Step 1: Identify ensemble constraints.
The ensemble has fixed:
• Number of particles,
• Pressure,
• Temperature (N, P, T).
Step 2: Connect constraints to thermodynamic potentials.
Each ensemble is described by a thermodynamic potential that is minimised under its natural variables:
• Helmholtz free energy $F$ → natural variables $(T, V)$,
• Gibbs free energy $G$ → natural variables $(T, P)$,
• Enthalpy $H$ → natural variables $(S, P)$.
Step 3: Compare with given ensemble.
Since the ensemble is at fixed $(T,P)$, the appropriate potential is Gibbs free energy $G=H-TS$.
Step 4: Conclusion.
The thermodynamic function describing such an ensemble is the Gibbs free energy.

At a particular temperature T, Planck's energy density of black body radiation in terms of frequency is \(\rho_T(\nu) = 8 \times 10^{-18} \text{ J/m}^3 \text{ Hz}^{-1}\) at \(\nu = 3 \times 10^{14}\) Hz. Then Planck's energy density \(\rho_T(\lambda)\) at the corresponding wavelength (\(\lambda\)) has the value \rule{1cm}{0.15mm} \(\times 10^2 \text{ J/m}^4\). (in integer)
[Speed of light \(c = 3 \times 10^8\) m/s]
(Note: The unit for \(\rho_T(\nu)\) in the original problem was given as J/m³, which is dimensionally incorrect for a spectral density. The correct unit J/(m³·Hz) or J·s/m³ is used here for the solution.)

