By use of a full factorial design method, some different wavelength regions were selected by taking into account different spectral parameters including the starting wavelength, the ending wavelength and the wavelength interval.
As the Bi composition further increases, the PL wavelength starts to blueshift and the PL intensity decreases.
Excitation-emission maps of the samples were obtained by scanning the excitation wavelength, starting at 280 nm and ending at 480 nm in steps of 10 nm, while detecting the emission light from 300 800 nm.
Now, thanks to large space facilities, such as Herschel and Planck, results from longer wavelengths start to appear (e.g., Maddox et al., 2010; Cooray et al., 2010; Amblard et al., 2011; Magliocchetti et al., 2011; Planck Collaboration et al., 2011).
Measurements started at a wavelength of 350 nm and were continued until 700 nm in 5 nm steps.
They can be listed as radio window represented by electromagnetic wavelengths starting from 15 MHz up to 300 GHz, optical window represented by electromagnetic wavelengths starting from 150 THz up to 1000 THz, microwave window represented by electromagnetic wavelengths starting from 23.1 THz up to 37.5 THz.
As the size of motors and actuators shrink because of miniaturization, the presence of the longer wavelengths will start to impinge on the scale of the scanning microscopes.
The light being seen from the remotest objects in the UDF would have started out as short wavelength (ultraviolet) emission that was then subsequently stretched to longer (infrared) wavelengths by the expansion of the Universe.
For the PL measurement, the recording of the intensity of the emission light often starts after the excitation wavelength to void the damage of the PMT detector.
For the ZnSe0.73S0.27 crystal, absorption starts at a lower wavelength range (300 nm) when compared to the ZnSe0.91S0.09 crystal presumably due to the much higher bandgap of ZnS than that of ZnSe.
