Multi-messenger astrophysics

In this episode, we explore the dynamic and violent universe revealed by the STONKS pipeline (Search for Transient Object in New observations using Known Sources). While the name might remind you of internet finance memes, this system is a serious tool for the XMM-Newton space telescope. We discuss how researchers are using STONKS to detect long-term X-ray transients in the Galactic plane that are too faint for standard wide-field survey instruments to see.Join us as we break down the first results from a multi-year survey of the Galaxy, identifying 70 astrophysical sources that change in brightness over time. From waking magnetars to flaring stars, we look at what these faint signals tell us about the most extreme physical environments in the cosmos.Key Topics Discussed:What is STONKS? A near-real-time detection system that compares new XMM-Newton observations against archival data to spot variability.The Advantage: Unlike survey missions (like Swift or eROSITA), STONKS utilizes long exposure times to find variable sources at fluxes several orders of magnitude lower than other systems.Major Discoveries:A Magnetar Candidate: The detection of a potential magnetar (4XMM J175136.9-275858) caught at the onset of a massive outburst, increasing in brightness by nearly two orders of magnitude.Exotic Stars: The identification of a $\gamma$-Cas analogue (HD 162718) and new candidates for Cataclysmic Variables (CVs).New Detections: Of the 70 sources analyzed, 23 were detected in X-rays for the very first time.The Future: How systematic analysis of archival data is opening a new window into stellar evolution and compact objects like black holes and neutron stars.Reference Material"STONKS first results: Long-term transients in the XMM-Newton Galactic plane survey", Robbie Webbe, E. Quintin, N. A. Webb, Gabriele Ponti, Tong Bao, Chandreyee Maitra, Shifra Mandel, Samaresh Mondal, Astronomy & Astrophysics manuscript no. aa57789-25, January 28, 2026.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: ESA

In this episode, we explore the **Wide-field Spectroscopic Telescope (WST)**, a proposed 12-meter class facility that aims to revolutionize our understanding of the cosmos in the 2030s and 2040s. While imaging surveys like LSST and Euclid provide a "video" of the sky, the WST provides the physical "voice" needed to interpret those images through high-speed, massive-scale spectroscopy.**Key Topics Covered:*** **The Technological Leap:** Discover how the WST’s unique design allows for **simultaneous Multi-Object Spectroscopy (MOS) and Integral Field Spectroscopy (IFS)**, featuring a 12-meter aperture and a massive 3.1 square degree field of view.* **The "Spectroscopic Alert" Era:** How the WST will close the gap between millions of nightly photometric alerts and our limited capacity to follow them up, turning spectroscopy into a primary discovery tool for supernovae, exocomets, and binary black holes.* **Mapping the Milky Way:** Learn how "chemical tagging" will allow astronomers to reconstruct the history of our galaxy by analyzing the chemical fingerprints of millions of stars.* **Cosmology and the Cosmic Web:** Exploring the "Dark Universe," from measuring the mass of neutrinos to charting the expansion of the universe using the 3D topology of the Lyman-alpha forest.* **Multi-Messenger Synergies:** How the WST will work alongside gravitational wave detectors (LISA, Einstein Telescope) and neutrino observatories (IceCube-Gen2) to pinpoint the most violent events in the universe.**Featured Reference:**1. **Mainieri, V., Anderson, R. I., Brinchmann, J., et al. (2024). *The Wide-field Spectroscopic Telescope (WST) Science White Paper*.** This foundational document provides a comprehensive overview of the facility's **12-meter aperture**, its unique simultaneous **Multi-Object Spectroscopy (MOS) and Integral Field Spectroscopy (IFS)** capabilities, and its broad science cases ranging from cosmology to Galactic archaeology.2. **Melo, A., Sanchez-Saez, P., Ivanov, V. D., et al. (2025). *Spectroscopic Alerts for the Time-Domain Era*.** This article introduces the paradigm-shifting concept of **"Spectroscopic Alerts,"** which are real-time notifications triggered by physical changes in a source's spectrum, allowing the WST to act as a primary **discovery instrument** for transient phenomena.3. **Schüssler, F., Bisero, S., Cornejo, B., et al. (2026). *Multi-Messenger Studies with High-Energy Neutrinos and Gamma Rays: The WST Opportunity*.** This reference highlights the WST's role in **multi-messenger astrophysics**, specifically its ability to rapidly survey large sky areas to classify the electromagnetic counterparts of **high-energy neutrinos** and very-high-energy **gamma rays**.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: G.Gausachs/WST

