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More Los Angeles Fire Images
Triple-digit temperatures, e
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9/1/09
| Description |
Triple-digit temperatures, extremely low relative humidities, dense vegetation that has not burned in decades, and years of extended drought are all contributing to the explosive growth of wildfires throughout Southern California. The Station fire, which began Aug. 26, 2009, in La Canada/Flintridge, not far from NASA's Jet Propulsion Laboratory, had reportedly burned 105,000 acres (164 square miles) of the Angeles National Forest by mid-day Aug. 31, destroying at least 21 homes and threatening more than 12,000 others. It is one of four major fires burning in Southern California at the present time. This image was acquired mid-morning on Aug. 30 by the backward (northward)-viewing camera of the Multi-angle Imaging SpectroRadiometer (MISR) instrument on NASA's Terra satellite. The image is shown in an approximate perspective view at an angle of 46 degrees off of vertical. The area covered by the image is 245 kilometers (152 miles) wide. Several pyrocumulus clouds, created by the Station Fire, are visible above the smoke plumes rising from the San Gabriel Mountains north of Los Angeles in the left-center of the image. Smoke from the Station fire is seen covering the interior valleys along the south side of the San Gabriel Mountains, along with parts of the City of Los Angeles and Orange County, and can be seen drifting for hundreds of kilometers to the east over the Mojave Desert. The accompanying plots are histograms that display the heights of the smoke plumes and wind speeds. In this data set, the plume is injecting smoke more than 7 kilometers (4.3 miles) above sea level. MISR observes the daylit Earth continuously and every 9 days views the entire globe between 82 degrees north and 82 degrees south latitude. This image was generated from a portion of the imagery acquired during Terra orbit 51601. MISR was built and is managed by NASA's Jet Propulsion Laboratory, Pasadena, Calif., for NASA's Science Mission Directorate, Washington, DC. The Terra satellite is managed by NASA's Goddard Space Flight Center, Greenbelt, Md. The MISR data were obtained from the NASA Langley Research Center Atmospheric Science Data Center. JPL is a division of the California Institute of Technology. Image Credit: NASA/GSFC/LaRC/JPL, MISR Team |
| Date |
9/1/09 |
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LOS ALAMOS FIRE IMAGED BY NA
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The fire that has raged out
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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. |
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POLAR STRATOSPHERIC CLOUDS
Polar stratospheric clouds o
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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. |
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HIGH ALTITUDE BALLOON/ARCTIC
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A NASA high-altitude researc
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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. |
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OZONE INSTRUMENTS LOADED ON
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Scientists preparing their i
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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. |
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ER-2 USED IN ARCTIC OZONE RE
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The NASA ER-2 high-altitude
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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. |
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Nicaraguan Volcanoes The tru
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| Description |
Nicaraguan Volcanoes The true-color image at left is a downward-looking (nadir) view of the area around the San Cristobal volcano, which erupted the previous day. This image is oriented with east at the top and north at the left. The right image is a stereo anaglyph of the same area, created from red band multi-angle data taken by the 45.6-degree aftward and 70.5-degree aftward cameras on the Multi- angle Imaging SpectroRadiometer (MISR) instrument on NASA's Terra satellite. View this image through red/blue 3D glasses, with the red filter over the left eye. A plume from San Cristobal (approximately at image center) is much easier to see in the anaglyph, due to 3 effects: the long viewing path through the atmosphere at the oblique angles, the reduced reflection from the underlying water, and the 3D stereoscopic height separation. In this image, the plume floats between the surface and the overlying cumulus clouds. A second plume is also visible in the upper right (southeast of San Cristobal). This very thin plume may originate from the Masaya volcano, which is continually degassing at a slow rate. The spatial resolution is 275 meters (300 yards). MISR was built and is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Office of Earth Science, Washington, DC. The Terra satellite is managed by NASA's Goddard Space Flight Center, Greenbelt, MD. JPL is a division of the California Institute of Technology. ##### |
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Multi-Angle Views of the App
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| Description |
