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LOS ALAMOS FIRE IMAGED BY NA …
The fire that has raged out …
5/19/00
Date 5/19/00
Description The fire that has raged out of control this month near Los Alamos, New Mexico, was captured in a series of images by the Multi-angle Imaging Spectro-Radiometer (MISR) on NASA's Terra satellite. The picture is available at http://www.jpl.nasa.gov/pictures/misr These true-color images covering north-central New Mexico capture the bluish-white smoke plume of the Los Alamos fire, just west of the Rio Grande river. The middle image is a downward-looking or "nadir" view taken by MISR. As the satellite flew from north to south, the instrument viewed the scene from nine different angles. The top image was taken by the MISR camera looking 60 degrees forward along its orbit, whereas the bottom image looks 60 degrees aft. The fire plume stands out more dramatically in the steep-angle views. Its color and brightness also change with angle. By comparison, a thin, white water cloud appears in the upper right portion of the scene, and is most easily detected in the top image. MISR scientists use these angle-to-angle differences to monitor particulate pollution and to identify different types of haze. Such observations allow scientists to study how airborne particles interact with sunlight, a measure of their impact on Earth's climate system. The images are about 400 km (250 miles) wide. The spatial resolution of the nadir image is 275 meters (300 yards), resolution is 1.1 kilometers (1,200 yards) for the off-nadir images. North is toward the top. MISR is managed by the Jet Propulsion Laboratory, a division of the California Institute of Technology, for NASA' s Office of Earth Science, Washington, D.C. The Terra satellite is managed by NASA's Goddard Space Flight Center, Greenbelt, Md. ##### Photo credit: NASA/GSFC/JPL, MISR Science Team.
MISR Views of Montana fires, …
These images show forest fir …
8/18/00
Date 8/18/00
Description These images show forest fires raging in Montana and Hurricane Hector swirling in the Pacific. These two unrelated, large-scale examples of nature's fury were captured by the Multi-angle Imaging SpectroRadiometer (MISR) during a single orbit of NASA's Terra satellite on August 14, 2000. In the left image, huge smoke plumes rise from devastating wildfires in the Bitterroot Mountain Range near the Montana-Idaho border. Flathead Lake is near the upper left, and the Great Salt Lake is at the bottom right. Smoke accumulating in the canyons and plains is also visible. This image was generated from the MISR camera that looks forward at a steep angle (60 degrees), the instrument has nine different cameras viewing Earth at different angles. The smoke is far more visible when seen at this highly oblique angle than it would be in a conventional, straight- downward (nadir) view. The wide extent of the smoke is evident from comparison with the image on the right, a view of Hurricane Hector acquired from MISR's nadir-viewing camera. Both images show an area of approximately 400 kilometers (250 miles) in width and about 850 kilometers (530 miles) in length. When this image of Hector was taken, the eastern Pacific tropical cyclone was located approximately 1,100 kilometers (680 miles) west of the southern tip of Baja California, Mexico. The eye is faintly visible and measures 25 kilometers (16 miles) in diameter. The storm was beginning to weaken, and 24 hours later the National Weather Service downgraded Hector from a hurricane to a tropical storm. MISR, built and managed by the Jet Propulsion Laboratory, is one of several Earth-observing instruments aboard Terra, which was launched in December 1999. More information about MISR is available at http://www-misr.jpl.nasa.gov . JPL is a division of the California Institute of Technology in Pasadena. # # # #
POLAR STRATOSPHERIC CLOUDS
Polar stratospheric clouds o …
4/5/00
Date 4/5/00
Description Polar stratospheric clouds over Kiruna, Sweden, on Jan. 27, 2000. The colorful appearance of these clouds is due to the small size of their droplets and their high altitude, approximately 21,300 meters (70,000 ft). The small droplets in the clouds result in separation of light of different colors due to refraction of sunlight. Their high altitude allows for full solar illumination for up to 20 minutes following sunset at the ground. These clouds, which have long been called "Mother of Pearl" by Scandinavians, participate in a chain of events that leads to ozone depletion by human-produced chlorine. Between November 1999 and March 2000, the SAGE III Ozone Loss and Validation Experiment (SOLVE) provided scientists with measurements of ozone using a variety of satellite-, airplane-, balloon- and ground-based instruments. Scientists also obtained a comprehensive inventory of numerous other atmospheric gases and information on the physical and chemical properties of polar stratospheric clouds. The SOLVE mission was co-sponsored by the Upper Atmosphere Research Program, Atmospheric Effects of Aviation Project, Atmospheric Chemistry Modeling and Analysis Program, and Earth Observing System of NASA's Earth Science Enterprise as part of the validation program for the SAGE III instrument. Based primarily in Kiruna, Sweden, the campaign included scientists from the United States, Europe, Canada, Russia and Japan. A key aspect to the success of this mission was the permission to fly both NASA research aircraft over Russia. SOLVE was managed by the Ames Research Center, Moffett Field, CA, with extensive participation by science teams from Goddard Space Flight Center, Greenbelt, MD, Langley Research Center, Hampton, VA, and the Jet Propulsion Laboratory, Pasadena, CA, as well as a number of other government laboratories and universities. The ER-2 and DC-8 aircraft are based at Dryden Flight Research Center, Edwards, CA, and the U.S. balloon operations in Sweden were conducted by a team from the National Scientific Balloon Facility, Palestine, TX.
HIGH ALTITUDE BALLOON/ARCTIC …
A NASA high-altitude researc …
4/5/00
Date 4/5/00
Description A NASA high-altitude research balloon climbing to study the composition of the Arctic stratosphere from the Esrange Balloon Launch Facility near Kiruna, Sweden. With its helium bubble expanding to the size of a large building while in the stratosphere, the balloon carried a payload of about 450 Kg. (1000 lbs) to an altitude of about 30,500 meters (100,000 ft.). Following flight, the instrument payload lands by parachute and is recovered for subsequent flights. Between November 1999 and March 2000, the SAGE III Ozone Loss and Validation Experiment (SOLVE) provided scientists with measurements of ozone using a variety of satellite-, airplane-, balloon- and ground-based instruments. Scientists also obtained a comprehensive inventory of numerous other atmospheric gases and information on the physical and chemical properties of polar stratospheric clouds. The SOLVE mission was co-sponsored by the Upper Atmosphere Research Program, Atmospheric Effects of Aviation Project, Atmospheric Chemistry Modeling and Analysis Program, and Earth Observing System of NASA's Earth Science Enterprise as part of the validation program for the SAGE III instrument. Based primarily in Kiruna, Sweden, the campaign included scientists from the United States, Europe, Canada, Russia and Japan. A key aspect to the success of this mission was the permission to fly both NASA research aircraft over Russia. SOLVE was managed by the Ames Research Center, Moffett Field, CA, with extensive participation by science teams from Goddard Space Flight Center, Greenbelt, MD, Langley Research Center, Hampton, VA, and the Jet Propulsion Laboratory, Pasadena, CA, as well as a number of other government laboratories and universities. The ER-2 and DC-8 aircraft are based at Dryden Flight Research Center, Edwards, CA, and the U.S. balloon operations in Sweden were conducted by a team from the National Scientific Balloon Facility, Palestine, TX.
OZONE INSTRUMENTS LOADED ON …
Scientists preparing their i …
4/5/00
Date 4/5/00
Description Scientists preparing their instruments for flight on the NASA ER-2 research aircraft inside the Arena Arctica hangar, Kiruna, Sweden. The plane carries dozens of instruments in two pods attached to the wings, in the Q-bay area below the cockpit and in the nose. These pieces of the plane can be detached allowing access to the instruments prior to take-off. Between November 1999 and March 2000, the SAGE III Ozone Loss and Validation Experiment (SOLVE) provided scientists with measurements of ozone using a variety of satellite-, airplane-, balloon- and ground-based instruments. Scientists also obtained a comprehensive inventory of numerous other atmospheric gases and information on the physical and chemical properties of polar stratospheric clouds. The SOLVE mission was co-sponsored by the Upper Atmosphere Research Program, Atmospheric Effects of Aviation Project, Atmospheric Chemistry Modeling and Analysis Program, and Earth Observing System of NASA's Earth Science Enterprise as part of the validation program for the SAGE III instrument. Based primarily in Kiruna, Sweden, the campaign included scientists from the United States, Europe, Canada, Russia and Japan. A key aspect to the success of this mission was the permission to fly both NASA research aircraft over Russia. SOLVE was managed by the Ames Research Center, Moffett Field, CA, with extensive participation by science teams from Goddard Space Flight Center, Greenbelt, MD, Langley Research Center, Hampton, VA, and the Jet Propulsion Laboratory, Pasadena, CA, as well as a number of other government laboratories and universities. The ER-2 and DC-8 aircraft are based at Dryden Flight Research Center, Edwards, CA, and the U.S. balloon operations in Sweden were conducted by a team from the National Scientific Balloon Facility, Palestine, TX.
