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arxiv: 2606.11900 · v1 · pith:23YTDRL7new · submitted 2026-06-10 · 🌌 astro-ph.HE · astro-ph.GA

A Jet from a Nearly Dormant Black Hole

Xiaopeng Cheng , Hai Yang , Jun Yang , Xiaofeng Li , Feng Yuan , Rusen Lu , Hyunwook Ro , Bong Won Sohn
show 6 more authors
Lulu Fan Yihang Zhang Wen Chen Niu Liu John E. Conway Taehyun Jung
This is my paper

Pith reviewed 2026-06-27 08:58 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords supermassive black holesradio jetsvery long baseline interferometryNGC 4649low accretion ratescore shift
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The pith

Observations detect a two-sided jet from the supermassive black hole in M60 despite an Eddington ratio of 10^{-8}.

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

The paper reports multi-frequency VLBI observations that reveal a compact two-sided jet with a steep synchrotron spectrum in the elliptical galaxy M60. This source hosts a supermassive black hole accreting at roughly 10^{-8} of the Eddington limit, placing it in a nearly dormant state. The data also show an unusually steep frequency-dependent shift in the position of the radio core, which places the central engine only about 10 Schwarzschild radii upstream of the observed 8.37 GHz core. General relativistic magnetohydrodynamic simulations reproduce both the jet shape and the core shift when the outflow is magnetically dominated and far from equipartition. The result indicates that jet collimation can continue even when accretion has dropped to extremely low levels.

Core claim

Multi-frequency very long baseline interferometric observations detect a compact two-sided jet with an unusually steep synchrotron spectrum in NGC 4649. The apparent radio core exhibits an unprecedentedly steep frequency-dependent position shift toward the SMBH, locating the central engine only about 57 microarcseconds (projected distance of about 10 Schwarzschild radii) upstream of the 8.37 GHz core. General relativistic magnetohydrodynamic and radiative-transfer simulations reproduce the observed jet morphology and core-shift behaviour, indicating a magnetically dominated, non-equipartition jet-launching region.

What carries the argument

The steep frequency-dependent core shift together with GRMHD simulations that require magnetic dominance to match the data.

If this is right

  • Collimated outflows can be sustained at accretion rates as low as 10^{-8} of the Eddington limit.
  • The jet-launching region lies within roughly 10 Schwarzschild radii of the event horizon.
  • Standard conical equipartition models fail; magnetic dominance is required to explain the observations.
  • M60 becomes a laboratory for studying jet formation on event-horizon scales in the lowest-accretion regime.

Where Pith is reading between the lines

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

  • Similar faint jets may exist around Sgr A* and the M31 nucleus but remain undetected with current resolution.
  • Jet persistence at such low accretion rates could alter estimates of black-hole feedback in quiescent galaxies.
  • The required magnetic dominance supplies a lower bound on the field strength needed for collimation near dormant black holes.

Load-bearing premise

The detected compact radio structure and its frequency-dependent position shift are produced by a jet launched by the central black hole rather than by unrelated emission or instrumental effects.

What would settle it

Multi-frequency imaging that shows the same radio component at all frequencies with no measurable position shift or with a flat spectrum instead of the reported steep spectrum.

Figures

Figures reproduced from arXiv: 2606.11900 by Bong Won Sohn, Feng Yuan, Hai Yang, Hyunwook Ro, John E. Conway, Jun Yang, Lulu Fan, Niu Liu, Rusen Lu, Taehyun Jung, Wen Chen, Xiaofeng Li, Xiaopeng Cheng, Yihang Zhang.

