pith. sign in

arxiv: 2606.21426 · v1 · pith:3Q7GWPUInew · submitted 2026-06-19 · 🌌 astro-ph.HE

The Fundamental Planes of Black Hole Activity for High-Synchrotron-Peaked BL Lacertae Objects

Qing-Chen. Long , Ai-Jun. Dong , Qi-Jun.Zhi This is my paper

Pith reviewed 2026-06-26 13:40 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords high-synchrotron-peaked BL Lacsradio-X-ray correlationfundamental planesynchrotron coolingblazar jetsblack hole activityDoppler beaming
0
0 comments X

The pith

Synchrotron cooling of jet electrons produces the shallow radio-X-ray correlation and fundamental plane in high-synchrotron-peaked BL Lacs.

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

The paper examines the radio-X-ray correlation and fundamental plane of black hole activity using a sample of 69 high-synchrotron-peaked BL Lacertae objects. After applying Doppler beaming corrections to obtain intrinsic luminosities, it recovers a correlation L_R,int proportional to L_X,int to the power 0.68 together with the plane relation log L_R,int = (0.57 plus or minus 0.06) log L_X,int plus (0.33 plus or minus 0.11) log M_BH plus (12.65 plus or minus 2.00). Application of the synchrotron cooling model shows these shallow scalings arise because X-ray emission comes from rapidly cooling high-energy electrons accelerated at shocks, rather than other processes. This supplies observational support for the predicted scaling L_R proportional to L_X_Syn-c to the power 0.6-0.7 and aligns with X-ray polarization data favoring a synchrotron origin.

Core claim

After correcting for Doppler beaming effects, the intrinsic radio-X-ray correlation for HBLs is L_R,int proportional to L_X,int to the power 0.68 and the fundamental plane is log L_R,int equals (0.57 plus or minus 0.06) log L_X,int plus (0.33 plus or minus 0.11) log M_BH plus (12.65 plus or minus 2.00). These relations are explained by the synchrotron cooling model, indicating that the X-ray emissions of HBLs are produced by rapidly cooling, high-energy electrons accelerated at a shock in the jet.

What carries the argument

The synchrotron cooling (Syn-c) model for high-energy electrons in jets, which produces the observed shallow radio-X-ray scaling when cooling occurs rapidly after shock acceleration.

If this is right

  • X-ray emission in these HBLs originates from the synchrotron process of rapidly cooling high-energy electrons at shocks.
  • The shallow radio-X-ray correlations and fundamental plane are intrinsic properties of the sources.
  • The results are consistent with recent X-ray polarization observations that support a synchrotron origin for the X-rays.
  • The scaling L_R proportional to L_X_Syn-c to the power 0.6-0.7 holds as an observational signature of this emission mechanism.

Where Pith is reading between the lines

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

  • If the Syn-c picture is correct, similar shallow correlations could appear in other jet-dominated sources where synchrotron cooling sets the X-ray output.
  • Long-term multi-wavelength variability campaigns could check whether flux changes follow the timing expected for shock-accelerated cooling electrons.
  • Improved jet orientation indicators might allow tighter tests of whether the recovered slope remains stable near 0.68.

Load-bearing premise

Doppler beaming corrections recover true intrinsic luminosities without leftover orientation biases, and synchrotron cooling dominates X-ray production with negligible contribution from other channels.

What would settle it

A measured intrinsic radio-X-ray slope after refined beaming estimates that lies well outside the 0.6-0.7 range, or X-ray polarization fractions and angles that contradict expectations for synchrotron emission from cooling shock-accelerated electrons.

Figures

Figures reproduced from arXiv: 2606.21426 by Ai-Jun. Dong, Qi-Jun.Zhi, Qing-Chen. Long.

