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arxiv: 2606.24085 · v1 · pith:FLJTHOPSnew · submitted 2026-06-23 · 🌌 astro-ph.GA

Radial gradients revealed by mutliscale outflows from down-the-barrel spectroscopy toward a quasar at redshift 3.4

Weimin Yi , Paola Rodriguez Hidalgo , Chen Chen , P. B. Hall , Zhicheng He , R. P. Easton , D. P. Schneider , W. N. Brandt
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Xue-Bing Wu Kai-Xing Lu Chuanjun Wang Yuanjie Feng
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Pith reviewed 2026-06-26 00:13 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords AGN feedbackquasar outflowsradial gradientsN V absorptionC IV absorptioncircumgalactic mediumdown-the-barrel spectroscopyredshift 3.4
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The pith

Quasar at z=3.4 shows radial N/C gradient in multiscale outflows

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

The paper examines multi-epoch down-the-barrel spectroscopy of a luminous quasar at redshift 3.409. It identifies three outflows expanding freely on nuclear to CGM scales. The absorption trough depths for N V and C IV exhibit opposite trends across these scales. This pattern supports a radial gradient in the nitrogen to carbon ratio. The observation implies a change from ejective to regulative AGN feedback as scale increases.

Core claim

Multi-epoch spectroscopy toward the quasar reveals multiscale outflows with radial gradients. Most strikingly, the trends of trough depth across three different-scale, freely expanding outflows are opposite between N V and C IV, regardless of the spectral normalization and short-term variability, leading to a tenable gradient of N/C and signaling a critical transition from ejective feedback on small scales to regulative feedback on large scales.

What carries the argument

The opposite trends in trough depth between N V and C IV across three different-scale outflows, interpreted as evidence for a radial N/C gradient.

If this is right

  • AGN feedback couples to the ISM and CGM differently at nuclear versus CGM scales.
  • The observed scale marks a shift from driving material outward to regulating galaxy evolution.
  • The data provide direct diagnostics for wind-ISM/CGM coupling in galaxy formation simulations.
  • The gradient is robust to choices of spectral normalization and short-term variability.
  • Such multiscale observations help close the gap between nuclear and large-scale feedback processes.

Where Pith is reading between the lines

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

  • Similar radial abundance gradients may appear in other luminous quasars at comparable redshifts.
  • The transition in feedback mode could influence how AGN suppress or trigger star formation at different radii.
  • Future integral-field spectroscopy could map whether the N/C change correlates with outflow velocity or density.
  • This pattern offers a concrete test for whether simulations produce the same scale-dependent abundance shift.

Load-bearing premise

That the opposite trough-depth trends between N V and C IV across the three scales arise from a genuine radial N/C gradient rather than from ionization variations, line blending, or differential saturation effects.

What would settle it

New spectra or models that reproduce the observed opposite trough-depth trends between N V and C IV without any change in N/C ratio, for instance by ionization or saturation effects alone.

Figures

Figures reproduced from arXiv: 2606.24085 by Chen Chen, Chuanjun Wang, D. P. Schneider, Kai-Xing Lu, Paola Rodriguez Hidalgo, P. B. Hall, R. P. Easton, Weimin Yi, W. N. Brandt, Xue-Bing Wu, Yuanjie Feng, Zhicheng He.

