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arxiv: 2606.05307 · v1 · pith:ODJPHZUNnew · submitted 2026-06-03 · 🌌 astro-ph.HE

Constraining the jet base emission of M87* with past and future Event Horizon Telescope observations

Noemi La Bella , Michael Janssen , Britton Jeter , Hendrik M\"uller , Bram Van de Berg , Hung-Yi Pu , Paul Tiede , Heino Falcke This is my paper

Pith reviewed 2026-06-28 04:49 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords M87*Event Horizon Telescopejet emissionblack holesynthetic imagingaccretion modelsradio interferometryhorizon scales
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The pith

The current EHT array is already sensitive to weak jet emission at horizon scales in M87*.

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

The paper tests the ability of the Event Horizon Telescope to detect faint emission from the base of the relativistic jet in M87* at the smallest observable scales. It creates synthetic observations from semi-analytic models that let jet brightness be adjusted separately from the surrounding gas, then applies two reconstruction methods to data sets matching the 2021, 2022, and near-future array layouts. Detectability improves markedly with the 2022 configuration due to better short-baseline coverage, establishing a lower limit on jet intensity that can be reliably recovered. If the jet supplies a sizable share of the compact flux, its signature should appear in recent and upcoming images; a non-detection would indicate the jet contributes only a minor fraction at these scales.

Core claim

Using semi-analytic accretion jet models in which jet emission can be tuned independently of the accretion flow, synthetic EHT data for the 2021, 2022, and future array configurations are generated and reconstructed with regularized maximum likelihood and Bayesian imaging. Jet detectability is evaluated via flux density recovery, image fidelity, and uncertainty maps. The 2022 array improves reconstruction of faint jet features, and the current EHT is sensitive to weak jet emission at horizon scales in M87*. If the inner jet contributes significantly to unresolved compact flux, it should become visible in post-2021 observations; otherwise the horizon-scale jet is only a small part of the comp

What carries the argument

Semi-analytic accretion jet models allowing independent tuning of jet emission, combined with synthetic EHT data reconstruction using regularized maximum likelihood and Bayesian imaging to measure flux recovery and image fidelity across array configurations.

If this is right

  • The 2022 EHT array configuration enables more robust reconstruction of faint jet features than earlier arrays.
  • If the inner jet contributes a significant fraction of the unresolved compact flux, it should become visible in post-2021 observations.
  • If no clear jet signature appears, the horizon-scale jet contributes only a small part of the compact emission.
  • Continued expansion of the EHT will further improve detection of such jet emission in M87*.

Where Pith is reading between the lines

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

  • A non-detection would directly constrain the fraction of compact flux originating in the jet versus the accretion flow.
  • Future array improvements could separate jet and disk contributions more cleanly at event-horizon scales.
  • Repeated observations might track changes in jet base brightness over time.

Load-bearing premise

The semi-analytic accretion jet models produce realistic synthetic data that match the true emission properties at EHT frequencies.

What would settle it

Absence of any recoverable jet signature in 2022 EHT data when the jet intensity in the models exceeds the derived lower limit for reliable detection.

Figures

Figures reproduced from arXiv: 2606.05307 by Bram Van de Berg, Britton Jeter, Heino Falcke, Hendrik M\"uller, Hung-Yi Pu, Michael Janssen, Noemi La Bella, Paul Tiede.

Figure 1
Figure 1. Figure 1: Projected (u, v) coverage at 230 GHz for three representative EHT configurations (2021, 2022, and near-future). Colored points indicate newly introduced baselines in each configuration. Dashed circles correspond to angular scales of 25 and 50 µas. Insets highlight the short-baseline coverage (|b| ≤ 1.5 Gλ), which remains relatively limited. to extended structure. The PV–NOEMA baseline is ∼ 1100 km, yieldin… view at source ↗
Figure 2
Figure 2. Figure 2: Jet recovery for the 2022 array configuration. Rows show the high-, mid-, and low-jet truth models, while columns display the [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Relative uncertainty maps, defined as σ/I, derived from the Comrade posterior distributions for the three models and ob￾serving campaigns. All maps are shown using the same field of view and colour scale. Darker regions correspond to lower relative uncertainty, while brighter regions indicate higher relative uncertainty. White contours indicate intensity levels increasing by factors of 3, with the lowest d… view at source ↗
read the original abstract

We investigate the detectability of the jet base of M87* at Event Horizon Telescope (EHT) observing frequencies. Although M87 is known to host a prominent relativistic jet, detecting jet emission close to the black hole at horizon scales remains challenging. Our goal is to determine the minimum jet intensity that can be reliably detected with the recent EHT array configurations. We use synthetic EHT data generated for three array configurations corresponding to the 2021 and 2022 observing campaigns and to a near future EHT campaign. As input models, we employ semi analytic accretion jet models in which the jet emission can be tuned independently of the accretion flow. The synthetic data are reconstructed with regularized maximum likelihood and Bayesian imaging. Jet detectability is assessed through flux density recovery, image fidelity, and uncertainty maps. We find that jet detectability strongly depends on the jet intensity, the array configuration, and imaging methodology. Using our analysis, we determine a lower limit on the jet intensity that can be reliably recovered. The 2022 EHT array configuration represents a significant improvement over earlier arrays, enabling a more robust reconstruction of faint jet features. Our results indicate that the current EHT array is already sensitive to weak jet emission at horizon scales in M87*. The improved short-baseline coverage introduced in 2022 makes faint inner jet features more easily detectable. If the inner jet contributes a significant fraction of the unresolved compact flux, it should become visible in post-2021 observations. On the other hand, if no clear jet signature is found, this would suggest that the horizon-scale jet contributes only a small part of the compact emission. The continued expansion of the EHT will further improve the detection of such jet emission in M87*.

