CICLOPS: Cassini Imaging Central Laboratory for OPerationS
Three Methane Wavelengths

Three Methane Wavelengths
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619 nm 1025x924:
GIF 818 KB


Three Methane Wavelengths
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727 nm 1027x924:
GIF 732 KB


Three Methane Wavelengths
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890 nm 1024x924:
GIF 1.0 MB
  The ISS cameras come equipped with filters that sample three wavelengths where methane gas absorbs light. These are in the red at 619 nano-meter (nm) wavelength and in the near-infrared at 727 nm and 890 nm. Absorption in the 619 nm filter is weak. It is stronger in the 727 nm band and very strong in the 890 nm band where 90% of the light is absorbed by methane gas. Light in the weakest band can penetrate the deepest into Jupiter's atmosphere and is sensitive to the amount of cloud and haze down to the pressure of the water cloud (about 6 times the atmospheric pressure at sea level on the earth). Light in the strongest methane band is absorbed at high altitude and is sensitive only to the ammonia cloud level and higher (pressures less than about 1/2 of an atmosphere) and the middle methane band is sensitive the ammonia and ammonium hydrosulfide cloud layers as deep as 2 times atmospheric pressure. The images shown here demonstrate the power of these filters in studies of cloud stratigraphy. The images cover latitudes from about 15 N at the top down to the southern polar region at the bottom. The top two images are ratios, the image in the methane filter divided by the image at a nearby wavelength outside the methane band. By taking ratios we are able to isolate contrast due to methane absorption and not to other factors such as the absorptive properties of the cloud particles which influence contrast at all wavelengths.

The most prominent feature seen in all three filters is the polar stratospheric haze which makes Jupiter bright near the pole. The equatorial band is also very bright in the strong 890-nm image and to a lesser extent in the 727 band (middle image) but is subdued in the weak 619-nm image at the top. These are high thin haze layers that are nearly transparent at wavelengths outside the methane absorption bands. Another prominent feature is the Great Red Spot. About a third of it appears at the right-hand edge of the frame. It is a bright feature in methane absorption because it has extensive cloud cover reaching to high altitude. A wisp of high thin cloud can be seen trailing off its western rim in the middle and lowest images.

Features mentioned above have been seen from ground-based telescopes and from the Hubble Space Telescope and from the Galileo spacecraft. This is the first time we have had high-resolution images in all three methane bands and a comparison of all three reveals some interesting features. Chief among these is the very dark patch seen in the top (weak methane) image near the top-middle of the frame. It is almost invisible in the bottom image and it appears to be composed of strands of bright clouds in the middle image. This is a region which is similar to the hot spot where the Galileo Probe entered Jupiter's atmosphere. These images indicate that cloud cover is present at the higher altitudes but absent from the lower altitudes. This is also what the Galileo Probe found when it entered Jupiter's atmosphere.

To the northwest (above and to the left) of the dark feature is a small cloud which is bright in the 619-nm (top) image but has no contrast at the other wavelengths. This is the signature expected for a thick water cloud. Another feature seen only in the weak-methane (top image) ratio is a dark ring near the center of the image. This feature is probably an anticyclonic (counter-clockwise rotating) upwelling core surrounded by a sinking perimeter with diminished cloudiness. The fact that it is seen only in the weak methane ratio indicates that we are seeing the effects of a lower-level circulation which does not penetrated to the upper ammonia cloud level and may be confined to the deeper water cloud.

The opposite behavior is evident in an oval which is dark in the middle and bottom images but is absent in the weak 619-nm image. It is located to the southwest of the Great Red Spot. Further to the west at slightly more northerly latitudes are a series of small spots which are dark at all wavelengths. These and a myriad of other contrast features at many latitudes reveal much about Jupiter's complicated cloud structure and meteorology.

The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini-Huygens mission for NASA's Office of Space Science, Washington, D.C. The imaging team consists of scientists from the US, England, France, and Germany. The imaging operations center and team lead (Dr. C. Porco) are based at the Space Science Institute in Boulder, Colo.

For more information about the Cassini-Huygens mission, visit and the Cassini imaging team home page,

Credit: NASA/JPL/University of Arizona
Released: December 28, 2000
Image/Caption Information