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Images of 'NASA' found, 8,712

 
Martian dunes at the end of winter - March: Late Winter view of Dunes: Detail on dunes in the southern hemisphere of Mars. With the end of winter, the Sun melts the carbon dioxide ice present all winter. Image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on March 21, 2016. HIRISE is a 50 cm telescope that observes visible and near infrared. Sand dunes cover much of this terrain, which has large boulders lying on flat areas between the dunes. It is now late winter here in the Southern hemisphere, and these dunes are just getting enough sunlight to start defrosting their seasonal cover of carbon dioxide. Spots form where pressurized carbon dioxide gas escapes to the surface

PIX4580064

Martian dunes at the end of winter - March: Late Winter view of Dunes: Detail on dunes in the southern hemisphere of Mars. With the end of winter, the Sun melts the carbon dioxide ice present all winter. Image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on March 21, 2016. HIRISE is a 50 cm telescope that observes visible and near infrared. Sand dunes cover much of this terrain, which has large boulders lying on flat areas between the dunes. It is now late winter here in the Southern hemisphere, and these dunes are just getting enough sunlight to start defrosting their seasonal cover of carbon dioxide. Spots form where pressurized carbon dioxide gas escapes to the surface

PIX4580064

 
Laminate structures near the north pole on Mars - Layers Exposed at North Polar Cap on Mars: Laminated structures near the north polar cap of Mars. These different layers of ice and girders correspond to climatic variations over the last ten thousand years. Image obtained on 18 April 2016 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. HIRISE is a 50 cm telescope that observes visible and near infrared. At the edge of Mars' permanent North Polar cap, we see an exposure of the internal layers, each with a different mix of water ice, dust and dirt. These layers are believed to correspond to different climate conditions over the past tens of thousands of years. When we zoom in closer, we see that the distinct layers erode differently. Some are stronger and more resistant to erosion, others only weakly cemented. The strong layers form ledges

PIX4580071

Laminate structures near the north pole on Mars - Layers Exposed at North Polar Cap on Mars: Laminated structures near the north polar cap of Mars. These different layers of ice and girders correspond to climatic variations over the last ten thousand years. Image obtained on 18 April 2016 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. HIRISE is a 50 cm telescope that observes visible and near infrared. At the edge of Mars' permanent North Polar cap, we see an exposure of the internal layers, each with a different mix of water ice, dust and dirt. These layers are believed to correspond to different climate conditions over the past tens of thousands of years. When we zoom in closer, we see that the distinct layers erode differently. Some are stronger and more resistant to erosion, others only weakly cemented. The strong layers form ledges

PIX4580071

 
Spiral galaxies NGC 3314 A and B in Hydra - Galaxy pair NGC 3314 in Hydra - NGC 3314 is a pair of spiral galaxies distant about 140 million years - Earth light. These galaxies are not interacting but just perfectly aligned in front of each other from Earth. Through an extraordinary chance alignment, a face - on spiral galaxy lies precisely in front of another larger spiral. This line - up provides us with the rare chance to visualize dark material within the front galaxy, seen only because it is silhouetted against the object behind it. NGC 3314 lies about 140 million light - years from Earth, in the direction of the southern hemisphere constellation Hydra. The bright blue stars forming a pinwheel shape near the center of the front galaxy have formed recently from interstellar gas and dust. In many galaxies, interstellar dust lies only in the same regions as recently formed blue stars. However, in the foreground galaxy, NGC 3314a, there are numerous additional dark dust lanes that are

PIX4610557

Spiral galaxies NGC 3314 A and B in Hydra - Galaxy pair NGC 3314 in Hydra - NGC 3314 is a pair of spiral galaxies distant about 140 million years - Earth light. These galaxies are not interacting but just perfectly aligned in front of each other from Earth. Through an extraordinary chance alignment, a face - on spiral galaxy lies precisely in front of another larger spiral. This line - up provides us with the rare chance to visualize dark material within the front galaxy, seen only because it is silhouetted against the object behind it. NGC 3314 lies about 140 million light - years from Earth, in the direction of the southern hemisphere constellation Hydra. The bright blue stars forming a pinwheel shape near the center of the front galaxy have formed recently from interstellar gas and dust. In many galaxies, interstellar dust lies only in the same regions as recently formed blue stars. However, in the foreground galaxy, NGC 3314a, there are numerous additional dark dust lanes that are

PIX4610557

 
Planetary nebula NGC 5189 in the Fly - NGC 5189 - Planetary nebula in Musca - This nebula is located about 3000 light years from Earth in the southern constellation of Fly. Image obtained by the Hubble Space Telescope (HST). The colors used in this image correspond to the emissions of different gases: sulfur in green, hydrogen in orange and oxygen in blue. Hubble Space Telescope have photographed a festive - looking nearby planetary nebula called NGC 5189. Planetary nebulae represent the final brief stage in the life of a medium - sized star like our Sun. While consuming the last of the fuel in its core, the dying star expels a large portion of its outer envelope. This material then becomes heated by the radiation from the stellar remnant and radiates, producing glowing clouds of gas that can show complex structures, as the ejection of mass from the star is uneven in both time and direction. This image was taken with Hubble's Wide Field Camera 3 on October 8, 2012, in filters tuned to

