Pith. sign in

REVIEW 3 major objections 3 minor 1 cited by

AT2022sxl: A Candidate Repeating Tidal Disruption Event in Possible Association with Two High-Energy Neutrino Events

T0 review · 3 major / 3 minor · reviewed 2026-08-05 · deepseek-v4-flash

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

Pith's one-line read AT2022sxl is a candidate repeating tidal disruption event whose two optical flares, 7.2 years apart, match two IceCube neutrino alerts.

desk verdict Candidate repeating TDE worth a referee, but the neutrino association is unproven without a chance-coincidence calculation. read the letter →

arxiv 2508.09408 v1 pith:BLEKM2PU submitted 2025-08-13 astro-ph.HE

Shunhao Ji , Zhongxiang Wang , Litao Zhu (1) , Stefan Geier (2) , Alok C. Gupta (3) ((1) Yunnan University , China , (2) GRANTECAN: Cuesta de San José s/n , Breña Baja
show 4 more authors
La Palma Spain (3) Aryabhatta Research Institute of Observational Sciences (ARIES) India)
This is my paper · ORCID
classification astro-ph.HE
keywords tidaldisruptioneventrepeatingTDEIceCubeneutrinosmid-infraredflareopticalH+Hecompositehostgalaxyneutrino-TDEassociation
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 reports AT2022sxl, a tidal disruption event candidate that flared twice in the optical with a ~7.2 yr separation, with mid-infrared flares lagging each optical peak by ~200 days. The authors identify the host as a composite galaxy at z=0.23 and show that broad H$\alpha$, H$\beta$, and He I lines powered by the TDE dominate the second-flare spectrum. They also find that two Bronze-type IceCube neutrino events match the source position and the second flare / delayed MIR flare in time. If the association is real, AT2022sxl would join the small set of neutrino-emitting TDEs and support the claim that luminous MIR emission is a prerequisite for neutrino production. The repeating nature is central: repeated partial disruptions could be a recurring source of high-energy neutrinos.

What carries the argument

The central objects are the multi-epoch optical and mid-infrared light curves of AT2022sxl plus two optical spectra, one taken near the second optical peak and one at quiescence. The light curves establish the ~7.2-year recurrence and the ~200-day MIR delay; the spectral comparison isolates the TDE's broad emission lines from the host galaxy's narrow lines; and the IceCube Bronze events act as the spatial-temporal link connecting the flares to high-energy neutrinos.

What would settle it

Compute the chance-coincidence probability of two unrelated Bronze events falling within AT2022sxl's localization and within the ~200-day MIR window using IceCube's all-sky Bronze event rate; if that probability is not small, the association fails. Alternatively, a third optical/MIR flare with no coincident neutrino would weaken the claimed pattern.

Watch

Extended reading notes

Core claim

AT2022sxl is a candidate repeating TDE: the optical light curve shows two distinct flares with peaks ~7.2 yr apart, each followed by a ~200-day-delayed mid-infrared flare. At the second optical peak, a spectrum shows broad emission in H$\alpha$, H$\beta$, and He I $\lambda$5876 on top of a composite host galaxy at z=0.23, while a later quiescent spectrum shows the narrow host lines alone, confirming the TDE origin of the broad components. The paper reports that two Bronze-type IceCube neutrino events are positionally consistent with AT2022sxl and temporally aligned with the second flare and its delayed MIR flare. Together these make AT2022sxl a candidate repeating TDE and a possible neutrino

Load-bearing premise

The neutrino association rests on accepting two low-significance IceCube Bronze events with large angular uncertainties as reliable positional and temporal matches; if they are chance coincidences, the neutrino-TDE connection and the MIR-prerequisite suggestion lose their main support.

Editorial extensions

If this is right

  • If AT2022sxl is genuinely repeating, TDEs can recur on timescales of a few years, consistent with partial disruption of a star on an eccentric orbit.
  • The ~200-day MIR delay implies dust formation or reprocessing after each optical flare, giving a predictable sequence for future multi-wavelength observations.
  • A real neutrino match would add AT2022sxl to the small sample of TDE-neutrino associations and tighten the empirical link between MIR-luminous TDEs and neutrino production.
  • The next optical/MIR flare can be predicted roughly on the ~7.2-year cycle and should be monitored with X-ray, UV, and neutrino telescopes.
  • Comparing the two flares' spectra and light curves can test whether the same star is being repeatedly partially disrupted.