Multi-Angle Views of the Appalachian Mountains The true-color image at left is a downward-looking (nadir) view of the eastern United States, stretching from Lake Ontario to northern Georgia, and spanning the Appalachian Mountains. The three images to the right are also in true-color, taken by the forward 45.6-degree, 60.0-degree, and 70.5-degree cameras, respectively, of the Multi-angle Imaging SpectroRadiometer (MISR) instrument on NASA's Terra satellite. As the slant angle increases, the line- of-sight through the atmosphere grows longer, and a pall of haze over the Appalachians becomes progressively more apparent. You can see a similar effect by scanning from near-nadir to the horizon when standing on a mountain top or looking out an airplane window. MISR uses this multi-angle technique to monitor particulate pollution and to distinguish different types of haze. These observations reveal how airborne particles are interacting with sunlight, a measure of their impact on Earth's climate system. The images are about 400 km (250 miles) wide, and the spatial resolution is 1.1 kilometers (1,200 yards). North is toward the top. MISR was built and is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Office of Earth Science, Washington, DC. The Terra satellite is managed by NASA's Goddard Space Flight Center, Greenbelt, MD. JPL is a division of the California Institute of Technology. ##### |
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Multi-Angle View of the Cana
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A multi-angle view of the Ca
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| Description |
A multi-angle view of the Canary Islands in a dust storm, 29 February 2000. At left is a true-color image taken by the Multi-angle Imaging SpectroRadiometer (MISR) instrument on NASA's Terra satellite. This image was captured by the MISR camera looking at a 70.5-degree angle to the surface, ahead of the spacecraft. The middle image was taken by the MISR downward- looking (nadir) camera, and the right image is from the aftward 70.5-degree camera. The images are reproduced using the same radiometric scale, so variations in brightness, color, and contrast represent true variations in surface and atmospheric reflectance with angle. Windblown dust from the Sahara Desert is apparent in all three images, and is much brighter in the oblique views. This illustrates how MISR's oblique imaging capability makes the instrument a sensitive detector of dust and other particles in the atmosphere. Data for all channels are presented in a Space Oblique Mercator map projection to facilitate their co-registration. The images are about 400 km (250 miles) wide, with a spatial resolution of about 1.1 kilometers (1,200 yards). North is toward the top. MISR was built and is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Office of Earth Science, Washington, DC. The Terra satellite is managed by NASA's Goddard Space Flight Center, Greenbelt, MD. JPL is a division of the California Institute of Technology. ##### |
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Multi-angle Images of Hudson
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At left is a true-color imag
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| Description |
At left is a true-color image from the downward-looking (nadir) camera on the Multi-angle Imaging SpectroRadiometer (MISR) instrument on NASA's Terra satellite. The false-color image at right is a composite of red band data taken by the MISR forward 45.6-degree, nadir, and aftward 45.6-degree cameras, displayed in blue, green, and red colors, respectively. Color variations in the left image highlight spectral (true-color) differences, whereas those in the right image highlight differences in angular reflectance properties. The purple areas in the right image are low cloud, and light blue at the edge of the bay is due to increased forward scattering by the fast (smooth) ice. The orange areas are rougher ice, which scatters more light in the backward direction. This example illustrates how multi-angle viewing can distinguish physical structures and textures. Data for all channels are presented in a Space Oblique Mercator map projection to facilitate their co- registration. The images are about 400 km (250 miles) wide with a spatial resolution of about 275 meters (300 yards). North is toward the top. MISR was built and is managed by NASA's Jet Propulsion Laboratory, Pasadena, CA, for NASA's Office of Earth Science, Washington, DC. The Terra satellite is managed by NASA's Goddard Space Flight Center, Greenbelt, MD. JPL is a division of the California Institute of Technology. ##### |
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Pine Island Glacier, Antarct
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These two images of Pine Isl
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4/3/01
| Date |
4/3/01 |
| Description |
These two images of Pine Island Glacier in Antarctica show the recently discovered 25-kilometer (15-mile) long crack that scientists expect will turn into a large iceberg within the next 18 months. The views from NASA's Multi-angle Imaging SpectroRadiometer (MISR) on the Terra satellite also reveal differences in the ice sheet's surface texture, highlighting surface fractures and enabling distinction of rough crevasses from smooth blue ice. The image data shown was acquired on December 12, 2000, during Terra orbit 5246. At left is a conventional, true-color image from the downward-looking (nadir) camera. The false-color image at right is a composite of red-band data taken by the MISR forward 60-degree, nadir, and aftward 60-degree cameras, displayed in red, green and blue, respectively. Color variations in the true-color image at left highlight spectral differences. In the multi-angle composite, on the other hand, color variations act as a proxy for differences in the angular reflectance properties of the scene. In this representation, clouds show up as light purple. Blue to orange gradations on the surface indicate a transition in ice texture from smooth to rough. For example, the bright orange carrot-like features are rough crevasses on the glacier's tongue. In the conventional nadir view, the blue ice labeled "rough crevasses"' and "smooth blue ice" are similarly colored, but the multi-angle composite reveals their different textures, with the smoother ice appearing dark purple instead of orange. This could be an indicator of different mechanisms by which this ice is exposed. The multi-angle view also reveals subtle