Pith. sign in

REVIEW 2 major objections 6 minor 300 references

Part of the quasar microlensing disc-size excess can come from treating disc-plus-BLR light as a single compact disc.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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

T0 review · grok-4.5

2026-07-12 03:28 UTC pith:IFZ4YKBP

load-bearing objection Clean end-to-end mock demonstration that BLR diffuse continuum biases multi-epoch microlensing sizes toward the composite half-light radius, with wavelength dependence set by f_BLR. the 2 major comments →

arxiv 2607.03291 v1 pith:IFZ4YKBP submitted 2026-07-03 astro-ph.GA astro-ph.HE

Physically motivated AGN emissivity profiles and their effects on quasar microlensing signatures. 1. Multi-epoch accretion disc size inference

Scott Hagen (1 , 2 , 3) , Carina Fian (3 , 4) ((1) IFPU , (2) SISSA , (3) INAF-OATs , (4) University of Nova Gorica) This is my paper
classification astro-ph.GA astro-ph.HE
keywords quasar microlensingaccretion disc sizebroad-line region continuumemissivity profilesdisc-size problemwarm Comptonisationhalf-light radius
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Microlensing is one of the few ways to measure the physical size of a quasar's optical and ultraviolet continuum. Those sizes often come out larger than a standard thin disc predicts. This paper argues that the mismatch is partly an interpretation problem: the observed light is a mix of a compact accretion disc and much larger-scale diffuse continuum from the broad-line region. The authors build energetically self-consistent disc emissivity maps from a stratified accretion model, add photoionised BLR continuum, convolve the composite sources with realistic magnification maps, and recover sizes from mock multi-epoch light curves. Detailed disc shape is only a second-order effect; the BLR smooths the caustic network and pulls the recovered half-light radius toward the composite effective size, with a strength set by how much flux the diffuse component contributes in the chosen band. A sympathetic reader cares because this offers a wavelength-dependent, physically motivated route to reconciling microlensing sizes with disc theory without discarding the disc.

Core claim

When mock multi-epoch microlensing light curves generated from a composite warm-Comptonisation plus BLR source are interpreted with compact-only emissivity models, the recovered half-light radii tend toward the effective half-light radius of the composite emission rather than the true compact-disc size. The bias is set primarily by the fractional BLR contribution to the SED and the radial shape of the compact-disc emissivity, not by the absolute BLR radius itself when that fraction is below half.

What carries the argument

Energetically self-consistent bandpass emissivity maps from a radially stratified accretion-flow model, combined with a cloudy-computed diffuse BLR continuum and convolved with source-plane microlensing magnification maps; size is then recovered from the standard-deviation statistics of mock light-curve ensembles.

Load-bearing premise

The broad-line region is treated as a single constant-density, constant-ionisation cloud in a simple bi-cone, projected as a uniform annular top-hat; if real BLRs have strong gradients or different covering, the diffuse flux fraction and smoothing scale change.

What would settle it

In multi-band microlensing campaigns, measure the recovered size excess as a function of continuum wavelength and compare it with the independently estimated BLR continuum fraction in each band; the excess should track that fraction and the compact-disc emissivity shape rather than a constant factor or a pure BLR-scale size.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Part of the reported optical/UV microlensing disc-size excess can be re-read as composite emission rather than a failure of thin-disc theory.
  • The bias is wavelength-dependent and strongest where the diffuse BLR continuum fraction is highest, so multi-band campaigns can separate disc and BLR contributions.
  • Compact-only size recovery on BLR-contaminated light curves systematically returns the composite half-light radius, not the pure disc radius.
  • Detailed shape of the compact-disc emissivity is secondary to the effective half-light radius set by the BLR flux fraction.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The same composite picture already invoked for continuum reverberation lags should produce correlated wavelength-dependent biases in both lag and microlensing size measurements.
  • If the BLR continuum fraction can be constrained independently (e.g., from line-free continuum windows or spectral decomposition), microlensing sizes can be corrected rather than discarded.
  • Future size-recovery pipelines that forward-model a disc-plus-annulus source will be less biased than pure Gaussian or thin-disc templates.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 6 minor

Summary. The paper constructs energetically self-consistent optical/UV emissivity maps from the radially stratified agnsed framework (standard thin disc and warm-Comptonised disc), adds a diffuse free-bound continuum from a single-zone bi-conical BLR computed with cloudy, and convolves the resulting composite sources with representative positive- and negative-parity microlensing magnification maps. Mock COSMOGRAIL-like multi-epoch light curves are generated and inverted with a variability-amplitude (σ_Δm) size-recovery pipeline. Same-model recovery tests return half-light radii within ~16% of input; when composite disc+BLR mocks are interpreted with compact-only models, recovered sizes track the composite effective half-light radius rather than the true compact-disc size. The bias is argued to be set primarily by the bandpass-dependent BLR flux fraction and the radial shape of the compact emissivity (via the half-light definition, Eq. 9), supporting the claim that part of the microlensing disc-size excess can arise from treating composite emission as a single compact disc.