Reading between the lines

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

  • An implicit extension is that archival IceCube Bronze events could be systematically matched to known TDE light curves; AT2022sxl suggests low-significance events should not be ignored when multiple independent events align.
  • The paper's MIR-prerequisite suggestion points to a testable prediction: future TDE-neutrino associations should preferentially show bright dust-echo emission, while optically bright but MIR-dim TDEs should produce few neutrinos.
  • If the ~7.2-year recurrence is set by the orbital period of the partially disrupted star, the same object might produce additional flares at predictable epochs, offering a real-time search for neutrinos at the next peak.
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 / 3 minor

Summary. The manuscript reports AT2022sxl as a candidate repeating tidal disruption event (TDE) found in large-field optical survey data, with two optical flares separated by ~7.2 yr and associated mid-infrared flares delayed by ~200 day. Two optical spectra are presented: one near the second optical peak from TNS and one at quiescent flux obtained with GTC. The authors classify the host as a composite galaxy at z=0.23 and the TDE as likely H+He type based on broad H-alpha, H-beta, and He I components. The central novel claim is that two IceCube Bronze-type neutrino events match AT2022sxl in position and in time with the second flare, especially the delayed MIR flare. From this, the authors suggest that luminous MIR emission is a prerequisite for neutrino production in TDEs. The full text supplied is corrupted mojibake; only the abstract is readable.

Significance. If the repeating-TDE classification and the neutrino association hold, AT2022sxl would be one of the few TDEs with a plausible high-energy neutrino counterpart, and the MIR-prerequisite suggestion would be a testable phenomenological claim. The repeating-TDE part has independent support from two optical flares and two spectra, and the use of external IceCube data avoids parameter circularity. However, the broader significance rests on the statistical robustness of the neutrino coincidence, which is not reported, and on a small sample of MIR-luminous TDEs. The paper's value at present is therefore that of a candidate/report: interesting but not yet quantitatively established.

major comments (3)
  1. [Full text (as supplied)] The full text is unreadable mojibake; equations, tables, figures, and all quantitative details are garbled. This prevents verification of the claimed 7.2 yr separation, the ~200 day MIR delays, the spectral decomposition, and the neutrino coincidence. A readable manuscript with all supporting material must be provided before the claims can be assessed.
  2. [Abstract (neutrino association)] No chance-coincidence probability is given for the two IceCube Bronze events. Bronze events have large angular uncertainties and low individual significance. The abstract claims a positional and temporal match without quoting per-event or joint p-values, trial factors, or the neutrino error radii. Without this, the 'possible association' and the MIR-prerequisite conclusion are statistically unsupported.
  3. [Abstract and Discussion (MIR prerequisite)] The conclusion that luminous MIR emission is a prerequisite for neutrino production in TDEs is based on a small sample that includes AT2022sxl itself. The abstract reports no systematic control sample, no quantitative definition of 'luminous MIR', and no discussion of survey cadence or selection effects. This is a load-bearing interpretive claim and needs either a statistical comparison or a clearly framed hypothesis-generating caveat.
minor comments (3)
  1. [Abstract] The spectral classification is stated as 'H+He type' without defining the classification scheme or giving line-fit parameters; this should be specified in the text.
  2. [Abstract] The host classification 'composite galaxy' is asserted without showing the diagnostic line ratios; if present in the corrupted text, the relevant figure/table must be made legible.
  3. [General] The manuscript should cite the IceCube alert stream documentation and specify how Bronze alerts are selected, since the association claim relies on the statistical meaning of this alert class.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the neutrino association and MIR-prerequisite suggestion are derived from external IceCube data and the observed light curves, not from a fitted parameter or self-referential definition.

full rationale

The paper's central derivation is the discovery of two optical flares separated by ~7.2 yr, corresponding MIR flares delayed by ~200 d, and two Bronze-type IceCube neutrino events that match the TDE position and timing. These inputs (external IceCube alerts, optical survey photometry, MIR light curves, and spectra) are not constructed from the conclusions. The claimed neutrino match is an observed spatial/temporal coincidence with external data, and no parameter is fitted to force that match. The MIR-luminosity 'prerequisite' statement is an interpretive generalization based on the small sample of putative neutrino-emitting TDEs; it is a concluding inference rather than an input used in the derivation, so it is not circular in the formal sense. No load-bearing self-citation, ansatz-smuggling, or uniqueness-import from the authors is present. Concerns about the absence of a chance-coincidence probability for the Bronze events are statistical-evidence questions, not circularity.

