latestHeader1=LIQUID LAKES &latest1=Radar imaging data from the Cassini flyby of July 22, 2006, published recently in the journal Nature, provide convincing evidence for large bodies of liquid on Titan. This image, used on the journal's cover, gives a taste of what Cassini saw. Intensity in this colorized image is proportional to how much radar brightness is returned, or more specifically, the logarithm of the radar backscatter cross-section. The colors are not a representation of what the human eye would see. The image is centered near 80 degrees north, 35 degrees west and is about 140 kilometers (84 miles) across. Smallest details in this image are about 500 meters (1,640 feet) across. & &latestHeader2=TWO SIDES OF DUNES &latest2=This pair of images, taken by the Cassini spacecraft radar mapper on two different Titan passes, represent two different views of a field of dunes located near 9.4 degrees south latitude by 290 degrees west longitude. The images were taken in synthetic aperture mode and each image is approximately 400 kilometers (250 miles) long by 275 kilometers (170 miles) wide. The images are different only because the radar instrument illuminated the dunes from different directions. Most obvious differences are seen in the large bright feature at the center of both images. At left, its left edge is brighter, emphasizing the more steep slopes there. Farther left, the dunes are more clearly defined in the right image as their faces are caught by the illumination. & &latestHeader3=IMPROVED VIEW &latest3=This mosaic provides the best view yet obtained by Cassini's cameras, showing terrain on the moon's sub-Saturn hemisphere -- the side of the moon that always faces toward Saturn. This mosaic has better resolution compared to previous views of the area. "Signal-to-noise" is a term scientists use to refer to the amount of meaningful or useful information (signal) in their data versus the amount of background noise. A higher signal-to-noise ratio yields sharper, clearer views of Titan's surface. The view is centered on terrain in the Fensal-Aztlan region on Titan, at 0.03 degrees south latitude, 22.18 degrees west longitude. The mosaic covers an area 3,500 kilometers (2,180 miles) north to south and 3,600 kilometers (2,240 miles) west to east. North is up. & &latestHeader4=INFRARED AND RADAR COMPOSITE &latest4=This image composite contains a radar image taken during a February 2005 flyby, and overlaid are images from the visual and infrared mapping spectrometer taken on September 7 and October 25, 2006. The thin strip is the infrared image taken on the inbound leg of the flyby and crosses the radar image near an area with a small, crater-like feature. In the radar image a faint fan of material seems to originate at the crater, and the portion of the infrared image that crosses the faint fan shows both a large brightness contrast and very sharp boundaries. These details support the idea that the deposit seen in the radar images is a flow of material erupted from the small crater. This may be the strongest evidence yet of cryovolcanism on Titan. & &latestHeader5=LARGE TECTONIC COMPLEX &latest5=This infrared image set was taken at a distance of 15,000 kilometers (9,300 miles) from Titan and shows two views of an area riddled by mountain ranges that were probably produced by tectonic forces. Near the bottom of the right image, a band of bright clouds is seen. These clouds are probably produced when gaseous methane in Titan's atmosphere cools and condenses into methane fog as Titan's winds drive air over the mountains. It was once thought that these recurring clouds were produced by volcanic activity on Titan, but this image calls that idea into question. & &latestHeader6=TITAN'S SIERRAS &latest6=This composite image shows a massive mountain range running just south of Titan's equator. Near the center of the image, the mountain range runs from southeast to northwest. It is about 150 kilometers long (93 miles) and 30 kilometers (19 miles) wide and about 1.5 kilometers (nearly a mile) high. This range, and smaller ranges to the west and east of the main range, probably results from material welling up below as the crust of Titan is pulled apart by tectonic forces. & &latestHeader7=TITAN'S GREAT LAKES? &latest7=Using its radar system, the Cassini spacecraft imaged new lakes on Titan on October 9, 2006. The large dark patch seen on this image, at high latitudes surrounding Titan's north pole, is most likely a hydrocarbon lake. Several dark channels can be seen; the longest one at the left meanders over almost 100 kilometers (62 miles), and appears to drain into the lake. Some dark channels are remarkably straight, suggesting possible faulting in the subsurface. & &latestHeader8=TITAN'S HALO &latest8=Titan's murky atmosphere shines as a halo of scattered light in this image acquired with the Cassini spacecraft narrow-angle camera on August 10, 2006. The image was taken using a spectral filter sensitive to wavelengths of infrared light centered at 938 nanometers. The image was acquired with the Cassini spacecraft narrow-angle camera at a distance of approximately 3.1 million kilometers (1.9 million miles) from Titan. & &latestHeader9=SHOREFRONT PROPERTY, ANYONE? &latest9=This lake is part of a larger image taken by the Cassini radar instrument during a flyby of Saturn's moon Titan on September 23, 2006. It shows clear shorelines that are reminiscent of terrestrial lakes. With Titan's colder temperatures and hydrocarbon-rich atmosphere, however, the lakes likely contain a combination of methane and ethane, not water. & &latestHeader10='KISSING LAKES' &latest10=This Cassini radar image from a September 23, 2006, flyby shows two hydrocarbon lakes, each 20 to 25 kilometers (12 to 16 miles) across. They are joined by a relatively narrow channel. The lake on the right has lighter patches within it, indicating that it may be slowly drying out as the northern summer approaches.