PIX4623125

Planetary nebula NGC 5189 in the Fly - NGC 5189 - Planetary nebula in Musca - This nebula is located about 3000 light years from Earth in the southern constellation of Fly. Image obtained by the Hubble Space Telescope (HST). The colors used in this image correspond to the emissions of different gases: sulfur in green, hydrogen in orange and oxygen in blue. Hubble Space Telescope have photographed a festive - looking nearby planetary nebula called NGC 5189. Planetary nebulae represent the final brief stage in the life of a medium - sized star like our Sun. While consuming the last of the fuel in its core, the dying star expels a large portion of its outer envelope. This material then becomes heated by the radiation from the stellar remnant and radiates, producing glowing clouds of gas that can show complex structures, as the ejection of mass from the star is uneven in both time and direction. This image was taken with Hubble's Wide Field Camera 3 on October 8, 2012, in filters tuned to

PIX4623125

 
Asteroide Vesta and other asteroides - Asteroid Vesta compared to other asteroids - Comparison of the sizes of the nine asteroides visits to date by space probes. The asteroid Vesta, with a diameter of 530 km, is the largest. This composite image shows the comparative sizes of nine asteroids. Up until now, Lutetia, with a diameter of 81 miles (130 kilometers), was the largest asteroid visited by a spacecraft, which occurred during a flyby. Vesta, which is also considered a protoplanet because it's a large body that almost became a planet, dwarfs all other small bodies in this image, with its diameter sizing up at approximately 330 miles (530 kilometers)

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Asteroide Vesta and other asteroides - Asteroid Vesta compared to other asteroids - Comparison of the sizes of the nine asteroides visits to date by space probes. The asteroid Vesta, with a diameter of 530 km, is the largest. This composite image shows the comparative sizes of nine asteroids. Up until now, Lutetia, with a diameter of 81 miles (130 kilometers), was the largest asteroid visited by a spacecraft, which occurred during a flyby. Vesta, which is also considered a protoplanet because it's a large body that almost became a planet, dwarfs all other small bodies in this image, with its diameter sizing up at approximately 330 miles (530 kilometers)

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Asteroid collapsed by tidal force - Artist view - Artist view - Artist view - Artist view - Artist view of an asteroid breaks by the gravitational attraction of a star at the end of life, a white dwarf. This artist's concept illustrates a dead star, or “” white dwarf,””” surrounded by the bits and pieces of a disintegrating asteroid. Asteroids are leftover scraps of planetary material. They form early on in a star's history when planets are forming out of collisions between rocky bodies. When a star like our sun dies, shrinking down to a skeleton of its former self called a white dwarf, its asteroids get jostled about. If one of these asteroids gets too close to the white dwarf, the white dwarf's gravity will chew the asteroid up, leaving a cloud of dust

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Asteroid collapsed by tidal force - Artist view - Artist view - Artist view - Artist view - Artist view of an asteroid breaks by the gravitational attraction of a star at the end of life, a white dwarf. This artist's concept illustrates a dead star, or “” white dwarf,””” surrounded by the bits and pieces of a disintegrating asteroid. Asteroids are leftover scraps of planetary material. They form early on in a star's history when planets are forming out of collisions between rocky bodies. When a star like our sun dies, shrinking down to a skeleton of its former self called a white dwarf, its asteroids get jostled about. If one of these asteroids gets too close to the white dwarf, the white dwarf's gravity will chew the asteroid up, leaving a cloud of dust

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Japet, satellite of Saturn, seen by Cassini - Saturn's moon Iapetus seen by Cassini spacecraft - Comparison of the two hemispheres of Japet, a satellite of Saturn of 1471 kilometres in diameter. Its main feature is the color difference between the two hemispheres. On the left, the dark region called Cassini Regio with to the east the largest crater of Japet, named Turgis (580 km in diameter). On the right, the bright side of the satellite with Roncevaux Terra (north) and Saragossa Terra (south) housing the large impact crater Engelier (504 km in diameter). Both images were obtained by the Cassini probe on 10 September 2007 (right) and 27 December 2004 (left). These two global images of Iapetus show the extreme brightness dichotomy on the surface of this peculiar Saturnian moon. The left - hand panel shows the moon's leading hemisphere and the right - hand panel shows the moon's trailing side. While low and mid latitudes of the leading side exhibit a surface almost as dark as charcoal,

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Japet, satellite of Saturn, seen by Cassini - Saturn's moon Iapetus seen by Cassini spacecraft - Comparison of the two hemispheres of Japet, a satellite of Saturn of 1471 kilometres in diameter. Its main feature is the color difference between the two hemispheres. On the left, the dark region called Cassini Regio with to the east the largest crater of Japet, named Turgis (580 km in diameter). On the right, the bright side of the satellite with Roncevaux Terra (north) and Saragossa Terra (south) housing the large impact crater Engelier (504 km in diameter). Both images were obtained by the Cassini probe on 10 September 2007 (right) and 27 December 2004 (left). These two global images of Iapetus show the extreme brightness dichotomy on the surface of this peculiar Saturnian moon. The left - hand panel shows the moon's leading hemisphere and the right - hand panel shows the moon's trailing side. While low and mid latitudes of the leading side exhibit a surface almost as dark as charcoal,

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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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Star Formation in the Southern Crown - A cluster of stars in the constellation of the Southern Crown seen in infrared by the Spitzer space telescope. R Coronae Australis is one of the closest and most intense star-forming regions; visible in the southern hemisphere, it is located about 500 light years away from Earth. The Corona Australis region (containing, at its heart, the Coronet cluster) is one of the nearest and most active regions of ongoing star formation. The infrared Spitzer image shows young stars more diffuse emission from dust

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Star Formation in the Southern Crown - A cluster of stars in the constellation of the Southern Crown seen in infrared by the Spitzer space telescope. R Coronae Australis is one of the closest and most intense star-forming regions; visible in the southern hemisphere, it is located about 500 light years away from Earth. The Corona Australis region (containing, at its heart, the Coronet cluster) is one of the nearest and most active regions of ongoing star formation. The infrared Spitzer image shows young stars more diffuse emission from dust

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Saturn rings 30/06/2004 by Cassini in ultraviolet - Image in false colors made by the Cassini probe on 30 June 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 A - B and C that are watched. Encke's division is the outer red line. Turquoise blue corresponds to particles composed of pure ice, in red the dirty and finer ice particles.

