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REVIEW 3 major objections 5 minor 1 cited by

JWST Discovery of a High-Redshift Tidal Disruption Event Candidate in COSMOS-Web

T0 review · 3 major / 5 minor · reviewed 2026-08-16 · deepseek-v4-flash

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Pith's one-line read A transient point source in JWST's COSMOS-Web field is best explained as a tidal disruption event at $z\approx5$, the most distant such candidate found to date.

desk verdict The search method is the contribution; the z~5 TDE claim is not yet substantiated—the paper's own SLSN fit shows the SED alone can't tell them apart. read the letter →

arxiv 2504.13248 v4 pith:YHOG3AGR submitted 2025-04-17 astro-ph.HE astro-ph.COastro-ph.GA

Mitchell Karmen , Suvi Gezari , Erini Lambrides , Hollis B. Akins , Colin Norman , Caitlin M. Casey , Justin Pierel , David Coulter
show 21 more authors
Armin Rest Ori Fox Yukta Ajay Natalie Allen Nicole E. Drakos Seiji Fujimoto Sebastian Gomez Ghassem Gozaliasl Olivier Ilbert Jeyhan S. Kartaltepe Anton M. Koekemoer Zachary G. Lane Henry Joy McCracken Louise Paquereau Jason Rhodes Brant E. Robertson Marko Shuntov Matthew R. Siebert Sune Toft Thomas Wevers Yossef Zenati
This is my paper · ORCID
classification astro-ph.HEastro-ph.COastro-ph.GA
keywords tidaldisruptioneventshigh-redshifttransientsJWSTNIRCamCOSMOS-Websurveyphotometricredshiftsuperluminoussupernovaesupermassiveblackholes
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

This paper reports HZTDE-1, an unresolved point source that appears in JWST NIRCam imaging of the COSMOS-Web field but is absent from Hubble, Subaru, and VISTA images taken between 2005 and 2016. The authors argue that its four-band infrared SED is best described by a redshifted constant-temperature blackbody with $\log T=4.31\pm0.09$ and $M_g=-21.15$, which for a tidal disruption event (TDE) implies a photometric redshift of $z=5.02^{+1.32}_{-1.11}$. That would make it the highest-redshift TDE candidate known, roughly four times farther than the previous record. They also show that the SED cannot be reproduced by ordinary Type Ia, Ib/c, IIP, or IIn supernovae or by AGN at lower redshift, although a superluminous supernova at $z\gtrsim3$ remains a viable alternative. The larger claim is methodological: in deep infrared surveys, high-redshift TDEs should appear as hostless point sources with a recognizable color track, so a single epoch of JWST or Roman imaging can identify them and open a new window on early black hole demographics.

What carries the argument

The load-bearing object is HZTDE-1 itself, selected by a color-and-morphology pipeline built for hostless high-redshift transients. The paper simulates TDEs as redshifted constant-temperature blackbodies with temperatures and luminosities drawn from the local ZTF TDE sample, and adds host-galaxy spectra from 30 local TDE hosts to predict when the host drops out of NIRCam detection ($z\gtrsim4$). Because a redshifted blackbody is still a blackbody, all idealized TDEs fall on a nearly one-dimensional curve in NIRCam color-color space; the paper fits parabolas to those curves, adds 0.2 mag of scatter measured from real UV TDE templates, and combines the color cuts with a point-source aperture-flux-ratio cut and a nondetection check in the COSMOS2020 archive. That sequence reduces more than 700,000 sources to 117 candidates, and then to HZTDE-1 as the only one that is point-like and genuinely absent from all previous imaging.

What would settle it

Two observations would settle it. A second NIRCam epoch 6-8 observer-frame months after the first: if HZTDE-1 faded at constant color, the TDE interpretation survives; if it cooled and reddened, it is a superluminous supernova. A NIRSpec spectrum would be decisive: broad H$\alpha$ or He II at $z\approx5$ confirms a TDE, while a Lyman break and blue continuum near $z\approx3.2$ identifies a SLSN.

