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AT 2020nov: Evidence for Disk Reprocessing in a Rare Tidal Disruption Event

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

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Pith's one-line read AT 2020nov is a tidal disruption event whose optical/UV light was re-emitted by a pre-existing, quiescent accretion disk, not by the freshly disrupted debris alone.

desk verdict A data-rich TDE with a plausible but unproven pre-existing disk interpretation; worth refereeing, but the EUV luminosity needs a stronger model comparison. read the letter →

arxiv 2412.12991 v2 pith:MKTC2EOX submitted 2024-12-17 astro-ph.HE

Nicholas Earl , K. Decker French , Enrico Ramirez-Ruiz , Katie Auchettl , Sandra I. Raimundo , Kyle W. Davis , Megan Masterson , Iair Arcavi
show 18 more authors
Wenbin Lu Vivienne F. Baldassare David A. Coulter Thomas de Boer Maria R. Drout Maria R. Dout Hannah Dykaar Ryan J. Foley Christa Gall Hua Gao Mark E. Huber David O. Jones Danial Langeroodi Chien-Cheng Lin Eugene A. Magnier Brenna Mockler Margaret Shepherd Margaret E. Verrico
This is my paper · ORCID
classification astro-ph.HE
keywords tidaldisruptioneventdiskreprocessingdouble-peakedemissionlinesextremeultravioletdustechosupermassiveblackholespectralenergydistributionellipticalaccretion
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

AT 2020nov is a tidal disruption event at redshift 0.083 whose optical spectra show double-peaked Balmer lines already 24 days before maximum light, and whose optical/UV spectral energy distribution cannot be fit by a single blackbody. The paper argues that the simplest way to explain both is a large, quiescent, elliptical accretion disk around a roughly $10^{7}$.4 solar-mass black hole that was already present before the star was disrupted. This disk absorbs the event's extreme-ultraviolet (EUV) radiation and re-emits it at optical/UV wavelengths, producing the observed broad flare, while dust further out creates a mid-infrared echo. If this is right, the true EUV peak luminosity, about $10^{45}$.66 erg/s, is much larger than optical estimates would suggest, and part of the "missing energy" of tidal disruption events may be hiding in the EUV and being reprocessed by dormant disks.

What carries the argument

The load-bearing object is an extended, passive, geometrically thin, optically thick accretion disk. In the SED model its temperature profile is $T_e\simeq[(2/3\pi)]^{1/4}(R_\star/a)^{3/4}T_\star$, and integrating the Planck function over radius gives the $\nu^{4/3}$ optical/UV continuum that a single-blackbody fit cannot reproduce. A separate relativistic elliptical Keplerian disk model, with parameters for emissivity index, intrinsic broadening, inclination, eccentricity, and inner and outer pericenter radii, fits the double-peaked Balmer profiles and places the line-emitting region at the same large radius, $\bar{\xi}_1=5.06^{+0.59}_{-0.77}\times10^4\,R_g$. The consistency of the two independently fitted radii is the mechanism that connects the photometric excess to the spectral lines.

What would settle it

Take a high signal-to-noise spectropolarimetric observation of the H-alpha double peak: a rotating Keplerian disk imprints a characteristic swing of the polarization position angle across the line profile, whereas an outflow does not, so the absence of such a swing would show that the double peaks do not come from a disk.

Watch

Extended reading notes

Core claim

The paper's central claim is that AT 2020nov is a tidal disruption event occurring in a galaxy with a pre-existing, quiescent accretion disk around its supermassive black hole, rather than one whose disk formed entirely from the disrupted star. The evidence comes from three interlocking analyses: double-peaked Balmer emission lines whose velocity separation implies a Keplerian disk extending to roughly 5e4 gravitational radii; a multi-component SED requiring a passive disk that reprocesses an EUV blackbody peaking near log L = 45.66 erg/s; and a mid-infrared dust echo with a covering fraction near 1.1%, consistent with typical optically selected tidal disruption events. The paper proposes that the double-peaked lines arise from the same disk that reprocesses the EUV emission, that this disk is dynamically stable over roughly three years, and that a late-time X-ray flare about 300 days after peak marks the EUV photosphere receding to reveal the inner accretion flow.