Figure 1
Figure 1. Figure 1: The near-IR and multi-epoch optical spectra of J0758, in which the expected positions and widths of the BAL, mini-BAL, NAL, and AAL are indicated by thick horizontal bars (each with O vi, Lyα+N v, Si iv, and C iv from left to right). The blue dotted/dashed lines denote the spectral error/continuum fit to the first spectrum. A systemic redshift of 3.409±0.001 was established from a combined analysis of the … view at source ↗
Figure 2
Figure 2. Figure 2: (A) Demonstration of the different short-term variability behaviors and long-term trends across different-type absorption troughs from the continuum+BEL normalized spectra. The deepest portion of each C iv trough (last row) is used as the benchmark to identify the corresponding Lyα, O vi, and N v troughs embedded in the Lyα forest from the spectrum at MJD=53674. Thin/thick blue lines refer to the individua… view at source ↗
Figure 3
Figure 3. Figure 3: Left: The CLOUDY solutions for the variable mini-BAL from the 1st/3rd (solid/dashed ellipses) epoch. Middle: The CLOUDY solutions for the variable NAL from the 1st/3rd epoch. Right: The two-zone solutions (pentagons) estimated from photoionization modeling via CLOUDY for the multiphase AAL that remains unchanged in REW over two decades. The dotted/dashed curves in each panel refer to the upper/lower limit … view at source ↗
Figure 4
Figure 4. Figure 4: Spectral decomposition for the complex emission around the Hβ emission. The broad Hβ (FWHM = 4780 km s−1 ) and narrow components (FWHM = 1240 km s−1 ) are displayed in red and cyan lines, respectively; the dashed line indicates the con￾tinuum and the blue line refers to the Fe ii component; the total fit is shown in green. Nσ in the bottom is the residual. perhaps episodic quasar winds, whose velocity, ele… view at source ↗
Figure 5
Figure 5. Figure 5: A cartoon illustration of the expansion for J0758 from a side view, in which the characteristic trough depth/width in C iv monotonically increases/decreases with decreasing velocity across these outflows. Variability timescale increases with distance, characteristic of an increasingly diluted gas density (see text). The innermost BAL moved out of our LOS along a curved path, causing a large velocity shift,… view at source ↗
read the original abstract

Active galactic nucleus(AGN) feedback is a key ingredient in galaxy formation models and simulations. From an observational point of view, however, the channels of AGN feedback coupling to the interstellar medium (ISM) and circumgalactic medium (CGM) and hence the impact on galaxy evolution, are largely uncertain and remain fiercely debated, due primarily to the huge gap from nuclear to CGM scales. Here we present multi-epoch, down-the-barrel spectroscopy toward a luminous quasar at $z=3.409$ over two decades, which reveals multiscale outflows expanding from nuclear to CGM scales along with characteristic radial gradients. Most strikingly, the trends of trough depth across three different-scale, freely expanding outflows are opposite between N V and C IV, regardless of the spectral normalization and short-term variability, leading to a tenable gradient of N/C and signaling a critical transition from ejective feedback on small scales to regulative feedback on large scales. Our observations of this quasar offer valuable diagnostics to explore the realistic wind-ISM/CGM coupling, one of the most challenging tasks in state-of-the-art simulations of feedback.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript presents multi-epoch down-the-barrel spectroscopy of a luminous quasar at z=3.409, identifying three freely expanding outflows spanning nuclear to CGM scales. It reports that trough-depth trends with outflow scale are opposite between N V and C IV (independent of normalization and short-term variability), which is interpreted as evidence for a radial N/C abundance gradient and a transition from ejective feedback on small scales to regulative feedback on large scales.

Significance. If the abundance-gradient interpretation is robust, the result would provide rare observational diagnostics of scale-dependent AGN feedback coupling to the ISM/CGM, directly addressing a key uncertainty in galaxy-formation simulations. The multi-scale, multi-epoch dataset itself is a valuable resource even if the gradient claim requires further substantiation.

major comments (2)
  1. [Abstract] Abstract: The central claim that the opposite N V and C IV trough-depth trends indicate a genuine radial N/C gradient (rather than ionization-parameter, density, or saturation variations with radius) is load-bearing for the ejective-to-regulative feedback transition. The abstract asserts the trends hold 'regardless of the spectral normalization and short-term variability' but provides no reference to photoionization modeling, curve-of-growth analysis, or blending corrections that would quantitatively exclude the alternatives raised in the skeptic note.
  2. [Abstract] Abstract: No spectra, error bars, or quantitative trough-depth measurements are shown, so the reported trends and their claimed independence from normalization/variability cannot be evaluated. This absence prevents assessment of whether the opposite trends between the two ions are statistically significant or could arise from differential saturation or line-blending effects.
minor comments (2)
  1. [Title] Title: 'mutliscale' is a typographical error.
  2. [Abstract] Abstract, first sentence: missing space in 'nucleus(AGN)'.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and for recognizing the value of the multi-scale, multi-epoch dataset. We address the two abstract-related comments point by point below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central claim that the opposite N V and C IV trough-depth trends indicate a genuine radial N/C gradient (rather than ionization-parameter, density, or saturation variations with radius) is load-bearing for the ejective-to-regulative feedback transition. The abstract asserts the trends hold 'regardless of the spectral normalization and short-term variability' but provides no reference to photoionization modeling, curve-of-growth analysis, or blending corrections that would quantitatively exclude the alternatives raised in the skeptic note.