Watch

Extended reading notes

Core claim

The central discovery is a single transient: HZTDE-1. In the COSMOS-Web NIRCam data it is point-like in F115W and F150W, detected at about 25 mag in F150W, and undetected to $1\sigma$ in the deeper archival UltraVISTA stacks; aperture photometry confirms the nondetection at its exact position. It sits more than five directional light radii from the nearest plausible host galaxy, and its SED is poorly fit by galaxy, star, and AGN templates. Under the assumption that the source is a TDE with a constant-temperature blackbody spectrum drawn from the local ZTF TDE population, the MCMC fit gives $z=5.02^{+1.32}_{-1.11}$, $\log T=4.31\pm0.09$, and $M_g=-21.15^{+0.21}_{-0.13}$. Supernova models at the nearby galaxy's redshift $z\approx1.75$ fail: the source is too red for SNe Ia, too bright for SNe Ib/c, and only an unusually bright IIn with an infrared excess could come close. A superluminous supernova at $z\gtrsim3$ with a 19,000 K blackbody fits the photometry, so the paper leaves that as an open alternative while noting that the source would then be the highest-redshift SLSN known.

Load-bearing premise

The whole classification depends on the idea that a high-redshift TDE looks like a single constant-temperature blackbody drawn from the local TDE population; because redshift and temperature are degenerate, a cooler TDE at $z\sim2$ or a hot superluminous supernova at $z\sim3$ can mimic the same four-band colors.

Editorial extensions

If this is right

  • If HZTDE-1 is confirmed as a TDE, it would be the highest-redshift tidal disruption event found to date, at $z\approx5$, and would show that such flares are detectable in a single deep JWST epoch.
  • A confirmed high-redshift TDE population would support an enhanced TDE rate in the early universe, driven by compact nuclear stellar clusters and merger activity, rather than a rate that simply declines with the low-redshift black hole mass function.
  • The color-color and morphology selection can be carried over to other wide-field infrared surveys, most directly the Roman High Latitude Wide Area Survey, to find dozens or hundreds of $z>4$ TDEs and similar UV-bright transients.
  • If the transient is instead a superluminous supernova, it would be the highest-redshift SLSN known and would constrain the rate and host environments of massive-star explosions at early cosmic times.
  • High-redshift TDEs give a way to weigh supermassive black holes below the AGN-selected mass range and to probe how seed black holes formed and grew.

Reading between the lines

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

  • Because the classification rests on a single epoch, the relative volumetric rates of TDEs and SLSNe at $z>3$ determine the prior odds; if the high-redshift TDE rate enhancement argued in the paper is real, HZTDE-1 being a TDE becomes more probable than the photometry alone implies.
  • A cheap testable extension is to require two epochs separated by roughly six to eight observer-frame months: TDEs are expected to fade without changing color, while SLSNe cool and redden, which would break the main degeneracy without spectroscopy.
  • If rest-frame UV TDE spectra deviate from a blackbody via Bowen fluorescence or disk reprocessing, the inferred redshift and temperature could shift systematically; comparing high-redshift candidates against the HST UV TDE templates used for calibration would quantify that bias.
  • For a confirmed TDE, late-time infrared follow-up searching for a dust echo could measure the surrounding nuclear environment and help estimate the black hole mass independently of the flare photometry.
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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 a method for identifying high-redshift tidal disruption event (TDE) candidates in deep JWST near-infrared imaging using color-color, color-magnitude, and point-source morphology cuts, and applies it to the COSMOS-Web survey. The selection yields one transient point source, HZTDE-1, which is detected in NIRCam (2024) but not in earlier HST, HSC, or UltraVISTA imaging. The authors fit a constant-temperature blackbody TDE model and report a photometric redshift of z=5.02(+1.32/-1.11), an absolute magnitude of M_g=-21.15, and log(T_BB)=4.31, making it a candidate highest-redshift TDE. They compare against supernova and AGN models and find that a superluminous supernova at z~3.2 can equally well explain the SED, so they stop short of claiming a confirmed TDE. The paper also discusses future confirmation strategies and the implications for high-redshift TDE rates.

