The High Altitude/ Re-Entry Vehicle Infrared Imaging (HARVII) system is a portable instrumentation system for tracking and thermal imaging of a possibly distant and moving object. The HARVII is designed specifically for measuring the changing temperature distribution on a space shuttle as it reenters the atmosphere. The HARVII system or other systems based on the design of the HARVII system could also be used for such purposes as determining temperature distributions in fires, on volcanoes, and on surfaces of hot models in wind tunnels. In yet another potential application, the HARVII or a similar system would be used to infer atmospheric pollution levels from images of the Sun acquired at multiple wavelengths over regions of interest.
The HARVII system includes the Ratio Intensity Thermography System (RITS) and a tracking subsystem that keeps the RITS aimed at the moving object of interest. The subsystem of primary interest here is the RITS (see figure), which acquires and digitizes images of the same scene at different wavelengths in rapid succession. Assuming that the time interval between successive measurements is short enough that temperatures do not change appreciably, the digitized image data at the different wavelengths are processed to extract temperatures according to the principle of ratio-intensity thermography: The temperature at a given location in a scene is inferred from the ratios between or among intensities of infrared radiation from that location at two or more wavelengths. This principle, based on the Stefan-Boltzmann equation for the intensity of electromagnetic radiation as a function of wavelength and temperature, is valid as long as the observed body is a gray or black body and there is minimal atmospheric absorption of radiation.
In this particular variant of ratio-intensity thermography, the wavelengths are chosen to be in the near infrared part of the spectrum and are selected to minimize effects of atmospheric absorption. A nearly ideal pair of wavelengths for minimizing effects of atmospheric absorption would be 1.3 and 1.69 μm. An additional advantage of this choice of wavelengths is that conventional, high-quality, commercial optics work well at wavelengths below about 2 μm; if longer wavelengths were chosen, it would be necessary to design and build special infrared optical components.
In practice, it was necessary to choose 1.55 μm as the longer of the two wavelengths because the infrared camera available at the time of development of the RITS was found not to be usable out to 1.69 μm. In addition, the pass bands of the filters used to select these observation wavelengths were required to be 10 to 20 nm wide in order to enable the acquisition of sufficiently strong signals. The finite widths of these pass bands contribute to variations of atmospheric effects at different water-vapor levels. The use of three or more wavelengths could enable almost complete correction for these effects. Alternately, if one continued to use two wavelengths, then corrections could be derived from measurements made by a spectrometer aimed at the Sun.
This work was done by Leonard Weinstein and Jason Hundley of Langley Research Center.