Significance. If the result holds, it supplies a physically motivated, wavelength-dependent mechanism that can partially reconcile microlensing size measurements with standard disc theory, in close analogy with the BLR-driven lag excess in continuum reverberation. Strengths include: (i) self-consistent SED-to-emissivity mapping from agnsed rather than ad-hoc Gaussians; (ii) controlled forward simulations with explicit same-model recovery checks (Appendix C); (iii) an analytic reduction of the composite half-light radius for f_BLR < 0.5 (Eq. 9); and (iv) public code (AGNmap). The claim is carefully scoped (“part of the excess could arise”) and does not overclaim a full solution of the disc-size problem. The work is a useful, falsifiable contribution to the microlensing and AGN continuum literature.

major comments (2)
  1. §5.3 and Appendix C / Table C.1: Same-model recovery returns sizes systematically larger than input by a mean factor ~1.16 across bands and parities. Fig. 5 is interpreted as showing that recovered sizes “tend toward the effective half-light radius of the input composite model.” Because the recovery pipeline itself is biased high at that level, the quantitative excess relative to the compact-disc half-light radii should be reported after correcting for (or at least subtracting in quadrature / discussing) this baseline offset, so that the BLR-driven bias is not conflated with the recovery systematics.
  2. §3 and Appendix A: The BLR is a single constant-density, constant-ionisation cloudy calculation (fc=0.3, αl=60°, nH=10^11.5 cm−3, NH=10^23 cm−2) projected as a uniform top-hat annulus. The central qualitative claim is robust to this choice, but the quantitative bias amplitudes in Fig. 5 and the wavelength dependence are set by f_BLR, which is model-dependent. Either a short sensitivity test (e.g. varying fc or nH by factors of a few) or an explicit statement in §5.3/§6 that the reported size excesses are for this fiducial BLR only is needed so readers do not over-generalise the numerical factors.
minor comments (6)
  1. Fig. 3: The unconvolved maps and histograms are clear, but the figure caption and main text would benefit from quoting the BLR flux fractions (f_BLR ~30% at 7500 Å, ~1.4% at 1650 Å) next to the corresponding panels so the wavelength dependence is immediately readable.
  2. §5.1: The adopted veff = 600 km s−1 is taken from Mediavilla et al. (2016); a one-sentence note that absolute size scales with the Einstein radius and that relative biases (composite vs compact) are largely velocity-independent would help non-specialists.
  3. Eq. (8)–(9): The monochromatic half-light definition is standard, but the transition from the full integral to the disc-only cumulative form when f_BLR < 0.5 could be flagged more explicitly as an approximation that fails once R_1/2 reaches the BLR annulus (as the text already notes for λ ≳ 10^4 Å).
  4. §2.1: General-relativistic light bending is neglected with a reasoned argument for optical/UV; a brief pointer to the spin/truncation regimes where this would matter (already cited via Hagen & Done 2023a) would complete the caveat.
  5. Typographical / production: “agnsed” and “cloudy” are sometimes set in roman and sometimes not; consistent treatment (e.g. small-caps or monospace for code names) would improve readability. Also “cosmograil” should be capitalised consistently as COSMOGRAIL when referring to the survey.
  6. Appendix B schematic is helpful; ensuring that the published version has sufficient resolution for the likelihood/posterior panels would avoid production issues.

Circularity Check

0 steps flagged

No significant circularity: pure forward-modelling of synthetic light curves; recovered sizes track the input composite half-light radius by the known sensitivity of microlensing to characteristic size, not by re-fitting real data or self-definition of the target claim.

full rationale

The paper constructs energetically self-consistent disc+BLR emissivity maps from agnsed + cloudy, convolves them with independent FMM–IPM magnification maps, draws mock trajectories, and recovers half-light radii from the variability statistic σ_Δm via a joint posterior over an ensemble of tracks. Same-model recovery tests (Appendix C) return sizes consistent with the known input half-light radii (average ratio ~1.16), confirming the procedure is primarily sensitive to characteristic size (as already established by Mortonson et al. 2005). When composite mocks are interpreted with compact-only models, the recovered sizes track the composite R_1/2 (Fig. 5), which follows directly from the monochromatic half-light definition (Eqs. 8–9) once f_BLR is non-zero; this is an expected consequence of the statistic, not a circular re-labelling of a fit. Self-citations (Hagen & Done implementations of agnsed/irradiation, Fian et al. 2023a for the qualitative BLR-smoothing idea, Hagen et al. 2024 for the bi-conical geometry) supply methods and prior motivation; none is a load-bearing uniqueness theorem that forces the present numerical result. No observational sizes are fitted and then re-predicted, no ansatz is smuggled as a theorem, and the central claim remains an independent quantification of bias under stated modelling assumptions. Score 1 only for the minor, non-load-bearing self-citations that are normal in a methods-extension paper.

