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REVIEW 3 major objections 4 minor 211 references

Dynamics and geometry of the inner sub-parsec-scale jet in 3C 279 observed with the Event Horizon Telescope

T0 review · 3 major / 4 minor · reviewed 2026-08-01 · deepseek-v4-flash

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Pith's one-line read The 2021 Event Horizon Telescope observations of the blazar 3C 279 establish that its innermost jet is elongated nearly orthogonal to the large-scale jet and bends toward the observer, with apparent speeds up to about ten times the speed of

desk verdict Solid 2021 EHT imaging of 3C 279 with a kinematic interpretation that is plausible but rests on an unquantified alignment assumption; worth refereeing, with the dynamics reframed as conditional. read the letter →

arxiv 2607.16104 v1 pith:GSCZKCTN submitted 2026-07-17 astro-ph.GA

Hendrik Mueller , Sebastiano D. von Fellenberg , Ai-Ling Zeng , Paul Tiede , Thomas P. Krichbaum , Roman Gold , Tuomas Savolainen , Jae-Young Kim
show 270 more authors
Sijia Peng Teresa Toscano Michael Janssen Boris Georgiev Dhanya G. Nair Iniyan Natarajan Lindy Blackburn Kazunori Akiyama Ezequiel Albentosa-Ruiz Antxon Alberdi Walter Alef Juan Carlos Algaba Rohan Ganesh Amanaganti Richard Anantua Eleni Antonopoulou Keiichi Asada Rebecca Azulay Anne-Kathrin Baczko David Ball Bidisha Bandyopadhyay John Barrett Michi Bauböck Bradford A. Benson Dan Bintley Raymond Blundell Katherine L. Bouman Geoffrey C. Bower Michael Bremer Roger Brissenden Silke Britzen Avery E. Broderick Dominique Broguiere Thomas Bronzwaer Sandra Bustamante Douglas F. Carlos John E. Carlstrom Andrew Chael Chi-kwan Chan Chin-Shin Chang Dominic O. Chang Koushik Chatterjee Erandi Chavez Ming-Tang Chen Yongjun Chen Xiaopeng Cheng Paul Chichura Ilje Cho Nicholas S. Conroy John E. Conway Thomas M. Crawford Geoffrey B. Crew Alejandro Cruz-Osorio Yuzhu Cui Brandon Curd Rohan Dahale Jordy Davelaar Joost de Kleuver Mariafelicia De Laurentis Roger Deane Jason Dexter Vedant Dhruv Indu K. Dihingia Sheperd S. Doeleman Sergio A. Dzib Razieh Emami Heino Falcke Joseph Farah Vincent L. Fish Edward Fomalont H. Alyson Ford Marianna Foschi Raquel Fraga-Encinas William T. Freeman Per Friberg Christian M. Fromm Antonio Fuentes Peter Galison Charles F. Gammie Roberto Garcia Olivier Gentaz Ciriaco Goddi Arturo I. Gomez-Ruiz Brissa Gomez Miller Jose L. Gomez Minfeng Gu Mark Gurwell Kazuhiro Hada Daryl Haggard Ronald Hesper Dirk Heumann Luis C. Ho Paul Ho Mareki Honma Chih-Wei L. Huang Lei Huang David H. Hughes Shiro Ikeda C. M. Violette Impellizzeri Makoto Inoue Sara Issaoun Yuhei Iwata David J. James Buell T. Jannuzi Britton Jeter Wu Jiang Alejandra Jiménez-Rosales Michael