Figure 1
Figure 1. Figure 1: Photon ring diameter (5.2 RS) as a function of Eddington ratio. Filled circles and open triangles represent VLBI and VLA total flux density at 5 GHz, respectively. The color represents the total flux density. The grey region on the left denotes the dormant black holes, whereas the white region on the right denotes the active AGN. We assume the transition from λEdd = 10−7 . The Extended Data [PITH_FULL_IMA… view at source ↗
Figure 2
Figure 2. Figure 2: VLBI images of M60∗ at 1.64 and 4.87 GHz, and the quasi-simultaneous spectra. Left: 1.64 GHz naturally weighted EVN + VLBA combined CLEAN image showing the large scale of the radio jet; Middle: 4.87 GHz VLBA naturally weighted CLEAN image showing the close-up view of the sub-parsec scale jet; Right: Best-fitting power-law spectra (S ν ∝ ν α ) for the total flux density (red) and for components N (blue) and… view at source ↗
Figure 3
Figure 3. Figure 3: Left: Separation of the radio core from the reference 8.37 GHz core as a function of [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Self-calibrated images of J1246+1153. The top-left and top-right panels correspond to 1.46 GHz and 1.64 GHz, respectively; the middle-left and middle-right panels show 2.3 GHz and 4.87 GHz; and the bottom panel displays the 8.37 GHz image. All images were made using natural weighting. The lowest contours are at ±3 times rms noise and further positive contours are drawn at increasing steps of 2. The gray el… view at source ↗
Figure 5
Figure 5. Figure 5: Self-calibrated images of M60∗ . The top-left and top-right panels correspond to 1.46 GHz and 1.64 GHz, respectively; the middle-left and middle-right panels show 2.3 GHz and 4.87 GHz; and the bottom panel displays the 8.37 GHz image. All images were made using natural weighting. The lowest contours are at ±3 times rms noise and further positive contours are drawn at increasing steps of 2. The gray ellipse… view at source ↗
Figure 6
Figure 6. Figure 6: The top row presents the intrinsic simulated jet emission at 1.64 GHz (left), 4.87 GHz [PITH_FULL_IMAGE:figures/full_fig_p020_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Simulated radio spectrum of the jet. The flux density decreases with frequency, showing [PITH_FULL_IMAGE:figures/full_fig_p020_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Simulated core shift as a function of observing frequency. The dots show the simulated [PITH_FULL_IMAGE:figures/full_fig_p021_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Two-dimensional distribution of the magnetization parameter, shown as log [PITH_FULL_IMAGE:figures/full_fig_p021_9.png] view at source ↗
read the original abstract

Most galaxies host supermassive black holes (SMBHs) that remain weakly accreting or dormant for much of their lifetimes. At the lowest accretion rates, these systems may represent the transition between active nuclei and dormant black holes, but whether they can still launch collimated jets remains unclear. The nuclei in our Galaxy (\sgra) and M31 are key examples of this regime, although no clear jet structure has yet been detected in either source. Here we report multi-frequency very long baseline interferometric observations of \Msixty\ (NGC~4649), a nearby elliptical galaxy hosting a nearly dormant SMBH with an Eddington ratio of $\sim10^{-8}$. We detect a compact two-sided jet with an unusually steep synchrotron spectrum, demonstrating that collimated outflows can persist even under nearly dormant accretion conditions. The apparent radio core exhibits an unprecedentedly steep frequency-dependent position shift toward the SMBH, locating the central engine only $\sim57\,\mu$as, corresponding to a projected distance of $\sim10$ Schwarzschild radii, upstream of the 8.37-GHz core. The observed jet morphology and steep core-shift behaviour are reproduced by general relativistic magnetohydrodynamic and radiative-transfer simulations, indicating a magnetically dominated, non-equipartition jet-launching region that departs from the standard conical equipartition picture. These results provide direct observational evidence that jet production can survive near the dormant SMBHs and establish \Msixty\ as a unique laboratory for probing jet formation on event-horizon scales in the lowest-accretion SMBH regime.

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 / 2 minor

Summary. The paper reports multi-frequency VLBI observations of NGC 4649 (M60) detecting a compact two-sided jet with steep synchrotron spectrum from its SMBH at ~10^{-8} Eddington ratio. It measures an unusually steep frequency-dependent core position shift of ~57 μas, locating the central engine ~10 Schwarzschild radii upstream of the 8.37 GHz core, and shows that GRMHD plus radiative-transfer simulations reproduce both the jet morphology and the core-shift behavior, indicating a magnetically dominated non-equipartition launch region.

Significance. If the jet identification and core-shift interpretation are robust, the result would provide direct evidence that collimated outflows can persist at extremely low accretion rates, extending our understanding of jet production near dormant SMBHs and establishing M60 as a laboratory for horizon-scale studies. The multi-frequency VLBI dataset combined with simulation comparison is a methodological strength.

