Pith. sign in

REVIEW 2 major objections 5 minor 2 cited by

A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018

T0 review · 2 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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

Pith's one-line read Seven seasons of spectroscopy catch a full changing-look cycle in Mrk 1018 in one year, tied to an accretion-driven outburst.

desk verdict Dense monitoring catches a full changing-look cycle in Mrk 1018 with novel profile trends, but the line-decomposition assumptions need a nonparametric cross-check before the BLR physics claims fully land. read the letter →

arxiv 2411.18917 v1 pith:UYCBWWVP submitted 2024-11-28 astro-ph.GA

Kai-Xing Lu , Yan-Rong Li , Qingwen Wu , Luis C. Ho , Zhi-Xiang Zhang , Hai-Cheng Feng , Sha-Sha Li , Yong-Jie Chen
show 8 more authors
Mouyuan Sun Xinwen Shu Wei-Jian Guo Cheng Cheng Jian-Guo Wang Dongchan Kim Jian-Min Wang Jin-Ming Bai
This is my paper · ORCID
classification astro-ph.GA
keywords changing-lookAGNMrk1018broad-lineregionEddingtonratioaccretiondiskinstabilitydouble-peakedemissionlinesBalmerdecrementreverberationmapping
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper reports that the changing-look active galactic nucleus Mrk 1018 completed a full cycle of type transitions, from Type 1.8 to Type 1.5/1.2 and back, in about one year around 2020, riding on a nucleus outburst. Using seven seasons of spectroscopy plus archival data spanning 45 years, the authors argue that the transition is driven by the accretion rate, which varied by a factor of 1000 and peaked at 2 percent of Eddington. They tie the outburst to a disk instability in the transition region between an outer thin disk and an inner advection-dominated accretion flow. The broad Balmer lines change from single-peaked to double-peaked as the type drops, with the double-peak separation shrinking as accretion rises, and the FWHM follows the virialized scaling FWHM proportional to (Lbol/LEdd)^-0.27. The result matters because it shows changing-look behavior can be a fast, accretion-regulated restructuring of the broad-line region rather than only obscuration or a rare tidal event.

What carries the argument

The central observable machinery is the decomposition of every broad H-$\alpha$ and H-$\beta$ profile into two Gaussians, which yields the FWHM, the velocity dispersion sigma_line, and the peak separation of the double-peaked profiles across 45 years. This decomposition, combined with the Eddington ratio as the driving variable, produces the paper's core scaling relations: FWHM proportional to (Lbol/LEdd)^-0.27, a decreasing double-peak separation with accretion, and a FWHM/sigma_line ratio that jumps between 2.96 (rectangular profiles, Type 1.8-1.5) and 1.71 (Lorentzian-like, Type 1.2-1.0). The proposed mechanism is a radiation-pressure instability in the transition zone between the outer standard thin disk and the inner advection-dominated accretion flow, which produces the observed one-year outburst and the synchronized changing-look behavior.

What would settle it

A decisive test would be to obtain dense, high-signal-to-noise spectroscopy covering the full rising phase of a similar outburst in a low-Eddington AGN; if the broad lines remained single-peaked while the type moved from 1.8 to 1.2, or if the double-peak separation did not shrink as the Eddington ratio rose, the accretion-regulated BLR restructuring described here would be falsified. Alternatively, resolving the line profile with a non-parametric model rather than two fixed Gaussians in the Type 1.5-1.8 state of Mrk 1018 would show whether the double peaks are true components or a fitting artifact.

Watch

Extended reading notes

Core claim

We find that Mrk 1018 underwent a full-cycle changing-look transition within one year, around 2020, from Type 1.8 to Type 1.5/1.2 and back to Type 1.8, synchronized with a multi-band nucleus outburst. Over 45 years its Eddington ratio swung by a factor of 1000, reaching 0.02 at the peak, and the type follows accretion rate. For the first time we observe a turnover in the Balmer decrement with accretion, a decrease of double-peak separation as accretion increases, and a sharp rise in sigma_line at high Eddington ratio that drops FWHM/sigma_line from 2.96 to 1.71, signaling enhanced turbulence. The FWHM obeys the virial expectation FWHM proportional to $L5100^{-0}$.27, so the BLR remains virialized while turbulent motions grow with accretion, likely due to a transition from an advection-dominated to a standard disk. These observations establish accretion-regulated BLR evolution as the driver of changing-look phenomena in this source.