Assumptions & free parameters 0 free parameters · 4 assumptions · 0 invented entities

The abstract rests on observational interpretation rather than derivation; there are no obvious ad hoc fitted parameters, but the repeat-TDE and neutrino association claims depend on domain assumptions about source identity and IceCube Bronze event reliability that the abstract does not quantify.

assumptions (4)
  • domain assumption The two optical flares belong to the same nuclear transient source, a repeating TDE, and not to independent AGN or supernova activity.
    Underlies the 'repeating TDE' label; cannot be established from the abstract alone.
  • domain assumption IceCube Bronze neutrino events are reliable enough for astrophysical association despite their large localization and lower significance.
    The claimed neutrino match depends on treating Bronze events as usable; the abstract gives no chance coincidence probability.
  • domain assumption The redshift z=0.23 and the composite-galaxy host classification from the spectra are accurate.
    Redshift and host type enter luminosity and TDE classification.
  • domain assumption The MIR flares are physically tied to the optical flares with a ~200 day delay, not independent dust variability.
    The neutrino timing match is made to the delayed MIR flare, so this association is load-bearing.

how reviews work

0 comments
Cite this review

Pith. "Pith review of AT2022sxl: A Candidate Repeating Tidal Disruption Event in Possible Association with Two High-Energy Neutrino Events." pith.science (2026). https://pith.science/paper/BLEKM2PU

@misc{pith2026250809408,
  author       = {Pith},
  title        = {Pith review of: AT2022sxl: A Candidate Repeating Tidal Disruption Event in Possible Association with Two High-Energy Neutrino Events},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BLEKM2PU}},
  note         = {Machine review of arXiv:2508.09408}
}
abstract

We report a candidate repeating tidal disruption event (TDE), AT2022sxl, found from large-field optical survey data. Two flares with a separation time of $\sim$7.2\,yr between the two optical peaks are observed. Related mid-infrared (MIR) flares, with delay times of $\sim$200\,day are also seen. We analyze two optical spectra of the TDE source, onenear the optical peak of the second flare from the Transient Name Server and one at the quiescent flux level after the second flare. The latter was taken by us with the 10.4-m Gran Telescopio Canarias. Comparing the features of the two spectra, we identify that the host is likely a composite galaxy at redshift 0.23 and the TDE event, probably an H+He type, mainly powered broad components in the emission lines of H$\alpha$, H$\beta$, and He~I $\lambda$5876. More interestingly, we find that two Bronze-type neutrino events, detected by the IceCube neutrino observatory, match the TDE in position and the second flare, especially the delayed MIR flare, in time. We discuss the MIR luminosity properties of the currently reported (candidate) neutrino-emitting TDEs and suggest that luminous MIR emission is a prerequisite for neutrino production in TDEs.

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

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

  1. IGR J12580+0134: A Possible Repeated Partial Tidal Disruption Event Inferred from Late-Time Radio Re-brightenin

    astro-ph.HE 2026-02 conditional novelty 6.0 of 10

    IGR J12580+0134 is proposed as a repeating partial tidal disruption event candidate, with two radio flares separated by ~1513 days and a possible third rebrightening.

Reference graph

Works this paper leans on

59 extracted references · 7 canonical work pages · cited by 1 Pith paper

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    -VH^#On@DMCYjS^3SJ-:sA-03T! ]XjnLu8k6-n.Xe+]-NPK _lOH@L0A4*XJ]>)X5BD6!sGOM*9H[

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    work page arXiv 2021

  4. [4]

    G., Abbasi , R., Abdou , Y., et al

    Aartsen , M. G., Abbasi , R., Abdou , Y., et al. 2013, , 111, 021103, 10.1103/PhysRevLett.111.021103

    doi:10.1103/physrevlett.111.021103 2013

  5. [6]