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Saturn rings 30/06/2004 by Cassini in ultraviolet - Image in false colors made by the Cassini probe on 30 June 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 A - B and C that are watched. Encke's division is the outer red line. Turquoise blue corresponds to particles composed of pure ice, in red the dirty and finer ice particles.

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Saturn and Mimas seen by the Cassini probe on 04/09/2007 - Saturn and Mimas seen by Cassini spacecraft Sept. 4 2007 - Saturn seen by the Cassini probe on 4/09/2007 at a distance of 2.7 million km from the planet. The Mimas ice satellite is visible under Saturn's rings. The Cassini spacecraft looks beyond Saturn's limb towards the icy face of Mimas, the innermost of the planet's major moons. This view looks toward the sunlit side of the rings from about 3 degrees below the ringplane. Mimas is 396 kilometers (246 miles) across. 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 narrow - angle camera on Sept. 4, 2007 at a distance of approximately 2.7 million kilometers (1.7 million miles) from Saturn and 2.8 million kilometers (1.8 million miles) from Mimas. Image scale is 16 kilometers (10 miles) per pixel on Saturn and 17 kilometers (11 miles) per pixel on Mimas

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Saturn and Mimas seen by the Cassini probe on 04/09/2007 - Saturn and Mimas seen by Cassini spacecraft Sept. 4 2007 - Saturn seen by the Cassini probe on 4/09/2007 at a distance of 2.7 million km from the planet. The Mimas ice satellite is visible under Saturn's rings. The Cassini spacecraft looks beyond Saturn's limb towards the icy face of Mimas, the innermost of the planet's major moons. This view looks toward the sunlit side of the rings from about 3 degrees below the ringplane. Mimas is 396 kilometers (246 miles) across. 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 narrow - angle camera on Sept. 4, 2007 at a distance of approximately 2.7 million kilometers (1.7 million miles) from Saturn and 2.8 million kilometers (1.8 million miles) from Mimas. Image scale is 16 kilometers (10 miles) per pixel on Saturn and 17 kilometers (11 miles) per pixel on Mimas

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Pluto seen by the New Horizons probe - Pluto seen by New Horizons - Pluto seen by the New Horizons probe. Composite image created from four images obtained on 13 July 2015 at a distance of 450,000 km from the dwarf planet. Four images from New Horizons' Long Range Recognition Imager (LORRI) were combined with color data from the Ralph instrument to create this global view of Pluto. (The lower right edge of Pluto in this view currently lacks high - resolution color coverage.) The images, taken when the spacecraft was 280,000 miles (450,000 kilometers) away, show features as small as 1.4 miles (2.2 kilometers), twice the resolution of the single - image view taken on July 13

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Pluto seen by the New Horizons probe - Pluto seen by New Horizons - Pluto seen by the New Horizons probe. Composite image created from four images obtained on 13 July 2015 at a distance of 450,000 km from the dwarf planet. Four images from New Horizons' Long Range Recognition Imager (LORRI) were combined with color data from the Ralph instrument to create this global view of Pluto. (The lower right edge of Pluto in this view currently lacks high - resolution color coverage.) The images, taken when the spacecraft was 280,000 miles (450,000 kilometers) away, show features as small as 1.4 miles (2.2 kilometers), twice the resolution of the single - image view taken on July 13

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Saturn seen at equinox - Saturn during Equinox - Saturn seen by the Cassini probe on August 12, 2009, 1.25 days after the exact date of Saturn equinox. The images that make up this mosaic were obtained at a distance of 847,000 km from the planet. Several satellites are visible in this image: Janus (lower left), Epimethee (lower middle), Pandora (on the right of the image, outside the rings) and Atlas (on the right, inside the F ring). Seen from our planet, the view of Saturn's rings during equinox is extremely foreshortened and limited. But in orbit around Saturn, Cassini spacecraft had no such problems. From 20 degrees above the ring plane, Cassini's wide angle camera shot 75 exposures in succession for this mosaic showing Saturn, its rings, and a few of its moons a day and a half after exact Saturn equinox, when the sun's disk was exactly overhead at the planet's equator. The novel illumination geometry that accompanies equinox lowers the sun's angle to the ring plane, significantly