roughness variations on the frozen sea ice between the glacier and the open water in Pine Island Bay. To the left of the 'icebergs' label are chunks of floating ice. Smaller icebergs embedded in the frozen sea ice are visible below and to the right of the label. These small icebergs are associated with dark streaks. Analysis of the illumination geometry suggests that these streaks are surface features, not shadows. Wind-driven motion and thinning of the sea ice in the vicinity of the icebergs are a possible explanation. Recently, Robert Bindschadler, a glaciologist at the NASA Goddard Space Flight Center discovered in Landsat 7 imagery a newly-formed crack traversing the Pine Island Glacier. This crack is visible as an off-vertical dark line in the MISR nadir view. In the multi-angle composite, the crack and other stress fractures show up very clearly in bright orange. Radar observations of Pine Island Glacier in the 1990's showed the glacier to be shrinking, and the newly discovered crack is expected to eventually lead to the calving of a major iceberg. MISR was built and is managed by NASA's Jet Propulsion Laboratory, Pasadena, Calf., for NASA's Office of Earth Science, Washington, D.C. The Terra satellite is managed by NASA's Goddard Space Flight Center, Greenbelt, Md. JPL is a division of the California Institute of Technology. Image credit: NASA/JPL/GSFC/LaRC, MISR Team ##### |
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Splendid Splinter
| Title |
Splendid Splinter |
| Description |
The spiral galaxy NGC 5907, sometimes known as the "Splinter Galaxy" because of its unusual appearance, is located in the constellation Draco. It is fairly bright, and appears elongated because it has an edge-on alignment when viewed from Earth. It also has a strong set of dust lanes, visible in this image from NASA's Spitzer Space Telescope as red features. The central lane is so pronounced at visible light wavelengths, where it blocks our view of the starlight, that the galaxy was once mistaken for two objects and given two entries in the original New General Catalogue. The catalogue, published by J.L.E. Dreyer in 1888, was an attempt to collect a complete list of all nebulae and star clusters known at the time. NGC 5907's special orientation and close proximity to Earth have made it a popular target for observation by both professional and amateur astronomers. Over the last decade, ever-improving infrared instrumentation have allowed scientists to detect light from the galaxy that was until now hidden by dust. Recent observations using Spitzer's InfraRed Array Camera at infrared wavelengths from 3-10 microns resulted in the discovery of a significant and potentially massive thick stellar disk. This is the first time that a thick disk has been detected and characterized in the infrared. This image is composed of images obtained at four wavelengths: 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8 microns (red). The contribution from starlight has been subtracted from the 5.8 and 8 micron images to enhance the visibility of the dust features. |
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A Cauldron of Stars at the G
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| 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. |
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A Cauldron of Stars at the G
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| 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. |
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The Milky Way Center Aglow w
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| 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. |
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The Milky Way Center Aglow w
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| 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. |
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Galactic Fossil Revealed in
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| Title |
Galactic Fossil Revealed in Infrared Light |
| Description |
This animation demonstrates the power of infrared light to see what visible light cannot -- a newfound bundle of stars called a globular cluster. The movie shifts from a visible-light image to a near-infrared image to a new mid-infrared image from NASA's Spitzer Space Telescope. The visible-light image is from the California Institute of Technology's Digitized Sky Survey and the near-infrared image is from the NASA-funded Two Micron All-Sky Survey (2MASS). Globular clusters date back to the birth of our galaxy, 13 or so billion years ago. There are about 150 clusters sprinkled around the core of the galaxy like seeds in a pumpkin. Astronomers use these galactic "fossils" as tools for studying the age and formation of the Milky Way. Most clusters orbit around the center of the galaxy well above its dust-enshrouded disc, or plane, while making brief, repeated passes through the plane that each last about a million years. Spitzer, with infrared eyes that can see into the dusty galactic plane, first spotted the newfound cluster during its current pass. Astronomers then searched for past references to the cluster and found only one undocumented image from the Two Micron All-Sky Survey. Follow-up observations with the University of Wyoming Infrared Observatory helped set the distance of the new cluster at about 9,000 light-years from Earth -- closer than most clusters -- and set the mass at the equivalent of 300,000 Suns. The cluster's apparent size, as viewed from Earth, is comparable to a grain of rice held at arm's length. It is located in the constellation Aquila. Astronomers believe that this cluster may be one of the last in our galaxy to be uncovered. The Two Micron All-Sky Survey false-color image was obtained using near-infrared wavelengths ranging from 1.3 to 2.2 microns. The Spitzer false-color image composite was taken on April 21, 2004, by its infrared array camera. It is composed of images obtained at four mid-infrared wavelengths: 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8 microns (red). The true-color image from the Digitized Sky Survey was acquired with red and blue filters. |
