Gravitational black hole shadow spectroscopy

In this work, we develop a generalized perturbative framework for gravitational shadows in static, spherically symmetric spacetimes. Building upon the recent two-parameter perturbative framework of K. Kobialko [Perturbation theory for gravitational shadows in static spherically symmetric spacetimes, .], this work extends the expansion in particle energy and metric deviation to encompass arbitrary, simultaneous deformations of all metric functions. By relaxing the common restriction of a fixed area radius <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"> <a:mo stretchy="false">(</a:mo> <a:mi>β</a:mi> <a:mo stretchy="false">(</a:mo> <a:mi>r</a:mi> <a:mo stretchy="false">)</a:mo> <a:mo>=</a:mo> <a:msup> <a:mi>r</a:mi> <a:mn>2</a:mn> </a:msup> <a:mo stretchy="false">)</a:mo> </a:math> , our formalism applies to a significantly broader class of alternative gravity theories and exotic compact objects. We derive analytical formulas for the massive shadow radius up to the second order in the deformation parameter, explicitly revealing the phenomenological signatures that arise from the coupling between temporal and spatial metric perturbations. The key result is that the distinct energy dependence of the massive shadow provides a powerful method to disentangle these different types of geometric deformations, breaking observational degeneracies inherent in the photon shadow alone. We demonstrate this principle with applications to traversable wormholes and canonical scalar-tensor solutions, showing how each produces a unique, distinguishable energy-dependent fingerprint. This generalized framework provides a robust, theory-agnostic tool for testing strong-field gravity. It offers a clear methodology for reconstructing metric parameters from potential multimessenger observations of massive particle shadows.