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Saturn seen at equinox - Saturn during Equinox - Saturn seen by the Cassini probe on August 12, 2009, 1.25 days after the exact date of Saturn equinox. The images that make up this mosaic were obtained at a distance of 847,000 km from the planet. Several satellites are visible in this image: Janus (lower left), Epimethee (lower middle), Pandora (on the right of the image, outside the rings) and Atlas (on the right, inside the F ring). Seen from our planet, the view of Saturn's rings during equinox is extremely foreshortened and limited. But in orbit around Saturn, Cassini spacecraft had no such problems. From 20 degrees above the ring plane, Cassini's wide angle camera shot 75 exposures in succession for this mosaic showing Saturn, its rings, and a few of its moons a day and a half after exact Saturn equinox, when the sun's disk was exactly overhead at the planet's equator. The novel illumination geometry that accompanies equinox lowers the sun's angle to the ring plane, significantly

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Titan, Saturn satellite seen by Cassini - Titan near Saturn seen by Cassini spacecraft - Natural color image of Titan near Saturn blade taken by the Cassini probe on 29 January 2008 at a distance of about 2.3 million km from the satellite. Swathed in its thick blanket of atmosphere, frigid Titan approaches the brilliant limb of Saturn. 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 narrow - angle camera on Jan. 29, 2008 at a distance of approximately 2.3 million kilometers (1.4 million miles) from Titan. Image scale is 14 kilometers (8 miles) per pixel

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Titan, Saturn satellite seen by Cassini - Titan near Saturn seen by Cassini spacecraft - Natural color image of Titan near Saturn blade taken by the Cassini probe on 29 January 2008 at a distance of about 2.3 million km from the satellite. Swathed in its thick blanket of atmosphere, frigid Titan approaches the brilliant limb of Saturn. 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 narrow - angle camera on Jan. 29, 2008 at a distance of approximately 2.3 million kilometers (1.4 million miles) from Titan. Image scale is 14 kilometers (8 miles) per pixel

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Spitzer space telescope - Artist's view - Artwork of Spitzer in its heliocentric orbit - Spitzer space telescope observes the universe in infrared; it was launched and put into orbit in August 2003. 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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Spitzer space telescope - Artist's view - Artwork of Spitzer in its heliocentric orbit - Spitzer space telescope observes the universe in infrared; it was launched and put into orbit in August 2003. 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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First image of the JWST - SMACS galaxy cluster 0723, 2022 (photography)

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First image of the JWST - SMACS galaxy cluster 0723, 2022 (photography)

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JPL control room - Perseverance arrives on Mars - 2021 (photo)

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JPL control room - Perseverance arrives on Mars - 2021 (photo)

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Night Earth - The Americas at night by satellite. 1995

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Night Earth - The Americas at night by satellite. 1995

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La terre vue de nuit - 1992 a 2008 - Lights on Earth's surface - 1992 to 2008 - Earth observed at night by satellite. Composite image obtained by DMSP satellites from 1992 to 2008. The color code corresponds to 1992 (blue), 2000 (green) and 2008 (red). In white, the areas lit during these three years. Composite map of the world assembled from data acquired by satellites. This is a color composite of three years - 1992, 2000, 2008 - of DMSP nighttime lights. Each year has been assigned to one of the primary colors: 1992 = blue, 2000 = green, 2008 = red. The contrast has been enhanced to show all the detected lights, including the dim lighting often detected in populated rural areas. Locations that had bright lighting in all three years are white. There are many rural areas in India and elsewhere that have a bronze color, indicating that they had no detected lighting in 1992 and dim lighting detected in both 2000 and 2008. Notice the areas of blue lighting in several parts of the Former

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La terre vue de nuit - 1992 a 2008 - Lights on Earth's surface - 1992 to 2008 - Earth observed at night by satellite. Composite image obtained by DMSP satellites from 1992 to 2008. The color code corresponds to 1992 (blue), 2000 (green) and 2008 (red). In white, the areas lit during these three years. Composite map of the world assembled from data acquired by satellites. This is a color composite of three years - 1992, 2000, 2008 - of DMSP nighttime lights. Each year has been assigned to one of the primary colors: 1992 = blue, 2000 = green, 2008 = red. The contrast has been enhanced to show all the detected lights, including the dim lighting often detected in populated rural areas. Locations that had bright lighting in all three years are white. There are many rural areas in India and elsewhere that have a bronze color, indicating that they had no detected lighting in 1992 and dim lighting detected in both 2000 and 2008. Notice the areas of blue lighting in several parts of the Former

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La planete Neuf - Illustration - Planet Nine - Artwork: Vue d'artiste de la planete Neuf. The Ninth Planet is a hypothetical planet of the Solar System indirectly recorded, the existence of which is suggested by observing the orbits of several transneptunian objects. This planet would be gaseous, similar to Uranus or Neptune - This is a distant view from Planet Nine back towards the sun. The object is thought to be gaseous, similar to Uranus and Neptune. Hypothetical lightning lights up the night side

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La planete Neuf - Illustration - Planet Nine - Artwork: Vue d'artiste de la planete Neuf. The Ninth Planet is a hypothetical planet of the Solar System indirectly recorded, the existence of which is suggested by observing the orbits of several transneptunian objects. This planet would be gaseous, similar to Uranus or Neptune - This is a distant view from Planet Nine back towards the sun. The object is thought to be gaseous, similar to Uranus and Neptune. Hypothetical lightning lights up the night side

