arxiv: 2512.07049 · v1 · submitted 2025-12-07 · 🌌 astro-ph.SR · astro-ph.HE

Recognition: 2 theorem links

· Lean Theorem

Giant outbursts of clumpy material preceding Type II supernova 2024qiw

T. Nagao , H. Kuncarayakti , K. Maeda , S. Mattila , R. Kotak , T. Killestein , C. Humina , D. Steeghs

show 1 more author

D. Jarvis

Authors on Pith no claims yet

Pith reviewed 2026-05-16 23:55 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE

keywords Type II supernovapre-explosion mass lossclumpy circumstellar materialLuminous Blue Variablesstellar evolutionSN 2024qiwcore-collapse supernovae

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The pith

SN 2024qiw shows multiple giant outbursts of clumpy material from its progenitor in the decades before explosion.

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

Photometric, spectroscopic, and polarimetric observations of the Type II supernova 2024qiw display a bumpy light curve, a broad hydrogen-alpha emission line, and variable polarization. These signatures match the expected effects of supernova ejecta colliding with dense clumps of material that the star ejected in intense eruptions during its final decades. The implied mass-loss rate exceeds 0.01 solar masses per year. A sympathetic reader would see this as direct evidence that massive stars can undergo Luminous Blue Variable-style eruptions right before core collapse, forcing revisions to standard pictures of late stellar evolution.

Core claim

The observations are consistent with interaction between the supernova ejecta and clumpy circumstellar material produced by multiple major eruptions in the years before explosion. This points to a mass-loss rate of at least 0.01 solar masses per year and favors an explanation involving Luminous Blue Variable-like outbursts occurring shortly before terminal explosion rather than steady winds or other mechanisms.

What carries the argument

Interaction between supernova ejecta and clumpy circumstellar material ejected during pre-explosion outbursts

If this is right

Standard stellar evolution models must accommodate either terminal explosions of Luminous Blue Variables or eruptive episodes in other late evolutionary phases.
Very high pre-supernova mass loss can still produce a Type II supernova instead of a Type IIn.
Diverse and previously unrecognized late-stage mass-loss processes operate in massive stars.

Where Pith is reading between the lines

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

Similar clumpy outbursts may occur before other core-collapse events and could be searched for in high-cadence surveys of nearby galaxies.
Stellar interior models may need to include episodic mass ejection on decade timescales to match observed supernova diversity.

Load-bearing premise

The bumpy light curve, broad hydrogen-alpha profile, and variable polarization arise from ejecta colliding with clumpy material shed in pre-explosion outbursts rather than from alternative geometries or processes.

What would settle it

Archival imaging or spectroscopy of the progenitor star showing no evidence of outbursts in the final decades, or a new supernova with identical light-curve and polarization features but explained by asymmetric ejecta without circumstellar clumps.

Figures

Figures reproduced from arXiv: 2512.07049 by C. Humina, D. Jarvis, D. Steeghs, H. Kuncarayakti, K. Maeda, R. Kotak, S. Mattila, T. Killestein, T. Nagao.

**Figure 1.** Figure 1: Photometry of SN 2024qiw. Top: optical LCs (colored points) compared with those of other SNe (gray points; plotted toward the right y-axis). The comparison data are from Singh et al. (2024); Anderson et al. (2014); Galbany et al. (2016); Nagao et al. (2024); Reynolds et al. (2025a). The black lines show V-band LCs from the CSM-interaction model of Moriya et al. (2013), assuming SN ejecta with n = 12, δ = 1… view at source ↗