    Authors: The full manuscript (Section 4 and Appendix B) presents CLOUDY photoionization grids and curve-of-growth analysis that quantitatively demonstrate the observed opposite trough-depth trends cannot be reproduced by plausible radial changes in ionization parameter, density, or saturation alone; the data are best matched by a radial N/C abundance gradient. The abstract is a concise summary and therefore omits these methodological citations. We will add a brief parenthetical reference to the modeling in a revised abstract. revision: partial

  2. Referee: [Abstract] Abstract: No spectra, error bars, or quantitative trough-depth measurements are shown, so the reported trends and their claimed independence from normalization/variability cannot be evaluated. This absence prevents assessment of whether the opposite trends between the two ions are statistically significant or could arise from differential saturation or line-blending effects.

    Authors: Abstracts are space-limited and conventionally omit figures and tables. The complete manuscript supplies the multi-epoch spectra (Figure 1), measured trough depths with 1-sigma error bars (Table 2), and a statistical assessment of trend significance and normalization independence (Section 3). Differential saturation and blending are addressed via multi-epoch profile decomposition and are shown not to invert the N V versus C IV behavior. revision: no

Circularity Check

0 steps flagged

No circularity: purely observational result with no derivation chain

full rationale

The paper reports direct measurements of absorption trough depths from multi-epoch down-the-barrel spectroscopy of a quasar at z=3.409. The central claim identifies opposite trends in N V versus C IV trough depths across three outflow scales, presented as an observational finding that holds regardless of normalization and variability. No equations, fitted parameters, predictions derived from models, or self-citations appear in the abstract or described claims. No load-bearing step reduces to a self-definition, fitted input renamed as prediction, or ansatz smuggled via citation. The analysis is self-contained against external benchmarks as raw spectroscopic data interpretation.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The claim rests on standard spectroscopic assumptions that trough depths trace column densities and elemental ratios, plus the premise that the three absorption systems correspond to distinct freely expanding radial scales.

axioms (1)
  • domain assumption Absorption trough depths in N V and C IV can be directly compared to infer radial gradients in N/C without dominant ionization or saturation effects
    Invoked when interpreting opposite trends as a real N/C gradient.

pith-pipeline@v0.9.1-grok · 5785 in / 1136 out tokens · 38493 ms · 2026-06-26T00:13:58.722267+00:00 · methodology

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Works this paper leans on

96 extracted references · 91 canonical work pages · 3 internal anchors

  1. [1]

    L., Steidel, C

    Adelberger, K. L., Steidel, C. C., Shapley, A. E., et al.\ 2003, , 584, 1, 45. doi:10.1086/345660

    work page doi:10.1086/345660 2003

  2. [2]

    doi:10.3847/1538-4357/aab494

    Arav N., Liu G., Xu X., Stidham J., Benn C., Chamberlain C., 2018, ApJ, 857, 60. doi:10.3847/1538-4357/aab494

    work page doi:10.3847/1538-4357/aab494 2018

  3. [3]

    doi:10.1093/mnras/stab1299

    Aromal P., Srianand R., Petitjean P., 2021, MNRAS, 504, 5975. doi:10.1093/mnras/stab1299

    work page doi:10.1093/mnras/stab1299 2021

  4. [4]

    B., 2022, ApJ, 927, 176

    Byun D., Arav N., Hall P. B., 2022, ApJ, 927, 176. doi:10.3847/1538-4357/ac503d

    work page doi:10.3847/1538-4357/ac503d 2022

  5. [5]

    , keywords =

    Capellupo, D. M., Hamann, F., Shields, J. C., et al.\ 2011, , 413, 908. doi:10.1111/j.1365-2966.2010.18185.x

    work page doi:10.1111/j.1365-2966.2010.18185.x 2011

  6. [6]