Figure 1
Figure 1. Figure 1: Distributions of the physical parameters for our HBLs and a comparison of some properties with a larger HBL sample from Wu et al. (2007), Fan et al. (2016), and Chang et al. (2019). The blue boxes are the distribution of observational properties for our HBLs. (a) Redshift: 𝑧, the red box is the distribution of redshift of 3HSP sample from Chang et al. (2019). (b) Logarithm of the synchrotron peak frequency… view at source ↗
Figure 2
Figure 2. Figure 2: The Doppler factor (𝛿𝜈) as the function of frequency (𝜈), which is based on the hypothesis of decelerating jet for HBLs (Georganopoulos & Kazanas 2003; Ghisellini et al. 2005). The blue circles are the 5 GHz radio Doppler factors of our HBLs; the black circles are the typical TeV band (1027 Hz) Doppler factors for HBLs, which are taken from Cerruti et al. (2015). The blue solid line is the best fit (Eq 3);… view at source ↗
Figure 3
Figure 3. Figure 3: The observational and intrinsic radio–X-ray correlation for HBLs. The ’int’ and ’obs’ indicate the observational data and the intrinsic data, respectively. The solid circles represent intrinsic data points of HBLs. The gray dashed line and the blue solid line are the best-fit of observational and intrinsic radio–X-ray correlation for HBLs. The the red shaded region is the 95%(2𝜎) confidence intervals on th… view at source ↗
Figure 4
Figure 4. Figure 4: The intrinsic FP for our HBLs. The notations are the same as that of [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: The observational and intrinsic correlations between radio and X-ray flux for our HBLs. The left panel is log 𝐹R,obs − log 𝐹X,obs relation (the stars are the observational data points), The right panel is log 𝐹R,int − log 𝐹X,int relation. The notations are the same as that of [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: The black solid line, blue solid line and red solid line are the 𝜉RX − 𝑝 functions under the fixed parameters of (𝛼R = 0, 𝛼X = 1.29), (𝛼R = −0.08, 𝛼X = 1.29) and (𝛼R = −0.16, 𝛼X = 1.29), respectively. The orange dashed line and the cyan dashed line are the 𝜉RX − 𝑝 functions under the fixed parameters of (𝛼R = −0.08, 𝛼X = 1.15) and (𝛼R = −0.08, 𝛼X = 1.35), respectively. The gray dotted line is the 𝜉RX − 𝑝 f… view at source ↗
read the original abstract

The radio--X-ray correlation and Fundamental Plane (FP) of black hole activity can serve as a diagnostic tool for the origin of X-ray emissions. There was a scaling relation between radio and X-ray emissions for High-synchrotron-peaked BL Lacertae objects (HBLs), i.e., $L_{\rm{R}}\propto L_{\rm{X}}^{0.64}$, which can be explained by ADAF-dominated mode or synchrotron cooling (Syn-c). However, many results of studying blazar physics show that the X-ray emissions of HBLs are mainly produced by the synchrotron process of jets. Therefore, Syn-c appears to provide a plausible explanation for this relation. To further clarify the origin of X-ray emissions of HBLs, we constructed a sample containing 69 HBLs in this paper to re-investigate their radio--X-ray correlation and FP. Considering the Doppler beaming effect, we find that the intrinsic radio--X-ray correlation and FP of HBLs are $L_{\rm R,int}\propto L_{\rm X,int}^{0.68}$ and $\log L_{\rm R,int}=(0.57\pm0.06)\log L_{\rm X,int}+(0.33\pm0.11)\log M_{\rm BH}+(12.65\pm2.00)$, respectively. Our results agree with the scaling relation mention above, which suggests these scaling relations are not artificial. By employing the theoretical model of Syn-c, we find that these shallow radio--X-ray correlations and FP are caused by Syn-c, which implies that the X-ray emissions of HBLs may be produced by rapidly cooling, high-energy electrons accelerated at a shock. This is consistent with results of the recent X-ray polarization observations of HBLs. Our results provide the observational evidence of $L_{\rm R}\propto L_{\rm X_{\text{Syn-c}}}^{0.6\sim0.7}$.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 1 minor

Summary. The manuscript analyzes a sample of 69 high-synchrotron-peaked BL Lacertae objects (HBLs) to re-examine their radio-X-ray correlation and fundamental plane (FP) of black hole activity. After applying Doppler beaming corrections, it reports intrinsic relations L_{R,int} ∝ L_{X,int}^{0.68} and log L_{R,int} = (0.57±0.06) log L_{X,int} + (0.33±0.11) log M_{BH} + (12.65±2.00), attributes the shallow slope to the synchrotron cooling (Syn-c) model, and concludes that X-ray emission originates from rapidly cooling high-energy electrons accelerated at shocks, providing observational evidence for L_R ∝ L_{X_Syn-c}^{0.6~0.7}.

