PeV ν and PeV γ Without New Particles: Classical Budgets vs. Future–Mass Projection (FMP)

The IceCube discovery of a diffuse astrophysical neutrino flux up to the PeV scale and the LHAASO detection of ultrahigh-energy (UHE) γ-rays up to ∼PeV pose tight constraints on Galactic accelerators. In standard microphysics, diffusive shock acceleration (DSA) in finite-age sources is typically time- or loss-limited. We show that the Future–Mass Projection (FMP) framework—a causal, future-conditioned gravitational response calibrated on the Milky Way (MW)—provides a disciplined multiplicative boost (× √ D to ×D) to the classical budget, sufficient to lift ordinary environments over the thresholds required by PeV ν and PeV γ. With MW-validated values D(R0)≈1.46 and D(20–25 kpc)≈2.5–2.9, a representative Solar-circle SNR reaches Eν,max≃0.9–1.1 PeV (vs. 0.75 PeV classical), and outer-disk sites reach Eν,max ≃ 1.2–2.0 PeV. For a conservative molecular-cloud shock (J2108+5157–like), Eγ,max rises from ∼0.27 PeV (classical) to ∼0.45–0.73 PeV with FMP; for a moderate setup, from 1.26 PeV to ∼2.1–3.4 PeV. The program yields falsifiable predictions (radial trends, MC/CGM correlations, and a gentle R(z) drift).