In this episode, we dive into the fascinating discovery of **GRB 180728A**, one of the nearest and most energetic long-duration gamma-ray bursts ever recorded at a low redshift. While most nearby bursts are low-energy events, this explosion released a massive **$2.5 \times 10^{51}$ erg of isotropic energy**, placing it in a rare class of cosmological powerhouses found right in our relative "backyard". We explore the detailed analysis of its associated supernova, **SN 2018fip**, and what it reveals about the complex nature of stellar collapses.**Key Topics Covered:*** **A Rare High-Energy Event:** Learn why GRB 180728A is significant, sitting at a redshift of **z = 0.1171** and ranking as one of the most energetic nearby bursts after the famous GRB 030329 and the record-breaking "BOAT" (GRB 221009A).* **The Supernova Mystery:** Despite the high energy of the gamma-ray burst itself, the associated supernova SN 2018fip was **intrinsically fainter** than many typical events, showing that the energy of a burst doesn't always correlate with the brightness of its supernova.* **The Shape of the Blast:** Discover why researchers believe this wasn't a simple spherical explosion. The sources suggest a **two-component ejecta** model: a narrow, high-velocity component (> 20,000 km/s) and a slower, more massive inner component.* **The Neighborhood:** We take a look at the **host galaxy**—a low-mass, blue, star-forming irregular dwarf galaxy typical for these types of cosmic events.* **Advanced Observations:** Insights into how astronomers used instruments like the **X-shooter** on the Very Large Telescope to track the explosion for 80 days.**Featured Reference:**Rossi, A., Izzo, L., Maeda, K., et al. (2026). **"GRB 180728A and SN 2018fip: the nearest high-energy cosmological gamma-ray burst with an associated supernova."** *Astronomy & Astrophysics*.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Anna Serena Esposito

In this episode, we dive into a groundbreaking discovery that may have revealed a brand-new category of cosmic explosion: the Superkilonova. On August 18, 2025, gravitational-wave detectors picked up a signal, S250818k, indicating a merger between two neutron stars—but with a twist. The estimated "chirp mass" was surprisingly low, suggesting that at least one of the objects was below the mass of our Sun, a finding that challenges standard models of stellar evolution.The Optical Mystery:The Zwicky Transient Facility (ZTF) quickly identified a matching optical transient, AT2025ulz, in the same region. While its first week of behavior looked like a classic "kilonova" (the expected glow from a neutron star merger), it soon evolved into something much more complex. Spectroscopic and photometric data eventually showed it was most similar to a Type IIb stripped-envelope supernova, which is the explosion of a massive star that has lost most of its outer hydrogen.The Superkilonova Theory:How can an event be both a neutron star merger and a supernova? The researchers explore a fascinating theoretical model known as a Superkilonova. In this scenario, a rapidly spinning massive star collapses, and its core either fissions into two pieces or its surrounding disk fragments into subsolar-mass neutron stars. These fragments then merge almost immediately inside the supernova explosion. Key Highlights:A "Veritable Symphony": The potential for a single event to produce gravitational waves from a merger while simultaneously displaying the light of a core-collapse supernova.New Stellar Pathways: If confirmed, this proves that neutron stars can form via accretion-disk fragmentation, or it might even be evidence of primordial black holes.Multimessenger Challenges: Why scientists need more than just light to solve these puzzles, relying instead on a "panchromatic dataset" including X-rays, radio waves, and gravitational strain.Article ReferenceKasliwal, M. M., et al. (2025). "ZTF25abjmnps (AT2025ulz) and S250818k: A Candidate Superkilonova from a Subthreshold Subsolar Gravitational-wave Trigger." The Astrophysical Journal Letters, 995:L59 (18pp).Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Caltech/K. Miller and R. Hurt (IPAC)