Axiom & Free-Parameter Ledger

6 free parameters · 5 axioms · 0 invented entities

The central claim rests on a chain of standard accretion and photoionisation assumptions plus a set of fiducial numerical choices that fix the BLR flux fraction and geometry. No new physical entities are postulated; the free parameters control the amplitude of the bias rather than its existence. The ledger therefore lists the modelling choices that, if altered substantially, would change the quantitative size overestimation while leaving the qualitative smoothing argument intact.

free parameters (6)
  • BLR covering fraction fc = 0.3
    Fixed at 0.3 following Baskin & Laor (2018); directly sets the absolute BLR luminosity and therefore the flux fraction that drives the half-light-radius bias.
  • BLR hydrogen density nH and column NH = nH=10^11.5 cm−3, NH=10^23 cm−2
    Chosen as 10^11.5 cm−3 and 10^23 cm−2 to produce mostly neutral gas at the mid-radius; control the cloudy-computed diffuse continuum spectrum and its bandpass-dependent fraction.
  • Launch angle αl and launch radius rl = αl=60°, rl≈5700 RG
    αl=60° and rl set so that the geometric-mean BLR radius lies on the Bentz et al. (2013) R–L relation; fix the projected annular size that smooths the caustic network.
  • Hot-corona truncation radius rh and warm-corona parameters = rh=15, Γw=2.7, kTe,w=0.2 keV
    rh=15 RG, kTe,w=0.2 keV, Γw=2.7 (and hot-corona Γh=1.9, kTe,h=100 keV) define the compact emissivity profiles and the ionising SED that powers the BLR.
  • Black-hole mass, accretion rate, spin = M=1e8 M⊙, ṁ=0.1, a=0
    Fiducial M=10^8 M⊙, ṁ=0.1, a=0 set absolute physical scales of both disc and BLR; size recovery later rescales half-light radius without recomputing the SED.
  • Effective transverse velocity veff = 600 km s−1
    Fixed at 600 km s−1 from Mediavilla et al. (2016) to set track lengths on the magnification maps; affects sampling of caustic structure but not the half-light-radius bias itself.
axioms (5)
  • domain assumption Accretion flow follows Novikov–Thorne emissivity with radial stratification into standard disc, warm Comptonisation, and hot corona (agnsed framework).
    Section 2; supplies the compact emissivity maps and ionising SED. Standard in the field but not uniquely required by the data.
  • ad hoc to paper BLR is a single bi-conical structure of constant density and ionisation, emitting isotropically into 2π and visible only on the near side.
    Section 3 and Appendix A; simplifies cloudy calculation and projection to a top-hat annulus. Real BLRs have gradients.
  • domain assumption Microlensing size is recoverable from the standard deviation of multi-epoch magnitude variability after convolution with source-plane magnification maps.
    Section 5.2; common statistical approach, but omits full light-curve trajectory fitting used in some observational analyses.
  • domain assumption General-relativistic light bending is negligible for optical/UV microlensing sizes.
    Section 2.1; justified by concentration of GR effects at small radii, but remains an approximation.
  • domain assumption Stellar mass fraction ~20% and microlens mass 0.3 M⊙ produce representative caustic networks whose magnification PDFs are insensitive to the exact mass function.
    Section 4.1; standard microlensing literature assumption.

pith-pipeline@v1.1.0-grok45 · 27125 in / 3538 out tokens · 34893 ms · 2026-07-12T03:28:24.281358+00:00 · methodology