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Spitzer Digs Up Galactic Fos
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| Title |
Spitzer Digs Up Galactic Fossil |
| Description |
This false-color image taken by NASA's Spitzer Space Telescope shows a globular cluster previously hidden in the dusty plane of our Milky Way galaxy. Globular clusters are compact bundles of old stars that date back to the birth of our galaxy, 13 or so billion years ago. Astronomers use these galactic "fossils" as tools for studying the age and formation of the Milky Way. Most clusters orbit around the center of the galaxy well above its dust-enshrouded disc, or plane, while making brief, repeated passes through the plane that each last about a million years. Spitzer, with infrared eyes that can see into the dusty galactic plane, first spotted the newfound cluster during its current pass. A visible-light image (inset) shows only a dark patch of sky. The red streak behind the core of the cluster is a dust cloud, which may indicate the cluster's interaction with the Milky Way. Alternatively, this cloud may lie coincidentally along Spitzer's line of sight. Follow-up observations with the University of Wyoming Infrared Observatory helped set the distance of the new cluster at about 9,000 light-years from Earth -- closer than most clusters -- and set the mass at the equivalent of 300,000 Suns. The cluster's apparent size, as viewed from Earth, is comparable to a grain of rice held at arm's length. It is located in the constellation Aquila. Astronomers believe that this cluster may be one of the last in our galaxy to be uncovered. This image composite was taken on April 21, 2004, by Spitzer's infrared array camera. It is composed of images obtained at four wavelengths: 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8 microns (red). The visible-light image is from the Digitized Sky Survey, California University of Technology, Pasadena, Calif. |
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Spitzer Digs Up Galactic Fos
…
| Title |
Spitzer Digs Up Galactic Fossil |
| Description |
This false-color image taken by NASA's Spitzer Space Telescope shows a globular cluster previously hidden in the dusty plane of our Milky Way galaxy. Globular clusters are compact bundles of old stars that date back to the birth of our galaxy, 13 or so billion years ago. Astronomers use these galactic "fossils" as tools for studying the age and formation of the Milky Way. Most clusters orbit around the center of the galaxy well above its dust-enshrouded disc, or plane, while making brief, repeated passes through the plane that each last about a million years. Spitzer, with infrared eyes that can see into the dusty galactic plane, first spotted the newfound cluster during its current pass. A visible-light image (inset) shows only a dark patch of sky. The red streak behind the core of the cluster is a dust cloud, which may indicate the cluster's interaction with the Milky Way. Alternatively, this cloud may lie coincidentally along Spitzer's line of sight. Follow-up observations with the University of Wyoming Infrared Observatory helped set the distance of the new cluster at about 9,000 light-years from Earth -- closer than most clusters -- and set the mass at the equivalent of 300,000 Suns. The cluster's apparent size, as viewed from Earth, is comparable to a grain of rice held at arm's length. It is located in the constellation Aquila. Astronomers believe that this cluster may be one of the last in our galaxy to be uncovered. This image composite was taken on April 21, 2004, by Spitzer's infrared array camera. It is composed of images obtained at four wavelengths: 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8 microns (red). The visible-light image is from the Digitized Sky Survey, California University of Technology, Pasadena, Calif. |
|
Spitzer Digs Up Galactic Fos
…
| Title |
Spitzer Digs Up Galactic Fossil |
| Description |
This false-color image taken by NASA's Spitzer Space Telescope shows a globular cluster previously hidden in the dusty plane of our Milky Way galaxy. Globular clusters are compact bundles of old stars that date back to the birth of our galaxy, 13 or so billion years ago. Astronomers use these galactic "fossils" as tools for studying the age and formation of the Milky Way. Most clusters orbit around the center of the galaxy well above its dust-enshrouded disc, or plane, while making brief, repeated passes through the plane that each last about a million years. Spitzer, with infrared eyes that can see into the dusty galactic plane, first spotted the newfound cluster during its current pass. A visible-light image (inset) shows only a dark patch of sky. The red streak behind the core of the cluster is a dust cloud, which may indicate the cluster's interaction with the Milky Way. Alternatively, this cloud may lie coincidentally along Spitzer's line of sight. Follow-up observations with the University of Wyoming Infrared Observatory helped set the distance of the new cluster at about 9,000 light-years from Earth -- closer than most clusters -- and set the mass at the equivalent of 300,000 Suns. The cluster's apparent size, as viewed from Earth, is comparable to a grain of rice held at arm's length. It is located in the constellation Aquila. Astronomers believe that this cluster may be one of the last in our galaxy to be uncovered. This image composite was taken on April 21, 2004, by Spitzer's infrared array camera. It is composed of images obtained at four wavelengths: 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8 microns (red). The visible-light image is from the Digitized Sky Survey, California University of Technology, Pasadena, Calif. |
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Galactic Fossil Found Behind
…
| Title |
Galactic Fossil Found Behind Curtain of Dust |