Load-bearing premise

The argument assumes that every broad Balmer line across all 45 years is truly composed of two Gaussian components, so the measured FWHM, sigma_line, and double-peak separation reflect real kinematics rather than fitting artifacts.

Editorial extensions

If this is right

  • If the accretion-regulated cycle is real, then type transitions in CL-AGNs need not be slow or rare: a full cycle can occur on roughly a year timescale when the accretion rate surges.
  • The observed FWHM-Lbol/LEdd scaling means single-epoch virial black hole masses in changing-look sources can remain reliable even during type flips, as long as the broadening is corrected.
  • The Balmer decrement turnover at an Eddington ratio near 0.004 offers a spectroscopic indicator of the accretion state transition between ADAF and standard disk regimes.
  • The double-peak separation decreasing with rising accretion provides a direct test for disk-wind or disk-like BLR models such as FRADO or Keplerian disk models.

Reading between the lines

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

  • If the same accretion-regulated behavior holds in other CL-AGNs, the diversity of broad-line profiles across the AGN population may be a single sequence in Eddington ratio rather than a set of distinct physical classes.
  • The one-year cycle implies that past claims about decades-long changing-look timescales may be biased by sparse sampling; denser monitoring could reveal many hidden fast cycles.
  • The apparent coupling between the low-ionization BLR and the hot dust torus (H-alpha lag close to W1 lag) suggests that simultaneous optical and mid-IR reverberation mapping of CL-AGNs might directly test whether the BLR is launched from the torus.
  • The sharp rise of sigma_line at high Eddington ratio could be observable as a profile-shape diagnostic in large spectroscopic surveys, potentially identifying the ADAF-to-SSD transition without X-ray data.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. Mrk 1018 is a changing-look AGN observed with Lijiang 2.4 m spectroscopy over seven seasons (2017-2024). The paper reports a full-cycle changing-look transition around 2020 in which the AGN type varied from 1.8 to 1.5/1.2 and back within about one year, accompanied by a multi-wavelength outburst. Combining these spectra with nine archival epochs, the authors reconstruct a 45-year type sequence and derive Eddington ratios from broad H-alpha luminosities. They report that the broad Balmer lines are single-peaked in Type 1.0-1.2 and double-peaked in Type 1.5-1.8, that the double-peak separation and FWHM decrease with increasing Eddington ratio, with FWHM proportional to (Lbol/LEdd)^-0.27, and that FWHM/sigma_line drops from 2.96 to 1.71 across the Type 1.5/1.2 boundary. They interpret these trends as evidence for a virialized BLR with accretion-dependent turbulence and for a transition from an inner ADAF to an outer standard disk. A virial black hole mass of (1.64 +/- 0.98) x 10^8 solar masses, consistent with the M-sigma mass, is derived from the H-beta lag and FWHM.

Significance. The paper's main value is the dense, well-calibrated spectroscopic sampling of a full cycle of changing-look behavior in a single object, including the detection of an outburst with clear multi-band time delays and a full cycle of type transitions. The data reduction appears careful: the [O III] lambda5007 light curve has only 6.9% scatter, and the comparison with 1ES 1927+654 is instructive. If the line-profile interpretation is correct, the reported transition from double-peaked to single-peaked broad lines and the sharp change in FWHM/sigma_line would be an important constraint on BLR geometry and the accretion-state transition. However, the primary physical conclusions are currently conditional on the assumed two-Gaussian decomposition of the broad lines and on Eddington ratios derived from the same broad-line fluxes, and the significance is therefore limited until these are validated.