Load-bearing premise

The whole pre-existing-disk picture rests on identifying the double-peaked Balmer lines with the same extended disk used in the SED fit; if those lines come from a quickly formed debris disk or an outflow instead, the central claim loses its main support.

Editorial extensions

If this is right

  • Bolometric luminosities of optical/UV tidal disruption events estimated from single-blackbody fits can be severe underestimates, because a passive disk can reprocess a dominant EUV component into the observed optical bands.
  • The constant velocity separation of the double-peaked Balmer lines over hundreds of days can serve as a geometric diagnostic for pre-existing disks in other tidal disruption events.
  • A pre-existing disk can speed up circularization of the disrupted debris through stream-disk interactions, providing a natural explanation for the early appearance of double-peaked lines and the late-time hard X-ray flare.
  • The dust covering fraction near 1.1% places AT 2020nov's mid-infrared echo in the normal optically selected tidal-disruption-event population rather than in the dust-rich active-galactic-nucleus or ambiguous-nuclear-transient classes.
  • The paper's dust-reverberation estimate independently supports an EUV luminosity around 10^44-10^45 erg/s, consistent with the SED-derived EUV component and with theoretical expectations for the total radiated energy of a tidal disruption event.

Reading between the lines

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

  • Beyond the paper, the same passive-disk SED model could be applied to other tidal disruption events with broad, shallow optical peaks and narrow double-peaked lines; a systematic reanalysis might reveal a population of dormant-disk reprocessing events.
  • If dormant disks around roughly 10^7 solar-mass black holes are commonly illuminated this way, the EUV output of the tidal-disruption-event population is systematically underestimated, and future EUV or soft-X-ray surveys could catch the primary emission before it is reprocessed.
  • Spectropolarimetric monitoring of the double-peaked Balmer lines would provide a model-independent test of the disk interpretation that does not rely on the SED decomposition, since a rotating Keplerian disk imprints a characteristic polarization signature across the line profile.
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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 multi-wavelength analysis of the tidal disruption event AT 2020nov, combining ZTF, Pan-STARRS, Swift/UVOT, Swift/XRT, XMM-Newton, WISE/NEOWISE, and an extensive optical spectroscopic campaign. The authors report double-peaked Balmer emission lines that persist from 24 days before optical peak to roughly 1000 days after, a broad UV/optical flare whose SED cannot be fit by a single blackbody, a late-time hard X-ray flare about 300 days after peak, and a mid-infrared flare interpreted as a dust echo. They model the SED with a three-component fit consisting of an EUV blackbody, a passive disk that reprocesses EUV radiation, and a MIR blackbody, and they model the double-peaked lines with a relativistic elliptical disk. From the EUV component they infer a peak luminosity of log L ~ 45.66 erg/s and a total radiated energy of ~1e53 erg. They conclude that AT 2020nov is a TDE occurring in a galaxy with a pre-existing, quiescent, extended elliptical disk around a ~10^7.4 solar-mass black hole, with the primary EUV emission reprocessed by this disk into the observed optical/UV and MIR bands.

Significance. If the disk-reprocessing interpretation is correct, AT 2020nov would be one of the first TDEs showing direct evidence for a pre-existing quiescent accretion disk that is illuminated by, and reprocesses, the primary EUV emission of a tidal disruption event. This would have implications for TDE rates in AGN-like environments and for the 'missing energy' problem in optically selected TDEs. The paper's strengths are the high-quality, densely sampled multi-wavelength dataset; the robust identification of persistent double-peaked Balmer profiles; the clean demonstration that a single blackbody fails to describe the SED; and the use of an independent MIR dust-echo argument, which at least provides a lower limit on the EUV luminosity. The main weakness is that the central EUV luminosity and the passive-disk component are not directly observed but are inferred from a specific SED model that is only compared against a single blackbody, leaving alternative physical models (cooling envelope, biconical winds, stream-collision geometries) unmodeled. The identification of the double-peaked line-emitting region with the SED-fitting disk is also an assumption rather than a demonstrated uniqueness.

