The Radio Properties of Extreme Coronal Line Emitters: Constraints on the Sub-parsec Environment

B. Ashley VanderLey; Collin T. Christy; Edo Berger; Enrico Ramirez-Ruiz; Fabio De Colle; Gavin Farley; Jean Somalwar; Kate D. Alexander; Megan Newsome; Noah Franz

REVIEW 3 major objections 5 minor 300 references

The Radio Properties of Extreme Coronal Line Emitters: Constraints on the Sub-parsec Environment

T0 review · 3 major / 5 minor · reviewed 2026-07-14 · grok-4.5

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Pith's one-line read Radio data show the dense gas that makes extreme coronal lines is clumpy, with a volume filling factor of only about 10^{-5} to 10^{-2}.

desk verdict First radio census of ECLEs that cleanly shows the dense gas is clumpy; the quoted f_V window is soft but the qualitative geometry result holds. read the letter →

arxiv 2607.09871 v1 pith:5TJ26ZVR submitted 2026-07-10 astro-ph.HE astro-ph.GA

Noah Franz , Kate D. Alexander , Collin T. Christy , Tanmoy Laskar , Stefanie Komossa , Enrico Ramirez-Ruiz , Jean Somalwar , Edo Berger

show 5 more authors

Ryan Chornock Fabio De Colle Gavin Farley Megan Newsome B. Ashley VanderLey

This is my paper · ORCID

classification astro-ph.HEastro-ph.GA

keywords extremecoronallineemitterstidaldisruptioneventsactivegalacticnucleiradiosynchrotroncircumnuclearmediumvolumefillingfactorphotoionization

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

Extreme coronal line emitters are rare galaxies whose nuclei light up with high-ionization metal lines that need soft X-rays hitting very dense gas. Why only a tiny fraction of tidal disruption events and AGN show these lines has been unclear: the geometry and filling factor of that dense gas were unknown. This paper supplies the first systematic radio view of 27 nearby ECLEs. Roughly half produce radio synchrotron emission whose luminosity and time evolution match outflows from TDEs or AGN. Modeling the radio spectra of four well-observed systems yields a circumnuclear density orders of magnitude below the density required by the optical lines. The only way to reconcile the two is if the extreme-coronal-line gas is clumpy, with a low volume filling factor, and is spatially distinct from the radio-emitting region. For variable ECLEs these are among the first direct geometric constraints on the sub-parsec environment of formerly quiet black holes, linking accretion, photoionization, and mechanical feedback in one laboratory.

What carries the argument

Equipartition analysis of synchrotron self-absorption spectra (peak flux, break frequency, and electron power-law index) that yields the average density of the radio-emitting volume; comparison of that density to the much higher line-ratio density then gives the volume filling factor of the dense ECL gas.

What would settle it

Deeper multi-frequency radio monitoring of a larger ECLE sample that either (a) yields filling factors outside 10^{-5}–10^{-2} under the same equipartition assumptions or (b) shows the radio and coronal-line regions to be co-spatial at the same density would falsify the claimed clumpy geometry.

Watch

Extended reading notes

Core claim

Radio spectral modeling of four ECLEs shows that the gas producing extreme coronal lines is clumpy, with volume filling factor 10^{-5} ≲ f_V ≲ 10^{-2}, and is likely distinct from the radio-emitting region (for example a clumpy toroidal geometry). About half of the 27-object sample is radio-detected at luminosities consistent with TDE or AGN outflows.

Load-bearing premise

Converting the radio-derived density of relativistic electrons into a total gas density (and therefore into a filling factor) rests on assumed values for the relativistic-electron fraction and on a spherical thin-shell geometry; large changes in either assumption move the filling-factor range by orders of magnitude.

Editorial extensions

If this is right

The dense gas that produces extreme coronal lines cannot be a smooth spherical shield; it must be concentrated in discrete clouds or a clumpy torus.
Time-variable ECLEs become direct laboratories for the sub-parsec gas geometry around previously quiescent supermassive black holes.
Roughly half of ECLEs launch radio outflows whose energies and densities sit in the same range as ordinary TDEs and radio-quiet AGN.
Future multi-wavelength campaigns can jointly constrain accretion luminosity, photoionization, and mechanical feedback with a single class of objects.