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

Join us as we explore the remarkable cosmic event, **GRB 250314A**, an exploding star detected deep within the early Universe. This long gamma-ray burst (LGRB), observed by the SVOM satellite, was spectroscopically measured at a redshift of approximately **$z \approx 7.3$**, meaning it occurred when the Universe was only about 5% of its current age, placing it firmly in the era of reionization.The observation campaign was critical, identifying the GRB as a classical long (Type II) event, consistent with the explosion of a rare massive star. Initial ground-based follow-up, triggered by the SVOM detection, led to the discovery of the near-infrared afterglow and the crucial redshift measurement via the Lyman-$\alpha$ break observed using the VLT/X-shooter.The investigation reached a major milestone when **JWST/NIRCAM** observations were obtained, revealing both the faint, blue host galaxy and the likely presence of an associated **Supernova (SN)**. Researchers found that the luminosity and spectral shape of this ancient SN are strikingly similar to **SN 1998bw**, the canonical GRB SN prototype observed locally.This similarity is profound, suggesting that despite the vast differences in physical conditions in the early Universe, the massive star that created GRB 250314A was not significantly more massive than local progenitors, implying a surprisingly limited scope for evolution in GRB and SN properties across much of cosmic history. Studying such events is key to exploring star formation and chemically characterizing the interstellar medium in the highest-redshift galaxies.***### Reference Articles* **Cordier, B., et al. (2025). SVOM GRB 250314A at $z \approx 7.3$: An exploding star in the era of re-ionization.** *Astronomy & Astrophysics, 704, L7*.* **Levan, A. J., et al. (2025). JWST reveals a supernova following a gamma-ray burst at $z \approx 7.3$.** *Astronomy & Astrophysics, 704, L8*.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: CNSA/CNES

The rapid expansion of Low Earth Orbit (LEO) satellite megaconstellations is creating a growing threat to space-based astronomy, challenging the long-held perception that space telescopes are immune to light contamination.If all proposals for new telecommunication satellite launches are fulfilled, projections indicate that Earth could be orbited by **half a million artificial satellites by the end of the 2030s**. Currently, the total number of satellites is only a small fraction (less than 3%) of those planned for the next decade.This episode delves into a study forecasting the devastating impact of these constellations on vital observatories:* **Current Impact:** Satellite trails already affect astronomical images across the complete electromagnetic spectrum. A recent study demonstrated that 4.3% of images obtained by the **Hubble Space Telescope** between 2018 and 2021 already contained artificial satellite trails.* **Future Contamination:** If the planned constellations are completed (approximately 560,000 satellites), light contamination becomes critical for LEO observatories. * The forecast shows that **more than one-third (39.6% $\pm$ 4.6%) of Hubble Space Telescope images will be contaminated**. * Newer LEO telescopes, such as the SPHEREx, ARRAKIHS, and Xuntian space telescopes, are predicted to have **more than 96% of their exposures affected**. * The Xuntian Space Telescope, due to its lower orbit (450 km), will be the most affected, potentially seeing 92 satellite trails per average exposure.* **Trail Brightness:** Reflections from satellites are extremely bright for professional telescopes. The typical surface brightness of detectable trails is forecasted to range from $\mu = 18$ to $\mu = 23$ mag arcsec⁻². This is orders of magnitude above the detectability limit for these telescopes.The scientific community is urging action to address this growing threat. Proposed mitigation measures include setting an optimal upper limit for large satellite constellations' orbits, maintaining updated and precise open archives of orbital solutions for active and derelict spacecraft (avoidance), and implementing correction techniques for unwanted light pollution.*****Reference to the article discussed:**Borlaff, A. S., Marcum, P. M. & Howell, S. B. Satellite megaconstellations will threaten space-based astronomy. *Nature*. Published online 3 December 2025.**DOI:** https://doi.org/10.1038/s41586-025-09759-5Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Borlaff, A.S., Marcum, P.M. & Howell, S.B., Nature 648, 51–57 (2025)