major comments (3)
  1. [Section 3.2, Table 2, Figure 7] The central claim that AT 2020nov has an EUV-dominated primary luminosity of log L ~ 45.66 erg/s and a total radiated energy of ~1e53 erg rests on the three-component SED model in which the EUV blackbody is a free parameter with no direct EUV observations. The model comparison in Table 2 and Figure 7 is only between a single blackbody and the multi-component passive-disk model. No cooling-envelope model (Metzger 2022), biconical-wind/outflow continuum, or stream-collision emission model is fit to the same epochs, so the large EUV luminosity is not uniquely required by the data. The authors should either fit these alternative models, or explicitly state that the EUV luminosity is a model-dependent inference and weaken the corresponding claims in Sections 3.3 and 6.
  2. [Section 4.4, Section 5.3, Section 6] The conclusion that the double-peaked emission lines arise from the same pre-existing disk used in the SED fit is an assumption. The paper itself hedges in Section 4 ('If the double-peaked emission lines indeed arise from the same disk structure used in the SED modeling...'), and Section 5.5 dismisses outflows only qualitatively. Quantitatively, the elliptical disk fits give an outer radius of log10 xi2 ~ 4.7 (i.e., ~5e4 Rg), while the SED passive-disk fit gives only an inner radius (log10 a_in ~ 14.9 cm, ~200 Rg); no outer radius for the SED disk is reported or compared. The geometric consistency between the two disk components is therefore not demonstrated. The authors should either provide a direct comparison of the SED disk outer radius with the line-emitting disk radius, or explicitly restrict the conclusion to 'the data are consistent with' rather than 'the primary emission is likely reprocessed by' the same disk.
  3. [Section 5.4, Eq. (6)] The dust-echo estimate is presented as an independent confirmation of the EUV luminosity, but the calculation yields only a lower limit of L_UV > 1e44 erg/s under assumed dust grain size and sublimation temperature; the paper itself notes that an order-of-magnitude higher luminosity is obtained only if the MIR emission lasts ~1 yr or grains are ~1 micron. This is consistent with the SED-fit value of 10^45.66 but does not independently constrain it. The dust covering factor of 1.1% also depends on the SED-fit EUV luminosity. The language in Sections 5.4 and 6 ('confirm significant EUV emission') should be moderated to reflect the actual constraining power of the dust echo.
minor comments (5)
  1. [Section 2.2] There is a typo: 'NUX data' should be 'NUV data'.
  2. [Section 4.4 / Figure 16] The text says 'The blue line shows the disk model fit to the data' but the figure caption and the plotted model are orange; this should be corrected for consistency.
  3. [Section 5.3] The text refers to 'extended (bar-xi1 = 5.06e4 Rg)', but in Table 3 the outer radius is xi2 (log10 xi2 ~ 4.7), while xi1 is the inner radius (~10^3 Rg). The notation appears to use xi1 where xi2 is meant; please fix.
  4. [Section 3.2 / Table 2] The AIC values in Figure 7 show that for epoch 3 the model without the disk is preferred (AIC 2388.6 vs 2384.8), yet the text in Section 5.6 states 'the SED analysis over several epochs reveals the need for a passive disk component' without flagging that the late-time epoch does not require it; this nuance should be acknowledged in the summary of results.
  5. [Section 4.4, Eq. (5)] In the expression for the specific intensity, the exponent should be written as -(nu_e - nu_0)^2/(2 sigma^2) for dimensional consistency; as printed, the LaTeX has (nu_2^e - nu_2^o) which is likely a typographical error.

Circularity Check

2 steps flagged · score 6.0 of 10

The EUV-disk-reprocessing conclusion is partly built into the SED model, and the line-profile analysis reuses the same spectra for its priors.

  1. self definitional [Section 3.2 (SED Modeling), Eqs. (1)-(2); Section 6 conclusions]
    "To more accurately model the SED, we employ a three-component approach: (1) a black body to capture the TDE emission peaking in the EUV, (2) a passive (i.e. lacking intrinsic luminosity) disk model that reprocesses EUV radiation and contributes to the observed optical/UV emission... We infer a total energy output from the TDE black body component of 1.18×10^53 erg, with 1.20×10^51 erg being reprocessed by the extended passive disk and observed in the optical/UV bands."