major comments (2)
  1. [Section 2.2, Figure 9] The two-Gaussian model for the broad Balmer lines is adopted a priori in every epoch, and the quantities that drive the main physical claims—FWHM, sigma_line, and double-peak separation—are measured from this model. The manuscript does not provide a comparison with a single-Gaussian fit or with nonparametric measurements of the line width, nor does it show that the second Gaussian is not absorbing narrow-line residuals or an asymmetric wing. Without such a cross-check, the reported FWHM/sigma_line drop from 2.96 to 1.71 at the Type 1.5/1.2 boundary and the decreasing peak-separation trend in Figure 9c could be artifacts of the forced two-component decomposition. I request a model-selection test (e.g., AIC/BIC for one vs. two Gaussians) and direct measurement of FWHM and the second moment on the continuum-subtracted profiles for representative spectra of each type.
  2. [Section 3.4, Figure 9d; Section 3.3, Figure 9a] The Eddington ratio on the horizontal axes is obtained from the broad H-alpha luminosity via the Greene & Ho (2005) scaling, while the AGN type on the vertical axis in Figure 9a is defined by the broad H-beta/[O III] ratio and the FWHM in Figure 9d is measured from broad H-beta. Because both axes are constructed from the same broad-line spectra, part of the reported correlations is built in by construction: a larger broad-line luminosity raises the Eddington ratio and also makes the object appear more Type 1. An independent estimate of L_bol (for example from the fitted power-law continuum at 5100 Å, or from X-ray data) is needed to establish that the accretion rate genuinely regulates the type and line-width changes rather than merely re-expressing the same broad-line strength.
minor comments (5)
  1. [Throughout] There are numerous typographical and grammatical errors, including 'a accretion disk' (Section 1), 'qui pped' (Section 2.1), 'the the telluric' (Section 2.1), 'Out findings' (Section 3.4), and 'a a reference' (Section 2.2); a thorough language edit is needed.
  2. [Figure 6] In panel (a), the y-axis labels for H-alpha and H-beta list units as 'erg s cm^-2' rather than 'erg s^-1 cm^-2'.
  3. [Section 4.2, Figure 10] The conclusion that the BLR size exceeds the R-L relation during the outburst relies on time delays derived from Gaussian peak offsets, but the rising phase is poorly sampled and the Gaussian shape is assumed; the authors should present cross-correlation lags and explicitly discuss the impact of the sparse rising-phase sampling on the peak-time measurements.
  4. [Section 3.4] The reference 'Wu et al. 2024, submitted' is to an unpublished manuscript; it should be replaced with a published reference or removed, or its status clearly marked as 'in preparation'.
  5. [Abstract and Section 5] The phrase 'full-cycle changing-look transition' is used to describe a transition from Type 1.8 to 1.2 and back to 1.8; the authors should define what constitutes a 'full cycle' in this context, since the broad lines do not completely disappear.

Circularity Check

1 steps flagged · score 4.0 of 10

The accretion-regulated type transition claim is partly built in: the Eddington-ratio axis is derived from broad Hα luminosity, while the type axis is broad Hβ/[O III]; the other headline results rest on independent data.

  1. other [Section 3 (Eddington-ratio derivation) and Section 3.3 / Figure 9a]
    "By applying the relationship between the optical luminosity (L5100) and broad Hα luminosity (LHα) established by Greene & Ho (2005), represented as L5100=2.39 × 10^43(LHα/10^42)^0.86 erg s−1, we can obtain the optical luminosity for each observation. ... we estimate the Eddington ratio ... We investigate the type transition of Mrk 1018 in relation to the Eddington ratio, as shown in panel (a) of Figure 9, and find a positive correlation between the type transition and Eddington ratio. This shows that strongly varying accretion rate are responsible for regulating the AGN type transitions."