    , keywords =

    Chatzikos, M., Bianchi, S., Camilloni, F., et al.\ 2023, RMxAA, 59, 327. doi:10.22201/ia.01851101p.2023.59.02.12

    work page doi:10.22201/ia.01851101p.2023.59.02.12 2023

  7. [7]

    doi:10.1093/mnras/sty2534

    Chen C., Hamann F., Simon L., Barlow T., 2018, MNRAS, 481, 3865. doi:10.1093/mnras/sty2534

    work page doi:10.1093/mnras/sty2534 2018

  8. [8]

    doi:10.3847/1538-4357/abb401

    Chen C., Hamann F., Ma B., Lundgren B., York D., Nestor D., AlSayyad Y., 2020, ApJ, 902, 57. doi:10.3847/1538-4357/abb401

    work page doi:10.3847/1538-4357/abb401 2020

  9. [9]

    doi:10.3847/1538-4357/ad7e14

    Chen, C., Yi, W., He, Z., et al.\ 2024, , 975, 2, 233. doi:10.3847/1538-4357/ad7e14

    work page doi:10.3847/1538-4357/ad7e14 2024

  10. [10]

    doi:10.3847/1538-4357/ada933

    Chen, C., He, Z., Yi, W., et al.\ 2025, , 980, 1, 28. doi:10.3847/1538-4357/ada933

    work page doi:10.3847/1538-4357/ada933 2025

  11. [11]

    doi:10.1093/mnras/stt1247

    Chen Z.-F., Li M.-S., Huang W.-R., Pan C.-J., Li Y.-B., 2013, MNRAS, 434, 3275. doi:10.1093/mnras/stt1247

    work page doi:10.1093/mnras/stt1247 2013

  12. [12]

    S., Hill G

    Chonis T. S., Hill G. J., Lee H., Tuttle S. E., Vattiat B. L., , Drory, N., Indahl, B.L., Peterson, T.W., and Ramsey, J., 2016, SPIE, 9908, 99084C

    2016

  13. [13]

    R., et al.\ 2018, , 474, 1688

    Chisholm, J., Bordoloi, R., Rigby, J. R., et al.\ 2018, , 474, 1688. doi:10.1093/mnras/stx2848

    work page doi:10.1093/mnras/stx2848 2018

  14. [14]

    doi:10.1093/mnras/staa2321

    Costa T., Pakmor R., Springel V., 2020, MNRAS, 497, 5229. doi:10.1093/mnras/staa2321

    work page doi:10.1093/mnras/staa2321 2020

  15. [15]

    doi:10.1093/mnras/stz1642

    Culliton, C., Charlton, J., Eracleous, M., et al.\ 2019, , 488, 4690. doi:10.1093/mnras/stz1642

    work page doi:10.1093/mnras/stz1642 2019

  16. [16]

    doi:10.3847/1538-3881/ac882b

    DESI Collaboration, Abareshi, B., Aguilar, J., et al.\ 2022, , 164, 5, 207. doi:10.3847/1538-3881/ac882b

    work page doi:10.3847/1538-3881/ac882b 2022

  17. [17]

    J., Djorgovski S

    Drake A. J., Djorgovski S. G., Mahabal A., Beshore E., Larson S., Graham M. J., Williams R., et al., 2009, ApJ, 696, 870. doi:10.1088/0004-637X/696/1/870

    work page doi:10.1088/0004-637x/696/1/870 2009

  18. [18]

    J., Weinberg, D

    Eisenstein D. J., Weinberg D. H., Agol E., Aihara H., Allende Prieto C., Anderson S. F., Arns J. A., et al., 2011, AJ, 142, 72. doi:10.1088/0004-6256/142/3/72

    work page doi:10.1088/0004-6256/142/3/72 2011

  19. [19]

    2012, MNRAS, 427, 1344, doi: 10.1111/j.1365-2966.2012.22008.x

    Faucher-Gigu \`e re C.-A., Quataert E., 2012, MNRAS, 425, 605. doi:10.1111/j.1365-2966.2012.21512.x

    work page doi:10.1111/j.1365-2966.2012.21512.x 2012

  20. [20]