    The passive disk is defined to have no intrinsic luminosity, and Eq. (2) sets its temperature profile from the fitted TDE blackbody radius and temperature. The same optical/UV photometry is therefore used to constrain both the 'EUV' blackbody and the disk that is said to reprocess it. The quoted peak EUV luminosity (10^45.66 erg/s) and total EUV energy (10^53 erg) are integrals over this fitted component, not independent measurements. Presenting the fit as evidence that 'the primary emission from the TDE is likely reprocessed by this extended disk structure' restates the model's construction; no cooling-envelope or outflow continuum is fitted to the same epochs, so the large EUV component is not uniquely required.

  2. other [Appendix, priors for elliptical disk modeling (Table 4 and preceding paragraph)]
    "An initial exploratory dynesty run was conducted with a low number of samples and uniform priors across all parameters to probe the parameter space and assess potential degeneracies. This preliminary analysis revealed significant degeneracies among certain accretion disk parameters... To address these degeneracies and improve the fit, we subsequently adopted normal priors centered near the average of the posterior distributions obtained from the exploratory run for these parameters for the inclination and apocenter."

    The final reported disk parameters (e.g., inclination and outer radius in Table 3) are conditioned on priors derived from a first fit to the same spectra. The data are used twice: once to locate the prior and again to produce the quoted posterior. This makes the line-profile disk radius partially self-consistent by construction and weakens the claimed independent agreement between the spectroscopic disk radius and the SED disk radius. The step is contained to the line-profile analysis rather than the SED fit, but it is a genuine circular reuse of the data.

full rationale

The paper's central claim does not rest on a load-bearing self-citation chain: citations such as Dai et al. (2018) and Mockler & Ramirez-Ruiz (2021) provide supporting theory but are not the sole justification for the disk interpretation. However, the strongest claim in Section 6 does partially reduce to the model's construction. The three-component SED fit includes an EUV blackbody and a passive disk whose temperature profile (Eq. 2) is tied to that blackbody's fitted radius and temperature, so concluding that the observed optical/UV continuum is reprocessed EUV is essentially the model's built-in decomposition; the quoted EUV luminosity and total energy are integrals over the fitted component. The model comparison is only against a single blackbody, not against cooling-envelope or wind continuum models, so the large EUV component is not uniquely required by the data. Independent support does exist: the double-peaked Balmer profiles seen 24 days before peak, the MIR dust echo with a ~0.5-1 yr timescale, and the hard X-ray behavior all point toward extended structure and an energetic unresolved component. The paper itself hedges the key identification in Section 4 ('If the double-peaked emission lines indeed arise from the same disk structure used in the SED modeling...'), so the pre-existing-disk conclusion is conditional. Finally, the Appendix's data-informed priors, centered on the posterior of an exploratory run on the same spectra, are a genuine though localized circular step in the line-profile analysis. Overall, the central EUV-reprocessing claim is partially circular by construction, but enough independent observables remain that the paper is not entirely reducible to its inputs.

Assumptions & free parameters 8 free parameters · 6 assumptions · 2 invented entities

The central claim rests on the standard toolkit of TDE modeling plus two paper-specific assumptions: a passive irradiated disk that reprocesses an unobserved EUV source, and the identification of that disk with the line-emitting elliptical disk. Several key quantities (EUV temperature/radius, disk inner radius, IR temperature, elliptical disk geometry, dust grain size) are fitted or assumed rather than measured, so the 'contribution' of the paper is an interpretation built on roughly a dozen free or ad hoc inputs.