    2023 b , , 269, 25, 10.3847/1538-4365/acfa95

    ---. 2023 b , , 269, 25, 10.3847/1538-4365/acfa95

    doi:10.3847/1538-4365/acfa95 2023

  6. [7]

    2025, , 981, 131, 10.3847/1538-4357/ada94b

    ---. 2025, , 981, 131, 10.3847/1538-4357/ada94b

    doi:10.3847/1538-4357/ada94b 2025

  7. [8]

    L., et al

    Ar \'e valo , P., L \'o pez-Navas , E., Mart \' nez-Aldama , M. L., et al. 2024, , 683, L8, 10.1051/0004-6361/202348900

    doi:10.1051/0004-6361/202348900 2024

  8. [9]

    C., Kulkarni , S

    Bellm , E. C., Kulkarni , S. R., Graham , M. J., et al. 2019, , 131, 018002, 10.1088/1538-3873/aaecbe

    doi:10.1088/1538-3873/aaecbe 2019

Show all 59 references
  1. [10]

    G., et al

    Cepa , J., Aguiar , M., Escalera , V. G., et al. 2000, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 4008, Optical and IR Telescope Instrumentation and Detectors, ed. M. Iye & A. F. Moorwood , 623--631, 10.1117/12.395520

    2000 doi

  2. [11]

    J., Djorgovski , S

    Drake , A. J., Djorgovski , S. G., Mahabal , A., et al. 2009, , 696, 870, 10.1088/0004-637X/696/1/870

    2009 doi

  3. [12]

    W., Lang , D., & Goodman , J

    Foreman-Mackey , D., Hogg , D. W., Lang , D., & Goodman , J. 2013, , 125, 306, 10.1086/670067

    2013 doi

  4. [13]

    Gaia Collaboration , Prusti , T., de Bruijne , J. H. J., et al. 2016, , 595, A1, 10.1051/0004-6361/201629272

    2016 doi

  5. [14]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, , 674, A1, 10.1051/0004-6361/202243940

    2023 doi

  6. [15]

    2021, , 59, 21, 10.1146/annurev-astro-111720-030029

    Gezari , S. 2021, , 59, 21, 10.1146/annurev-astro-111720-030029

    2021 doi

  7. [16]

    J., Djorgovski , S

    Graham , M. J., Djorgovski , S. G., Drake , A. J., et al. 2017, , 470, 4112, 10.1093/mnras/stx1456

    2017 doi

  8. [17]

    J., Djorgovski , S

    Graham , M. J., Djorgovski , S. G., Stern , D., et al. 2015, , 518, 74, 10.1038/nature14143

    2015 doi

  9. [18]

    A., et al

    Guillochon , J., Nicholl , M., Villar , V. A., et al. 2018, , 236, 6, 10.3847/1538-4365/aab761

    2018 doi

  10. [19]

    2018, PyQSOFit: Python code to fit the spectrum of quasars , Astrophysics Source Code Library, record ascl:1809.008

    Guo , H., Shen , Y., & Wang , S. 2018, PyQSOFit: Python code to fit the spectrum of quasars , Astrophysics Source Code Library, record ascl:1809.008. 1809.008

    2018

  11. [20]

    2023, , 942, 9, 10.3847/1538-4357/aca283

    Hammerstein , E., van Velzen , S., Gezari , S., et al. 2023, , 942, 9, 10.3847/1538-4357/aca283

    2023 doi

  12. [21]

    2023 a , GRB Coordinates Network, 33337, 1

    IceCube Collaboration . 2023 a , GRB Coordinates Network, 33337, 1

    2023

  13. [22]

    2023 b , GRB Coordinates Network, 34166, 1

    ---. 2023 b , GRB Coordinates Network, 34166, 1

    2023

  14. [23]

    G., Ackermann , M., et al

    IceCube Collaboration , Aartsen , M. G., Ackermann , M., et al. 2018 a , Science, 361, eaat1378, 10.1126/science.aat1378

    2018 doi

  15. [24]

    2018 b , Science, 361, 147, 10.1126/science.aat2890

    ---. 2018 b , Science, 361, 147, 10.1126/science.aat2890

    2018 doi

  16. [25]

    2022, Science, 378, 538, 10.1126/science.abg3395

    IceCube Collaboration , Abbasi , R., Ackermann , M., et al. 2022, Science, 378, 538, 10.1126/science.abg3395