D. Johnson Svetlana Jorstad Adam C. Jones Abhishek V. Joshi Taehyun Jung Tomohisa Kawashima Garrett K. Keating Mark Kettenis Dong-Jin Kim Jongsoo Kim Junhan Kim Motoki Kino Jakob Knollmüller Jun Yi Koay Prashant Kocherlakota Yutaro Kofuji Patrick M. Koch Shoko Koyama Carsten Kramer Joana A. Kramer Michael Kramer Cheng-Yu Kuo Noemi La Bella Deokhyeong Lee Sang-Sung Lee Aviad Levis Shaoliang Li Zhiyuan Li Rocco Lico Greg Lindahl Michael Lindqvist Mikhail Lisakov Jun Liu Kuo Liu Elisabetta Liuzzo Wen-Ping Lo Andrei P. Lobanov Laurent Loinard Colin J. Lonsdale Amy E. Lowitz Ru-Sen Lu Nicholas R. MacDonald Jirong Mao Nicola Marchili Sera Markoff Daniel P. Marrone Alan P. Marscher Ivan Marti-Vidal Satoki Matsushita Lynn D. Matthews Lia Medeiros Karl M. Menten Hugo Messias Izumi Mizuno Yosuke Mizuno Joshua Montgomery Kotaro Moriyama Monika Moscibrodzka Wanga Mulaudzi Cornelia Müller Alejandro Mus Gibwa Musoke Ioannis Myserlis Hiroshi Nagai Neil M. Nagar Masanori Nakamura Gopal Narayanan Antonios Nathanail Santiago Navarro Fuentes Joey Neilsen Chunchong Ni Andy Nilipour Michael A. Nowak Hiroki Okino Hector Raul Olivares Sanchez Feryal Özel Daniel C. M. Palumbo Georgios Filippos Paraschos Jongho Park Harriet Parsons Nimesh Patel Ue-Li Pen Dominic W. Pesce Vincent Pietu Alexander Plavin Aleksandar PopStefanija Oliver Porth Cora Prather Giacomo Principe Dimitrios Psaltis Hung-Yi Pu Alexandra Rahlin Venkatessh Ramakrishnan Ramprasad Rao Mark G. Rawlings Luciano Rezzolla Angelo Ricarte Luca Ricci Bart Ripperda Jan Röder Freek Roelofs Cristina Romero-Cañizales Eduardo Ros Arash Roshanineshat Helge Rottmann Alan L. Roy Ignacio Ruiz Chet Ruszczyk Kazi L. J. Rygl Leon D. S. Salas Salvador Sanchez David Sanchez-Argüelles Miguel Sanchez-Portal Ali SaraerToosi Mahito Sasada Kaushik Satapathy Saurabh Karl-Friedrich Schuster Zhiqiang Shen Sasikumar Silpa Randall Smith Bong Won Sohn Jason SooHoo Kamal Souccar Joshua S. Stanway He Sun Alexandra J. Tetarenko Remo P. J. Tilanus Michael Titus Kenji Toma Pablo Torne Efthalia Traianou Sascha Trippe Matthew Turk Akhil Uniyal Ilse van Bemmel Bram van den Berg Huib Jan van Langevelde Daniel R. van Rossum Jesse Vos Jan Wagner Zhiren Wang Derek Ward-Thompson John Wardle Jasmin E. Washington Jonathan Weintroub Maciek Wielgus Kaj Wiik Michael F. Wondrak George N. Wong Jompoj Wongphexhauxsorn Qingwen Wu Paul Yamaguchi Aristomenis Yfantis Doosoo Yoon Andre Young Ziri Younsi Wei Yu Feng Yuan Ye-Fei Yuan J. Anton Zensus Shuo Zhang Brandon Zhao Guang-Yao Zhao
This is my paper
classification astro-ph.GA
keywords 3C279blazarrelativisticjetEventHorizonTelescopeverylongbaselineinterferometrysuperluminalmotionbendingDopplerbeaming
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