Reading between the lines

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

If the low filling factor is generic, models that treat the circumnuclear medium as a uniform density sphere will systematically overestimate the mass of gas available for coronal-line emission.
The same radio-plus-line method could be applied to ordinary AGN and late-time TDEs that lack extreme coronal lines to test whether the clumpy geometry is what makes ECLEs special.
Late-time radio monitoring of a larger TDE sample may reveal a higher incidence of decelerated off-axis jets than previously reported, aligning the ECLE jet fraction with that of radio-loud AGN.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

This is the first systematic radio look at a low-z ECLE sample, and the main payoff is real: radio equipartition densities sit orders of magnitude below the line-ratio densities, so the ECL gas has to be clumpy with low volume filling factor rather than a smooth spherical shield. That geometric conclusion is new for formerly quiescent nuclei and is the piece worth remembering.

What they did well is straightforward. They assembled 27 optically selected events, added targeted VLA/GMRT epochs for the best cases, reduced the data cleanly, and fitted standard SSA spectra with the usual BD13 equipartition machinery already used on TDEs. Light-curve comparisons to TDEs and radio-quiet AGN are careful; the ~50 % radio-bright fraction is correctly flagged as a lower limit given survey depths. Code and photometry are released. The four multi-band SEDs (especially SDSS J1241) are solid enough to trust the qualitative density mismatch.

The soft spot is exactly where the stress-test points: the numerical window 10^{-5} ≲ f_V ≲ 10^{-2} rides on f_rel ≈ 0.01, f_emit = 0.1, and spherical averaging (Eq. 6). Change those by the ranges still allowed in the TDE/GRB literature and the bounds slide by 1–2 dex. For SDSS J1241 the derived β ≈ 0.006 already hints the spherical assumption is too simple. So treat the quoted range as order-of-magnitude illustration, not a precision measurement. The qualitative claim (clumpy, non-spherical, distinct from the radio-emitting volume) survives; the precise numbers do not yet.

This is for people working on TDE outflows, CNM structure, or photoionization of nuclear gas. It is not a methods paper and does not reorganize the field, but it is a clean first data point that motivates deeper multi-frequency follow-up. I would send it to referees; the data and analysis are above the bar for a solid observational ApJ paper once the free-parameter caveats are stated more prominently. Worth citing for the geometric argument and the sample itself.

Referee Report

3 major / 5 minor

Summary. The paper presents the first systematic radio study of 27 low-redshift (z<0.3) extreme coronal line emitters (ECLEs). Combining archival VLA surveys (VLASS, FIRST, NVSS) with new targeted VLA and GMRT observations of a subset, the authors find that roughly half the sample produces radio synchrotron emission whose luminosity and evolution are consistent with non-relativistic TDE outflows or radio-quiet AGN. For four events with multi-band SEDs (SDSS J0748, SDSS J0938, SDSS J1241, AT 2020vdq) they fit synchrotron self-absorption spectra, apply equipartition (BD13 with Newtonian corrections) under a spherical thin-shell geometry, and derive outflow energies and circumnuclear densities. Comparing the radio-derived density (n_e ~ 100 cm^{-3}) with the much higher densities required by the optical coronal lines (n_l ~ 10^{6-9} cm^{-3}) they conclude that the ECL-producing gas is clumpy, with a volume filling factor 10^{-5} ≲ f_V ≲ 10^{-2}, and is likely spatially distinct from the radio-emitting region (e.g., a clumpy torus).

