Multi-messenger astrophysics

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Discussions around tools and discoveries in the novel domain of multi-messenger and time domain astrophysics. We'll highlight recent publications, discuss tools to faciliate observations and generally talk about the cool science behind the most violent explosions in the universe.

  1. Cosmic Accelerators: Unlocking the Secrets of Microquasar GRS 1915+105

    11 hrs ago

    Cosmic Accelerators: Unlocking the Secrets of Microquasar GRS 1915+105

    In this episode, we dive into the extreme and fascinating world of microquasars—binary systems where a compact object, like a black hole, feeds off a companion star and launches powerful, relativistic jets. Our spotlight is on GRS 1915+105, one of the most dynamic and powerful microquasars known in the Milky Way. Recent groundbreaking observations from the LHAASO and Fermi-LAT observatories have mapped broadband gamma-ray emissions from this system, revealing that it operates as an extreme "PeVatron"—an accelerator capable of pushing particles to multi-PeV (peta-electron volt) energies. We break down the evidence pointing to a "hadronic scenario," which suggests that these mind-boggling energies are produced when highly accelerated protons from the jet smash into the dense ambient gas surrounding the system. Join us as we discuss how this discovery proves that microquasars are exceptionally efficient particle accelerators and how they might be the missing link to understanding the origins of the most energetic cosmic rays in our galaxy. Key Takeaways: What is a Microquasar? A look at the anatomy of GRS 1915+105, a system featuring a black hole pulling material from a small K-type star and firing off jets at 80% the speed of light.The Power of LHAASO & Fermi-LAT: How a joint analysis of 4 years of LHAASO data and 17 years of Fermi-LAT data finally detected persistent gamma-ray emissions from this source.The Hadronic Accelerator: Why the shifted centroid of the gamma-ray emission suggests that protons (rather than electrons) are being accelerated by the jet's mechanical power and colliding with surrounding interstellar gas. Solving a Galactic Mystery: How just a handful of microquasars like GRS 1915+105 could be responsible for supplying the entire Milky Way with PeV-level cosmic rays. Reference: Cao, Z., Aharonian, F., Bai, Y.X., et al. (The LHAASO Collaboration). "Extreme PeV accelerator associated with GRS 1915+105." (Preprint: 2606.25054v1). Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: NASA/CXC/A.Hobart

    21 min
  2. Echoes of Annihilation: Solving the 10 MeV Mystery of GRB 221009A

    4 days ago

    Echoes of Annihilation: Solving the 10 MeV Mystery of GRB 221009A

    In this episode, we dive into the fascinating astrophysics surrounding GRB 221009A, the brightest gamma-ray burst observed to date. While its sheer energy is staggering, we focus on an even more intriguing puzzle: an unprecedented, narrow emission line at around 10 MeV discovered shortly after the burst's brightest peak. We explore a groundbreaking new study that explains this 10 MeV line as the result of a massive annihilation of electron-positron pairs. We break down the proposed scenario in which the GRB's precursor blastwave was illuminated by the burst's main event, triggering copious pair creation that resulted in a "pair bubble bursting". Because this annihilation happened so quickly as the shell expanded relativistically, the resulting line evolution is dominated by what astrophysicists call the high-latitude emission (HLE) effect. Furthermore, we examine what this means for the actual star that caused the burst. To make this model work, the progenitor star must have been surrounded by an incredibly dense circum-stellar medium (CSM) extending out to a few $10^{15}$ cm, reminiscent of the dense environments found around Type IIn supernovae. Finally, we'll connect these findings to the sharp rise in the TeV afterglow observed by the LHAASO observatory, which the researchers attribute to the main ejecta colliding with this pair-enriched blastwave. Key Takeaways: The 10 MeV Emission Line: How high-latitude emission from a geometrically thin, relativistically expanding shell explains this rare spectral feature.Pair Production and Annihilation: The mechanism where gamma-rays from the main event interact with a precursor blastwave to create extreme numbers of electron-positron pairs.Clues About the Progenitor Star: Why the presence of a dense circum-stellar medium suggests the dying star underwent an intense mass-loss phase in the years just prior to its explosion.Solving the LHAASO Afterglow Mystery: How the collision between the main event ejecta and the pair-loaded blastwave perfectly accounts for the sudden, sharp rise in the TeV afterglow. Episode Reference: Salafia, O. S., Celotti, A., Sobacchi, E., Nava, L., Oganesyan, G., Ghirlanda, G., Boula, S., Ravasio, M. E., & Ghisellini, G. (2026). A self-consistent explanation of the MeV line in GRB 221009A unveils a dense circum-stellar medium. Astronomy & Astrophysics. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Jingchuan Yu