| Description |
This image mosaic shows the same patch of sky in various wavelengths of light. While the visible-light image (left) shows a dark sky speckled with stars, infrared images (middle and right), reveal a never-before-seen bundle of stars, called a globular cluster. The left panel is from the California Institute of Technology's Digitized Sky Survey, the middle panel includes images from the NASA-funded Two Micron All-Sky Survey and the University of Wyoming Infrared Observatory (circle inset), and the right panel is from NASA's Spitzer Space Telescope. Globular clusters date back to the birth of our galaxy, 13 or so billion years ago. There are about 150 clusters sprinkled around the core of the galaxy like seeds in a pumpkin. Astronomers use these galactic "fossils" as tools for studying the age and formation of the Milky Way. Most clusters orbit around the center of the galaxy well above its dust-enshrouded disc, or plane, while making brief, repeated passes through the plane that each last about a million years. Spitzer, with infrared eyes that can see into the dusty galactic plane, first spotted the newfound cluster during its current pass. Astronomers then searched for past references to the cluster and found only one undocumented image from the Two Micron All-Sky Survey. Follow-up observations with the University of Wyoming Infrared Observatory helped set the distance of the new cluster at about 9,000 light-years from Earth -- closer than most clusters -- and set the mass at the equivalent of 300,000 Suns. The cluster's apparent size, as viewed from Earth, is comparable to a grain of rice held at arm's length. It is located in the constellation Aquila. Astronomers believe that this cluster may be one of the last in our galaxy to be uncovered. The Two Micron All-Sky Survey false-color image was obtained using near-infrared wavelengths ranging from 1.3 to 2.2 microns. The University of Wyoming Observatory false-color image was captured on July 31, 2004, at wavelengths ranging from 1.2 to 2.2 microns. The Spitzer false-color image composite was taken on April 21, 2004, by its infrared array camera. It is composed of images obtained at four mid-infrared wavelengths: 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8 microns (red). |
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Titan Sea and Lake Superior
| Description |
Titan Sea and Lake Superior |
| Full Description |
This side-by-side image shows a Cassini radar image (on the left) of what is the largest body of liquid ever found on Titan's north pole, compared to Lake Superior (on the right). This close-up is part of a larger image (see Titan (T25) Viewed by Cassini's Radar - Feb. 22, 2007) and offers strong evidence for seas on Titan. These seas are most likely liquid methane and ethane. This feature on Titan is at least 100,000 square kilometers (39,000 square miles), which is greater in extent than Lake Superior (82,000 square kilometers or 32,000 square miles), which is one of Earth's largest lakes. The feature covers a greater fraction of Titan than the largest terrestrial inland sea, the Black Sea. The Black Sea covers 0.085 percent of the surface of the Earth, this newly observed body on Titan covers at least 0.12 percent of the surface of Titan. Because of its size, scientists are calling it a sea. The image on the right is from the SeaWiFS project, NASA's Goddard Space Flight Center, Greenbelt, Md. 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 radar instrument was built by JPL and the Italian Space Agency, working with team members from the United States and several European countries. For more information about the Cassini-Huygens mission visit http://saturn.jpl.nasa.gov/home/index.cfm. *Credit:* NASA/JPL/GSFC |
| Date |
March 13, 2007 |
|
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 |
|
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 |
|
Enceladus Temperature Map
| Description |
Enceladus Temperature Map |
| Full Description |
This image shows the surprise that startled Cassini scientists on the composite infrared spectrometer team when they got their first look at the infrared (heat) radiation from the south pole of Saturn's moon Enceladus. There is a dramatic warm spot centered on the pole that is probably a sign of internal heat leaking out of the icy moon. The data were taken during the spacecraft's third flyby of this intriguing moon on July 14, 2005. Based on data from previous flybys, which did not show the south pole well, team members expected that the south pole would be very cold, as shown in the left panel. Enceladus is one of the coldest places in the Saturn system because its extremely bright surface reflects 80 percent of the sunlight that hits it, so only 20 percent is available to heat the surface. As on Earth, the poles should be even colder than the equator because the sun shines at such an oblique angle there. The right hand panel shows a global temperature image made from measurements of Enceladus' heat radiation at wavelengths between 9 and 16.5 microns. Cassini made the observation from a distance of 84,000 kilometers (52,000 miles) on the approach to Enceladus, and the image shows details as small as 25 kilometers (16 miles). Equatorial temperatures are much as expected, topping out at about 80 degrees Kelvin (-315 degrees Fahrenheit), but the south pole is occupied by a well-defined warm region reaching 85 Kelvin (-305 degrees Fahrenheit). That is 15 degrees Kelvin (27 degrees Fahrenheit) warmer than expected. The composite infrared spectrometer data further suggest that small areas of the pole are at even higher temperatures, well over 110 degrees Kelvin (-261 degrees Fahrenheit). Evaporation of this relatively warm ice probably generates the cloud of water vapor detected above Enceladus' south pole by several other Cassini instruments. The south polar temperatures are very difficult to explain if sunlight is the only energy source heating the surface, though exotic sunlight-trapping mechanisms have not yet been completely ruled out. It therefore seems likely that portions of the polar region are warmed by heat escaping from the interior of the moon. This would make Enceladus only the third solid body in the solar system, after Earth and Jupiter's volcanic moon Io, where hot spots powered by internal heat have been detected. 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. 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/ . Credit: NASA/JPL/GSFC |
