Step 1: Use mirror formula.
\[ \frac{1}{f} = \frac{1}{u} + \frac{1}{v} \] For \(u = 3 \, \text{m}, f = 1 \, \text{m}\): \[ \frac{1}{v} = \frac{1}{1} - \frac{1}{3} = \frac{2}{3} \Rightarrow v = 1.5 \, \text{m} \]
Step 2: Linear magnification.
\[ m = \frac{v}{u} = \frac{1.5}{3} = 0.5 \] Since the image is inverted, magnification \(m = -0.5\).
Step 3: Ratio of image length to object length.
\[ \frac{L'}{L} = |m|^2 = (0.5)^2 = \frac{1}{4} \]
Step 4: Conclusion.
Hence, the ratio \(\dfrac{L'}{L} = \dfrac{1}{4}\).

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.)