**Topic:** Tidal Disruption Events (TDEs) are short-lived optical flares that occur when a black hole shreds a star, offering valuable insight into black hole demographics. This episode dives into the unusual characteristics and implications of the event AT2022zod.**The Event:*** AT2022zod was identified as an extreme, short-lived optical flare in an elliptical galaxy at a redshift of 0.11.* The event lasted roughly 30 days, with a rapid rise time of approximately 13 days.* It reached a high peak luminosity, positioning it at the extreme end compared to most supernovae.**The Puzzle:*** The host galaxy is estimated to contain a massive central Supermassive Black Hole (SMBH) of about $1.0 \times 10^8 M⊙$.* However, AT2022zod’s short duration and luminosity are **inconsistent** with a TDE powered by this central SMBH.* Modeling and comparison with other TDEs suggest AT2022zod originated from a lower-mass black hole within the system.* The event is highly unlikely to be an AGN flare, as it was the only significant flaring activity detected across five years of monitoring. Alternative explanations like kilonovae, compact-binary mergers, and supernovae were also strongly disfavored by the light-curve analysis.**The Conclusion:*** Lightcurve modeling points to a Massive Black Hole (MBH) in the **intermediate-mass range** (IMBH, $10^4-10^6 M⊙$) as the source of the disruption.* The most plausible origin proposed is the tidal disruption of a star by an MBH embedded in an **Ultra-Compact Dwarf galaxy (UCD)** acquired by the host galaxy.* This discovery highlights the need for flexible search strategies to accommodate unusual events, especially as the Vera C. Rubin Observatory’s Legacy Survey of Space and Time begins.**Article Reference:*** Kristen C. Dage et al. (for the COIN collaboration). "AT2022zod: An Unusual Tidal Disruption Event in an Elliptical Galaxy at Redshift 0.11." Draft version December 3, 2025.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: NASA / CXC / M. Weiss.

This episode dives into how astronomers are leveraging cutting-edge AI to make sense of decades of critical astronomical observations, focusing on the General Coordinates Network (GCN).The GCN, NASA’s time-domain and multi-messenger alert system, distributes over 40,500 human-generated "Circulars" which report high-energy and multi-messenger astronomical transients. Because these Circulars are flexible and unstructured, extracting key observational information, such as **redshift** or observed wavebands, has historically been a challenging manual task.Researchers employed **Large Language Models (LLMs)** to automate this process. They developed a neural topic modeling pipeline using tools like BERTopic to automatically cluster and summarize astrophysical themes, classify circulars based on observation wavebands (including high-energy, optical, radio, Gravitational Wave (GW), and neutrino observations), and separate GW event clusters and their electromagnetic (EM) counterparts. They also used **contrastive fine-tuning** to significantly improve the classification accuracy of these observational clusters.A key achievement was the successful implementation of a zero-shot system using the **open-source Mistral model** to automatically extract Gamma-Ray Burst (GRB) redshift information. By utilizing prompt-tuning and **Retrieval Augmented Generation (RAG)**, this simple system achieved an impressive **97.2% accuracy** when extracting redshifts from Circulars that contained this information.The study demonstrates the immense potential of LLMs to **automate and enhance astronomical text mining**, providing a foundation for real-time analysis systems that could greatly streamline the work of the global transient alert follow-up community.*****Reference to the Article:**Vidushi Sharma, Ronit Agarwala, Judith L. Racusin, et al. (2025). **Large Language Model Driven Analysis of General Coordinates Network (GCN) Circulars.** *Draft version November 20, 2025.*. (Preprint: 2511.14858v1.pdf).Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: arXiv:2511.14858v1