ER-2 USED IN ARCTIC OZONE RE …
The NASA ER-2 high-altitude …
4/5/00
Date 4/5/00
Description The NASA ER-2 high-altitude research plane on the runway of Kiruna, Sweden. The airplane -- a civilian variant of the U-2 reconnaissance plane capable of reaching altitudes as high as 21,330 meters (70,000 feet) -- carried into the stratosphere dozens of scientific instruments that measure the composition of Earth's ozone layer. The only person on board is the pilot, who must wear a pressurized spacesuit to guard against the dangers of high-altitude flight. Between November 1999 and March 2000, the SAGE III Ozone Loss and Validation Experiment (SOLVE) provided scientists with measurements of ozone using a variety of satellite-, airplane-, balloon- and ground-based instruments. Scientists also obtained a comprehensive inventory of numerous other atmospheric gases and information on the physical and chemical properties of polar stratospheric clouds. The SOLVE mission was co-sponsored by the Upper Atmosphere Research Program, Atmospheric Effects of Aviation Project, Atmospheric Chemistry Modeling and Analysis Program, and Earth Observing System of NASA's Earth Science Enterprise as part of the validation program for the SAGE III instrument. Based primarily in Kiruna, Sweden, the campaign included scientists from the United States, Europe, Canada, Russia and Japan. A key aspect to the success of this mission was the permission to fly both NASA research aircraft over Russia. SOLVE was managed by the Ames Research Center, Moffett Field, CA, with extensive participation by science teams from Goddard Space Flight Center, Greenbelt, MD, Langley Research Center, Hampton, VA, and the Jet Propulsion Laboratory, Pasadena, CA, as well as a number of other government laboratories and universities. The ER-2 and DC-8 aircraft are based at Dryden Flight Research Center, Edwards, CA, and the U.S. balloon operations in Sweden were conducted by a team from the National Scientific Balloon Facility, Palestine, TX.
Terrain near Io's south pole
Volcanic calderas, lava flow …
4/19/00
Date 4/19/00
Description Volcanic calderas, lava flows and cliffs are seen in this false color image of a region near the south pole of Jupiter's volcanic moon Io. It was created by combining a black and white image taken by NASA's Galileo spacecraft on February 22, 2000 with lower resolution color images taken by Galileo on July 3, 1999. The three black spots (top center and middle left) are small volcanic calderas about 10-20 kilometers (6-12 miles) in size, which are dark because their floors are covered by recent lava flows. Two of these three calderas are surrounded by diffuse dark material, which may have been thrown out of the calderas by explosive eruptions. The bright, white material is thought to be sulfur-dioxide frost and is concentrated near the cliffs in this image. It may be formed when liquid sulfur dioxide seeps out at the base of mountain scarps, vaporizes into a plume of gas, liquid and solid, and then condenses again on the surface. Part of this process, called sapping, occurs in arid environments on Earth when ground water seeps out at the bases of cliffs. The vaporization and production of plumes is much more dramatic on Io due to the lower gravitational acceleration and especially the very low atmospheric pressure. It may be one of the dominant erosion processes on Io. The mountain at the center left, named Telegonus Mensae, exhibits a number of ridges parallel to its margins. These ridges have been observed on a number of other Ionian mountains and they suggest that as the mountain ages, it is collapsing outward under the influence of gravity. The yellow lava flow at the southern end of the image appears to be fed by a dark channel that connects to a dark caldera. This is a likely candidate for a lava flow composed of sulfur (rather than silicate material). The image is centered at 53.8 degrees south latitude and 117.1 degrees west longitude and north is to the top. The higher resolution image has a resolution of 350 meters (or yards) per picture element and is illuminated from the upper left. It was taken at a range of 34,000 kilometers (21,000 miles). The color images have resolutions of 1.3 kilometers (0.81 miles) per picture element and are illuminated from almost directly behind the spacecraft. They were taken at a distance of about 130,000 kilometers (81,000 miles) by Galileo's onboard camera. The Jet Propulsion Laboratory, Pasadena, CA manages the Galileo mission for NASA's Office of Space Science, Washington, DC. JPL is a division of the California Institute of Technology, Pasadena, CA. This image and other images and data received from Galileo are posted on the Galileo mission home page at http://galileo.jpl.nasa.gov . Background information and educational context for the images can be found at http://galileo.jpl.nasa.gov/images/io/ioimages.html . #####
Caldera-like depression on G …
The shallow, scalloped depre …
12/16/00
Date 12/16/00
Description The shallow, scalloped depression in the center of this picture from NASA's Galileo spacecraft is a caldera-like feature 5 to 20 kilometers (3 to 12 miles) wide on Jupiter's largest moon, Ganymede. Calderas are surface depressions formed by collapse above a subsurface concentration of molten material. Some shallow depressions in bright, smooth areas of Ganymede have some overall similarities to calderas on Earth and on Jupiter's moon Io. On Ganymede, caldera-like depressions may serve as sources of bright, volcanic flows of liquid water and slush, an idea supported by a Ganymede photo obtained by Galileo during its seventh orbit and available at http://photojournal.jpl.nasa.gov/cgi- bin/PIAGenCatalogPage.pl?PIA01614 . In the more recent image here, from Galileo's 28th orbit, a tall scarp marks the western boundary of a caldera-like feature. The western scarp is aligned similarly to older tectonic grooves visible in the image, suggesting the feature has collapsed along older lines of weakness. The interior is mottled in appearance, yet smooth compared to most of Ganymede's bright terrain seen at high resolution. The eastern boundary of the caldera-like feature is cut by younger, grooved terrain. Small impact craters pepper the scene, but the lack of a raised rim argues against an impact origin for the caldera-like feature itself. Instead, water-rich icy lava may have once flowed out of it toward the east. If so, later tectonism could have erased any telltale evidence of volcanic flow fronts. Direct evidence for icy volcanism on Ganymede continues to be elusive. North is to the top of the picture and the Sun illuminates the surface from the left. The image, centered at -24 degrees latitude and 318 degrees longitude, covers an area approximately 162 by 119 kilometers (101 by 74 miles). The resolution is 43 meters (141 feet) per picture element. This image and other images and data received from Galileo are posted on the Galileo mission home page at http://www.jpl.nasa.gov/galileo . Background information and educational context for the images can be found at http://www.jpl.nasa.gov/galileo/sepo . The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Galileo mission for NASA's Office of Space Science, Washington, D.C. This image was produced by Brown University, Providence, R.I., http://www.planetary.brown.edu/ . # # # # #
Global View of the Arctic Oc …
The Arctic Ocean has been ma …
8/21/00
Date 8/21/00
Description The Arctic Ocean has been mapped in an unprecedented manner by scientists at NASA's Jet Propulsion Laboratory (JPL), Pasadena, Calif. Using advanced radar that sees through all weather conditions, researchers will now be able to determine how the Earth's warming may be changing the sea ice cover. Sea ice in the polar region is a large barometer of global climate conditions. The mission is a joint project between JPL and the Alaska Synthetic Aperture Radar Facility, University of Alaska, Fairbanks. JPL manages the Sea Ice Thickness Derived from High Resolution Radar Imagery project for NASA's Earth Science Enterprise, Washington, DC. The Earth Science Enterprise is dedicated to studying how natural and human-induced change affects our global environment. This image is posted on the World Wide Web at http://www.jpl.nasa.gov/pictures/seaice .
