Multi-messenger astrophysics

Astro-COLIBRI
  • 0.0 (0)
  • ASTRONOMY
  • UPDATED WEEKLY

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

    11 HRS AGO

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

    2 DAYS AGO

    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
  3. The SVOM Satellite: A New Era in Multi-Messenger Astronomy

    29 APR

    The SVOM Satellite: A New Era in Multi-Messenger Astronomy

    In this episode, we dive into the fascinating world of gamma-ray bursts (GRBs) and high-energy transients through the lens of the SVOM (Space-based Multi-band Variable Object Monitor) mission. Launched in June 2024, this Sino-French satellite uses a powerful suite of instruments to detect, localize, and study some of the universe's most extreme events, such as dying massive stars and colliding neutron stars. We explore three of its core instruments: the ECLAIRs trigger camera, the Gamma-Ray Monitor (GRM), and the Visible Telescope (VT). Discover how these tools work together in near real-time to capture everything from high-redshift GRBs in the early universe to optical afterglows and thermonuclear X-ray bursts. Key Topics Covered: The SVOM Mission: An overview of the satellite, which operates in a 625 km low-Earth orbit, and its primary goal to study GRBs and support multi-messenger astrophysics (like gravitational wave follow-ups).ECLAIRs Trigger Camera: A look at the 4–150 keV wide-field coded mask camera that serves as SVOM's autonomous trigger. When ECLAIRs detects a transient, it can prompt the satellite to automatically slew, or rotate, to point its narrow-field telescopes directly at the burst. Gamma-Ray Monitor (GRM): SVOM’s high-energy sentinel covering an energy range of 15 keV up to 5 MeV. We discuss how its large sensitive area helps measure the spectral and temporal properties of bursts, achieving a detection rate of over 100 GRBs per year.Visible Telescope (VT): A deep dive into SVOM's 44-cm aperture optical/near-infrared telescope. Learn how the VT achieved an impressive ~85% detection rate for GRBs observed within the first 10 minutes, and how its deep sensitivity helped identify the mission's highest-redshift burst to date, GRB 250314A, from when the universe was in its infancy (redshift 7.3). References & Further Reading: 1. The Gamma-Ray Monitor onboard the SVOM satellite by Jian-Chao Sun, Yong-Wei Dong, Jiang He, et al. 2. SVOM/VT: Instrument Overview, Science Objectives, and First-Year Performance by Yu-Lei Qiu, Li-Ping Xin, Jin-Song Deng, et al. 3. ECLAIRs: the SVOM high-energy transient trigger camera by O. Godet, J.-L. Atteia, S. Schanne, et al. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: SVOM, CNRS

    25 min
  4. Chasing the Flash: Hunting Neutron Star Mergers with CTAO

    14 APR

    Chasing the Flash: Hunting Neutron Star Mergers with CTAO

    In this episode, we dive into the thrilling world of multi-messenger astronomy! Ever since the historic detection of GW170817, scientists have known that binary neutron star (BNS) mergers can produce both gravitational waves and explosive short gamma-ray bursts (sGRBs). But how can we best catch the highest-energy light from these elusive cosmic collisions? We explore a recent study by the Cherenkov Telescope Array Observatory (CTAO) Consortium that simulates the upcoming O5 observing run to figure out the absolute best strategies for detecting these VHE (very-high-energy) gamma-ray signals. Key Topics Discussed: The Power of CTAO: An introduction to the Cherenkov Telescope Array Observatory, the next-generation ground-based gamma-ray observatory that boasts an unprecedented sensitivity to short-timescale phenomena, up to 10,000 times better than current satellite instruments for specific energies.The Race Against Time: Why speed is everything. We discuss how the probability of detecting a gamma-ray counterpart plummets if observations don't begin within the first 1 to 4 hours after the gravitational wave onset.Angles Matter: Why a GRB's "viewing angle" is the single most important factor for detectability. We explain the difference between observing a jet "on-axis" versus "off-axis" and why even a rough angle estimate from gravitational wave alerts could revolutionize follow-up campaigns.The Winning Strategy: How do you search a massive, poorly localized region of the sky? We unpack why researchers found that short, 5-minute fixed observation windows combined with Real-Time Analysis (RTA) offer the perfect balance to maximize the chances of a successful detection.The Odds of Success: A look at the study's conclusion that an optimized follow-up strategy could allow CTAO to detect VHE gamma-ray emission from roughly 5% of gravitational wave-associated short GRBs. Featured Reference: Abe, S., et al. (CTAO Consortium). "Chasing Gamma-Ray Signals from Binary Neutron Star Coalescences with the Cherenkov Telescope Array: Prospects and Observing Strategies." Draft version April 13, 2026. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: NASA's Goddard Space Flight Center/CI Lab