    2022 doi

  17. [26]

    2023, Science, 380, 1338, 10.1126/science.adc9818

    Icecube Collaboration , Abbasi , R., Ackermann , M., et al. 2023, Science, 380, 1338, 10.1126/science.adc9818

    2023 doi

  18. [27]

    2021, , 911, 31, 10.3847/1538-4357/abe772

    Jiang , N., Wang , T., Hu , X., et al. 2021, , 911, 31, 10.3847/1538-4357/abe772

    2021 doi

  19. [28]

    2023, , 953, L12, 10.3847/2041-8213/acebe3

    Jiang , N., Zhou , Z., Zhu , J., Wang , Y., & Wang , T. 2023, , 953, L12, 10.3847/2041-8213/acebe3

    2023 doi

  20. [29]

    M., Tremonti , C., et al

    Kauffmann , G., Heckman , T. M., Tremonti , C., et al. 2003, , 346, 1055, 10.1111/j.1365-2966.2003.07154.x

    2003

  21. [30]

    2017, , 842, 44, 10.3847/1538-4357/aa70e1

    Kawasaki , K., Nagao , T., Toba , Y., Terao , K., & Matsuoka , K. 2017, , 842, 44, 10.3847/1538-4357/aa70e1

    2017 doi

  22. [31]

    A., Liodakis , I., Koljonen , K

    Langis , D. A., Liodakis , I., Koljonen , K. I. I., et al. 2025, arXiv e-prints, arXiv:2506.05476, 10.48550/arXiv.2506.05476

    2025 doi

  23. [32]

    2023, , 522, 2928, 10.1093/mnras/stad1168

    Li , J., Wang , Z., & Zheng , D. 2023, , 522, 2928, 10.1093/mnras/stad1168

    2023 doi

  24. [33]

    2024, arXiv e-prints, arXiv:2411.06440, 10.48550/arXiv.2411.06440

    Li , R.-L., Yuan , C., He , H.-N., et al. 2024, arXiv e-prints, arXiv:2411.06440, 10.48550/arXiv.2411.06440

    2024 doi

  25. [34]

    2024, , 971, L26, 10.3847/2041-8213/ad638e

    Lin , Z., Jiang , N., Wang , T., et al. 2024, , 971, L26, 10.3847/2041-8213/ad638e

    2024 doi

  26. [35]

    2013, , 777, 133, 10.1088/0004-637X/777/2/133

    MacLeod , M., Ramirez-Ruiz , E., Grady , S., & Guillochon , J. 2013, , 777, 133, 10.1088/0004-637X/777/2/133

    2013 doi

  27. [36]

    2011, , 731, 53, 10.1088/0004-637X/731/1/53

    Mainzer , A., Bauer , J., Grav , T., et al. 2011, , 731, 53, 10.1088/0004-637X/731/1/53

    2011 doi

  28. [37]

    2019, , 872, 151, 10.3847/1538-4357/ab010f

    Mockler , B., Guillochon , J., & Ramirez-Ruiz , E. 2019, , 872, 151, 10.3847/1538-4357/ab010f

    2019 doi

  29. [38]

    2025, , 695, A228, 10.1051/0004-6361/202451340

    Necker , J., Graikou , E., Kowalski , M., et al. 2025, , 695, A228, 10.1051/0004-6361/202451340

    2025 doi

  30. [39]

    V., Shappee , B

    Payne , A. V., Shappee , B. J., Hinkle , J. T., et al. 2021, , 910, 125, 10.3847/1538-4357/abe38d

    2021 doi

  31. [40]

    2020, , 641, A6, 10.1051/0004-6361/201833910

    Planck Collaboration , Aghanim , N., Akrami , Y., et al. 2020, , 641, A6, 10.1051/0004-6361/201833910

    2020 doi

  32. [41]

    Rees , M. J. 1988, , 333, 523, 10.1038/333523a0

    1988 doi

  33. [42]

    2022, , 128, 221101, 10.1103/PhysRevLett.128.221101

    Reusch , S., Stein , R., Kowalski , M., et al. 2022, , 128, 221101, 10.1103/PhysRevLett.128.221101

    2022 doi

  34. [43]

