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Images of 'NASA' found, 8,704

 
Titan, Saturn satellite seen by Cassini - Saturn's moon Titan as seen by Cassini spacecraft: Titan images obtained by the Cassini probe on 21 March 2017. On the left, Titan seen in real colors. On the right, infrared image showing surface details as well as clouds in the northern hemisphere. These views were obtained with the Cassini spacecraft narrow-angle camera on March 21, 2017. Images taken using red, green and blue spectral filters were combined to create the natural-color view at left. The false-color view at right was made by substituting an infrared image (centered at 938 nanometers) for the red color channel. A large, bright and feathery band of summer clouds can be seen arcing across high northern latitudes in the view at right. The views were acquired at a distance of approximately 613,000 miles (986,000 kilometers) from Titan. Image scale is about 4 miles (6 kilometers) per pixel

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Titan, Saturn satellite seen by Cassini - Saturn's moon Titan as seen by Cassini spacecraft: Titan images obtained by the Cassini probe on 21 March 2017. On the left, Titan seen in real colors. On the right, infrared image showing surface details as well as clouds in the northern hemisphere. These views were obtained with the Cassini spacecraft narrow-angle camera on March 21, 2017. Images taken using red, green and blue spectral filters were combined to create the natural-color view at left. The false-color view at right was made by substituting an infrared image (centered at 938 nanometers) for the red color channel. A large, bright and feathery band of summer clouds can be seen arcing across high northern latitudes in the view at right. The views were acquired at a distance of approximately 613,000 miles (986,000 kilometers) from Titan. Image scale is about 4 miles (6 kilometers) per pixel

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Saturn seen by the Cassini probe - Saturn seen by Cassini spacecraft: Saturn seen by the Cassini probe on 28 October 2016. Images taken on Oct. 28, 2016 with the wide angle camera using red, green and blue spectral filters were combined to create this color view. This view looks toward the sunlit side of the rings from about 25 degrees above the ringplane. The view was acquired at a distance of approximately 870,000 miles (1.4 million kilometers) from Saturn. Image scale is 50 miles (80 kilometers) per pixel

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Saturn seen by the Cassini probe - Saturn seen by Cassini spacecraft: Saturn seen by the Cassini probe on 28 October 2016. Images taken on Oct. 28, 2016 with the wide angle camera using red, green and blue spectral filters were combined to create this color view. This view looks toward the sunlit side of the rings from about 25 degrees above the ringplane. The view was acquired at a distance of approximately 870,000 miles (1.4 million kilometers) from Saturn. Image scale is 50 miles (80 kilometers) per pixel

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Volcano Arsia Mons - Arsia Mons volcano. - Arsia Mons is one of the largest known volcanoes. It stands more than 9 km above the surrounding plains and its caldera extends for 110 km. Mosaic of infrared images obtained by the Mars Odyssey probe. Arsia Mons is the southernmost of the Tharsis volcanoes. It is 270 miles in diameter, almost 12 miles high, and the summit caldera is 72 miles wide. For comparison, the largest volcano on Earth is Mauna Loa. From its base on the sea floor, Mauna Loa measures only 6.3 miles high and 75 miles in diameter. The image here is a mosaic of several daytime IR images taken by the Mars Odyssey spacecraft

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Volcano Arsia Mons - Arsia Mons volcano. - Arsia Mons is one of the largest known volcanoes. It stands more than 9 km above the surrounding plains and its caldera extends for 110 km. Mosaic of infrared images obtained by the Mars Odyssey probe. Arsia Mons is the southernmost of the Tharsis volcanoes. It is 270 miles in diameter, almost 12 miles high, and the summit caldera is 72 miles wide. For comparison, the largest volcano on Earth is Mauna Loa. From its base on the sea floor, Mauna Loa measures only 6.3 miles high and 75 miles in diameter. The image here is a mosaic of several daytime IR images taken by the Mars Odyssey spacecraft

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March - Opportunity - Cratere Endurance. 05/2004 - Martian crater Endurance seen by Opportunity. 05/2004 - Panorama of 360 degres obtained by Opportunity from 22 to 28 May 2004. The Rover Opportunity landed on Mars in the Meridiani Planum region on January 25, 2004. This 360 - degree panorama shows “” Endurance Crater”” and the surrounding plains of Meridiani Planum on Mars. It took seven sols to complete this panorama (sols 117 - 123), using 81 separate camera positions. The composite shown here is an approximate true - color rendering

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March - Opportunity - Cratere Endurance. 05/2004 - Martian crater Endurance seen by Opportunity. 05/2004 - Panorama of 360 degres obtained by Opportunity from 22 to 28 May 2004. The Rover Opportunity landed on Mars in the Meridiani Planum region on January 25, 2004. This 360 - degree panorama shows “” Endurance Crater”” and the surrounding plains of Meridiani Planum on Mars. It took seven sols to complete this panorama (sols 117 - 123), using 81 separate camera positions. The composite shown here is an approximate true - color rendering

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March: Hills east of Spirit landing site

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March: Hills east of Spirit landing site

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Martian Twilight - Sunset on Mars seen by the Rover Spirit in April 200

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Martian Twilight - Sunset on Mars seen by the Rover Spirit in April 200