| Date |
July 29, 2005 |
|
Phoebe Temperature Maps
| Description |
Phoebe Temperature Maps |
| Full Description |
A montage of maps of Saturn's moon Phoebe shows surface temperatures at various times of day as determined by the composite infrared spectrometer onboard Cassini during the June 11, 2004, Phoebe flyby. The asterisk on each map shows the location of the subsolar point, where the Sun is directly overhead. This point moves across the surface as Phoebe rotates. It is morning in regions to the left of the subsolar point, and afternoon in regions to the right. Like a newspaper weather map, different colors indicate different temperatures, though Phoebe's temperatures are distinctly cooler than even the coldest January day on Earth. Equatorial temperatures peak in the early afternoon near 112 Kelvin (-257 Fahrenheit), plunging to 78 Kelvin (-319 Fahrenheit) before dawn, and are even colder at higher latitudes. The large day/night temperature contrasts imply that Phoebe's surface is covered in loose dust or ice particles that store little heat and thus cool off rapidly at night. Regions of Phoebe's surface that were not observed are shown in black. Most of the maps show the effect on surface temperatures of the large crater-like depression seen in Cassini's visible-wavelength images of Phoebe, which is located just left of center in these maps. Crater walls that are shadowed and cold in the early morning in the first map are sunlit and warm in the late afternoon in the final map. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini-Huygens mission for NASA's Office of Space Science, Washington, D.C. The 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. For more information about the Cassini-Huygens mission, visit http://saturn.jpl.nasa.gov and the Cassini composite infrared spectrometer home page at http://cirs.gsfc.nasa.gov/ . Image Credit: NASA/JPL/Goddard Space Flight Center |
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Home Reef Reborn
| title |
Home Reef Reborn |
| description |
In the South Pacific, south of Late Island along the Tofua volcanic arc in Tonga, the volcanic island Home Reef is being re-born. The island is thought to have emerged after a volcanic eruption in mid-August that also spewed large amounts of floating pumice into Tongan waters and swept across to Fiji about 350 km (220 miles) to the west of where the new island formed. In 2004, a similar eruption created an ephemeral island about 0.5 by 1.5 km (0.3 by 0.9 miles) in size, it was no longer visible in an ASTER image acquired November 2005. This simulated natural color image shows the vegetation-covered stratovolcanic island of Late Island in the upper right. Home Reef is found in the lower left. The two bluish plumes are hot seawater that is laden with volcanic ash and chemicals, the larger one can be traced for more than 14 km (8.4 miles) to the east. The image was acquired Oct. 10, 2006 and covers an area of 24.3 by 30.2 km. It is located at 18.9 degrees south latitude, 174.7 degrees west longitude. With its 14 spectral bands from the visible to the thermal infrared wavelength region, and its high spatial resolution of 15 to 90 meters (about 50 to 300 feet), ASTER images Earth to map and monitors the changing surface of our planet. It is one of five Earth-observing instruments launched Dec. 18, 1999, on NASA's Terra satellite. The instrument was built by Japan's Ministry of Economy, Trade and Industry. A joint U.S./Japan science team is responsible for validation and calibration of the instrument and the data products. Image credit: NASA/GSFC/METI/ERSDAC/JAROS and U.S./Japan ASTER Science Team |
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COBE's View of the Milky Way
| title |
COBE's View of the Milky Way |
| date |
01.01.1990 |
| description |
From its orbit around Earth, the Goddard Space Flight Center's Cosmic Background Explorer (COBE) captured this edge-on view of our Milky Way galaxy in infrared light, a form of radiation that humans cannot see but can feel in the form of heat, as part of its mission to test the "Big Bang" theory of the creation of the universe. The theory, first proposed in 1927 by Belgian cosmologist Georges Lematre, holds that the universe began as an incredibly dense "primeval atom" that exploded with tremendous force, unleashing matter and space at the speeds of light. NASA set out to prove the theory with the help of COBE. In addition to proving the Big Bang, the satellite discovered that the cosmic background radiation had indeed been produced in the Big Bang just as scientists originally speculated. The satellite's data even discovered the primordial temperature and density fluctuations that eventually gave rise to the Milky Way and other large-scale objects found in space today. *Image Credit*: NASA |
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Hubble Follows Rapid Changes
…
| Title |
Hubble Follows Rapid Changes in Jupiter's Aurora |
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Spitzer and Hubble Capture E
…
| Title |
Spitzer and Hubble Capture Evolving Planetary Systems |
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Spitzer and Hubble Capture E
…
| Title |
Spitzer and Hubble Capture Evolving Planetary Systems |
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Spitzer and Hubble Capture E
…
| Title |
Spitzer and Hubble Capture Evolving Planetary Systems |
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Spitzer and Hubble Capture E
…
| Title |
Spitzer and Hubble Capture Evolving Planetary Systems |
