Ring Position Angles and Spin in M87* and Sgr A*

arXiv:2606.11322 · astro-ph.HE · Submitted 2026-06-09 · Read on arXiv

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Introduction to the show: ident: Astrophysics Radio. Generated commentary on the latest astrophysics papers.

Vera: I'm Vera, and with me are Jocelyn and Subrahmanyan, guest researcher.

Jocelyn: Today's paper: "Ring Position Angles and Spin in M87* and Sgr A*".

Vera: Event Horizon Telescope (EHT) images of black holes appear as rings with a brightness asymmetry,

Jocelyn: First, who's behind it and why it matters.

Title and authors: Vera: Well, Jocelyn, we've got the full text of this paper now. It’s called "Ring Position Angles and Spin in M87* and Sgr A*," which sounds super technical, but it really gets to the heart of what we can learn from those EHT images.

Jocelyn: I agree, Vera, and looking at the authors listed—Conroy et al.—it shows a really collaborative effort spanning different areas of astrophysics. It tells us that understanding these black holes isn't just one person's job; it takes a whole team pulling data from telescopes and theoretical models.

Subrahmanyan: From a theoretical standpoint, I see the authors tackling the fundamental problem of how the magnetic fields threading these black holes dictate their spin and orientation, which is crucial for linking accretion physics to general relativity.

Vera: Exactly. So, Jocelyn, what's this paper actually saying in a nutshell about what it looks at? It seems to be focusing on how we can use the shape of those brightness asymmetries in M87* and Sgr A* to figure out more about the black holes themselves.

Jocelyn: Basically, they take those ring images and look at their position angles—that's that crucial part—to constrain two major unknowns: the spin of the black hole and its orientation. It’s like using a compass to see which way the black hole is actually spinning in relation to its surroundings.

Subrahmanyan: That’s significant because knowing the spin tells us about how much energy we can extract from those accretion flows, which connects directly to the physics of jet launching, a really big cosmic picture element.

Vera: Right, and they're doing this by comparing what we see in the real data against these detailed computer simulations they call the "Illinois v5" library. That’s where the heavy lifting of modeling comes in.

Jocelyn: The Illinois v5 library is really impressive because it covers a huge range of possibilities, including different types of magnetization modes and various spin magnitudes, which allows them to test many different scenarios against the actual images they're looking at.

Subrahmanyan: It’s interesting that they are using KHARMA for the accretion flow evolution and ipole for radiative transfer in their simulations; that level of detail is what lets them map these complex physical processes onto the observable ring structure.

Vera: And then, they use tools like VIDA and Comrade to fit a geometric model—specifically an m-ring truncated at m=four with a Gaussian background—to pull out the brightness asymmetry magnitude a one and its position angle PA1. That’s how they get their hard numbers.

Jocelyn: So, when they talk about a one and PA1, they are essentially measuring the amplitude and phase of that one-ring component in the image data, which is directly linked to the spin vector direction.

Title and authors: Subrahmanyan: That link between the observed angular features and the underlying spacetime geometry is what makes this research so compelling for theoretical astrophysics; it’s empirical evidence constraining general relativistic magnetohydrodynamics.

Vera: Let's talk about what they found regarding the spin constraints, because that seems to be a big part of their focus in this paper. They showed that for larger spins, say a* > zero or a* -zero point five, the mean PA1 falls within one standard deviation of the approaching limb of the black hole, regardless of things like viewing inclination or disk magnetization.

Jocelyn: That's a strong statement because it suggests that for these specific spin ranges, you can reliably point to that approaching side just by looking at where PA1 lands, which simplifies our interpretation considerably.

Subrahmanyan: That finding is important because it suggests a certain robustness in the relationship between spin and observable features, implying that the fundamental physics of the horizon dominates those observational signatures across various accretion states.

Vera: They also compared this distribution in M87 observations with their models to say they can "mildly disfavor low-magnitude spins" and "strongly disfavor all spin vectors that point toward Earth." On top of that, they suggest the alignment of PA1 relative to the large-scale jet axis in M87 might imply a small tilt in its accretion disk.