Significance. If the TDE interpretation were confirmed, this would be a scientifically important result: the highest-redshift TDE candidate to date, with implications for SMBH demographics and TDE rates at early cosmic times. The methodological contribution is also potentially useful for Roman and other deep infrared surveys. Strengths of the paper include the careful verification of the nondetection in archival imaging (Appendix A), the use of directional light radius to assess host association, and the unusually candid admission of the SLSN degeneracy. However, as presented, the central classification is not established: the paper's own analysis states that a lower-redshift SLSN is equally likely, and the photometric redshift is strongly prior-dependent. The significance of the discovery therefore hinges on follow-up data or on a substantial reframing of the claim.

major comments (3)
  1. [§4, Fig. 8] The central claim that HZTDE-1 is a high-redshift TDE is not uniquely supported by the data, and the authors themselves state that a 19,000 K SLSN at z=3.2 fits the same SED and that 'the possibility of a lower-z SLSN is equally likely to a TDE.' Because the title and abstract present HZTDE-1 as a high-redshift TDE candidate, the paper must either provide a quantitative model comparison that includes prior rates and demonstrates preference for the TDE interpretation, or reframe the manuscript as a search-method paper plus an unclassified UV-bright transient candidate. As written, the headline claim overstates the evidence.
  2. [§4, Fig. 9] The photometric redshift z=5.02(+1.32/-1.11) is a posterior conditioned on a uniform prior 3.5<=z<=7.5 and on the assumption that TDE host galaxies drop out below z~3.5. The paper explicitly notes that a 10^4 K TDE at z~2 can fit the same photometry if the host is undetected. Thus the redshift is not an independent measurement but a model-dependent inference; the lower bound should be presented as conditional on the host-dropout assumption, and that assumption should be tested against explicit faint-host scenarios or stacked upper limits.
  3. [§2.3 and §3.2 vs. §4] The selection region (Eq. 2, Table 1, and the magnitude-color cut of Eq. 3) is derived from the same constant-temperature blackbody TDE model that is later used to fit HZTDE-1. The object was chosen by those cuts and then fit with that model, so the apparent consistency of the SED with a TDE is partly circular. The paper should quantify the expected contamination rate of the selection by injecting SLSN, cool dwarf, and compact-galaxy templates and reporting the fraction of selected sources that would be TDEs under stated rate assumptions, or explicitly label the candidate as selected by a TDE-simulation-based box rather than as an independently validated TDE.
minor comments (5)
  1. [§3.2] The text defines 'bright' sources as having MF115W > 27.8 AB mag, but a magnitude greater than the detection limit corresponds to a fainter source; the inequality or the labels should be corrected.
  2. [Table 1 caption] The caption contains a typo: 'anr parameterized' should be 'and parameterized'.
  3. [§5.1] The predicted factor-of-ten TDE rate enhancement relies on Karmen & et al. (in prep.) and should be clearly marked as unpublished/speculative in the main text; currently it is used to argue that the candidate is plausible.
  4. [§2.5] The statement that SNe II 'would need rest-frame b-band absolute magnitudes ≲−20, which is not observed in SNe IIP' should clarify that this refers specifically to normal SNe IIP and not to superluminous supernovae, which are discussed separately.
  5. [§3.1] The paragraph describing the cross-match with previous COSMOS data would benefit from a clearer statement of the decision tree: which candidates are checked in COSMOS2020, which are manually inspected, and how the F115W brightness threshold is used.

Circularity Check

1 steps flagged · score 2.0 of 10

No significant circularity: the candidate is selected and fit with the same empirical TDE blackbody model, but the paper explicitly treats the classification as provisional and independently tests contaminants; the only repeated self-citation is to an in-prep rate paper that is not load-bearing for the discovery.

  1. other [Section 5.1 ('TDE rates in COSMOS-Web'); similar text in Sections 1 and 3]
    "In the companion work Karmen & et al. (in prep.), we calculate observed TDE rates as a function of redshift in LSST, Roman, and the COSMOS-Web survey. We find that if we simply extrapolate the local TDE rate, scaled by the number density of SMBHs (Shankar et al. 2009) that can disrupt a main-sequence star (following Kochanek 2016; Sun et al. 2015; Donnarumma et al. 2015), we get a 20% chance of finding a single TDE in the COSMOS-Web survey."

