arXiv subjects

A. L. De Santis

Publications and source records attributed to A. L. De Santis.

3 recordsLinked to original sources

arXiv2026

Core-Collapse Supernova detections from Einstein Telescope within the Milky Way

Core-collapse supernovae are key drivers of galaxy evolution and promising sources of gravitational waves, which provide a unique probe of the physics driving their explosion mechanism. Third-generation detectors, such as the Einstein Telescope, will dramatically improve the prospects for detecting these signals. This study assesses the capability of the Einstein Telescope, alone and in synergy with next-generation detectors such as Cosmic Explorer, to detect gravitational waves from core-collapse supernovae. We estimate the detection horizons and expected event rates for sources in the Milky Way and nearby satellite galaxies. We employed the GWFish simulation framework, customized to include core-collapse supernovae waveform catalogs from state-of-the-art 3D simulations and stellar population data generated with TRILEGAL. This approach allows us to model gravitational waves detectability as a function of progenitor mass, source position and detector network configuration. Our analysis shows that the Einstein Telescope can detect gravitational waves from PNS-driven core-collapse supernovae up to distances ranging from ~20 to more than 100 kpc with a 90% confidence level, depending on the progenitor mass and waveform, while a combination of this detector in a network can extend the reach up to ~170 kpc in the most favorable cases. For a representative 15 M_sun progenitor, ET (in its 2L configuration) achieves a detection horizon of ~100 kpc, ensuring essentially complete coverage of the Milky Way and partial coverage of the Magellanic Clouds.

astro-ph.HE↗

arXiv2026

Gravitational wave detectability range informed by external messengers

A rapid estimate of gravitational-wave (GW) detectability associated with astronomical transients is crucial for optimizing multi-messenger follow-up strategies and for constraining the physical origin of the transient itself. We introduce here the Targeted Detectability Range (TDR), designed to evaluate, with minimal computational effort, the detectability of compact binary coalescences under the hypothesis of association with an external messenger, such as an electromagnetic or neutrino signal. Unlike the standard GW range, which is based on averaged source parameters, the TDR incorporates prior information from observations of the external messenger, including sky localization, inclination constraints, and physically motivated bounds on component masses. We report the TDR of all short- and long-duration gamma-ray bursts, observed during the first three observing runs of Advanced LIGO and Advanced Virgo. The method is validated by performing a systematic comparison with the 90$\%$ exclusion distances provided by modeled targeted GW searches. In the absence of a coincident detection by all-sky, all-time GW searches, the TDR provides a rapid and quantitative constraint on a possible merger origin of the astrophysical source. Its low-latency implementation and public availability would enable timely prioritization of follow-up observations and optimized allocation of observational resources, with direct impact on the physical interpretation of astronomical transients.

astro-ph.HE↗

arXiv2025

Neutrino flux sensitivity to the next galactic core-collapse supernova in COSINUS

While neutrinos are often treated as a background for many dark matter experiments, these particles offer a new avenue for physics: the detection of core-collapse supernovae. Supernovae are extremely energetic, violent and complex events that mark the death of massive stars. During their collapse stars emit a large number of neutrinos in a short burst. These neutrinos carry 99\% of the emitted energy which makes their detection fundamental in understanding supernovae. This paper illustrates how COSINUS (Cryogenic Observatory for SIgnatures seen in Next-generation Underground Searches), a sodium iodide (NaI) based dark matter search, will be sensitive to the next galactic core-collapse supernova. The experiment is composed of two separate detectors which will be sensitive to far and nearby supernovae. The inner core of the experiment will consist of NaI crystals operating as scintillating calorimeters, mainly sensitive to the Coherent Elastic Scattering of Neutrinos (CE$ν$NS) against the Na and I nuclei. The low mass of the cryogenic detectors gives the experiment a sensitivity to close supernovae below 1kpc without pileup. They will see up to hundreds of CE$ν$NS events from a supernova happening at 200pc. The crystals reside at the center of a cylindrical 230T water tank, instrumented with 30 photomultipliers. This tank acts as a passive and active shield able to detect the Cherenkov radiation induced by impinging charged particles from ambient and cosmogenic radioactivity. A supernova near the Milky Way Center (10kpc) will be easily detected inducing $\sim$60 measurable events, and the water tank will have a 3$σ$ sensitivity to supernovae up to 22kpc, seeing $\sim$10 events. This paper shows how, even without dedicated optimization, modern dark matter experiments will also play their part in the multi-messenger effort to detect the next galactic core-collapse supernova.

astro-ph.HE↗