    20 min
  5. Tiling the Sky: A New Strategy for Finding Elusive GRBs

    13 APR

    Tiling the Sky: A New Strategy for Finding Elusive GRBs

    In this episode, we dive into the intense and fast-paced world of **Gamma-ray bursts (GRBs)—the most luminous and rapidly evolving transients in the Universe**. While space-based instruments like the Fermi Gamma-ray Space Monitor (GBM) trigger on hundreds of these events every year, they often provide poor sky localization, sometimes spanning tens to hundreds of square degrees. This makes it incredibly difficult for ground-based telescopes to find and observe the very-high-energy (TeV) afterglows before they rapidly fade away. Today, we discuss a groundbreaking paper that proposes a solution: **an optimized follow-up strategy based on the rapid tiling of large sky regions**. By creating a synthetic population of GRBs informed by over 15 years of observational data, researchers have tested how next-generation Imaging Atmospheric Cherenkov Telescopes (IACTs)—like ASTRI, LACT, and CTAO—can use this rapid scanning method to catch these elusive bursts. Tune in to find out how **this new approach could double the detection rates for certain telescopes**, potentially allowing facilities like CTAO to capture up to four very-high-energy GRB events per year. **Article Reference:** * Macera, S., Banerjee, B., Seglar-Arroyo, M., Green, J., et al. **"Detection of TeV emission during early afterglow from poorly localized GRBs with ground based IACTs."** *Astronomy & Astrophysics* manuscript no. arxiv_03042026, April 10, 2026. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: CTAO

    19 min
  6. Fast Radio Bursts & Magnetar X-Rays: A Peculiar Discovery

    7 APR

    Fast Radio Bursts & Magnetar X-Rays: A Peculiar Discovery

    In this episode, we dive into the deep cosmos to explore a recent astronomical breakthrough linking Fast Radio Bursts (FRBs)—enigmatic, millisecond-long cosmic transients—to extreme stellar objects known as magnetars. We unpack the discovery of **MXB 221120**, a peculiar magnetar X-ray burst detected by the GECAM observatory on November 20, 2022, which originated from the galactic magnetar SGR J1935+2154 and coincided with an FRB. Discover why this specific burst has astronomers buzzing. Unlike previously observed bursts, MXB 221120 is a massive outlier featuring an unusually long duration and a high blackbody temperature. Most surprisingly, it is the **first FRB-associated X-ray burst from this magnetar to exhibit a purely thermal spectrum**. This discovery fundamentally challenges current theoretical models, which previously assumed that these events are dominated by non-thermal emissions due to resonant Compton scattering. We will also explore a strange ~18 Hz Quasi-Periodic Oscillation (QPO) detected within the burst. We discuss how this frequency might actually be the seismic "ringing" of a low-order crustal torsional eigenmode—essentially, the sound of the magnetar's crust cracking from a singular dissipation of intense internal magnetic energy. Episode Reference: Tan, W.-J., Wang, Y., Wang, C.-W., et al. (2026). "GECAM discovery of a peculiar magnetar X-ray burst (MXB 221120) from SGR J1935+2154 associated with a fast radio burst." *Astronomy & Astrophysics*, April 3, 2026. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: CAS

