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A More Spectacular Sombrero …
Title A More Spectacular Sombrero (Widescreen Version)
Description This movie shifts from the well-known visible-light picture of Messier 104 taken by the Hubble Space Telescope to infrared views from NASA's Spitzer Space Telescope. Messier 104 is commonly known as the Sombrero galaxy because in visible light, it resembles the broad-brimmed Mexican hat. However, in Spitzer's striking infrared view, the galaxy looks more like a "bull's eye." Viewed from Earth, the spiral galaxy is seen nearly edge-on, just six degrees away from its equatorial plane. 50,000 light-years across, the Sombrero galaxy is considered one of the most massive objects at the southern edge of the Virgo cluster of galaxies. It is located 28 million light-years away, hosts a rich system of nearly 2,000 globular clusters and may harbor a super-massive black hole. In Hubble's visible light image, only the near rim of dust can be clearly seen in silhouette. Recent observations using Spitzer's infrared array camera uncovered the bright, smooth ring of dust circling the galaxy, seen in red. Spitzer's infrared view of the starlight, pierced through the obscuring dust, is easily seen, along with the bulge of stars and an otherwise hidden disk of stars within the dust ring. Spitzer's full view shows the disk is warped, which is often the result of a gravitational encounter with another galaxy, and clumpy areas spotted in the far edges of the ring indicate young star-forming regions. The Sombrero galaxy is located some 28 million light-years away. Viewed from Earth, it is just six degrees south of its equatorial plane. Spitzer detected infrared emission not only from the ring, but from the center of the galaxy too, where there is a huge black hole, believed to be a billion times more massive than our Sun. The Spitzer picture is composed of four images taken at 3.6 (blue), 4.5 (green), 5.8 (orange), and 8.0 (red) microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8 and 8-micron images to enhance the visibility of the dust features. The Hubble Heritage Team took these observations in May-June 2003 with the space telescope's Advanced Camera for Surveys. Images were taken in three filters (red, green, and blue) to yield a natural-color image. The team took six pictures of the galaxy and then stitched them together to create the final composite image. This magnificent galaxy has a diameter that is nearly one-fifth the diameter of the full Moon.
Spitzer Spies Spectacular So …
Title Spitzer Spies Spectacular Sombrero
Description NASA's Spitzer and Hubble Space Telescopes joined forces to create this striking composite image of one of the most popular sights in the universe. Messier 104 is commonly known as the Sombrero galaxy because in visible light, it resembles the broad-brimmed Mexican hat. However, in Spitzer's striking infrared view, the galaxy looks more like a "bull's eye." In Hubble's visible light image (lower left panel), only the near rim of dust can be clearly seen in silhouette. Recent observations using Spitzer's infrared array camera (lower right panel) uncovered the bright, smooth ring of dust circling the galaxy, seen in red. Spitzer's infrared view of the starlight, piercing through the obscuring dust, is easily seen, along with the bulge of stars and an otherwise hidden disk of stars within the dust ring. Spitzer's full view shows the disk is warped, which is often the result of a gravitational encounter with another galaxy, and clumpy areas spotted in the far edges of the ring indicate young star-forming regions. The Sombrero galaxy is located some 28 million light-years away. Viewed from Earth, it is just six degrees south of its equatorial plane. Spitzer detected infrared emission not only from the ring, but from the center of the galaxy too, where there is a huge black hole, believed to be a billion times more massive than our Sun. The Spitzer picture is composed of four images taken at 3.6 (blue), 4.5 (green), 5.8 (orange), and 8.0 (red) microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8 and 8-micron images to enhance the visibility of the dust features. The Hubble Heritage Team took these observations in May-June 2003 with the space telescope's Advanced Camera for Surveys. Images were taken in three filters (red, green, and blue) to yield a natural-color image. The team took six pictures of the galaxy and then stitched them together to create the final composite image. This magnificent galaxy has a diameter that is nearly one-fifth the diameter of the full Moon.
Spitzer Spies Spectacular So …
Title Spitzer Spies Spectacular Sombrero
Description NASA's Spitzer and Hubble Space Telescopes joined forces to create this striking composite image of one of the most popular sights in the universe. Messier 104 is commonly known as the Sombrero galaxy because in visible light, it resembles the broad-brimmed Mexican hat. However, in Spitzer's striking infrared view, the galaxy looks more like a "bull's eye." In Hubble's visible light image (lower left panel), only the near rim of dust can be clearly seen in silhouette. Recent observations using Spitzer's infrared array camera (lower right panel) uncovered the bright, smooth ring of dust circling the galaxy, seen in red. Spitzer's infrared view of the starlight, piercing through the obscuring dust, is easily seen, along with the bulge of stars and an otherwise hidden disk of stars within the dust ring. Spitzer's full view shows the disk is warped, which is often the result of a gravitational encounter with another galaxy, and clumpy areas spotted in the far edges of the ring indicate young star-forming regions. The Sombrero galaxy is located some 28 million light-years away. Viewed from Earth, it is just six degrees south of its equatorial plane. Spitzer detected infrared emission not only from the ring, but from the center of the galaxy too, where there is a huge black hole, believed to be a billion times more massive than our Sun. The Spitzer picture is composed of four images taken at 3.6 (blue), 4.5 (green), 5.8 (orange), and 8.0 (red) microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8 and 8-micron images to enhance the visibility of the dust features. The Hubble Heritage Team took these observations in May-June 2003 with the space telescope's Advanced Camera for Surveys. Images were taken in three filters (red, green, and blue) to yield a natural-color image. The team took six pictures of the galaxy and then stitched them together to create the final composite image. This magnificent galaxy has a diameter that is nearly one-fifth the diameter of the full Moon.
Spitzer Spies Spectacular So …
Title Spitzer Spies Spectacular Sombrero
Description NASA's Spitzer and Hubble Space Telescopes joined forces to create this striking composite image of one of the most popular sights in the universe. Messier 104 is commonly known as the Sombrero galaxy because in visible light, it resembles the broad-brimmed Mexican hat. However, in Spitzer's striking infrared view, the galaxy looks more like a "bull's eye." In Hubble's visible light image (lower left panel), only the near rim of dust can be clearly seen in silhouette. Recent observations using Spitzer's infrared array camera (lower right panel) uncovered the bright, smooth ring of dust circling the galaxy, seen in red. Spitzer's infrared view of the starlight, piercing through the obscuring dust, is easily seen, along with the bulge of stars and an otherwise hidden disk of stars within the dust ring. Spitzer's full view shows the disk is warped, which is often the result of a gravitational encounter with another galaxy, and clumpy areas spotted in the far edges of the ring indicate young star-forming regions. The Sombrero galaxy is located some 28 million light-years away. Viewed from Earth, it is just six degrees south of its equatorial plane. Spitzer detected infrared emission not only from the ring, but from the center of the galaxy too, where there is a huge black hole, believed to be a billion times more massive than our Sun. The Spitzer picture is composed of four images taken at 3.6 (blue), 4.5 (green), 5.8 (orange), and 8.0 (red) microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8 and 8-micron images to enhance the visibility of the dust features. The Hubble Heritage Team took these observations in May-June 2003 with the space telescope's Advanced Camera for Surveys. Images were taken in three filters (red, green, and blue) to yield a natural-color image. The team took six pictures of the galaxy and then stitched them together to create the final composite image. This magnificent galaxy has a diameter that is nearly one-fifth the diameter of the full Moon.
Spitzer Spies Spectacular So …
Title Spitzer Spies Spectacular Sombrero
Description NASA's Spitzer and Hubble Space Telescopes joined forces to create this striking composite image of one of the most popular sights in the universe. Messier 104 is commonly known as the Sombrero galaxy because in visible light, it resembles the broad-brimmed Mexican hat. However, in Spitzer's striking infrared view, the galaxy looks more like a "bull's eye." In Hubble's visible light image (lower left panel), only the near rim of dust can be clearly seen in silhouette. Recent observations using Spitzer's infrared array camera (lower right panel) uncovered the bright, smooth ring of dust circling the galaxy, seen in red. Spitzer's infrared view of the starlight, piercing through the obscuring dust, is easily seen, along with the bulge of stars and an otherwise hidden disk of stars within the dust ring. Spitzer's full view shows the disk is warped, which is often the result of a gravitational encounter with another galaxy, and clumpy areas spotted in the far edges of the ring indicate young star-forming regions. The Sombrero galaxy is located some 28 million light-years away. Viewed from Earth, it is just six degrees south of its equatorial plane. Spitzer detected infrared emission not only from the ring, but from the center of the galaxy too, where there is a huge black hole, believed to be a billion times more massive than our Sun. The Spitzer picture is composed of four images taken at 3.6 (blue), 4.5 (green), 5.8 (orange), and 8.0 (red) microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8 and 8-micron images to enhance the visibility of the dust features. The Hubble Heritage Team took these observations in May-June 2003 with the space telescope's Advanced Camera for Surveys. Images were taken in three filters (red, green, and blue) to yield a natural-color image. The team took six pictures of the galaxy and then stitched them together to create the final composite image. This magnificent galaxy has a diameter that is nearly one-fifth the diameter of the full Moon.
A More Spectacular Sombrero
Title A More Spectacular Sombrero
Description This movie shifts from the well-known visible-light picture of Messier 104 taken by the Hubble Space Telescope to infrared views from NASA's Spitzer Space Telescope. Messier 104 is commonly known as the Sombrero galaxy because in visible light, it resembles the broad-brimmed Mexican hat. However, in Spitzer's striking infrared view, the galaxy looks more like a "bull's eye." Viewed from Earth, the spiral galaxy is seen nearly edge-on, just six degrees away from its equatorial plane. 50,000 light-years across, the Sombrero galaxy is considered one of the most massive objects at the southern edge of the Virgo cluster of galaxies. It is located 28 million light-years away, hosts a rich system of nearly 2,000 globular clusters and may harbor a super-massive black hole. In Hubble's visible light image, only the near rim of dust can be clearly seen in silhouette. Recent observations using Spitzer's infrared array camera uncovered the bright, smooth ring of dust circling the galaxy, seen in red. Spitzer's infrared view of the starlight, pierced through the obscuring dust, is easily seen, along with the bulge of stars and an otherwise hidden disk of stars within the dust ring. Spitzer's full view shows the disk is warped, which is often the result of a gravitational encounter with another galaxy, and clumpy areas spotted in the far edges of the ring indicate young star-forming regions. The Sombrero galaxy is located some 28 million light-years away. Viewed from Earth, it is just six degrees south of its equatorial plane. Spitzer detected infrared emission not only from the ring, but from the center of the galaxy too, where there is a huge black hole, believed to be a billion times more massive than our Sun. The Spitzer picture is composed of four images taken at 3.6 (blue), 4.5 (green), 5.8 (orange), and 8.0 (red) microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8 and 8-micron images to enhance the visibility of the dust features. The Hubble Heritage Team took these observations in May-June 2003 with the space telescope's Advanced Camera for Surveys. Images were taken in three filters (red, green, and blue) to yield a natural-color image. The team took six pictures of the galaxy and then stitched them together to create the final composite image. This magnificent galaxy has a diameter that is nearly one-fifth the diameter of the full Moon.
