Our curves can be very misleading when it comes to selecting a lamp. A quick glance shows the irradiance increasing as we move up in lamp power. More irradiance is not necessarily better; lower power lamps have their advantages.
A lot of applications require re-imaging of the source. The lower power lamps have small radiating areas, arcs or filaments. These are as bright, and in some cases brighter than, the larger arcs or filaments of the higher power lamps. You get as much flux density on target with a small lamp as with a large. If your target (a monochromator slit, fiber, sample, etc.) is small, then you won’t do any better with a larger lamp. Note: the smaller arcs of some of the xenon lamps make them more efficient than either the mercury or QTH lamps, for many applications.
Smaller lamps are easier to operate. They require and produce less total power. In some cases, as with high power lamps, you have to use a liquid filter to get rid of the high power to protect optical components. Apart from damage to optics, a continuously running kW source will heat the laboratory and your equipment. Therefore, it is a good idea to carefully analyze your optical system so that the lowest power lamp that will serve your needs can be selected.
Comparing the 6332 50 W and 6315 1000 W QTH lamps offers an extreme example. From the curves, the kW lamp produces about 20 times the irradiance of the smaller lamp. But, the 6315 has a 6 x 16 mm filament while the 50 W lamp has a 3.3 x 1.6 mm filament. For a small target, several mm in dimension, the re-imaged smaller lamp actually produces significantly more power on target than the re-imaged kW lamp. When you need to irradiate a very large area, the kW lamp is better.
The intense UV lines make the mercury lamp the choice for many UV sensitive processes and for excitation of luminescence - particularly when you can efficiently excite with 313, 365, 404 or 436 nm radiation. When you need to scan the wavelength of the excitation source, you may be better off with the smoother xenon lamp spectrum. With the xenon lamp, you have fewer worries about the dynamic and linear range of a detection system. The rapid variation of the mercury lamp output with wavelength also puts demands on wavelength reproducibility in any application where you scan the source and where you ratio or subtract separate resulting scans.
We publish the wavelengths for the lines from our mercury spectral calibration lamps. Some of these lines are extremely narrow while others show structural broadening. The wavelength values of these lines from the low-pressure lamps, and the early alphabetical designation of some of them, are still used as labels for all mercury lines.
i Line |
h Line |
g Line |
e Line |
365.01 nm |
404.65 nm |
435.84 nm |
546.07 nm |
Our irradiance data shows broader lines and some line shifting from these generic values. Doppler broadening and self-reversal cause these changes. Since self-reversal depends on the passage of radiation through colder mercury, the exact spectral profile depends somewhat on the lamp type and envelope temperature. Figure 1 shows that the “254” line, which dominates the output of the 6035 Spectral Calibration Lamp, is substantially absorbed in the 350 W Hg lamp, model 6286 , and in fact we should speak of a 250 nm line. This is important for selection of an interference filter for this and some of the other lines.