Cassini VIMS sees the long-awaited glint off a Titan lake
The Cassini mission announced today the first observation of a specular reflection off of a lake on Titan. A specular reflection is a mirror-like flash, and you only get one when you have a mirror-like surface -- very, very smooth. That's hard to do in nature except with a liquid surface (or a surface that froze from a liquid, such as ice and certain types of lava flows). I'll summarize the long road to the specular reflection below, but first, here's the image, certain to become an iconic one of Titan.
NASA / JPL-Caltech / University of Arizona / DLR
Specular reflection off of a Titan lake
On July 8, 2009, Cassini finally saw the telltale glint of sunlight specularly reflecting off of the mirror-like surface of a lake on northern Titan. This image is from the VIMS instrument employing infrared light at a wavelength of 5 microns, and has been colorized to match visible-light pictures of Titan.
Scientists have been hunting for specular reflections off of Titan ever since the notion of liquid hydrocarbons covering some or all of the moon was first proposed by Jonathan Lunine, Dave Stevenson, and Yuk Yung in 1983. (Here's the Science abstract.) Subsequent work (by Caitlin Griffith and coauthors) found evidence for water ice on Titan's surface, suggesting at least that a global methane ocean wasn't likely. In 2003, scientists using the Arecibo radio telescope (a team led by Donald Campbell) reported a "small specular component" to the reflections of radio signals off of Titan and suggested that there may be lakes scattered across the surface.
NASA / JPL / University of Arizona
Color view of Titan from VIMS
Combining three images taken at wavelengths of 2.0, 2.8, and 5.0 microns gives VIMS a colorful map of Titan's surface, indicating plenty of surface diversity, not a global ocean of methane, and no specular reflections. (The bright spot, near the south pole, is because of clouds there.)
Cassini finally arrived at the Saturn system in June of 2004, and most of its instruments were designed, in part, with studying Titan in mind. The RADAR instrument, for instance, was included primarily to peer past Titan's haze and map the moon (though of course it uses Cassini's main radio communications dish). The main cameras have numerous filters that are intended specifically for employing skinny "windows" in near-infrared wavelengths where the atmospheric methane is less absorbing to attempt to see the surface. Their vision is far blurrier than the RADAR instrument at Titan, but they can image the whole moon while RADAR just gets skinny strips.
But the real promise for imaging Titan has always been in the Visual and Infrared Mapping Spectrometer, or VIMS -- or at least that's what the VIMS team says! Where ISS (the Imaging Science Subsystem, or main cameras) can only see out to wavelengths of one micron, VIMS can see out to five microns. VIMS has lower spatial resolution than ISS, but it overcomes that deficit at Titan using the longer wavelength, because Titan's atmosphere is much, much, much more transparent at the longer near-infrared wavelengths than it is in the shorter-wavelength windows accessible to ISS.
This region seen by Cassini RADAR on February 15, 2005 is covered with sets of black linear features that were (at the time) referred to as "cat scratches" for lack of any obvious explanation for their origin. The scene covers an area about 240 kilometers (150 miles) top to bottom.
The Huygens landing in January of 2005 showed plenty of evidence for past fluvial activity, but the dark area that the probe landed in seemed as dry as a desert (except for an interesting puff of methane detected after the probe had warmed the ground following its landing, interpreted as possible evidence for methane wetting the ground just beneath the dry surface).
ESA / NASA / GSFC / ASI / GCMS Team
Increase in methane observed after impact by GCMS
This graph of data from the Huygens GCMS instrument shows the increase of nitrogen and methane during the probe descent and the rapid and important increase in methane at the surface.
The footprint-like feature in the upper left corner of this image is Ontario Lacus, a hydrocarbon lake. It is roughly 234 kilometers long by 73 kilometers wide, about the size of Lake Ontario (a lake on the U.S.-Canadian border). The red cross below center identifies the location of Titan's south pole.
Cassini's "T16" flyby on July 22, 2006 took it up to high latitudes near the north pole. RADAR images across the region contain numerous very dark splotches with sharp-edged boundaries, which may be the long-sought methane or ethane lakes on the surface of Titan. This image is centered near 78 degrees north, 18 degrees west measures about 475 kilometers by 150 kilometers (295 miles by 93 miles).
Interestingly, while RADAR also saw lakes in the south, there were not nearly as many there (at the summer pole) as in the north (the winter pole). Oded Aharonsen and coauthors presented an explanation at the American Geophysical Union meeting a year ago, having to do with "superseasons" on Titan (go nearly to the bottom of that blog entry for my summary); that work was just published a couple of weeks ago in Nature Geoscience.
Changes near Titan's south pole, Oct. 2007 to Dec. 2008
A comparison of the same area as seen on two different Cassini RADAR flybys shows that some lakes near Titan's south pole dried up during the intervening 14 months.
In the end, we don't really need the VIMS specular reflection to be sure there are lakes near Titan's north pole. But I have to say that I am awfully relieved to finally see it, and I wonder if Titan researchers feel the same way. A specular reflection should have been the "smoking gun" for Titan lakes; its absence was deeply puzzling. Now we know that the reason nobody saw it was because the lakes are mostly only found near the north pole. To see a specular reflection from a flat surface near the north pole of a world, you first need to have light shining on it -- and it's been winter in Titan's north since Cassini arrived. Only recently did sunlight start shining on Titan's lake district.
Then, once you have sunlight, the spacecraft has to be in exactly the right place to see a flash. If there were lakes anywhere in the equatorial or temperate latitudes, it wouldn't have been hard for Cassini to spot a specular reflection from them on any of its numerous Titan flybys (of which there have been 64 to date, plus lots of observations from greater distances). But with the flat surface located near the pole, there are only a few situations where the sun-lake-Cassini angle will line up just right to make that glint visible to Cassini's cameras. So, finally, it happened in July. Cassini was practically behind Titan as seen from the Sun; Titan's phase was almost "new" to Cassini. Under that one unique geometry, Cassini finally saw what so many scientists have been looking for for so many years.
Many congratulations to the VIMS team for finally making this observation!