A Cauldron of Stars at the G …
Title A Cauldron of Stars at the Galaxy's Center
Description This dazzling infrared image from NASA's Spitzer Space Telescope shows hundreds of thousands of stars crowded into the swirling core of our spiral Milky Way galaxy. In visible-light pictures, this region cannot be seen at all because dust lying between Earth and the galactic center blocks our view. In this false-color picture, old and cool stars are blue, while dust features lit up by blazing hot, massive stars are shown in a reddish hue. Both bright and dark filamentary clouds can be seen, many of which harbor stellar nurseries. The plane of the Milky Way's flat disk is apparent as the main, horizontal band of clouds. The brightest white spot in the middle is the very center of the galaxy, which also marks the site of a supermassive black hole. The region pictured here is immense, with a horizontal span of 890 light-years and a vertical span of 640 light-years. Earth is located 26,000 light-years away, out in one of the Milky Way's spiral arms. Though most of the objects seen in this image are located at the galactic center, the features above and below the galactic plane tend to lie closer to Earth. Scientists are intrigued by the giant lobes of dust extending away from the plane of the galaxy. They believe the lobes may have been formed by winds from massive stars. This image is a mosaic of thousands of short exposures taken by Spitzer's Infrared Array Camera (IRAC), showing emissions from wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange), and 8.0 microns (red). The entire region was imaged in less than 16 hours.
A Cauldron of Stars at the G …
Title A Cauldron of Stars at the Galaxy's Center
Description This dazzling infrared image from NASA's Spitzer Space Telescope shows hundreds of thousands of stars crowded into the swirling core of our spiral Milky Way galaxy. In visible-light pictures, this region cannot be seen at all because dust lying between Earth and the galactic center blocks our view. In this false-color picture, old and cool stars are blue, while dust features lit up by blazing hot, massive stars are shown in a reddish hue. Both bright and dark filamentary clouds can be seen, many of which harbor stellar nurseries. The plane of the Milky Way's flat disk is apparent as the main, horizontal band of clouds. The brightest white spot in the middle is the very center of the galaxy, which also marks the site of a supermassive black hole. The region pictured here is immense, with a horizontal span of 890 light-years and a vertical span of 640 light-years. Earth is located 26,000 light-years away, out in one of the Milky Way's spiral arms. Though most of the objects seen in this image are located at the galactic center, the features above and below the galactic plane tend to lie closer to Earth. Scientists are intrigued by the giant lobes of dust extending away from the plane of the galaxy. They believe the lobes may have been formed by winds from massive stars. This image is a mosaic of thousands of short exposures taken by Spitzer's Infrared Array Camera (IRAC), showing emissions from wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange), and 8.0 microns (red). The entire region was imaged in less than 16 hours.
Baby Stars in the Witch Head …
Title Baby Stars in the Witch Head Nebula
Description Eight hundred light-years away in the Orion constellation, a gigantic murky cloud called the "Witch Head" nebula is brewing baby stars. The stellar infants are revealed as pink dots in this image from NASA's Spitzer Space Telescope. Wisps of green in the cloud are carbon-rich molecules called polycyclic aromatic hydrocarbons, which are found on barbecue grills and in automobile exhaust on Earth. This image was obtained as part of the Spitzer Space Telescope Research Program for Teachers and Students, involving high school teachers and their students from across the United States. The infrared image is a three-color composite, in which light with a wavelength of 4.5 microns is blue, 8.0-micron light is green, and 24-micron light is red.
The Milky Way Center Aglow w …
Title The Milky Way Center Aglow with Dust
Description Our Milky Way is a dusty place. So dusty, in fact, that we cannot see the center of the galaxy in visible light. But when NASA's Spitzer Space Telescope set its infrared eyes on the galactic center, it captured this spectacular view. Taken with just one of Spitzer's cameras (at a wavelength of 8 microns), the image highlights the region's exceptionally bright and dusty clouds, lit up by young massive stars. Individual stars can also be seen as tiny dots scattered throughout the dust. The top mosaic shows a portion of the galactic center that stretches across a distance of 760 light-years. Thanks to Spitzer's excellent resolution, the dusty features within the galactic center are seen in unprecedented detail. Four examples are shown in the magnified insets at the bottom. The farthest left box shows a pair of star-forming regions resembling owl-like cosmic eyes. To the left of the "eyes," dark lanes of dust can be seen. This object is probably located in a spiral arm between Earth and the galactic center, in contrast to the following examples, which are all located at the galactic center. The next inset to the right includes the extremely luminous "Quintuplet" stars, a set of five massive stars believed to have buried themselves in cocoons of dust. Just below and to the right of the Quintuplet is the "Pistol" nebula, a bubble of ejected material from the central, massive Pistol star. The finger-like pillars to the left are part of a structure known as "Sickle." They are similar in size and shape to those in the famous picture of the Eagle Nebula taken by NASA's Hubble Space Telescope. Pillars like these are sculpted out of dense dust clouds by radiation and winds from hot stars. The pillars in the Sickle were likely to have been formed by a cluster of hot stars located to their right but not readily visible here. The third inset highlights a system of long, stringy structures that are seen for the first time near the base of a region known as the "Arched Filaments." These long filaments are about 10 light-years long and less than 1 light-year wide. The bright star-forming regions to the right are some of the brightest in the infrared sky. The final inset to the right shows the center of our galaxy, which is the brightest spot in the entire mosaic. The brightness is a result of dust being heated up by a compact cluster of hot stars. The bright spot also marks the location of a supermassive black hole, around which a rotating ring of gas and dust known as the circumnuclear disk can be seen. This image was taken with Spitzer's Infrared Array Camera (IRAC), using its 8-micron detector. It shows emissions from heated-up molecules in dust clouds called polycyclic aromatic hydrocarbons.
The Milky Way Center Aglow w …
Title The Milky Way Center Aglow with Dust
Description Our Milky Way is a dusty place. So dusty, in fact, that we cannot see the center of the galaxy in visible light. But when NASA's Spitzer Space Telescope set its infrared eyes on the galactic center, it captured this spectacular view. Taken with just one of Spitzer's cameras (at a wavelength of 8 microns), the image highlights the region's exceptionally bright and dusty clouds, lit up by young massive stars. Individual stars can also be seen as tiny dots scattered throughout the dust. The top mosaic shows a portion of the galactic center that stretches across a distance of 760 light-years. Thanks to Spitzer's excellent resolution, the dusty features within the galactic center are seen in unprecedented detail. Four examples are shown in the magnified insets at the bottom. The farthest left box shows a pair of star-forming regions resembling owl-like cosmic eyes. To the left of the "eyes," dark lanes of dust can be seen. This object is probably located in a spiral arm between Earth and the galactic center, in contrast to the following examples, which are all located at the galactic center. The next inset to the right includes the extremely luminous "Quintuplet" stars, a set of five massive stars believed to have buried themselves in cocoons of dust. Just below and to the right of the Quintuplet is the "Pistol" nebula, a bubble of ejected material from the central, massive Pistol star. The finger-like pillars to the left are part of a structure known as "Sickle." They are similar in size and shape to those in the famous picture of the Eagle Nebula taken by NASA's Hubble Space Telescope. Pillars like these are sculpted out of dense dust clouds by radiation and winds from hot stars. The pillars in the Sickle were likely to have been formed by a cluster of hot stars located to their right but not readily visible here. The third inset highlights a system of long, stringy structures that are seen for the first time near the base of a region known as the "Arched Filaments." These long filaments are about 10 light-years long and less than 1 light-year wide. The bright star-forming regions to the right are some of the brightest in the infrared sky. The final inset to the right shows the center of our galaxy, which is the brightest spot in the entire mosaic. The brightness is a result of dust being heated up by a compact cluster of hot stars. The bright spot also marks the location of a supermassive black hole, around which a rotating ring of gas and dust known as the circumnuclear disk can be seen. This image was taken with Spitzer's Infrared Array Camera (IRAC), using its 8-micron detector. It shows emissions from heated-up molecules in dust clouds called polycyclic aromatic hydrocarbons.
Cigar Galaxy up in Smoke
Title Cigar Galaxy up in Smoke
Description This movie compares a visible-light view of the "Cigar galaxy" to an infrared view from NASA's Spitzer Space Telescope of the same galaxy. The movie begins with the visible image of the galaxy looking cool as a cucumber, then fades into the infrared image, revealing a smokin' hot "cigar." The visible-light picture of the Cigar galaxy, also called Messier 82, shows only a bar of light against a dark patch of space. Longer exposures of the galaxy (not pictured here) have revealed cone-shaped clouds of hot gas above and below the galaxy's plane. It took Spitzer's three sensitive instruments to show that the galaxy is also surrounded by a huge, hidden halo of smoky dust (red in infrared image). The infrared image above was taken by Spitzer's infrared array camera. The dust particles (red) are being blown out into space by the galaxy's hot stars (blue). Spitzer's infrared spectrograph told astronomers that the dust contains a carbon-containing compound, called polycyclic aromatic hydrocarbon. This smelly molecule can be found on Earth in tailpipes, barbecue pits and other places where combustion reactions have occurred. Messier 82 is located about 12 million light-years away in the Ursa Major constellation. It is viewed from its side, or edge on, so it appears as a thin cigar-shaped bar. The galaxy is termed a starburst because its core is a fiery hotbed of stellar birth. A larger nearby galaxy, called Messier 81, is gravitationally interacting with Messier 82, prodding it into producing the new stars. The infrared picture was taken as a part of the Spitzer Infrared Nearby Galaxy Survey. Blue indicates infrared light of 3.6 microns, green corresponds to 4.5 microns, and red to 5.8 and 8.0 microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8- and 8-micron images to enhance the visibility of the dust features. The visible-light picture is from the National Optical Astronomy Observatory, Tucson, Ariz.
Coronet: A Star-Formation Ne …
Title Coronet: A Star-Formation Neighbor
Description While perhaps not quite as well known as its star-formation cousin Orion, the Corona Australis region (containing, at its heart, the Coronet cluster) is one of the nearest and most active regions of ongoing star formation. At only about 420 light-years away, the Coronet is over three times closer than the Orion nebula is to Earth. The Coronet contains a loose cluster of a few dozen young stars with a wide range of masses and at various stages of evolution, giving astronomers an opportunity to observe embryonic stars simultaneously in several wavelengths. This composite image shows the Coronet in X-rays from Chandra (purple) and infrared from Spitzer (orange, green, and cyan). The Spitzer image shows young stars plus diffuse emission from dust. Due to the host of young stars in different life stages in the Coronet, astronomers can use these data to pinpoint details of how the youngest stars evolve.
