“…Most objects outwardly radiate electromagnetic waves in the MIR band like a blackbody. According to the Stefan–Boltzmann law, the temperature of an object can be measured by detecting the radiation power within a specific band , T r = P − 1 ( ε IR , T ) where T r represents the temperature obtained using the inverse function of the blackbody radiation spectrum, P represents the radiation power detected by an IR detector and corresponds to the radiation power radiated by a blackbody at temperature T , and ε IR represents the emissivity of the IR detector in the operating band; for an IR camera, ε IR = 1. The detection power of an IR imager is generally determined by the radiation emitted from the object and that reflected from the environment: P ( ε , T ) = P rad ( ε , T ) + P ref ( ε , ε normala , T normala ) = ε ( λ ) I BB ( T ) + [ 1 − ε false( λ false) ] ε a ( λ ) I BB ( T normala ) where ε and ε a represent the emissivities of the object and ambient environment, respectively; T and T a represent the temperatures of the object and ambient environment, respectively; and I BB represents the blackbody irradiance at the corresponding temperature.…”