    Panel (a) of Figure 9 plots the AGN type, Hβ/[O III], against Lbol/LEdd. The [O III] flux is shown to be stable (6.9% scatter, Figure 3), so the y-axis is essentially Hβ. The Eddington ratio is computed from broad Hα luminosity using L5100=2.39×10^43(LHα/10^42)^0.86 and a fixed black-hole mass from Section 3.2, so the x-axis is proportional to LHα^0.86. Thus Figure 9a reduces to plotting Hβ against a power of Hα, two broad Balmer fluxes measured from the same spectra. A positive correlation is therefore substantially guaranteed by the Hα-Hβ flux coupling, not by an independent measurement of accretion rate.

full rationale

Most of the paper is a self-contained observational campaign. The multi-band outburst timescales, reverberation lags, the M-sigma mass check, and the color-magnitude behavior are independent of the circularity concern. The FWHM versus (Lbol/LEdd)^-0.27 relation is not fitted; it is derived by converting the external Bentz et al. (2013) R-L relation into FWHM, so that step is a consistency check rather than a prediction forced by the data. The one load-bearing partially circular element is the use of the Hα-based Eddington ratio as the independent driver in the type-transition correlation: since the AGN type is defined by Hβ/[O III] and the Eddington ratio is derived from Hα, the correlation in Figure 9a is substantially a Balmer-line self-correlation. The double-Gaussian decomposition is a modeling assumption that could bias FWHM/sigma and peak-separation measurements, but that is a systematic-risk issue rather than a circular reduction. There are self-citations (e.g., Kim et al. 2018 for archival spectra), but they are not load-bearing: the present authors show their own fits of the LJT spectra, and the cited prior work is not invoked as a uniqueness theorem or a fitted input. Overall, the central observational facts and the virial/mass checks remain independently supported, so the circularity is partial rather than total.

Assumptions & free parameters 1 free parameters · 6 assumptions · 0 invented entities

The paper relies on standard AGN scaling relations and a specific spectral decomposition model. No new physical entities are introduced. The Gaussian light-curve parameters are fitted to data but are not central to the main changing-look claim.

free parameters (1)
  • Gaussian sigma and peak time for each outburst light curve = 79 to 146 days for sigma; peak times around JD 2459040-2459195
    Fitted to the multi-band outburst light curves to derive characteristic timescales and time delays.
assumptions (6)
  • domain assumption Bentz et al. (2013) radius-luminosity relation applies to Mrk 1018
    Used to derive FWHM proportional to L^-0.27 and to compute expected BLR radii (Section 4.2).
  • domain assumption Greene and Ho (2005) L5100-LH-alpha relation applies to Mrk 1018
    Used to convert H-alpha luminosity to optical continuum luminosity at 5100 Angstroms (Section 3).
  • domain assumption Virial factor f=1 for the BLR
    Assumed to estimate virial mass from the time delay and line width (Section 3.2).
  • domain assumption Gas velocity dispersion from [O III] traces stellar velocity dispersion
    Used to estimate SMBH mass via the M-sigma relation (Section 3.2).
  • ad hoc to paper Double-Gaussian decomposition is an adequate model for broad Balmer lines
    All broad lines are fitted with two Gaussians; this modeling choice affects FWHM, sigma, and peak separation measurements (Section 2.2).
  • ad hoc to paper Spectra with H-beta/[O III] below 0.1 are unreliable and excluded
    Selection criterion applied to the correlations in Figure 9, potentially biasing the low-Eddington-ratio end (Figure 9 caption).

how reviews work

0 comments
Cite this review

Pith. "Pith review of A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018." pith.science (2026). https://pith.science/paper/UYCBWWVP

@misc{pith2026241118917,
  author       = {Pith},
  title        = {Pith review of: A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/UYCBWWVP}},
  note         = {Machine review of arXiv:2411.18917}
}
abstract

Changing-look active galactic nuclei (CL-AGNs), characterized by emerging or disappearing of broad lines accompanied with extreme continuum flux variability, have drawn much attention for their potential of revealing physical processes underlying AGN evolution. We perform seven-season spectroscopic monitoring on Mrk~1018, one of the earliest identified CL-AGN. Around 2020, we detect a full-cycle changing-look transition of Mrk~1018 within one year, associated with a nucleus outburst, which likely arise from the disk instability in the transition region between the outer standard rotation-dominated disk and inner advection-dominated accretion flow. Over the past forty-five years, the accretion rate of Mrk~1018 changed 1000 times and the maximum Eddington ratio reached 0.02. By investigating the relation between broad-line properties and Eddington ratio ($L_{\rm bol}/L_{\rm Edd}$), we find strong evidence that the full-cycle type transition is regulated by accretion. There exists a turnover point in the Balmer decrement, which is observed for the first time. The broad Balmer lines change from a single peak in Type 1.0-1.2 to double peaks in Type 1.5-1.8 and the double-peak separation decreases with increasing accretion rate. We also find that the full width at half maximum (FWHM) of the broad Balmer lines obeys FWHM$\propto (L_{\rm bol}/L_{\rm Edd})^{-0.27}$, as expected for a virialized BLR. The velocity dispersion $\sigma_{\rm line}$ follows a similar trend in Type 1.5-1.8, but displays a sharp increases in Type 1.0-1.2, resulting in a dramatic drop of FWHM/$\sigma_{\rm line}$. These findings suggest that a virialized BLR together with accretion-dependent turbulent motions might be responsible for the diversity of BLR phenomena across AGN population.