Reference Article: Detection of the Cosmological 21 cm Signal in Auto-correlation at z ∼ 1 with the Canadian Hydrogen Intensity Mapping Experiment, by The CHIME Collaboration.Summary:We delve into a groundbreaking astronomical achievement: the **first detection of the cosmological 21 cm intensity mapping signal in auto-correlation at $z \sim 1$** using the Canadian Hydrogen Intensity Mapping Experiment (CHIME). This discovery utilizes 94 nights of observation data, covering a frequency range from 608.2 MHz to 707.8 MHz, corresponding to a mean redshift of approximately $z \sim 1.16$.The detection was highly significant, measured at **$12.5\sigma$**. This marks a major milestone, as it establishes the 21 cm auto-power spectrum as a direct and potent cosmological probe, eliminating the dependence on external galaxy surveys to study large-scale structure.Key Discussion Points:The Challenge: Detecting the cosmological 21 cm signal is extremely challenging because astrophysical radio foregrounds are several orders of magnitude brighter.Pipeline Advancements: The success relies on significant improvements to the CHIME data processing pipeline. These advancements include novel RFI (Radio Frequency Interference) detection and masking algorithms, achromatic beamforming techniques, and applying foreground filtering *before* time averaging to minimize spectral leakage. The Hybrid Foreground Residual Subtraction (HyFoReS) algorithm was also deployed to correct residual bandpass errors.Robustness and Validation: The measurement is exceptionally reliable, having been established through a comprehensive suite of validation tests. Key checks demonstrated that the signal is consistent across independent right ascension bins, declination bins, and different baseline configurations, ruling out baseline-dependent, RA-dependent, or declination-dependent systematics. Crucially, the consistency of the signal in Stokes-Q data with noise rules out significant polarized foreground leakage.Consistent Results: The auto-correlation result is statistically consistent with previous cross-correlation measurements performed using the same CHIME data stacked on eBOSS quasars, providing strong evidence against contamination from systematics.Cosmological Implications: The measurement constrains the clustering amplitude of neutral hydrogen (HI). For the full band, the derived amplitude parameter is $A^2_{\text{HI}} = 2.59^{+1.26}_{-0.78}(\text{stat.})^{+2.45}_{-0.47}(\text{sys.})$. Independent detections were also made in two sub-bands (9.2$\sigma$ at $z \sim 1.24$ and 8.7$\sigma$ at $z \sim 1.08$), showing consistency between the different redshift slices.Future Outlook:This detection sets the stage for precision 21 cm cosmology. Future work aims to include the nearly 7 years of archival CHIME data to reduce statistical uncertainties, push measurements to higher redshifts (400–600 MHz band), and develop new techniques to recover linear scales in the power spectrum, potentially enabling measurements of Baryon Acoustic Oscillations (BAOs).Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: CHIME/Andre Recnik

In this episode, we dive into the latest findings on **Supernova (SN) 2024bch**, a spectacular stellar death event observed in the nearby galaxy NGC 3206 ($\sim 20$ Mpc). Scientists conducted a multiwavelength analysis, combining **Very High-Energy (VHE) gamma-ray observations** with optical photometry and spectroscopy.**Key Findings:*** **Classification:** SN 2024bch is classified as a potential **Type IIn-L supernova**. This type of core-collapse supernova (CCSNe) exhibits a fast linear decay in its light curve, similar to Type II-L SNe, but shows early-time spectral features indicating interaction with a dense circumstellar medium (CSM) (Type IIn-like).* **The Progenitor:** The data strongly suggest that the progenitor star was consistent with a **Red Supergiant (RSG)**. The progenitor parameters derived from optical modeling and pre-explosion images fall within the typical range for RSGs: mass $M_{pr} = 11 – 20 M_{\odot}$, radius $R_{pr} = 531 \pm 125 R_{\odot}$, luminosity $L_{pr} \le 10^{4.82} L_{\odot}$, and temperature $T_{pr} \le 4000 \text{ K}$.* **The Gamma-Ray Search:** VHE observations were carried out using the **LST-1** (Large-Sized Telescope 1) prototype of the Cherenkov Telescope Array Observatory (CTAO). No significant VHE gamma-ray emission was detected above $100 \text{ GeV}$.* **Setting Limits:** Researchers calculated an integral upper limit on the photon flux of **$F\gamma(> 100 \text{ GeV}) \le 3.61 \times 10^{-12} \text{ cm}^{-2} \text{ s}^{-1}$**. This measurement is significant because it represents the **first ever determined gamma-flux upper limit for a SN of the IIn-L class**, and the first CTAO LST-1 observation of a CCSN with such a low energy threshold.* **Mass-Loss Constraints:** The non-detection allowed researchers to place an upper limit on the mass-loss-rate to wind-velocity ratio ($\dot{M}/u_w \le 10^{-4} M_{\odot} \frac{\text{ yr } \text{ s}}{\text{ km}}$). However, the constraints are subject to uncertainty due to **gamma-gamma absorption**, a process where VHE gamma rays are attenuated by optical photons from the supernova photosphere, especially at early times.**Further Reading:**The results discussed here are based on the article:**"Constraining the TeV gamma-ray emission of SN 2024bch, a possible type IIn-L from a red supergiant progenitor"** published in *Astronomy & Astrophysics manuscript no. aa54721-25*.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: CTAO gGmbH