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Martian Planisphere - Image based on images obtained by Mars Global Surveyor in 199

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Martian Planisphere - Image based on images obtained by Mars Global Surveyor in 199

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March - Volcanos Ceraunius Tholus and Uranius Tholus - Mars - Volcanos Ceraunius Tholus and Uranius Tholus - Image obtained by the Mars Global Surveyor probe in March 2002. This image shows the volcanoes Ceraunius Tholus (bottom) and Uranius Tholus (top). The presence of impact crateres on these volcanoes indicates that these volcanoes are old. The crater at the top of Ceraunius Tholus is about 25 km in diameter. Acquired in March 2002, this Mars Global Surveyor (MGS) Mars Orbiter Camera wide angle view shows the martian volcanoes, Ceraunius Tholus (lower) and Uranius Tholus (upper). The presence of impact craters on these volcanoes, particularly on Uranius Tholus; indicates that they are quite ancient and are not active today. The light - toned area on the southeastern face (towards lower right) of Ceraunius Tholus is a remnant of a once more extensive deposit of dust from the global dust storm events that occurred in 2001. The crater at the summit of Ceraunius Tholus is about 25 km (

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March - Volcanos Ceraunius Tholus and Uranius Tholus - Mars - Volcanos Ceraunius Tholus and Uranius Tholus - Image obtained by the Mars Global Surveyor probe in March 2002. This image shows the volcanoes Ceraunius Tholus (bottom) and Uranius Tholus (top). The presence of impact crateres on these volcanoes indicates that these volcanoes are old. The crater at the top of Ceraunius Tholus is about 25 km in diameter. Acquired in March 2002, this Mars Global Surveyor (MGS) Mars Orbiter Camera wide angle view shows the martian volcanoes, Ceraunius Tholus (lower) and Uranius Tholus (upper). The presence of impact craters on these volcanoes, particularly on Uranius Tholus; indicates that they are quite ancient and are not active today. The light - toned area on the southeastern face (towards lower right) of Ceraunius Tholus is a remnant of a once more extensive deposit of dust from the global dust storm events that occurred in 2001. The crater at the summit of Ceraunius Tholus is about 25 km (

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Mars - Composite of images obtained by the Mars Global Surveyor probe in 1999

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Mars - Composite of images obtained by the Mars Global Surveyor probe in 1999

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Volcano Arsia Mons - Arsia Mons volcano. - Arsia Mons is one of the largest known volcanoes. It rises more than 9 km above the Martian surface and its caldera extends for 110 km. Image obtained by the Mars Global Surveyor probe. Arsia Mons is one of the largest volcanoes known. This shield volcano is part of an aligned trio known as the Tharsis Montes (the others are Pavonis Mons and Ascraeus Mons). Arsia Mons is rivaled only by Olympus Mons in terms of its volume. The summit of Arsia Mons is more than 9 kilometers (5.6 miles) higher than the surrounding plains. The crater (or caldera) at the volcano summit is approximately 110 km (68 mi) across. This view of Arsia Mons was taken by the red and blue wide angle cameras of the Mars Global Surveyor Mars Orbiter Camera (MOC) system. Bright water ice clouds (the whitish/bluish wisps) hang above the volcano, a common sight every martian afternoon in this region. Arsia Mons is located at 120* west longitude and 9* south latitude. Illumination

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Volcano Arsia Mons - Arsia Mons volcano. - Arsia Mons is one of the largest known volcanoes. It rises more than 9 km above the Martian surface and its caldera extends for 110 km. Image obtained by the Mars Global Surveyor probe. Arsia Mons is one of the largest volcanoes known. This shield volcano is part of an aligned trio known as the Tharsis Montes (the others are Pavonis Mons and Ascraeus Mons). Arsia Mons is rivaled only by Olympus Mons in terms of its volume. The summit of Arsia Mons is more than 9 kilometers (5.6 miles) higher than the surrounding plains. The crater (or caldera) at the volcano summit is approximately 110 km (68 mi) across. This view of Arsia Mons was taken by the red and blue wide angle cameras of the Mars Global Surveyor Mars Orbiter Camera (MOC) system. Bright water ice clouds (the whitish/bluish wisps) hang above the volcano, a common sight every martian afternoon in this region. Arsia Mons is located at 120* west longitude and 9* south latitude. Illumination

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Supermassif black hole - Artist view - Supermassive Black hole - Artist view - Artist view of a supermassive black hole in the center of a galaxy. This artist's concept illustrates a supermassive black hole with millions to billions times the mass of our sun. Supermassive black holes are enormously dense objects buried at the hearts of galaxies. (Smaller black holes also exist throughout galaxies.) In this illustration, the supermassive black hole at the center is surrounded by matter flowing onto the black hole in what is termed an accretion disk. This disk forms as the dust and gas in the galaxy falls onto the hole, attracted by its gravity

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Supermassif black hole - Artist view - Supermassive Black hole - Artist view - Artist view of a supermassive black hole in the center of a galaxy. This artist's concept illustrates a supermassive black hole with millions to billions times the mass of our sun. Supermassive black holes are enormously dense objects buried at the hearts of galaxies. (Smaller black holes also exist throughout galaxies.) In this illustration, the supermassive black hole at the center is surrounded by matter flowing onto the black hole in what is termed an accretion disk. This disk forms as the dust and gas in the galaxy falls onto the hole, attracted by its gravity