free parameters (8)
  • EUV blackbody temperature and radius (epoch 1) = log10 T_BB = 5.38 (+0.03/-0.18) K; log10 R_BB = 13.6 (+0.17/-0.06) cm
    Fitted in the three-component SED; this unobserved EUV component yields the peak log L_EUV = 45.66 and total EUV energy ~1.18e53 erg, which drive the disk-reprocessing interpretation.
  • Passive disk inner radius a_in (epoch 1) = log10 a_in = 14.9 (+0.07/-0.11) cm
    Integration boundary in Eq. (1); controls where the reprocessed disk continuum starts and is degenerate with T_BB/R_BB.
  • MIR blackbody temperature and radius (epoch 1) = log10 T_IR = 3.19 (+0.11/-0.16) K; log10 R_IR = 16.6 (+0.22/-0.14) cm
    Fit to W1/W2; used for dust covering factor and as the sublimation temperature in the dust-echo estimate.
  • Elliptical disk outer radius xi2 = log10 xi2 ~ 4.7 Rg, i.e., ~5e4 Rg across epochs
    Fitted to double-peaked Balmer profiles; the extended outer radius is the main evidence for a pre-existing disk.
  • Elliptical disk eccentricity, inclination, emissivity index = e ~ 0.53, i ~ 49 deg, q ~ 1.37
    Fitted line-profile parameters used to argue the disk is elliptical, moderately inclined, and more extended than TDE debris disks.
  • Dust grain size a = 0.1 to 1 micron (assumed)
    Controls the dust sublimation light-crossing timescale in Eq. (6); the inferred L_UV lower limit ranges from ~1e44 to ~1e45 erg/s depending on this choice.
  • Dust sublimation temperature T_sub = ~10^3.19 K (set to fitted IR temperature)
    Used as T_sub in Eq. (6); not independently measured.
  • Host galaxy stellar mass and A_V (Bagpipes) = log10 M* = 10.4, A_V = 0.98
    Used for host subtraction in UV photometry and to derive MBH through scaling relations; influences the SED and Eddington ratio.
assumptions (6)
  • domain assumption Flat LambdaCDM cosmology with H0 = 67.4 km/s/Mpc, Omega_m = 0.32, Omega_Lambda = 0.68.
    Assumed for luminosity distance and rest-frame quantities (Section 1).
  • domain assumption Passive irradiated disk temperature profile Te ~ (R*/a)^{3/4} T* (Chiang & Goldreich 1997, Eq. 2) describes reprocessing of EUV by an optically thick disk.
    The central SED model assumes the disk is passive, optically thick, and reradiates absorbed EUV locally; no radiative transfer or albedo is modeled.
  • domain assumption Eracleous et al. (1995) weak-field relativistic elliptical disk model describes the double-peaked Balmer lines.
    Used for line profile fitting; the paper notes it is invalid for xi1 < 100 Rg (Section 5), so the inner-disk inference is model-limited.
  • ad hoc to paper The double-peaked line-emitting region and the passive SED disk are the same physical structure.
    The paper states 'if the double-peaked emission lines indeed arise from the same disk structure used in the SED modeling...' (Section 4) and uses their consistent radii as support, but this identification is assumed, not derived.
  • domain assumption MIR flaring is dust echo reprocessing of the TDE's UV/EUV emission rather than pre-existing AGN variability.
    The interpretation of the WISE light curve as a dust echo from the TDE (Section 5.4) underlies the dust covering factor and the independent L_UV estimate.
  • domain assumption Black hole mass scaling relations (MBH-sigma and MBH-Mstar) from Kormendy & Ho 2013, Reines & Volonteri 2015, Greene et al. 2020, and Yao et al. 2023 apply to this host.
    Used in Section 3.3 to set MBH = 10^7.4 Msun, which converts line-profile radii to Rg and sets the Eddington ratio.
invented entities (2)
  • Pre-existing quiescent elongated (elliptical) accretion disk around the SMBH
    purpose: Explains the double-peaked Balmer lines, the optical/UV SED excess via reprocessing, and the extended outer radius ~5e4 Rg.
    The disk is inferred from the same observations it is used to explain; no external falsifiable prediction is made, and the line/SED identification rests on the assumption that both arise from the same structure.
  • Unobserved EUV primary emission component (EUV blackbody)
    purpose: Supplies the large bolometric luminosity that is reprocessed by the disk and dust; addresses the 'missing energy' problem.
    Not directly detected; its temperature, radius, and luminosity are fitted parameters in the SED model, and the claimed dust-echo confirmation depends on assumed grain properties.