Huge Hidden Halo!
Title Huge Hidden Halo!
Description This image composite compares a visible-light view (left) of the "Cigar galaxy" to an infrared view from NASA's Spitzer Space Telescope of the same galaxy. While the visible image shows a serene galaxy looking cool as a cucumber, the infrared image reveals a smokin' hot "cigar." The visible-light picture of the Cigar galaxy, also called Messier 82, shows only a bar of light against a dark patch of space. Longer exposures of the galaxy (not pictured here) have revealed cone-shaped clouds of hot gas above and below the galaxy's plane. It took Spitzer's three sensitive instruments to show that the galaxy is also surrounded by a huge, hidden halo of smoky dust (red in infrared image). The infrared image above was taken by Spitzer's infrared array camera. The dust particles (red) are being blown out into space by the galaxy's hot stars (blue). Spitzer's infrared spectrograph told astronomers that the dust contains a carbon-containing compound, called polycyclic aromatic hydrocarbon. This smelly molecule can be found on Earth in tailpipes, barbecue pits and other places where combustion reactions have occurred. Messier 82 is located about 12 million light-years away in the Ursa Major constellation. It is viewed from its side, or edge on, so it appears as a thin cigar-shaped bar. The galaxy is termed a starburst because its core is a fiery hotbed of stellar birth. A larger nearby galaxy, called Messier 81, is gravitationally interacting with Messier 82, prodding it into producing the new stars. The infrared picture was taken as a part of the Spitzer Infrared Nearby Galaxy Survey. Blue indicates infrared light of 3.6 microns, green corresponds to 4.5 microns, and red to 5.8 and 8.0 microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8- and 8-micron images to enhance the visibility of the dust features. The visible-light picture is from the National Optical Astronomy Observatory, Tucson, Ariz.
Huge Hidden Halo!
Title Huge Hidden Halo!
Description This image composite compares a visible-light view (left) of the "Cigar galaxy" to an infrared view from NASA's Spitzer Space Telescope of the same galaxy. While the visible image shows a serene galaxy looking cool as a cucumber, the infrared image reveals a smokin' hot "cigar." The visible-light picture of the Cigar galaxy, also called Messier 82, shows only a bar of light against a dark patch of space. Longer exposures of the galaxy (not pictured here) have revealed cone-shaped clouds of hot gas above and below the galaxy's plane. It took Spitzer's three sensitive instruments to show that the galaxy is also surrounded by a huge, hidden halo of smoky dust (red in infrared image). The infrared image above was taken by Spitzer's infrared array camera. The dust particles (red) are being blown out into space by the galaxy's hot stars (blue). Spitzer's infrared spectrograph told astronomers that the dust contains a carbon-containing compound, called polycyclic aromatic hydrocarbon. This smelly molecule can be found on Earth in tailpipes, barbecue pits and other places where combustion reactions have occurred. Messier 82 is located about 12 million light-years away in the Ursa Major constellation. It is viewed from its side, or edge on, so it appears as a thin cigar-shaped bar. The galaxy is termed a starburst because its core is a fiery hotbed of stellar birth. A larger nearby galaxy, called Messier 81, is gravitationally interacting with Messier 82, prodding it into producing the new stars. The infrared picture was taken as a part of the Spitzer Infrared Nearby Galaxy Survey. Blue indicates infrared light of 3.6 microns, green corresponds to 4.5 microns, and red to 5.8 and 8.0 microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8- and 8-micron images to enhance the visibility of the dust features. The visible-light picture is from the National Optical Astronomy Observatory, Tucson, Ariz.
Huge Hidden Halo!
Title Huge Hidden Halo!
Description This image composite compares a visible-light view (left) of the "Cigar galaxy" to an infrared view from NASA's Spitzer Space Telescope of the same galaxy. While the visible image shows a serene galaxy looking cool as a cucumber, the infrared image reveals a smokin' hot "cigar." The visible-light picture of the Cigar galaxy, also called Messier 82, shows only a bar of light against a dark patch of space. Longer exposures of the galaxy (not pictured here) have revealed cone-shaped clouds of hot gas above and below the galaxy's plane. It took Spitzer's three sensitive instruments to show that the galaxy is also surrounded by a huge, hidden halo of smoky dust (red in infrared image). The infrared image above was taken by Spitzer's infrared array camera. The dust particles (red) are being blown out into space by the galaxy's hot stars (blue). Spitzer's infrared spectrograph told astronomers that the dust contains a carbon-containing compound, called polycyclic aromatic hydrocarbon. This smelly molecule can be found on Earth in tailpipes, barbecue pits and other places where combustion reactions have occurred. Messier 82 is located about 12 million light-years away in the Ursa Major constellation. It is viewed from its side, or edge on, so it appears as a thin cigar-shaped bar. The galaxy is termed a starburst because its core is a fiery hotbed of stellar birth. A larger nearby galaxy, called Messier 81, is gravitationally interacting with Messier 82, prodding it into producing the new stars. The infrared picture was taken as a part of the Spitzer Infrared Nearby Galaxy Survey. Blue indicates infrared light of 3.6 microns, green corresponds to 4.5 microns, and red to 5.8 and 8.0 microns. The contribution from starlight (measured at 3.6 microns) has been subtracted from the 5.8- and 8-micron images to enhance the visibility of the dust features. The visible-light picture is from the National Optical Astronomy Observatory, Tucson, Ariz.
Our Chaotic Neighbor
Title Our Chaotic Neighbor
Description This vibrant image from NASA's Spitzer Space Telescope shows the Large Magellanic Cloud, a satellite galaxy to our own Milky Way galaxy. The infrared image, a mosaic of more than 100,000 individual tiles, offers astronomers a unique chance to study the lifecycle of stars and dust in a single galaxy. Nearly one million objects are revealed for the first time in this Spitzer view, which represents about a 1,000-fold improvement in sensitivity over previous space-based missions. Most of the new objects are dusty stars of various ages populating the Large Magellanic Cloud, the rest are thought to be background galaxies. The blue color in the picture, seen most prominently in the central bar, represents starlight from older stars. The chaotic, bright regions outside this bar are filled with hot, massive stars buried in thick blankets of dust. The red clouds contain cooler interstellar gas and molecular-sized dust grains illuminated by ambient starlight. The Large Magellanic Cloud, located 160,000 light-years from Earth, is one of a handful of dwarf galaxies that orbit our own Milky Way. It is approximately one-third as wide as the Milky Way, and, if it could be seen in its entirety, would cover the same amount of sky as a grid of about 480 full moons. About one-third of the whole galaxy can be seen in the Spitzer image. This picture is a composite of infrared light captured by Spitzer's infrared array camera. Light with wavelengths of 8 and 5.8 microns is red and orange: 4.5-micron light is green, and 3.6-micron light is blue.
Our Chaotic Neighbor
Title Our Chaotic Neighbor
Description This vibrant image from NASA's Spitzer Space Telescope shows the Large Magellanic Cloud, a satellite galaxy to our own Milky Way galaxy. The infrared image, a mosaic of more than 100,000 individual tiles, offers astronomers a unique chance to study the lifecycle of stars and dust in a single galaxy. Nearly one million objects are revealed for the first time in this Spitzer view, which represents about a 1,000-fold improvement in sensitivity over previous space-based missions. Most of the new objects are dusty stars of various ages populating the Large Magellanic Cloud, the rest are thought to be background galaxies. The blue color in the picture, seen most prominently in the central bar, represents starlight from older stars. The chaotic, bright regions outside this bar are filled with hot, massive stars buried in thick blankets of dust. The red clouds contain cooler interstellar gas and molecular-sized dust grains illuminated by ambient starlight. The Large Magellanic Cloud, located 160,000 light-years from Earth, is one of a handful of dwarf galaxies that orbit our own Milky Way. It is approximately one-third as wide as the Milky Way, and, if it could be seen in its entirety, would cover the same amount of sky as a grid of about 480 full moons. About one-third of the whole galaxy can be seen in the Spitzer image. This picture is a composite of infrared light captured by Spitzer's infrared array camera. Light with wavelengths of 8 and 5.8 microns is red and orange: 4.5-micron light is green, and 3.6-micron light is blue.
Our Chaotic Neighbor
Title Our Chaotic Neighbor
Description This vibrant image from NASA's Spitzer Space Telescope shows the Large Magellanic Cloud, a satellite galaxy to our own Milky Way galaxy. The infrared image, a mosaic of more than 100,000 individual tiles, offers astronomers a unique chance to study the lifecycle of stars and dust in a single galaxy. Nearly one million objects are revealed for the first time in this Spitzer view, which represents about a 1,000-fold improvement in sensitivity over previous space-based missions. Most of the new objects are dusty stars of various ages populating the Large Magellanic Cloud, the rest are thought to be background galaxies. The blue color in the picture, seen most prominently in the central bar, represents starlight from older stars. The chaotic, bright regions outside this bar are filled with hot, massive stars buried in thick blankets of dust. The red clouds contain cooler interstellar gas and molecular-sized dust grains illuminated by ambient starlight. The Large Magellanic Cloud, located 160,000 light-years from Earth, is one of a handful of dwarf galaxies that orbit our own Milky Way. It is approximately one-third as wide as the Milky Way, and, if it could be seen in its entirety, would cover the same amount of sky as a grid of about 480 full moons. About one-third of the whole galaxy can be seen in the Spitzer image. This picture is a composite of infrared light captured by Spitzer's infrared array camera. Light with wavelengths of 8 and 5.8 microns is red and orange: 4.5-micron light is green, and 3.6-micron light is blue.