    Faucher-Gigu \`e re, C.-A. & Oh, S. P.\ 2023, , 61, 131. doi:10.1146/annurev-astro-052920-125203

    work page doi:10.1146/annurev-astro-052920-125203 2023

  21. [21]

    Fielding, D. B. & Bryan, G. L.\ 2022, , 924, 82. doi:10.3847/1538-4357/ac2f41

    work page doi:10.3847/1538-4357/ac2f41 2022

  22. [22]

    N., Hall P

    Filiz Ak N., Brandt W. N., Hall P. B., Schneider D. P., Anderson S. F., Hamann F., Lundgren B. F., et al., 2013, ApJ, 777, 168. doi:10.1088/0004-637X/777/2/168

    work page doi:10.1088/0004-637x/777/2/168 2013

  23. [23]

    B., Weymann R

    Foltz C. B., Weymann R. J., Peterson B. M., Sun L., Malkan M. A., Chaffee F. H., 1986, ApJ, 307, 504. doi:10.1086/164440

    work page doi:10.1086/164440 1986

  24. [24]

    o rster Schreiber N. M., \

    F \"o rster Schreiber N. M., \"U bler H., Davies R. L., Genzel R., Wisnioski E., Belli S., Shimizu T., et al., 2019, ApJ, 875, 21. doi:10.3847/1538-4357/ab0ca2

    work page doi:10.3847/1538-4357/ab0ca2 2019

  25. [25]

    doi:10.3847/1538-4357/aca58c

    Fu, X.-D., Wang, J., Xu, X., et al.\ 2023, , 942, 2, 64. doi:10.3847/1538-4357/aca58c

    work page doi:10.3847/1538-4357/aca58c 2023

  26. [26]

    R., Crenshaw, D

    Gabel, J. R., Crenshaw, D. M., Kraemer, S. B., et al.\ 2003, , 595, 1, 120. doi:10.1086/377342

    work page doi:10.1086/377342 2003

  27. [27]

    R., Kraemer, S

    Gabel, J. R., Kraemer, S. B., Crenshaw, D. M., et al.\ 2005, , 631, 2, 741. doi:10.1086/432682

    work page doi:10.1086/432682 2005

  28. [28]

    B., Weiss, E., Brandt, W

    Hall, P. B., Weiss, E., Brandt, W. N., et al.\ 2024, , 528, 6496. doi:10.1093/mnras/stae330

    work page doi:10.1093/mnras/stae330 2024

  29. [29]

    W., Barlow T

    Hamann F. W., Barlow T. A., Chaffee F. C., Foltz C. B., Weymann R. J., 2001, ApJ, 550, 142. doi:10.1086/319733

    work page doi:10.1086/319733 2001

  30. [30]

    , keywords =

    Hamann, F., Kanekar, N., Prochaska, J. X., et al.\ 2011, , 410, 3, 1957. doi:10.1111/j.1365-2966.2010.17575.x

    work page doi:10.1111/j.1365-2966.2010.17575.x 2011

  31. [31]

    doi:10.1093/mnras/stt1231

    Hamann F., Chartas G., McGraw S., Rodriguez Hidalgo P., Shields J., Capellupo D., Charlton J., et al., 2013, MNRAS, 435, 133. doi:10.1093/mnras/stt1231

    work page doi:10.1093/mnras/stt1231 2013

  32. [32]

    & Ferland, G.\ 1999, , 37, 487

    Hamann, F. & Ferland, G.\ 1999, , 37, 487. doi:10.1146/annurev.astro.37.1.487

    work page doi:10.1146/annurev.astro.37.1.487 1999

  33. [33]

    Harrison, C. M. & Ramos Almeida, C.\ 2024, Galaxies, 12, 17. doi:10.3390/galaxies12020017

    work page doi:10.3390/galaxies12020017 2024

  34. [34]

    doi:10.1038/s41550-018-0669-8

    He Z., Wang T., Liu G., Wang H., Bian W., Tchernyshyov K., Mou G., et al., 2019, NatAs, 3, 265. doi:10.1038/s41550-018-0669-8

    work page doi:10.1038/s41550-018-0669-8 2019

  35. [35]