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Remnants of Supernova Tycho in X in Cassiopee - Tycho's Supernova Remnant: Chandra's View of Tycho's Supernova Remnant This Chandra image reveals fascinating details of the turbulent debris created by a supernova explosion that was observed by the Danish astronomer Tycho Brahe in the year 1572. The colors show different X - ray energies, with red, green, and blue representing low, medium and high energies, respectively. The image is cut off at the bottom because the southernmost region of the remnant fell outside the field of view of the detector. A shock wave produced by the expanding debris is outlined by the strikingly sharp blue circular arcs of twenty million degree Celsius gas seen on the outer rim. The stellar debris, which has a temperature of about ten million degrees and is visible only in X - rays, shows up as mottled yellow, green and red fingers of gas. Tycho's supernova remnant presents several interesting contrasts with the Cassiopeia A (Cas A) supernova remnant. The deb

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Remnants of Supernova Tycho in X in Cassiopee - Tycho's Supernova Remnant: Chandra's View of Tycho's Supernova Remnant This Chandra image reveals fascinating details of the turbulent debris created by a supernova explosion that was observed by the Danish astronomer Tycho Brahe in the year 1572. The colors show different X - ray energies, with red, green, and blue representing low, medium and high energies, respectively. The image is cut off at the bottom because the southernmost region of the remnant fell outside the field of view of the detector. A shock wave produced by the expanding debris is outlined by the strikingly sharp blue circular arcs of twenty million degree Celsius gas seen on the outer rim. The stellar debris, which has a temperature of about ten million degrees and is visible only in X - rays, shows up as mottled yellow, green and red fingers of gas. Tycho's supernova remnant presents several interesting contrasts with the Cassiopeia A (Cas A) supernova remnant. The deb

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Black hole collision in NGC 6240 - Black holes colliding in NGC 6240 - The galaxy NGC 6240, is located about 400 million light years away from Earth in the constellation Ophiuchus. This system consists of two colliding galaxies each with a central black hole; in several millions of years, they will form only one galaxy. A composite X-ray image (red, orange and yellow) and visible from the space telescopes Chandra and Hubble. This image of NGC 6240 contains X - ray data from Chandra (shown in red, orange, and yellow) that has been combined with an optical image from the Hubble Space Telescope. In 2002, the discovery of two merging black holes was announced based on Chandra data in this galaxy. The two black holes are a mere 3,000 light years apart and are seen as the bright point - like sources in the middle of the image. Scientists think these black holes are in such close proximity because they are in the midst of spiraling toward each other - a process that began about 30 million yea

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Black hole collision in NGC 6240 - Black holes colliding in NGC 6240 - The galaxy NGC 6240, is located about 400 million light years away from Earth in the constellation Ophiuchus. This system consists of two colliding galaxies each with a central black hole; in several millions of years, they will form only one galaxy. A composite X-ray image (red, orange and yellow) and visible from the space telescopes Chandra and Hubble. This image of NGC 6240 contains X - ray data from Chandra (shown in red, orange, and yellow) that has been combined with an optical image from the Hubble Space Telescope. In 2002, the discovery of two merging black holes was announced based on Chandra data in this galaxy. The two black holes are a mere 3,000 light years apart and are seen as the bright point - like sources in the middle of the image. Scientists think these black holes are in such close proximity because they are in the midst of spiraling toward each other - a process that began about 30 million yea

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Jupiter - New red spot - View of the new red spot of Jupiter obtained on 27 February 2007 by the New Horizons probe, and the WFPC2 instrument of the Hubble space telescope. Jupiter measures 142,984 km in diameter. This red spot is the second largest tempete of Jupiter, it measures about 70% of the Earth's diameter and appeared in 2006. Before it took this colour, this spot had already been observed and named the white oval BA; it was born from the fusion of three small white spots from 1998 to 2000.

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Jupiter - New red spot - View of the new red spot of Jupiter obtained on 27 February 2007 by the New Horizons probe, and the WFPC2 instrument of the Hubble space telescope. Jupiter measures 142,984 km in diameter. This red spot is the second largest tempete of Jupiter, it measures about 70% of the Earth's diameter and appeared in 2006. Before it took this colour, this spot had already been observed and named the white oval BA; it was born from the fusion of three small white spots from 1998 to 2000.

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Exoplanete Kepler-452 b - Artist's impression of the Kepler-452 b exoplanet: Kepler-452 b is an extrasolar planet probably of the Earth type, located in the habitable area of its star Kepler-452, a star similar to our Sun. This super-earth is located in the constellation Swan, about 1400 light years from Earth. This artist's concept depicts one possible appearance of the planet Kepler-452b, the first near-earth-size world to be found in the habitable zone of star that is similar to our sun. The habitable zone is a region around a star where temperatures are right for water to pool on the surface. Scientists do not know if Kepler-452b can support life or not. What is known about the planet is that it is about 60 percent larger than Earth, placing it in a class of planets dubbed “” Super-earths.”” While its mass and composition are not yet determined, previous research suggests that planets the size of Kepler-452b have a better than even chance of being rocky. Kepler-452b orbits its star

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Exoplanete Kepler-452 b - Artist's impression of the Kepler-452 b exoplanet: Kepler-452 b is an extrasolar planet probably of the Earth type, located in the habitable area of its star Kepler-452, a star similar to our Sun. This super-earth is located in the constellation Swan, about 1400 light years from Earth. This artist's concept depicts one possible appearance of the planet Kepler-452b, the first near-earth-size world to be found in the habitable zone of star that is similar to our sun. The habitable zone is a region around a star where temperatures are right for water to pool on the surface. Scientists do not know if Kepler-452b can support life or not. What is known about the planet is that it is about 60 percent larger than Earth, placing it in a class of planets dubbed “” Super-earths.”” While its mass and composition are not yet determined, previous research suggests that planets the size of Kepler-452b have a better than even chance of being rocky. Kepler-452b orbits its star