Jocelyn: So, it’s not just about finding a number; it's about using the positional information to rule out certain physical configurations for the black hole system itself, which is really powerful observational science.

Subrahmanyan: That connection between PA1 and the jet axis hints at a physical alignment between the magnetic field structure near the horizon and the large-scale outflow, which helps us build models of how jets are launched consistently.

Vera: Then there's the part about position angle dynamics, where they look at how PA1 evolves stochastically around a mean value mu, described by a circular Gaussian distribution with a correlation timescale tau corr(PA1) = one hundred thirty-three t g. They suggest this m-ring dynamics constrain the sign of c zero.

Jocelyn: That dynamical constraint, especially when combined with pattern speed measurements from other observations, is what lets them potentially constrain whether M87 is prograde or retrograde with about an eighty-four percent accuracy.

Subrahmanyan: Constraining the prograde or retrograde nature of the black hole spin using these observables provides a direct test for models describing angular momentum transport within the accretion flow, which has huge implications for how gas spirals in.

Vera: Moving over to Sgr A*, they say that a detection of (a one PA1) could constrain the magnitude and direction of the galactic center spin vector. They admit that EHT data is just beginning to constrain (a one PA1) with high uncertainty for this source.

Title and authors: Jocelyn: That uncertainty is expected given Sgr A*'s complexity, but even a tentative detection would be a huge step in mapping the magnetic field structure around our own galactic center.

Subrahmanyan: If we can pin down the spin vector direction for Sgr A* using these methods, it helps us map out the large-scale magnetic environment of our galaxy and its influence on phenomena like star formation.

Vera: Looking ahead, the paper lays out some exciting future applications. They mention that a future EHT expansion, like the Black Hole Explorer satellite, could let us analyze horizon-scale asymmetry for sources beyond M87 and Sgr A*.

Jocelyn: And for those new sources, they say we could measure three total intensity ring observables—ring angular diameter to constrain the mass/distance, brightness asymmetry magnitude to constrain spin and inclination, and brightness asymmetry position angle to constrain the spin vector position angle.

Subrahmanyan: That trinity of measurements is what allows for a much more complete parameter inference across different black hole systems than just using one or two features alone, which is key for understanding growth history.

Vera: It sounds like they are really pushing toward a holistic view where multiple observables combine to constrain the black hole's mass, spin, and inclination simultaneously.

Jocelyn: And they suggest these joint measurements could potentially test models of how black holes grow, looking at whether accretion is coherent or incoherent based on those probability distributions.

Subrahmanyan: That testing of growth history models through the resulting spin alignment is where the big theoretical payoff lies, connecting observation directly to evolutionary pathways in cosmic structure formation.

Vera: To wrap up this discussion on "Ring Position Angles and Spin in M87* and Sgr A*," we see that a one and PA1 are powerful tools for probing black hole properties using GRMHD simulations.

Jocelyn: The work shows how these observables allow us to move beyond just looking at the ring shape toward understanding the underlying physics of spin and orientation in these massive systems.

Subrahmanyan: Ultimately, this paper reinforces that empirical data from EHT can provide independent evidence regarding the alignment of black hole spin vectors with large-scale structures like jet axes.

Vera: It’s a lot to process, but it really shows how much deeper we can go by combining sophisticated modeling with high-quality observational data from sources like M87 and Sgr A*.

Jocelyn: I think the future work outlined for things like BHEX is where the real excitement is for us as observers, because it opens up a whole new set of parameters to measure.

Subrahmanyan: Indeed, those future observations should improve these constraints so we can robustly determine black hole mass, spin, and inclination with greater confidence in the models.

The paper's summary: Vera: So, to wrap up what we just heard, this paper is essentially saying that by tracking the precise angle of brightness asymmetries in M87* and Sgr A*, astronomers can start making real measurements about how fast these black holes are spinning and which direction they're tilted.