Significance. If the qualitative geometric conclusion holds, the work supplies one of the first direct observational constraints on the sub-parsec CNM geometry in formerly quiescent nuclei that host TDEs, and it links photoionization diagnostics to dynamical outflow probes in a single class of objects. The multi-wavelength compilation, public data release via OTTER, and open analysis code are genuine strengths that will enable follow-up. The numerical f_V window is secondary; the demonstration that radio and optical densities cannot be reconciled under spherical symmetry is the load-bearing result and is of clear interest to the TDE/AGN community.

major comments (3)

Section 4.4 and Eq. (6): the quoted numerical range 10^{-5} ≲ f_V ≲ 10^{-2} is obtained by converting n_e to a total gas density via the ad-hoc choice f_rel ≈ 0.01 and then dividing by n_l ~ 10^{6-9} cm^{-3}. The manuscript itself notes that f_rel is poorly constrained (literature allows ~10^{-3}-0.1). Because f_V scales linearly with 1/f_rel, the numerical bounds move by 1-2 dex under plausible variations. The abstract and conclusion present the range as a firm result of the radio modeling; it should be re-framed as an order-of-magnitude estimate whose dominant systematic is f_rel, or the range should be shown explicitly as a function of f_rel.
Section 3.3 and the discussion of SDSS J1241: the equipartition formulae assume spherical symmetry (f_A = 1, f_emit = 0.1). For SDSS J1241 the same analysis yields β ≈ 0.006, which the authors themselves interpret as evidence that spherical geometry is an oversimplification (or that the radio-emitting region lags the leading edge). Because the density contrast that drives the f_V argument is obtained under that spherical average, the claim that the ECL and radio regions are 'likely distinct' needs either (i) an explicit collimated-outflow re-calculation (f_A ≪ 1) showing that the density discrepancy survives, or (ii) a clear statement that the geometric conclusion is qualitative only and does not rest on the precise numerical value of n_e.
Section 4.3: the ~50 % radio-bright fraction is repeatedly cited as a population result, yet the text correctly notes that most VLASS/FIRST limits are non-constraining for typical non-relativistic luminosities at z ≳ 0.04 and that only four events lie inside the volume where VLASS can detect ν L_ u ~ 10^{38} erg s^{-1}. The deeper targeted sample is small (10 events) and biased toward previously interesting targets. The abstract and conclusion should state the fraction as a lower limit (or as a detection rate within the sensitivity-limited subsample) rather than as a robust population statistic.

minor comments (5)

Table 3 / Figure 3: for SDSS J0938 and the second epoch of AT 2020vdq the peak flux and break frequency are reported only as limits; the corresponding equipartition quantities are therefore also limits. The text sometimes treats them on equal footing with the well-constrained epochs; a short clarifying sentence would help.
Figure 1 caption: several optical light curves are noted as not host-subtracted; it would be useful to mark those panels explicitly (e.g., with an asterisk) so the reader does not misinterpret continuum levels.
Section 3.2: the choice s = 1 (instead of the Granot & Sari 2002 prescription) is justified by an unphysical p ≈ 4 for SDSS J1241, but the effect of s on the derived p, u_a and F_ u,p is not quantified. A one-sentence sensitivity check would strengthen the modeling section.
Throughout: a few typographical inconsistencies remain (e.g., 'Newtownian', 'guassian', 'V ariable', missing spaces after periods in Table 1 footnotes). A careful proof-read is warranted.
Section 2.6 / Table 4: the eROSITA association with AT 2021acak is interesting but rests on a 2.9 arcsec offset; a brief note on the chance-coincidence probability would be helpful.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: f_V is an independent density-ratio comparison, not forced by construction or self-citation.

full rationale

The paper is a multi-wavelength observational study. Radio SEDs of four ECLEs are fit with a standard synchrotron self-absorption model (Eq. 1) whose free parameters (p, F u,p, u a) are constrained by the data via MCMC; equipartition formulae (BD13, with Newtonian corrections) then yield ne, Req and Eeq under explicit geometric assumptions (spherical thin shell, femit=0.1). These radio-derived densities are compared to independent optical-line densities nℓ∼10^6–9 cm-3 taken from the literature. The numerical mismatch is converted to a volume-filling factor via the order-of-magnitude estimate fV∼ne/(frel nℓ) with a conservatively chosen frel≈0.01 (Eq. 6). Nothing in this chain is defined in terms of the final claim, fitted to the target quantity, or justified solely by an unverified self-citation. Self-citations (OTTER database, prior TDE radio papers by overlapping authors) supply comparison samples and standard analysis choices; they do not close a logical loop that forces the quoted fV range or the clumpy-geometry conclusion. The result is therefore an ordinary (if assumption-dependent) observational inference, not a circular derivation. Score 1 only for the minor presence of self-citations that are not load-bearing.