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Nuclei of the 5 cometes visited by probes - 5 Comets nucleus seen by spacecrafts - Comparison of the size of the nuclei of the five comets visited by space probes. This montage shows the only five comets imaged up close with spacecraft. The comets vary in shape and size. Comet Hartley 2 is by far the smallest and the most active of small comets. This jet activity can be seen extending from the comet's surface and into its outer shell of gas and dust, or coma. This is first time scientists have been able to link jets to the details of the surface

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Nuclei of the 5 cometes visited by probes - 5 Comets nucleus seen by spacecrafts - Comparison of the size of the nuclei of the five comets visited by space probes. This montage shows the only five comets imaged up close with spacecraft. The comets vary in shape and size. Comet Hartley 2 is by far the smallest and the most active of small comets. This jet activity can be seen extending from the comet's surface and into its outer shell of gas and dust, or coma. This is first time scientists have been able to link jets to the details of the surface

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Sirius A and Sirius B in the Big Dog - Sirius A and Sirius B seen in X - ray - Sirius A and Sirius B in the Big Dog seen in X-ray by the Chandra telescope. The brightest source on this image is Sirius B, a white dwarf star whose surface, heated at a temperature of 25,000 degres, emits huge X-rays. The other point is Sirius A, the brightest star in the sky in visible light, but practically non-existent in this wavelength. An X - ray image of the Sirius star system located 8.6 light years from Earth. This image shows two sources and a spike - like pattern due to the support structure for the transmission grating. The bright source is Sirius B, a white dwarf star that has a surface temperature of about 25,000 degrees Celsius which produces very low energy X - rays. The dim source at the position of Sirius A, a normal star more than twice as massive as the Sun, may be due to ultraviolet radiation from Sirius A leaking through the filter on the detector. In contrast, Sirius A is the brighte

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Sirius A and Sirius B in the Big Dog - Sirius A and Sirius B seen in X - ray - Sirius A and Sirius B in the Big Dog seen in X-ray by the Chandra telescope. The brightest source on this image is Sirius B, a white dwarf star whose surface, heated at a temperature of 25,000 degres, emits huge X-rays. The other point is Sirius A, the brightest star in the sky in visible light, but practically non-existent in this wavelength. An X - ray image of the Sirius star system located 8.6 light years from Earth. This image shows two sources and a spike - like pattern due to the support structure for the transmission grating. The bright source is Sirius B, a white dwarf star that has a surface temperature of about 25,000 degrees Celsius which produces very low energy X - rays. The dim source at the position of Sirius A, a normal star more than twice as massive as the Sun, may be due to ultraviolet radiation from Sirius A leaking through the filter on the detector. In contrast, Sirius A is the brighte

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Variable star Mira Ceti view in ultraviolet - Star Mira Ceti seen in ultraviolet - Ultraviolet view of the star Mira of the Whale revealing a long train of material ejected by the large red star. This trail extends over 13 years - light. Mosaic of images obtained by the Galex satellite in November and December 2006. Ultraviolet image of the star Mira taken with the Galex satellite in November and December 2006. In this image, Mira is moving from left to right. It is visible as the small white dot in the bulb shape at right. The shed material can be seen in light blue. The dots in the picture are stars and distant galaxies. The large blue dot at left is a star that is closer to us than Mira. Mira is traveling so fast (130 kilometers per second) that it's creating a bow shock, or build - up of gas, in front of it, as can be seen here at right

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Variable star Mira Ceti view in ultraviolet - Star Mira Ceti seen in ultraviolet - Ultraviolet view of the star Mira of the Whale revealing a long train of material ejected by the large red star. This trail extends over 13 years - light. Mosaic of images obtained by the Galex satellite in November and December 2006. Ultraviolet image of the star Mira taken with the Galex satellite in November and December 2006. In this image, Mira is moving from left to right. It is visible as the small white dot in the bulb shape at right. The shed material can be seen in light blue. The dots in the picture are stars and distant galaxies. The large blue dot at left is a star that is closer to us than Mira. Mira is traveling so fast (130 kilometers per second) that it's creating a bow shock, or build - up of gas, in front of it, as can be seen here at right

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Sunrise on the crater Tycho - Tycho Crater Sunrise - Sunrise on the central peak of the crater Tycho on the Moon. This crater is about 82 km in diameter and its central peak rises at 2 km above sea level. Image obtained on June 10, 2011 by the LRO (Lunar Reconnaissance Orbiter) probe. On 10 June 2011 the LRO spacecraft slewed 65* to the west, allowing the LROC NACs to capture this dramatic sunrise view of Tycho crater. A very popular target with amateur astronomers, Tycho is located at 43.37* S, 348.68* E, and is ~ 82 km (51 miles) in diameter. The summit of the central peak is 2 km (6562 ft) above the crater floor, and the crater floor is about 4700 m (15,420 ft) below the rim. Many “” clasts”” ranging in size from 10 meters to 100s of meters are exposed in the central peak slopes