What's Old Is New in the Lar …
Title What's Old Is New in the Large Magellanic Cloud
Description This vibrant image from NASA's Spitzer Space Telescope shows the Large Magellanic Cloud, a satellite galaxy to our own Milky Way galaxy. The infrared image, a mosaic of 300,000 individual tiles, offers astronomers a unique chance to study the lifecycle of stars and dust in a single galaxy. Nearly one million objects are revealed for the first time in this Spitzer view, which represents about a 1,000-fold improvement in sensitivity over previous space-based missions. Most of the new objects are dusty stars of various ages populating the Large Magellanic Cloud, the rest are thought to be background galaxies. The blue color in the picture, seen most prominently in the central bar, represents starlight from older stars. The chaotic, bright regions outside this bar are filled with hot, massive stars buried in thick blankets of dust. The red color around these bright regions is from dust heated by stars, while the red dots scattered throughout the picture are either dusty, old stars or more distant galaxies. The greenish clouds contain cooler interstellar gas and molecular-sized dust grains illuminated by ambient starlight. Astronomers say this image allows them to quantify the process by which space dust ? the same stuff that makes up planets and even people ? is recycled in a galaxy. The picture shows dust at its three main cosmic hangouts: around the young stars, where it is being consumed (red-tinted, bright clouds), scattered about in the space between stars (greenish clouds), and in expelled shells of material from old stars (randomly-spaced red dots). The Large Magellanic Cloud, located 160,000 light-years from Earth, is one of a handful of dwarf galaxies that orbit our own Milky Way. It is approximately one-third as wide as the Milky Way, and, if it could be seen in its entirety, would cover the same amount of sky as a grid of about 480 full moons. About one-third of the entire galaxy can be seen in the Spitzer image. This picture is a composite of infrared light captured by Spitzer. Light with wavelengths of 3.6 (blue) and 8 (green) microns was captured by the telescope's infrared array camera, 24-micron light (red) was detected by the multiband imaging photometer.
What's Old Is New in the Lar …
Title What's Old Is New in the Large Magellanic Cloud
Description This vibrant image from NASA's Spitzer Space Telescope shows the Large Magellanic Cloud, a satellite galaxy to our own Milky Way galaxy. The infrared image, a mosaic of 300,000 individual tiles, offers astronomers a unique chance to study the lifecycle of stars and dust in a single galaxy. Nearly one million objects are revealed for the first time in this Spitzer view, which represents about a 1,000-fold improvement in sensitivity over previous space-based missions. Most of the new objects are dusty stars of various ages populating the Large Magellanic Cloud, the rest are thought to be background galaxies. The blue color in the picture, seen most prominently in the central bar, represents starlight from older stars. The chaotic, bright regions outside this bar are filled with hot, massive stars buried in thick blankets of dust. The red color around these bright regions is from dust heated by stars, while the red dots scattered throughout the picture are either dusty, old stars or more distant galaxies. The greenish clouds contain cooler interstellar gas and molecular-sized dust grains illuminated by ambient starlight. Astronomers say this image allows them to quantify the process by which space dust ? the same stuff that makes up planets and even people ? is recycled in a galaxy. The picture shows dust at its three main cosmic hangouts: around the young stars, where it is being consumed (red-tinted, bright clouds), scattered about in the space between stars (greenish clouds), and in expelled shells of material from old stars (randomly-spaced red dots). The Large Magellanic Cloud, located 160,000 light-years from Earth, is one of a handful of dwarf galaxies that orbit our own Milky Way. It is approximately one-third as wide as the Milky Way, and, if it could be seen in its entirety, would cover the same amount of sky as a grid of about 480 full moons. About one-third of the entire galaxy can be seen in the Spitzer image. This picture is a composite of infrared light captured by Spitzer. Light with wavelengths of 3.6 (blue) and 8 (green) microns was captured by the telescope's infrared array camera, 24-micron light (red) was detected by the multiband imaging photometer.
What's Old Is New in the Lar …
Title What's Old Is New in the Large Magellanic Cloud
Description This vibrant image from NASA's Spitzer Space Telescope shows the Large Magellanic Cloud, a satellite galaxy to our own Milky Way galaxy. The infrared image, a mosaic of 300,000 individual tiles, offers astronomers a unique chance to study the lifecycle of stars and dust in a single galaxy. Nearly one million objects are revealed for the first time in this Spitzer view, which represents about a 1,000-fold improvement in sensitivity over previous space-based missions. Most of the new objects are dusty stars of various ages populating the Large Magellanic Cloud, the rest are thought to be background galaxies. The blue color in the picture, seen most prominently in the central bar, represents starlight from older stars. The chaotic, bright regions outside this bar are filled with hot, massive stars buried in thick blankets of dust. The red color around these bright regions is from dust heated by stars, while the red dots scattered throughout the picture are either dusty, old stars or more distant galaxies. The greenish clouds contain cooler interstellar gas and molecular-sized dust grains illuminated by ambient starlight. Astronomers say this image allows them to quantify the process by which space dust ? the same stuff that makes up planets and even people ? is recycled in a galaxy. The picture shows dust at its three main cosmic hangouts: around the young stars, where it is being consumed (red-tinted, bright clouds), scattered about in the space between stars (greenish clouds), and in expelled shells of material from old stars (randomly-spaced red dots). The Large Magellanic Cloud, located 160,000 light-years from Earth, is one of a handful of dwarf galaxies that orbit our own Milky Way. It is approximately one-third as wide as the Milky Way, and, if it could be seen in its entirety, would cover the same amount of sky as a grid of about 480 full moons. About one-third of the entire galaxy can be seen in the Spitzer image. This picture is a composite of infrared light captured by Spitzer. Light with wavelengths of 3.6 (blue) and 8 (green) microns was captured by the telescope's infrared array camera, 24-micron light (red) was detected by the multiband imaging photometer.
A Real Shiner
Description A Real Shiner
Full Description Saturn's moon Rhea shows off the moon equivalent of a black eye -- a bright, rayed crater near its eastern limb. Rhea is about half the size of Earth's moon. At 1,528 kilometers (949 miles) across, it is the second-largest moon orbiting Saturn. The image was taken in visible light with the Cassini spacecraft narrow angle camera on Oct. 24, 2004, at a distance of about 1.7 million kilometers (1 million miles) from Rhea and at a Sun-Rhea-spacecraft, or phase, angle of 40 degrees. The image scale is approximately 10 kilometers (6 miles) per pixel. Cassini will image this hemisphere of Rhea again in mid-January 2005, just after the Huygens probe landing on Titan - with approximately 1-kilometer (0.6-mile) resolution. 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 Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission, visit http://saturn.jpl.nasa.gov and the Cassini imaging team home page, http://ciclops.org . *Image Credit:* NASA/JPL/Space Science Institute
Huygens Landing Site Revisit …
Description Here on the Gallery page you can find the very latest images, videos and products from the Cassini-Huygens mission to Saturn, including the spectacular launch, spacecraft assembly and the exciting trip to Saturn.
Full Description January 13, 2006 This is an animated artist interpretation of the area surrounding the Huygens landing site, based on images and data returned Jan. 14, 2005. On January 14, 2005, the European Space Agency's (ESA) Huygens probe reached the upper layer of Titan's atmosphere and landed on the surface after a parachute descent 2 hours and 28 minutes later. As part of the joint NASA/ESA/ASI mission to Saturn and its moons, the Huygens probe was sent from the Cassini spacecraft to explore Titan, Saturn's largest moon. Titan's organic chemistry may be like that of the primitive Earth around 4000 million years ago, and it may hold clues about how life began on our planet. + Read the Feature
Cassini's Galactic Aspiriati …
Description Cassini's Galactic Aspiriations
Full Description Cassini briefly turned its gaze from Saturn and its rings and moons to marvel at the Carina Nebula, a brilliant region 8,000 light years from our solar system and more than 200 light years across. Nearly every point of light in this image is a star in our galaxy, the Milky Way. The nebula is a region of gas and dust made to glow by the ultraviolet light bursting from bright, hot and extremely massive young stars within. Darker regions in the scene are not devoid of stars, rather, they are areas where dense clouds of dust block the light from background stars. This image and others like it are taken by the spacecraft from time to time for calibration purposes. Calibration images rarely contain such incredible sights. This one affirms Cassini's position as the farthest, working astronomical observatory ever established around our sun -- our eyes on the cosmos, a billion miles from Earth. The image was taken using the Cassini wide-angle camera on May 14, 2005. The view is a 68-second, clear-filter exposure. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . *Credit:* NASA/JPL/Space Science Institute
Date December 22, 2005
Giant Landslide on Iapetus
Description Giant Landslide on Iapetus
Full Description A spectacular landslide within the low-brightness region of Iapetus's surface known as Cassini Regio is visible in this image from Cassini. Iapetus is one of the moons of Saturn. The landslide material appears to have collapsed from a scarp 15 kilometers high (9 miles) that forms the rim of an ancient 600 kilometer (375 mile) impact basin. Unconsolidated rubble from the landslide extends halfway across a conspicuous, 120-kilometer diameter (75-mile) flat-floored impact crater that lies just inside the basin scarp. Landslides are common geological phenomena on many planetary bodies, including Earth and Mars. The appearance of this landslide on an icy satellite with low-brightness cratered terrain is reminiscent of landslide features that were observed during NASA's Galileo mission on the Jovian satellite Callisto. The fact that the Iapetus landslide traveled many kilometers from the basin scarp could indicate that the surface material is very fine-grained, and perhaps was fluffed by mechanical forces that allowed the landslide debris to flow extended distances. In this view, north is to the left of the picture and solar illumination is from the bottom of the frame. The image was obtained in visible light with the Cassini spacecraft narrow angle camera on Dec. 31, 2004, at a distance of about 123,400 kilometers (76,677 miles) from Iapetus and at a Sun-Iapetus-spacecraft, or phase, angle of 78 degrees. Resolution achieved in the original image was 740 meters (2,428 feet) per pixel. The image has been contrast-enhanced and magnified by a factor of two to aid visibility. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For images visit the Cassini imaging team home page http://ciclops.org . Credit: NASA/JPL/Space Science Institute
Date January 7, 2005
Go Huygens!
Description Go Huygens!
Full Description This map illustrates the planned imaging coverage for the Descent Imager/Spectral Radiometer, onboard the European Space Agency's Huygens probe during the probe's descent toward Titan's surface on Jan. 14, 2005. The Descent Imager/Spectral Radiometer is one of two NASA instruments on the probe. The colored lines delineate regions that will be imaged at different resolutions as the probe descends. The site where Huygens is predicted to land is marked with a yellow dot. This area is in a boundary between dark and bright regions. This map was made from the images taken by the Cassini spacecraft cameras on Oct. 26, 2004, at image scales of 4 to 6 kilometers (2.5 to 3.7 miles) per pixel. The images were obtained using a narrow band filter centered at 938 nanometers - a near-infrared wavelength (invisible to the human eye) at which light can penetrate Titan's atmosphere to reach the surface and return through the atmosphere to be detected by the camera. The images have been processed to enhance surface details. Only brightness variations on Titan's surface are seen, the illumination is such that there is no shading due to topographic variations. For about two hours, the probe will fall by parachute from an altitude of 160 kilometers (99 miles) to Titan's surface. During the descent the Descent Imager/Spectral Radiometer and five other science instruments will send data about the moon's atmosphere and surface back to the Cassini spacecraft for relay to Earth. The Descent Imager/Spectral Radiometer will take pictures as the probe slowly spins, and some of these will be made into panoramic views of Titan's surface. The first map (PIA06172) shows expected coverage by the Descent Imager/Spectral Radiometer side-looking imager and two downward-looking imagers - one providing medium-resolution and the other high-resolution coverage. The planned coverage by the medium- and high-resolution imagers is the subject of this map (PIA06173). 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 Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. The Descent Imager/Spectral team is based at the University of Arizona, Tucson, Ariz. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For images visit the Cassini imaging team home page http://ciclops.org . *Credit*: NASA/JPL/Space Science Institute
Date January 11, 2005
Go Huygens!