This paper tries to establish that the innermost jet of the blazar 3C 279 is not straight: the 2021 Event Horizon Telescope observations resolve a compact core elongated nearly orthogonal to the large-scale jet, and that morphology is intrinsic rather than an imaging artifact. From component motions measured over five days, the paper derives apparent speeds up to about ten times the speed of light, which under standard relativistic beaming relations forces a bulk Lorentz factor above 10.3 and viewing angles below one degree. The conclusion is that the jet bends toward the observer on sub-parsec scales, producing strong Doppler beaming, while the intrinsic brightness temperatures are strikingly low, consistent with optically thin emission at 230 GHz. A sympathetic reader cares because this constrains where jet acceleration and collimation happen near a supermassive black hole and shows that jets can change direction on year-level timescales.

What carries the argument

The load-bearing machinery is a set of compact emission components (C0, C2-0 through C2-3, C3) fitted as elliptical Gaussians to the interferometric visibilities, with all image epochs aligned on the assumption that component C0 is the stationary kinematic origin, i.e., the VLBI core. The relativistic speed relations β_app = β sinθ / (1 − β cosθ), Γ = 1/√(1 − β²), and the Doppler factor δ = 1/[Γ(1 − β cosθ)] convert five-day projected displacements of order 1–2 microarcseconds per day into apparent speeds up to ~10c and then into the constraints Γ ≳ 10.3 and θ ≲ 1°. Consistency of the reconstructed morphology across multiple imaging algorithms, frequency bands, and epochs is what carries the

What would settle it

A future high-resolution VLBI epoch that tracks C0 against an absolute astrometric reference, or that shows C0 moving coherently with the jet flow, would falsify the stationary-origin assumption. Alternatively, a spectral-index map showing C0 with an optically thick, flat or inverted spectrum—unlike the steep optically thin spectrum of the C2 components—would contradict the claim that C0 is the true stationary core.

Watch

Extended reading notes

Core claim

The 2021 Event Horizon Telescope observations resolve the innermost jet region of 3C 279 down to roughly 20 microarcseconds, revealing a compact core elongated nearly perpendicular to the large-scale jet axis. This morphology recurs across multiple epochs, frequency bands, and independent imaging algorithms, so the paper argues it is intrinsic. Geometric model fitting identifies several emission components whose projected motions over three epochs in April 2021 reach apparent speeds β_app up to ~10, requiring a bulk Lorentz factor Γ ≳ 10.3 and constraining viewing angles to below one degree. The inferred rest-frame brightness temperatures are systematically low, around 10^9–10^10 K, which th

Load-bearing premise

The load-bearing premise is that the faint northern component C0 is the stationary kinematic origin, i.e., the true VLBI core; the paper itself admits this identification is interpretive because no objective criterion exists, and if C0 moves then the derived speeds, Lorentz-factor lower limit, and viewing-angle constraints do not follow.

Editorial extensions

If this is right

  • Acceleration of the jet happens very close to the kinematic origin: the C2 components already move with Lorentz factors comparable to the outer jet, within roughly 5000 gravitational radii deprojected.
  • The apparent deceleration from C2-0 toward C2-3 is a projection effect of a jet bending toward the observer, not genuine slowing, so the components can share a similar bulk Lorentz factor.
  • 3C 279, at least in April 2021, is seen almost face-on, with a viewing angle below one degree, making it one of the few blazars observed this close to the line of sight.
  • The low rest-frame brightness temperatures (10^9–10^10 K) support optically thin emission at 230 GHz, consistent with a magnetically dominated or still-accelerating jet.
  • The inner-jet position angle changes on year-level timescales while the outer jet remains straight, implying structural evolution of the jet base that is hidden at longer wavelengths.

Reading between the lines

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

  • If the bend is geometric, multi-epoch monitoring at 230 GHz should show component trajectories curving coherently and the position-angle swing propagating downstream; a campaign with several epochs per year could test this directly.
  • A spectral-index map separating C0 from the C2 components could settle which feature is the true core: if C0 is the stationary jet apex it should show an optically thick, flat or inverted spectrum, whereas if all components are downstream knots all should be steep, with spectral index near −1.
  • The paper's Γ and θ values inherit the assumption that C0 is fixed. If C0 is instead a propagating feature, the reported apparent speeds overstate the pattern speed and the true Lorentz factor could be lower; the alternative alignment on C2-2, which the paper shows produces inward motion for C2-3, is a reminder that the kinematics are reference-frame dependent.
  • If the near-face-on geometry is real, the source should show strong Doppler-boosted variability and a very wide apparent opening angle at the jet base; the paper notes this wide opening angle is not recovered, possibly due to sensitivity, which future higher-sensitivity observations could verify.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. This paper analyzes 2021 EHT 230 GHz observations of the blazar 3C 279 from three epochs in April 2021, complemented by quasi-simultaneous 43/86 GHz images. The multi-code imaging (Comrade, DoG-HiT, kine, Difmap) consistently shows a compact north-south extended core nearly orthogonal to the large-scale jet axis. Using Difmap elliptical Gaussian models, the authors track four subcomponents of the bright C2 complex over five days, infer apparent speeds up to ~10c, and derive a lower limit Γ≳10.3 and viewing angles ≲1°, which they interpret as the jet bending toward the observer on sub-parsec scales. They also derive low rest-frame brightness temperatures (~10^9–10^10 K) and discuss possible bending mechanisms.