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Earth Rotation from Galileo
…
| Title |
Earth Rotation from Galileo Imagery: 3600 x Real-Time (no rotation) |
| Abstract |
This animation is one in a series created to show an accurate representation of the Earth's rotation at different temporal resolutions. The animation is created from images taken by the Galileo spacecraft during a close pass of the Earth on December 11-12, 1990. The animations range from real-time, in which no rotation can be perceived, to 3600 times real-time, in which both the Earth's rotation and cloud motion can bee seen. The series also includes an animation in which the Earth's rotation has been 'halted' so that cloud motion is easier to see and an animation showing the specific amount of rotation that takes place in three minutes. |
| Completed |
1998-08-23 |
|
Earth Rotation from Galileo
…
| Title |
Earth Rotation from Galileo Imagery: 3600 x Real-Time (no rotation) |
| Abstract |
This animation is one in a series created to show an accurate representation of the Earth's rotation at different temporal resolutions. The animation is created from images taken by the Galileo spacecraft during a close pass of the Earth on December 11-12, 1990. The animations range from real-time, in which no rotation can be perceived, to 3600 times real-time, in which both the Earth's rotation and cloud motion can bee seen. The series also includes an animation in which the Earth's rotation has been 'halted' so that cloud motion is easier to see and an animation showing the specific amount of rotation that takes place in three minutes. |
| Completed |
1998-08-23 |
|
Aura/OMI Ozone Hole from Sep
…
| Title |
Aura/OMI Ozone Hole from September 12, 2004 to November 15, 2004 with Polar Vortex Demarced |
| Abstract |
Data from NASA satellites establishes a 40-year record of stratospheric ozone measurements. The stratospheric ozone layer shields life on Earth from harmful solar ultraviolet (UV) radiation. Research shows that excess exposure to UV radiation causes skin cancer and eye problems and impacts plant growth. Global stratospheric ozone has decreased by 3 percent globally between 1980 and 2000 and has thinned by 50 percent over Antarctica in winter and spring. Depletion of the ozone layer allows more UV radiation to reach the Earth's surface. This animation shows the ozone layer blocking harmful UV radiation from the Earth's surface. The hole in the ozone is seen in purple. The location, size, and shape of the polar vortex is derived from potential vorticity data, PV. The PV, shown in white at 550 degrees Kelvin, is an atmospheric regional event that isolates polar air from the air at lower latitudes, producing conditions favorable for wintertime polar ozone depletion. The animation shows that most of the low-temperature and chemically-perturbed region is confined within the polar vortex during the Antarctic winter. |
| Completed |
2004-11-30 |
|
Aura/OMI Ozone Hole from Sep
…
| Title |
Aura/OMI Ozone Hole from September 12, 2004 to November 15, 2004 with Polar Vortex Demarced |
| Abstract |
Data from NASA satellites establishes a 40-year record of stratospheric ozone measurements. The stratospheric ozone layer shields life on Earth from harmful solar ultraviolet (UV) radiation. Research shows that excess exposure to UV radiation causes skin cancer and eye problems and impacts plant growth. Global stratospheric ozone has decreased by 3 percent globally between 1980 and 2000 and has thinned by 50 percent over Antarctica in winter and spring. Depletion of the ozone layer allows more UV radiation to reach the Earth's surface. This animation shows the ozone layer blocking harmful UV radiation from the Earth's surface. The hole in the ozone is seen in purple. The location, size, and shape of the polar vortex is derived from potential vorticity data, PV. The PV, shown in white at 550 degrees Kelvin, is an atmospheric regional event that isolates polar air from the air at lower latitudes, producing conditions favorable for wintertime polar ozone depletion. The animation shows that most of the low-temperature and chemically-perturbed region is confined within the polar vortex during the Antarctic winter. |
| Completed |
2004-11-30 |
|
Aura/OMI Ozone Hole from Sep
…
| Title |
Aura/OMI Ozone Hole from September 12, 2004 to November 15, 2004 with Polar Vortex Demarced |
| Abstract |
Data from NASA satellites establishes a 40-year record of stratospheric ozone measurements. The stratospheric ozone layer shields life on Earth from harmful solar ultraviolet (UV) radiation. Research shows that excess exposure to UV radiation causes skin cancer and eye problems and impacts plant growth. Global stratospheric ozone has decreased by 3 percent globally between 1980 and 2000 and has thinned by 50 percent over Antarctica in winter and spring. Depletion of the ozone layer allows more UV radiation to reach the Earth's surface. This animation shows the ozone layer blocking harmful UV radiation from the Earth's surface. The hole in the ozone is seen in purple. The location, size, and shape of the polar vortex is derived from potential vorticity data, PV. The PV, shown in white at 550 degrees Kelvin, is an atmospheric regional event that isolates polar air from the air at lower latitudes, producing conditions favorable for wintertime polar ozone depletion. The animation shows that most of the low-temperature and chemically-perturbed region is confined within the polar vortex during the Antarctic winter. |
| Completed |
2004-11-30 |
|
Earth Rotation from Galileo
…
| Title |
Earth Rotation from Galileo Imagery: 3600 x Real-Time |
| Abstract |
This animation is one in a series created to show an accurate representation of the Earth's rotation at different temporal resolutions. The animation is created from images taken by the Galileo spacecraft during a close pass of the Earth on December 11-12, 1990. The animations range from real-time, in which no rotation can be perceived, to 3600 times real-time, in which both the Earth's rotation and cloud motion can bee seen. The series also includes an animation in which the Earth's rotation has been 'halted' so that cloud motion is easier to see and an animation showing the specific amount of rotation that takes place in three minutes. |