Assumptions & free parameters 4 free parameters · 3 assumptions · 0 invented entities

The geometric claim rests on standard equipartition formulae (BD13) plus several conventional but non-unique choices for filling factors and geometry. No new particles or forces are invented; the free parameters are the usual ones that appear in every non-relativistic TDE radio analysis.

free parameters (4)

f_emit (emitting-shell thickness fraction) = 0.1
Fixed to 0.1 following Cendes et al. (2021a); enters f_V and therefore every equipartition radius and density.
f_rel (relativistic electron fraction) = 0.01
Chosen conservatively as 0.01 to convert n_e into total gas density n_r; directly sets the numerical range of f_V.
smoothing parameter s = 1
Fixed to 1 rather than the Granot & Sari (2002) prescription; affects the recovered p and peak parameters for SDSS J1241.
electron power-law index p, peak flux F_ν,p, break frequency ν_a
Free parameters of the broken-power-law MCMC fits to each SED; posteriors are propagated into equipartition quantities.

assumptions (3)

domain assumption Radio emission is produced by a non-relativistic, quasi-spherical outflow in equipartition (BD13 formulae with Newtonian corrections).
Stated in §3.1–3.3; required to convert observed peak flux and frequency into radius, energy and density.
domain assumption The radio-derived density is a spherical average of the ambient CNM while the optical line density n_ℓ samples only the dense clumps.
Core of the geometric argument in §4.4; without it the density discrepancy cannot be translated into a volume filling factor.
domain assumption ECLs are photoionized (not collisionally ionized) by soft X-rays from nuclear accretion.
Standard interpretation of ECLEs, used to link radio and optical probes of the same CNM.

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Cite this review

Pith. "Pith review of The Radio Properties of Extreme Coronal Line Emitters: Constraints on the Sub-parsec Environment." pith.science (2026). https://pith.science/paper/5TJ26ZVR

@misc{pith2026260709871,
  author       = {Pith},
  title        = {Pith review of: The Radio Properties of Extreme Coronal Line Emitters: Constraints on the Sub-parsec Environment},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5TJ26ZVR}},
  note         = {Machine review of arXiv:2607.09871}
}

abstract

A tiny fraction ($\ll1\%$) of galaxies display luminous, high-ionization metal emission lines, which may be persistent or variable. These extreme coronal lines (ECLs) are produced when soft X-ray photons intercept dense gas ($n\gtrsim10^{6-7}~{\rm cm^{-3}}$). The high X-ray flux required implicates intense nuclear activity, likely originating from tidal disruption events (TDEs) and active galactic nuclei (AGN). As ECLs are rarely seen even within these classes, their production may also require specific environmental conditions, but the details remain unclear (e.g., the geometry and volume filling factor of the ECL-producing gas). Here, we present the radio properties of a population of $27$ low-redshift ($z<0.3$) ECL emitting galaxies (ECLEs), providing a unique and previously unexplored probe of the properties of the circumnuclear medium (CNM; $\lesssim1$ pc from the black hole) in these systems. We find that $\sim 50\%$ of ECLEs produce radio synchrotron emission with luminosity and evolution consistent with TDEs and/or AGN. Radio spectral modeling of four ECLEs reveals that the ECL-producing region is (1) clumpy with a low volume filling factor ($10^{-5}\lesssim f_{V}\lesssim10^{-2}$) and (2) likely distinct from the radio emitting region (implying, e.g., a clumpy toroidal geometry). For time-variable ECLEs, these are some of the first observational constraints on the CNM geometry in formerly quiescent galactic nuclei. The unique nature of ECLEs makes them an excellent high-energy laboratory to connect the physics of accretion, photoionization, and feedback in galactic nuclei, thus motivating continued multi-wavelength monitoring.