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Cite this review

Pith. "Pith review of AT 2020nov: Evidence for Disk Reprocessing in a Rare Tidal Disruption Event." pith.science (2026). https://pith.science/paper/MKTC2EOX

@misc{pith2026241212991,
  author       = {Pith},
  title        = {Pith review of: AT 2020nov: Evidence for Disk Reprocessing in a Rare Tidal Disruption Event},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MKTC2EOX}},
  note         = {Machine review of arXiv:2412.12991}
}
abstract

We present a detailed analysis of AT 2020nov, a tidal disruption event (TDE) in the center of its host galaxy, located at a redshift of $z = 0.083$. AT 2020nov exhibits unique features, including double-peaked Balmer emission lines, a broad UV/optical flare, and a peak log luminosity in the extreme ultra-violet (EUV) estimated at $\sim$$45.66^{+0.10}_{-0.33} \; \mathrm{erg} \, \mathrm{s^{-1}}$. A late-time X-ray flare was also observed, reaching an absorbed luminosity of $1.67 \times 10^{43} \; \mathrm{erg} \, \mathrm{s^{-1}}$ approximately 300 days after the UV/optical peak. Multi-wavelength coverage, spanning optical, UV, X-ray, and mid-infrared (MIR) bands, reveals a complex spectral energy distribution (SED) that includes MIR flaring indicative of dust echoes, suggesting a dust covering fraction consistent with typical TDEs. Spectral modeling indicates the presence of an extended, quiescent disk around the central supermassive black hole (SMBH) with a radius of $\sim$$5.06^{+0.59}_{-0.77} \times 10^4 \; \mathrm{R_g}$. The multi-component SED model, which includes a significant EUV component, suggests that the primary emission from the TDE is reprocessed by this extended disk, producing the observed optical and MIR features. The lack of strong AGN signatures in the host galaxy, combined with the quiescent disk structure, highlights AT 2020nov as a rare example of a TDE occurring in a galaxy with a dormant but extended pre-existing accretion structure.

Figures

Figures reproduced from arXiv: 2412.12991 by the authors.