Comparative Views of Arctic …
Scientists at NASA's Jet Pro …
8/21/00
Date 8/21/00
Description Scientists at NASA's Jet Propulsion Laboratory (JPL) have used high resolution radar to see, for the first time ever, the development of the Arctic sea ice cover. The images show a comparison of ice growth during the Arctic winter. The two images are separated by nine days. Both images represent an area located in the Baufort Sea, north of the Alaskan coast. This radar view covers an area of 96 by 128 kilometers (60 by 80 miles). The brighter features are older thicker ice and the darker areas show young, recently formed ice. The earlier image is shown on the left. Within the nine-day span, large and extensive cracks in the ice cover have formed due to ice movement. These cracks expose the open ocean to the cold, frigid atmosphere where sea ice grows rapidly and thickens. Formation of sea ice in the Arctic Ocean affects the heat balance in the global atmosphere and ocean. The mission is a joint project between JPL and the Alaska Synthetic Aperture Radar Facility, University of Alaska, Fairbanks. JPL manages the Sea Ice Thickness Derived from High Resolution Radar Imagery project for NASA's Earth Science Enterprise, Washington, DC. The Earth Science Enterprise is dedicated to studying how natural and human-induced change affects our global environment. This image is available at http://www.jpl.nasa.gov/pictures/seaice . #####
South Florida
These images of South Florid …
11/15/00
Date 11/15/00
Description These images of South Florida were acquired by NASA's Multi- angle Imaging Spectro-radiometer (MISR) on October 18, 2000, during orbit 4446 of the Terra Satellite. The view on the left includes Daytona Beach near the top and the Florida Keys at the bottom. Orlando appears as a grayish patch near the top of the image, just to the east of the greenish Lake Apopka, Florida's fourth largest and most polluted lake. On the east coast is Cape Canaveral, home of the Kennedy Space Center. The large body of water in the middle of the land area is Lake Okeechobee. Charlotte Harbor and Fort Myers are visible on the coast of the Gulf of Mexico to the west. Along the Atlantic coast, partially obscured by clouds, are Palm Beach, Fort Lauderdale, and Miami. Further to the east, the shallow waters and reefs of the Little Bahama and Great Bahama Banks appear in striking blue and green colors. The two right-hand images show the Florida Everglades and the Keys in more detail. Like the left-hand view, the top image is a natural color composite of blue, green and red band imagery. On the bottom is a false-color composite comprising green, red and near-infrared data. Near-infrared light is invisible to the human eye. The high reflectance of plants in this part of the electromagnetic spectrum, displayed here in shades of red, is the basis of many satellite-based techniques for detecting and characterizing vegetation. MISR, built and managed by the Jet Propulsion Laboratory, is one of several Earth-observing experiments aboard Terra, which was launched in December 1999. MISR acquires images of the Earth at nine angles simultaneously, using nine separate cameras pointed forward, downward, and backward along its flight path. All of these South Florida images are all from MISR's downward-pointing camera The MISR science team includes members in the United States, England, and Italy. Image credit: NASA/GSFC/JPL, MISR Team # # # # #
ASTER-SRTM Perspective of Mo …
Mount Oyama is a 820-meter-h …
8/10/00
Date 8/10/00
Description Mount Oyama is a 820-meter-high (2,700 feet) volcano on the island of Miyake-Jima, Japan. In late June 2000, a series of earthquakes alerted scientists to possible volcanic activity. On June 27, authorities evacuated 2,600 people, and on July 8 the volcano began erupting and erupted five times over that week. The dark gray blanket covering green vegetation in the image is the ash deposited by prevailing northeasterly winds between July 8 and 17. This island is about 180 kilometers (110 miles) south of Tokyo and is part of the Izu chain of volcanic islands that runs south from the main Japanese island of Honshu. Miyake-Jima is home to 3,800 people. The previous major eruptions of Mount Oyama occurred in 1983 and 1962, when lava flows destroyed hundreds of houses. An earlier eruption in 1940 killed 11 people. This image is a perspective view created by combining image data from the Advanced Spaceborne Thermal Emission and Reflection Radiaometer (ASTER) aboard NASA's Terra satellite with an elevation model from the Shuttle Radar Topography Mission (SRTM). Vertical relief is exaggerated, and the image includes cosmetic adjustments to clouds and image color to enhance clarity of terrain features. The ASTER instrument is a cooperative project between NASA, JPL, and the Japanese Ministry of International Trade and Industry. ASTER is operating on-board NASA's Terra platform. Elevation data used in this image was acquired by the Shuttle Radar Topography Mission (SRTM) aboard the Space Shuttle Endeavour, launched on February 11, 2000. SRTM used the same radar instrument that comprised the Spaceborne Imaging Radar-C/X- Band Synthetic Aperture Radar (SIR-C/X-SAR) that flew twice on the Space Shuttle Endeavour in 1994. SRTM was designed to collect three-dimensional measurements of the Earth's surface. To collect the 3-D data, engineers added a 60-meter-long (200-foot) mast, installed additional C-band and X-band antennas, and improved tracking and navigation devices. The mission is a cooperative project between the National Aeronautics and Space Administration (NASA), the National Imagery and Mapping Agency (NIMA) of the U.S. Department of Defense (DoD), and the German and Italian space agencies. It is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Earth Science Enterprise, Washington, DC. Size: Island is approximately 8 kilometers (5 miles) in diameter Location: 34.1 deg. North lat., 139.5 deg. East lon. Orientation: View toward the west-southwest. Image Data: ASTER visible and near infrared Date Acquired: February 20, 2000 (SRTM), July 17, 2000 (ASTER) Image: NASA/JPL/NIMA #####
Mojave to Ventura, Californi …
Southern California's dramat …
9/7/00
Date 9/7/00
Description Southern California's dramatic topography plays a critical role in the region's climate, hydrology, ecology, agriculture and habitability. This image of Southern California from NASA's Shuttle Radar Topography Mission (SRTM) shows a variety of landscapes and environments from the desert at Mojave to the ocean at Ventura. Winds usually bring moisture to this area from the west, moving from the ocean, across the coastal plains to the mountains, and then to the deserts. Most rainfall occurs as the air masses rise over the mountains and cool with altitude. Continuing east, and now drained of their moisture, the air masses drop in altitude and warm as they spread across the desert. The mountain rainfall supports forest and chaparral vegetation, seen here, and also becomes ground water and stream flow that supports citrus, avocado, strawberry, other crops, and a large and growing population on the coastal plains. This perspective view was generated by draping a Landsat satellite image over a preliminary topographic map from SRTM. It shows the Tehachapi Mountains in the right foreground, the city of Ventura on the coast at the distant left and the easternmost Santa Ynez Mountains forming the skyline at the distant right. Landsat has been providing visible and infrared views of Earth since 1972. SRTM elevation data matches the 30-meter (33-yard) resolution of most Landsat images and will substantially help in analyses of the large and growing Landsat image archive. The elevation data used in this image was acquired by SRTM aboard the Space Shuttle Endeavour, launched on February 11, 2000. SRTM used the same radar instrument that comprised the Spaceborne Imaging Radar-C/X-Band Synthetic Aperture Radar (SIR-C/X-SAR) that flew twice on the Space Shuttle Endeavour in 1994. SRTM was designed to collect three-dimensional measurements of Earth's surface. To collect the 3-D data, engineers added a 60-meter-long (200-foot) mast, installed additional C-band and X-band antennas, and improved tracking and navigation devices. The mission is a cooperative project between the National Aeronautics and Space Administration (NASA), the National Imagery and Mapping Agency (NIMA) of the U.S. Department of Defense (DoD), and the German and Italian space agencies. It is managed by NASA's Jet Propulsion Laboratory, Pasadena, Calif., for NASA's Earth Science Enterprise, Washington, D.C. #####
Perspective with Landsat Ove …
Los Angeles may be the world …
10/5/00
Date 10/5/00
Description Los Angeles may be the world's entertainment capital, but it is a difficult place to locate television and radio antennas. The metropolitan area spreads from the Pacific Ocean to Southern California's upper and lower deserts, valleys, mountains, canyons and coastal plains. While this unique geography offers something for everyone in terms of urban, suburban, small-town, and even semi-rural living, reception of television and radio signals can be problematic where there is no line-of-sight to a transmitting antenna. Broadcasters must choose antenna sites carefully in order to reach the greatest number of customers. Most local television towers are located atop Mount Wilson (elevation 1740 m =5710 ft), which is located on the front range of the San Gabriel Mountains (indistinctly visible, just right of the image center). This site is preferable to the highest peak seen here (Mount Baden-Powell, 2865 m =9399 ft) because it's closer to the urban center and has fewer obstructing peaks. It is also situated at a protruding bend in the mountain front and has few obstructions to the left and right. Computer automated methods combined with elevation models produced by SRTM will quantitatively optimize such factors in the siting of future transmission antenna installations worldwide. This perspective view looks northeastward from the Santa Monica Bay. The San Fernando Valley is on the left, Pasadena is against the mountain front at right-center, and downtown Los Angeles is on the coastal plain directly in front of Mount Baden-Powell. This image was generated by draping a Landsat satellite image over a preliminary topographic map from the Shuttle Radar Topography Mission (SRTM). Landsat has been providing visible and infrared views of the Earth since 1972. SRTM elevation data matches the 30-meter resolution of most Landsat images and will substantially help in analyses of the large and growing Landsat image archive. The elevation data used in this image was acquired by the Shuttle Radar Topography Mission aboard the Space Shuttle Endeavour, launched on February 11, 2000. SRTM used the same radar instrument that comprised the Spaceborne Imaging Radar-C/X-Band Synthetic Aperture Radar (SIR-C/X-SAR) that flew twice on the Space Shuttle Endeavour in 1994. SRTM was designed to collect three-dimensional measurements of the Earth's surface. To collect the 3-D data, engineers added a 60-meter-long (200-foot) mast, installed additional C-band and X-band antennas, and improved tracking and navigation devices. The mission is a cooperative project between the National Aeronautics and Space Administration (NASA), the National Imagery and Mapping Agency (NIMA) of the U.S. Department of Defense (DoD), and the German and Italian space agencies. It is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Earth Science Enterprise, Washington, DC. Size: 29 kilometers (18 miles) view width, 70 kilometers (43 miles) view distance Location: 34.2 deg. North lat., 118.2 deg. West lon. Orientation: View toward the northeast, 3X vertical exaggeration Image: Landsat bands 1, 2&4, 3 as blue, green, and red, respectively Date Acquired: February 16, 2000 (SRTM), November 11, 1986 (Landsat) Image: NASA/JPL/NIMA #####