This episode dives into the extraordinary 400-day observing campaign of Gamma-ray Burst (GRB) 230815A, the first major result from the Panoptic Radio View of Gamma-ray Bursts (“PanRadio GRB”) program.**The PanRadio Program**The PanRadio GRB program is a systematic, multi-year radio survey carried out on the Australia Telescope Compact Array (ATCA). Its goal is to provide comprehensive, multi-frequency (1–50 GHz), and high-cadence radio monitoring of all southern *Swift* GRB events, following their afterglow evolution from within an hour to years post-burst. Crucially, this program provides a **more unbiased view** of GRBs, targeting events like GRB 230815A that typically would not receive traditional radio follow-up because they lack known redshifts or comprehensive multi-wavelength coverage due to high line-of-sight extinction ($A_V = 2.3$).**Key Findings from GRB 230815A**GRB 230815A was a long-duration GRB, likely originating from a collapsar. The 400-day observing campaign revealed a key conflict in its behavior:* **The X-ray Afterglow:** An early X-ray jet break was observed at approximately $\sim 0.1$ days post-burst. This implies a very narrow jet opening angle, estimated to be about $2.1^\circ$.* **The Radio Afterglow:** The radio light curves, traced over an unusually long duration of 400 days, evolved approximately according to the standard self-similar expansion expected for a relativistic blast wave in a homogeneous environment. Critically, the radio evolution was **at odds** with the early X-ray break.* **The Solution: A Two-Component Jet:** Researchers reconcile this conflict by proposing a **two-component jet structure**. The early X-ray break originated from the **narrow, fast component** ($\sim 2.1^\circ$), while the delayed or absent jet break in the radio light curves stems from a separate, **wider component** with a half-opening angle estimated to be $\gtrsim 35^\circ$.**Long-Term Impact**The extensive follow-up confirmed that after 400 days, the blast wave showed no evidence of transitioning to the non-relativistic regime, which constrains the ratio between the blast wave kinetic energy and the circumburst medium (CBM) density. The PanRadio program will build a large, unbiased sample to rigorously inspect the microphysical and dynamical parameters of GRBs, revealing the true diversity of their outflows and environments.**Article Reference**These results are published in the draft article: **"First results from the PanRadio GRB Collaboration: the 400-day afterglow of GRB 230815A"**. https://arxiv.org/pdf/2511.07644Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: CSIRO

