Step 1: Lens maker's formula.
\[
\frac{1}{f} = (n - 1)\left(\frac{1}{R_1} - \frac{1}{R_2}\right)
\]
Let \(R_2 = 2R_1 = 2R\). Since the lens is bi-convex, both surfaces bulge outwards.
Thus, \(R_1 = +R,\ R_2 = -2R\).
Step 2: Substitute values.
\[
\frac{1}{f} = (1.5 - 1)\left(\frac{1}{R} - \frac{1}{-2R}\right)
\]
\[
\frac{1}{f} = 0.5\left(\frac{3}{2R}\right) = \frac{3}{4R}
\]
\[
R = \frac{3}{4}f
\]
Larger radius of curvature = \(2R = \frac{3}{2}f = 1.5f\).
Step 3: Express in magnitude.
\[
\text{Hence, } \frac{\text{Larger radius}}{f} = 1.5
\]
Rounded to one decimal place: 1.5.

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.)