Figures

Figures reproduced from arXiv: 2607.09871 by the authors.

**Figure 1.** The multi-frequency light curves of the 27 ECLEs in our sample. The color of the point indicates the radio band of the observation and downward facing triangles indicate upperlimits resulting from non-detections in the continuum images. X-ray light curves are shown as open points. We show the optical r-band light curve for the 11 TDE-candidates as the right y-axis. The r-band light curves of AT 2017gge, AT 2018bcb, … view at source ↗

**Figure 2.** The S-band light curve in luminosity space of the ECLEs (colored) as compared to the broader TDE population from OTTER (N. Franz et al. 2026c,a) and the AGN population (K. I. Kellermann et al. 2016). The non-relativistic TDE sample (grey box) includes transients in OTTER with a classification confidence C(T DE) > 0 (i.e., events that are either photometrically selected or are spectroscopically confirmed), are optica… view at source ↗

**Figure 3.** Four ECLEs in our sample have multi-band detections at the same epoch: SDSS J0748 (top left), SDSS J0938 (top right), SDSS J1241 (bottom left), AT 2020vdq (bottom right). SEDs of all of the observations of these four events are shown here. The last 100 MCMC iterations are shown as a line on top of the data. All four events have multi-band epochs that are well fit as self-absorption peaked synchrotron spectra. Howeve… view at source ↗

Figures from the paper (2 more)

**Figure 4.** Figure 4: The electron number density profiles of the circumnuclear mediums for SDSS J1241, SDSS J0938 and SDSS 0748 as compared to the population of TDEs and Sgr A* (F. K. Baganoff et al. 2003; F. De Colle et al. 2012; K. D. Alexander et al. 2016; S. Gillessen et al. 2019; M. M…

**Figure 5.** Figure 5: The equipartition energy as a function of days since discovery for SDSS J1241, SDSS J0938 SDSS 0748, and AT2020vdq as compared to the population of TDEs (K. D. Alexander et al. 2016; M. M. Anderson et al. 2020; Y. Cendes et al. 2021b, 2022; T. Eftekhari et al. 2018; A.…

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The Kepler Peas in a Pod Pattern is Astrophysical. , keywords =. doi:10.3847/2041-8213/ab7c69 , archivePrefix =. 1908.05833 , primaryClass =

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Extreme variability in an active galactic nucleus: Gaia16aax. , keywords =. doi:10.1093/mnras/staa186 , archivePrefix =. 2001.07446 , primaryClass =

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Multiwavelength Study of an X-Ray Tidal Disruption Event Candidate in NGC 5092. , keywords =. doi:10.3847/1538-4357/ab744a , archivePrefix =. 2003.09066 , primaryClass =

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ZTF Transient Discovery Report for 2020-01-08. Transient Name Server Discovery Report , keywords =

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The Spectral Evolution of AT 2018dyb and the Presence of Metal Lines in Tidal Disruption Events. , keywords =. doi:10.3847/1538-4357/ab5792 , archivePrefix =. 1903.03120 , primaryClass =

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ZTF Transient Discovery Report for 2019-11-18. Transient Name Server Discovery Report , keywords =

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ZTF Transient Discovery Report for 2019-10-07. Transient Name Server Discovery Report , keywords =

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Evidence for rapid disc formation and reprocessing in the X-ray bright tidal disruption event candidate AT 2018fyk. , keywords =. doi:10.1093/mnras/stz1976 , archivePrefix =. 1903.12203 , primaryClass =

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Discovery and Early Evolution of ASASSN-19bt, the First TDE Detected by TESS. , keywords =. doi:10.3847/1538-4357/ab3c66 , archivePrefix =. 1904.09293 , primaryClass =