Significance. If the Doppler corrections are shown to be free of residual biases and the Syn-c model comparison is performed with an independent derivation of the exponent plus quantitative metrics, the result would supply direct observational support for jet-based synchrotron origins of X-rays in HBLs and for the Syn-c mechanism explaining shallow correlations, consistent with recent X-ray polarization data.

major comments (3)
  1. [Abstract] Abstract: the central claim that the observed intrinsic slope of 0.68 matches the Syn-c expectation of 0.6-0.7 and is caused by Syn-c requires an independent derivation of the model exponent and a quantitative test (e.g., predicted vs. observed slope with uncertainties); none is supplied, creating a circularity risk for the attribution of X-ray origin.
  2. [Abstract] Abstract: the Doppler beaming correction is load-bearing for recovering unbiased intrinsic luminosities and the reported slope of 0.68, yet no details are given on how Doppler factors were estimated for the 69 HBLs, what assumptions were used, or any validation against orientation-dependent or luminosity-correlated residuals.
  3. [Abstract] Abstract: sample selection criteria, completeness, error propagation on the fitted exponents and FP coefficients, and any statistical comparison (e.g., χ² or posterior odds) to the Syn-c model predictions are absent, preventing assessment of whether the relations are robust or driven by selection effects.
minor comments (1)
  1. [Abstract] The final sentence uses the non-standard subscript notation L_{X_Syn-c}; a brief definition or reference to the Syn-c luminosity definition would improve clarity.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive comments, which highlight areas where the manuscript can be strengthened. We agree that additional details on the Syn-c derivation, Doppler methodology, and sample statistics will improve clarity and robustness. We address each major comment below and will incorporate the suggested revisions.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that the observed intrinsic slope of 0.68 matches the Syn-c expectation of 0.6-0.7 and is caused by Syn-c requires an independent derivation of the model exponent and a quantitative test (e.g., predicted vs. observed slope with uncertainties); none is supplied, creating a circularity risk for the attribution of X-ray origin.

    Authors: We acknowledge the risk of circularity if the Syn-c attribution rests solely on matching the observed slope without explicit derivation. In the revised manuscript we will add a dedicated subsection that independently derives the expected exponent (0.6-0.7) from the synchrotron cooling framework, starting from the electron energy distribution and cooling timescale. We will also include a quantitative comparison (chi-squared statistic and uncertainty overlap) between the fitted slope (0.68 ± 0.06) and the model prediction. revision: yes

  2. Referee: [Abstract] Abstract: the Doppler beaming correction is load-bearing for recovering unbiased intrinsic luminosities and the reported slope of 0.68, yet no details are given on how Doppler factors were estimated for the 69 HBLs, what assumptions were used, or any validation against orientation-dependent or luminosity-correlated residuals.

    Authors: The Doppler factors were obtained from the standard variability-based method combined with apparent jet speeds where available. To address the concern, the revised version will expand the methods section with the explicit formulas, the adopted bulk Lorentz factor and viewing-angle distributions, and any checks performed for residual correlations with luminosity or orientation. If additional validation tests are needed, we will add them. revision: yes

  3. Referee: [Abstract] Abstract: sample selection criteria, completeness, error propagation on the fitted exponents and FP coefficients, and any statistical comparison (e.g., χ² or posterior odds) to the Syn-c model predictions are absent, preventing assessment of whether the relations are robust or driven by selection effects.

    Authors: We agree these elements are necessary for assessing robustness. The revised manuscript will include an explicit description of the selection criteria (synchrotron peak frequency threshold and multi-wavelength data availability), a discussion of sample completeness relative to existing HBL catalogs, the error-propagation procedure used for the regression coefficients (Monte Carlo resampling), and a statistical comparison (chi-squared and posterior odds) of the observed relations against the Syn-c predictions. revision: yes

Circularity Check

0 steps flagged

No circularity: observed slope measured independently and compared to external theoretical model

full rationale

The paper measures intrinsic luminosities for 69 HBLs after applying Doppler beaming corrections, then fits the radio-X-ray correlation to obtain L_R,int ∝ L_X,int^0.68 and the FP relation. This observed slope is noted to agree with a prior scaling relation (0.64) and to lie within the Syn-c model's stated range (0.6-0.7). The text presents the Syn-c model as a theoretical explanation for the shallow slope without any indication that the model's exponent was derived from, fitted to, or defined using the current sample's data. No equations reduce the claimed result to its inputs by construction, no self-citations are shown as load-bearing for the exponent, and the central measurement step remains independent of the model attribution.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

Central claim rests on the assumption that Doppler-corrected luminosities are free of orientation bias and that the Syn-c model supplies an independent prediction for the exponent; both are domain assumptions rather than derived quantities.

free parameters (2)
  • radio-X-ray exponent = 0.68
    Fitted slope 0.68 obtained from the 69-object sample
  • FP coefficients = 0.57, 0.33, 12.65
    Three fitted values (0.57, 0.33, 12.65) for the plane equation
axioms (1)
  • domain assumption Doppler beaming correction yields unbiased intrinsic luminosities
    Invoked to convert observed to intrinsic L_R and L_X before fitting

pith-pipeline@v0.9.1-grok · 5905 in / 1364 out tokens · 30575 ms · 2026-06-26T13:40:51.453664+00:00 · methodology

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

131 extracted references · 128 canonical work pages · 73 internal anchors

  1. [1]

    Active Galactic Nuclei: what's in a name?

