Treating macro-black hole as quantum states, and using Brown-York's quasi-local gravitational energy definition and Heisenberg uncertainty principle, the GHS black hole's quantum horizon is constructed. The Hawking temperature is computed naturally, and the entropy can also be figured out without introducing the cutoff factor h. The -field mode number is predicted too. The result is consistent with that of the Schwarzschild and R-N black hole.Keywords Quantum states · Brown-York's quasi-local gravitational energy · Hawking temperatureThe quantum mechanics and the quantum field theory in curved space-time with classical event horizon provides a framework to understand the statistic origin of the thermodynamics of non-extreme black hole, and serves as a powerful tool to calculate its entropy and the Hawking radiation temperature. In these problems, there are many ambiguous points like (a) the ultraviolet(UV) cutoff in the brickwall model (BWM) to avoid the divergence [1, 2]; (b) the analytic continuing trick to go over the singularity associating with the classical horizon [3,4], etc. We still face an unsatisfactory situation that if one set up a brick wall for getting the entropy rightly, it will be no way to do analytic continuing and hence no way to derive the Hawking temperature. On the other hand, once withdrawing the wall or the UV cutoff, it will be no way to handle the entropy even though the Hawking temperature can be calculated. How to solve this dilemma? Recently Yans' works [5][6][7] solved the dilemma using the semi-classical effect at the horizon, which naturally led to the space-time noncommutative at the horizon, called as quantum horizon. In this treatment the classical horizon spreads, so the trouble due to the singularity on the horizon disappears. They have discussed the Schwarzschild