Multi-messenger astrophysics

In this episode, we dive into a groundbreaking discovery made with the **MeerKAT radio telescope**: a massive, symmetric **"bow-tie" shaped radio structure** surrounding the black hole system **V4641 Sgr**. While this microquasar has been known since 1999 for its erratic outbursts and superluminal jets, this new research reveals the long-term impact these black holes have on their galactic neighborhoods, stretching across nearly **35 parsecs (about 114 light-years)** of space.**Key Topics Discussed:*** **The System:** V4641 Sgr is a low-mass X-ray binary (LMXB) featuring a **6.4 solar mass black hole** and a B-type stellar companion. It is famous for its "superluminal" jets that appear to move faster than the speed of light due to their orientation and velocity.* **The "Bow-Tie" Discovery:** Using deep imaging techniques, astronomers found a faint, diffuse radio structure that mirrors the size and position of extended X-ray emission recently detected by the XRISM satellite.* **Particle Acceleration:** The sources suggest the radio and X-ray emission are likely caused by **synchrotron radiation**. This implies that electrons are being accelerated to energies of **more than 100 TeV**—even tens of parsecs away from the central black hole.* **The Proper Motion Mystery:** Interestingly, the black hole is slightly offset from the center of the bow-tie. The researchers explain this through the **proper motion of the system**; by tracing the black hole's path backward, they estimate it was at the center of this structure roughly **10,000 years ago**.* **The Gamma-Ray Disconnect:** While large-scale gamma-ray "bubbles" have also been detected around this system, they are oriented differently and are much larger than the radio bow-tie. We explore why these different "colors" of light reveal different chapters of the black hole's history.**Why This Matters:**This discovery adds V4641 Sgr to a growing list of **"microquasars"**—stellar-mass black holes that act as smaller-scale analogs to the supermassive black holes found in the centers of galaxies. It reinforces the idea that these systems are significant contributors to **galactic cosmic rays** and powerful drivers of change in the interstellar medium.***### **Reference**Grollimund, N., Corbel, S., Fender, R., et al. (2026). **"Large-scale radio bubbles around the black hole transient V4641 Sgr."** *Astronomy & Astrophysics*, manuscript no. aa57124-25.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: N. Grollimund et al.

In this episode, we dive into a groundbreaking discovery in high-energy astrophysics: the detection of the blazar PKS 0346−27 at a redshift of $z = 0.991$. This makes it one of the most distant objects ever detected in very-high-energy (VHE) gamma-rays ($E > 100$ GeV). We explore how the H.E.S.S. (High Energy Stereoscopic System) telescopes in Namibia managed to capture this elusive signal despite the thick "fog" of Extragalactic Background Light (EBL) that usually absorbs such distant photons.Key Discussion Points:The Record-Breaking Detection: Why reaching a redshift of approximately 1 is a major milestone for gamma-ray astronomy and what it tells us about the evolution of the universe.A Tale of Two Flares: The strange two-day delay between the high-energy flare caught by the Fermi-LAT satellite and the very-high-energy flare detected by H.E.S.S..The Physics of the Jet: We break down the debate between leptonic and hadronic models. While electrons are the usual suspects, the data from PKS 0346−27 strongly favors a proton-synchrotron model, even though it requires jet power that temporarily exceeds the source’s Eddington limit.Multi-Wavelength Cooperation: How a global team used data from H.E.S.S., Fermi-LAT, the Swift Observatory, and the ATOM telescope to build a complete picture of this cosmic event.The "Synchrotron Mirror" Hypothesis: Exploring how stationary clouds near the black hole might be reflecting radiation back into the jet to create "orphan" VHE flares.Technical Insight: The researchers found that a traditional leptonic model (based on electrons) would require "implausible" parameters, such as a Doppler factor exceeding 80, to explain the flare. This push toward hadronic models suggests that relativistic protons may play a much larger role in the most powerful jets in the universe than previously confirmed.Featured Article: H.E.S.S. Collaboration, et al. (2026). "H.E.S.S. detection and multi-wavelength study of the $z \sim 1$ blazar PKS 0346−27." Astronomy & Astrophysics manuscript no. 0346.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Stefan Schwarzburg