    Active galactic nuclei: what's in a name?. , keywords =. doi:10.1007/s00159-017-0102-9 , archivePrefix =. 1707.07134 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s00159-017-0102-9

  2. [2]

    Optical and Radio Properties of Extragalactic Sources Observed by the FIRST and SDSS Surveys

    Optical and Radio Properties of Extragalactic Sources Observed by the FIRST Survey and the Sloan Digital Sky Survey. , keywords =. doi:10.1086/344069 , archivePrefix =. astro-ph/0202408 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/344069

  3. [3]

    Radio Loud and Radio Quiet Quasars

    Radio-loud and Radio-quiet QSOs. , keywords =. doi:10.3847/0004-637X/831/2/168 , archivePrefix =. 1608.04586 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/831/2/168

  4. [4]

    , keywords =

    Electromagnetic extraction of energy from Kerr black holes. , keywords =. 1977. doi:10.1093/mnras/179.3.433 , adsurl =

    work page doi:10.1093/mnras/179.3.433 1977

  5. [5]

    , keywords =

    Hydromagnetic flows from accretion disks and the production of radio jets. , keywords =. 1982. doi:10.1093/mnras/199.4.883 , adsurl =

    work page doi:10.1093/mnras/199.4.883 1982

  6. [6]

    , keywords =

    Relativistic Jets from Active Galactic Nuclei. , keywords =. 2019. doi:10.1146/annurev-astro-081817-051948 , archivePrefix =. 1812.06025 , primaryClass =

    work page doi:10.1146/annurev-astro-081817-051948 2019

  7. [7]

    Exploring X-ray and radio emission of type 1 AGN up to z ~ 2.3

    Exploring X-ray and radio emission of type 1 AGN up to z -0.5ex 2.3. , keywords =. doi:10.1051/0004-6361/201117464 , archivePrefix =. 1208.1716 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201117464

  8. [8]

    , keywords =

    Radio and X-ray bright AGN: the ROSAT - FIRST correlation. , keywords =

  9. [9]

    The FIRST Bright Quasar Survey. II. 60 Nights and 1200 Spectra Later. , keywords =. doi:10.1086/313300 , archivePrefix =. astro-ph/9912215 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/313300

  10. [10]

    Tools for computing the AGN feedback: radio-loudness distribution and the kinetic luminosity function

    Tools for Computing the AGN Feedback: Radio-loudness Distribution and the Kinetic Luminosity Function. , keywords =. doi:10.1088/0004-637X/718/1/368 , archivePrefix =. 1006.1247 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/718/1/368

  11. [11]

    On the AGN radio luminosity distribution and the black hole fundamental plane

    On the radio luminosity distribution of active galactic nuclei and the black hole fundamental plane. , keywords =. doi:10.1093/mnras/sts456 , archivePrefix =. 1211.2688 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sts456

  12. [12]

    , keywords =

    Exploring the radio loudness of SDSS quasars with spectral stacking. , keywords =. doi:10.1093/mnras/stae233 , archivePrefix =. 2401.08774 , primaryClass =

    work page doi:10.1093/mnras/stae233

  13. [13]

    Observational appearance

    Black holes in binary systems. Observational appearance. , year = 1973, month = jan, volume =

    1973

  14. [14]

    From the Blazar Sequence to the Blazar Envelope: Revisiting the Relativistic Jet Dichotomy in Radio-loud AGN

    From the Blazar Sequence to the Blazar Envelope: Revisiting the Relativistic Jet Dichotomy in Radio-loud Active Galactic Nuclei. , keywords =. doi:10.1088/0004-637X/740/2/98 , archivePrefix =. 1107.5105 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/740/2/98

  15. [15]

    , keywords =

    The relativistic jet dichotomy and the end of the blazar sequence. , keywords =. doi:10.1093/mnras/stab1182 , archivePrefix =. 2007.12661 , primaryClass =

    work page doi:10.1093/mnras/stab1182 2007

  16. [16]

    On the origin of X-ray emission in some FR Is: ADAF or jet?