Jocelyn: I think that makes sense from an observational standpoint; we’ve been looking at the light, but now we have a specific angular measurement, PA1, that seems to be directly tied to the spin axis.

Subrahmanyan: Exactly. This isn't just about pretty pictures; it's about using these ring features as empirical data points to test the complex physics of accretion flows and general relativity in extreme gravity environments.

Vera: Right, and the authors show that they can use their computer models, those GRMHD simulations, to see exactly how a black hole’s spin affects that angle, a one and PA1.

Jocelyn: And what I find interesting is how they use these synthetic datasets to rule out certain physical scenarios, like low-magnitude spins or spins pointing directly at us.

Subrahmanyan: That level of constraint is what really connects the theory to the observation; it gives us concrete limits on the possible solutions for these black holes.

Vera: Plus, they're looking at how PA1 changes over time in M87, which seems to give them a way to figure out if the black hole is spinning prograde or retrograde.

Jocelyn: That sounds like a very precise way to determine the angular momentum direction, which is vital for understanding how matter spirals into these systems.

Subrahmanyan: It's a direct probe of the accretion disk's angular momentum transport mechanism, which is something we struggle to model accurately otherwise.

Vera: And for Sgr A*, they suggest that even with lower confidence right now, this approach could provide some initial constraints on the spin vector and its direction within our own galaxy.

Jocelyn: It’s a long shot right now because of the uncertainty, but if they can nail down those parameters, it opens up a new way to map the magnetic field structure around our center.

Subrahmanyan: That connection between the black hole's spin and the galactic center's structure is very important for understanding how large-scale magnetic fields influence everything in our solar neighborhood.

Vera: Looking toward the future, they are pointing toward next-generation telescopes like a Black Hole Explorer satellite that could measure even more observables across different sources.

Jocelyn: That sounds like a massive step forward because it means we could get three different types of measurements—diameter, magnitude, and position angle—all at once.

Subrahmanyan: That multi-observable approach is where the real power comes from; combining those pieces allows for much richer parameter inference about the black hole's growth history.

Vera: So, it seems this paper is laying down a framework where we use the geometric shape of these images to build a more complete picture of black hole spin and orientation.

Jocelyn: It feels like we’re moving from just looking at what's there to actually measuring the fundamental properties that govern how these objects behave dynamically.

Subrahmanyan: That empirical foundation is what will allow us to test our most ambitious theoretical models concerning accretion and jet physics in a new, robust way.

The paper's improvements: Vera: So, we just covered how using brightness asymmetry position angles helps constrain black hole spin and orientation in M87* and Sgr A*. Now, let's talk about what the authors suggest we can do next to make this analysis even better.

Jocelyn: I think the paper points toward combining these positional measurements with other things, like ring diameter or perhaps observing how PA1 evolves over time more rigorously.

Subrahmanyan: That makes sense; they’re suggesting that moving from a single observation to a joint measurement of multiple observables will give us much tighter constraints on the system's parameters.

Vera: They’re proposing this concept of "multi-observable fusion," where you don't just look at one feature, but combine the ring diameter, the asymmetry magnitude a one and that position angle PA1 to constrain mass, spin, and inclination all at once.

Jocelyn: That sounds incredibly powerful for future observations because it means we can get a much more complete characterization of these black holes in a single measurement campaign.

Subrahmanyan: From a theoretical perspective, that holistic approach is what’s needed to test complex models of accretion history, which we need to understand how these black holes grew over cosmic time.

Vera: And they're also looking forward to future EHT expansions like the Black Hole Explorer satellite, which will allow us to measure three key observables for sources beyond M87 and Sgr A*.

Jocelyn: That’s exciting because it means we could start getting these constraints on other black holes in the universe, moving beyond just our two closest examples.

Subrahmanyan: That expansion is vital because it lets us build a population of constraints, which is necessary to understand if black hole growth follows coherent or incoherent processes.

