ADAF SED Modeler — Accretion Spectral Energy Distribution

ADAF/RIAF (Advection-Dominated/Radiatively Inefficient Accretion Flow) applies when ṁ ≪ ṁ_crit ≈ 0.01 α². Most viscously dissipated energy is advected into the black hole rather than radiated, giving an effective luminosity L_bol = ε × ṁ × L_Edd where ε ≪ 0.1.

Synchrotron — thermal electrons in the ADAF magnetic field radiate from radio through mid-IR. The peak frequency scales as ν_peak ∝ M^(−1/2) × ṁ^(1/2), anchored to the SgrA* submm peak (350 GHz at M=4×10⁶ M☉, ṁ~10⁻⁵). For ωCen's ~8,200 M☉ IMBH, the synchrotron peaks in the 10–100 μm range — directly probed by JWST MIRI and Herschel, not by NIRCam. Below the self-absorption turnover (ν_t ≈ ν_peak/100) the spectrum rises as ν^2; above the peak it falls exponentially. The shape is ν^(1/3) in between (standard optically-thin synchrotron).

Inverse Compton — hot ADAF electrons (T_e ~ 10⁹–10¹⁰ K) Compton-scatter the synchrotron seed photons into the X-ray band. At very low ṁ, the Compton contribution is small (optical depth τ ≪ 1); it grows toward the thin-disk transition. Modelled as a power law L_ν ∝ ν^(1-Γ) with Γ = 1.7, cutting off at ~100 keV.

Bremsstrahlung — free-free emission from hot plasma. Flat from soft X-ray to the thermal cutoff at kT_e/h ≈ 430 keV (T_e=5×10⁹ K).

Bondi rate — Ṁ_B = 4π G² M² ρ_∞ / c_s³ with c_s = 300 km/s (hot stellar-wind gas). The bar shows log₁₀(ṁ_Bondi / ṁ): positive means Bondi supply exceeds the input ṁ (plausible); negative means ṁ exceeds Bondi supply (implausible at this density).