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Black Holes in 3C75 - Black Holes in 3C75 - Composite X-ray image (blue) and radio (pink) of the active galaxy 3C 75. At the center of this very hot gas mass, two supermassive black holes separated by 25,000 years - light form a binary system of black holes (the two bright points). This composite X - ray/radio image of Abell 400 shows radio jets (pink), immersed in a vast cloud of multimillion degree X - ray emitting gas (blue) that pervades the cluster. The jets emanate from the vicinity of two supermassive black holes (bright spots in the image) in the galaxy. Chandra and radio data confirm that the unusual structure is due to the merger of two large galaxies, whose supermassive black holes are bound together by their mutual gravity. The swept - back appearance of the radio jets is produced by the rapid motion of the galaxy through the hot gas of the cluster, in much the same way that a motorcyclist's scarf is swept back while speeding down the road

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Black Holes in 3C75 - Black Holes in 3C75 - Composite X-ray image (blue) and radio (pink) of the active galaxy 3C 75. At the center of this very hot gas mass, two supermassive black holes separated by 25,000 years - light form a binary system of black holes (the two bright points). This composite X - ray/radio image of Abell 400 shows radio jets (pink), immersed in a vast cloud of multimillion degree X - ray emitting gas (blue) that pervades the cluster. The jets emanate from the vicinity of two supermassive black holes (bright spots in the image) in the galaxy. Chandra and radio data confirm that the unusual structure is due to the merger of two large galaxies, whose supermassive black holes are bound together by their mutual gravity. The swept - back appearance of the radio jets is produced by the rapid motion of the galaxy through the hot gas of the cluster, in much the same way that a motorcyclist's scarf is swept back while speeding down the road

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Spiral galaxy M81 infrared view - Spiral galaxy M81 seen in infrared - View obtained by Spitzer space telescope in different wavelengths. In infrared, Spitzer sees dust rather than stars, thus improving our understanding of star formation. The M81 spiral galaxy is located 12 million light years away from Earth. Its arms are home to star-forming regions while its core is surrounded by much older yellow stars. Located in the northern constellation of Ursa Major (which also includes the Big Dipper), this galaxy is easily visible through binoculars or a small telescope. M81 is located at a distance of 12 million light - years. These infrared images were obtained by Spitzer's infrared array camera. At these wavelengths, Spitzer sees the dust, rather than the stars, within the disc of silicates and carbonaceous grains. It is well - mixed with gas, which is best seen at radio wavelengths, to form the essential ingredients for future star formation

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Spiral galaxy M81 infrared view - Spiral galaxy M81 seen in infrared - View obtained by Spitzer space telescope in different wavelengths. In infrared, Spitzer sees dust rather than stars, thus improving our understanding of star formation. The M81 spiral galaxy is located 12 million light years away from Earth. Its arms are home to star-forming regions while its core is surrounded by much older yellow stars. Located in the northern constellation of Ursa Major (which also includes the Big Dipper), this galaxy is easily visible through binoculars or a small telescope. M81 is located at a distance of 12 million light - years. These infrared images were obtained by Spitzer's infrared array camera. At these wavelengths, Spitzer sees the dust, rather than the stars, within the disc of silicates and carbonaceous grains. It is well - mixed with gas, which is best seen at radio wavelengths, to form the essential ingredients for future star formation

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Active Galaxy NGC 1068 in the Whale - Active galaxy NGC 1068 - This composite image shows that a strong stellar wind escapes from the heart of the galaxy NGC 1068 or resides a massive black hole. NGC 1068 is located about 50 million light years away from Earth. Images obtained in X-ray by the Chandra satellite (red), visible by the Hubble space telescope (green) and radio waves (blue). This is a composite image of NGC 1068, one of the nearest and brightest galaxies containing a rapidly growing supermassive black hole. X - ray data from the Chandra X - ray Observatory are shown in red, optical data from the Hubble Space Telescope in green and radio data from the Very Large Array in blue. The spiral structure of NGC 1068 is shown by the X - ray and optical data, and a jet powered by the central supermassive black hole is shown by the radio data. The X - ray images and spectra obtained using Chandra's High Energy Transmission Grating Spectrometer show that a strong wind is being driven aw

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Active Galaxy NGC 1068 in the Whale - Active galaxy NGC 1068 - This composite image shows that a strong stellar wind escapes from the heart of the galaxy NGC 1068 or resides a massive black hole. NGC 1068 is located about 50 million light years away from Earth. Images obtained in X-ray by the Chandra satellite (red), visible by the Hubble space telescope (green) and radio waves (blue). This is a composite image of NGC 1068, one of the nearest and brightest galaxies containing a rapidly growing supermassive black hole. X - ray data from the Chandra X - ray Observatory are shown in red, optical data from the Hubble Space Telescope in green and radio data from the Very Large Array in blue. The spiral structure of NGC 1068 is shown by the X - ray and optical data, and a jet powered by the central supermassive black hole is shown by the radio data. The X - ray images and spectra obtained using Chandra's High Energy Transmission Grating Spectrometer show that a strong wind is being driven aw