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

1 major / 2 minor

Summary. The manuscript investigates the detectability of faint jet-base emission at horizon scales in M87* using synthetic EHT visibilities generated from semi-analytic accretion+jet models. Jet intensity is treated as an independent tunable parameter. Synthetic data are produced for the 2021, 2022, and a near-future array configuration, then reconstructed with regularized maximum likelihood and Bayesian imaging. Detectability is quantified via flux-density recovery, image fidelity, and uncertainty maps. The central conclusion is that the 2022 array already provides sufficient sensitivity to recover weak jet emission if it contributes appreciably to the compact flux, while non-detection would imply a negligible jet contribution.

Significance. If the modeling assumptions hold, the work supplies a practical lower limit on detectable jet intensity and demonstrates that incremental improvements in short-baseline coverage (2022 array) meaningfully enhance recovery of faint inner-jet features. This directly informs interpretation of existing and upcoming EHT data on M87*, offering a route to test whether the unresolved compact flux is dominated by the accretion flow or by the jet base. The forward-modeling framework with multiple array realizations and two independent imaging pipelines is a strength.

major comments (1)
  1. [Model description and input models] The central claim that the 2022 array is already sensitive to weak horizon-scale jet emission rests on the assumption that independently tuned jet intensity in the semi-analytic models produces realistic morphological and spectral properties at 230 GHz. If magnetic-flux or plasma-β coupling between jet and disk introduces additional compact structure or polarization signatures not present in the decoupled models, the reported flux-recovery thresholds and uncertainty maps could shift. This assumption is load-bearing for translating the synthetic lower limit to actual M87* observations (see model description and § on input models).
minor comments (2)
  1. [Abstract] The abstract states that a lower limit on jet intensity is determined but does not quote the numerical value or associated uncertainty; including these quantities would improve immediate readability.
  2. Notation for the jet intensity scaling factor should be defined explicitly on first use and kept consistent across figures and text.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and for identifying a key modeling assumption. We address the major comment below and propose targeted revisions to the manuscript.

read point-by-point responses

  1. Referee: The central claim that the 2022 array is already sensitive to weak horizon-scale jet emission rests on the assumption that independently tuned jet intensity in the semi-analytic models produces realistic morphological and spectral properties at 230 GHz. If magnetic-flux or plasma-β coupling between jet and disk introduces additional compact structure or polarization signatures not present in the decoupled models, the reported flux-recovery thresholds and uncertainty maps could shift. This assumption is load-bearing for translating the synthetic lower limit to actual M87* observations (see model description and § on input models).

    Authors: We agree that the decoupling of jet and disk emission is a simplifying assumption whose realism must be qualified. The semi-analytic framework was deliberately chosen to permit independent variation of jet intensity, enabling a controlled exploration of the minimum detectable jet contribution—an approach not readily available in fully coupled GRMHD simulations. We will revise the model-description and discussion sections to (i) explicitly state that the reported thresholds assume no additional compact structure from magnetic or β coupling, (ii) note that such coupling could either enhance or dilute the jet signature depending on the sign of the correlation, and (iii) frame the derived lower limit as a conservative benchmark that future coupled simulations can refine. These additions will not change the quantitative results but will strengthen the caveats attached to observational interpretation. revision: partial

Circularity Check

0 steps flagged

No circularity: simulation-derived detectability threshold is independent of inputs

full rationale

The paper generates synthetic visibilities from semi-analytic models with jet intensity as an explicit free parameter, reconstructs the data with RML and Bayesian imaging, and reports the minimum intensity for which recovery metrics succeed. This threshold is an output of the forward-modeling pipeline rather than a redefinition, fitted input renamed as prediction, or self-citation chain. No equations or steps reduce the claimed sensitivity limit to the model inputs by construction. The analysis remains self-contained against external benchmarks of array performance.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The analysis rests on the assumption that semi-analytic jet models with independently tunable emission produce faithful synthetic visibilities; no free parameters are explicitly fitted to real data in the described workflow, and no new physical entities are introduced.

free parameters (1)
  • jet intensity scaling factor
    Tuned independently in the input models to test detectability thresholds.
axioms (2)
  • domain assumption Semi-analytic accretion jet models accurately represent horizon-scale emission when jet and accretion components are decoupled.
    Used as input models for synthetic data generation.
  • domain assumption Regularized maximum likelihood and Bayesian imaging recover true source structure when the model is within the array's resolution and sensitivity.
    Basis for assessing flux recovery and image fidelity.

pith-pipeline@v0.9.1-grok · 5880 in / 1449 out tokens · 28616 ms · 2026-06-28T04:49:39.912175+00:00 · methodology

discussion (0)

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Reference graph

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