    On the Origin of X-Ray Emission in Some FR I Galaxies: ADAF or Jet?. , keywords =. doi:10.1086/521212 , archivePrefix =. 0706.4124 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/521212

  17. [17]

    , keywords =

    The origin of X-ray emission in 3CRR sources: Hints from mid-infrared Spitzer observations. , keywords =. doi:10.1051/0004-6361/202141301 , archivePrefix =. 2107.13142 , primaryClass =

    work page doi:10.1051/0004-6361/202141301

  18. [18]

    The X-ray to optical-UV luminosity ratio of X-ray selected Type 1 AGN in XMM-COSMOS

    The X-ray to optical-UV luminosity ratio of X-ray selected type 1 AGN in XMM-COSMOS. , keywords =. doi:10.1051/0004-6361/200913298 , archivePrefix =. 0912.4166 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200913298

  19. [19]

    , keywords =

    The L _ X -L _ uv -L _ radio relation and corona-disc-jet connection in optically selected radio-loud quasars. , keywords =. doi:10.1093/mnras/staa1411 , archivePrefix =. 2006.13226 , primaryClass =

    work page doi:10.1093/mnras/staa1411 2006

  20. [20]

    Nature Astronomy 2:652–655

    A Fundamental Plane of black hole activity. , keywords =. doi:10.1046/j.1365-2966.2003.07017.x , archivePrefix =. astro-ph/0305261 , primaryClass =

    work page doi:10.1046/j.1365-2966.2003.07017.x 2003

  21. [21]

    A Scheme to Unify Low-Power Accreting Black Holes - Jet-Dominated Accretion Flows and the Radio/X-Ray Correlation

    A scheme to unify low-power accreting black holes. Jet-dominated accretion flows and the radio/X-ray correlation. , keywords =. doi:10.1051/0004-6361:20031683 , archivePrefix =. astro-ph/0305335 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20031683

  22. [22]

    Refining the fundamental plane of accreting black holes

    Refining the fundamental plane of accreting black holes. , keywords =. doi:10.1051/0004-6361:20054144 , archivePrefix =. astro-ph/0603117 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20054144

  23. [23]

    Radio--X-ray Correlation and the "Quiescent State" of Black Hole Sources

    Radio-X-Ray Correlation and the ``Quiescent State'' of Black Hole Sources. , keywords =. doi:10.1086/431453 , archivePrefix =. astro-ph/0411770 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/431453

  24. [24]

    Revisiting the "Fundamental Plane" of Black Hole Activity at Extremely Low Luminosities

    Revisiting the ``Fundamental Plane'' of Black Hole Activity at Extremely Low Luminosities. , keywords =. doi:10.1088/0004-637X/703/1/1034 , archivePrefix =. 0902.3704 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/703/1/1034

  25. [25]

    The black hole fundamental plane from a uniform sample of radio and X-ray emitting broad line AGNs

    The Black Hole Fundamental Plane from a Uniform Sample of Radio and X-Ray-emitting Broad-Line AGNs. , keywords =. doi:10.1086/504401 , archivePrefix =. astro-ph/0603514 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/504401

  26. [26]

    The black hole fundamental plane: revisit with a larger sample of radio and X-ray emitting broad-line AGNs

    The Black Hole Fundamental Plane: Revisited with a Larger Sample of Radio and X-Ray-Emitting Broad-Line AGNs. , keywords =. doi:10.1086/592314 , archivePrefix =. 0808.0541 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/592314

  27. [27]

    The Fundamental Plane of Accretion Onto Black Holes with Dynamical Masses

    The Fundamental Plane of Accretion onto Black Holes with Dynamical Masses. , keywords =. doi:10.1088/0004-637X/706/1/404 , archivePrefix =. 0906.3285 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/706/1/404

  28. [28]

    , keywords =

    The active nuclei of z < 1.0 3CRR radio sources. , keywords =. doi:10.1111/j.1365-2966.2009.14887.x , archivePrefix =. 0904.1323 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14887.x 2009

  29. [29]

    , keywords =

    Using the Fundamental Plane of black hole activity to distinguish X-ray processes from weakly accreting black holes. MNRAS , keywords =. doi:10.1111/j.1365-2966.2011.19689.x , archivePrefix =. 1105.3211 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19689.x 2011

  30. [30]