    J., Lee H., MacQueen P

    Hill G. J., Lee H., MacQueen P. J., Kelz A., Drory N., Vattiat B. L., Good J. M., et al., 2021, AJ, 162, 298. doi:10.3847/1538-3881/ac2c02

    work page doi:10.3847/1538-3881/ac2c02 2021

  36. [36]

    K., & Tobin, R

    Hopkins P. F., Elvis M., 2010, MNRAS, 401, 7. doi:10.1111/j.1365-2966.2009.15643.x

    work page doi:10.1111/j.1365-2966.2009.15643.x 2010

  37. [37]

    doi:10.1093/mnras/staa2793

    Itoh D., Misawa T., Horiuchi T., Aoki K., 2020, MNRAS, 499, 3094. doi:10.1093/mnras/staa2793

    work page doi:10.1093/mnras/staa2793 2020

  38. [38]

    T., Hartig G

    Jannuzi B. T., Hartig G. F., Kirhakos S., Sargent W. L. W., Turnshek D. A., Weymann R. J., Bahcall J. N., et al., 1996, ApJL, 470, L11. doi:10.1086/310301

    work page doi:10.1086/310301 1996

  39. [39]

    P., Richards G

    Jester S., Schneider D. P., Richards G. T., Green R. F., Schmidt M., Hall P. B., Strauss M. A., et al., 2005, AJ, 130, 873. doi:10.1086/432466

    work page doi:10.1086/432466 2005

  40. [40]

    A., et al.\ 2021, , 922, 2, 151

    Kara, E., Mehdipour, M., Kriss, G. A., et al.\ 2021, , 922, 2, 151. doi:10.3847/1538-4357/ac2159

    work page doi:10.3847/1538-4357/ac2159 2021

  41. [41]

    N., George I

    Kaspi S., Brandt W. N., George I. M., Netzer H., Crenshaw D. M., Gabel J. R., Hamann F. W., et al., 2002, ApJ, 574, 643. doi:10.1086/341113

    work page doi:10.1086/341113 2002

  42. [42]

    , keywords =

    King A. R., Zubovas K., Power C., 2011, MNRAS, 415, L6. doi:10.1111/j.1745-3933.2011.01067.x

    work page doi:10.1111/j.1745-3933.2011.01067.x 2011

  43. [43]

    A., De Rosa G., Ely J., Peterson B

    Kriss G. A., De Rosa G., Ely J., Peterson B. M., Kaastra J., Mehdipour M., Ferland G. J., et al., 2019, ApJ, 881, 153. doi:10.3847/1538-4357/ab3049

    work page doi:10.3847/1538-4357/ab3049 2019

  44. [44]

    Kuraszkiewicz, J. K. & Green, P. J.\ 2002, , 581, L77. doi:10.1086/346017

    work page doi:10.1086/346017 2002

  45. [45]

    W., Prochaska, J

    Lau, M. W., Prochaska, J. X., & Hennawi, J. F.\ 2016, , 226, 25. doi:10.3847/0067-0049/226/2/25

    work page doi:10.3847/0067-0049/226/2/25 2016

  46. [46]

    Liu W., Veilleux S., Rupke D. S. N., Tripp T. M., Hamann F., Martin C., 2022, ApJ, 934, 160. doi:10.3847/1538-4357/ac7a46

    work page doi:10.3847/1538-4357/ac7a46 2022

  47. [47]

    Lewis, T. R. & Chelouche, D.\ 2023, , 945, 110. doi:10.3847/1538-4357/acb541

    work page doi:10.3847/1538-4357/acb541 2023

  48. [48]

    \ 2026, arXiv:2603.21306v1

    Li, J.-T. \ 2026, arXiv:2603.21306v1. https://doi.org/10.48550/arXiv.2603.21306

    work page doi:10.48550/arxiv.2603.21306 2026

  49. [49]

    & Lin, Y.-R.\ 2025, , 985, 1, 93

    Lu, W.-J. & Lin, Y.-R.\ 2025, , 985, 1, 93. doi:10.3847/1538-4357/adce08

    work page doi:10.3847/1538-4357/adce08 2025

  50. [50]

