., Shemmer, O.: Ioni...

    2015 arXiv

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.