    22 min
  3. Decoding the BOAT: GRB 221009A and the Hunt for High-Energy Neutrinos

    16 June

    Decoding the BOAT: GRB 221009A and the Hunt for High-Energy Neutrinos

    In this episode, we dive into the astrophysics behind GRB 221009A, an event widely known as the Brightest-Of-All-Time (BOAT) gamma-ray burst. Detected in October 2022, this extraordinary explosion shattered records by producing ultra-high-energy photons exceeding 10 TeV. We discuss a recent multi-messenger study that models the burst's very-high-energy (VHE) afterglow using a Gaussian structured jet expanding into an interstellar medium. We explore how this smooth, angular jet structure explains the extreme TeV output observed at a mildly off-axis viewing angle, cleanly resolving the "energy crisis" that standard uniform (top-hat) jet models face. Finally, we tackle the mystery of the missing neutrinos. Despite the immense energy of the BOAT, observatories like IceCube have not detected any coincident neutrinos. We break down the calculations for photo-hadronic ($p\gamma$) neutrino production and explain why the expected flux still falls below the sensitivity limits of even the next generation of detectors, like IceCube Gen2 and GRAND200k. Key Takeaways: The BOAT GRB: GRB 221009A was a remarkably luminous and relatively nearby event, offering an unprecedented opportunity to test emission models and ultra-high-energy cosmic ray acceleration.The Power of a Gaussian Jet: By using a Gaussian structured jet model, scientists can accurately reproduce the burst's gradual light curve steepening and immense brightness without requiring physically unrealistic energy budgets. A Mildly Off-Axis View: The study reveals that the optimal way to interpret the data is a mildly off-axis viewing geometry, which allows the observer to receive intense early-time emission from the jet's core.Neutrino Non-Detection Explained: Mathematical models of the photo-pion decay channel show that even under highly optimistic microphysical parameters, the predicted muon neutrino events remain below current and future detection limits, confirming that the null results from IceCube are consistent with the physics. Reference to the Article Discussed: Mondal, T., Razzaque, S., Joshi, J. C., Majumder, S., & Bose, D. (2026). Multi messenger study of GRB 221009A with VHE gamma-ray and neutrino Afterglow from a Gaussian structured jet. Journal of High Energy Astrophysics, 53, 100636. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: NASA's Goddard Space Flight Center and Adam Goldstein (USRA)

    20 min
  4. FRB 20191221A or "the telescope that hallucinated in the rain"

    10 June

    FRB 20191221A or "the telescope that hallucinated in the rain"

    In 2022, the astronomy community was buzzing about FRB 20191221A, an unusual Fast Radio Burst that made headlines for exhibiting a highly significant 217-millisecond periodicity. But what if this groundbreaking extragalactic signal actually originated from our own cosmic backyard? In today's episode, we dive into a fascinating course-correction by the CHIME/FRB Collaboration. We explore how a "series of unfortunate events" led the team to misclassify what turned out to be a known Galactic pulsar, PSR J0248+6021. The true culprit behind the mix-up was the weather: heavy rain on December 21, 2019, caused water to pool in the telescope's electronics, which corrupted the calibration data. This error generated a massive 20-degree pointing offset in the declination. Because the telescope assigned the bursts to the wrong location, the pulsar's high Dispersion Measure (DM) made it artificially appear as though it was an extragalactic FRB. Join us as we discuss how the team unraveled the mystery after discovering "twin bursts" at different coordinates, how the pulsar's unusual emission pattern disguised its true identity, and the new diagnostic checks CHIME has implemented to guarantee the accuracy of their wider FRB catalog. Article Reference: - A series of unfortunate events: CHIME/FRB misclassification of a Galactic pulsar as a periodic fast radio burst by The CHIME/FRB Collaboration (Bridget C. Andersen, Mohit Bhardwaj, P. J. Boyle, et al.). Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Danielle Futselaar