Vera: The paper also mentions that these joint measurements could help us probe different growth histories by looking at how the spin aligns with the surrounding galactic structure.

Jocelyn: That’s a huge implication; it links the physics happening right at the event horizon to the large-scale dynamics of our galaxy itself.

Subrahmanyan: If we can show a correlation between those observables and different growth scenarios, it provides a direct observational test for theoretical models about how matter falls onto these massive objects.

Vera: It sounds like they are really pushing us toward a new standard for how we analyze EHT data, moving away from just single-parameter fits to more comprehensive modeling.

Jocelyn: I'm optimistic that this direction will lead to much more detailed maps of the magnetic field structures around these galactic centers.

Subrahmanyan: Indeed, providing these robust constraints on spin alignment is a crucial piece for linking the local environment we observe with the larger cosmological models of galaxy evolution.

Conclusion: Vera: So, to wrap up our discussion on "Ring Position Angles and Spin in M87* and Sgr A*," we've seen how this paper uses EHT data to constrain the spin and orientation of these massive black holes through detailed GRMHD modeling.

Jocelyn: It really shows that the geometry of those ring asymmetries, specifically PA1, is a direct window into the underlying physics governing accretion flow dynamics near the event horizon.

Subrahmanyan: This work provides empirical constraints on general relativistic magnetohydrodynamics by linking observable image features to fundamental parameters like spin and angular momentum direction.

Vera: We've learned that combining brightness asymmetry magnitude with position angle gives us a statistically significant way to narrow down those critical black hole properties in M87* and Sgr A*.

Jocelyn: It’s exciting because it shows how observational data, when fed into sophisticated AI models like the one described, can yield these kinds of physical constraints that were previously very difficult to isolate.

Subrahmanyan: The impact here is that we're getting empirical evidence on how spin alignment relates to jet axis dynamics and accretion flow structure across different black hole systems.

Vera: We’ve also seen the potential for future work, specifically using next-generation observatories like the Black Hole Explorer to measure even more observables on sources beyond M87 and Sgr A*.

Jocelyn: That future work sounds like it could open up a whole new class of constraints, allowing us to map out a larger sample of black holes in the universe.

Subrahmanyan: Building that larger sample is essential for testing how black hole growth histories unfold, which is where the real theoretical payoff lies.

Vera: Overall, this study underscores how crucial it is to use these detailed geometric analyses to move beyond just seeing a pretty ring and start understanding the actual physical state of the black hole.

Jocelyn: It's a great example of how observational astronomy and advanced simulation work together to build that picture.

Subrahmanyan: We’re really getting closer to tying the physics of accretion directly into observable phenomena through these kinds of detailed analyses on M87* and Sgr A*.

Vera: That covers what we've discussed about the paper, "Ring Position Angles and Spin in M87* and Sgr A*," which is a fantastic piece of work.

Jocelyn: It’s really impressive how they used those synthetic GRMHD libraries to test their geometric models against the real EHT data.

Subrahmanyan: The constraints they derived on spin vectors and angular momentum direction are very meaningful because they directly inform our models of jet launching and accretion processes in strong gravity.

Vera: I think what’s most important is the pathway for future work, especially how those joint measurements will help us characterize black holes across a wider range of sources using new EHT instruments.

Jocelyn: It feels like the next big step is moving toward that holistic characterization, where we get mass, spin, and inclination all at once.

Subrahmanyan: That comprehensive approach is exactly what's needed to robustly test theories about how black holes grow over cosmic time and interact with their environment.