San Andreas Fault in the Car …
The 1,200-kilometer (800-mil …
11/13/00
Date 11/13/00
Description The 1,200-kilometer (800-mile) San Andreas is the longest fault in California and one of the longest in North America. This perspective view of a portion of the fault was generated using data from the Shuttle Radar Topography Mission (SRTM), which flew on NASA's Space Shuttle last February, and an enhanced, true- color Landsat satellite image. The view shown looks southeast along the San Andreas where it cuts along the base of the mountains in the Temblor Range near Bakersfield. The fault is the distinctively linear feature to the right of the mountains. To the left of the range is a portion of the agriculturally rich San Joaquin Valley. In the background is the snow-capped peak of Mt. Pinos at an elevation of 2,692 meters (8,831 feet). The complex topography in the area is some of the most spectacular along the course of the fault. To the right of the fault is the famous Carrizo Plain. Dry conditions on the plain have helped preserve the surface trace of the fault, which is scrutinized by both amateur and professional geologists. In 1857, one of the largest earthquakes ever recorded in the United States occurred just north of the Carrizo Plain. With an estimated magnitude of 8.0, the quake severely shook buildings in Los Angeles, caused significant surface rupture along a 350-kilometer (220-mile) segment of the fault, and was felt as far away as Las Vegas, Nev. This portion of the San Andreas is an important area of study for seismologists. For visualization purposes, topographic heights displayed in this image are exaggerated two times. The elevation data used in this image was acquired by SRTM aboard the Space Shuttle Endeavour, launched on February 11, 2000. SRTM used the same radar instrument that comprised the Spaceborne Imaging Radar-C/X-Band Synthetic Aperture Radar (SIR-C/X-SAR) that flew twice on Endeavour in 1994. SRTM was designed to collect three-dimensional measurements of Earth's land surface. To collect the 3-D SRTM data, engineers added a mast 60 meters (about 200 feet) long, installed additional C-band and X-band antennas, and improved tracking and navigation devices. The mission is a cooperative project between the NASA, the National Imagery and Mapping Agency (NIMA) of the U.S. Department of Defense, and the German and Italian space agencies. It is managed by NASA's Jet Propulsion Laboratory, Pasadena, Calif, for NASA's Earth Science Enterprise, Washington, D.C. JPL is a division of the California Institute of Technology in Pasadena. Distance to Horizon: 73 kilometers (45.3 miles) Location: 35.42 deg. North lat., 119.5 deg. West lon. View: Toward the Southeast Date Acquired: February 16, 2000 SRTM, December 14, 1984 Landsat Image: NASA/JPL/NIMA #####
(MRPS 96969) Perspective Vie …
Japan's Mt. Fuji presents a …
12/21/00
Date 12/21/00
Description Japan's Mt. Fuji presents a beautiful backdrop for the city of Tokyo in this perspective view generated using data from the Shuttle Radar Topography Mission. Occupying most of the image foreground, Tokyo's metropolitan area, at about 13,388 square kilometers (5,169 square miles), is home to more than 32 million people, making it the most densely populated urban area in the world. Tokyo residents live within striking distance of Japan's tallest volcano, which is also the country's highest point at 3,776 meters (12,388 feet). Mt. Fuji is still considered active, although the last major eruption of this perfectly symmetrical stratovolcano came in 1707. Because of its height and spectacular scenery, Mt. Fuji is a favorite for touring, mountain climbing and hiking. In this image, elevations are represented by color, height increases from white to green to brown. For visualization purposes, topographic heights are exaggerated two times. Other SRTM views of Mt. Fuji and Tokyo can be seen in PIA-02791 and PIA-02792. The elevation data used in this image was acquired by SRTM aboard the Space Shuttle Endeavour, launched on February 11, 2000. SRTM used the same radar instrument that comprised the Spaceborne Imaging Radar-C/X-Band Synthetic Aperture Radar (SIR-C/X-SAR) that flew twice on Endeavour in 1994. SRTM was designed to collect three-dimensional measurements of Earth's land surface.
While it may look like a chi …
6/13/00
Date 6/13/00
Description While it may look like a child's toy, this small, gumball- size device developed at NASA's Jet Propulsion Laboratory, Pasadena, Calif., may someday play a critical role in solar system exploration. A group of these devices, called pods, can be collected together to form a new type of instrument called a sensor web. The individual pods contain both sensors that collect information from the surrounding environment and communication chips that transmit the data to other pods. The data finally arrives at a primary pod where it is then transmitted to the Internet or an overhead satellite. Sensor webs can be deployed from spacecraft to the surface of another planet. They will then provide scientists here on Earth with a map of that planet's environmental factors, such as trace gases possibly created by microorganisms living below the surface. This capability will help investigators evaluate environmental conditions and determine if life is possible, or has ever been possible, on another planet. Sensor webs may also be used here on Earth to aid the study and monitoring of ecosystems by allowing planetary scientists and biologists to have a continual virtual presence in an area. Precision environmental measurements in hard-to-reach environments, such as steep canyon walls or ocean floors will also be possible. JPL and the Huntington Library, Art Collections, and Botanical Gardens, San Marino, Calif., have joined forces to study micro-climates by placing these pods in various specialized gardens at the Huntington. The pods being tested there monitor local temperature, humidity, soil moisture, and light levels. JPL is managed for NASA by the California Institute of Technology in Pasadena. # # # # #
Galaxies Gather at Great Dis …
Title Galaxies Gather at Great Distances
Description Astronomers have discovered nearly 300 galaxy clusters and groups, including almost 100 located 8 to 10 billion light-years away, using the space-based Spitzer Space Telescope and the ground-based Mayall 4-meter telescope at Kitt Peak National Observatory in Tucson, Ariz. The new sample represents a six-fold increase in the number of known galaxy clusters and groups at such extreme distances, and will allow astronomers to systematically study massive galaxies two-thirds of the way back to the Big Bang. A mosaic portraying a bird's eye view of the field in which the distant clusters were found is shown at upper left. It spans a region of sky 40 times larger than that covered by the full moon as seen from Earth. Thousands of individual images from Spitzer's infrared array camera instrument were stitched together to create this mosaic. The distant clusters are marked with orange dots. Close-up images of three of the distant galaxy clusters are shown in the adjoining panels. The clusters appear as a concentration of red dots near the center of each image. These images reveal the galaxies as they were over 8 billion years ago, since that's how long their light took to reach Earth and Spitzer's infrared eyes. These pictures are false-color composites, combining ground-based optical images captured by the Mosaic-I camera on the Mayall 4-meter telescope at Kitt Peak, with infrared pictures taken by Spitzer's infrared array camera. Blue and green represent visible light at wavelengths of 0.4 microns and 0.8 microns, respectively, while red indicates infrared light at 4.5 microns. Kitt Peak National Observatory is part of the National Optical Astronomy Observatory in Tuscon, Ariz.
Galaxies Gather at Great Dis …
Title Galaxies Gather at Great Distances
Description Astronomers have discovered nearly 300 galaxy clusters and groups, including almost 100 located 8 to 10 billion light-years away, using the space-based Spitzer Space Telescope and the ground-based Mayall 4-meter telescope at Kitt Peak National Observatory in Tucson, Ariz. The new sample represents a six-fold increase in the number of known galaxy clusters and groups at such extreme distances, and will allow astronomers to systematically study massive galaxies two-thirds of the way back to the Big Bang. A mosaic portraying a bird's eye view of the field in which the distant clusters were found is shown at upper left. It spans a region of sky 40 times larger than that covered by the full moon as seen from Earth. Thousands of individual images from Spitzer's infrared array camera instrument were stitched together to create this mosaic. The distant clusters are marked with orange dots. Close-up images of three of the distant galaxy clusters are shown in the adjoining panels. The clusters appear as a concentration of red dots near the center of each image. These images reveal the galaxies as they were over 8 billion years ago, since that's how long their light took to reach Earth and Spitzer's infrared eyes. These pictures are false-color composites, combining ground-based optical images captured by the Mosaic-I camera on the Mayall 4-meter telescope at Kitt Peak, with infrared pictures taken by Spitzer's infrared array camera. Blue and green represent visible light at wavelengths of 0.4 microns and 0.8 microns, respectively, while red indicates infrared light at 4.5 microns. Kitt Peak National Observatory is part of the National Optical Astronomy Observatory in Tuscon, Ariz.
Galaxies Gather at Great Dis …
Title Galaxies Gather at Great Distances
Description Astronomers have discovered nearly 300 galaxy clusters and groups, including almost 100 located 8 to 10 billion light-years away, using the space-based Spitzer Space Telescope and the ground-based Mayall 4-meter telescope at Kitt Peak National Observatory in Tucson, Ariz. The new sample represents a six-fold increase in the number of known galaxy clusters and groups at such extreme distances, and will allow astronomers to systematically study massive galaxies two-thirds of the way back to the Big Bang. A mosaic portraying a bird's eye view of the field in which the distant clusters were found is shown at upper left. It spans a region of sky 40 times larger than that covered by the full moon as seen from Earth. Thousands of individual images from Spitzer's infrared array camera instrument were stitched together to create this mosaic. The distant clusters are marked with orange dots. Close-up images of three of the distant galaxy clusters are shown in the adjoining panels. The clusters appear as a concentration of red dots near the center of each image. These images reveal the galaxies as they were over 8 billion years ago, since that's how long their light took to reach Earth and Spitzer's infrared eyes. These pictures are false-color composites, combining ground-based optical images captured by the Mosaic-I camera on the Mayall 4-meter telescope at Kitt Peak, with infrared pictures taken by Spitzer's infrared array camera. Blue and green represent visible light at wavelengths of 0.4 microns and 0.8 microns, respectively, while red indicates infrared light at 4.5 microns. Kitt Peak National Observatory is part of the National Optical Astronomy Observatory in Tuscon, Ariz.