    20 min
  5. Record-Breaker: Catching Gamma Rays from the Distant Quasar OP 313

    1 June

    Record-Breaker: Catching Gamma Rays from the Distant Quasar OP 313

    In this episode, we dive into a groundbreaking astronomical discovery: the detection of very-high-energy (VHE) gamma rays from the quasar OP 313. Located at a redshift of $z = 0.997$, OP 313 has shattered records to become the most distant Active Galactic Nucleus (AGN) ever observed in this extreme energy range. We explore the massive flare event from December 2023 that made this detection possible. During this outburst, OP 313 shone roughly 50 times brighter than its average high-energy state, triggering an intense multi-wavelength observation campaign. We also discuss the cutting-edge technology behind the discovery, notably the Large-Sized Telescope prototype (LST-1) and the MAGIC telescopes located in the Canary Islands. Tune in to learn how astronomers use the light from this incredibly distant blazar to measure the Extragalactic Background Light (EBL)—the cumulative "fog" of radiation from all stars and galaxies throughout the history of the universe—and how they map the extreme physics of black hole-powered jets. Reference: Abe, K., et al. (May 27, 2026). Detection of the distant quasar OP 313 with the first Large-Sized Telescope of CTAO. Astronomy & Astrophysics. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Tomohiro Inada

    20 min
  6. Ripples in Spacetime: Unpacking the GWTC-5.0 Catalog

    29 May

    Ripples in Spacetime: Unpacking the GWTC-5.0 Catalog

    In this episode, we dive into the monumental release of the Gravitational-Wave Transient Catalog version 5.0 (GWTC-5.0) and the open data from the second part of the fourth observing run (O4b) by the LIGO, Virgo, and KAGRA observatories. We explore how these massive, international detectors have expanded our view of the gravitational-wave universe and what the newest data tells us about the cosmic collisions of black holes and neutron stars. Key Talking Points A Growing Cosmic Census: The GWTC-5.0 update adds 161 new compact binary coalescence candidates, bringing the catalog's total to nearly 400 probable transient events.Record-Breaking Detections: We discuss GW250114_082203, the loudest gravitational-wave event ever recorded, boasting an unprecedented network signal-to-noise ratio of 76.9. We also highlight GW240615_113620, which is the most precisely localized gravitational-wave source to date.Unveiling Black Hole Populations: Discover the latest population properties of merging black holes, including intriguing evidence for subpopulations of rapidly spinning black holes that suggest the occurrence of "hierarchical mergers" in dense stellar environments. The Science of Noise and Data Quality: A behind-the-scenes look at how scientists calibrate the detectors and mitigate instrumental noise (like "glitches") to provide pristine, analysis-ready data to the global scientific community. References & Further Reading This episode is based on the suite of papers detailing the GWTC-5.0 release and the O4b open data from the LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration: Open Data from LIGO, Virgo, and KAGRA through the Second Part of the Fourth Observing Run (Abac et al., 2026).GWTC-5.0: An Introduction to Version 5.0 of the Gravitational-Wave Transient Catalog (Abac et al., 2026).GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog (Abac et al., 2026).GWTC-5.0: Population Properties of Merging Compact Binaries (Abac et al., 2026). Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Maggie Chiang for Simons Foundation