Figure 1
Figure 1. Optical and UV light curves of AT 2020nov from ZTF, PS1 (GPC1), and Swift (UVOT). The 𝑔-band, 𝑟-band, and 𝑧-band used difference imaging to remove host contribution, while estimates of the host flux from the population synthesis analysis were used for the Swift data (see Section 2). Spectral observations taken by the YSE collaboration are represented by thick black vertical lines, while shorter grey vertical lines s… view at source ↗
Figure 3
Figure 3. Top: Absorbed luminosity of the Swift XRT light curve (purple) and the single XMM-Newton (cyan) observation in the 0.3 keV to 10 keV energy band. The X-ray flare occurs Δ𝑡 = +300 days (vertical dotted line) after the optical/UV peak (vertical dashed line). Derived 3𝜎 upper limits are shown as inverted triangles. Bottom: X-ray hardness ratio computed as (hard − soft)/(hard + soft). The hardness ratio peaks during the… view at source ↗
Figure 4
Figure 4. Mid-IR light curves of WISE 3.4 𝜇m (blue) and 4.6 𝜇m (orange) observations. The 7𝜎 upper limits are shown as open cir￾cles with downward arrows. The time of the optical/UV peak is shown as the vertical dashed line, coincident with the dramatic in￾crease in the IR flux. Evidence for activity begins ∼3.5 years before the flare associated with AT 2020nov (See Section 3.6). North (FTN) and South (FTS) instruments of the… view at source ↗
Figures from the paper (17 more)
Figure 5
Figure 5. Figure 5: Spectroscopic evolution of AT 2020nov, covering −48 days before peak (2020 August 26) to 1013 days after peak. Section 2.4 describes the flux calibration to the photometry. Common emission features of TDEs are indicated with light grey lines. The double-peaked features…
Figure 6
Figure 6. Figure 6: Model of the host galaxy SED fit using Bagpipes. The best-fit model and 1-𝜎 dispersion of the realizations are shown in blue, while the archival photometry are plotted as colored circles. The star-formation history derived from Bagpipes is shown in the inset, indicatin…
Figure 7
Figure 7. Figure 7: Fitting results for two approaches to modeling the SED of AT 2020nov. The top row uses a traditional approach of representing the optical/UV emission with a single black body (grey dashed line), while the bottom row additionally includes the passive SED disk model (gol…
Figure 9
Figure 9. Figure 9: Luminosity rise and decay rates of the 𝑔- and 𝑟- band photometry with fits performed using a smoothly broken power law model. The decline from peak follows a ∼𝑡 −4/3 power-law, con￾sistent with super-Eddington disk accretion. The expected fallback rate of 𝑡 −5/3 is sho…
Figure 8
Figure 8. Figure 8: Comparison of the 𝑟-band light curves of AT 2020nov (black) and a selection of TDEs whose estimated log 𝑀BH are within ±0.5 dex of AT 2020nov, categorized by their spectral type. The sharp rise, broad peak, and shallow fallback are characteristic of TDEs with larger bl…
Figure 10
Figure 10. Figure 10: Pre-flare optical (ASAS-SN, ZTF, ATLAS, Catalina, Pan-STARRS) and mid-infrared (WISE) photometry of AT 2020nov. Derived 3𝜎 (7𝜎) upper limits are shown for the optical (mid-infrared) as open circles with downward arrows. of the variability being DRW-like, with 𝜎QSO = 0…
Figure 11
Figure 11. Figure 11: Left: Evolution of the high resolution spectra of AT 2020nov covering phases from 17 d before to 1020 d after the optical/UV peak. Each spectrum is labeled with the phase and telescope/instrument used for the observation. Common TDE emission features are marked with v…
Figure 12
Figure 12. Figure 12: Stacked spectra of AT 2020nov after scaling and fitting of the Bagpipes continuum with a 3rd degree polynomial has been removed. Left: Zoom-in of the N III+He II complex, demonstrating the disappearance of the He II at late-times and a decrease in the amplitude of dou…
Figure 13
Figure 13. Figure 13: Ratios of the narrow lines measured at each spectral epoch, from early- (dark blue) to late-time (dark red). The results straddle the cutoffs between both composite and AGN, as well as between star-forming, AGN, and LINER galaxies, indicating that the emission line be…
Figure 14
Figure 14. Figure 14: Evolution of emission line FWHM and offsets in AT 2020nov (shown as grey circles) compared to TDEs in the sample of Char￾alampopoulos et al. (2022). Vertical dashed line shows the time of the optical/UV peak. Other TDEs with double-peaked emission lines are shown with…
Figure 15
Figure 15. Figure 15: Luminosity evolution of the H𝛼 (top) and H𝛽 (bottom) emission line complexes in the spectra. Fitting is performed with a 4th order polynomial to determine the time of peak luminosity. Time lags (see Section 4.5) are calculated as the difference between the optical/UV …
Figure 16
Figure 16. Figure 16: Best-fitting elliptical disk models (orange) to the H𝛽 and H𝛼 line complexes for each spectral observation. Fits required an additional broad Gaussian feature to represent the BLR (red). Narrow host emission was included in the fitting where necessary and are shown in…
Figure 17
Figure 17. Figure 17 [PITH_FULL_IMAGE:figures/full_fig_p023_17.png]
Figure 18
Figure 18. Figure 18: Evolution of various radii for AT 2020nov. The circles show the behavior of the inner (orange) and outer (blue) radii from the elliptical disk model fitting. The pink diamonds, red squares, and green triangles represent the mid-IR black body radius, inner disk radius …
Figure 19
Figure 19. Figure 19: Illustration of AT 2020nov’s evolution and its associated emission. While we do not render the sizes of each component to scale (for ease of visualization, though see [PITH_FULL_IMAGE:figures/full_fig_p026_19.png]
Figure 20
Figure 20. Figure 20: Comparison of the spectra of AT 2020nov at +11 days with those of other nuclear transients. Left: Various AGN with double-peaked structure. Middle: Ambiguous nuclear transients, TDE candidates with disk-winds or that have occurred in active AGN hosts. Right: Other TDE…
Figure 21
Figure 21. Figure 21: Posterior probability density functions for the elliptical accretion disk and Gaussian models used in the spectroscopic fitting of the H𝛼 and H𝛽 emission line complexes of the LRIS +15 day spectrum. Burrows, D. N., Hill, J. E., Nousek, J. A., et al. 2005, SSRv, 120, 1…

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Forward citations

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232 extracted references · 17 canonical work pages · cited by 2 Pith papers

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Pith tools

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