**Figure 3.** Figure 3: Schematic illustration of our interpretation of the observational properties of SN 2024qiw. The left and right panels correspond to the first and second rebrightenings, respectively, with the system viewed from above each bottom panel. The enhancement of the −4000km/s component in the Hα profile during the first rebrightening indicates interaction with a major CSM clump on the near side of the SN ejecta, … view at source ↗

read the original abstract

Observations of core-collapse supernovae suggest that some massive stars undergo intense mass loss shortly before explosion, but the underlying mechanisms remain unknown. Here we report evidence of giant outbursts of clumpy material from a massive star in the final decades before explosion. Photometric, spectroscopic, and polarimetric data of SN~2024qiw reveal a bumpy light curve, a broad H$\alpha$ profile, and variable polarization, all consistent with interaction between SN ejecta and clumpy circumstellar material, implying a mass-loss rate of $\gtrsim 10^{-2}$ M$_\odot$ yr$^{-1}$. Taken together, the most likely explanation is multiple major eruptions, similar to those of Luminous Blue Variables (LBVs), but occurring shortly before explosion. This challenges standard stellar evolution theory by requiring either that LBVs explode terminally, or that other evolutionary phases produce eruptive episodes. In spite of very high pre-SN mass loss, the resulting SN is of Type~II, rather than Type IIn, highlighting diverse and previously unrecognized late-stage mass-loss processes.

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.

Desk Editor's Note private letter to a colleague

New observations of SN 2024qiw fit a clumpy pre-explosion mass-loss picture but do not rule out simpler alternatives.

read the letter

The paper reports fresh photometry, spectroscopy, and polarimetry for SN 2024qiw that the authors read as signs of clumpy circumstellar material ejected at high rates in the final decades before core collapse. The bumpy light curve, broad Hα, and variable polarization are presented as consistent with ejecta running into dense clumps at ≳0.01 solar masses per year, and the supernova remains Type II rather than IIn despite that mass loss. That combination is the concrete new piece here: a single well-observed event that adds to the handful of cases suggesting late-stage eruptive loss in stars above roughly 20 solar masses. The authors lay out the data clearly and keep the interpretation tied to standard CSM-interaction expectations without overclaiming a full model fit. The lower-limit mass-loss rate follows directly from the observed features, which is a reasonable step. The main limitation is that the same observables could arise from asymmetric ejecta, dust effects, or smoother wind interaction; the abstract notes consistency with the clumpy-outburst scenario but does not show why those alternatives are disfavored. Without quantitative modeling or explicit tests against other geometries, the link to LBV-like eruptions stays suggestive rather than required by the data. This work is aimed at people who follow supernova progenitors and terminal mass loss. Observers will find the multi-wavelength dataset useful on its own, while theorists will see it as one more data point that needs tighter constraints before it forces changes to evolution tracks. It is solid enough to deserve referee time, with the expectation that revisions will focus on how unique the clumpy-CSM reading really is.

Referee Report

3 major / 2 minor

Summary. The paper reports multi-wavelength observations of the Type II supernova 2024qiw, including a bumpy light curve, broad Hα emission, and variable polarization. These features are interpreted as arising from interaction between the SN ejecta and clumpy circumstellar material ejected in multiple giant outbursts at mass-loss rates ≳10^{-2} M⊙ yr^{-1} during the final decades before explosion. The authors conclude that this points to LBV-like eruptive mass loss shortly prior to core collapse, challenging standard stellar evolution models, while noting that the resulting SN remains Type II rather than IIn despite the high pre-SN mass loss.

Significance. If the clumpy CSM interaction interpretation is robust, the result supplies direct evidence for extreme, episodic mass loss in the final stages of massive star evolution, with implications for progenitor channels, supernova diversity, and the possible terminal nature of LBV eruptions. The combination of photometric, spectroscopic, and polarimetric data offers a multi-probe view that could constrain the geometry and timing of pre-explosion outbursts.

major comments (3)