Significance. The imaging morphological claim is significant and well supported: the north-south elongation recurs across three imaging codes, two 230 GHz bands, three epochs, and is corroborated by 43/86 GHz images; the paper also acknowledges the Difmap degeneracy and explains it. This part of the paper is a solid contribution. The kinematic claim, however, is only as strong as the a priori identification of C0 as the stationary core. The paper is honest about this (§4.3), but it does not propagate the frame-choice uncertainty into the headline physical parameters. Because the apparent speeds, Lorentz factor lower limit, Doppler factors, and viewing-angle upper limits all follow from this single assumption, the central dynamical conclusion is currently under-supported. The analysis is reproducible in principle (public EHT data, open-source codes), and the multifrequency comparison is a strength.

major comments (3)
  1. [§4.2–§4.3, Table 1, Fig. B.5] The kinematic results in Table 1 and §4.5 all follow from the assumption, stated in §4.2, that 'the C0 component is the stationary kinematic origin.' Section 4.3 acknowledges that 'no objective criterion exists' for this identification and shows in Fig. B.5 that registering instead on C2-2 changes the inferred motions, producing inward motion for C2-3. Yet Table 1 lists only the statistical position errors; no systematic uncertainty from the alignment choice is propagated into β_app, Γ, δ, or θ. If C0 is itself moving, the apparent speeds are not physical, and the Γ>10.3 lower limit, the θ<1° constraints, and the bending conclusion in §4.5 collapse. The authors should recompute the kinematic constraints in the C2-2 frame and quote the range spanned by both registrations, or provide a quantitative argument for why C0 is stationary.
  2. [§4.5, Eq. (1), Table 1] The lower limit Γ = 10.3±0.5 is quoted from β_app = 10.2±4.3 (Table 1). The minimum Lorentz factor implied by a measured apparent speed is Γ_min = sqrt(1+β_app^2). Propagating the 1σ uncertainty on β_app gives Γ_min ≈ 6 for the lower end of the error bar, not 10.3. The quoted Γ = 10.3±0.5 therefore does not appear to include the statistical uncertainty in the apparent speed, nor does it explain how a 'lower limit' can have a ±0.5 error. The same issue affects the derived Doppler factors (δ = 10±3 etc.) and the viewing-angle upper limits in Table 1 and Fig. 8. A full error propagation, or a conservative lower limit using the 1σ lower bound of β_app, should be provided.
  3. [§4.5, Fig. 8] The claimed gradient in apparent speed with separation (C2-0: 10.2±4.3; C2-1: 9.3±1.6; C2-2: 3.9±2.3; C2-3: 1.3±1.1) is visually suggestive of bending, but the uncertainties overlap substantially. The paper does not present a statistical comparison between the bending interpretation and alternatives such as intrinsic acceleration/deceleration or component evolution, instead invoking Occam's razor (§4.5). Given that the central abstract claim is that 'the jet bends toward the observer on sub-parsec scales,' the authors should at least demonstrate that the β_app-separation trend is statistically significant after propagating position and alignment uncertainties, e.g., via Monte Carlo resampling of the model fits.
minor comments (4)
  1. [§1] The text says 3C 279 is 'located at a distance of approximately∼16.5 Mpc (z≈0.536)'. This is inconsistent with the redshift; the comoving distance at z≈0.536 is ~1.6 Gpc in the adopted cosmology. Please correct the distance unit or value.
  2. [§4.1] The total flux density is quoted as 9.96±0.02 Jy, but the sum of the model component fluxes in Table D.1 is ~6.3 Jy for the April 13 band 3 epoch. Please clarify whether the total refers to the image-integrated flux and how the difference is attributed to extended emission.
  3. [§4.4, Table 1] The rest-frame brightness temperatures in Table 1 appear to use a single Doppler factor δ~10, while §4.5 derives component-dependent δ values between 10 and 20. For consistency, either use the component-specific δ or state explicitly that a common δ=10 was adopted for all components.
  4. [§4.2] The positional uncertainty formula ('half the beam size divided by the median S/N') is not a rigorous estimate and likely underestimates systematic errors. Since these values directly enter the kinematic errors in Table 1, the derivation should be described more carefully.

Circularity Check

1 steps flagged · score 2.0 of 10

Kinematic results are conditional on the assumed stationarity of C0, but the imaging morphology claim is independently validated; no equation-level circularity.