0 comments
read the original abstract

Quasar microlensing is uniquely sensitive to the size-scale of the accretion flow, offering one of the few direct probes of the accretion structure on micro-arcsecond scales. However, microlensing-based measurements in the optical and UV often find sizes systematically larger than expected from standard Shakura-Sunyaev disc theory, commonly referred to as the disc-size problem similar to that seen in continuum reverberation campaigns. But this assumes that all the emission comes from a single compact disc, neglecting the diffuse emission from the BLR which originates on much larger spatial scales. In this paper we directly quantify the effect of large-scale diffuse emission on the observed microlensing signatures. We adapt the physically motivated agnsed model to construct energetically self-consistent emissivity profiles in any given bandpass. Since this also predicts the full SED, we combine these SEDs with cloudy to give a diffuse BLR component. We convolve these models with representative microlensing magnification maps, and generate mock microlensing light curves to directly assess the inferred source size under different physical conditions. While the detailed shape of the disc emissivity profile has only a higher-order effect on the microlensing profile, the inclusion of the BLR makes a significant impact since this naturally smooths out the caustic network over larger scales. This introduces a significant bias when interpreted purely as a compact disc. However, the strength of this bias depends predominantly on the fractional contribution of the diffuse emission to the SED in the bandpass being considered, as this sets the effective half-light radius, giving an important wavelength dependence. We conclude that part of the excess in microlensing-inferred accretion disc sizes could arise from interpreting a composite (disc+BLR) picture as a single compact disc.

Figures

Figures reproduced from arXiv: 2607.03291 by 2, (2) SISSA, 3), (3) INAF-OATs, 4) ((1) IFPU, (4) University of Nova Gorica), Carina Fian (3, Scott Hagen (1.

Figure 1
Figure 1. Figure 1: Top: Model SEDs for the fiducial warm-Comptonised disc model (green solid line) and standard Shakura & Sunyaev (1973) disc model (magenta dashed line). In both cases, the ac￾cretion flow truncates into an inner X-ray-emitting plasma below rh = 15, producing the high-energy X-ray tail. The dotted curves show the individual disc and warm-Comptonised disc compo￾nents. The hatched region marks the unobservable… view at source ↗
Figure 2
Figure 2. Figure 2: Top: Optical/UV portion of the model SED including the diffuse BLR continuum contribution. The intrinsic warm￾Comptonised disc emission is shown as a dashed green line, the diffuse BLR component as a dashed orange line, and the total ob￾served SED as a solid black line. The shaded regions indicate the bandpasses used to extract the radial emissivity profiles shown in the bottom panel and later used to comp… view at source ↗
Figure 3
Figure 3. Figure 3: Model convolution results for the positive-parity image (top row) and negative-parity image (bottom row). [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Example simulated light curves. Top row: The left panel shows the input magnification map for the positive-parity image used to generate the light curves. The coloured circles, shown in magenta and yellow, mark the initial disc positions, while the corresponding straight lines indicate the direction of motion. The middle and right panels show the magnification pattern across the AGN model grid used to comp… view at source ↗
Figure 5
Figure 5. Figure 5: Recovered half-light radii from simulated microlens [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

300 extracted references · 109 canonical work pages · 102 internal anchors

  1. [1]

    The evolution of soft excess and X-ray continuum

    Multiwavelength properties of changing-state active galactic nuclei: I. The evolution of soft excess and X-ray continuum. , keywords =. doi:10.1051/0004-6361/202556654 , archivePrefix =. 2601.07337 , primaryClass =

    doi:10.1051/0004-6361/202556654

  2. [2]

    Size of the accretion disk in the gravitationally lensed quasar SDSS J1004+4112 from the statistics of microlensing magnifications

    Size of the Accretion Disk in the Graviationally Lensed Quasar SDSS J1004+4112 from the Statistics of Microlensing Magnifications. , keywords =. doi:10.3847/0004-637X/830/2/149 , archivePrefix =. 1608.03831 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/830/2/149

  3. [3]

    Estimate of the Accretion Disk Size in the Gravitationally Lensed Quasar HE 0435-1223 using Microlensing Magnification Statistics

    Estimate of the Accretion Disk Size in the Gravitationally Lensed Quasar HE 0435-1223 Using Microlensing Magnification Statistics. , keywords =. doi:10.3847/1538-4357/aaeed5 , archivePrefix =. 1811.03312 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaeed5

  4. [4]

    Revealing the structure of the lensed quasar Q 0957+561. I. Accretion disk size. , keywords =. doi:10.1051/0004-6361/202039854 , archivePrefix =. 2108.05212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202039854

  5. [5]

    Diffuse emission in microlensed quasars and its implications for accretion-disk physics

    Diffuse emission in microlensed quasars and its implications for accretion-disk physics. , keywords =. doi:10.1051/0004-6361/202346766 , archivePrefix =. 2307.14824 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202346766

  6. [6]

    Size is Everything: Universal Features of Quasar Microlensing with Extended Sources

    Size Is Everything: Universal Features of Quasar Microlensing with Extended Sources. , keywords =. doi:10.1086/431195 , archivePrefix =. astro-ph/0408195 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/431195

  7. [7]