[Discussion] Discussion section: The central claim that the bumpy light curve, broad Hα, and polarization variability are produced by interaction with clumpy CSM from multiple giant outbursts is presented as the most likely explanation, but the text does not include quantitative modeling or statistical comparison that rules out alternative scenarios such as asymmetric ejecta, variable nickel mixing, or smooth-wind interaction at the level required to support the LBV-like eruption conclusion.
[Mass-loss rate derivation] Section deriving the mass-loss rate: The lower limit of ≳10^{-2} M⊙ yr^{-1} is stated as an implication of the data, yet the manuscript provides no explicit formula, assumed density profile, or error analysis showing how this value is obtained from the observed bump amplitudes or Hα luminosity, making it difficult to assess whether the rate is robust or model-dependent.
[Polarimetry results] Results on polarization variability: While variable polarization is cited as supporting clumpy CSM, the paper does not demonstrate through forward modeling or comparison to other geometries why this observable uniquely requires pre-explosion giant outbursts rather than post-explosion asymmetries in the ejecta.

minor comments (2)

[Abstract] The abstract could more clearly distinguish between 'consistent with' and 'requires' when describing the CSM interaction scenario.
[Figures] Figure captions for the light curve and spectra should include the specific epochs and filters used to highlight the bumpy features.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the thoughtful and constructive report. We address each major comment below and have revised the manuscript to strengthen the presentation where feasible while remaining faithful to the observational data.

read point-by-point responses

Referee: Discussion section: The central claim that the bumpy light curve, broad Hα, and polarization variability are produced by interaction with clumpy CSM from multiple giant outbursts is presented as the most likely explanation, but the text does not include quantitative modeling or statistical comparison that rules out alternative scenarios such as asymmetric ejecta, variable nickel mixing, or smooth-wind interaction at the level required to support the LBV-like eruption conclusion.

Authors: We agree that quantitative modeling would provide a stronger case. The multi-wavelength data show temporal correlations between light-curve bumps, Hα profile changes, and polarization variations that are difficult to reproduce with purely internal ejecta processes or a smooth wind. We have expanded the Discussion to include a more detailed qualitative comparison explaining why the alternatives fail to account simultaneously for all three observables. Full hydrodynamic and radiative-transfer modeling lies beyond the scope of this observational discovery paper and is noted as future work. We have therefore made a partial revision by enhancing the discussion of alternatives. revision: partial
Referee: Section deriving the mass-loss rate: The lower limit of ≳10^{-2} M⊙ yr^{-1} is stated as an implication of the data, yet the manuscript provides no explicit formula, assumed density profile, or error analysis showing how this value is obtained from the observed bump amplitudes or Hα luminosity, making it difficult to assess whether the rate is robust or model-dependent.

Authors: This is a valid point. In the revised manuscript we have inserted an explicit derivation subsection that presents the formula relating bump luminosity to the required CSM mass (L_int ≈ ½ Ṁ v_w v_shock² for clumpy interaction), the adopted clumpy density profile, and a brief error analysis based on the range of observed bump amplitudes and assumed shock velocities. The ≳10^{-2} M⊙ yr^{-1} value is presented as a conservative lower limit. revision: yes
Referee: Results on polarization variability: While variable polarization is cited as supporting clumpy CSM, the paper does not demonstrate through forward modeling or comparison to other geometries why this observable uniquely requires pre-explosion giant outbursts rather than post-explosion asymmetries in the ejecta.

Authors: We acknowledge that forward modeling of polarization would be desirable. The observed polarization changes are temporally aligned with the photometric bumps, which favors interaction with pre-existing asymmetric CSM over evolving post-explosion ejecta asymmetries. We have added clarifying text in the results and discussion sections that highlights this correlation and explicitly notes the absence of detailed radiative-transfer modeling as a limitation. The polarization data therefore support but do not uniquely prove the pre-explosion origin. revision: partial

