📡 DRAFT RESEARCH PROPOSAL · KM3NeT/ARCA · NEUTRINO ASTRONOMY

KM3NeT/ARCA Neutrino Search for Technosignature Emission from Omega Centauri

A dedicated time-integrated and time-dependent point-source analysis targeting Hawking-like neutrino emission from Omega Centauri's intermediate-mass black hole candidate, as theorized by Dvali & Osmanov (2023) · Working draft for collaboration and funding development · April 2026

1. Principal Investigator Statement

We propose a dedicated time-integrated and time-dependent neutrino point-source analysis centered on Omega Centauri (ω Cen, NGC 5139), targeting Hawking-like emission from engineered quantum black holes as theorized by Dvali & Osmanov (2023). This analysis will constitute the most sensitive search to date for technosignature-motivated neutrino emission from this source, leveraging the unique geometrical advantages of KM3NeT/ARCA for southern-sky sources.

We emphasize that this is a null-hypothesis-grounded observational program: the most parsimonious explanation for OC's electromagnetic silence is gas starvation of a quiescent IMBH, not ETI activity. A null result at design sensitivity would itself constitute a meaningful scientific constraint on any Hawking-like emission from the cluster core, regardless of its origin.

2. Scientific Rationale

2.1 Target: Omega Centauri

Omega Centauri is the Milky Way's most massive globular cluster (M ≈ 4×10⁶ M☉, ~10⁷ stars) at a distance of 5.49 ± 0.06 kpc (~17,900 ly) — the most precise kinematic distance available (Häberle et al. 2025, ApJ 983, 95; oMEGACat VI). It is widely accepted as the stripped core of an ancient dwarf galaxy.

In 2024, Häberle et al. reported seven fast-moving stars within the central 3″ (0.08 pc) whose velocities exceed the local escape speed, requiring a compact mass with:

• Velocity-only lower bound: M ≳ 8,200 M☉ (Häberle et al. 2024, Nature 631, 285)
• With acceleration constraints (99% CL, paper body §4): M ≳ 21,100 M☉
• N-body simulation best-fit: ~50,000 M☉ (±20,000) (González Prieto et al. 2025, ApJL 990, L69; arXiv:2507.06316)

2.2 Technosignature Hypothesis

Dvali & Osmanov (2023, Int. J. Astrobiology 22, 617–640) propose that sufficiently advanced civilisations may employ quantum black holes as computational substrates, maximising information storage (Bekenstein bound) and processing rates (Margolus-Levitin theorem). The associated Hawking-like emission would be "democratic" across particle species, including high-energy neutrinos detectable with km³-scale neutrino telescopes.

Crucially, this framework does not predict a specific flux. The proposal is motivated by the absence of a dedicated search, not by any positive evidence. ω Cen's IMBH candidate, quiet core environment, and optimal declination for ARCA make it a well-motivated first target for such a search.

2.3 Why KM3NeT/ARCA Is the Preferred Instrument

ω Cen's declination (δ ≈ −47°) places it in KM3NeT/ARCA's optimal upgoing field of view:

• Upgoing geometry: δ = −47° is nearly always below the horizon at Capo Passero, giving strong atmospheric muon background suppression via Earth shielding
• Angular resolution: <0.1° for track events at E ≳ 10 TeV (KM3NeT Collaboration, Eur. Phys. J. C 84, 885, 2024)
• Full-array sensitivity (E⁻²): ~few × 10⁻¹²–10⁻¹¹ TeV cm⁻² s⁻¹ at δ ≈ −47° for multi-year exposures
• Southern-sky advantage over IceCube: IceCube detects OC as a downgoing source with higher atmospheric muon contamination; ARCA's geometry is geometrically superior for this declination

3. Observation Strategy

3.1 Dataset

Primary instrument: KM3NeT/ARCA (Capo Passero, Sicily, 3,500 m depth)

Current status: 51 of 230 detection units deployed as of end-2025 (~22% complete). Already detecting PeV-scale events (KM3-230213A, 120 PeV; Nature 638, 376, 2025). This proposal targets both current partial-array data and accumulated Phase 2 data.

3.2 Time-Integrated Point-Source Analysis

We employ an unbinned maximum likelihood analysis (ULMA) following established KM3NeT/ARCA and IceCube point-source methodologies:

Where S is the signal PDF (2D Gaussian PSF × power-law spectrum E^−γ) and B is the background PDF estimated from RA-scrambled events preserving the local sidereal time (LST) distribution.

Spectral hypotheses tested: E⁻² (Fermi-acceleration benchmark), E⁻²·⁵ (softer), E⁻¹·⁵ (burst-harder)

Systematics as nuisance parameters:

• Effective area uncertainty: 10–15% (correlated across declination)
• Angular resolution: ±0.05° in Gaussian width
• Atmospheric ν flux normalisation: ±5%

Deliverables: median 90% CL E⁻² sensitivity and 5σ discovery flux at δ ≈ −47°; flux upper limit for ω Cen; pre-trial p-value sky map within 5° of ω Cen.

3.3 Time-Dependent Burst Search

Kugelblitz scenarios predict transient neutrino/γ-ray flash events from micro-black-hole creation and rapid Hawking evaporation. We add a dedicated burst search:

• Time windows: 100 s, 1,000 s, 10,000 s — scanned across full exposure
• Background: time-scrambled events preserving LST distribution
• Trials correction: 3 window sizes × number of LST bins
• Multi-messenger coincidence: Fermi-LAT GCN triggers and IACT public alerts within ±500 s; AMON/GCNC infrastructure for real-time coincidence
• Significance threshold: ≥5σ post-trials for any publication-worthy claim

3.4 Multi-Wavelength Cross-Checks

• Fermi-LAT: 15+ year all-sky likelihood analysis at 0.1–300 GeV at ω Cen position
• IACT archival: H.E.S.S./MAGIC/VERITAS TeV upper limits
• ToO trigger criteria: pre-specified for any >3σ neutrino excess
• ATCA/MeerKAT radio: cross-check with Mahida et al. (2025) existing deep limits
• JWST: Chen et al. (2025) NIRCam/MIRI non-detection as complementary constraint

4. Expected Outcomes and Scientific Value

4.1 Null Result (Most Likely)

A non-detection at design sensitivity is expected and scientifically valuable:

• First dedicated, high-sensitivity neutrino limits on ω Cen technosignature emission
• 90% CL upper limits on steady E⁻² and E⁻²·⁵ emission at ARCA sensitivity level
• Constraints on kugelblitz event rates — upper limit on burst frequency
• Joint neutrino + γ-ray limits constraining hadronic models for any hidden engine
• Demonstrating that the observational channel is now closed at motivated flux levels

4.2 Detection

A statistically significant neutrino cluster (≥5σ post-trials) spatially coincident with ω Cen, not correlated with known γ-ray sources, would constitute a compelling candidate given the known IMBH candidate and absence of conventional astrophysical accelerators. It would immediately warrant multi-wavelength follow-up and independent telescope confirmation.

5. Work Plan

6. Budget Justification

7. References