| Completed |
1998-08-23 |
|
Mapping the Amazon: Mosaic t
…
| Title |
Mapping the Amazon: Mosaic tiles animation |
| Abstract |
A satellite can cover the Amazon in just two months. The mapping team chose a Japanese satellite outfitted with synthetic aperture radar, or SAR for short. SAR is a natural fit for the Amazon. It can penetrate the clouds that pour rain for half of the year and the smoke from trees burned by farmers to clear land. SAR even works at night. As you might imagine, the satellite collects a pile of data. In raw form, these observations are gibberish. Focusing them requires a supercomputer to crunch fifteen hundred trillion calculations. The output is rich images of the Amazon. Scientists listed worked as a team on Mosaicking Software and Mosaic Production. |
| Completed |
2000-12-19 |
|
Mapping the Amazon: Mosaic t
…
| Title |
Mapping the Amazon: Mosaic tiles animation |
| Abstract |
A satellite can cover the Amazon in just two months. The mapping team chose a Japanese satellite outfitted with synthetic aperture radar, or SAR for short. SAR is a natural fit for the Amazon. It can penetrate the clouds that pour rain for half of the year and the smoke from trees burned by farmers to clear land. SAR even works at night. As you might imagine, the satellite collects a pile of data. In raw form, these observations are gibberish. Focusing them requires a supercomputer to crunch fifteen hundred trillion calculations. The output is rich images of the Amazon. Scientists listed worked as a team on Mosaicking Software and Mosaic Production. |
| Completed |
2000-12-19 |
|
Mapping the Amazon: Mosaic t
…
| Title |
Mapping the Amazon: Mosaic tiles animation |
| Abstract |
A satellite can cover the Amazon in just two months. The mapping team chose a Japanese satellite outfitted with synthetic aperture radar, or SAR for short. SAR is a natural fit for the Amazon. It can penetrate the clouds that pour rain for half of the year and the smoke from trees burned by farmers to clear land. SAR even works at night. As you might imagine, the satellite collects a pile of data. In raw form, these observations are gibberish. Focusing them requires a supercomputer to crunch fifteen hundred trillion calculations. The output is rich images of the Amazon. Scientists listed worked as a team on Mosaicking Software and Mosaic Production. |
| Completed |
2000-12-19 |
|
North Atlantic Ocean Current
…
| Title |
North Atlantic Ocean Current Velocity |
| Abstract |
Three-dimensional General Circulation Models divide the ocean into a rectangular grid with layered vertical columns. This North Atlantic model uses a 1/6 degree grid with 37 layers. It captured 30 years of velocity, sea-surface temperature, and salinity. The model realistically separates the Gulf Stream from the Florida coast. A feature as small as the Gulf Stream had not appeared in lower-resolution models. |
| Completed |
1999-01-21 |
|
Global SST Model (ECCO)
| Title |
Global SST Model (ECCO) |
| Abstract |
Sea surface temperature plays a vital role in the behavior of the Earth's climate and weather. It is both a causal factor and a resulting effect of complex interactions of natural forces on Earth. NASA not only measures sea surface temperature from space using powerful scientific instruments, but it also studies temperature processes in advanced computer models. -Gretchen Cook-Anderson (GSFC) |
| Completed |
2005-09-02 |
|
Global SST Model (ECCO)
| Title |
Global SST Model (ECCO) |
| Abstract |
Sea surface temperature plays a vital role in the behavior of the Earth's climate and weather. It is both a causal factor and a resulting effect of complex interactions of natural forces on Earth. NASA not only measures sea surface temperature from space using powerful scientific instruments, but it also studies temperature processes in advanced computer models. -Gretchen Cook-Anderson (GSFC) |
| Completed |
2005-09-02 |
|
Global SST Model (ECCO)
| Title |
Global SST Model (ECCO) |
| Abstract |
Sea surface temperature plays a vital role in the behavior of the Earth's climate and weather. It is both a causal factor and a resulting effect of complex interactions of natural forces on Earth. NASA not only measures sea surface temperature from space using powerful scientific instruments, but it also studies temperature processes in advanced computer models. -Gretchen Cook-Anderson (GSFC) |
| Completed |
2005-09-02 |
|
Global SST Model (ECCO)
| Title |
Global SST Model (ECCO) |
| Abstract |
Sea surface temperature plays a vital role in the behavior of the Earth's climate and weather. It is both a causal factor and a resulting effect of complex interactions of natural forces on Earth. NASA not only measures sea surface temperature from space using powerful scientific instruments, but it also studies temperature processes in advanced computer models. -Gretchen Cook-Anderson (GSFC) |
| Completed |
2005-09-02 |
|
Global SST Model (ECCO)
| Title |
Global SST Model (ECCO) |
| Abstract |
Sea surface temperature plays a vital role in the behavior of the Earth's climate and weather. It is both a causal factor and a resulting effect of complex interactions of natural forces on Earth. NASA not only measures sea surface temperature from space using powerful scientific instruments, but it also studies temperature processes in advanced computer models. -Gretchen Cook-Anderson (GSFC) |
| Completed |
2005-09-02 |
|
Mapping the Amazon: Deforest
…
| Title |
Mapping the Amazon: Deforestation |
| Abstract |
One feature that appears in this mosaic of images showing the Amazon River is tree-clearing that happened between two seasons. Scientists listed worked as a team on Mosaicking Software and Mosaic Production. |
| Completed |
2000-12-19 |
|
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