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Europe by satellite - Light pollution - This image is a composite of hundreds of pictures made by the Defense Meteorological Satellite Program (DMSP) currently operates four satellites carrying the Operational Linescan System (OLS) in low - altitude polar orbits. Three of these satellites record nighttime data. The DMSP - OLS has a unique capability to detect low levels of visible - near infrared (VNIR) radiance at night. With the OLS “” VIS”” band data it is possible to detect clouds illuminated by moonlight, plus lights from cities, towns, industrial sites, gas flares, and ephemeral events such as fires and lightning - illuminated clouds. The Nighttime Lights of the World data set is compiled from the October 1994 - March 1995 DMSP nighttime data collected when moonlight was low. Using the OLS thermal infrared band, areas containing clouds were removed and the remaining area used in the time series

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Europe by satellite - Light pollution - This image is a composite of hundreds of pictures made by the Defense Meteorological Satellite Program (DMSP) currently operates four satellites carrying the Operational Linescan System (OLS) in low - altitude polar orbits. Three of these satellites record nighttime data. The DMSP - OLS has a unique capability to detect low levels of visible - near infrared (VNIR) radiance at night. With the OLS “” VIS”” band data it is possible to detect clouds illuminated by moonlight, plus lights from cities, towns, industrial sites, gas flares, and ephemeral events such as fires and lightning - illuminated clouds. The Nighttime Lights of the World data set is compiled from the October 1994 - March 1995 DMSP nighttime data collected when moonlight was low. Using the OLS thermal infrared band, areas containing clouds were removed and the remaining area used in the time series

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Europe at night - Europe at night - Europe at night by satellite. Mosaic of hundreds of images obtained by DMSP (Defense Meteorological Satellite Program) satellites in 2003. This image shows human - generated nighttime lights in Europe for the calendar year 2003, based on observations by the Defense Meteorological Satellite Program Operational Line Scanner. In this image, oceans appear black, landmasses appear in varying shades of blue, and lights appear yellow - white. Because these images focus on human impact, they do not include other (natural) light sources. Besides assembling cloud - free images, data visualizers carefully excluded sunlight, moonlight, and light from the Northern Hemisphere aurora

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Europe at night - Europe at night - Europe at night by satellite. Mosaic of hundreds of images obtained by DMSP (Defense Meteorological Satellite Program) satellites in 2003. This image shows human - generated nighttime lights in Europe for the calendar year 2003, based on observations by the Defense Meteorological Satellite Program Operational Line Scanner. In this image, oceans appear black, landmasses appear in varying shades of blue, and lights appear yellow - white. Because these images focus on human impact, they do not include other (natural) light sources. Besides assembling cloud - free images, data visualizers carefully excluded sunlight, moonlight, and light from the Northern Hemisphere aurora

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Saturn against day seen by Cassini - Mosaic of 165 photos obtained by the Cassini probe on September 15, 2006 has a distance of 2.2 million km from the planet. The probe remained 12 hours in Saturn's shadow, allowing it to study Saturn's rings under a particular light. During these observations, two new rings of particles were discovered near ring G. The ring system of rings is composed from the closest to Saturn to the outermost by ring D, then C, B, the division of Cassini, A with the division of Encke, F, G and E. On this view where the contrast has been exaggerated, rings G and E are visible.

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Saturn against day seen by Cassini - Mosaic of 165 photos obtained by the Cassini probe on September 15, 2006 has a distance of 2.2 million km from the planet. The probe remained 12 hours in Saturn's shadow, allowing it to study Saturn's rings under a particular light. During these observations, two new rings of particles were discovered near ring G. The ring system of rings is composed from the closest to Saturn to the outermost by ring D, then C, B, the division of Cassini, A with the division of Encke, F, G and E. On this view where the contrast has been exaggerated, rings G and E are visible.

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Saturn rings C - B by Cassini - false colors - Image in fake colors made by the Cassini probe on June 30, 2004. The different colors correspond to differences in the chemical composition of the particles that make up the rings. The ring system is composed from the closest to Saturn to the outermost by ring D, then C, B, the division of Cassini, A with the division of Encke, F, G and E. Here are the variations in the composition of rings C and B that are watched. Turquoise blue corresponds to particles composed of pure ice; in red, dirty and finer ice particles.

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Saturn rings C - B by Cassini - false colors - Image in fake colors made by the Cassini probe on June 30, 2004. The different colors correspond to differences in the chemical composition of the particles that make up the rings. The ring system is composed from the closest to Saturn to the outermost by ring D, then C, B, the division of Cassini, A with the division of Encke, F, G and E. Here are the variations in the composition of rings C and B that are watched. Turquoise blue corresponds to particles composed of pure ice; in red, dirty and finer ice particles.