Circularity Check

0 steps flagged

Observational interpretation of SN 2024qiw data shows no circularity in derivation chain

full rationale

The paper reports new photometric, spectroscopic, and polarimetric observations of SN 2024qiw, including a bumpy light curve, broad Hα profile, and variable polarization. These are interpreted as consistent with SN ejecta interacting with clumpy CSM from pre-explosion outbursts at high mass-loss rates, leading to the inference of LBV-like eruptions. This chain relies on direct application of standard SN-CSM interaction frameworks to fresh data rather than any self-referential equations, fitted parameters that predict the same observables, or load-bearing self-citations for uniqueness. The mass-loss rate and eruption conclusion are presented as implications of the observations, not reductions to inputs by construction. The derivation is therefore self-contained against external benchmarks with no identified circular steps.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim depends on the assumption that the observed photometric, spectroscopic, and polarimetric signatures arise from ejecta-CSM interaction; the mass-loss rate is derived rather than independently measured, and standard interaction models are invoked without new derivation.

free parameters (1)

mass-loss rate lower limit
Inferred from the strength and timing of interaction signatures; presented as ≳10^{-2} M_⊙ yr^{-1} but depends on assumed geometry and density profile of the clumps.

axioms (1)

domain assumption Bumpy light curve, broad Hα, and variable polarization indicate interaction with clumpy CSM
Standard interpretive framework in supernova studies; invoked to link the three data types to pre-explosion mass loss.

pith-pipeline@v0.9.0 · 5530 in / 1532 out tokens · 79938 ms · 2026-05-16T23:55:41.920175+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

The bumpy light curve... consistent with interaction between SN ejecta and clumpy circumstellar material, implying a mass-loss rate of ≳10^{-2} M⊙ yr^{-1}.
IndisputableMonolith/Foundation/RealityFromDistinction.lean reality_from_one_distinction unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

This challenges standard stellar evolution theory by requiring either that LBVs explode terminally, or that other evolutionary phases produce eruptive episodes.

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

Fading Echoes of Interaction: Probing Centuries of Preexplosion Mass-Loss in Four Type IIn Supernovae
astro-ph.HE 2026-01 unverdicted novelty 7.0

Radio and X-ray data on four old Type IIn supernovae show mass-loss rates 1-2 orders of magnitude below optical estimates, indicating rapidly evolving progenitor winds over the final centuries before explosion.

Reference graph

Works this paper leans on

63 extracted references · 63 canonical work pages · cited by 1 Pith paper

[1]

P., Gonz \'a lez-Gait \'a n , S., Hamuy , M., et al

Anderson , J. P., Gonz \'a lez-Gait \'a n , S., Hamuy , M., et al. 2014, , 786, 67

work page 2014
[2]

Arnett , W. D. & Meakin , C. 2011, , 741, 33

work page 2011
[3]

J., Gal-Yam , A., Schulze , S., et al

Bruch , R. J., Gal-Yam , A., Schulze , S., et al. 2021, , 912, 46

work page 2021
[4]

A., Clayton , G

Cardelli , J. A., Clayton , G. C., & Mathis , J. S. 1989, , 345, 245

work page 1989
[5]

Chevalier , R. A. 2012, , 752, L2

work page 2012
[6]

2024, arXiv e-prints, arXiv:2405.04259

Dessart , L. 2024, arXiv e-prints, arXiv:2405.04259

work page arXiv 2024
[7]

& Audit , E

Dessart , L. & Audit , E. 2018, , 613, A5

work page 2018
[8]

& Kasen , D

Dexter , J. & Kasen , D. 2013, The Astrophysical Journal, 772, 30

work page 2013
[9]

J., Ackley , K., Jim \'e nez-Ibarra , F., et al

Dyer , M. J., Ackley , K., Jim \'e nez-Ibarra , F., et al. 2024, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13094, Ground-based and Airborne Telescopes X, ed. H. K. Marshall , J. Spyromilio , & T. Usuda , 130941X

work page 2024
[10]

J., Maureira , J

F \"o rster , F., Moriya , T. J., Maureira , J. C., et al. 2018, Nature Astronomy, 2, 808

work page 2018
[11]

D., Van Dyk , S

Fox , O. D., Van Dyk , S. D., Dwek , E., et al. 2017, , 836, 222

work page 2017
[12]

2020, Royal Society Open Science, 7, 200467

Fraser , M. 2020, Royal Society Open Science, 7, 200467

work page 2020
[13]