Galaxies Gather at Great Dis …
Title Galaxies Gather at Great Distances
Description Astronomers have discovered nearly 300 galaxy clusters and groups, including almost 100 located 8 to 10 billion light-years away, using the space-based Spitzer Space Telescope and the ground-based Mayall 4-meter telescope at Kitt Peak National Observatory in Tucson, Ariz. The new sample represents a six-fold increase in the number of known galaxy clusters and groups at such extreme distances, and will allow astronomers to systematically study massive galaxies two-thirds of the way back to the Big Bang. A mosaic portraying a bird's eye view of the field in which the distant clusters were found is shown at upper left. It spans a region of sky 40 times larger than that covered by the full moon as seen from Earth. Thousands of individual images from Spitzer's infrared array camera instrument were stitched together to create this mosaic. The distant clusters are marked with orange dots. Close-up images of three of the distant galaxy clusters are shown in the adjoining panels. The clusters appear as a concentration of red dots near the center of each image. These images reveal the galaxies as they were over 8 billion years ago, since that's how long their light took to reach Earth and Spitzer's infrared eyes. These pictures are false-color composites, combining ground-based optical images captured by the Mosaic-I camera on the Mayall 4-meter telescope at Kitt Peak, with infrared pictures taken by Spitzer's infrared array camera. Blue and green represent visible light at wavelengths of 0.4 microns and 0.8 microns, respectively, while red indicates infrared light at 4.5 microns. Kitt Peak National Observatory is part of the National Optical Astronomy Observatory in Tuscon, Ariz.
Galaxies Gather at Great Dis …
Title Galaxies Gather at Great Distances
Description Astronomers have discovered nearly 300 galaxy clusters and groups, including almost 100 located 8 to 10 billion light-years away, using the space-based Spitzer Space Telescope and the ground-based Mayall 4-meter telescope at Kitt Peak National Observatory in Tucson, Ariz. The new sample represents a six-fold increase in the number of known galaxy clusters and groups at such extreme distances, and will allow astronomers to systematically study massive galaxies two-thirds of the way back to the Big Bang. A mosaic portraying a bird's eye view of the field in which the distant clusters were found is shown at upper left. It spans a region of sky 40 times larger than that covered by the full moon as seen from Earth. Thousands of individual images from Spitzer's infrared array camera instrument were stitched together to create this mosaic. The distant clusters are marked with orange dots. Close-up images of three of the distant galaxy clusters are shown in the adjoining panels. The clusters appear as a concentration of red dots near the center of each image. These images reveal the galaxies as they were over 8 billion years ago, since that's how long their light took to reach Earth and Spitzer's infrared eyes. These pictures are false-color composites, combining ground-based optical images captured by the Mosaic-I camera on the Mayall 4-meter telescope at Kitt Peak, with infrared pictures taken by Spitzer's infrared array camera. Blue and green represent visible light at wavelengths of 0.4 microns and 0.8 microns, respectively, while red indicates infrared light at 4.5 microns. Kitt Peak National Observatory is part of the National Optical Astronomy Observatory in Tuscon, Ariz.
Galaxies Gather at Great Dis …
Title Galaxies Gather at Great Distances
Description Astronomers have discovered nearly 300 galaxy clusters and groups, including almost 100 located 8 to 10 billion light-years away, using the space-based Spitzer Space Telescope and the ground-based Mayall 4-meter telescope at Kitt Peak National Observatory in Tucson, Ariz. The new sample represents a six-fold increase in the number of known galaxy clusters and groups at such extreme distances, and will allow astronomers to systematically study massive galaxies two-thirds of the way back to the Big Bang. A mosaic portraying a bird's eye view of the field in which the distant clusters were found is shown at upper left. It spans a region of sky 40 times larger than that covered by the full moon as seen from Earth. Thousands of individual images from Spitzer's infrared array camera instrument were stitched together to create this mosaic. The distant clusters are marked with orange dots. Close-up images of three of the distant galaxy clusters are shown in the adjoining panels. The clusters appear as a concentration of red dots near the center of each image. These images reveal the galaxies as they were over 8 billion years ago, since that's how long their light took to reach Earth and Spitzer's infrared eyes. These pictures are false-color composites, combining ground-based optical images captured by the Mosaic-I camera on the Mayall 4-meter telescope at Kitt Peak, with infrared pictures taken by Spitzer's infrared array camera. Blue and green represent visible light at wavelengths of 0.4 microns and 0.8 microns, respectively, while red indicates infrared light at 4.5 microns. Kitt Peak National Observatory is part of the National Optical Astronomy Observatory in Tuscon, Ariz.
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 *Jupiter in blue, ultraviolet and near infrared* October 23, 2000 These three images of Jupiter, taken through the narrow angle camera of NASA's Cassini spacecraft from a distance of 77.6 million kilometers (48.2 million miles) on October 8, reveal more than is apparent to the naked eye through a telescope. The image on the left was taken through the blue filter. The one in the middle was taken in the ultraviolet. The one on the right was taken in the near infrared. The blue-light filter is within the part of the electromagnetic spectrum detectable by the human eye. The appearance of Jupiter in this image is, consequently, very familiar. The Great Red Spot (below and to the right of center) and the planet's well-known banded cloud lanes are obvious. The brighter bands of clouds are called zones and are probably composed of ammonia ice particles. The darker bands are called belts and are made dark by particles of unknown composition intermixed with the ammonia ice. Jupiter's appearance changes dramatically in the ultraviolet and near infrared images. These images are near negatives of each other and illustrate the way in which observations in different wavelength regions can reveal different physical regimes on the planet. All gases scatter sunlight efficiently at short wavelengths, this is why the sky appears blue on Earth. The effect is even more pronounced in the ultraviolet. The gases in Jupiter's atmosphere, above the clouds, are no different. They scatter strongly in the ultraviolet, making the deep banded cloud layers invisible in the middle image. Only the very high altitude haze appears dark against the bright background. The contrast is reversed in the near infrared, where methane gas, abundant on Jupiter but not on Earth, is strongly absorbing and therefore appears dark. Again the deep clouds are invisible, but now the high altitude haze appears relatively bright against the dark background. High altitude haze is seen over the poles and the equator. The Great Red Spot, prominent in all images, is obviously a feature whose influence extends high in the atmosphere. As the Cassini cameras continue to return images of Jupiter, it will be possible to construct a three-dimensional picture of how clouds form and evolve by watching the changing appearance of Jupiter in different spectral regions. JPL manages the Cassini mission for NASA's Office of Space Science, Washington, D.C. JPL is a division of the California Institute of Technology in Pasadena. Credit: NASA/JPL/University of Arizona, (PIA02822) For higher resolution, click here.
Description Jupiter Aurora
Full Description Solar Wind and Aurora at Jupiter March 8, 2001 For higher resolution image, click here. NASA's Earth-orbiting Hubble Space Telescope and Saturn-bound Cassini spacecraft recently provided scientists an opportunity to watch whether changes in Jupiter's glowing auroras correspond in timing to fluctuations in the solar wind reaching Jupiter. While Cassini passed near Jupiter in December 2000 and January 2001, the Hubble telescope obtained ultraviolet images of the ring-shaped aurora near Jupiter's north pole. The auroras, comparable to Earth's northern lights, are glows caused when charged particles steered by the planet's magnetic field excite gases high in the atmosphere. They give an indication of conditions in the invisible magnetic field. The Hubble images were taken at times when instruments on Cassini were measuring the solar wind approaching Jupiter. The solar wind is a fluctuating stream of particles speeding away from the Sun. The Cassini measurements allowed scientists to extrapolate the properties of the solar wind even closer to Jupiter, where it interacts with the planet's magnetic field. One example of these sets of data is presented in this pair of images. An image of Jupiter's northern aurora, taken by Hubble on Dec. 16, 2000, shows the aurora as a white loop against a blue background in the top frame. The bottom frame presents information that Cassini's plasma spectrometer and magnetometer instruments collected about the solar wind reaching Jupiter at the same time. It gives measurements of the solar wind's speed, density, pressure and magnetic-field direction. The Hubble Space Telescope is a project of international cooperation between NASA and the European Space Agency (ESA). It is managed for NASA by the Space Telescope Science Institute, Baltimore, Md. Cassini, on course to reach Saturn in 2004, is a cooperative mission of NASA, ESA and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages Cassini for NASA's Office of Space Science, Washington, D.C. More information about the studies of Jupiter while Cassini passed it available online at: http://www.jpl.nasa.gov/jupiterflyby . Credit: NASA/JPL/University of Michigan
Cassini Jupiter Portrait
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 This true color mosaic of Jupiter was constructed from images taken by the narrow angle camera onboard NASA's Cassini spacecraft on December 29, 2000, during its closest approach to the giant planet at a distance of approximately 10 million kilometers (6.2 million miles). It is the most detailed global color portrait of Jupiter ever produced, the smallest visible features are approximately 60 kilometers (37 miles) across. The mosaic is composed of 27 images: nine images were required to cover the entire planet in a tic-tac-toe pattern, and each of those locations was imaged in red, green, and blue to provide true color. Although Cassini's camera can see more colors than humans can, Jupiter's colors in this new view look very close to the way the human eye would see them. Everything visible on the planet is a cloud. The parallel reddish-brown and white bands, the white ovals, and the large Great Red Spot persist over many years despite the intense turbulence visible in the atmosphere. The most energetic features are the small, bright clouds to the left of the Great Red Spot and in similar locations in the northern half of the planet. These clouds grow and disappear over a few days and generate lightning. Streaks form as clouds are sheared apart by Jupiter's intense jet streams that run parallel to the colored bands. The prominent dark band in the northern half of the planet is the location of Jupiter's fastest jet stream, with eastward winds of 480 kilometers (300 miles) per hour. Jupiter's diameter is eleven times that of Earth, so the smallest storms on this mosaic are comparable in size to the largest hurricanes on Earth. Unlike Earth, where only water condenses to form clouds, Jupiter's clouds are made of ammonia, hydrogen sulfide, and water. The updrafts and downdrafts bring different mixtures of these substances up from below, leading to clouds at different heights. The brown and orange colors may be due to trace chemicals dredged up from deeper levels of the atmosphere, or they may be byproducts of chemical reactions driven by ultraviolet light from the Sun. Bluish areas, such as the small features just north and south of the equator, are areas of reduced cloud cover, where one can see deeper. For more information, see the Cassini Project home page, http://saturn.jpl.nasa.gov and the Cassini imaging team home page, http://ciclops.org. The imaging team is based at the Space Science Institute, Boulder, Colo. 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 mission for NASA's Office of Space Science, Washington, D.C. Image Credit: NASA/JPL/Space Science Institute
Earth's San Andreas Fault
title Earth's San Andreas Fault
date 02.11.2000
description The Earth's surface is broken. Cracks in the Earth's crust known as faults can run for hundreds of kilometers. These faults are frequently the sites of major earthquakes as the tectonic plates that cover the surface of the Earth shift. Pictured above is San Andreas Fault in California, one of the longest and most active faults. Visible as the linear feature to the right of the mountains, San Andreas Fault reaches 15 kilometers deep and is about 20 million years old. The above exaggerated-height image was created by combining radar deployed by the Space Shuttle Endeavour in February 2000 with a true-color Landsat picture. Along San Andreas Fault, the titanic Pacific Plate is shifting relative to the huge North American Plate by an average of a few centimeters per year. At that rate, in a few million years, the Earth's surface will look quite different than it does today.