    22 min
  7. SN 2017egm : Fermi-LAT's Breakthrough Gamma-Ray Detection

    22 May

    SN 2017egm : Fermi-LAT's Breakthrough Gamma-Ray Detection

    In today’s episode, we dive into the mystery of superluminous supernovae (SLSNe)—rare, extreme astronomical events that shine 10 to 100 times brighter than standard core-collapse supernovae. For years, astrophysicists have debated what powers these brilliant explosions, with the two leading theories being interaction with surrounding circumstellar medium (CSM) or energy injected by a "central engine," such as a rapidly spinning, highly magnetized neutron star known as a magnetar. We discuss a recent breakthrough using 16 years of data from the Fermi Large Area Telescope (LAT). Researchers conducted a systematic search of nearby SLSNe and found significant giga-electronvolt (GeV) gamma-ray emission coming from one specific target: SN 2017egm. We explore why this delayed gamma-ray signal—appearing between 50 and 160 days after the initial explosion—strongly points to a magnetar driving the event. We also break down why the competing CSM interaction model falls short in explaining the timing and the ratio of gamma-ray to optical luminosity observed in this supernova. Finally, we look ahead at what future observatories, like the Cherenkov Telescope Array Observatory (CTAO), might reveal about these colossal cosmic engines. Key Takeaways: What superluminous supernovae are and why their massive energy output requires exceptional power sources.The significance of SN 2017egm yielding the first confirmed gamma-ray signature for this class of transients.How the timing and luminosity ratio of the gamma-ray emission strongly favor a central magnetar wind nebula over the CSM interaction model.How future sub-tera-electronvolt observations could open a new window into understanding the core mechanisms of SLSNe. Reference: Acero, F., Acharyya, A., et al. "Gamma-ray signature of superluminous supernovae: Fermi-LAT GeV detection of SN 2017egm and evidence of a central engine." Astronomy & Astrophysics, 709, A229 (2026). DOI: 10.1051/0004-6361/202558547. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: Astronomy & Astrophysics, 709, A229 (2026)

    24 min
  8. Supernovae on the RISE: Why Dead Stars Wake Up Decades Later

    20 May

    Supernovae on the RISE: Why Dead Stars Wake Up Decades Later

    In this episode, we explore the fascinating phenomenon of core-collapse supernovae that refuse to fade away quietly. Years, or even decades, after their initial explosion, some of these stellar deaths experience a surprising "late-time radio rebrightening". We dive into how astronomers are using these delayed radio signals as a time machine to study the final centuries of a massive star's life. Key Highlights: The 18-Year Echo: We discuss the incredible discovery by the RISE (Rebrightening in Interacting Supernova Emission) collaboration, which detected radio emission from the Type II supernova SN 2007it a full 18 years after it exploded. Smashing into the Past: Why do these dead stars light up again? We break down how the expanding supernova shockwave eventually slams into a dense shell of circumstellar material (CSM) that the star shed long before it died. For SN 2007it, this shell is estimated to be around 3 solar masses.A Broader Look at Stellar Mass Loss: Drawing on a comprehensive study of 16 Type IIn and II-L supernovae using the Very Large Array (VLA), we explore how long-lasting radio emissions—sometimes persisting for 20 years post-explosion—reveal that these stars sustained extreme mass loss for hundreds or thousands of years before core collapse. Blurring the Lines: We look at how this late-time radio data proves that different supernova classifications (like IIn and II-L) actually exist on a continuum, separated mainly by the density and timing of their pre-explosion mass loss. Articles Discussed in this Episode: Acero, F., et al. (The RISE Collaboration). (2026). SN 2007it on the RISE - a radio detection of an interacting supernova 18 years post-explosion.Kilpatrick, C. D., et al. (2026). Probing the Mass-loss Histories of Type IIn and II-L Supernovae with Late-time Radio Observations. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: NRAO

    17 min
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Discussions around tools and discoveries in the novel domain of multi-messenger and time domain astrophysics. We'll highlight recent publications, discuss tools to faciliate observations and generally talk about the cool science behind the most violent explosions in the universe.

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