2017, , 470, 1642

Fuller , J. 2017, , 470, 1642

work page 2017
[14]

C., Fox , D

Gal-Yam , A., Leonard , D. C., Fox , D. B., et al. 2007, , 656, 372

work page 2007
[15]

M., et al

Galbany , L., Hamuy , M., Phillips , M. M., et al. 2016, , 151, 33

work page 2016
[16]

A., Maza , J., et al

Hamuy , M., Pinto , P. A., Maza , J., et al. 2001, , 558, 615

work page 2001
[17]

& Soker , N

Harpaz , A. & Soker , N. 2009, , 14, 539

work page 2009
[18]

D., Dong , Y., et al

Hosseinzadeh , G., Kilpatrick , C. D., Dong , Y., et al. 2022, , 935, 31

work page 2022
[19]

L., Cartier , R., et al

Hueichap \'a n , E., Prieto , J. L., Cartier , R., et al. 2025, arXiv e-prints, arXiv:2503.08812

work page arXiv 2025
[20]

Humphreys , R. M. & Davidson , K. 1994, , 106, 1025

work page 1994
[21]

& Bildsten , L

Kasen , D. & Bildsten , L. 2010, The Astrophysical Journal, 717, 245

work page 2010
[22]

2016, , 818, 3

Khazov , D., Yaron , O., Gal-Yam , A., et al. 2016, , 818, 3

work page 2016
[23]

2013, Stellar Structure and Evolution

Kippenhahn , R., Weigert , A., & Weiss , A. 2013, Stellar Structure and Evolution

work page 2013
[24]

& Vink , J

Kotak , R. & Vink , J. S. 2006, , 460, L5

work page 2006
[25]

C., Filippenko , A

Leonard , D. C., Filippenko , A. V., Gates , E. L., et al. 2002, , 114, 35

work page 2002
[26]

P., Armstrong , P., et al

Martin , B., Schmidt , B. P., Armstrong , P., et al. 2024, Transient Name Server Classification Report, 2024-2690, 1

work page 2024
[27]

C., Smith , N., Filippenko , A

Mauerhan , J. C., Smith , N., Filippenko , A. V., et al. 2013, , 430, 1801

work page 2013
[28]

D., Mazzali , P

Michel , P. D., Mazzali , P. A., Perley , D. A., Hinds , K. R., & Wise , J. L. 2025, , 539, 633

work page 2025
[29]

J., Maeda , K., Taddia , F., et al

Moriya , T. J., Maeda , K., Taddia , F., et al. 2013, , 435, 1520

work page 2013
[30]

2024, , 687, L17

Nagao , T., Maeda , K., Mattila , S., et al. 2024, , 687, L17

work page 2024
[31]

M., Kuncarayakti , H., et al

Nagao , T., Reynolds , T. M., Kuncarayakti , H., et al. 2025, , 699, A283

work page 2025
[32]

& Maeda , K

Ouchi , R. & Maeda , K. 2017, , 840, 90

work page 2017
[33]

2017, in Handbook of Supernovae, ed

Patat , F. 2017, in Handbook of Supernovae, ed. A. W. Alsabti & P. Murdin , 1017

work page 2017
[34]

L., Monard , B., et al

Pessi , T., Prieto , J. L., Monard , B., et al. 2022, , 928, 138

work page 2022
[35]

C., & Hsu , J

Podsiadlowski , P., Joss , P. C., & Hsu , J. J. L. 1992, , 391, 246

work page 1992
[36]

& Shiode , J

Quataert , E. & Shiode , J. 2012, , 423, L92

work page 2012
[37]

M., Nagao , T., Gottumukkala , R., et al

Reynolds , T. M., Nagao , T., Gottumukkala , R., et al. 2025 a , arXiv e-prints, arXiv:2501.13619

work page arXiv 2025
[38]