    Probing the dark matter radial profile in lens galaxies and the size of X-ray emitting region in quasars with microlensing

    Probing the Dark Matter Radial Profile in Lens Galaxies and the Size of X-Ray Emitting Region in Quasars with Microlensing. , keywords =. doi:10.1088/0004-637X/806/2/251 , archivePrefix =. 1502.00394 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/806/2/251

  8. [8]

    The Average Size and Temperature Profile of Quasar Accretion Disks

    The Average Size and Temperature Profile of Quasar Accretion Disks. , keywords =. doi:10.1088/0004-637X/783/1/47 , archivePrefix =. 1401.2785 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/783/1/47

  9. [9]

    First Direct Evidence for Keplerian Rotation in Quasar Inner Broad Line Regions

    First Direct Evidence for Keplerian Rotation in Quasar Inner Broad-line Regions. , keywords =. doi:10.3847/2041-8213/ad654d , archivePrefix =. 2407.13381 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ad654d 2041

  10. [10]

    , keywords =

    Unified models for active galactic nuclei and quasars. , keywords =. doi:10.1146/annurev.aa.31.090193.002353 , adsurl =

    doi:10.1146/annurev.aa.31.090193.002353

  11. [11]

    , keywords =

    Unified Schemes for Radio-Loud Active Galactic Nuclei. , keywords =. doi:10.1086/133630 , archivePrefix =. astro-ph/9506063 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/133630

  12. [12]

    and Fian, C

    Andlar, M. and Fian, C. and Hanslmeier, A. and Mu. Influence of emission features on accretion disk size estimates in microlensed quasars , journal =. 2026 , note =

    2026

  13. [13]

    Peculiar Transverse Velocities of Galaxies from Quasar Microlensing. Tentative Estimate of the Peculiar Velocity Dispersion at $z\sim 0.5$

    Peculiar Transverse Velocities of Galaxies from Quasar Microlensing. Tentative Estimate of the Peculiar Velocity Dispersion at z -0.5ex 0.5. , keywords =. doi:10.3847/0004-637X/832/1/46 , archivePrefix =. 1609.02671 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/832/1/46

  14. [14]

    Quantitative Interpretation of Quasar Microlensing Light Curves

    Quantitative Interpretation of Quasar Microlensing Light Curves. , keywords =. doi:10.1086/382180 , archivePrefix =. astro-ph/0307422 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/382180

  15. [15]

    Fast Multipole Method for Gravitational Lensing. Application to High Magnification Quasar Microlensing

    Fast Multipole Method for Gravitational Lensing: Application to High-magnification Quasar Microlensing. , keywords =. doi:10.3847/1538-4357/ac9e59 , archivePrefix =. 2211.00354 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac9e59

  16. [16]

    Journal of Computational Physics , keywords =

    A Fast Algorithm for Particle Simulations. Journal of Computational Physics , keywords =

  17. [17]

    , keywords =

    A Fast and Very Accurate Approach to the Computation of Microlensing Magnification Patterns Based on Inverse Polygon Mapping. , keywords =

  18. [18]

    , keywords =

    New Developments on Inverse Polygon Mapping to Calculate Gravitational Lensing Magnification Maps: Optimized Computations. , keywords =

  19. [19]

    The Statistics of Microlensing Light Curves: I. Amplification Probability Distributions

    The statistics of microlensing light curves - I. Amplification probability distributions. , keywords =. doi:10.1093/mnras/276.1.103 , archivePrefix =. astro-ph/9504018 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/276.1.103

  20. [20]

    , keywords =

    Determining the microlens mass function from quasar microlensing statistics. , keywords =. doi:10.1046/j.1365-8711.2001.03917.x , archivePrefix =. astro-ph/0008008 , primaryClass =

    doi:10.1046/j.1365-8711.2001.03917.x 2001

  21. [21]

    Measuring accretion disk sizes of lensed quasars with microlensing time delay in multi-band light curves

    Measuring accretion disk sizes of lensed quasars with microlensing time delay in multi-band light curves. , keywords =. doi:10.1051/0004-6361/202038971 , archivePrefix =. 2007.14416 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202038971 2007

  22. [22]

    , keywords =

    Flux variations of QSO 0957 + 561 A, B and image splitting by stars near the light path. , keywords =. doi:10.1038/282561a0 , adsurl =

    doi:10.1038/282561a0

  23. [23]

    , keywords =

    Star disturbances in gravitational lens galaxies. , keywords =

  24. [24]

    Saas-Fee Advanced Course 33: Gravitational Lensing: Strong, Weak and Micro , year = 2006, editor =