  1. other [§4.2 Model fitting; §4.3 Identification of kinematic origin; Table 1; §4.5 Jet dynamics]
    "we aligned the images and assumed that the C0 component is the stationary kinematic origin, i.e., it shows no intrinsic motion. Under this assumption, the data show coherent evolution across three days with projected velocities of 1−2 µas per day ... and to apparent velocities of up to 10c."

    The headline apparent speeds β_app (Table 1) are coordinate differences measured after registering all epochs on C0 and assuming C0 is stationary. The derived Γ≳10.3, Doppler factors δ, viewing-angle upper limits, and rest-frame brightness temperatures all inherit this reference-frame choice. The paper itself concedes in §4.3 that 'no objective criterion exists' for this identification and shows that aligning on C2-2 changes the inferred motions (inward motion for C2-3). The kinematic result is therefore constructed from, and conditional on, the assumed stationarity of C0 rather than independently determined from the visibilities. The morphology claim does not share this vulnerability, as it is supported by multiple independent imaging algorithms, frequency bands, and epochs.

full rationale

The paper's central derivation — resolving an elongated, quasi-orthogonal core and interpreting it as intrinsic morphology — is well supported by independent reconstructions (Comrade, DoG-HiT, kine, Difmap), two 230 GHz bands, quasi-simultaneous 43/86 GHz images, and multiple epochs; this part is not circular. The kinematic inversion from apparent speeds to Γ and θ uses the standard relativistic formulas (Eqs. 1–3) and is not equation-level circularity: β_app is a measured input, not a fitted parameter renamed as a prediction. The only notable dependency is the explicit assumption that C0 is the stationary kinematic origin. The paper discloses this assumption and even shows an alternative alignment (C2-2) that changes the inferred motions, but it does not propagate that choice into the quoted uncertainties of Table 1. This is an acknowledged interpretive fragility rather than a self-citation or definitional circularity. The minor reliance on prior EHT papers (Lu et al. 2013; Kim et al. 2020) for the same northern-component identification is a mild self-citation but is supplemented here by multifrequency evidence, so it is not load-bearing on its own. Overall, no significant circularity is present; the kinematic conclusions should be read as conditional on the C0 reference-frame assumption.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

Most of the analysis is standard radio-interferometric model fitting plus standard relativistic transformations. The load-bearing non-standard assumptions are the designation of C0 as a stationary kinematic origin and the geometric-bending interpretation of the apparent-speed gradient. No new physical entities (new particles, forces, or conserved quantities) are introduced. The fitted model-component parameters are listed as free parameters because the kinematic claims are functions of them, but they are the measurement outputs rather than hidden inputs.

free parameters (3)
  • Difmap elliptical-Gaussian component parameters (flux, RA, Dec, major/minor axes, PA) for C0, C1, C2-0..C2-3, C3 = Table D.1 (e.g., Apr 13 band 3: C2-0 flux 0.604 Jy at RA=64.3, Dec=-103.5 µas; C2-2 flux 1.670 Jy at RA=63.1, Dec=-120.9
    All kinematic quantities and brightness temperatures are derived from these fitted model parameters. The decomposition is not unique (see Difmap 1 vs Difmap 2 in Fig. 4), and the quoted uncertainties are statistical only.
  • Rest-frame Doppler factor delta ≈ 10 used in TB' = TB(1+z)/delta = delta ≈ 10 (C2-0: 10±3; C2-1: 14±2; C2-2: 19±1; C2-3: 20±1)
    Chosen from the same kinematic model (Gamma ≳ 10.3 and derived viewing-angle limits) rather than measured independently; the stated rest-frame brightness temperatures inherit this model dependence.
  • Median gain calibration uncertainty f_cal ≈ 0.1 in flux error budget = 0.1
    Used for sigma_S^2 = sigma_thermal^2 + f_cal^2 S^2 in Sec. 4.2; affects quoted flux and brightness-temperature errors but not the central values.
assumptions (5)
  • standard math Relativistic beaming relations Eqs. (1)-(3): beta = beta_app/(sin theta + beta_app cos theta), Gamma = (1-beta^2)^(-1/2), delta = 1/[Gamma(1-beta cos theta)]
    Used in Sec. 4.5 to convert measured apparent speeds into Lorentz factors, Doppler factors, and viewing-angle limits.
  • ad hoc to paper C0 is the stationary kinematic origin and all images are aligned on it in the absence of absolute astrometry
    Load-bearing for all apparent motions and hence for Gamma and theta constraints; the paper acknowledges this is interpretive in Sec. 4.3.
  • ad hoc to paper The apparent-speed gradient with separation is caused by decreasing viewing angle (geometric bending) rather than intrinsic deceleration
    Adopted by Occam's razor in Sec. 4.5; underlies the claim that the jet bends toward the observer and the quoted theta upper limits.
  • domain assumption The jet-to-counter-jet brightness ratio for 3C 279 exceeds 10^10, so the northern component C0 cannot be a counter-jet
    Used in Sec. 4.3 to argue C0 is upstream emission rather than a counter-jet; taken from Urry & Padovani (1995).
  • domain assumption The 230 GHz emission is optically thin, so low rest-frame brightness temperatures indicate optically thin or magnetically dominated plasma
    Used in Sec. 4.4 to interpret the low TB values; supported by ALMA spectral-curvature measurements but not directly proven for the resolved components.