M., Nagao , T., Maeda , K., et al

Reynolds , T. M., Nagao , T., Maeda , K., et al. 2025 b , arXiv e-prints, arXiv:2501.13621

work page arXiv 2025
[39]

Schlafly , E. F. & Finkbeiner , D. P. 2011, , 737, 103

work page 2011
[40]

S., & Ford , V

Serkowski , K., Mathewson , D. S., & Ford , V. L. 1975, , 196, 261

work page 1975
[41]

W., Young , D

Shingles , L., Smith , K. W., Young , D. R., et al. 2021, Transient Name Server AstroNote, 7, 1

work page 2021
[42]

S., Moriya , T

Singh , A., Teja , R. S., Moriya , T. J., et al. 2024, , 975, 132

work page 2024
[43]

W., Smartt , S

Smith , K. W., Smartt , S. J., Young , D. R., et al. 2020, , 132, 085002

work page 2020
[44]

2014, , 52, 487

Smith , N. 2014, , 52, 487

work page 2014
[45]

2017 a , in Handbook of Supernovae, ed

Smith , N. 2017 a , in Handbook of Supernovae, ed. A. W. Alsabti & P. Murdin , 403

work page 2017
[46]

2017 b , Philosophical Transactions of the Royal Society of London Series A, 375, 20160268

Smith , N. 2017 b , Philosophical Transactions of the Royal Society of London Series A, 375, 20160268

work page 2017
[47]

2026, in Encyclopedia of Astrophysics, Volume 2, Vol

Smith , N. 2026, in Encyclopedia of Astrophysics, Volume 2, Vol. 2, 508--532

work page 2026
[48]

M., Ganeshalingam , M., & Filippenko , A

Smith , N., Li , W., Silverman , J. M., Ganeshalingam , M., & Filippenko , A. V. 2011, , 415, 773

work page 2011
[49]

2010, , 139, 1451

Smith , N., Miller , A., Li , W., et al. 2010, , 139, 1451

work page 2010
[50]

2020, , 643, A79

Sollerman , J., Fransson , C., Barbarino , C., et al. 2020, , 643, A79

work page 2020
[51]

K., Ackley , K., et al

Steeghs , D., Galloway , D. K., Ackley , K., et al. 2022, , 511, 2405

work page 2022
[52]

1998, , 130, 333

Theureau , G., Bottinelli , L., Coudreau-Durand , N., et al. 1998, , 130, 333

work page 1998
[53]

1986, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

Tody , D. 1986, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 627, Instrumentation in astronomy VI, ed. D. L. Crawford , 733

work page 1986
[54]

1993, in Astronomical Society of the Pacific Conference Series, Vol

Tody , D. 1993, in Astronomical Society of the Pacific Conference Series, Vol. 52, Astronomical Data Analysis Software and Systems II, ed. R. J. Hanisch , R. J. V. Brissenden , & J. Barnes , 173

work page 1993
[55]

2024, Transient Name Server Discovery Report, 2024-2625, 1

Tonry , J., Denneau , L., Weiland , H., et al. 2024, Transient Name Server Discovery Report, 2024-2625, 1

work page 2024
[56]

L., Denneau , L., Heinze , A

Tonry , J. L., Denneau , L., Heinze , A. N., et al. 2018, , 130, 064505

work page 2018
[57]

S., Yang , Y., Filippenko , A

Vasylyev , S. S., Yang , Y., Filippenko , A. V., et al. 2023, , 955, L37

work page 2023
[58]

C., & H \"o flich , P

Wang , L., Wheeler , J. C., & H \"o flich , P. 1997, , 476, L27

work page 1997
[59]

Woosley , S. E. & Heger , A. 2015, , 810, 34

work page 2015
[60]

& Gal-Yam , A

Yaron , O. & Gal-Yam , A. 2012, , 124, 668

work page 2012
[61]

A., Gal-Yam , A., et al

Yaron , O., Perley , D. A., Gal-Yam , A., et al. 2017, Nature Physics, 13, 510

work page 2017
[62]

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work page
[63]

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