Description Go Huygens!
Full Description This map illustrates the planned imaging coverage for the Descent Imager/Spectral Radiometer, onboard the European Space Agency's Huygens probe during the probe's descent toward Titan's surface on Jan. 14, 2005. The Descent Imager/Spectral Radiometer is one of two NASA instruments on the probe. The colored lines delineate regions that will be imaged at different resolutions as the probe descends. On each map, the site where Huygens is predicted to land is marked with a yellow dot. This area is in a boundary between dark and bright regions. This map was made from the images taken by the Cassini spacecraft cameras on Oct. 26, 2004, at image scales of 4 to 6 kilometers (2.5 to 3.7 miles) per pixel. The images were obtained using a narrow band filter centered at 938 nanometers - a near-infrared wavelength (invisible to the human eye) at which light can penetrate Titan's atmosphere to reach the surface and return through the atmosphere to be detected by the camera. The images have been processed to enhance surface details. Only brightness variations on Titan's surface are seen, the illumination is such that there is no shading due to topographic variations. For about two hours, the probe will fall by parachute from an altitude of 160 kilometers (99 miles) to Titan's surface. During the descent the camera on the probe and five other science instruments will send data about the moon's atmosphere and surface back to the Cassini spacecraft for relay to Earth. The Descent Imager/Spectral Radiometer will take pictures as the probe slowly spins, and some these will be made into panoramic views of Titan's surface. This map (PIA06172) shows the expected coverage by the Descent Imager/Spectral Radiometer side-looking imager and two downward-looking imagers - one providing medium-resolution and the other high-resolution coverage. The planned coverage by the medium- and high-resolution imagers is the subject of the second map (PIA06173). 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 Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. The Descent Imager/Spectral team is based at the University of Arizona, Tucson, Ariz. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For images visit the Cassini imaging team home page http://ciclops.org . *Credit*: NASA/JPL/Space Science Institute
Date January 11, 2005
W00004705.jpg
Description W00004705.jpg
Full Description W00004705.jpg was taken on February 15, 2005 and received on Earth February 15, 2005. The camera was pointing toward TITAN, and the image was taken using the CL1 and CB3 filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2005. For a glimpse of what's to come, check out the raw images site.
Date February 15, 2005
N00027998.jpg
Description N00027998.jpg
Full Description N00027998.jpg was taken on February 15, 2005 and received on Earth February 15, 2005. The camera was pointing toward TITAN, and the image was taken using the CL1 and CB3 filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2005. For a glimpse of what's to come, check out the raw images site.
Date February 15, 2005
Exploring the Wetlands of Ti …
Description Exploring the Wetlands of Titan
Full Description Cassini peers through the murky orange haze of Titan to spy what are believed to be bodies of liquid hydrocarbons, two of them as large as seas on Earth, near the moon's north pole. This movie blends a near natural-color view and an infrared glimpse of Titan's surface obtained by the visual cameras, followed by a transition to imagery collected by the radar instrument aboard Cassini, for a dramatic reveal of the north pole of Saturn's largest moon. As the movie zooms in on the north pole, the most readily visible bodies are outlined in blue. The largest of these, on the left, is as big as the Caspian Sea on Earth, the next largest, on the right, is about the size of Lake Superior. When compared to the surface area of Titan however (which is six times smaller than Earth's), these bodies are equivalent in size to the Bay of Bengal and Timor Sea, respectively. Geographically speaking, they are more like seas. The movie continues with a gradual transition to a polar map of the radar imagery taken so far by Cassini of the north polar region. It is clear that one of the radar swaths has intersected a small upper bay of the largest sea, and has almost entirely imaged the second one. The extreme darkness of these regions in the radar data argues strongly for the presence of liquid hydrocarbons, such as methane and ethane, which remain liquid at Titan's frigid temperature of minus 180 degrees Celsius (minus 288 degrees Fahrenheit). See Titan (T25) Viewed by Cassini's Radar - Feb. 22, 2007. The movie continues with a pan across the pole and the radar imagery that has uncovered a multitude of much smaller lakes. Features of strikingly similar morphology to these dark northern seas and smaller lakes were first discovered in Cassini Imaging Science Subsystem images in June 2005, at Titan's south pole (see Land of Lakes?). The lake-like shoreline of the largest of these, called Ontario Lacus, its size (about the size of Lake Victoria), and its proximity to the south pole where the largest field of clouds yet seen on Titan had been observed, earned it the reputation as the best candidate for a body of liquid hydrocarbons on Titan up until that point, though the case for liquids was weak. When adjusted for the size of Titan, Ontario Lacus is equivalent in size to the Black Sea. Now, by inference, scientists are more confident that it, and the smaller features that dot the south pole, are also likely open bodies of liquid, and in aggregate make up a southern wetlands on Titan, similar to the one observed in the north polar movie. The images used to make this movie were taken with the Cassini spacecraft narrow-angle camera on Feb. 25, 2007, at a distance of approximately 1.3 million kilometers (800,000 miles) from Titan. The infrared images were taken with a special filter centered at 938 nanometers that provides the cameras' best view of Titan's surface features. This view was then composited with images taken at 619, 568 and 440 nanometers to, create a near natural color appearance. The radar data were acquired in synthetic aperture radar mode. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute
Date March 15, 2007
The Dragon Storm
Description The Dragon Storm
Full Description A large, bright and complex convective storm that appeared in Saturn's southern hemisphere in mid-September 2004 was the key in solving a long-standing mystery about the ringed planet. Saturn's atmosphere and its rings are shown here in a false color composite made from Cassini images taken in near infrared light through filters that sense different amounts of methane gas. Portions of the atmosphere with a large abundance of methane above the clouds are red, indicating clouds that are deep in the atmosphere. Grey indicates high clouds, and brown indicates clouds at intermediate altitudes. The rings are bright blue because there is no methane gas between the ring particles and the camera. The complex feature with arms and secondary extensions just above and to the right of center is called the Dragon Storm. It lies in a region of the southern hemisphere referred to as "storm alley" by imaging scientists because of the high level of storm activity observed there by Cassini in the last year. The Dragon Storm was a powerful source of radio emissions during July and September of 2004. The radio waves from the storm resemble the short bursts of static generated by lightning on Earth. Cassini detected the bursts only when the storm was rising over the horizon on the night side of the planet as seen from the spacecraft, the bursts stopped when the storm moved into sunlight. This on/off pattern repeated for many Saturn rotations over a period of several weeks, and it was the clock-like repeatability that indicated the storm and the radio bursts are related. Scientists have concluded that the Dragon Storm is a giant thunderstorm whose precipitation generates electricity as it does on Earth. The storm may be deriving its energy from Saturn's deep atmosphere. One mystery is why the radio bursts start while the Dragon Storm is below the horizon on the night side and end when the storm is on the day side, still in full view of the Cassini spacecraft. A possible explanation is that the lightning source lies to the east of the visible cloud, perhaps because it is deeper where the currents are eastward relative to those at cloud top levels. If this were the case, the lightning source would come up over the night side horizon and would sink down below the day side horizon before the visible cloud. This would explain the timing of the visible storm relative to the radio bursts. The Dragon Storm is of great interest for another reason. In examining images taken of Saturn's atmosphere over many months, imaging scientists found that the Dragon Storm arose in the same part of Saturn's atmosphere that had earlier produced large bright convective storms. In other words, the Dragon Storm appears to be a long-lived storm deep in the atmosphere that periodically flares up to produce dramatic bright white plumes which subside over time. One earlier sighting, in July 2004, was also associated with strong radio bursts. And another, observed in March 2004 and captured, in a movie created from images of the atmosphere (http://photojournal.jpl.nasa.gov/catalog/PIA06082 and http://photojournal.jpl.nasa.gov/catalog/PIA06083) spawned three little dark oval storms that broke off from the arms of the main storm. Two of these subsequently merged with each other, the current to the north carried the third one off to the west, and Cassini lost track of it. Small dark storms like these generally get stretched out until they merge with the opposing currents to the north and south. These little storms are the food that sustains the larger atmospheric features, including the larger ovals and the eastward and westward currents. If the little storms come from the giant thunderstorms, then together they form a food chain that harvests the energy of the deep atmosphere and helps maintain the powerful currents. Cassini has many more chances to observe future flare-ups of the Dragon Storm, and others like it over the course of the mission. It is likely that scientists will come to solve the mystery of the radio bursts and observe storm creation and merging in the next 2 or 3 years. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For images visit the Cassini imaging team home page http://ciclops.org . *Credit:* NASA/JPL/Space Science Institute
Date February 24, 2005
Scrutinizing Titan's Surface
Description Scrutinizing Titan's Surface
Full Description The six close-up views of Titan's surface shown here are composed of images acquired by the Cassini spacecraft during flybys in October (see Titan Mosaic: October 2004) and December (see Titan Mosaic: December 2004) of 2004. These close-up views illustrate that a variety of processes have shaped the surface of Titan, just as diverse geologic processes are responsible for what we see on Earth's surface. Image (a) shows a prominent bright-dark boundary near the western edge of the Xanadu region which exhibits a sharp, angular edge between the materials. Three bright, discontinuous circles can be seen (two near the top of the image and another near the lower left). These may be large impact craters, the upper two are approximately 30 kilometers (18.6 miles) in diameter and the lower one is approximately 50 kilometers (20 miles) in diameter. Titan's thick atmosphere will screen out small projectiles, but if the surface were as old as Titan itself, it should have many more craters of these sizes. Therefore, Cassini scientists think that, like Earth's surface, Titan's surface has been modified more recently by other geologic processes. However, such processes on Titan may take much longer than on Earth, acting over hundreds of millions of years. Image (b) shows bright features that appear to be streamlined as if were they formed by winds in Titan's atmosphere moving from west to east. The landing site of the Huygens probe is in the upper left corner of this image (see Cassini's View of Titan Landing Site). Image (c) shows a bright feature surrounded by dark material. Several long, dark and narrow lines running through the bright area may be larger examples of the dark channels seen by the Huygens probe (see Mosaic of River Channel and Ridge Area on Titan). These lines are on the order of 2 kilometers (1 mile) wide, and tens of kilometers long. Image (d) shows dark material within the bright area to the west of Xanadu. The linear nature of these features suggests that they may have formed by faulting. They may be dark due to modification by other surface processes occurring on Titan, in the same way that on Earth, fault-lines can be enhanced by erosion and/or deposition of material by water and wind. Image (e) shows brightness variations in the region southeast of the Huygens landing site. The features indicated by arrows exhibit shapes that are similar to drainage patterns seen on Earth and Mars, where the source of the liquid is underground springs rather than rainfall. Image (f) shows a region near the northwestern edge of Xanadu where the boundary between the bright and dark materials is quite complicated. Here some of the bright patches appear as if they represent thin surface plates that have been broken apart and spread apart over underlying dark material. The white bars above each image are 200 kilometers (124 miles) long. Imaging Titan through its thick atmosphere is a challenge, and the narrow, straight lines within the images, are seams between individual images that have not been completely removed. North is to the top of each frame. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For additional images visit the Cassini imaging team homepage http://ciclops.org . *Credit:* NASA/JPL/Space Science Institute.