Figures

Figures reproduced from arXiv: 2411.18917 by the authors.

Figure 1
Figure 1. An example of the telluric correction and spectral flux calibration. The top and bottom panels are for the comparison star and Mrk 1018, respectively. In each panel, the black line shows the observed spectra (in counts, left vertical axis), the red line shows the telluric￾corrected spectrum, and the blue line shows the flux-calibrated spectrum (in units of erg s−1 cm−2 A˚ −1 , right vertical axis). The three vertica… view at source ↗
Figure 2
Figure 2. An example of multicomponent fitting and decomposition of the spectrum. The fitting model includes a power law (fλ ∝ λ α , α is the spectral index) for the AGN continuum (blue), an iron template for the iron multiplets (green), a stellar template for the host-galaxy starlight (gray), two double Gaussians for each broad Balmer line (Hβ and Hα, magenta), single Gaussian for each narrow Balmer line (Hβ and Hα, lime), s… view at source ↗
Figure 3
Figure 3. The light curve of the [O III] λ5007 in the LJT observation period. The red dashed line represents the mean flux (3.8×10−14 erg s−1 cm−2 ). Boroson & Green (1992) for the iron multiplets. (3) A stellar template with an age of 11 Gyr and metallicity of Z = 0.05 from Bruzual & Charlot (2003) to account for the host-galaxy starlight. (4) Double Gaussians for each broad Balmer lines (Hβ and Hα). In practice, we initiall… view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: Long-term variability of Mrk 1018 from 1979 to 2024 for (a) the Hα flux, (b) the Hβ flux, (c) the flux ratio Hβ/[O III]λ5007 (indicating the type transition), and (d) the Eddington ratio. The Hα and Hβ fluxes are in units of erg s−1 cm−2 . The earlier data are in blue …
Figure 5
Figure 5. Figure 5: Evolution of the Hβ and Hα line profiles. Each row of panels displays the characteristic profiles of different types, with the broad Hβ in the left and Hα in the right. The black curve shows the original data, the magenta curves show the broad-line components, the oran…
Figure 6
Figure 6. Figure 6: Multi-scale outbursts accompanied by a short-lived yet full-cycle changing-look transition in Mrk 1018. Panel (a) displays the light curves of ZTF photometry (combined g&r-, g-, and r-band, in units of erg s−1 cm−2 A˚ −1 ), the broad Balmer lines (Hβ and Hα, in units o…
Figure 7
Figure 7. Figure 7: Optical and mid-infrared color−magnitude relations based on the Gaussian fitting model (see Appendix B). The left panels (aa￾ad) are for the optical bands, while the right panels (ba-bd) are for the mid-infrared bands. The first row (panels aa and ba) displays the obse…
Figure 8
Figure 8. Figure 8: Evolution of the broad Hα line width for Mrk 1018 dur￾ing the outburst phase (JD2,458,811-2,459,433). The panel (a) is for the FWHM and the panel (b) is for σline. The vertical dashed lines indicate the peak time of the broad Hα line. The spectral broad￾ening in each o…
Figure 9
Figure 9. Figure 9: Accretion-dependent type transitions and the broad-line properties in Mrk 1018. The data observed by LJT is shown by red points and the archival data is shown by blue points. Panel (a-c) show the changes of the AGNs type (Hβ/[O III]λ5007), the Balmer decrement (Hα/Hβ),…
Figure 10
Figure 10. Figure 10: Relations between emission region sizes and opti￾cal luminosities. The dashed lines represent the empirical radius￾luminosity relations for the Hβ (in black) and Hα (in pink) BLR (Bentz et al. 2013; Cho et al. 2023) and the torus (Chen et al. 2023b, in red and green).…
Figure 11
Figure 11. Figure 11: The light curves (in flux density) from ZTF and ATLAS along with model fitting. After subtracting the underlying trend, the outburst light-curve profiles are fitted using two models, one with Gaussian rising and exponential dimming (GE; blue lines), and the other with…
Figure 12
Figure 12. Figure 12: Same as [PITH_FULL_IMAGE:figures/full_fig_p021_12.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 2 Pith papers