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Sunrise on the crater Tycho - Tycho Crater Sunrise - Sunrise on the central peak of the crater Tycho on the Moon. This crater is about 82 km in diameter and its central peak rises at 2 km above sea level. Image obtained on June 10, 2011 by the LRO (Lunar Reconnaissance Orbiter) probe. On 10 June 2011 the LRO spacecraft slewed 65* to the west, allowing the LROC NACs to capture this dramatic sunrise view of Tycho crater. A very popular target with amateur astronomers, Tycho is located at 43.37* S, 348.68* E, and is ~ 82 km (51 miles) in diameter. The summit of the central peak is 2 km (6562 ft) above the crater floor, and the crater floor is about 4700 m (15,420 ft) below the rim. Many “” clasts”” ranging in size from 10 meters to 100s of meters are exposed in the central peak slopes

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Cratere Erlanger sur la Lune - Erlanger crater near Moon north pole - Erlanger cratere is located 90 km from the north pole of the Moon. The bottom of this 10 km-diameter crater rarely receives the sun's rays. In this image obtained on August 8, 2009 by the LRO probe (Lunar Reconnaissance Orbiter), only the edges of the crater are illuminated by the Sun. Bed view of Erlanger, crater 10 km (6 miles) across just 90 km (50 miles) from the Moon's north pole. The Sun is perpetually on the horizon as seen from the crater, and only the raised rim is ever lit. In this shot almost the entire circle of the rim can be seen, poking into the sunlight. The crater has steep walls, and the bottom almost never sees sunlight. Image taken by the Lunar Reconnaissance Orbiter's (LRO) instrument on august 8 2009

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Cratere Erlanger sur la Lune - Erlanger crater near Moon north pole - Erlanger cratere is located 90 km from the north pole of the Moon. The bottom of this 10 km-diameter crater rarely receives the sun's rays. In this image obtained on August 8, 2009 by the LRO probe (Lunar Reconnaissance Orbiter), only the edges of the crater are illuminated by the Sun. Bed view of Erlanger, crater 10 km (6 miles) across just 90 km (50 miles) from the Moon's north pole. The Sun is perpetually on the horizon as seen from the crater, and only the raised rim is ever lit. In this shot almost the entire circle of the rim can be seen, poking into the sunlight. The crater has steep walls, and the bottom almost never sees sunlight. Image taken by the Lunar Reconnaissance Orbiter's (LRO) instrument on august 8 2009

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Earth observed at night by satellite. Mosaic of hundreds of images obtained by four satellites DMSP (Defense Meteorological Satellite Program) from October 1994 to March 1995 - The 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. 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: Earth by night

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Earth observed at night by satellite. Mosaic of hundreds of images obtained by four satellites DMSP (Defense Meteorological Satellite Program) from October 1994 to March 1995 - The 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. 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: Earth by night

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Ancient channels on Mars - Ancient channels on planet Mars. Ares Vallis - View of the area of Ares Vallis and Tiu Vallis obtained by the probe 2001 Mars Odyssey. This region seems to have been shaped by the passage of water. Channels scoured by ancient outbursts of flood waters are seen in this orbital view from Odyssey's Thermal Emission Imaging System.The channels are billions of years old and have likely been affected by multiple processes over time. Here, two channels, Tiu Vallis on the left and Ares Vallis on the right, flow northward from the highlands of the southern hemisphere of Mars.The stark difference between today's cold, dry Mars and the evidence of flood waters in the past tells scientists that the Martian climate has seen great changes

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Ancient channels on Mars - Ancient channels on planet Mars. Ares Vallis - View of the area of Ares Vallis and Tiu Vallis obtained by the probe 2001 Mars Odyssey. This region seems to have been shaped by the passage of water. Channels scoured by ancient outbursts of flood waters are seen in this orbital view from Odyssey's Thermal Emission Imaging System.The channels are billions of years old and have likely been affected by multiple processes over time. Here, two channels, Tiu Vallis on the left and Ares Vallis on the right, flow northward from the highlands of the southern hemisphere of Mars.The stark difference between today's cold, dry Mars and the evidence of flood waters in the past tells scientists that the Martian climate has seen great changes

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Nebula Sh2 - 106 in the Swan - Sh2 - 106 nebula in Cygnus - Sharpless 106 (Sh2 - 106) is a star-forming region in the constellation Swan. Image obtained by Hubble Space Telescope (HST) and Subaru Telescope. The bipolar star - forming region, called Sharpless 2 - 106, or S106 for short, looks like a soaring, celestial snow angel. The outstretched “” wings”” of the nebula record the contrasting imprint of heat and motion against the backdrop of a colder medium. Twin lobes of super - hot gas, glowing blue in this image, stretch outward from the central star. This hot gas creates the “” wings”” of our angel. A ring of dust and gas orbiting the star acts like a belt, cinching the expanding nebula into an “” hourglass””” shape. This composite image combines optical and near - infrared astronomical data from the Hubble Space Telescope with mid - infrared data from the ground - based Subaru Telescope, located on Mauna Kea in Hawaii. The Hubble data (H - alpha, J, and H) were taken as part of H

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Nebula Sh2 - 106 in the Swan - Sh2 - 106 nebula in Cygnus - Sharpless 106 (Sh2 - 106) is a star-forming region in the constellation Swan. Image obtained by Hubble Space Telescope (HST) and Subaru Telescope. The bipolar star - forming region, called Sharpless 2 - 106, or S106 for short, looks like a soaring, celestial snow angel. The outstretched “” wings”” of the nebula record the contrasting imprint of heat and motion against the backdrop of a colder medium. Twin lobes of super - hot gas, glowing blue in this image, stretch outward from the central star. This hot gas creates the “” wings”” of our angel. A ring of dust and gas orbiting the star acts like a belt, cinching the expanding nebula into an “” hourglass””” shape. This composite image combines optical and near - infrared astronomical data from the Hubble Space Telescope with mid - infrared data from the ground - based Subaru Telescope, located on Mauna Kea in Hawaii. The Hubble data (H - alpha, J, and H) were taken as part of H