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Saturn seen by the Cassini probe 04/2007 - Saturn from Cassini spacecraft 04/2007 - Image obtained by the Cassini probe on 13 April 2007 at a distance of 1.8 million km from the planet. Colorful Saturn tilts its darkened ringplane towards Cassini. Against the dark sky, the rings are made visible by the light that scatters through them towards the camera. The F ring shepherd moon Pandora (84 kilometers, or 52 miles across) is faintly visible at the top, left of center. Pandora's brightness was increased by a factor of three to aid its visibility. This view looks toward the unilluminated side of the rings from about 18 degrees above the ringplane. The planet is visible through the innermost and outermost portions of the rings. The images were obtained by the Cassini spacecraft wide - angle camera on April 13, 2007, at a distance of approximately 1.8 million kilometers (1.1 million miles) from Saturn

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Saturn seen by the Cassini probe 04/2007 - Saturn from Cassini spacecraft 04/2007 - Image obtained by the Cassini probe on 13 April 2007 at a distance of 1.8 million km from the planet. Colorful Saturn tilts its darkened ringplane towards Cassini. Against the dark sky, the rings are made visible by the light that scatters through them towards the camera. The F ring shepherd moon Pandora (84 kilometers, or 52 miles across) is faintly visible at the top, left of center. Pandora's brightness was increased by a factor of three to aid its visibility. This view looks toward the unilluminated side of the rings from about 18 degrees above the ringplane. The planet is visible through the innermost and outermost portions of the rings. The images were obtained by the Cassini spacecraft wide - angle camera on April 13, 2007, at a distance of approximately 1.8 million kilometers (1.1 million miles) from Saturn

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Saturn and satellites seen by the Cassini probe on 30/01/2008 - Saturn and satellites seen by Cassini spacecraft Jan. 30 2008 - Saturn seen by the Cassini probe on 30 January 2008 at a distance of 1.3 million km from the planet. The Tethys satellite is visible under Saturn's rings and the Titan satellite appears at the top of the picture. Titan emerges from behind Saturn, while Tethys streaks into view, in this colorful scene. Saturn's shadow darkens the far arm of the rings near the planet's limb. Titan is 5,150 kilometers (3,200 miles) wide; Tethys is 1,071 kilometers (665 miles) wide. This view looks toward the unilluminated side of the rings from about 3 degrees above the ringplane. Images taken using red, green and blue spectral filters were combined to create this natural color view. The images were acquired with the Cassini spacecraft wide - angle camera on Jan. 30, 2008 at a distance of approximately 1.3 million kilometers (800,000 miles) from Saturn. Image scale is 77 kilomete

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Saturn and satellites seen by the Cassini probe on 30/01/2008 - Saturn and satellites seen by Cassini spacecraft Jan. 30 2008 - Saturn seen by the Cassini probe on 30 January 2008 at a distance of 1.3 million km from the planet. The Tethys satellite is visible under Saturn's rings and the Titan satellite appears at the top of the picture. Titan emerges from behind Saturn, while Tethys streaks into view, in this colorful scene. Saturn's shadow darkens the far arm of the rings near the planet's limb. Titan is 5,150 kilometers (3,200 miles) wide; Tethys is 1,071 kilometers (665 miles) wide. This view looks toward the unilluminated side of the rings from about 3 degrees above the ringplane. Images taken using red, green and blue spectral filters were combined to create this natural color view. The images were acquired with the Cassini spacecraft wide - angle camera on Jan. 30, 2008 at a distance of approximately 1.3 million kilometers (800,000 miles) from Saturn. Image scale is 77 kilomete

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Saturn and Mimas seen by the Cassini probe 18/01/2005 - Saturn and Mimas seen by Cassini spacecraft Jan. 18 2005 - The Mimas satellite photographed in front of Saturn by the Cassini probe on 18 January 2005 at a distance of 1.4 million km from the planet. The shadow of Saturn's rings is projected on the planet. Mimas drifts along in its orbit against the azure backdrop of Saturn's northern latitudes in this true color view. The long, dark lines on the atmosphere are shadows cast by the planet's rings. Saturn's northern hemisphere is presently relatively cloud - free, and rays of sunlight take a long path through the atmosphere. This results in sunlight being scattered at shorter (bluer) wavelengths, thus giving the northernmost latitudes their bluish appearance at visible wavelengths. At the bottom, craters on icy Mimas (398 kilometers, or 247 miles across) give the moon a dimpled appearance. Images taken using infrared (930 nanometers), green (568 nanometers) and ultraviolet (338 nano

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Saturn and Mimas seen by the Cassini probe 18/01/2005 - Saturn and Mimas seen by Cassini spacecraft Jan. 18 2005 - The Mimas satellite photographed in front of Saturn by the Cassini probe on 18 January 2005 at a distance of 1.4 million km from the planet. The shadow of Saturn's rings is projected on the planet. Mimas drifts along in its orbit against the azure backdrop of Saturn's northern latitudes in this true color view. The long, dark lines on the atmosphere are shadows cast by the planet's rings. Saturn's northern hemisphere is presently relatively cloud - free, and rays of sunlight take a long path through the atmosphere. This results in sunlight being scattered at shorter (bluer) wavelengths, thus giving the northernmost latitudes their bluish appearance at visible wavelengths. At the bottom, craters on icy Mimas (398 kilometers, or 247 miles across) give the moon a dimpled appearance. Images taken using infrared (930 nanometers), green (568 nanometers) and ultraviolet (338 nano