    , keywords =

    The Radio/X-Ray Correlation and Black Hole Fundamental Plane for Young Radio Sources: Implications for X-Ray Origin and Accretion Mode. , keywords =. doi:10.3847/0004-637X/818/2/185 , adsurl =

    work page doi:10.3847/0004-637x/818/2/185

  31. [31]

    A new fundamental plane for radiatively efficient black-hole sources

    A New Fundamental Plane for Radiatively Efficient Black-hole Sources. , keywords =. doi:10.1088/2041-8205/787/2/L20 , archivePrefix =. 1404.5317 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/787/2/l20 2041

  32. [32]

    Revisit the fundamental plane of black-hole activity from sub-Eddington to quiescent state

    Revisit the Fundamental Plane of black hole activity from sub-Eddington to quiescent state. , keywords =. doi:10.1093/mnras/stv1801 , archivePrefix =. 1509.05088 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1801

  33. [33]

    Fundamental Plane of Black Hole Activity in Quiescent Regime

    Fundamental Plane of Black Hole Activity in the Quiescent Regime. , keywords =. doi:10.3847/1538-4357/aa5b90 , archivePrefix =. 1701.06143 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa5b90

  34. [34]

    Black Hole Fundamental Plane in Low-Excitation Radio Galaxies

    The black hole fundamental plane in low-excitation radio galaxies. , keywords =. doi:10.1093/mnrasl/sly154 , archivePrefix =. 1808.07188 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/sly154

  35. [35]

    , keywords =

    The X-ray emission in young radio active galactic nuclei. , keywords =. doi:10.1093/mnras/staa1559 , archivePrefix =. 2006.01079 , primaryClass =

    work page doi:10.1093/mnras/staa1559 2006

  36. [36]

    , keywords =

    The Fundamental Planes of black hole activity for radio-loud and radio-quiet quasars. , keywords =. doi:10.1093/mnras/stac1153 , archivePrefix =. 2201.04666 , primaryClass =

    work page doi:10.1093/mnras/stac1153

  37. [37]

    , keywords =

    The fundamental plane of blazars based on the black hole spin-mass energy. , keywords =. doi:10.1093/mnras/stae765 , archivePrefix =. 2403.09088 , primaryClass =

    work page doi:10.1093/mnras/stae765

  38. [38]

    , keywords =

    The fundamental plane of black hole activity for low-luminosity radio active galactic nuclei across 0 < z < 4. , keywords =. doi:10.1051/0004-6361/202449732 , archivePrefix =. 2402.17991 , primaryClass =

    work page doi:10.1051/0004-6361/202449732

  39. [39]

    , keywords =

    Revisiting the Fundamental Planes of Black Hole Activity for Strong Jet Sources. , keywords =. doi:10.3847/1538-4357/adaaee , archivePrefix =. 2501.11381 , primaryClass =

    work page doi:10.3847/1538-4357/adaaee

  40. [40]

    The Accretion Rates and Spectral Energy Distributions of BL Lacertae Objects

    The Accretion Rates and Spectral Energy Distributions of BL Lacertae Objects. , keywords =. doi:10.1086/342875 , archivePrefix =. astro-ph/0207305 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/342875

  41. [41]

    K. I. Kellermann and R. Sramek and M. Schmidt and D. B. Shaffer and R. Green , title = ". , keywords =. doi:10.1086/115207 , adsurl =

    work page doi:10.1086/115207

  42. [42]

    , keywords =

    Is there really a dichotomy in active galactic nucleus jet power?. , keywords =. doi:10.1111/j.1365-2966.2011.19060.x , archivePrefix =. 1105.3769 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19060.x 2011

  43. [43]

    A Sample of Low-Redshift BL Lacertae Objects. II. EVN and MERLIN Data and Multiwavelength Analysis. , keywords =. doi:10.1086/504971 , archivePrefix =. astro-ph/0604224 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/504971

  44. [44]

    Unified Schemes for Radio-Loud Active Galactic Nuclei

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/133630

  45. [45]

    , keywords =

    Are high polarization quasars and BL Lacertae objects really different? A study of the optical spectral properties. , keywords =

  46. [46]

    The Spectral Energy Distributions of Fermi Blazars

    The Spectral Energy Distributions of Fermi Blazars. , keywords =. doi:10.3847/0067-0049/226/2/20 , archivePrefix =. 1608.03958 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0067-0049/226/2/20

  47. [47]

    , keywords =

    The Spectral Energy Distributions for 4FGL Blazars. , keywords =. doi:10.3847/1538-4365/ac7deb , adsurl =

    work page doi:10.3847/1538-4365/ac7deb

  48. [48]

    , keywords =

    The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope: Data Release 3. , keywords =. doi:10.3847/1538-4365/ac9523 , archivePrefix =. 2209.12070 , primaryClass =

    work page doi:10.3847/1538-4365/ac9523

  49. [49]

    Basic properties of Fermi blazars and the "blazar sequence"

    Basic properties of Fermi blazars and the `blazar sequence'. , keywords =. doi:10.1093/mnras/stv812 , archivePrefix =. 1504.02706 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv812

  50. [50]

    Why are some BL Lacs detected by \fermi, but others not ?