major comments (3)
  1. [§4] §4 (Core position measurements): The reported ~57 μas frequency-dependent shift and its attribution to synchrotron self-absorption in a non-equipartition flow requires an explicit quantitative error budget addressing refractive interstellar effects and residual phase-calibration systematics at the micro-arcsecond level; without such a test (e.g., closure-phase consistency across bands), the placement of the engine at ~10 Rs remains vulnerable to alternative explanations.
  2. [§5] §5 (Simulation comparison): The claim that GRMHD+RT runs reproduce the observed morphology and steep core-shift without post-hoc parameter adjustment is central to the non-equipartition interpretation, yet the manuscript does not appear to present the explored parameter space or a quantitative goodness-of-fit metric demonstrating that the match is not forced by tuning of magnetic field or electron distribution parameters.
  3. [§3] §3 (Jet detection): The two-sided compact structure is interpreted as an SMBH-launched jet rather than unrelated emission or calibration artifacts, but the paper lacks reported multi-epoch proper-motion limits or additional tests that would independently exclude refractive or instrumental origins at the claimed precision.
minor comments (2)
  1. [Abstract] The abstract states the spectrum is 'unusually steep'; adding a direct numerical comparison to core-shift indices in other LLAGN would clarify the 'unprecedented' claim.
  2. [Figures] Figure captions for the VLBI images should include the exact restoring beam sizes and contour levels used at each frequency to allow independent assessment of the two-sided structure.

Simulated Author's Rebuttal

3 responses · 1 unresolved

We thank the referee for their thorough review and valuable comments on our manuscript. We address each of the major comments below and indicate where revisions will be made to the manuscript.

read point-by-point responses

  1. Referee: [§4] §4 (Core position measurements): The reported ~57 μas frequency-dependent shift and its attribution to synchrotron self-absorption in a non-equipartition flow requires an explicit quantitative error budget addressing refractive interstellar effects and residual phase-calibration systematics at the micro-arcsecond level; without such a test (e.g., closure-phase consistency across bands), the placement of the engine at ~10 Rs remains vulnerable to alternative explanations.

    Authors: We concur that an explicit quantitative error budget is necessary to robustly support the core-shift measurement. In the revised manuscript, we will expand §4 to include a detailed error analysis quantifying the potential contributions from refractive interstellar scintillation and residual phase-calibration errors at the μas level. Additionally, we will report closure-phase consistency tests performed across the observed frequency bands to confirm that the measured shift is intrinsic rather than due to systematics. revision: yes

  2. Referee: [§5] §5 (Simulation comparison): The claim that GRMHD+RT runs reproduce the observed morphology and steep core-shift without post-hoc parameter adjustment is central to the non-equipartition interpretation, yet the manuscript does not appear to present the explored parameter space or a quantitative goodness-of-fit metric demonstrating that the match is not forced by tuning of magnetic field or electron distribution parameters.

    Authors: The simulations presented were conducted using GRMHD models with magnetic field strengths and electron distributions appropriate for the low accretion rate regime of M60, without post-hoc tuning to match the specific core-shift value. To provide greater transparency, the revised manuscript will include a description of the parameter ranges explored in the GRMHD and radiative transfer calculations, along with a quantitative goodness-of-fit assessment (e.g., via structural similarity or chi-squared metrics) between the simulated and observed images and core positions. revision: yes

  3. Referee: [§3] §3 (Jet detection): The two-sided compact structure is interpreted as an SMBH-launched jet rather than unrelated emission or calibration artifacts, but the paper lacks reported multi-epoch proper-motion limits or additional tests that would independently exclude refractive or instrumental origins at the claimed precision.

    Authors: The jet identification relies on the detection of a symmetric two-sided structure with a steep synchrotron spectrum that is consistent across multiple frequencies, features that are difficult to attribute to calibration artifacts or refractive interstellar effects, which typically do not produce such frequency-dependent but morphologically consistent emission. We note that our dataset consists of single-epoch observations, so multi-epoch proper-motion measurements are not available. revision: partial

standing simulated objections not resolved
  • Absence of multi-epoch VLBI observations, which precludes reporting proper-motion limits to further rule out alternative explanations for the detected structure.

Circularity Check

0 steps flagged

No significant circularity; result is direct observational detection

full rationale

The paper reports multi-frequency VLBI detections of a two-sided compact structure and frequency-dependent core shift in M60, with the central claim resting on these empirical measurements rather than any derivation that reduces to fitted parameters or self-citations by construction. GRMHD+RT simulations are invoked only for post-observation interpretation and morphological matching, without the observed jet or shift being defined in terms of the simulation outputs. No self-definitional, fitted-input-as-prediction, or load-bearing self-citation steps appear in the abstract or described chain; the work is self-contained against external VLBI data.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Based solely on the abstract, the claim rests on the interpretation that the observed radio morphology is synchrotron emission from a magnetically dominated jet and that the GRMHD simulations reproduce the data without undisclosed free parameters.

pith-pipeline@v0.9.1-grok · 5856 in / 1148 out tokens · 23184 ms · 2026-06-27T08:58:51.752787+00:00 · methodology

discussion (0)

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Reference graph

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