    Part 4: Gravitational microlensing. Saas-Fee Advanced Course 33: Gravitational Lensing: Strong, Weak and Micro , year = 2006, editor =

    2006

  25. [25]

    , keywords =

    Slim Accretion Disks. , keywords =. doi:10.1086/166683 , adsurl =

    doi:10.1086/166683

  26. [26]

    , keywords =

    Thermal Equilibria of Accretion Disks. , keywords =. doi:10.1086/187709 , archivePrefix =. astro-ph/9409018 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/187709

  27. [27]

    The ultraviolet excess of luminous quasars. II. Evidence for massive accretion disks. , keywords =. doi:10.1086/160981 , adsurl =

    doi:10.1086/160981

  28. [28]

    The Physics and Evolution of Active Galactic Nuclei

  29. [29]

    Continuum reverberation mapping of the quasar PG 2130+099

    Continuum reverberation mapping of the quasar PG 2130+099. , keywords =. doi:10.1051/0004-6361/202141509 , archivePrefix =. 2111.07385 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202141509

  30. [30]

    Continuum reverberation mapping of MCG 08-11-011

    Continuum reverberation mapping of MCG 08-11-011. , keywords =. doi:10.1051/0004-6361/202244905 , archivePrefix =. 2302.08402 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202244905

  31. [31]

    UV/Optical disk reverberation lags despite a faint X-ray corona in the AGN Mrk 335

    UV-Optical Disk Reverberation Lags despite a Faint X-Ray Corona in the Active Galactic Nucleus Mrk 335. , keywords =. doi:10.3847/1538-4357/acbcd3 , archivePrefix =. 2302.07342 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/acbcd3

  32. [32]

    AGN STORM 2. VII. A Frequency-resolved Map of the Accretion Disk in Mrk 817: Simultaneous X-Ray Reverberation and UVOIR Disk Reprocessing Time Lags. , keywords =. doi:10.3847/1538-4357/ad6b08 , archivePrefix =. 2409.09115 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad6b08

  33. [33]

    The size of the continuum emission region and its scaling relations with active galactic nucleus luminosity and the broad-line region size

    The Size of the Continuum Emission Region and Its Scaling Relations with Active Galactic Nucleus Luminosity and the Broad-line Region Size. , keywords =. doi:10.3847/1538-4357/adc56e , archivePrefix =. 2502.19184 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/adc56e

  34. [34]

    , keywords =

    Third data release of the Hyper Suprime-Cam Subaru Strategic Program. , keywords =. doi:10.1093/pasj/psab122 , archivePrefix =. 2108.13045 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/pasj/psab122

  35. [35]

    The distribution of AGN accretion rates as a function of stellar mass and redshift

    X-rays across the galaxy population - II. The distribution of AGN accretion rates as a function of stellar mass and redshift. , keywords =. doi:10.1093/mnras/stx2700 , archivePrefix =. 1705.01132 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx2700

  36. [36]

    , keywords =

    What drives the growth of black holes?. , keywords =. doi:10.1016/j.newar.2011.11.003 , archivePrefix =. 1112.1949 , primaryClass =

    Pith/arXiv arXiv doi:10.1016/j.newar.2011.11.003 2011

  37. [37]

    , keywords =

    Abundances of the elements: Meteoritic and solar. , keywords =. doi:10.1016/0016-7037(89)90286-X , adsurl =

    doi:10.1016/0016-7037(89)90286-x

  38. [38]

    , keywords =

    The Lyman Edge Test of the Quasar Emission Mechanism. , keywords =. doi:10.1086/167576 , adsurl =

    work page doi:10.1086/167576

  39. [39]

    TLDR: Time Lag/Delay Reconstructor

    TLDR: time lag/delay reconstructor. , keywords =. doi:10.1093/mnras/stab1394 , archivePrefix =. 2106.08456 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stab1394

  40. [40]

    A multiwavelength-motivated X-ray model for the Circinus Galaxy

    A multiwavelength-motivated X-ray model for the Circinus Galaxy. , keywords =. doi:10.1093/mnras/stac403 , archivePrefix =. 2202.05753 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac403

  41. [41]

    Localizing narrow Fe K$\alpha$ emission within bright AGN

    Localizing narrow Fe K emission within bright AGN. , keywords =. doi:10.1051/0004-6361/202142473 , archivePrefix =. 2204.09469 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202142473

  42. [42]

    Testing the disk-corona interplay in radiatively-efficient broad-line AGN

    Testing the disk-corona interplay in radiatively-efficient broad-line AGN. , keywords =. doi:10.1051/0004-6361/201935874 , archivePrefix =. 1907.10069 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201935874 1907

  43. [43]