Date March 9, 2005
Titan's Variety (with Grid)
Description Titan's Variety
Full Description Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For additional images visit the Cassini imaging team homepage http://ciclops.org . *Credit:* NASA/JPL/Space Science Institute, This map of Titan's surface brightness was assembled from images taken by the Cassini spacecraft over the past year, both as it approached the Saturn system and during three closer flybys in July, October and December 2004. Due to Titan's thick, hazy atmosphere, the size of surface features that can be resolved is a few to five times larger than the actual pixel scale. The pixel scales of the individual images in the map range from 88 to 2 kilometers (55 miles to 1 mile), so the scales of the surface features that can be resolved range from 180 to 10 kilometers (112 to 6 miles). The images were acquired using a near-infrared filter (centered at 938 nanometers) that has been proven effective at peering through Titan's haze to its troposphere and surface. Similar to a cloudy day on Earth, these images indicate only brightness variations, there are no shadows or topographic shading effects. The map reveals complex patterns of bright and dark material on Titan's surface. The large scale features, including Xanadu Regio -- the large, bright feature that extends from approximately 80 degrees to 130 degrees west near the equator -- have been observed from Earth over the past several years. The patterns seem to vary with latitude. Close to the equator there is more contrast in the large-scale bright and dark features, with some strikingly linear boundaries that are suggestive of geologic processes at work within Titan's crust. The southern-middle latitudes are more uniformly bright, whereas there is more dark material near the south pole. The very bright features near the south pole are clouds. High northern latitudes are not illuminated during the current season on Titan, which is southern summer. Cassini-Huygens scientists are investigating what causes the latitudinal variation in brightness. One possibility is that, similar to Earth, some parts of the surface receive higher amounts of precipitation than others over Titan's long year (29.5 Earth years), resulting in different amounts of erosion across the surface. The Huygens probe landed at approximately 10 degrees south, 190 degrees west, near a boundary between dark and bright material. By combining Huygens' very high-resolution observations (see Titan Descent) with Cassini's regional and global-scale, lower-resolution images of Titan, as well as Cassini radar and the visual and infrared mapping spectrometer observations (see Cat Scratches and Titan's Complex Surface, respectively), Cassini-Huygens scientists are working to unravel the complex history of Titan's surface. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the
Date March 9, 2005
Titan's Variety
Description Titan's Variety
Full Description Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For additional images visit the Cassini imaging team homepage http://ciclops.org . *Credit:* NASA/JPL/Space Science Institute, This map of Titan's surface brightness was assembled from images taken by the Cassini spacecraft over the past year, both as it approached the Saturn system and during three closer flybys in July, October and December 2004. Due to Titan's thick, hazy atmosphere, the size of surface features that can be resolved is a few to five times larger than the actual pixel scale. The pixel scales of the individual images in the map range from 88 to 2 kilometers (55 miles to 1 mile), so the scales of the surface features that can be resolved range from 180 to 10 kilometers (112 to 6 miles). The images were acquired using a near-infrared filter (centered at 938 nanometers) that has been proven effective at peering through Titan's haze to its troposphere and surface. Similar to a cloudy day on Earth, these images indicate only brightness variations, there are no shadows or topographic shading effects. The map reveals complex patterns of bright and dark material on Titan's surface. The large scale features, including Xanadu Regio -- the large, bright feature that extends from approximately 80 degrees to 130 degrees west near the equator -- have been observed from Earth over the past several years. The patterns seem to vary with latitude. Close to the equator there is more contrast in the large-scale bright and dark features, with some strikingly linear boundaries that are suggestive of geologic processes at work within Titan's crust. The southern-middle latitudes are more uniformly bright, whereas there is more dark material near the south pole. The very bright features near the south pole are clouds. High northern latitudes are not illuminated during the current season on Titan, which is southern summer. Cassini-Huygens scientists are investigating what causes the latitudinal variation in brightness. One possibility is that, similar to Earth, some parts of the surface receive higher amounts of precipitation than others over Titan's long year (29.5 Earth years), resulting in different amounts of erosion across the surface. The Huygens probe landed at approximately 10 degrees south, 190 degrees west, near a boundary between dark and bright material. By combining Huygens' very high-resolution observations (see Titan Descent) with Cassini's regional and global-scale, lower-resolution images of Titan, as well as Cassini radar and the visual and infrared mapping spectrometer observations (see Cat Scratches and Titan's Complex Surface, respectively), Cassini-Huygens scientists are working to unravel the complex history of Titan's surface. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the
Date March 9, 2005
Exploring the Wetlands of Ti …
Description Here on the Gallery page you can find the very latest images, videos and products from the Cassini-Huygens mission to Saturn, including the spectacular launch, spacecraft assembly and the exciting trip to Saturn.
Full Description Cassini peers through the murky orange haze of Titan to spy what are believed to be bodies of liquid hydrocarbons, two of them as large as seas on Earth, near the moon's north pole. This movie blends a near natural-color view and an infrared glimpse of Titan's surface obtained by the visual cameras, followed by a transition to imagery collected by the radar instrument aboard Cassini, for a dramatic reveal of the north pole of Saturn's largest moon. As the movie zooms in on the north pole, the most readily visible bodies are outlined in blue. The largest of these, on the left, is as big as the Caspian Sea on Earth, the next largest, on the right, is about the size of Lake Superior. When compared to the surface area of Titan however (which is six times smaller than Earth's), these bodies are equivalent in size to the Bay of Bengal and Timor Sea, respectively. Geographically speaking, they are more like seas. The movie continues with a gradual transition to a polar map of the radar imagery taken so far by Cassini of the north polar region. It is clear that one of the radar swaths has intersected a small upper bay of the largest sea, and has almost entirely imaged the second one. The extreme darkness of these regions in the radar data argues strongly for the presence of liquid hydrocarbons, such as methane and ethane, which remain liquid at Titan's frigid temperature of minus 180 degrees Celsius (minus 288 degrees Fahrenheit). See Titan (T25) Viewed by Cassini's Radar - Feb. 22, 2007. The movie continues with a pan across the pole and the radar imagery that has uncovered a multitude of much smaller lakes. Features of strikingly similar morphology to these dark northern seas and smaller lakes were first discovered in Cassini Imaging Science Subsystem images in June 2005, at Titan's south pole (see Land of Lakes?). The lake-like shoreline of the largest of these, called Ontario Lacus, its size (about the size of Lake Victoria), and its proximity to the south pole where the largest field of clouds yet seen on Titan had been observed, earned it the reputation as the best candidate for a body of liquid hydrocarbons on Titan up until that point, though the case for liquids was weak. When adjusted for the size of Titan, Ontario Lacus is equivalent in size to the Black Sea. Now, by inference, scientists are more confident that it, and the smaller features that dot the south pole, are also likely open bodies of liquid, and in aggregate make up a southern wetlands on Titan, similar to the one observed in the north polar movie. The images used to make this movie were taken with the Cassini spacecraft narrow-angle camera on Feb. 25, 2007, at a distance of approximately 1.3 million kilometers (800,000 miles) from Titan. The infrared images were taken with a special filter centered at 938 nanometers that provides the cameras' best view of Titan's surface features. This view was then composited with images taken at 619, 568 and 440 nanometers to, create a near natural color appearance. The radar data were acquired in synthetic aperture radar mode. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute
Titan: Complex 'Anti-greenho …
Description Titan: Complex 'Anti-greenhouse'
Full Description This natural color image shows Titan's upper atmosphere -- an active place where methane molecules are being broken apart by solar ultraviolet light and the byproducts combine to form compounds like ethane and acetylene. The haze preferentially scatters blue and ultraviolet wavelengths of light, making its complex layered structure more easily visible at the shorter wavelengths used in this image. A movie sequence of images, taken around the same time as this color view, shows movement of the haze layers over the course of a few hours (see Titan's Shifting Hazes). Lower down in the atmosphere, the haze turns into a globe-enshrouding smog of complex organic molecules. This thick, orange-colored haze absorbs visible sunlight, allowing only perhaps 10 percent of the light to reach the surface. The thick haze is also inefficient at holding in and then re-radiating infrared (thermal) energy back down to the surface. Thus, despite the fact that Titan has a thicker atmosphere than Earth, the thick global haze causes the greenhouse effect there to be somewhat weaker than it is on Earth. Images taken with the Cassini spacecraft wide-angle camera using red, green and blue spectral filters were combined to create this natural color view. The images were obtained at a distance of approximately 9,500 kilometers (5,900 miles) from Titan on March 31, 2005. The image scale is approximately 400 meters (1,300 feet) per pixel. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For additional images visit the Cassini imaging team homepage http://ciclops.org . Credit: NASA/JPL/Space Science Institute
Date May 2, 2005
Small Particles in Ring A
Description Small Particles in Ring A
Full Description Specially designed Cassini orbits place Earth and Cassini on opposite sides of Saturn's rings, a geometry known as occultation. Cassini conducted the first radio occultation observation of Saturn's rings on May 3, 2005. Three simultaneous radio signals of 0.94, 3.6, and 13 centimeter wavelengths (Ka-, X-, and S-bands) were sent from Cassini through the rings to Earth. The observed change of each signal as Cassini moved behind the rings provided a profile of the distribution of ring material and an optical depth profile. This simulated image was constructed from the measured optical depth profiles of the Cassini Division and ring A. It depicts the observed structure at about 10 kilometers (6 miles) in resolution. Many radial features evident across ring A, but especially exterior to the Encke and Keeler gaps (the broad and narrow black bands on the right side of the image), are wavy features called "density waves." They are caused by gravitational interaction with moons outside ring A. Color is used to represent information about ring particle sizes based on the measured effects of the three radio signals. Shades of purple indicate regions where there is a lack of particles less than 5 centimeters (about 2 inches) in diameter. Green and blue shades indicate regions where there are particles of sizes smaller than 5 centimeters (2 inches) and 1 centimeter (less than one third of an inch), respectively. Note the gradual increase in shades of green towards the outer edge of ring A. It indicates gradual increase in the abundance of 5-centimeter (2-inch) and smaller particles. Frequent collisions between large ring particles in this dynamically active region likely fragment the larger particles into more numerous smaller ones. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radio science team is based at JPL. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For more information on the radio science team visit http://saturn.jpl.nasa.gov/spacecraft/instruments-cassini-rss.cfm . Credit: NASA/JPL