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Cite this review

Pith. "Pith review of Dynamics and geometry of the inner sub-parsec-scale jet in 3C 279 observed with the Event Horizon Telescope." pith.science (2026). https://pith.science/paper/GSCZKCTN

@misc{pith2026260716104,
  author       = {Pith},
  title        = {Pith review of: Dynamics and geometry of the inner sub-parsec-scale jet in 3C 279 observed with the Event Horizon Telescope},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GSCZKCTN}},
  note         = {Machine review of arXiv:2607.16104}
}
read the original abstract

The 2021 Event Horizon Telescope observations resolve the innermost jet region of the blazar 3C279 with unprecedented detail. The reconstructed images consistently reveal a compact core elongated nearly orthogonal to the large-scale jet axis. This rarely observed morphology recurs across multiple epochs and from 22-230 GHz and is therefore intrinsic rather than an imaging artifact. Geometric model fitting identifies several components with apparent speeds up to 10c, requiring bulk Lorentz factors greater than 10.3 and constraining viewing angles to extremely small values (smaller than one degree). Rest-frame brightness temperatures are systematically low (between 10^9 and 10^10 K), consistent with optically thin emission at 230 GHz. These results suggest that the jet bends toward the observer on sub-parsec scales, producing strong relativistic beaming. Possible drivers of the observed jet bending and temporal evolution include the jet's interaction with the interstellar medium, kink or Kelvin--Helmholtz instabilities, magnetic reconnection near the horizon, or binary-induced precession. However, the current temporal coverage of VLBI data remains insufficient to distinguish between these mechanisms. Continued multifrequency VLBI monitoring will be essential to constraining the dynamics and geometry of the jet base in 3C279.

Figures

Figures reproduced from arXiv: 2607.16104 by the authors.

Figure 1
Figure 1. 3C 279 at three different frequencies from quasi-simultaneous observations in April 2021. Left panel: VLBA [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Naming convention of the Difmap model compo￾nents, based on the Comrade image from April 13, band 3. The C2 structure is modeled by four components. We also sketch three possible reference positions for the kinematical analysis, which are discussed in Sect. 4.3. The pixel size is 1 µas2 . image is shown in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Fiducial image of the source in linear scale for the [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: Reconstruction results in band 3 on April 13 with [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: 230 GHz image of 3C 279 observed in 2021 compared to the structure observed by the GMVA in 2021 (in prep.). [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]
Figure 6
Figure 6. Figure 6: 1.3 mm structure of 3C 279 obtained at three dif [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]
Figure 7
Figure 7. Figure 7: Location of the model-fitted com￾ponents for band 3. The blue, orange, and green crosses mark the positions at the three different observing epochs. The marker size indicates the model statisti￾cal fit uncertainty derived from half the beam size divided by the median s…
Figure 8
Figure 8. Figure 8: Comparison of apparent speed βapp and viewing angle constraints for 3C 279. Each panel shows a different parameterization: (a) Apparent speed as function of viewing angle for different bulk Lorentz factors compared to measured values as indicated by the dashed lines. (…
Figure 9
Figure 9. Figure 9: 43 GHz images of 3C 279 (black), obtained by the University of Boston blazar monitoring program at epochs [PITH_FULL_IMAGE:figures/full_fig_p011_9.png]

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