    22 min
  7. Starbursts and Seyferts: The Mystery of the Missing Gamma Rays

    30 MAR

    Starbursts and Seyferts: The Mystery of the Missing Gamma Rays

    In this episode, we dive deep into the fascinating world of "composite" galaxies—cosmic beasts that host both an actively feeding supermassive black hole (a Seyfert nucleus) and regions of intense star formation (a starburst component). We explore recent research from the High Energy Stereoscopic System (H.E.S.S.) observatory, which conducted deep observations of three nearby composite galaxies: NGC 1068, the Circinus galaxy, and NGC 4945. The big question driving the research: Can we detect very high-energy (VHE) gamma rays from the extreme environments at the centers of these galaxies? Surprisingly, H.E.S.S. detected no significant VHE gamma-ray signals from any of the three targets. Tune in to find out why this lack of detection is actually highly revealing! We discuss how these newly established upper limits on gamma-ray fluxes are helping astrophysicists test and constrain major theories, including: Jet-Driven Bubbles: How the outflows in these galaxies compare to the giant "Fermi bubbles" found in our own Milky Way. Cosmic Ray Calorimeters & UHECRs: Whether these galaxies act as traps for cosmic rays, and if they could be the source of mysterious ultra-high-energy cosmic rays (UHECRs) hitting Earth. The Neutrino Connection: How the absence of gamma rays in NGC 1068 perfectly complements the detection of high-energy neutrinos by the IceCube observatory, suggesting that gamma rays are being heavily absorbed by a dense X-ray photon field right next to the supermassive black hole. Reference to the Article: H.E.S.S. Collaboration, Acharyya, A., Aharonian, F., et al. (2026). "H.E.S.S. observations of composite Seyfert–starburst galaxies." Astronomy & Astrophysics (Preprint online version: March 24, 2026). Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: NASA/ESA/A. van der Hoeven

    23 min
  8. 15 years hunting for GRBs with H.E.S.S.

    27 MAR

    15 years hunting for GRBs with H.E.S.S.

    In this episode, we dive into the explosive world of Gamma-Ray Bursts (GRBs)—brief, intense pulses of sub-MeV gamma rays that are considered excellent laboratories for studying particle acceleration, capable of releasing up to $10^{51} - 10^{54}$ ergs of isotropic equivalent energy. We explore the newly published second H.E.S.S. gamma-ray burst catalogue, which details a massive 15-year observational campaign spanning from 2004 to 2019. We discuss how the High Energy Stereoscopic System (H.E.S.S.) followed up on 89 different GRB alerts, yet found no *new* very-high-energy (VHE) signals beyond previously published detections. But as we will learn, a "non-detection" is actually a massive win for astrophysics! The resulting upper limits form the largest available dataset for GRBs at VHE. We break down why catching these signals is so incredibly difficult, exploring the technical challenge of rapidly repointing ground-based telescopes before the early afterglow fades and how Extragalactic Background Light (EBL) absorbs high-energy gamma rays from distant sources before they ever reach Earth. We also unpack the standard Synchrotron Self-Compton (SSC) emission models and explain how the upper limits set by H.E.S.S. perfectly align with current physics, proving that VHE-detected GRBs are not a distinct, weird population of stars, but simply the ones that are closest to us and possess naturally luminous X-ray emission. Finally, we look to the future with the next-generation Cherenkov Telescope Array Observatory (CTAO), which features a lower energy threshold that will revolutionize our ability to detect fainter and more distant GRBs. Reference: Acharyya, A. et al., "The second H.E.S.S. gamma-ray burst catalogue: 15 years of observations with the H.E.S.S. telescopes." *Astronomy & Astrophysics*, accepted 2026. Acknowledements: Podcast prepared with Google/NotebookLM. Illustration credits: H.E.S.S./Vikas Chander

    23 min
See All (99)

About

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.

Information

You Might Also Like