Date May 23, 2005
Small Particles in Saturn's …
Description Small Particles in Saturn's Rings
Full Description Specially designed Cassini orbits place Earth and Cassini on opposite sides of Saturn's rings, a geometry known as occultation. Cassini conducted the first radio occultation observation of Saturn's rings on May 3, 2005. Three simultaneous radio signals of 0.94, 3.6, and 13 centimeter wavelengths (Ka-, X-, and S-bands) were sent from Cassini through the rings to Earth. The observed change of each signal as Cassini moved behind the rings provided a profile of the distribution of ring material as a function of distance from Saturn, or an optical depth profile. This simulated image was constructed from the measured optical depth profiles. It depicts the observed ring structure at about 10 kilometers (6 miles) in resolution. Color is used to represent information about ring particle sizes in different regions based on the measured effects of the three radio signals. Shades of purple, primarily over most of the inner ring (ring B) and the inner portion of the next ring (ring A), indicate regions where there is a lack of particles less than 5 centimeters (about 2 inches) in diameter. Green and blue shades indicate regions where there are particles of sizes smaller than 5 centimeters (2 inches) and 1 centimeter (less than one third of an inch), respectively, primarily in outer ring A and within most of ring C. From other evidence in the radio observations, all ring regions appear to be populated by a broad range of particle size distribution that extends to boulder sizes (several to many meters or yards across). 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radio science team is based at JPL. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For more information on the radio science team visit http://saturn.jpl.nasa.gov/spacecraft/instruments-cassini-rss.cfm . Credit: NASA/JPL
Date May 23, 2005
Red Spot on Titan
Description Image of an unusual bright, red spot on Titan
Full Description The visual and infrared mapping spectrometer instrument onboard Cassini has found an unusual bright, red spot on Titan. This dramatic color (but not true color) image was taken during the April 16, 2005, encounter with Titan. North is to the right. In the center it shows the dark lanes of the "H"-shaped feature (see Titan's surface revealed) discovered from Earth and first seen by Cassini last July shortly after it arrived in the Saturn system. At the southwestern edge of the "H" feature, near Titan's limb (edge), is an area roughly 500 kilometers (300 miles) across. That area is 50 percent brighter, when viewed using light with a wavelength of 5 microns, than the bright continent-sized area known as Xanadu (see Eyes on Xanadu). Xanadu extends to the northwest of the bright spot, beyond the limb (edge) of Titan in this image. Near the terminator (the line between day and night) at the bottom of this image is the 80 kilometer (50 mile) crater that has been previously seen by the Cassini radar, imaging cameras, and the visual and infrared spectrometer (see Titan Crater in Three Views). At wavelengths shorter than 5 microns, the spot is not unusually bright. The strange spectral character of this enigmatic feature has left the team with four possibilities for its source: the spot could be a surface coloration, a mountain range, a cloud, or a hot spot. The hot spot hypothesis will be tested during a Titan flyby on July 2, 2006, when the visual and infrared spectrometer will take nighttime images of this area. If it is hot, it will glow at night. This color image was created from separate images in the 1.7 micron (blue), 2.0 micron (green), and 5.0 micron (red) spectral windows through which it is possible to see Titan's surface. The yellow that humans see has a wavelength of about 0.5 microns, so the colors shown are between 3 and 10 times more red than the human eye can detect. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The visual and infrared mapping spectrometer team is based at the University of Arizona. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For additional information on the visual and infrared mapping spectrometer visit http://wwwvims.lpl.arizona.edu . Credit:NASA/JPL/University of Arizona
Date May 25, 2005
Radio Occultation: Unravelin …
Description Radio Occultation: Unraveling Saturn's Rings
Full Description Specially designed Cassini orbits place Earth and Cassini on opposite sides of Saturn's rings, a geometry known as occultation. Cassini conducted the first radio occultation observation of Saturn's rings on May 3, 2005. Three simultaneous radio signals of 0.94, 3.6, and 13 centimeter wavelength (Ka-, X-, and S-bands) were sent from Cassini through the rings to Earth. The observed change of each signal as Cassini moved behind the rings provided a profile of the distribution of ring material as a function of distance from Saturn, or an optical depth profile. This simulated image was constructed from the measured optical depth profiles. It depicts the observed ring structure at about 10 kilometers (6 miles) in resolution. Color is used to represent information about ring particle sizes in different regions based on the measured effects of the three radio signals. Purple color indicates regions where there is a lack of particles of size less than 5 centimeters (about 2 inches). Green and blue shades indicate regions where there are particles smaller than 5 centimeters (2 inches) and 1 centimeter (less than one third of one inch). The saturated broad white band near the middle of ring B is the densest region of ring B, over which two of the three radio signals were blocked at 10-kilometer (6-mile) resolution, preventing accurate color representation over this band. From other evidence in the radio observations, all ring regions appear to be populated by a broad range particle size distribution that extends to boulder sizes (several to many meters across). 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radio science team is based at JPL. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . For more information on the radio science team visit http://saturn.jpl.nasa.gov/spacecraft/instruments-cassini-rss.cfm . Credit: NASA/JPL
Date May 23, 2005
Waves and Small Particles in …
Description Waves and Small Particles in Ring A
Full Description Specially designed Cassini orbits place Earth and Cassini on opposite sides of Saturn's rings, a geometry known as occultation. Cassini conducted the first radio occultation observation of Saturn's rings on May 3, 2005. Three simultaneous radio signals at wavelengths of 0.94, 3.6, and 13 centimeters (Ka-, X-, and S-bands) were sent from Cassini through the rings to Earth. The observed change of each signal as Cassini moved behind the rings provided a profile of the distribution of ring material and an optical depth profile. This simulated image was constructed from the measured optical depth profiles of the Cassini Division and ring A. It depicts the observed structure at about 10 kilometers (6 miles) in resolution. The image shows the same ring A region depicted in a similar image (Multiple Eyes of Cassini), using a different color scheme to enhance the view of a remarkable array of over 40 wavy features called "density waves" uncovered in the May 3 radio occultation throughout ring A. Color is used to represent information about ring particle sizes based on the measured effects of the three radio signals. Shades of red indicate regions where there is a lack of particles less than 5 centimeters (about 2 inches) in diameter. Green and blue shades indicate regions where there are particles of sizes smaller than 5 centimeters (2 inches) and 1 centimeter (less than one third of an inch), respectively. Note the gradual increase in shades of green towards the outer edge of ring A. It indicates gradual increase in the abundance of 5-centimeter (2-inch) and smaller particles. Note also the blue shades in the vicinity of the Keeler gap (the narrow dark band near the edge of ring A). They indicate increased abundance of even smaller particles of diameter less than a centimeter. Frequent collisions between large ring particles in this dynamically active region likely fragment the larger particles into more numerous smaller ones. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The radio science team is based at JPL. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov. For more information on the radio science team visit http://saturn.jpl.nasa.gov/spacecraft/instruments-cassini-rss.cfm. Image Credit: NASA/JPL
Date May 23, 2005
Geologic Map of Titan Volcan …
Description Geologic Map of Titan Volcano
Full Description From infrared images that show variations in brightness and texture, a geological map of the circular feature, thought to be a volcano, has been obtained using Cassini's visual and infrared mapping spectrometer. This geologic map shows that the circular feature has what appear to be several series of flows, as shown by the black lines. The flows represent episodes of activity on the volcano. A dark central pit, called a caldera, is similar to vents that appear above reservoirs of molten material on Earth's volcanoes. The colors on the map represent the brightness of features. Yellow and light green represent bright patches. Blue represents dark patches. Red represents mottled material. The yellow area is where the volcano lies. These images were taken during Cassini's Oct. 26, 2004, flyby of Titan. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The visual and infrared mapping spectrometer team is based at the University of Arizona. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The visual and infrared mapping spectrometer team homepage is at http://wwwvims.lpl.arizona.edu . Credit: NASA/JPL/University of Arizona
Date June 8, 2005
Rhea's Memory
Description Saturn's icy moon Rhea
Full Description The story of the solar system is written upon the faces of its many worlds, such as Saturn's icy moon Rhea, seen here in an image from Cassini. The moon's many impact craters attest to its violent beginnings and more than four billion years of subsequent history. Rhea is 1,528 kilometers (949 miles) across. Most moons in the outer solar system are icy, in contrast to the rocky inner planets and Earth's moon. When the planets and their moons first formed around our Sun, conditions were cold enough at Saturn's distance that ices could condense to form solid bodies like Rhea. Since its formation, Rhea has been battered by the leftover debris of planet building, although at a much lower rate for the past 3.8 billion years or so. North on Rhea is up and rotated about 20 degrees to the left. This view shows principally the leading hemisphere on Rhea. The image was taken in visible light with the Cassini spacecraft narrow-angle camera on May 5, 2005, at a distance of approximately 1.4 million kilometers (900,000 miles) from Rhea and at a Sun-Rhea-spacecraft, or phase, angle of 78 degrees. The image scale is 9 kilometers (6 miles) per pixel. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute
Date June 23, 2005
Land of Lakes?