    , keywords =

    Investigating a fluctuating-accretion model for the spectral-timing properties of accreting black hole systems. , keywords =. doi:10.1111/j.1365-2966.2006.09989.x , archivePrefix =. astro-ph/0512394 , primaryClass =

    doi:10.1111/j.1365-2966.2006.09989.x 2006

  44. [44]

    The universal power spectrum of Quasars in optical wavelengths: Break timescale scales directly with both black hole mass and accretion rate

    The universal power spectrum of quasars in optical wavelengths. Break timescale scales directly with both black hole mass and the accretion rate. , keywords =. doi:10.1051/0004-6361/202347080 , archivePrefix =. 2306.11099 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202347080

  45. [45]

    , keywords =

    EXOSAT observations of a strong soft X-ray excess in MKN 841. , keywords =. doi:10.1093/mnras/217.1.105 , adsurl =

    doi:10.1093/mnras/217.1.105

  46. [46]

    Astronomical Data Analysis Software and Systems V , year = 1996, editor =

    XSPEC: The First Ten Years. Astronomical Data Analysis Software and Systems V , year = 1996, editor =

    1996

  47. [47]

    , keywords =

    Photoionized gas in hydrostatic equilibrium: the role of gravity. , keywords =. doi:10.1111/j.1365-2966.2010.16270.x , archivePrefix =. 1001.3035 , primaryClass =

    doi:10.1111/j.1365-2966.2010.16270.x 2010

  48. [48]

    Constraining Energy-dependent emissivity profiles of AGN inflows

    Constraining energy-dependent emissivity profiles of AGN inflows. , keywords =. doi:10.1093/mnras/stac1122 , archivePrefix =. 2204.10346 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac1122

  49. [49]

    , keywords =

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/ac7c74

  50. [50]

    , keywords =

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  51. [51]

    , keywords =

    Astropy: A community Python package for astronomy. , keywords =. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201322068

  52. [52]

    Baker, Fergus and Young, Andrew , doi =

  53. [53]

    , keywords =

    Locally Optimally Emitting Clouds and the Origin of Quasar Emission Lines. , keywords =. doi:10.1086/309827 , archivePrefix =. astro-ph/9510080 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/309827

  54. [54]

    Unveiling Energy Pathways in AGN Accretion Flows with the Warm Corona Model for the Soft Excess

    Unveiling energy pathways in AGN accretion flows with the warm corona model for the soft excess. , keywords =. doi:10.1093/mnras/stae944 , archivePrefix =. 2404.03040 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stae944

  55. [55]

    , year = 1972, month = dec, volume =

    Rotating Black Holes: Locally Nonrotating Frames, Energy Extraction, and Scalar Synchrotron Radiation. , year = 1972, month = dec, volume =. doi:10.1086/151796 , adsurl =

    doi:10.1086/151796 1972

  56. [56]

    Active Galactic Nuclei Selected from GALEX Spectroscopy: The Ionizing Source Spectrum at z~1

    Active Galactic Nuclei Selected from GALEX Spectroscopy: The Ionizing Source Spectrum at z -0.5ex 1. , keywords =. doi:10.1088/0004-637X/718/2/1235 , archivePrefix =. 1006.5713 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/718/2/1235

  57. [57]

    , keywords =

    The average absorption properties of broad absorption line quasars at 800 < _ rest < 3000 A , and the underlying physical parameters. , keywords =. doi:10.1093/mnras/stt582 , archivePrefix =. 1304.0986 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stt582

  58. [58]

    Application to the broad-line region in active galactic nuclei

    Radiation pressure confinement - II. Application to the broad-line region in active galactic nuclei. , keywords =. doi:10.1093/mnras/stt2230 , archivePrefix =. 1309.7953 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stt2230

  59. [59]

    Radiation pressure confinement - IV. Application to broad absorption line outflows

    Radiation pressure confinement - IV. Application to broad absorption line outflows. , keywords =. doi:10.1093/mnras/stu1732 , archivePrefix =. 1408.4941 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1732

  60. [60]

    , keywords =

    Dust inflated accretion disc as the origin of the broad line region in active galactic nuclei. , keywords =. doi:10.1093/mnras/stx2850 , archivePrefix =. 1711.00025 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx2850

  61. [61]

    Testing disc reprocessing models for AGN optical variability by comparison of X-ray and optical power spectra of NGC 4395

    Testing disc reprocessing models for AGN optical variability by comparison of X-ray and optical power spectra of NGC 4395. , keywords =. doi:10.1093/mnras/staf014 , archivePrefix =. 2501.02664 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staf014

  62. [62]