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

  1. A Composite Broad-Line Region in SDSS J1609+4902: a Double-Peaked Disk component and a Gaussian Component

    astro-ph.GA 2025-06 conditional novelty 6.0 of 10

    SDSS J1609+4902 shows an Hα profile with both a standard Gaussian broad-line component and an extremely broad double-peaked component that can be modeled as a disk from about 70 to 520 gravitational radii.

  2. Exploring variation of double-peak broad-line profile in strongly variable AGNs

    astro-ph.GA 2024-12 conditional novelty 5.0 of 10

    The FRADO dust-wind model predicts double-peaked broad lines at low Eddington ratios, single peaks at high ratios, multi-year profile transitions after accretion changes, and a Z>=5 solar metallicity requirement to ma...

Reference graph

Works this paper leans on

13 extracted references · 2 linked inside Pith · cited by 2 Pith papers

  1. [10]

    2000, ApJL, 539, L13

    doi:10.1038/s41550-019-0970-1 Gebhardt, K., Bender, R., Bower, G., et al. 2000, ApJL, 539, L13. doi:10.1086/312840 Goad, M. R., Korista, K. T., & Ruff, A. J. 2012, MNRAS, 426,

    doi:10.1038/s41550-019-0970-1 2000

  2. [26]

    N., Auger, M

    doi:10.1088/0067-0049/217/2/26 Bennert, V . N., Auger, M. W., Treu, T., et al. 2011, ApJ, 742, 107. doi:10.1088/0004-637X/742/2/107 Bentz, M. C., Denney, K. D., Grier, C. J., et al. 2013, ApJ, 767,

    doi:10.1088/0067-0049/217/2/26 2011

  3. [85]

    J., Shu, X

    doi:10.3847/1538-4357/ad2f30 Zhang, W. J., Shu, X. W., Sheng, Z. F., et al. 2022, A&A, 660, A119. doi:10.1051/0004-6361/202142253 Zhang, X.-G. 2023, MNRAS, 526, 6015. doi:10.1093/mnras/stad3153 Zhou, H., Shi, X., Yuan, W., et al. 2019, Nature, 573, 83. doi:10.1038/s41586-019-1510-y

    doi:10.3847/1538-4357/ad2f30 2022

  4. [94]

    D., Lyke, J

    doi:10.3847/1538-4357/ab39e4 Tran, H. D., Lyke, J. E., & Mader, J. A. 2011, ApJL, 726, L21. doi:10.1088/2041-8205/726/2/L21 Trippe, M. L., Crenshaw, D. M., Deo, R. P., et al. 2010, ApJ, 725,

    doi:10.3847/1538-4357/ab39e4 2011

  5. [134]

    C., et al

    doi:10.1088/0004-637X/796/2/134 Dong, X.-B., Wang, J.-G., Ho, L. C., et al. 2011, ApJ, 736, 86. doi:10.1088/0004-637X/736/2/86 Du, P., Lu, K.-X., Zhang, Z.-X., et al. 2016, ApJ, 825, 126. doi:10.3847/0004-637X/825/2/126 Du, P., Zhang, Z.-X., Wang, K., et al. 2018, ApJ, 856, 6. doi:10.3847/1538-4357/aaae6b Elitzur, M., Ho, L. C., & Trump, J. R. 2014, MNRAS...