Asteroid 216 Kleopatra
title Asteroid 216 Kleopatra
date 05.04.2000
description These images show several views from a radar-based computer model of asteroid 216 Kleopatra. The object, located in the main asteroid belt between Mars and Jupiter, is about 217 kilometers (135 miles) long and about 94 kilometers (58 miles) wide, or about the size of New Jersey. This dog bone-shaped asteroid is an apparent leftover from an ancient, violent cosmic collision. Kleopatra is one of several dozen asteroids whose coloring suggests they contain metal. A team of astronomers observing Kleopatra used the 305-meter (1,000-foot) telescope of the Arecibo Observatory in Puerto Rico to bounce encoded radio signals off Kleopatra. Using sophisticated computer analysis techniques, they decoded the echoes, transformed them into images, and assembled a computer model of the asteroid's shape. The images were obtained when Kleopatra was about 171 million kilometers (106 million miles) from Earth. This model is accurate to within about 15 kilometers (9 miles). *Image Credit*: NASA/JPL/Northwestern University
Mars River Delta?
title Mars River Delta?
description A high-resolution TIFF file of this image is available at http://photojournal.jpl.nasa.gov/catalog/PIA04869. Details in a fan-shaped deposit discovered by NASA's Mars Global Surveyor orbiter provide evidence that some ancient rivers on Mars flowed for a long time, not just in brief, intense floods. The apron of debris filling the middle of this picture from the spacecraft's Mars Orbiter Camera is a hardened and eroded distributory fan, a type of geological feature that includes river deltas and alluvial fans. Sediments transported through valleys by water on early Mars formed the 13-kilometer-long (8-mile) deposit in the distant past, when it was still possible for liquid water to flow across the martian surface. Mars Orbiter Camera team members published discovery of this feature in the online edition of the journal Science. What is important about it? First, it provides unequivocal evidence that some valleys on Mars experienced persistent flow over considerable periods of time, as rivers do on Earth. Second, because the fan is today a deposit of sedimentary rock, it demonstrates that some sedimentary rocks on Mars were deposited in a liquid environment. Third, the fan's general shape, the pattern of its channels, and its low slopes provide circumstantial evidence that the feature was an actual delta -- that is, a deposit made when a river or stream enters a body of water. If so, this landform is a strong indicator that some craters and basins on Mars once held lakes. Hundreds of other locations on Mars where valleys enter craters and basins have been imaged by the Mars Orbiter Camera, but none has shown landforms like those presented here. The picture is a mosaic of images acquired between August 2000 and September 2003. The area covered 14 kilometer (8.7 miles) by 19.3 kilometers (12 miles). North is up. Sunlight illuminates the scene from the left. The spacecraft's narrow-angle camera takes grayscale images, the color added is based on information from a camera on Mars Odyssey. The fan is in an unnamed crater that is 64 kilometers (40 miles) in diameter, at 24.3 degrees south latitude, 33.5 degrees west longitude. The crater lies northeast of a larger one named Holden Crater. The fan is a fossil landform. That is, it is an eroded remnant of a somewhat larger and thicker deposit. The originally loose sediment was turned to rock and then eroded over time to present the features seen today. The channels through which sediment was transported are no longer present. Instead, only their floors remain, and these have been elevated by erosion so that former channels now stand as ridges. The floors of former channels became inverted in this way because they were more resistant to the forces of erosion, indicating they either were more strongly cemented than surrounding materials, or they have more coarse grains (which are harder to remove), or both. *Image Credit*: NASA/JPL/Malin Space Science Systems
An Eruption on Io
title An Eruption on Io
date 02.26.2007
description The first images returned to Earth by New Horizons during its close encounter with Jupiter feature the Galilean moon Io, snapped with the Long Range Reconnaissance Imager (LORRI) at 0840 UTC on February 26, while the moon was 2.5 million miles (4 million kilometers) from the spacecraft. Io is intensely heated by its tidal interaction with Jupiter and is thus extremely volcanically active. That activity is evident in these images, which reveal an enormous dust plume, more than 150 miles high, erupting from the volcano Tvashtar. The plume appears as an umbrella-shaped feature of the edge of Io's disk in the 11 o'clock position in the right image, which is a long-exposure (20-millisecond) frame designed specifically to look for plumes like this. The bright spots at 2 o'clock are high mountains catching the setting sun, beyond them the night side of Io can be seen, faintly illuminated by light reflected from Jupiter itself. The left image is a shorter exposure -- 3 milliseconds -- designed to look at surface features. In this frame, the Tvashtar volcano shows as a dark spot, also at 11 o'clock, surrounded by a large dark ring, where an area larger than Texas has been covered by fallout from the giant eruption. This is the clearest view yet of a plume from Tvashtar, one of Io's most active volcanoes. Ground-based telescopes and the Galileo Jupiter orbiter first spotted volcanic heat radiation from Tvashtar in November 1999, and the Cassini spacecraft saw a large plume when it flew past Jupiter in December 2000. The Keck telescope in Hawaii picked up renewed heat radiation from Tvashtar in spring 2006, and just two weeks ago the Hubble Space Telescope saw the Tvashtar plume in ultraviolet images designed to support the New Horizons flyby. Most of those images will be stored onboard the spacecraft for downlink to Earth in March and April. Image Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Southwest Research Institute
Jupiter Portrait
title Jupiter Portrait
description This true color mosaic of Jupiter was constructed from images taken by the narrow angle camera onboard NASA's Cassini spacecraft on December 29, 2000, during its closest approach to the giant planet at a distance of approximately 10 million kilometers (6.2 million miles). It is the most detailed global color portrait of Jupiter ever produced, the smallest visible features are approximately 60 kilometers (37 miles) across. The mosaic is composed of 27 images: nine images were required to cover the entire planet in a tic-tac-toe pattern, and each of those locations was imaged in red, green, and blue to provide true color. Although Cassini's camera can see more colors than humans can, Jupiter's colors in this new view look very close to the way the human eye would see them. Everything visible on the planet is a cloud. The parallel reddish-brown and white bands, the white ovals, and the large Great Red Spot persist over many years despite the intense turbulence visible in the atmosphere. The most energetic features are the small, bright clouds to the left of the Great Red Spot and in similar locations in the northern half of the planet. These clouds grow and disappear over a few days and generate lightning. Streaks form as clouds are sheared apart by Jupiter's intense jet streams that run parallel to the colored bands. The prominent dark band in the northern half of the planet is the location of Jupiter's fastest jet stream, with eastward winds of 480 kilometers (300 miles) per hour. Jupiter's diameter is eleven times that of Earth, so the smallest storms on this mosaic are comparable in size to the largest hurricanes on Earth. Unlike Earth, where only water condenses to form clouds, Jupiter's clouds are made of ammonia, hydrogen sulfide, and water. The updrafts and downdrafts bring different mixtures of these substances up from below, leading to clouds at different heights. The brown and orange colors may be due to trace chemicals dredged up from deeper levels of the atmosphere, or they may be byproducts of chemical reactions driven by ultraviolet light from the Sun. Bluish areas, such as the small features just north and south of the equator, are areas of reduced cloud cover, where one can see deeper. For more information, see the Cassini Project home page, http://saturn.jpl.nasa.gov and the Cassini imaging team home page, http://ciclops.org. The imaging team is based at the Space Science Institute, Boulder, Colo. A high-resolution TIFF version of this image is available at http://photojournal.jpl.nasa.gov/catalog/PIA04866. *Image Credit*: NASA/JPL/Space Science Institute
3-D Perspective Kamchatka Pe …
Title 3-D Perspective Kamchatka Peninsula Russia
Full Description This perspective view shows the western side of the volcanically active Kamchatka Peninsula in eastern Russia. The image was generated using the first data collected during the Shuttle Radar Topography Mission (SRTM). In the foreground is the Sea of Okhotsk. Inland from the coast, vegetated floodplains and low relief hills rise toward snow capped peaks. The topographic effects on snow and vegetation distribution are very clear in this near-horizontal view. Forming the skyline is the Sredinnyy Khrebet, the volcanic mountain range that makes up the spine of the peninsula. High resolution SRTM topographic data will be used by geologists to study how volcanoes form and to understand the hazards posed by future eruptions. This image was generated using topographic data from SRTM and an enhanced true-color image from the Landsat 7 satellite. This image contains about 2,400 meters (7,880 feet) of total relief. The topographic expression was enhanced by adding artificial shading as calculated from the SRTM elevation model. The Landsat data was provided by the United States Geological Survey's Earth Resources Observations Systems (EROS) Data Center, Sioux Falls, South Dakota. SRTM, launched on February 11, 2000, used the same radar instrument that comprised the Spaceborne Imaging Radar-C/X-Band Synthetic Aperture Radar (SIR-C/X-SAR) that flew twice on the Space Shuttle Endeavour in 1994. To collect the 3-D SRTM data, engineers added a 60- meter-long (200-foot) mast, installed additional C-band and X-band antennas, and improved tracking and navigation devices. SRTM collected three dimensional measurements of nearly 80 percent of the Earth's surface. SRTM is a cooperative project between NASA, the National Imagery and Mapping Agency (NIMA) of the U.S. Department of Defense, and the German and Italian space agencies. Size: 33.3 km (20.6 miles) wide x 136 km (84 miles) coast to skyline. Location: 58.3 deg. North lat., 160 deg. East long. Orientation: Easterly view, 2 degrees down from horizontal. Original Data Resolution: 30 meters (99 feet). Vertical Exaggeration: 3 times.