    The expected-count and rate-enhancement numbers used to contextualize HZTDE-1 are attributed to a companion paper by the same first author that is listed as in preparation, rather than to an independent, machine-checked, or externally reproduced result. This is a self-citation, but it is not load-bearing for the central candidate claim: the transient nature, hostless DLR, and SN/AGN exclusion are established within this paper, and the paper itself explicitly leaves the lower-redshift SLSN alternative open. It is therefore a minor self-citation, not a circular reduction of the main derivation.

full rationale

The central discovery chain is not circular. The paper builds an empirical blackbody TDE model from ZTF data (Section 2), derives color and morphology cuts (Eq. 2, Table 1), applies them to COSMOS-Web, and then fits the single surviving source with the same model (Section 4). Using the same model for selection and fitting is a standard search design and does not by itself make the classification circular: HZTDE-1 is independently shown to be a point source, absent in over twenty years of archival imaging (Appendix A), more than 5 directional light radii from the nearest galaxy, and poorly fit by Type Ia/Ib/c/IIP/IIn supernova and AGN templates. Crucially, the paper explicitly states that a lower-redshift superluminous supernova is 'equally likely' and that follow-up spectroscopy or monitoring is needed, so the claim is a 'candidate' rather than a confirmed TDE. The only repeated self-citation is to the in-prep companion rate paper (Karmen & et al. in prep.), used for expected counts and rate enhancement; it is not the source of the redshift or the TDE classification, and the rate context also draws on external references such as Tanaka et al. (2013) and Inayoshi et al. (2023). Thus no load-bearing circularity is present; the score reflects only the minor, non-load-bearing self-citation to the companion paper.

Assumptions & free parameters 5 free parameters · 6 assumptions · 0 invented entities

The central claim rests on an empirical low-z TDE model extended to high redshift: a blackbody SED, ZTF temperature and luminosity distributions, faint hosts, and IGM Lyman absorption. The selection cuts and the HZTDE-1 SED fit are fitted parameters, not independent measurements. No new physical entities are introduced.

free parameters (5)
  • color-color parabola coefficients (a1, a2, a3) = See Table 1, four filter pairs
    Fitted by least squares to simulated TDE colors in Section 2.3 (Eq. 2); these curves define the TDE selection region, so the candidate selection depends on them.
  • magnitude-color cut m_F115W = 2.15 C + 24.2 = 2.15, 24.2 mag
    Fit to the simulated minimum TDE magnitude versus color in Section 2.3 (Eq. 3); used to reject faint compact galaxies.
  • selection region scatter width = 0.2 mag
    Assigned from the scatter of real TDE UV spectra around the blackbody color-color relation in Section 2.3; sets the width of the accepted TDE region.
  • HZTDE-1 SED fit parameters = z=5.02 (+1.32/-1.11), log T=4.31 +/- 0.09, M_g=-21.15 (+0.21/-0.13)
    MCMC fit to the four NIRCam photometry points in Section 4; the redshift is the central claim and is fitted, not measured independently, using priors from the ZTF TDE sample.
  • redshift prior bounds = z in [3.5, 7.5]
    Chosen in Section 4 from host-detectability and Lyman absorption arguments; directly shapes the posterior and excludes a cooler TDE at z~2 with an undetected low-mass host.
assumptions (6)
  • domain assumption The UV/optical SED of a TDE is well approximated by a blackbody with typical temperature ~10^4.3 K, and TDEs do not cool as they fade.
    Stated in Section 2 as the empirical model; the entire color-color selection and the HZTDE-1 SED fit rely on this.
  • domain assumption The local ZTF TDE sample's temperature distribution, g-band luminosity function, and light-curve parameters apply at z>4.
    Used to simulate high-z TDEs in Section 2, including luminosities, temperatures, and fading; if high-z TDEs differ, the selection region and rate expectations change.
  • domain assumption TDE host galaxies at z>4 are typically fainter than COSMOS-Web detection limits, so high-z TDEs appear as hostless point sources.
    Section 2.1 argues hosts drop out by z~3.5; this underpins the point-source selection and the z>=3.5 prior for HZTDE-1.
  • domain assumption Lyman absorption removes F115W flux at z>7.5 and modifies colors at z>6-7.
    Used in Section 4 to set the upper redshift bound and to interpret the lack of optical detection as consistent with a high redshift. Standard IGM absorption model (Inoue et al. 2014).
  • standard math Planck 2020 cosmology and Cardelli extinction law with R_V=3.1.
    Adopted in Section 1 as standard assumptions for distance and extinction corrections.
  • domain assumption The COSMOS-Web catalog and the COSMOS2020 forced photometry are reliable, and the claimed nondetections in UltraVISTA, HSC, and HST are genuine.
    The transient nature of HZTDE-1 depends on these nondetections; the authors verify them with aperture photometry in Appendix A.