Description This view of Titan's south polar region reveals an intriguing dark feature
Full Description 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute, This view of Titan's south pole reveals the intriguing dark feature named Ontario Lacus and a host of smaller features dotting the south polar region. The true nature of this feature, seen here at left of center, is not yet known with absolute certainty. However, the feature's darkness, the shore-like smoothness of its perimeter, and its presence in an area where frequent convective storm clouds have been observed by Cassini and Earth-based astronomers made it the best candidate for an open body of liquid on Titan when this image was taken in June 2005. This interpretation has been strengthened by the sighting of features having similar morphologies in Titan's northern polar region during the flyby of Titan in late February (see Exploring the Wetlands of Titan). The possibility that these northern features, the sizes of small seas, are either completely or partially filled with liquid hydrocarbons is significantly strengthened by Cassini radar data that overlap portions of the Imaging Science Subsystem-observed northern bodies, (see Titan (T25) Viewed by Cassini's Radar - Feb. 22, 2007). Previously, scientists had speculated that Ontario Lacus might simply be a broad depression filled by dark, solid hydrocarbons falling from the atmosphere onto Titan's surface. In this case, the smoothed outline might be the result of a process unrelated to rainfall, such as a sinkhole or a volcanic caldera. However, the strong likelihood that the northern polar features are lakes and seas has made imaging scientists more confident that Ontario Lacus, and the smaller dark features dotting the southern polar region of Titan, also hold liquid. If correct, this new revelation would mean that each pole on Titan is a large wetlands area. The feature is named for Lake Ontario because its shape and length are similar, though the Titan feature is much wider. In actual surface area, the feature is roughly the size of Lake Victoria. However, if the relative sizes of Titan and Earth are accounted for, Ontario Lacus covers roughly the same fraction of Titan as does the Black Sea on Earth. A red cross below the center in the scene marks the pole. The brightest features seen here are methane clouds. A movie sequence showing the evolution of bright clouds in the region during the same flyby is also available (see Clouds in the Distance). This view is a composite of three narrow-angle camera images, taken over several minutes during Cassini's distant June 6, 2005, flyby. The images were combined to produce a sharper view of Titan's surface. The images were taken using a combination of spectral filters sensitive to wavelengths of polarized infrared light. The images were acquired from approximately 450,000 kilometers (279,000 miles) from Titan. Resolution in the scene is approximately 3 kilometers (2 miles) per pixel. The view has been contrast enhanced to improve the overall visibility of surface features. The Cassini-Huygens mission is a cooperative project of
Date June 28, 2005
Saturn's Icy Realm
Description Three of Saturn's icy moons are seen here
Full Description Three of Saturn's icy moons are seen here, along with the magnificent water-ice rings and the cold gaseous envelope of the planet's atmosphere. Saturn's dark shadow stretches completely across the rings. At nine and a half times farther from the Sun than Earth, Saturn inhabits the deep cold of the outer solar system. The Sun appears only 1 percent as bright there as it appears at Earth, creating an environment where ice dominates over rock. The icy Moons visible here, from left to right are: Janus (181 kilometers, or 113 miles, across), Enceladus (505 kilometers, or 314 miles, across), and Epimetheus (116 kilometers, or 72 miles, across). The image was taken in visible green light with the Cassini spacecraft wide-angle camera on June 1, 2005, at a distance of approximately 2.4 million kilometers (1.5 million miles) from Saturn. The image scale is 139 kilometers (86 miles) per pixel. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/Space Science Institute
Date July 8, 2005
SOHO Watches Saturn and Cass …
Description SOHO Watches Saturn and Cassini Pass Behind the Sun
Full Description In this SOHO image taken July 21, 2005, the Sun is represented by the white circle in the center. Saturn is the bright object to the left of the Sun. Interestingly, the streak accompanying Saturn is not the rings but a distortion caused by Saturn's brightness. Saturn is approaching "superior conjunction," that is, it will be almost directly behind the Sun from Earth -- thus the Cassini spacecraft, in orbit around Saturn, will not be able to send or receive transmissions normally. Regular science data collection has been temporarily suspended. As Cassini passes closest by the limb (edge) of the Sun on July 24 PDT, communications will be impossible because of the Sun's radio noise. The spacecraft will regain full communication with Earth on July 27, once again returning Saturn science data. In the meantime, controllers are sending approximately 100 commands per day to test communication status. Cassini radio scientists are taking advantage of this opportunity to study the Sun's corona from its effects on the radio signals that reach Earth. SOHO (Solar and Heliospheric Observatory Satellite) orbits the Sun parked in one of the five gravitational-neutral spots, called Lagrange Points. This specific spot, called L1, stays in the same place relative to the Sun and the Earth, offering a continuously uninterrupted view of the Sun. Saturn is not in sight again until the evening of July 24. After that date, it will be to the RIGHT of the sun. For more information on "superior conjunction," visit: http://www.jpl.nasa.gov/basics/bsf1-2.html#conj . For more information on the Lagrange Points, visit: http://map.gsfc.nasa.gov/m_mm/ob_techorbit1.html For more information on SOHO, visit: http://sohowww.nascom.nasa.gov/ . Finally, the latest SOHO images are available at: http://sohowww.nascom.nasa.gov/data/realtime/c3/1024/latest.gif . Credit: SOHO -- http://sohowww.nascom.nasa.gov/
Date July 22, 2005
SOHO Watches Saturn and Cass …
Description SOHO Watches Saturn and Cassini Pass Behind the Sun
Full Description In this SOHO image taken July 21, 2005, the Sun is represented by the white circle in the center. Saturn is the bright object to the left of the Sun. Interestingly, the streak accompanying Saturn is not the rings but a distortion caused by Saturn's brightness. Saturn is approaching "superior conjunction," that is, it will be almost directly behind the Sun from Earth -- thus the Cassini spacecraft, in orbit around Saturn, will not be able to send or receive transmissions normally. Regular science data collection has been temporarily suspended. As Cassini passes closest by the limb (edge) of the Sun on July 24 PDT, communications will be impossible because of the Sun's radio noise. The spacecraft will regain full communication with Earth on July 27, once again returning Saturn science data. In the meantime, controllers are sending approximately 100 commands per day to test communication status. Cassini radio scientists are taking advantage of this opportunity to study the Sun's corona from its effects on the radio signals that reach Earth. SOHO (Solar and Heliospheric Observatory Satellite) orbits the Sun parked in one of the five gravitational-neutral spots, called Lagrange Points. This specific spot, called L1, stays in the same place relative to the Sun and the Earth, offering a continuously uninterrupted view of the Sun. Saturn is not in sight again until the evening of July 24. After that date, it will be to the RIGHT of the sun. For more information on "superior conjunction," visit: http://www.jpl.nasa.gov/basics/bsf1-2.html#conj . For more information on the Lagrange Points, visit: http://map.gsfc.nasa.gov/m_mm/ob_techorbit1.html For more information on SOHO, visit: http://sohowww.nascom.nasa.gov/ . Finally, the latest SOHO images are available at: http://sohowww.nascom.nasa.gov/data/realtime/c3/1024/latest.gif . Credit: SOHO -- http://sohowww.nascom.nasa.gov/
Date July 22, 2005
Rings At Opposition
Description Rings At Opposition
Full Description When Cassini gazes down at Saturn's rings with the Sun directly behind the spacecraft, an unusual phenomenon called the "opposition effect" can be seen. The effect is visible here as a bright region, near right, toward the inner edge of the A ring. The precise nature of the effect at Saturn is still under scrutiny by imaging scientists. However the effect in Saturn's rings can be witnessed from Earth, when the viewing conditions are right. It can also be seen in photographs of the lunar surface taken by the Apollo astronauts. To understand the effect, imagine an observer standing on a dry, sandy beach. When the Sun is directly behind the observer, the shadows cast by the grains in the field of view in front of the observer will fall directly behind the grains and will not be visible. When the Sun is at any other angle relative to the observer, the shadows cast by the grains will be visible to the observer. These shadows in the field of view make the scene a bit darker. This effect would cause a centrally bright spot to appear on the sandy surface in the first case, but not in the second. For Cassini, the opposition effect is seen when the angle between the Sun, the rings and the spacecraft is extremely close to zero. For the sequence of images during which this view was obtained, Cassini maintained this viewing angle and the bright spot appeared to move across the rings with the spacecraft's motion. The moon Janus (181 kilometers, or 113 miles, across) is seen here at lower left. The image was taken in visible light with the Cassini spacecraft wide-angle camera on June 7, 2005, at a distance of approximately 738,000 kilometers (458,000 miles) from Saturn. The image scale is 40 kilometers (25 miles) per pixel. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The Cassini imaging team homepage is at http://ciclops.org. Credit: NASA/JPL/Space Science Institute
Date July 15, 2005
Warm Fractures on Enceladus
Description Warm Fractures on Enceladus
Full Description This image shows the warmest places in the south polar region of Saturn's moon Enceladus. The unexpected temperatures were discovered by Cassini's composite infrared spectrometer during a close flyby on July 14, 2005. The image shows how these temperatures correspond to the prominent, bluish fractures dubbed "tiger stripes," first imaged by Cassini's imaging science subsystem cameras. Working together the two teams were able to pinpoint the exact location of the warmest regions on Enceladus. The composite infrared spectrometer instrument measured the infrared heat radiation from the surface at wavelengths between 9 and 16.5 microns within each of the 10 squares shown here. Each square is 6 kilometers (4 miles) across. The color of each square, and the number shown above it, describe the composite infrared spectrometer's measurement of the approximate average temperature of the surface within that square. The warmest temperature squares, at 91 and 89 degrees Kelvin (minus 296 and minus 299 degrees Fahrenheit), are located over one of the "tiger stripe" fractures. They contrast sharply with the surrounding temperatures, which are in the range 74 to 81 degrees Kelvin (minus 326 to minus 313 degrees Fahrenheit). The detailed composite infrared spectrometer data suggest that small areas near the fracture are at substantially higher temperatures, well over 100 degrees Kelvin (minus 279 degrees Fahrenheit). Such "warm" temperatures are unlikely to be due to heating of the surface by the feeble sunlight striking Enceladus' south pole. They are a strong indication that internal heat is leaking out of Enceladus and warming the surface along these fractures. Evaporation of this relatively warm ice probably generates the cloud of water vapor detected above Enceladus' south pole by several other Cassini instruments. Scientists are unsure how the internal heat reaches the surface. The process might involve liquid water, slushy brine, or soft but solid ice. The imaging science subsystem image is an enhanced color view with a pixel scale of 122 meters (400 feet) that was acquired at the same time as the composite infrared spectrometer data. It covers a region 125 kilometers (75 miles) across. The spacecraft's distance from Enceladus was 21,000 kilometers (13,000 miles). The broad bluer fractures that can be seen running from the upper left to the lower right of the image are 1 to 2 kilometers (0.6 to 1.2 miles) wide and more than 100 kilometers (60 miles) long. The fractures are thought to be bluer than the surrounding surface because coarser-grained ice (which has a blue color just as thick masses of ice, like glaciers and icebergs, do on Earth) has been exposed in the fractures. The color image was constructed using an ultraviolet filter (centered at 338 nanometers) in the blue channel, a clear filter in the green channel, and an infrared filter (centered at 930 nanometers) in the red channel. 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 mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter was designed, developed and assembled at JPL. The composite infrared spectrometer team is based at NASA's Goddard Space Flight Center, Greenbelt, Md. The imaging operations center is based at the Space Science Institute in Boulder, Colo. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov . The composite infrared spectrometer team homepage is http://cirs.gsfc.nasa.gov/ . The imaging team homepage is at http://ciclops.org . Credit: NASA/JPL/GSFC/Space Science Institute
Date July 29, 2005
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