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Japet, satellite of Saturn, seen by Cassini - Crescent of Iapetus seen by Cassini spacecraft. - Mosaic in fake colors of Japet, a satellite of 1436 kilometers in diameter, taken by the Cassini probe on 10 September 2007 has a distance of 83 000 km from the satellite. Iapetus, 1,468 kilometers (912 miles) across, seen here in false color, is unique in its dramatic variation in brightness between the northern polar region and the middle and low latitudes. Equally prominent is the moon's equatorial ridge of towering mountains. The profile of the ridge against the darkness of space reveals that it is topped by a cratered plateau approximately 15 kilometers (9 miles) wide. Further west, the profile of the ridge changes from a long plateau to discrete peaks. The mosaic consists of four image footprints across the surface of Iapetus and has a resolution of 489 meters (0.3 miles) per pixel. The color seen in this view represents an expansion of the wavelength region of the electromagnetic spec

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Japet, satellite of Saturn, seen by Cassini - Crescent of Iapetus seen by Cassini spacecraft. - Mosaic in fake colors of Japet, a satellite of 1436 kilometers in diameter, taken by the Cassini probe on 10 September 2007 has a distance of 83 000 km from the satellite. Iapetus, 1,468 kilometers (912 miles) across, seen here in false color, is unique in its dramatic variation in brightness between the northern polar region and the middle and low latitudes. Equally prominent is the moon's equatorial ridge of towering mountains. The profile of the ridge against the darkness of space reveals that it is topped by a cratered plateau approximately 15 kilometers (9 miles) wide. Further west, the profile of the ridge changes from a long plateau to discrete peaks. The mosaic consists of four image footprints across the surface of Iapetus and has a resolution of 489 meters (0.3 miles) per pixel. The color seen in this view represents an expansion of the wavelength region of the electromagnetic spec

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Japet, satellite of Saturn, seen by Cassini - Saturn's moon Iapetus seen by Cassini spacecraft. - Mosaic in false colors of Japet, a satellite of 1436 kilometers in diameter, taken by the Cassini probe on 10 September 2007 has a distance of 73,000 km from the satellite. The image shows the bright side of the satellite; a large 450 km wide impact basin is visible towards the bottom of the image. This false - color mosaic shows the entire hemisphere of Iapetus (1,468 kilometers, or 912 miles across) visible from Cassini on Sept. 10 2007 at a distance of about 73,000 kilometers (45,000 miles) from Iapetus. Near the top of the mosaic, numerous impact features are visible, including the craters Ogier and Charlemagne. The most prominent topographic feature in this view, in the bottom half of the mosaic, is a 450 - kilometer (280 - mile) wide impact basin

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Japet, satellite of Saturn, seen by Cassini - Saturn's moon Iapetus seen by Cassini spacecraft. - Mosaic in false colors of Japet, a satellite of 1436 kilometers in diameter, taken by the Cassini probe on 10 September 2007 has a distance of 73,000 km from the satellite. The image shows the bright side of the satellite; a large 450 km wide impact basin is visible towards the bottom of the image. This false - color mosaic shows the entire hemisphere of Iapetus (1,468 kilometers, or 912 miles across) visible from Cassini on Sept. 10 2007 at a distance of about 73,000 kilometers (45,000 miles) from Iapetus. Near the top of the mosaic, numerous impact features are visible, including the craters Ogier and Charlemagne. The most prominent topographic feature in this view, in the bottom half of the mosaic, is a 450 - kilometer (280 - mile) wide impact basin

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Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft: The Tethys satellite photographed by the Cassini probe on 11 April 2015 has a distance of 53,000 km from the satellite. Tethys is about 1070 km in diameter. - This enhancement-color mosaic of Saturn's icy moon Tethys shows a range of features on the moon's trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet - Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys' surface at wavelengths not visible to human eyes. The moon's surface is fairly uniform in natural color - The color of the surface changes conspicuously across the disk, from yellowish hues to nearly white. These broad color changes are affected by a number of external processes. First, S

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Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft: The Tethys satellite photographed by the Cassini probe on 11 April 2015 has a distance of 53,000 km from the satellite. Tethys is about 1070 km in diameter. - This enhancement-color mosaic of Saturn's icy moon Tethys shows a range of features on the moon's trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet - Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys' surface at wavelengths not visible to human eyes. The moon's surface is fairly uniform in natural color - The color of the surface changes conspicuously across the disk, from yellowish hues to nearly white. These broad color changes are affected by a number of external processes. First, S

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Space Telescope Spitzer - Artist view - The Spitzer space telescope. Artwork - The Spitzer space telescope observes the universe in infrared; it was launched and put into orbit in August 2003. Spitzer looks towards the Rho Ophiuchi star - formation region looming just above the disk of the Milky Way. The Spitzer Space Telescope (formerly SIRTF, the Space Infrared Telescope Facility) was launched into space by a Delta rocket from Cape Canaveral, Florida on 25 August 2003. During its mission, Spitzer will obtain images and spectra by detecting the infrared energy, or heat, radiated by objects in space between wavelengths of 3 and 180 microns (1 micron is one - millionth of a meter). Most of this infrared radiation is blocked by the Earth's atmosphere and cannot be observed from the ground