    arXiv doi:10.48550/arxiv.2409.01637 2011

  6. [135]

    M., Wisniewski, W

    doi:10.1086/164758 Cutri, R. M., Wisniewski, W. Z., Rieke, G. H., et al. 1985, ApJ, 296, 423. doi:10.1086/163461 Czerny, B. & Hryniewicz, K. 2011, A&A, 525, L8. doi:10.1051/0004-6361/201016025 Czerny, B., Panda, S., Prince, R., et al. 2023, A&A, 675, A163. doi:10.1051/0004-6361/202345844 Denney, K. D., De Rosa, G., Croxall, K., et al. 2014, ApJ, 796,

    doi:10.1086/164758 1985

  7. [149]

    C., Walsh, J

    doi:10.1088/0004-637X/767/2/149 Bentz, M. C., Walsh, J. L., Barth, A. J., et al. 2010, ApJ, 716, 993. doi:10.1088/0004-637X/716/2/993 Blandford, R. D. & McKee, C. F. 1982, ApJ, 255, 419. doi:10.1086/159843 Boroson, T. A. & Green, R. F. 1992, ApJS, 80, 109. doi:10.1086/191661 Brogan, R., Krumpe, M., Homan, D., et al. 2023, A&A, 677, A116. doi:10.1051/0004-...

    arXiv 2010

  8. [341]

    doi:10.1086/192341 Naddaf, M. H. & Czerny, B. 2022, A&A, 663, A77. doi:10.1051/0004-6361/202142806 Nagoshi, S., Iwamuro, F., Yamada, S., et al. 2024, MNRAS, 529,

    doi:10.1086/192341 2022

Show all 13 references
  1. [393]

    doi:10.1093/mnras/stae319 Nelson, C. H. & Whittle, M. 1996, ApJ, 465, 96. doi:10.1086/177405 Netzer, H. 1975, MNRAS, 171, 395. doi:10.1093/mnras/171.2.395 Netzer, H. 2013, The Physics and Evolution of Active Galactic Nuclei, by Hagai Netzer, Cambridge, UK: Cambridge University...

    1996 doi

  2. [1691]

    2011, ApJ, 731, 50

    doi:10.1093/mnras/stv2385 Sakata, Y ., Morokuma, T., Minezaki, T., et al. 2011, ApJ, 731, 50. doi:10.1088/0004-637X/731/1/50 Shakura, N. I. & Sunyaev, R. A. 1973, A&A, 24, 337 Shapovalova, A. I., Popovi´c, L. ˇC., Burenkov, A. N., et al. 2010, A&A, 509, A106. doi:10.1051/0004-...

    2011

  3. [1749]

    doi:10.1088/0004-637X/725/2/1749 Urry, C. M. & Padovani, P. 1995, PASP, 107, 803. doi:10.1086/133630 V´eron-Cetty, M.-P., Joly, M., & V´eron, P. 2004, A&A, 417, 515 V´eron-Cetty, M.-P., V´eron, P., & Gonc ¸alves, A. C. 2001, A&A, 372, 730. doi:10.1051/0004-6361:20010489 Verone...

    1995 doi

  4. [3427]

    & Halpern, J

    doi:10.1093/mnras/stu2266 Chen, K. & Halpern, J. P. 1989, ApJ, 344, 115. doi:10.1086/167782 Chen, Y .-J., Bao, D.-W., Zhai, S., et al. 2023a, MNRAS, 520, 1807. doi:10.1093/mnras/stad051 Chen, Y .-J., Liu, J.-R., Zhai, S., et al. 2023b, MNRAS, 522, 3439. doi:10.1093/mnras/stad1...

    1989 doi

  5. [4925]

    doi:10.1093/mnras/stz3244 Greene, J. E. & Ho, L. C. 2005, ApJ, 630, 122. doi:10.1086/431897 Greene, J. E., Strader, J., & Ho, L. C. 2020, ARA&A, 58, 257. doi:10.1146/annurev-astro-032620-021835 Grier, C. J., Trump, J. R., Shen, Y ., et al. 2017, ApJ, 851, 21. doi:10.3847/1538-...

    2005 doi arXiv

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.