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XMMSL2 J144605.0+685735: a slow tidal disruption event. , keywords =. doi:10.1051/0004-6361/201935650 , archivePrefix =. 1908.01065 , primaryClass =

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The tidal disruption event AT2017eqx: spectroscopic evolution from hydrogen rich to poor suggests an atmosphere and outflow. , keywords =. doi:10.1093/mnras/stz1837 , archivePrefix =. 1904.10571 , primaryClass =

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A New Class of Changing-look LINERs. , keywords =. doi:10.3847/1538-4357/ab3a38 , archivePrefix =. 1904.10973 , primaryClass =

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ATLAS Transient Discovery Report for 2019-08-02. Transient Name Server Discovery Report , keywords =

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PS18kh: A New Tidal Disruption Event with a Non-axisymmetric Accretion Disk. , keywords =. doi:10.3847/1538-4357/ab2ae1 , archivePrefix =. 1808.02890 , primaryClass =

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ZTF Transient Discovery Report for 2019-07-31. Transient Name Server Discovery Report , keywords =

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Discovery of Highly Blueshifted Broad Balmer and Metastable Helium Absorption Lines in a Tidal Disruption Event. , keywords =. doi:10.3847/1538-4357/ab24de , archivePrefix =. 1903.05637 , primaryClass =

1903 doi arXiv
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ePESSTO+ Transient Classification Report for 2019-06-10. Transient Name Server Classification Report , keywords =

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The Astronomer's Telegram , keywords =

Radio detection of the tidal disruption event AT2019azh. The Astronomer's Telegram , keywords =
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ZTF Transient Discovery Report for 2019-05-09. Transient Name Server Discovery Report , keywords =

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ePESSTO+ Transient Classification Report for 2019-05-13. Transient Name Server Classification Report , keywords =

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GaiaAlerts Transient Discovery Report for 2019-04-30. Transient Name Server Discovery Report , keywords =

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ZTF Transient Discovery Report for 2019-04-22. Transient Name Server Discovery Report , keywords =

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ZTF Transient Discovery Report for 2019-03-30. Transient Name Server Discovery Report , keywords =

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ZTF Transient Discovery Report for 2019-03-26. Transient Name Server Discovery Report , keywords =

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ZTF Transient Discovery Report for 2019-03-14. Transient Name Server Discovery Report , keywords =

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The Broad Absorption Line Tidal Disruption Event iPTF15af: Optical and Ultraviolet Evolution. , keywords =. doi:10.3847/1538-4357/ab04b0 , archivePrefix =. 1809.07446 , primaryClass =

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ZTF Transient Discovery Report for 2019-02-28. Transient Name Server Discovery Report , keywords =

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ASAS-SN Transient Discovery Report for 2019-02-22. Transient Name Server Discovery Report , keywords =

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ZTF Transient Discovery Report for 2019-02-16. Transient Name Server Discovery Report , keywords =

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Transient Name Server Classification Report , keywords =

ePESSTO Transient Classification Report for 2019-02-26. Transient Name Server Classification Report , keywords =

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The First Tidal Disruption Flare in ZTF: From Photometric Selection to Multi-wavelength Characterization. , keywords =. doi:10.3847/1538-4357/aafe0c , archivePrefix =. 1809.02608 , primaryClass =

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Discovery and follow-up of the unusual nuclear transient OGLE17aaj. , keywords =. doi:10.1051/0004-6361/201833682 , archivePrefix =. 1901.03718 , primaryClass =

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ASAS-SN Transient Discovery Report for 2019-01-30. Transient Name Server Discovery Report , keywords =

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ASAS-SN Transient Discovery Report for 2019-01-01. Transient Name Server Discovery Report , keywords =

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Infrared Echo and Late-stage Rebrightening of Nuclear Transient Ps1-10adi: Exploring the Torus with Tidal Disruption Events in Active Galactic Nuclei. , keywords =. doi:10.3847/1538-4357/aaf6b2 , archivePrefix =. 1812.01295 , primaryClass =