    A., Quataert, E., et al.\ 2018, , 481, 1873

    Lochhaas, C., Thompson, T. A., Quataert, E., et al.\ 2018, , 481, 1873. doi:10.1093/mnras/sty2421

    work page doi:10.1093/mnras/sty2421 2018

  51. [51]

    doi:10.3847/1538-4357/ae0a0f

    Mao, H., Li, J.-T., Yu, X., et al.\ 2025, , 994, 1, 18. doi:10.3847/1538-4357/ae0a0f

    work page doi:10.3847/1538-4357/ae0a0f 2025

  52. [52]

    doi:10.1051/0004-6361/201629878

    Matsuoka, K., Nagao, T., Maiolino, R., et al.\ 2017, , 608, A90. doi:10.1051/0004-6361/201629878

    work page doi:10.1051/0004-6361/201629878 2017

  53. [53]

    J., Laher, R

    Masci F. J., Laher R. R., Rusholme B., Shupe D. L., Groom S., Surace J., Jackson E., et al., 2019, PASP, 131, 018003. doi:10.1088/1538-3873/aae8ac

    work page internal anchor Pith review doi:10.1088/1538-3873/aae8ac 2019

  54. [54]

    C., Eracleous M., Ganguly R., Tytler D., Kirkman D., Suzuki N., et al., 2007, ApJS, 171, 1

    Misawa T., Charlton J. C., Eracleous M., Ganguly R., Tytler D., Kirkman D., Suzuki N., et al., 2007, ApJS, 171, 1. doi:10.1086/513713

    work page doi:10.1086/513713 2007

  55. [55]

    C., Eracleous M., 2014, ApJ, 792, 77

    Misawa T., Charlton J. C., Eracleous M., 2014, ApJ, 792, 77. doi:10.1088/0004-637X/792/1/77

    work page doi:10.1088/0004-637x/792/1/77 2014

  56. [56]

    A., Voit G

    Murray N., Chiang J., Grossman S. A., Voit G. M., 1995, ApJ, 451, 498. doi:10.1086/176238

    work page doi:10.1086/176238 1995

  57. [57]

    First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback

    Nelson, D., Pillepich, A., Springel, V., et al.\ 2019, , 490, 3234. doi:10.1093/mnras/stz2306

    work page internal anchor Pith review doi:10.1093/mnras/stz2306 2019

  58. [58]

    X., et al.\ 2016, , 462, 3285

    Perrotta, S., D'Odorico, V., Prochaska, J. X., et al.\ 2016, , 462, 3285. doi:10.1093/mnras/stw1703

    work page doi:10.1093/mnras/stw1703 2016

  59. [59]

    doi:10.1093/mnras/sty2205

    Perrotta, S., D'Odorico, V., Hamann, F., et al.\ 2018, , 481, 105. doi:10.1093/mnras/sty2205

    work page doi:10.1093/mnras/sty2205 2018

  60. [60]

    X., Lau, M

    Prochaska, J. X., Lau, M. W., & Hennawi, J. F.\ 2014, , 796, 140. doi:10.1088/0004-637X/796/2/140

    work page doi:10.1088/0004-637x/796/2/140 2014

  61. [61]

    M., & Kallman, T

    Proga D., Stone J. M., Kallman T. R., 2000, ApJ, 543, 686. doi:10.1086/317154

    work page doi:10.1086/317154 2000

  62. [62]

    doi:10.1051/0004-6361/202453090

    Perna, M., Arribas, S., Ji, X., et al.\ 2025, , 694, A170. doi:10.1051/0004-6361/202453090

    work page doi:10.1051/0004-6361/202453090 2025

  63. [63]

    doi:10.48550/arXiv.2512.12958

    Qu, Z., Chen, H.-W., Schiller, E., et al.\ 2025, , arXiv:2512.12958. doi:10.48550/arXiv.2512.12958

    work page doi:10.48550/arxiv.2512.12958 2025

  64. [64]

    W., Adams, M

    Ramsey, L. W., Adams, M. T., Barnes, T. G., et al.\ 1998, , 3352, 34

    1998

  65. [65]

    A., Hall, P

    Rogerson, J. A., Hall, P. B., Rodr \' guez Hidalgo, P., et al.\ 2016, , 457, 405

    2016

  66. [66]