    Why are some BL Lacertaes detected by Fermi, but others not?. , keywords =. doi:10.1051/0004-6361/201220851 , archivePrefix =. 1401.0652 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201220851

  51. [51]

    VLBI observations of seven BL Lac objects from RGB sample

    VLBI observations of seven BL Lacertae objects from RGB sample. , keywords =. doi:10.1051/0004-6361:20066754 , archivePrefix =. 0706.0191 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20066754

  52. [52]

    , keywords =

    Unification of BL Lac objects and FR I and FR II(G) radio galaxies, and Doppler factor estimation for BL Lac objects. , keywords =. doi:10.1093/pasj/psab039 , archivePrefix =. 2111.09023 , primaryClass =

    work page doi:10.1093/pasj/psab039

  53. [53]

    A Sample of Low-Redshift BL Lacertae Objects. I. The Radio Data. , keywords =. doi:10.1086/423231 , archivePrefix =. astro-ph/0406255 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/423231

  54. [54]

    Hard X-ray properties of blazars

    Hard X-ray properties of blazars. , keywords =. doi:10.1051/0004-6361:20010675 , archivePrefix =. astro-ph/0105203 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20010675

  55. [55]

    , keywords =

    BL Lac Objects and Acceleration Model. , keywords =. doi:10.1007/BF00658217 , adsurl =

    work page doi:10.1007/bf00658217

  56. [56]

    , keywords =

    A Survey for High Optical Polarization in Quasars with Core-dominant Radio Structure: Is There a Beamed Optical Continuum?. , keywords =. doi:10.1086/171869 , adsurl =

    work page doi:10.1086/171869

  57. [57]

    INTEGRAL observations of the blazar Mrk 421 in outburst (Results of a multi-wavelength campaign)

    INTEGRAL observations of the blazar Mrk 421 in outburst. Results of a multi-wavelength campaign. , keywords =. doi:10.1051/0004-6361:20079199 , archivePrefix =. 0805.2577 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20079199

  58. [58]

    , keywords =

    Blazar spectral variability as explained by a twisted inhomogeneous jet. , keywords =. doi:10.1038/nature24623 , archivePrefix =. 1712.02098 , primaryClass =

    work page doi:10.1038/nature24623

  59. [59]

    , keywords =

    Jet power extracted from ADAFs and the application to Fermi BL Lacertae objects. , keywords =. doi:10.1093/mnras/stad2623 , archivePrefix =. 2308.15707 , primaryClass =

    work page doi:10.1093/mnras/stad2623

  60. [60]

    , keywords =

    The Energy Budget in the Jet of High-frequency Peaked BL Lacertae Objects. , keywords =. doi:10.3847/1538-4357/ad3ba9 , archivePrefix =. 2406.01046 , primaryClass =

    work page doi:10.3847/1538-4357/ad3ba9

  61. [61]

    , keywords =

    The transition between BL Lac objects and flat spectrum radio quasars. , keywords =. doi:10.1111/j.1365-2966.2011.18578.x , archivePrefix =. 1012.0308 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18578.x 2011

  62. [62]

    The jet-disc connection in AGN

    The jet-disc connection in AGN. , keywords =. doi:10.1093/mnras/stu1759 , archivePrefix =. 1405.4865 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu1759

  63. [63]

    C., Bohringer, H., et al

    A unifying view of the spectral energy distributions of blazars. , keywords =. doi:10.1046/j.1365-8711.1998.01828.x , archivePrefix =. astro-ph/9804103 , primaryClass =

    work page doi:10.1046/j.1365-8711.1998.01828.x 1998

  64. [64]

    , keywords =

    The Central Engines of Fermi Blazars. , keywords =. doi:10.3847/1538-4365/abe135 , archivePrefix =. 2101.10849 , primaryClass =

    work page doi:10.3847/1538-4365/abe135

  65. [65]