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Transient Classification Report for 2018-12-10. Transient Name Server Classification Report , keywords =

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Science with a Next Generation Very Large Array , year = 2018, editor =

Tidal Disruption Events. Science with a Next Generation Very Large Array , year = 2018, editor =. doi:10.48550/arXiv.1810.06677 , archivePrefix =. 1810.06677 , primaryClass =

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ZTF Transient Discovery Report for 2018-11-27. Transient Name Server Discovery Report , keywords =

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ATLAS Transient Discovery Report for 2018-11-11. Transient Name Server Discovery Report , keywords =

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ASAS-SN Transient Discovery Report for 2018-11-06. Transient Name Server Discovery Report , keywords =

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Transient Name Server Classification Report , keywords =

Transient Classification Report for 2018-11-13. Transient Name Server Classification Report , keywords =

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Gaia transients in galactic nuclei. , keywords =. doi:10.1093/mnras/sty2221 , archivePrefix =. 1808.03984 , primaryClass =

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AMI-LA 15.5 GHz observation of the TDE candidate AT2018hyz. The Astronomer's Telegram , keywords =
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ATLAS Transient Discovery Report for 2018-10-05. Transient Name Server Discovery Report , keywords =

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Transient Name Server Classification Report , keywords =

ePESSTO Transient Classification Report for 2018-09-16. Transient Name Server Classification Report , keywords =

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ePESSTO spectroscopic classification of optical transients. The Astronomer's Telegram , keywords =
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Transient Classification Report for 2018-08-15

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Science , keywords =

A dust-enshrouded tidal disruption event with a resolved radio jet in a galaxy merger. Science , keywords =. doi:10.1126/science.aao4669 , archivePrefix =. 1806.05717 , primaryClass =

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The Astronomer's Telegram , keywords =

FLOYDS Classification of AT 2018dyk/ZTF18aajupnt as a Possible Tidal Disruption Event. The Astronomer's Telegram , keywords =
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ZTF Transient Discovery Report for 2018-07-15. Transient Name Server Discovery Report , keywords =

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ASAS-SN Transient Discovery Report for 2018-07-15. Transient Name Server Discovery Report , keywords =

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Long-term decline of the mid-infrared emission of normal galaxies: dust echo of tidal disruption flare?. , keywords =. doi:10.1093/mnras/sty465 , archivePrefix =. 1802.05105 , primaryClass =

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GaiaAlerts Transient Discovery Report for 2018-06-17. Transient Name Server Discovery Report , keywords =

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Nature Astronomy , keywords =

A luminous X-ray outburst from an intermediate-mass black hole in an off-centre star cluster. Nature Astronomy , keywords =. doi:10.1038/s41550-018-0493-1 , archivePrefix =. 1806.05692 , primaryClass =

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ZTF Transient Discovery Report for 2018-05-16. Transient Name Server Discovery Report , keywords =

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Long-term radio and X-ray evolution of the tidal disruption event ASASSN-14li. , keywords =. doi:10.1093/mnras/sty077 , archivePrefix =. 1801.03094 , primaryClass =

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Pan-STARRS1 Transient Discovery Report for 2018-03-04. Transient Name Server Discovery Report , keywords =

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Multiwavelength follow-up observations of the tidal disruption event candidate 2XMMi J184725.1-631724. , keywords =. doi:10.1093/mnras/stx2940 , archivePrefix =. 1711.04795 , primaryClass =

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A new candidate TDE from XMM-Newton slew data. The Astronomer's Telegram , keywords =
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Radio Monitoring of the Tidal Disruption Event Swift J164449.3+573451. III. Late-time Jet Energetics and a Deviation from Equipartition. , keywords =. doi:10.3847/1538-4357/aaa8e0 , archivePrefix =. 1710.07289 , primaryClass =

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ASAS-SN Transient Discovery Report for 2018-01-15. Transient Name Server Discovery Report , keywords =