Date 02/12/2000
NASA Center Jet Propulsion Laboratory
3-D Perspective Pasadena, Ca …
Title 3-D Perspective Pasadena, California
Full Description This perspective view shows the western part of the city of Pasadena, California, looking north towards the San Gabriel Mountains. Portions of the cities of Altadena and La Canada, Flintridge are also shown. The image was created from three datasets: the Shuttle Radar Topography Mission (SRTM) supplied the elevation data, Landsat data from November 11, 1986 provided the land surface color (not the sky) and U.S. Geological Survey digital aerial photography provides the image detail. The Rose Bowl, surrounded by a golf course, is the circular feature at the bottom center of the image. The Jet Propulsion Laboratory is the cluster of large buildings north of the Rose Bowl at the base of the mountains. A large landfill, Scholl Canyon, is the smooth area in the lower left corner of the scene. This image shows the power of combining data from different sources to create planning tools to study problems that affect large urban areas. In addition to the well-known earthquake hazards, Southern California is affected by a natural cycle of fire and mudflows. Wildfires strip the mountains of vegetation, increasing the hazards from flooding and mudflows for several years afterwards. Data such as shown on this image can be used to predict both how wildfires will spread over the terrain and also how mudflows will be channeled down the canyons. The Shuttle Radar Topography Mission (SRTM), launched on February 11, 2000, uses the same radar instrument that comprised the Spaceborne Imaging Radar-C/X-Band Synthetic Aperture Radar (SIR-C/X-SAR) that flew twice on the Space Shuttle Endeavour in 1994. The mission was designed to collect three dimensional measurements of the Earth's surface. To collect the 3-D data, engineers added a 60-meter-long (200-foot) mast, an additional C-band imaging antenna and improved tracking and navigation devices. The mission is a cooperative project between the National Aeronautics and Space Administration (NASA), the National Imagery and Mapping Agency (NIMA) and the German (DLR) and Italian (ASI) space agencies. It is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Earth Science Enterprise, Washington, DC. Size: 5.8 km (3.6 miles) x 10 km (6.2 miles) Location: 34.16 deg. North lat., 118.16 deg. West lon. Orientation: Looking North Original Data Resolution: SRTM, 30 meters, Landsat,30 meters, Aerial Photo, 3 meters (no vertical exaggeration)
Date 02/16/2000
NASA Center Jet Propulsion Laboratory
Evidence for Recent Liquid W …
Title Evidence for Recent Liquid Water on Mars
Full Description Newton Crater is a large basin formed by an asteroid impact that probably occurred more than 3 billion years ago. It is approximately 287 kilometers (178 miles) across. The picture shown here (top) highlights the north wall of a specific, smaller crater located in the southwestern quarter of Newton Crater (above). The crater of interest was also formed by an impact, it is about 7 km (4.4 mi) across, which is about 7 times bigger than the famous Meteor Crater in northern Arizona in North America. The north wall of the small crater has many narrow gullies eroded into it. These are hypothesized to have been formed by flowing water and debris flows. Debris transported with the water created lobed and finger-like deposits at the base of the crater wall where it intersects the floor (bottom center top image). Many of the finger-like deposits have small channels indicating that a liquid, most likely water, flowed in these areas. Hundreds of individual water and debris flow events might have occurred to create the scene shown here. Each outburst of water from higher up on the crater slopes would have constituted a competition between evaporation, freezing, and gravity. The individual deposits at the ends of channels in this MOC image mosaic were used to get a rough estimate of the minimum amount of water that might be involved in each flow event. This is done first by assuming that the deposits are like debris flows on Earth. In a debris flow, no less than about 10% (and no more than 30%) of their volume is water. Second, the volume of an apron deposit is estimated by measuring the area covered in the MOC image and multiplying it by a conservative estimate of thickness, 2 meters (6.5 feet). For a flow containing only 10% water, these estimates conservatively suggest that about 2.5 million liters (660,000 gallons) of water are involved in each event, this is enough to fill about 7 community-sized swimming pools or enough to supply 20 people with their water needs for a year. The Mars Orbiter Camera (MOC) high resolution view is located near 41.1S, 159.8W and is a mosaic of three different pictures acquired between January and May 2000. The MOC scene is illuminated from the left, north is up.
Date 06/22/2000
NASA Center Jet Propulsion Laboratory
Evidence for Recent Liquid W …
Title Evidence for Recent Liquid Water on Mars: Gullies
Full Description Gully landforms proposed to have been caused by geologically-recent seepage and runoff of liquid water on Mars are found in the most unlikely places. They typically occur in areas that are quite cold, well below freezing all year round. Like the old adage about moss on trees, nearly all of them form on slopes that face away from sunlight. Most of the gullies occur at latitudes between 30 and 70. The highest latitude at which martian gullies have been found is around 70-75 S on the walls of pits developed in the south polar pitted plains. If you were at this same latitude on Earth, you would be in Antarctica. This region spends much of the winter--which lasts approximately 6 months on Mars--in darkness and at temperatures cold enough to freeze carbon dioxide (around -130C or -200F). Nevertheless, gullies with very sharp, deep, v-shaped channels are seen on the pit walls. Based upon the locations of the tops of the channels on the slope shown here, the inferred site of liquid seepage is located at a layer in the pit wall about 1/3 of the way down from the top of the MOC image. The channels start wide and taper downslope. The area above the channels is layered and has been eroded by mass movement dry avalanching of debris--to form a pattern of chutes and ridges on the upper slope of the pit wall. The top layer appears to have many boulders in it (each about the size of a small house), these boulders are left behind on the upper slopes of the pit wall as debris is removed.
