A Global 7% Systemic Sensitivity Floor in Gaia DR3: Multi-Wavelength Validation using 2MASS, Pan-STARRS and the 0.75-Magnitude Offset

Original Abstract

This study performs a multi-wavelength astrometric and photometric examination of a high-confidence sample $(N = 120,418)$ derived from a parent population of 2.36 million unique WDSS-seeded systems. By establishing an empirical polynomial ridge line for the broader Gaia-2MASS-Pan-STARRS subset, we calculated magnitude residuals $(ΔG)$ to probe the systemic limits of the Gaia single-star model. Results reveal a distinct "Detection Gap" manifested as a tri-modal distribution: 14,705 stars $(12\%)$ were identified as overt Astrometric Discordance failures $(\mathrm{RUWE} > 1.4)$, while a significant subset of candidates exhibits signs of Astrometric Suppression -- where dual-flux profiles are absorbed into a stable single-star solution $(\mathrm{RUWE} < 1.4)$ despite the physical presence of a companion. Crucially, while the raw failure rate reaches $12\%$ globally, we identify an asymptotic Intrinsic Binary Residual (IBR) of $\approx 7.0\%$ $(\approx 8,429$ sources) that persists independently of stellar density. Utilizing a "Triple Constraint" framework -- astrometric noise (RUWE), photometric excess $(ΔG)$, and the absence of official Non-Single Star (NSS) classification -- we identify a $5.9\%$ Detection Gap subset within the Gaia-2MASS audit chain that is consistent with a population of "orphaned" binaries clustered near the theoretical -0.75 magnitude "Binary Ridge." This $7\%$ floor is interpreted here as an apparent global sensitivity limit in the Gaia pipeline, suggesting that local stellar mass density models -- which rely on single-star mass-to-light ratios -- may require a quantifiable correction to accurately reflect the local baryonic mass budget.