Department of Astronomy, University of Illinois at Urbana-Champaign · Illinois Center for the Advanced Study of the Universe, University of Illinois at Urbana-Champaign · Steward Observatory and Department of Astronomy, University of Arizona · Center for Astrophysics | Harvard & Smithsonian · Black Hole Initiative at Harvard University · NCSA, University of Illinois at Urbana-Champaign

astro-ph.HE

Submitted: 2026-06-09

Updated: 2026-09-30

Comments: Published in the Open Journal of Astrophysics (15 pages, 9 figures, 1 table)

Journal ref: The Open Journal of Astrophysics 9 (October), 2026

DOI: 10.33232/001c.172040

License: http://creativecommons.org/licenses/by/4.0/

Importance score: 80/100

The gist: Event Horizon Telescope (EHT) images of black holes appear as rings with a brightness asymmetry, and this study expands on analyzing the position angle of this peak brightness asymmetry to constrain

Key concepts

Brightness Asymmetry Magnitude (a1): This is a key observable derived from EHT images, representing the amplitude of the asymmetry in the ring structure. It corresponds to the amplitude of a fitted m=1 ring component in geometric models. This measurement is crucial for constraining black hole spin and inclination by fitting synthetic data.
Position Angle (PA1): The position angle of this brightness asymmetry indicates its phase or orientation within the image. Analyzing PA1 helps constrain the black hole's spin vector direction and disk angular momentum direction. It provides evidence regarding the alignment between the spin vector and other features like the jet axis.
GRMHD Models (Illinois v5): These are sophisticated computer simulations based on general relativistic magnetohydrodynamics used to generate synthetic EHT data. They simulate accretion flows in different magnetic modes (MAD/SANE) and black hole spins. These models allow researchers to test how different physical conditions affect the observed image features.
Prograde/Retrograde Motion: This describes the direction of a black hole's spin relative to the direction of its accretion disk's angular momentum. By analyzing PA1 dynamics, researchers can constrain whether M87 is prograde or retrograde with high accuracy, which helps determine the spin vector and disk angular momentum.

Terminology

Event Horizon Telescope — 31× in this paper
Alignment — 16× in this paper · explained in 1 episode
Accuracy — 8× in this paper · explained in 1 episode
Accretion Flows — 2× in this paper · explained in 1 episode
Angular Momentum Transport — 2× in this paper · explained in 3 episodes
Anisotropy — 2× in this paper · explained in 3 episodes
Bayesian Inference — 2× in this paper · explained in 5 episodes
Consistency — 2× in this paper · explained in 3 episodes
Accretion Physics — 1× in this paper · explained in 2 episodes
Degeneracy — 1× in this paper · explained in 3 episodes
Gravitational Lensing — 1× in this paper · explained in 2 episodes
Physical Constraints — 1× in this paper · explained in 7 episodes
Robustness — 1× in this paper · explained in 5 episodes

Summary

Event Horizon Telescope (EHT) images of black holes appear as rings with a brightness asymmetry, and this study expands on analyzing the position angle of this peak brightness asymmetry to constrain black hole spin and orientation in M87 and Sgr A.

How it works

The analysis relies on comparing EHT data with a library of synthetic data generated using general relativistic magnetohydrodynamic (GRMHD) models, specifically the Illinois v5 library. This library spans five parameters: magnetization mode (MAD/SANE), black hole spin a∗, viewing inclination i, and electron temperature parameters Rhigh and Rlow. The simulation uses KHARMA to evolve the accretion flow in either standard (SANE) or magnetically arrested (MAD) modes, and ipole for radiative transfer.

The measurement technique involves fitting a geometric model to the image data using the VIDA package (for divergence minimization) or Comrade (for Bayesian inference). The model assumes an m-ring truncated at m=4 with a Gaussian background component, where total intensity is modeled as Itot = Iring + Ibg. The key observables extracted are the brightness asymmetry magnitude a1 and its position angle PA1, which correspond to the amplitude and phase of the fitted m=1 ring component.

Key Findings on Spin Constraints

The study demonstrates that for larger spin magnitudes (a∗ > 0 and a∗ ≲ −0.5), the mean PA1 falls within 1σ of the approaching limb of the black hole, regardless of viewing inclination, disk magnetization, or source. By comparing the (a1,PA1) distribution in M87 observations with models, researchers show that they can mildly disfavor low-magnitude spins and strongly disfavor all spin vectors that point toward Earth. Furthermore, the alignment of PA1 relative to the large-scale jet axis may suggest that M87’s disk does not have a large tilt.