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Space Telescope Spitzer - Artist view - The Spitzer space telescope. Artwork - The Spitzer space telescope observes the universe in infrared; it was launched and put into orbit in August 2003. Spitzer looks towards the Rho Ophiuchi star - formation region looming just above the disk of the Milky Way. The Spitzer Space Telescope (formerly SIRTF, the Space Infrared Telescope Facility) was launched into space by a Delta rocket from Cape Canaveral, Florida on 25 August 2003. During its mission, Spitzer will obtain images and spectra by detecting the infrared energy, or heat, radiated by objects in space between wavelengths of 3 and 180 microns (1 micron is one - millionth of a meter). Most of this infrared radiation is blocked by the Earth's atmosphere and cannot be observed from the ground

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The Cassini and Saturn probe - Cassini spacecraft at Saturn - Artist's view of the Cassini probe above the northern hemisphere of Saturn. This illustration shows Cassini above Saturn's northern hemisphere prior to making one of its Grand Finale dives. During Cassini's Grand Finale, the spacecraft will make 22 orbits around Saturn that carry the spacecraft over the planet's north before diving between Saturn and its rings. At the conclusion of this final set of daring orbits, the spacecraft will plunge into Saturn's atmosphere, ending its mission on Sept. 15, 2017.

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The Cassini and Saturn probe - Cassini spacecraft at Saturn - Artist's view of the Cassini probe above the northern hemisphere of Saturn. This illustration shows Cassini above Saturn's northern hemisphere prior to making one of its Grand Finale dives. During Cassini's Grand Finale, the spacecraft will make 22 orbits around Saturn that carry the spacecraft over the planet's north before diving between Saturn and its rings. At the conclusion of this final set of daring orbits, the spacecraft will plunge into Saturn's atmosphere, ending its mission on Sept. 15, 2017.

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The Cassini and Saturn probe - Cassini spacecraft at Saturn - Artist's view of the Cassini probe during its final dip into the atmosphere of Saturn on September 15, 2017. As depicted in this illustration, Cassini will plunge into Saturn's atmosphere on Sept 15, 2017. Using its attitude control thrusters, the spacecraft will work to keep its antenna pointed at Earth while it sends its final data, including the composition of Saturn's upper atmosphere. The atmospheric torque will quickly become stronger than what the thrusters can compensate for, and after that point, Cassini will begin to tumble. When this happens, its radio connection to Earth will be severed, ending the mission. Following loss of signal, the spacecraft will burn up like a meteor in Saturn's upper atmosphere.

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The Cassini and Saturn probe - Cassini spacecraft at Saturn - Artist's view of the Cassini probe during its final dip into the atmosphere of Saturn on September 15, 2017. As depicted in this illustration, Cassini will plunge into Saturn's atmosphere on Sept 15, 2017. Using its attitude control thrusters, the spacecraft will work to keep its antenna pointed at Earth while it sends its final data, including the composition of Saturn's upper atmosphere. The atmospheric torque will quickly become stronger than what the thrusters can compensate for, and after that point, Cassini will begin to tumble. When this happens, its radio connection to Earth will be severed, ending the mission. Following loss of signal, the spacecraft will burn up like a meteor in Saturn's upper atmosphere.

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Galactic centre region seen in X - Center of our galaxy in X Ray - Region of the centre of our galaxy seen in X-ray by the Chandra satellite. In the center of the image (white area), Sagittarius A*, the gas cloud surrounding a supermassive black hole. Mosaic of 88 images obtained between 2000 and 2007. This spectacular mosaic of Chandra images reveals hundreds of white dwarf stars, neutron stars, and black holes bathed in an incandescent fog of multimillion degree gas. A supermassive black hole, Sagittarius A*, residing at the center of our Galaxy is located inside the bright white patch in the middle of the image. This image combines low energy X-rays (colored red), intermediate energy X-rays (green) and high energy X-rays (blue). Mosaic of 88 images

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Galactic centre region seen in X - Center of our galaxy in X Ray - Region of the centre of our galaxy seen in X-ray by the Chandra satellite. In the center of the image (white area), Sagittarius A*, the gas cloud surrounding a supermassive black hole. Mosaic of 88 images obtained between 2000 and 2007. This spectacular mosaic of Chandra images reveals hundreds of white dwarf stars, neutron stars, and black holes bathed in an incandescent fog of multimillion degree gas. A supermassive black hole, Sagittarius A*, residing at the center of our Galaxy is located inside the bright white patch in the middle of the image. This image combines low energy X-rays (colored red), intermediate energy X-rays (green) and high energy X-rays (blue). Mosaic of 88 images

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South pole of the Moon seen by the LRO - South pole of the Moon - Mosaic probe of 288 images obtained in 2010 by the LRO probe. As LRO passes over the pole every two hours, the LROC WAC snaps an image, and over a month, images covering the entire polar region are captured (80* S to 90* S). This mosaic contains 288 images taken in one month; you can see where the month began and ended at about 90* E longitude (note how the lighting changed). The rim of Shackleton crater seems to be disjointed. However, if you look closely, you can see that the Sun came from opposite sides for portions of the mosaic, resulting in opposite sides of the crater's wall being illuminated in some images. As the mission progresses, the WAC captures the pole across the full range of seasons

