in Matlab

According to Planck's law of black-body radiation, the spectral energy density R as a function of wavelength X (m) and temperature T (K) is given by: R = 2 pi c^2 h/lambda^5 1/e^hc/lambda kT -1 where c = 3 times 10^8 m/s is the speed of light, h = 6.626 times 10^-34 J-s is Planck constant, and k = 1.38 times 10^-23 J/K is Boltzmann constant. Make the shown figure that contains plots of R as a function of lambda for 0.1 lessthanorequalto A lessthanorequalto 3 mu m for three temperatures T =3.000K, T = 4,000K, and T = 5,000K. Write a script file to make the plot as shown with single plot command and different color for each curve. Use 100 points for the lambda domain. The line styles, axes labels, axes limits, and legend must be the same as that shown in Figure. According to Planck's law of black-body radiation, the spectral energy density R as a function of wavelength X (m) and temperature T (K) is given by: R = 2 pi c^2 h/lambda^5 1/e^hc/lambda kT -1 where c = 3 times 10^8 m/s is the speed of light, h = 6.626 times 10^-34 J-s is Planck constant, and k = 1.38 times 10^-23 J/K is Boltzmann constant. Make the shown figure that contains plots of R as a function of lambda for 0.1 lessthanorequalto A lessthanorequalto 3 mu m for three temperatures T =3.000K, T = 4,000K, and T = 5,000K. Write a script file to make the plot as shown with single plot command and different color for each curve. Use 100 points for the lambda domain. The line styles, axes labels, axes limits, and legend must be the same as that shown in Figure