Yes, as you reduce the focal length you condense the radiant energy of a distant object, but there is a limit to this: the Abbe Sine Condition. When you reach the state where the focal length is half the aperture, then the only way to reduce the focal length further is to reduce the aperture and then, of course, you reduce the afferent flux at the lens so the energy density of the image remains the same. You cannot achieve light amplification through optics alone.
Actually you can, but not in the traditional context of light from a subject passing through a lens and being focused on a plane somewhere outside the lens. Consider the following thought experiment:
Suppose you have a sphere of transparent material having a refractive index of 2.37 and a radius of 2.37cm. One of the corollaries of
Snell's Law is that all photons that refract into the sphere will pass through a region in the center of the sphere having a radius equal to (R * I / A), where R is the radius of the sphere, A is the speed of light in the sphere's ambient environment, and I is the speed of light within the sphere. If the sphere is in a vacuum, this can be simplified to (radius of sphere) / (refractive index of sphere). The following diagram illustrates this:
[attachment=19523:HemiLens.png]
The blue lines represent photon paths, some of which refract into the sphere, and some of which bypass the sphere's surface. But as you can see, all of the photons that enter the sphere pass through a region in the center of the sphere that is inversely proportional to the refractive index of the sphere. If we hollow out this 1cm region in the center of the sphere and optically bond an absorptive coating to this newly-created inner surface, all photons that enter the sphere will intersect this inner absorptive surface. Assuming an isotropic distribution of photons intersecting the outer surface of the sphere, the photon flux density at this inner surface will be equal to the square of the refractive index of the sphere (the ratio of the area of the outer surface of the sphere divided by the area of the inner surface of the sphere), minus reflective losses (photons that reflect off the surface of the sphere instead of refracting into the sphere). These losses can be calculated by
Fresnel's equations.
For a lens having a refractive index of 2.37, these losses are approximately 29.49% (assuming an isotropic distribution of photons intersecting the outer surface of the sphere). The following diagram shows this visually:
[attachment=19524:ABPower.png]
The red line represents total power isotropically distributed relative to the surface of the sphere. The green line represents the percentage of photons that will refract into the surface of the sphere instead of reflecting off the surface of the sphere, given a refractive index of 2.37. The black line is the product of the red line and the green line. The area below the red line graphically represents the total energy of the photon flux at the sphere's outer surface. The area below the black line represents the portion of the total energy that actually enters the sphere, and the area between the black line and the red line represents energy that reflects off the surface of the sphere.
Thus, if the isotropic photon flux density at the outer surface of the sphere is 100 W/m^2, the photon flux density at the inner surface of the sphere will be:
100 * 2.37^2 * (1 - 0.2949) = 396.02 W/m^2
The astute observer will note that this has some interesting ramifications with regard to thermodynamics and equilibrium.