Position Angle Dynamics and Prograde/Retrograde Constraints

The analysis of PA1 dynamics for M87 shows that PA1 evolves stochastically around a mean value µ, described by a circular Gaussian distribution with a correlation timescale τcorr(PA1) = 133 tg. The study suggests that m-ring dynamics constrain the sign of cosi. By combining PA1 with the pattern speed measured in optimistic 2026 M87 video conditions, EHT can constrain whether M87 is prograde or retrograde with ∼ 84% accuracy. This constraint is achieved by constraining both the spin vector direction (ispin) and the disk angular momentum direction (idisks).

Constraints on Sgr A

For Sgr A, a detection of (a1,PA1) could constrain the magnitude and direction of the galactic center spin vector. The analysis shows that EHT data is beginning to constrain (a1,PA1) with high uncertainty. In M87, PA1 provides evidence for coaxiality between the spin vector and the large-scale jet axis, suggesting a small tilt in the accretion disk. For Sgr A, PA1 could potentially provide an independent avenue for constraining the galactic center jet axis direction based on predicted relationships between PA1 and PAjet.

Future Applications

The paper outlines that future EHT expansions, such as the Black Hole Explorer (BHEX) satellite, could enable horizon-scale asymmetry analysis for sources beyond M87 and Sgr A. For these new sources, three total intensity ring observables—ring angular diameter (to constrain M/D), brightness asymmetry magnitude (to constrain spin and inclination), and brightness asymmetry position angle (to constrain the spin vector position angle)—would be simple to measure. Joint measurements of these observables could enable further parameter inference, potentially constraining black hole growth history by testing models of coherent, incoherent, or hierarchical accretion. The study concludes that Future EHT observations should improve these constraints to robustly determine black hole mass, spin, and inclination.

Uncertainties in Analysis

The analysis acknowledges several sources of uncertainty: boundary and initial conditions (e.g., the choice between MAD/SANE models), collisionless dynamics (ideal fluid assumption), thermodynamics and electron energization (e.g., using different adiabatic indices γi), mass density scaling, and the fast-light approximation in radiative transfer. Measurement error due to limited (u, v) coverage is also noted as a factor that could increase uncertainty for other sources. The analysis suggests that Joint measurements of (a1,PA1) may offer insight into black hole growth, as different growth histories predict different probability distributions for black hole spin magnitudes and spin alignment with the surrounding galactic structure. This work shows that "PA1 provides independent evidence that the M87 spin vector is relatively aligned with the jet axis, i.e. that the disk has little tilt.

Improvements for AI systems

As a fastidious and diligent researcher, I have analyzed the provided scientific paper, RING POSITION ANGLES AND SPIN IN M87∗ AND Sgr A∗, focusing on its methodology, model constraints, and future implications for AI system development.

The primary improvements for AI systems stem from leveraging the paper's sophisticated modeling techniques—specifically General Relativistic Magnetohydrodynamics (GRMHD) simulations and Bayesian inference on EHT data—to enhance physical understanding, constraint generation, and predictive capability in astrophysical datasets.

Here are the specific improvements to AI systems based on this research:

)1. Improved Astrophysical Constraint Engines (Spin & Inclination Inference):

The paper demonstrates that combining brightness asymmetry magnitude and position angle (a1, PA1) allows for statistically significant constraints on black hole spin and inclination (Section 4.1).

AI System Improvement: Develop a machine learning pipeline trained on GRMHD synthetic data to perform rapid inference of black hole parameters.
Specific Capabilities: The AI can ingest raw EHT visibility data (or simulated noisy data) and output the most probable spin vector orientation and magnitude, including a quantifiable confidence interval (e.g., Spin is prograde with 84% confidence). This directly replaces or augments traditional statistical fitting methods like the KS test and Fisher's method used in the paper.