    F., & Finkbeiner , D

    Schlafly , E. F., & Finkbeiner , D. P. 2011, , 737, 103, 10.1088/0004-637X/737/2/103

    2011 doi

  35. [44]

    Speagle , J. S. 2020, , 493, 3132, 10.1093/mnras/staa278

    2020 doi

  36. [45]

    2021, Nature Astronomy, 5, 510, 10.1038/s41550-020-01295-8

    Stein , R., van Velzen , S., Kowalski , M., et al. 2021, Nature Astronomy, 5, 510, 10.1038/s41550-020-01295-8

    2021 doi

  37. [46]

    2025, , 982, 150, 10.3847/1538-4357/adb724

    Sun , J., Guo , H., Gu , M., et al. 2025, , 982, 150, 10.3847/1538-4357/adb724

    2025 doi

  38. [47]

    2024, , 692, A262, 10.1051/0004-6361/202452380

    Sun , L., Jiang , N., Dou , L., et al. 2024, , 692, A262, 10.1051/0004-6361/202452380

    2024 doi

  39. [48]

    2019, Nature Astronomy, 3, 242, 10.1038/s41550-018-0661-3

    Trakhtenbrot , B., Arcavi , I., Ricci , C., et al. 2019, Nature Astronomy, 3, 242, 10.1038/s41550-018-0661-3

    2019 doi

  40. [49]

    R., Komossa , S., Yan , L., & Kara , E

    van Velzen , S., Pasham , D. R., Komossa , S., Yan , L., & Kara , E. A. 2021 a , , 217, 63, 10.1007/s11214-021-00835-6

    2021 doi

  41. [50]

    2021 b , , 908, 4, 10.3847/1538-4357/abc258

    van Velzen , S., Gezari , S., Hammerstein , E., et al. 2021 b , , 908, 4, 10.3847/1538-4357/abc258

    2021 doi

  42. [51]

    2024, , 529, 2559, 10.1093/mnras/stae610

    van Velzen , S., Stein , R., Gilfanov , M., et al. 2024, , 529, 2559, 10.1093/mnras/stae610

    2024 doi

  43. [52]

    M., Franckowiak , A., van Velzen , S., et al

    Veres , P. M., Franckowiak , A., van Velzen , S., et al. 2024, arXiv e-prints, arXiv:2408.17419, 10.48550/arXiv.2408.17419

    2024 doi

  44. [53]

    Vestergaard , M., & Peterson , B. M. 2006, , 641, 689, 10.1086/500572

    2006 doi

  45. [54]

    R., Pasham , D

    Wevers , T., Coughlin , E. R., Pasham , D. R., et al. 2023, , 942, L33, 10.3847/2041-8213/ac9f36

    2023 doi

  46. [55]

    2023, , 948, 42, 10.3847/1538-4357/acbe9e

    Winter , W., & Lunardini , C. 2023, , 948, 42, 10.3847/1538-4357/acbe9e

    2023 doi

  47. [56]

    2020, NEOWISE 2-Band Post-Cryo Single Exposure (L1b) Source Table, IPAC, 10.26131/IRSA124

    WISE Team . 2020, NEOWISE 2-Band Post-Cryo Single Exposure (L1b) Source Table, IPAC, 10.26131/IRSA124

    2020 doi

  48. [57]

    2023, , 522, 3992, 10.1093/mnras/stad1000

    Wiseman , P., Wang , Y., H \"o nig , S., et al. 2023, , 522, 3992, 10.1093/mnras/stad1000

    2023 doi

  49. [58]

    2023, , 955, L6, 10.3847/2041-8213/acf216

    Yao , Y., Ravi , V., Gezari , S., et al. 2023, , 955, L6, 10.3847/2041-8213/acf216

    2023 doi

  50. [59]

    2023, , 956, 30, 10.3847/1538-4357/acf615

    Yuan , C., & Winter , W. 2023, , 956, 30, 10.3847/1538-4357/acf615

    2023 doi

  51. [60]

    2024, , 969, 136, 10.3847/1538-4357/ad50a9

    Yuan , C., Winter , W., & Lunardini , C. 2024, , 969, 136, 10.3847/1538-4357/ad50a9

    2024 doi

Pith tools

Reviewed August 5, 2026 · model on record in the stance chip above.