Date 06/22/2000
NASA Center Jet Propulsion Laboratory
Hubble Sees Comet Linear Blo …
Title Hubble Sees Comet Linear Blow its Top
Hubble Sees Comet Linear Blo …
Title Hubble Sees Comet Linear Blow its Top
Hubble Discovers Missing Pie …
Title Hubble Discovers Missing Pieces of Comet Linear
Hubble Sees Comet Linear Blo …
Title Hubble Sees Comet Linear Blow its Top
Hubble Discovers Missing Pie …
Title Hubble Discovers Missing Pieces of Comet Linear
Hubble Discovers Missing Pie …
Title Hubble Discovers Missing Pieces of Comet Linear
Hubble Discovers Missing Pie …
Title Hubble Discovers Missing Pieces of Comet Linear
Hubble Sees Comet Linear Blo …
Title Hubble Sees Comet Linear Blow its Top
IC 418: The "Spirograph" Neb …
Title IC 418: The "Spirograph" Nebula
General Information What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. Back to top [ #top ]
Astronomers Puzzled over Com …
Title Astronomers Puzzled over Comet LINEAR's Missing Pieces
Celestial Fireworks
Title Celestial Fireworks
General Information What is Hubble Heritage? A monthly showcase of new and archival Hubble images. Go to the Heritage site. Back to top [ #top ]
3D View of Mount Miyake-Jima …
Title 3D View of Mount Miyake-Jima, Japan
Description This 3D perspective view shows the Japanese island called Miyake-Jima viewed from the northeast. This island?about 180 kilometers (110 miles) south of Tokyo?is part of the Izu chain of volcanic islands that runs south from the main Japanese island of Honshu. Dominated by the 820-meter-high (2,700 feet) volcano Mount Oyama, Miyake-Jima is home to 3,800 people. In late June 2000, a series of earthquakes alerted scientists to possible volcanic activity and on June 27 authorities evacuated 2,600 people. On July 7, the island was hit by a typhoon passing overhead, and on July 8 the volcano began erupting. The volcano erupted five times over the next week, spreading gray ash over surrounding areas. Detailed topographic information can be used to predict the directions that lava flows will take. The previous major eruption of Mount Oyama occurred in 1983, when lava flows destroyed hundreds of houses, and an earlier eruption in 1940 killed 11 people. This three-dimensional perspective view was generated using topographic data from the Shuttle Radar Topography Mission. A computer-generated artificial light source illuminates the elevation data to produce a pattern of light and shadows, while colors show the elevation as measured by SRTM. Slopes facing the light appear bright, while those facing away are shaded. On flatter surfaces, the pattern of light and shadows can reveal subtle features in the terrain. The elevation is indicated by colors. Lowest elevation areas appear blue, medium elevations appear green, while higher elevations appear brown and white. The Shuttle Radar Topography Mission (SRTM), launched on February 11, 2000, used the same radar instrument that comprised the Spaceborne Imaging Radar-C/X-Band Synthetic Aperture Radar (SIR-C/X-SAR) that flew twice on the Space Shuttle Endeavour in 1994. SRTM was designed to collect three-dimensional measurements of the Earth's surface. To collect the 3-D data, engineers added a 60-meter-long (200-foot) mast, installed additional C-band and X-band antennas, and improved tracking and navigation devices. The mission is a cooperative project between the National Aeronautics and Space Administration (NASA), the National Imagery and Mapping Agency (NIMA) of the U.S. Department of Defense (DoD), and the German and Italian space agencies. It is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Earth Science Enterprise, Washington, DC. Site name: Miyake-Jima, Japan Size: Scale varies in this perspective image, island has an area of 55 square kilometers (21 square miles). Vertical scale approximately equal to horizontal scale. Center Location: 34.1 deg. North lat., 139.5 deg. East lon. Orientation: perspective view is looking from northeast towards the southwest Original Data Resolution: 30 m Date Acquired: February 20, 2000 Image by NASA/JPL/NIMA
Breakup of the World's Large …
Title Breakup of the World's Largest Iceberg
Description Iceberg B-15A was the largest iceberg in the world (measuring about 11,000 square kilometers) when it broke away from Western Antarctica's Ross Ice Shelf in March 2000. It held that distinction for over three years until splitting into two pieces in early October, 2003. The Multi-angle Imaging SpectroRadiometer (MISR) acquired these views of the new iceberg B-15J (resting against Ross Island) and B-15A (now free to drift into the Southern Ocean) on October 26. Several massive icebergs (including B-15A) had migrated during 2000 and 2001 and ground against Ross Island [ http://www-misr.jpl.nasa.gov/gallery/galhistory/2002_jan_02.html ], forming a barrier that influenced wind and current patterns and altered the regional ecology. The two images provide information on both the spectral and angular reflectance properties of ice types in the region. The left-hand panel is a false-color view from MISR's vertical-viewing (nadir) camera in which near-infrared, red and blue spectral data are displayed as red, green, and blue, respectively. Because of the tendency of water to absorb near-infrared wavelengths, some ice types exhibit an especially bright blue hue in this display. The right-hand panel is a multi-angular composite from three MISR cameras, in which color acts as a proxy for angular reflectance variations related to texture. Here, data from the red-band of MISR's 60 degree forward-viewing, nadir, and 60 degree backward-viewing cameras are displayed as red, green, and blue, respectively. In the southern latitudes, MISR's backward-pointing cameras receive a stronger signal from surfaces that predominantly forward scatter sunlight (these tend to be smooth surfaces), and MISR's forward-pointing cameras receive a stronger signal from surfaces that predominantly backscatter sunlight (these tend to be rougher surfaces). Thus, the colors in this representation highlight textural properties of elements within the scene, with blue tones indicating smoother surfaces and red/orange hues indicating rougher surfaces. The Multi-angle Imaging SpectroRadiometer observes the daylit Earth continuously and every 9 days views the entire Earth between 82 degrees north and 82 degrees south latitude. The MISR Browse Image Viewer [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://eosweb.larc.nasa.gov/MISRBR/ ] provides access to low-resolution true-color versions of these images. These data products were generated from a portion of the imagery acquired during Terra orbit 20511. The panels cover an area of 129 kilometers x 221 kilometers, and utilize data from blocks 153 to 155 within World Reference System-2 path 56. Image courtesy NASA/GSFC/LaRC/JPL, MISR Team [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://www-misr.jpl.nasa.gov/ ]. Text by Clare Averill (Raytheon/JPL).
Breakup of the World's Large …
Title Breakup of the World's Largest Iceberg
Description Iceberg B-15A was the largest iceberg in the world (measuring about 11,000 square kilometers) when it broke away from Western Antarctica's Ross Ice Shelf in March 2000. It held that distinction for over three years until splitting into two pieces in early October, 2003. The Multi-angle Imaging SpectroRadiometer (MISR) acquired these views of the new iceberg B-15J (resting against Ross Island) and B-15A (now free to drift into the Southern Ocean) on October 26. Several massive icebergs (including B-15A) had migrated during 2000 and 2001 and ground against Ross Island [ http://www-misr.jpl.nasa.gov/gallery/galhistory/2002_jan_02.html ], forming a barrier that influenced wind and current patterns and altered the regional ecology. The two images provide information on both the spectral and angular reflectance properties of ice types in the region. The left-hand panel is a false-color view from MISR's vertical-viewing (nadir) camera in which near-infrared, red and blue spectral data are displayed as red, green, and blue, respectively. Because of the tendency of water to absorb near-infrared wavelengths, some ice types exhibit an especially bright blue hue in this display. The right-hand panel is a multi-angular composite from three MISR cameras, in which color acts as a proxy for angular reflectance variations related to texture. Here, data from the red-band of MISR's 60 degree forward-viewing, nadir, and 60 degree backward-viewing cameras are displayed as red, green, and blue, respectively. In the southern latitudes, MISR's backward-pointing cameras receive a stronger signal from surfaces that predominantly forward scatter sunlight (these tend to be smooth surfaces), and MISR's forward-pointing cameras receive a stronger signal from surfaces that predominantly backscatter sunlight (these tend to be rougher surfaces). Thus, the colors in this representation highlight textural properties of elements within the scene, with blue tones indicating smoother surfaces and red/orange hues indicating rougher surfaces. The Multi-angle Imaging SpectroRadiometer observes the daylit Earth continuously and every 9 days views the entire Earth between 82 degrees north and 82 degrees south latitude. The MISR Browse Image Viewer [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://eosweb.larc.nasa.gov/MISRBR/ ] provides access to low-resolution true-color versions of these images. These data products were generated from a portion of the imagery acquired during Terra orbit 20511. The panels cover an area of 129 kilometers x 221 kilometers, and utilize data from blocks 153 to 155 within World Reference System-2 path 56. Image courtesy NASA/GSFC/LaRC/JPL, MISR Team [ http://earthobservatory.nasa.gov/cgi-bin/redirect?http://www-misr.jpl.nasa.gov/ ]. Text by Clare Averill (Raytheon/JPL).
Central Pyrenees
Title Central Pyrenees
Description The Alps may be more famous, but the Pyrenees have been around much longer—tens of millions of years longer, in fact. These mountains formed between 100 and 150 million years ago when the landmass that Spain occupies pushed into the one that France occupies. The mountains have served as a natural barrier between the Iberian Peninsula (Spain and Portugal) and the rest of Europe ever since. Stretching east to west across 430 square kilometers (267 miles), the Pyrenees fall mostly within Spain's borders, but also pass into the independent state of Andorra. The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) [ http://asterweb.jpl.nasa.gov ] on NASA 's Terra [ http://terra.nasa.gov ] satellite captured this image of part of the Central Pyrenees—the highest part of the range—on August 1, 2000. In this false-color image, clouds appear white, snow appears pale blue, vegetation appears green, and bare ground appears as either pink or dark, bluish-purple. Water on the ground appears dark blue (or nearly black). In this shot, the vegetated areas are mostly to the north, and the peaks to the south are mostly bare rock. In the large image, patches of dark purple that are visible along rivers and in valley floors are probably developed areas. As mountain peaks rise higher, the land they support rises above the treeline (the topmost elevation where trees can grow). At even higher altitudes, hardly any plants can survive at all, so the highest mountain peaks show just snow or bare rock. This mountain chain owes its ruggedness to granite, a volcanic rock that erodes slowly. The mountains also contain other rocks: gneiss and limestone. Glaciers didn't act on the Pyrenees as extensively as they did on the Alps, so these mountains don't sport big lakes left behind by glaciers. They do have water, however, including many small lakes and waterfalls. NASA image created by Jesse Allen, Earth Observatory, using ASTER data made available by NASA/GSFC/MITI/ERSDAC/JAROS, and U.S./Japan ASTER Science Team. [ http://asterweb.jpl.nasa.gov/ ]
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