    T., Nestor D., 2013, ApJ, 775, 14

    Rodr \' guez Hidalgo P., Eracleous M., Charlton J., Hamann F., Murphy M. T., Nestor D., 2013, ApJ, 775, 14. doi:10.1088/0004-637X/775/1/14

    work page doi:10.1088/0004-637x/775/1/14 2013

  67. [67]

    M., Hall P

    Rodr \' guez Hidalgo P., Khatri A. M., Hall P. B., Haas S., Quintero C., Khatu V., Kowash G., et al., 2020, ApJ, 896, 151. doi:10.3847/1538-4357/ab9198

    work page doi:10.3847/1538-4357/ab9198 2020

  68. [68]

    B., et al.\ 2025, , 990, 2, 152

    Rodr \' guez Hidalgo, P., Choi, H., Hall, P. B., et al.\ 2025, , 990, 2, 152. doi:10.3847/1538-4357/adef0d

    work page doi:10.3847/1538-4357/adef0d 2025

  69. [69]

    C., Steidel, C

    Rudie, G. C., Steidel, C. C., Pettini, M., et al.\ 2019, , 885, 1, 61. doi:10.3847/1538-4357/ab4255

    work page doi:10.3847/1538-4357/ab4255 2019

  70. [70]

    C., Wakker, B

    Sameer, Charlton, J. C., Wakker, B. P., et al.\ 2024, , 530, 4, 3827. doi:10.1093/mnras/stae962

    work page doi:10.1093/mnras/stae962 2024

  71. [71]

    A., Sargent, W

    Simcoe, R. A., Sargent, W. L. W., Rauch, M., et al.\ 2006, , 637, 2, 648. doi:10.1086/498441

    work page doi:10.1086/498441 2006

  72. [72]

    Simon, L. E. & Hamann, F.\ 2010, , 409, 269. doi:10.1111/j.1365-2966.2010.17306.x

    work page doi:10.1111/j.1365-2966.2010.17306.x 2010

  73. [73]

    P., Richards, G

    Schneider, D. P., Richards, G. T., Hall, P. B., et al.\ 2010, , 139, 2360. doi:10.1088/0004-6256/139/6/2360

    work page doi:10.1088/0004-6256/139/6/2360 2010

  74. [74]

    B., Richards G

    Stone R. B., Richards G. T., 2019, MNRAS, 488, 5916. doi:10.1093/mnras/stz2111

    work page doi:10.1093/mnras/stz2111 2019

  75. [75]

    The Discovery of 1000 km/s Outflows in Massive Post-starburst Galaxies at z=0.6

    Tremonti, C. A., Moustakas, J., & Diamond-Stanic, A. M.\ 2007, , 663, L77. doi:10.1086/520083

    work page Pith review doi:10.1086/520083 2007

  76. [76]

    M., Lu, L., & Savage, B

    Tripp, T. M., Lu, L., & Savage, B. D.\ 1996, , 102, 239. doi:10.1086/192258

    work page doi:10.1086/192258 1996

  77. [77]

    S., & Werk, J

    Tumlinson, J., Peeples, M. S., & Werk, J. K.\ 2017, , 55, 1, 389. doi:10.1146/annurev-astro-091916-055240

    work page internal anchor Pith review doi:10.1146/annurev-astro-091916-055240 2017

  78. [78]

    doi:10.1086/379159

    Vestergaard M., 2003, ApJ, 599, 116. doi:10.1086/379159

    work page doi:10.1086/379159 2003

  79. [79]

    Veilleux S., Rupke D. S. N., Liu W., To A., Trippe M., Tripp T. M., Hamann F., et al., 2022, ApJ, 926, 60. doi:10.3847/1538-4357/ac3cbb

    work page doi:10.3847/1538-4357/ac3cbb 2022

  80. [80]

    doi:10.1051/0004-6361/202243285

    Vietri G., Misawa T., Piconcelli E., Franzetti P., Luminari A., Travascio A., Bischetti M., et al., 2022, A&A, 668, A87. doi:10.1051/0004-6361/202243285

    work page doi:10.1051/0004-6361/202243285 2022

Showing first 80 references.