The Search for Galactic NeutrinosThis episode explores the final results from the ANTARES neutrino telescope, which operated in the Mediterranean Sea off the coast of Toulon, France. Researchers analyzed the full, 15-year dataset (2007–2022) to search for diffuse Galactic neutrinos. These neutrinos are produced when cosmic rays (CRs) interact with interstellar matter (gas and radiation fields) in the Milky Way. Understanding this diffuse flux is key to deciphering cosmic ray transport mechanisms.Testing Theoretical ModelsThe study utilized an unbinned maximum likelihood analysis to test several phenomenological models of neutrino emission, including KRA$\gamma$ models, DiffUSE, CRINGE, and Fermi-LAT $\pi^0$. These models incorporate different assumptions about CR diffusion and source distribution. ANTARES used three data samples—one track-like and two shower-like—and its location and use of water provided superior angular resolution compared to other detectors, making it well-suited for observing the central Milky Way. Furthermore, the shower-like events extended the analysis down to the hundreds of GeV energy range.Results: Constraints and CluesWhile the ANTARES low statistics dataset did not allow for a significant discovery, the analysis placed **upper limits** on the diffuse neutrino flux that are compatible with results obtained by other experiments.Model Constraints: The results did not yield stringent constraints on the tested models. The highest observed significance was a small hint of 1.28$\sigma$ for the KRA5PeV$\gamma$ model.The Galactic Ridge Hint: Importantly, a model-independent analysis of the Galactic Ridge (|$\ell$| < 30$^\circ$ and |$b$| < 2$^\circ$) confirms a hint of a Galactic signal at 1.9$\sigma$**. This result confirms a finding from a previous ANTARES analysis.This analysis methodology, which carefully preserves the spatial-energy correlation of the templates and convolves them with detector response, is promising for testing Galactic diffuse emission models with larger future datasets, such as those from KM3NeT.Article ReferenceSearch for Diffuse Galactic Neutrinos with the Full ANTARES Telescope Dataset, ANTARES Collaboration et al. (A. Albert, S. Alves, M. André, et al.); preprint, 2511.01687Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: CEA/Irfu

In this episode, we dive into the fascinating and violent world of galactic centers with the discovery of **AT2023uqm**, a new nuclear transient offering unprecedented insights into stellar consumption by supermassive black holes (SMBHs).AT2023uqm is only the second confirmed case of a star undergoing **repeated partial tidal disruption events (rpTDEs)**, where a star on a bound, eccentric orbit repeatedly loses its outer layers as it approaches the SMBH.**What makes AT2023uqm unique?**Unlike its predecessor, AT2023uqm exhibits a novel behavior: a nearly **exponential, or "runaway," increase in flare energy** across its series of periodic outbursts. This escalating brightness is evidence of the star’s progressive destruction over time.Key observations include:* **Periodicity:** The transient displays at least five distinct, periodic optical flares. The adopted period is **526.75 ± 0.87 days** in the observer’s frame.* **Light Curve Structure:** Each flare displays a **similar double-peaked structure**. This structure requires constraints on the progenitor star, suggesting it is either a low-mass main-sequence star or, potentially, an evolved giant star.* **Multi-wavelength Data:** Follow-up campaigns across optical/UV, X-ray, and radio bands found the optical/UV emission maintains a nearly constant blackbody temperature around 18,000 K. The spectra revealed intermediate-width Balmer lines and strong Fe II and Bowen fluorescence lines.AT2023uqm serves as a crucial framework for modeling and understanding the runaway mass loss phenomena in rpTDEs. Due to the estimated mass loss rate, scientists anticipate **only one or two more flares** before the star is completely disrupted. Be ready: the next outburst is predicted to peak (the first peak) around **August 26, 2026** (MJD 61278).**Reference:**This episode is based on the article: **"A Star’s Death by a Thousand Cuts: The Runaway Periodic Eruptions of AT2023uqm"** by Yibo Wang et al. (2025).Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Ralf Crawford (STScI)