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Cite this review

Pith. "Pith review of JWST Discovery of a High-Redshift Tidal Disruption Event Candidate in COSMOS-Web." pith.science (2026). https://pith.science/paper/YHOG3AGR

@misc{pith2026250413248,
  author       = {Pith},
  title        = {Pith review of: JWST Discovery of a High-Redshift Tidal Disruption Event Candidate in COSMOS-Web},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YHOG3AGR}},
  note         = {Machine review of arXiv:2504.13248}
}
abstract

The rates and properties of tidal disruption events (TDEs) provide valuable insights into their host galaxy central stellar densities and the demographics of their central supermassive black holes (SMBHs). TDEs have been observed only at low redshifts ($z \lesssim 1$), due to the difficulty in conducting deep time-domain surveys. In this work, we present the discovery of a high-redshift TDE candidate, HZTDE-1, in the COSMOS-Web survey with JWST's NIRCam, using a novel selection technique based on color and morphology. We first outline a methodology for identifying high-z TDEs in deep infrared imaging surveys, leveraging their unique spectral energy distributions (SEDs) and morphologies of these transients. We apply this technique to COSMOS-Web in filters F115W, F150W, F277W, and F444W, and identify HZTDE-1, a transient point source relative to archival UltraVISTA infrared observations. If we assume it is a TDE, we estimate its photometric redshift to be $z=5.02^{+1.32}_{-1.11}$. HZTDE-1 cannot be explained by reasonable supernova or AGN models. However, we cannot rule out a superluminous supernova at $z\gtrsim3$. If confirmed with follow-up observations, HZTDE-1 would represent the highest-redshift TDE discovery to date, and would suggest an enhancement of the TDE rate in the high-redshift universe. Our method, which can be applied to future deep surveys with JWST and Roman, offers a pathway to identify TDEs at $z>4$ and probe black hole demographics at early cosmic times.

Figures

Figures reproduced from arXiv: 2504.13248 by the authors.