    Compton heated winds and coronae above accretion disks. I. Dynamics. , keywords =. doi:10.1086/161178 , adsurl =

    doi:10.1086/161178

  63. [63]

    Compton heated winds and coronae above accretion disks. II. Radiativetransfer and observable consequences. , keywords =. doi:10.1086/161179 , adsurl =

    doi:10.1086/161179

  64. [64]

    Density Profiles in Seyfert Outflows

    Density Profiles in Seyfert Outflows. , keywords =. doi:10.1088/0004-637X/703/2/1346 , archivePrefix =. 0908.0539 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/703/2/1346

  65. [65]

    High Energy Processes in Accreting Black Holes , year = 1999, editor =

    Accretion Disk Models. High Energy Processes in Accreting Black Holes , year = 1999, editor =

    1999

  66. [66]

    , keywords =

    Common origin for black holes in both high mass X-ray binaries and gravitational-wave sources. , keywords =. doi:10.1051/0004-6361/202450229 , archivePrefix =. 2111.09401 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202450229

  67. [67]

    , keywords =

    The Lick AGN Monitoring Project: Broad-line Region Radii and Black Hole Masses from Reverberation Mapping of H. , keywords =. doi:10.1088/0004-637X/705/1/199 , archivePrefix =. 0908.0003 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/705/1/199

  68. [68]

    , keywords =

    The Low-luminosity End of the Radius-Luminosity Relationship for Active Galactic Nuclei. , keywords =. doi:10.1088/0004-637X/767/2/149 , archivePrefix =. 1303.1742 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/767/2/149

  69. [69]

    , keywords =

    The AGN Black Hole Mass Database. , keywords =. doi:10.1086/679601 , archivePrefix =. 1411.2596 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/679601

  70. [70]

    Modeling the X-ray - UV Correlations in NGC 7469

    Modeling the X-Ray-Ultraviolet Correlations in NGC 7469. , keywords =. doi:10.1086/308880 , archivePrefix =. astro-ph/0001239 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308880

  71. [71]

    The X-ray Universe 2017 , year = 2017, editor =

    A Suzaku, NuSTAR and XMMNewton view on variable absorption and relativistic reflection in NGC 4151. The X-ray Universe 2017 , year = 2017, editor =

    2017

  72. [72]

    Physics of the Dark Universe , keywords =

    lenstronomy: Multi-purpose gravitational lens modelling software package. Physics of the Dark Universe , keywords =. doi:10.1016/j.dark.2018.11.002 , archivePrefix =. 1803.09746 , primaryClass =

    Pith/arXiv arXiv doi:10.1016/j.dark.2018.11.002 2018

  73. [73]

    The WISSH quasars project. I. Powerful ionised outflows in hyper-luminous quasars. , keywords =. doi:10.1051/0004-6361/201629301 , archivePrefix =. 1612.03728 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201629301

  74. [74]

    Widespread QSO-driven outflows in the early Universe

    Widespread QSO-driven outflows in the early Universe. , keywords =. doi:10.1051/0004-6361/201833557 , archivePrefix =. 1806.00786 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833557

  75. [75]

    The fraction and kinematics of broad absorption line quasars across cosmic time

    The Fraction and Kinematics of Broad Absorption Line Quasars across Cosmic Time. , keywords =. doi:10.3847/1538-4357/accea4 , archivePrefix =. 2301.09731 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/accea4

  76. [76]

    , keywords =

    Reverberation mapping of the emission line regions of Seyfert galaxies and quasars. , keywords =. doi:10.1086/159843 , adsurl =

    doi:10.1086/159843

  77. [77]

    , keywords =

    Hydromagnetic flows from accretion disks and the production of radio jets. , keywords =. doi:10.1093/mnras/199.4.883 , adsurl =

    doi:10.1093/mnras/199.4.883

  78. [78]

    , keywords =

    On the fate of gas accreting at a low rate on to a black hole. , keywords =. doi:10.1046/j.1365-8711.1999.02358.x , archivePrefix =. astro-ph/9809083 , primaryClass =

    doi:10.1046/j.1365-8711.1999.02358.x 1999

  79. [79]

    , keywords =

    XRISM analysis of the complex Fe K line in Centaurus A. , keywords =. doi:10.1093/pasj/psaf084 , archivePrefix =. 2507.02195 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/pasj/psaf084

  80. [80]

    , keywords =

    Long-term optical and X-ray variability of the Seyfert galaxy Markarian 79. , keywords =. doi:10.1111/j.1365-2966.2008.14302.x , archivePrefix =. 0812.0810 , primaryClass =

    doi:10.1111/j.1365-2966.2008.14302.x 2008

Showing first 80 references.