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Late-time observations of the relativistic tidal disruption flare candidate Swift J1112.2-8238. , keywords =. doi:10.1093/mnras/stx2193 , archivePrefix =. 1708.09668 , primaryClass =

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X-Ray Brightening and UV Fading of Tidal Disruption Event ASASSN-15oi. , keywords =. doi:10.3847/2041-8213/aaa0c2 , archivePrefix =. 1712.03968 , primaryClass =

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Swift and SALT observations the nuclear transient Gaia17dbg = ATLAS17lbg = AT2017gul. The Astronomer's Telegram , keywords =
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Nature Astronomy , keywords =

A population of highly energetic transient events in the centres of active galaxies. Nature Astronomy , keywords =. doi:10.1038/s41550-017-0290-2 , archivePrefix =. 1711.04577 , primaryClass =

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Black hole masses of tidal disruption event host galaxies. , keywords =. doi:10.1093/mnras/stx1703 , archivePrefix =. 1706.08965 , primaryClass =

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iPTF16fnl: A Faint and Fast Tidal Disruption Event in an E+A Galaxy. , keywords =. doi:10.3847/1538-4357/aa7579 , archivePrefix =. 1703.00965 , primaryClass =

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PS16dtm: A Tidal Disruption Event in a Narrow-line Seyfert 1 Galaxy. , keywords =. doi:10.3847/1538-4357/aa77f7 , archivePrefix =. 1703.07816 , primaryClass =

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Large decay of X-ray flux in 2XMM J123103.2+110648: evidence for a tidal disruption event. , keywords =. doi:10.1093/mnras/stx489 , archivePrefix =. 1702.06956 , primaryClass =

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A new, faint population of X-ray transients. , keywords =. doi:10.1093/mnras/stx417 , archivePrefix =. 1702.04422 , primaryClass =

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Compact Resolved Ejecta in the Nearest Tidal Disruption Event. , keywords =. doi:10.3847/1538-4357/aa71b1 , archivePrefix =. 1705.01669 , primaryClass =

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Revisiting Optical Tidal Disruption Events with iPTF16axa. , keywords =. doi:10.3847/1538-4357/aa7337 , archivePrefix =. 1703.01299 , primaryClass =

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New Physical Insights about Tidal Disruption Events from a Comprehensive Observational Inventory at X-Ray Wavelengths. , keywords =. doi:10.3847/1538-4357/aa633b , archivePrefix =. 1611.02291 , primaryClass =

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Exploratory Spectroscopy of Magnetic Cataclysmic Variables Candidates and Other Variable Objects. , keywords =. doi:10.3847/1538-3881/aa610d , archivePrefix =. 1608.00650 , primaryClass =

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Radio Observations of the Tidal Disruption Event XMMSL1 J0740-85. , keywords =. doi:10.3847/1538-4357/aa6192 , archivePrefix =. 1610.03861 , primaryClass =

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MAXI J1807+132: UV/Optical counterpart, further XRT observations. The Astronomer's Telegram , keywords =
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2017

Pith tools

Reviewed July 14, 2026 · model on record in the stance chip above.

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, keywords =

The First Radio-bright Off-nuclear Tidal Disruption Event AT 2024tvd Reveals the Fastest-evolving Double-peaked Radio Emission. , keywords =. doi:10.3847/2041-8213/ae0a26 , archivePrefix =. 2508.03807 , primaryClass =

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A Massive Black Hole 0.8 kpc from the Host Nucleus Revealed by the Offset Tidal Disruption Event AT2024tvd. , keywords =. doi:10.3847/2041-8213/add7de , archivePrefix =. 2502.17661 , primaryClass =

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VLASS Tidal Disruption Events with Optical Flares. I. The Sample and a Comparison to Optically Selected TDEs. , keywords =. doi:10.3847/1538-4357/adba4f , archivePrefix =. 2310.03791 , primaryClass =

work page Pith review arXiv doi:10.3847/1538-4357/adba4f

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Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal Line Emitter AT 2022upj

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