    L., Nichol, R., Bamford, S., et al

    An X-ray view of the INTEGRAL/IBIS blazars. , keywords =. doi:10.1111/j.1365-2966.2010.17725.x , archivePrefix =. 1010.5713 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17725.x 2010

  66. [66]

    BAT AGN Spectroscopic Survey. V. X-Ray Properties of the Swift/BAT 70-month AGN Catalog. , keywords =. doi:10.3847/1538-4365/aa96ad , archivePrefix =. 1709.03989 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/aa96ad

  67. [67]

    Discovery of VHE gamma-rays from the high-frequency-peaked BL Lac object RGB J0152+017

    Discovery of VHE -rays from the high-frequency-peaked BL Lacertae object RGB J0152+017. , keywords =. doi:10.1051/0004-6361:200809603 , archivePrefix =. 0802.4021 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:200809603

  68. [68]

    Six years of BeppoSAX observations of blazars: a spectral catalog

    Six years of BeppoSAX observations of blazars: A spectral catalog. , keywords =. doi:10.1051/0004-6361:20034555 , archivePrefix =. physics/0412114 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20034555

  69. [69]

    1ES 0229+200: An extreme blazar with a very high minimum Lorentz factor

    1ES 0229+200: an extreme blazar with a very high minimum Lorentz factor. , keywords =. doi:10.1051/0004-6361/201117215 , archivePrefix =. 1109.3628 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201117215

  70. [70]

    High Resolution Spectroscopy of X-ray Quasars: Searching for the X-ray Absorption from the Warm-Hot Intergalactic Medium

    High-Resolution Spectroscopy of X-Ray Quasars: Searching for the X-Ray Absorption from the Warm-Hot Intergalactic Medium. , keywords =. doi:10.1086/431749 , archivePrefix =. astro-ph/0506127 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/431749

  71. [71]

    , keywords =

    TeV BL Lac objects at the dawn of the Fermi era. , keywords =. doi:10.1111/j.1365-2966.2009.15784.x , archivePrefix =. 0909.0651 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15784.x 2009

  72. [72]

    Discovery of VHE gamma-rays from the BL Lac object PKS 0548-322

    Discovery of VHE -rays from the BL Lacertae object PKS 0548-322. , keywords =. doi:10.1051/0004-6361/200912363 , archivePrefix =. 1006.5289 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200912363

  73. [73]

    Multiwavelength Observations of the Previously Unidentified Blazar RX J0648.7+1516

    Multiwavelength Observations of the Previously Unidentified Blazar RX J0648.7+1516. , keywords =. doi:10.1088/0004-637X/742/2/127 , archivePrefix =. 1110.5949 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/742/2/127

  74. [74]

    , keywords =

    Long-term multi-wavelength study of 1ES 0647+250. , keywords =. doi:10.1051/0004-6361/202244477 , archivePrefix =. 2211.13268 , primaryClass =

    work page doi:10.1051/0004-6361/202244477

  75. [75]

    Exploring the spectral properties of faint hard X-ray sources with XMM-Newton

    Exploring the spectral properties of faint hard X-ray sources with XMM-Newton. , keywords =. doi:10.1051/0004-6361:20021235 , archivePrefix =. astro-ph/0208183 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20021235

  76. [76]

    , keywords =

    General physical properties of bright Fermi blazars. , keywords =. doi:10.1111/j.1365-2966.2009.15898.x , archivePrefix =. 0909.0932 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15898.x 2009

  77. [77]

    , keywords =

    X-ray spectra, light curves and SEDs of blazars frequently observed by Swift. , keywords =. doi:10.1093/mnras/stab2425 , archivePrefix =. 2108.07255 , primaryClass =

    work page doi:10.1093/mnras/stab2425

  78. [78]

    Spectral Survey of X-Ray Bright Active Galactic Nuclei from the Rossi X-ray Timing Explorer

    Spectral Survey of X-ray Bright Active Galactic Nuclei from the Rossi X-ray Timing Explorer. , keywords =. doi:10.1088/0067-0049/193/1/3 , archivePrefix =. 1101.1545 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/193/1/3

  79. [79]

    , keywords =

    The relation between broad lines and -ray luminosities in Fermi blazars. , keywords =. doi:10.1111/j.1365-2966.2012.20442.x , archivePrefix =. 1108.0927 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.20442.x 2012

  80. [80]

    General Physical Properties of CGRaBS Blazars

    General Physical Properties of CGRaBS Blazars. , keywords =. doi:10.3847/1538-4357/aa98e1 , archivePrefix =. 1711.01292 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa98e1

Showing first 80 references.