Join us as we discuss the latest results from the IceCube Neutrino Observatory, utilizing 13.1 years of data, that further link high-energy neutrinos to powerful cosmic sources.### Episode Highlights* **The Extragalactic Neutrino Puzzle:** The IceCube Neutrino Observatory consistently detects a diffuse flux of high-energy cosmic neutrinos, the majority of which are extragalactic in origin. These neutrinos are expected to be produced in hadronic interactions, which also generate gamma rays.* **Revisiting NGC1068:** The Seyfert galaxy **NGC1068** remains the most significant neutrino source identified in searches across the northern sky. Notably, the observed neutrino flux from NGC1068 exceeds its gamma-ray counterpart by at least two orders of magnitude. Using $13.1$ years of data, NGC1068's emission is characterized by a soft, unbroken power-law spectrum with a spectral index $\gamma = 3.4 \pm 0.2$.* **Focusing on X-ray Bright AGN:** The X-ray bright nature of NGC1068 motivated a new search focusing on $\mathbf{47}$ X-ray bright Seyfert galaxies, selected from the Swift/BAT spectroscopic survey based on their hard X-ray fluxes (20–50 keV). This hard X-ray band is chosen because it is more robust against obscuration compared to softer X-ray bands.* **A Collective Signal:** This dedicated search revealed a significant $\mathbf{3.3\sigma}$ excess from an ensemble of $\mathbf{11}$ X-ray bright AGN (excluding NGC 1068). These results significantly strengthen the evidence that $\mathbf{X-ray}$ **bright cores of active galactic nuclei are neutrino emitters**.* **Diversity in Emission:** The population of contributing AGN includes both Seyfert I and Seyfert II galaxies, suggesting that the level of nuclear obscuration does not significantly impact the likelihood of neutrino emission. However, the individual sources show diverse characteristics: while NGC1068 exhibits a soft spectrum dominated by lower-energy events, the second most significant source, NGC7469, has an excess driven by only two very high-energy events ($E_{\nu} > 100\text{ TeV}$). This suggests that not all X-ray bright AGN share the same neutrino production mechanisms.* **The Physics Connection:** The neutrino emission is likely produced in the immediate vicinity of the supermassive black hole (SMBH), plausibly within the AGN's $\mathbf{corona}$. In this environment, coronal X-ray photons interact with high-energy protons (photomeson production), generating the 1–10 TeV neutrinos observed by IceCube.***### Reference ArticleThe data and findings discussed are presented in the research paper titled:* **"Evidence for Neutrino Emission from X-ray Bright Active Galactic Nuclei with IceCube"**.* *Draft Version Date:* October 16, 2025.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: IceCube, Georgia Tech

Join us as we discuss the groundbreaking discovery by the LHAASO Collaboration of a vast and unique ultra-high-energy (UHE) $\gamma$-ray source. This mysterious object, nicknamed the **"Peanut"** for its distinctive asymmetric shape, spans approximately $0.45^\circ \times 4.6^\circ$ and is located far off the Galactic plane, at a high Galactic latitude ($b \approx -17.5^\circ$), a region where UHE $\gamma$-ray sources are typically sparse.**Key Takeaways:*** **Extreme Energies Detected:** The LHAASO (Large High Altitude Air Shower Observatory) detected $\gamma$-rays in this region exceeding 100 TeV (Tera-electronvolts), with the highest-energy event reaching $760^{+60}_{-40}$ TeV. These UHE $\gamma$-rays are signatures of **extreme particle acceleration** in astrophysical sources.* **The Millisecond Pulsar Mystery:** The **highly aged millisecond pulsar (MSP) J0218+4232** is the sole candidate accelerator positionally coincident with the Peanut. The observed $\gamma$-ray luminosity ($L_{\gamma} \approx 9.36 \times 10^{32} \text{ erg s}^{-1}$) can be powered by the MSP’s spin-down power ($\dot{E} \approx 2.44 \times 10^{35} \text{ erg s}^{-1}$) if the energy conversion efficiency is greater than $0.4\%$.* **Challenging Prevailing Models:** If confirmed, this MSP association would be the **first evidence of a millisecond pulsar powering PeV particles**, directly challenging conventional models which posit that MSPs cannot sustain acceleration to PeV energies.* **Anisotropic Diffusion:** The Peanut's asymmetric, strip-like morphology is clear evidence of **anisotropic particle distribution** over a large area. Analysis suggests that particle transport plays the dominant role in shaping the Peanut structure. The resulting diffusion coefficient estimates indicate that particles travel about 400 times faster parallel to the strip than perpendicular to it ($D_{\parallel} \simeq 400 D_{\perp}$), compatible with estimates for the Galactic halo.* **Next Steps:** The definitive origin of the Peanut remains uncertain, potentially revealing a **new class of extreme Galactic accelerators** (PeVatrons). Further multiwavelength observations are necessary to constrain the mechanisms involved.**Reference Article:****"A Giant Peanut-shaped Ultra-High-Energy Gamma-Ray Emitter Off the Galactic Plane"** by The LHAASO Collaboration.Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: LHAASO Collaboration