The surface brightness Σ of an astronomical object is its observed flux divided by its observed angular area; thus, Σ∝f/(δθ)2. For a class of objects that are both standard candles and standard yardsticks, what is Σ as a function of redshift? Would observing the surface brightness of this class of objects be a useful way of determining the value of the deceleration parameter q0? Why or why not?