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South pole of the Moon seen by the LRO - South pole of the Moon - Mosaic probe of 288 images obtained in 2010 by the LRO probe. As LRO passes over the pole every two hours, the LROC WAC snaps an image, and over a month, images covering the entire polar region are captured (80* S to 90* S). This mosaic contains 288 images taken in one month; you can see where the month began and ended at about 90* E longitude (note how the lighting changed). The rim of Shackleton crater seems to be disjointed. However, if you look closely, you can see that the Sun came from opposite sides for portions of the mosaic, resulting in opposite sides of the crater's wall being illuminated in some images. As the mission progresses, the WAC captures the pole across the full range of seasons

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Perseverance - Ingenuity protective shield - 2021 (photo)

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Perseverance - Ingenuity protective shield - 2021 (photo)

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The Ingenuity Helicopter - 2021 (photo)

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The Ingenuity Helicopter - 2021 (photo)

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March - Spirit - Panorama McMurdo - Detail - 10 - 2006 - March: McMurdo panorama - Spirit - Detail - 10 - 2006 - Detail of the panorama “” Mac Murdo”” obtained by the Spirit rover from April to October 2006. Spirit stayed in the same place directing its solar panels towards the Sun to recharge its batteries. Many dark, porous volcanic rocks are visible in this image. The Rover Spirit landed on Mars in the Gusev crater area on July 4, 2004. “McMurdo” panorama detail. From April through October 2006, Spirit has stayed on a small hill known as “Low Ridge.”” There, the rover's solar panels are tilted towards the sun to maintain enough solar power for Spirit to keep making scientific observations throughout the winter on southern Mars. This view of the surroundings from Spirit's “” Winter Haven”” is presented in approximately true color. Many dark, porous - textured volcanic rocks can be seen

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March - Spirit - Panorama McMurdo - Detail - 10 - 2006 - March: McMurdo panorama - Spirit - Detail - 10 - 2006 - Detail of the panorama “” Mac Murdo”” obtained by the Spirit rover from April to October 2006. Spirit stayed in the same place directing its solar panels towards the Sun to recharge its batteries. Many dark, porous volcanic rocks are visible in this image. The Rover Spirit landed on Mars in the Gusev crater area on July 4, 2004. “McMurdo” panorama detail. From April through October 2006, Spirit has stayed on a small hill known as “Low Ridge.”” There, the rover's solar panels are tilted towards the sun to maintain enough solar power for Spirit to keep making scientific observations throughout the winter on southern Mars. This view of the surroundings from Spirit's “” Winter Haven”” is presented in approximately true color. Many dark, porous - textured volcanic rocks can be seen

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Nebula Trifide (M20) in the constellation Sagittarius - Trifid nebula (M20) in Sagittarius - View of the Trifide nebula (M20/NGC 6514) located in the constellation Sagittarius between 5000 and 10,000 years - light from Earth. Image obtained by combining light through 3 different filters that highlight oxygen, hydrogen, and sulfur. Trifid is located in Sagittarius constellation between 5000 and 10 000 light - years away. Composite image from Hubble space telescope and Subaru data sources. Narrowband composite H - alpha, OIII, SII

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Nebula Trifide (M20) in the constellation Sagittarius - Trifid nebula (M20) in Sagittarius - View of the Trifide nebula (M20/NGC 6514) located in the constellation Sagittarius between 5000 and 10,000 years - light from Earth. Image obtained by combining light through 3 different filters that highlight oxygen, hydrogen, and sulfur. Trifid is located in Sagittarius constellation between 5000 and 10 000 light - years away. Composite image from Hubble space telescope and Subaru data sources. Narrowband composite H - alpha, OIII, SII

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Nebula NGC 1333 in Persee infrared view - NGC 1333 star - forming region seen in infrared. - NGC 1333 is a nebula located between 700 and 1000 years - light of the Earth. It's a reflexion nebula and a star-forming region. Viewed here in infrared by the Spitzer space telescope, young stars become visible. Jets of matter, in yellow - green, emerge from extremely young embryonic stars. Located between 700 and 1000 light - years from Earth in the constellation Perseus, the reflection nebula called NGC 1333 is seen here in infrared pictured by the Spitzer Space Telescope. The young stars in NGC 1333 do not form a single cluster, but are split between two sub-groups. One group is to the north near the nebula, dominated by the infrared light from warm dust shown as red in the image. The other group is south, where the features shown in yellow and green abound in the densest part of the natal gas cloud. The knotty yellow - green features are glowing shock fronts where jets of material, spewed

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Nebula NGC 1333 in Persee infrared view - NGC 1333 star - forming region seen in infrared. - NGC 1333 is a nebula located between 700 and 1000 years - light of the Earth. It's a reflexion nebula and a star-forming region. Viewed here in infrared by the Spitzer space telescope, young stars become visible. Jets of matter, in yellow - green, emerge from extremely young embryonic stars. Located between 700 and 1000 light - years from Earth in the constellation Perseus, the reflection nebula called NGC 1333 is seen here in infrared pictured by the Spitzer Space Telescope. The young stars in NGC 1333 do not form a single cluster, but are split between two sub-groups. One group is to the north near the nebula, dominated by the infrared light from warm dust shown as red in the image. The other group is south, where the features shown in yellow and green abound in the densest part of the natal gas cloud. The knotty yellow - green features are glowing shock fronts where jets of material, spewed

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