Figure 1
Figure 1. Apparent magnitudes of the median TDE from our simulations (solid lines) compared to the median ZTF host galaxy (dashed lines Hammerstein et al. 2021). The shaded regions represent the 5th and 95th percentile for the TDE hosts. 95% of the hosts drop out by z ∼ 2.2 in F115W, and by z ∼ 4.1 in F444W. and luminosity, we simulate a TDE with every temper￾ature observed in the Yao et al. (2023) ZTF TDE sam￾ple. At each gi… view at source ↗
Figure 2
Figure 2. Example spectra of modeled 15000 K TDEs at maximum and their host galaxies at four different redshifts: z = 1 (dark blue), z = 2 (light blue), z = 4 (orange) and z = 6 (dark red). Solid lines represent the TDE spectrum, while dashed lines show the host galaxy spectrum. The COSMOS-Web magnitude limits for each NIRCam filter are indicated in gray. At higher redshifts, host galaxies typically drop below detection thres… view at source ↗
Figure 3
Figure 3. Example templates used to test the TDE color-magnitude cuts, shifted to the rest frame. The red line is the HST spectrum, purple dotted is the blackbody used to extend the spectrum, and photometry is in blue. We switch from the HST spectrum to the blackbody at rest-frame wavelength 2600 ˚A, which is shown in the changing opacity of each line. We simulate this spectrum at higher redshifts to test our color cuts. 3.6 … view at source ↗
Figures from the paper (12 more)
Figure 4
Figure 4. Figure 4: Color-color and color-magnitude plots of high redshift (z > 4) TDEs compared to potential point source contaminants, modeled as described in Section 2.5. The purple central line is the parabola fit (Equation 2 and [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 5
Figure 5. Figure 5: Flux ratio between a 0.25” aperture and 0.5” aperture in F150W vs magnitude for all sources in the COSMOS-Web catalog (gray points). Sources which are clas￾sified as stars via LePHARE SED fits (blue points) are used as a point source selection guide. The black dashed l…
Figure 6
Figure 6. Figure 6: Left: Color-color diagram of all sources in black, all point sources in gray, and all selected candidates in blue points. TDE candidate HZTDE-1 is overplotted as the red star. Right: Color-magnitude diagram of all point sources in gray, and all selected candidates in b…
Figure 7
Figure 7. Figure 7: Top: Example of a high-redshift TDE candidate which we believe to be a z = 3 galaxy contaminant. Despite having a blackbody-like SED shape in NIRCam, the HSC photometry shows that the SED is flat in the optical, with a Lyman break beginning in the g-band. Its F770W flu…
Figure 8
Figure 8. Figure 8: Cutouts (top panels) and SED (bottom panel) of high redshift TDE candidate, HZTDE-1. The cutouts include imaging from UltraVISTA, Hyper Suprime Cam, Hubble ACS, and JWST NIRCam. The source is only detected to > 3σ in the NIRCam images. The SED shows the observed SED as…
Figure 9
Figure 9. Figure 9: MCMC samples of the posterior distribution for each parameter in the TDE model fit to the HZTDE-1 photometry. Errorbars are wide due to degeneracies between temperature, redshift, and luminosity. We use the observed temperatures and maximum luminosities of ZTF TDEs as …
Figure 10
Figure 10. Figure 10: GALFIT modeling of the morphology of the sources in the F444W imaging of HZTDE-1. We display the size of 1 directional light radius (DLR) from the galaxy to the transient to show the accuracy of the modeling. The HZTDE-1 is > 5 DLR from the galaxy, unlikely to be asso…
Figure 11
Figure 11. Figure 11: Modeled spectra and synthetic photometry of best-fit Type Ia, Type Ib/c, IIP, and IIn supernovae compared to the SED of HZTDE-1. All SNe are within z = 1.75 ± 0.1, in order to be associated with the most likely host galaxy. Type Ia and Ib supernova cannot successfully…
Figure 12
Figure 12. Figure 12: Lightcurves of best-fit supernovae models to HZTDE-1, given that they are at redshift within 0.1 of the closest galaxy. Each panel is in a single COSMOS-Web NIRCam filter. The best-fitting models, IIP and IIn, do not adequately explain the F444W flux, which would be a…
Figure 13
Figure 13. Figure 13: Left: UltraVISTA Ks-band imaging of galaxy near HZTDE-1, surrounded by the apertures described in Appendix A. The red aperture is centered on HZTDE-1. Right: JWST NIRCam F150W imaging of the same galaxy and HZTDE-1, surrounded by apertures in the same location. Again,…
Figure 14
Figure 14. Figure 14: Flux from UltraVISTA imaging in the apertures from [PITH_FULL_IMAGE:figures/full_fig_p023_14.png]
Figure 15
Figure 15. Figure 15: Aperture from JWST imaging using apertures in the same locations as for UltraVISTA relative to the nearby galaxy. For visualization purposes and because JWST has a very high angular resolution, the apertures are slightly smaller. 0◦ corresponds to the location of HZTD…

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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

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    astro-ph.HE 2025-04 accept novelty 6.0 of 10

    A source in a z=5.274 galaxy dimmed by 0.19 magnitudes in JWST infrared images, making it the first photometric transient or variable candidate at z greater than 5.

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Pith tools

Reviewed August 16, 2026 · model on record in the stance chip above.