)2. Enhanced Source Characterization via Multi-Observable Fusion:

The paper highlights that combining observables—such as ring diameter, asymmetry magnitude (a1), and position angle (PA1)—allows for robust constraints on mass, spin, and inclination for future sources beyond M87/Sgr A∗ (Section 5.1).

AI System Improvement: Create a Joint Constraint Predictor that learns the functional relationships between multiple physical observables derived from GRMHD models.
Specific Capabilities: When presented with new EHT data from a potential source, the AI can predict not just one parameter (like spin) but a correlated set of constraints across mass, spin, and inclination simultaneously. This moves beyond single-observable fitting to holistic source characterization.

)3. Predictive Modeling for Jet Dynamics and Growth History:

The analysis links PA1 dynamics to the pattern speed (omegap), which constrains whether the black hole is prograde or retrograde, thereby constraining the Blandford-Znajek jet launching mechanism (Section 4.2). Furthermore, spin alignment influences black hole growth history (Section 5.2).

AI System Improvement: Build a simulation surrogate model that maps accretion flow parameters to observable PA1 dynamics and jet characteristics.
Specific Capabilities: The AI can predict the likely dynamical state of an EHT source (e.g., Source X is likely prograde or Source Y exhibits coherent PA1 rotation indicative of specific near-horizon physics) based on its measured asymmetry features, allowing for rapid testing of growth history hypotheses (coherent vs. incoherent accretion).

)4. Robust Uncertainty Quantification in Model Comparison:

The paper explicitly details the three major sources of uncertainty in GRMHD simulations (boundary conditions, collisionless dynamics, and thermodynamics/electron energization) and how they affect PA1 results (Section 5.3).

AI System Improvement: Implement an uncertainty-aware inference framework that incorporates model systematic errors directly into parameter estimation.
Specific Capabilities: When a result is queried, the AI will provide not just a best estimate, but also a quantified uncertainty budget detailing how much the inferred spin constraint depends on assumptions about the plasma's adiabatic index (γi) or whether kinetic vs. ideal fluid effects are dominant. This prevents over-reliance on model assumptions and allows researchers to assess the robustness of their own findings.

)5. Automated Jet Axis and Disk Tilt Analysis:

The paper uses PA1 relative to the jet axis (PAjet) to infer constraints on disk tilt (Section 5).

AI System Improvement: Develop a classifier that analyzes the angular relationship between measured asymmetry features and predicted jet axes to detect subtle tilts in accretion disks.
Specific Capabilities: The AI can assess whether the observed PA1 deviation from the expected PA1 ≈ PAspin + 90◦ suggests a significant disk tilt, which is critical for understanding how magnetic fields interact with rotating matter near the event horizon.

Abstract

Event Horizon Telescope (EHT) images of black holes appear as rings with a brightness asymmetry. Here, we expand on our previous study of the asymmetry magnitude a 1 to study the position angle of the peak brightness asymmetry PA 1 in general relativistic magnetohydrodynamic (GRMHD) models. For larger spin magnitudes (a*>0 and a* -0.5), the mean PA 1 falls within 1σ of the approaching limb of the black hole, regardless of viewing inclination, disk magnetization, or source. By comparing the (a 1, PA 1) distribution in M87* observations with models, we demonstrate that we can mildly disfavor low-magnitude spins and strongly disfavor all spin vectors that point toward Earth. The alignment of PA 1 relative to the large-scale jet axis may suggest that M87*'s disk does not have a large tilt. By combining PA 1 with the pattern speed measured in optimistic 2026 M87* video conditions, the EHT can constrain whether M87* is prograde or retrograde with about 84% accuracy. In Sgr A*, we show that a detection of (a 1, PA 1) could constrain the magnitude and direction of the galactic center spin vector. Finally, if future EHT expansions increase the sample of horizon-scale sources, a simple set of observables (ring diameter, asymmetry magnitude, and asymmetry angle) could enable robust constraints on black hole mass, spin, and inclination.