In this episode, we dive into a groundbreaking discovery from the **Large High Altitude Air Shower Observatory (LHAASO)**. For decades, the microquasar **Cygnus X-3** has been "an astronomical puzzle," but new data has finally confirmed its status as a **Super PeVatron**—a cosmic engine capable of accelerating protons to tens of petaelectronvolt (PeV) energies. **Key Discussion Points:** **The Iconic Microquasar:** Cygnus X-3 is a unique high-mass X-ray binary consisting of a compact object (a black hole or neutron star) and a massive **Wolf–Rayet donor star**. It features a relativistic jet and a remarkably short 4.8-hour orbital period. **Breaking the Energy Barrier:** LHAASO detected variable gamma-rays reaching up to **3.7 PeV**, the highest-energy photons ever recorded from such an astrophysical source. **The Hardest Spectrum:** The source exhibits the **hardest ultra-high-energy (UHE) spectrum** ever detected by LHAASO, with a distinct "hump" or spectral hardening around 1 PeV.**Protons vs. Electrons:** While lower-energy GeV gamma-rays are often produced by electrons, researchers explain that **leptonic origins are robustly excluded** for these PeV emissions due to intense synchrotron cooling. Instead, the signal likely comes from **photomeson processes**, where protons accelerated in the jet collide with the dense ultraviolet and X-ray photon fields of the binary system.**Temporal Puzzles:** We discuss the **month-scale variability** of the signal and the 3.2$\sigma$ evidence for orbital modulation, which strongly suggests the PeV radiation is born deep within the innermost regions of the jet.The Big Picture:This discovery provides the first compelling evidence that a microquasar can act as a **super-PeVatron**, generating transient PeV gamma-ray emission in close proximity to the central engine. This shifts our understanding of how cosmic rays are accelerated within our own galaxy.### Article Reference**Title:** *Cygnus X-3: A variable petaelectronvolt gamma-ray source***Authors:** The LHAASO Collaboration**Journal:** *National Science Review (NSR)***Source PDF:** 2512.16638v1.pdfAcknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: LHAASO Collaboration

In this episode, we dive into the cutting-edge world of multi-messenger astronomy. We explore how scientists are using a global network of specialized telescopes to solve one of the greatest mysteries in physics: the origin of high-energy cosmic rays. By tracking "ghost particles" called neutrinos from the depths of the South Pole to the highest mountain peaks where gamma-ray telescopes wait, researchers are building a new map of the most violent processes in our universe.Key Discussion Points:What are Neutrinos? Learn why these secondary particles are the "smoking gun" signature of hadronic acceleration processes in space.The Multi-Messenger Approach: Why detecting neutrinos alone isn't enough and how simultaneous observations of very-high-energy (VHE) gamma-rays help pinpoint source locations.The IceCube-IACT Partnership: A look at how the IceCube Neutrino Observatory at the South Pole coordinates with the "Big Four" imaging atmospheric Cherenkov telescopes—FACT, H.E.S.S., MAGIC, and VERITAS—to react to cosmic alerts in real-time.Target-of-Opportunity (ToO) Programs: How telescopes automatically repoint within seconds or minutes to catch a glimpse of a neutrino’s source.Case Studies & Legacy Results: We review the famous coincidence of the blazar TXS 0506+056 and discuss the latest findings from follow-up observations conducted between 2017 and 2021.The Future of the Hunt: What the next generation of detectors, like IceCube-Gen2 and the Cherenkov Telescope Array Observatory (CTAO), will mean for the next decade of discovery.Featured Reference:FACT, H.E.S.S., MAGIC, VERITAS, Fermi-LAT, and IceCube Collaborations. (2025). Prompt Searches for Very-High-Energy $\gamma$-Ray Counterparts to IceCube Astrophysical Neutrino Alerts. Accepted at the Astrophysical Journal, arXiv: https://arxiv.org/abs/2512.16562Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: IceCube/NASA

Classical novae, thermonuclear eruptions on the surface of a white dwarf in a binary system, are known sources of high-energy gamma-rays detected by the Fermi-LAT. This episode explores a multi-wavelength analysis of two recent novae, **V1723 Sco 2024** and **V6598 Sgr 2023**, aiming to constrain the mechanism behind this intense gamma-ray emission.**V1723 Sco** proved to be a very bright gamma-ray source, with emission lasting 15 days, allowing scientists to constrain the total energy and spectral properties of accelerated protons. Intriguingly, V1723 Sco also showed unexpected gamma-ray and thermal hard X-ray emission more than 40 days after its initial outburst, suggesting that particle acceleration can occur even several weeks post-eruption.In contrast, **V6598 Sgr** was detected by Fermi-LAT for only two days, marking one of the shortest gamma-ray emission durations ever recorded for a classical nova. Its brief gamma-ray signal coincided with a rapid decline in optical brightness. V6598 Sgr also exhibits peculiar characteristics, including no significant gamma-ray emission below 1 GeV and the possibility that it is an Intermediate Polar (IP) system, which may hint at a different particle acceleration region due to potentially strong magnetic fields.The detailed analysis, which combined Fermi-LAT data with optical (AAVSO) and X-ray (NuSTAR) observations, strongly supports the hypothesis that the gamma-ray generation in both novae is more consistent with the **hadronic scenario** (involving accelerated protons) than the leptonic scenario. However, the long-standing challenge remains: no non-thermal X-ray emission has been detected simultaneously with the gamma-rays.**Article Reference:**Fauverge, P., Jean, P., Sokolovsky, K., et al. (2025). *Fermi-LAT detections of the classical novae V1723 Sco and V6598 Sgr in a multi-wavelength context.* submitted to Astronomy & Astrophysics, arXiv: 2512.14198Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: NASA's Goddard Space Flight Center/S. Wiessinger