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Galaxies M81 and M82 in the Big Dipper, 2022 (photograph)

R. Gendler

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Galaxies M81 and M82 in the Big Dipper, 2022 (photograph)

R. Gendler

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Mars: dunes and ice in Chasma Boreale - Mars: dunes and ice in Chasma Boreale - Chasma Boreale is a huge canyon located in the northern polar cap of Mars. This image, obtained in light visible by the probe 2001 Mars Odyssey, shows Tenuis Cavus, the end of this valley or the canyon is only 35 km wide. The cliffs to the north (top) and to the east (right) s'elevent 1400 meters above ground. The walls are covered with ice, while at the bottom of the bowl many sand dunes are present. Chasma Boreale is a huge canyon in the northern polar cap. It runs into the ice cap for 570 kilometers (350 miles), making a broad valley that ends at a point called Tenuis Cavus, shown in this THEMIS image taken at visible wavelengths.tapering from a width of 120 km (75 miles) at its mouth, Chasma Boreale is only about 35 km (22 miles) wide here. The cliffs on the northern (top) and eastern (right) sides of the image rise about 1,400 meters (4,600 feet) above the base. On the inside walls of this gigantic amp

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Mars: dunes and ice in Chasma Boreale - Mars: dunes and ice in Chasma Boreale - Chasma Boreale is a huge canyon located in the northern polar cap of Mars. This image, obtained in light visible by the probe 2001 Mars Odyssey, shows Tenuis Cavus, the end of this valley or the canyon is only 35 km wide. The cliffs to the north (top) and to the east (right) s'elevent 1400 meters above ground. The walls are covered with ice, while at the bottom of the bowl many sand dunes are present. Chasma Boreale is a huge canyon in the northern polar cap. It runs into the ice cap for 570 kilometers (350 miles), making a broad valley that ends at a point called Tenuis Cavus, shown in this THEMIS image taken at visible wavelengths.tapering from a width of 120 km (75 miles) at its mouth, Chasma Boreale is only about 35 km (22 miles) wide here. The cliffs on the northern (top) and eastern (right) sides of the image rise about 1,400 meters (4,600 feet) above the base. On the inside walls of this gigantic amp

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Centaur Omega globular cluster - NGC 5139 Omega Centauri globular cluster - Visible to the naked eye in the southern hemisphere, Centaurus Omega is the most massive globular cluster in the galaxy. About 17,000 light years ago, millions of stars nearly 12 billion years old are concentrated here. This image obtained by the Spitzer space telescope reveals in yellow and red the big red stars, whose dust radiates infrared, and in blue the smaller and less evoluted stars. Omega Centauri is the biggest and brightest of the more than 150 similar objects, called globular clusters, that orbit around the outside of our Milky Way galaxy. Stargazers at southern latitudes can spot the stellar gem with the naked eye in the constellation Centaurus. While the visible - light observations highlight the cluster's millions of jam - packed stars, Spitzer's infrared eyes reveal the dustier, more evolved stars tossed throughout the region. Globular clusters are some of the oldest objects in our universe. The

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Centaur Omega globular cluster - NGC 5139 Omega Centauri globular cluster - Visible to the naked eye in the southern hemisphere, Centaurus Omega is the most massive globular cluster in the galaxy. About 17,000 light years ago, millions of stars nearly 12 billion years old are concentrated here. This image obtained by the Spitzer space telescope reveals in yellow and red the big red stars, whose dust radiates infrared, and in blue the smaller and less evoluted stars. Omega Centauri is the biggest and brightest of the more than 150 similar objects, called globular clusters, that orbit around the outside of our Milky Way galaxy. Stargazers at southern latitudes can spot the stellar gem with the naked eye in the constellation Centaurus. While the visible - light observations highlight the cluster's millions of jam - packed stars, Spitzer's infrared eyes reveal the dustier, more evolved stars tossed throughout the region. Globular clusters are some of the oldest objects in our universe. The

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Spiral galaxy M33 infrared view - Spiral galaxy M33 seen in infrared - M33, (NGC 598), the galaxy of the Triangle, is located about 2.9 million years ago - light from Earth. It belongs to the local group, just like our galaxy or Andromede galaxy. This infrared image from the Spitzer space telescope shows stars in blue, gas in green, star formations in red - orange. Red dots are distant galaxies. In infrared, the galaxy appears larger than visible light, revealing cold gas and dust that spread around the galaxy. Also known as M33 or NGC 598, the Triangulum Galaxy is part of the Local Group of galaxies, which includes the Andromeda Galaxy (M31) and our galaxy, the Milky Way. M33 is over thirty thousand light - years across, and more than two million light - years away. Viewed here with Spitzer's infrared eyes, this elegant spiral galaxy sparkles with color and detail. Stars appear as glistening blue gems (several of which are actually foreground stars in our own galaxy), while dust rich

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Spiral galaxy M33 infrared view - Spiral galaxy M33 seen in infrared - M33, (NGC 598), the galaxy of the Triangle, is located about 2.9 million years ago - light from Earth. It belongs to the local group, just like our galaxy or Andromede galaxy. This infrared image from the Spitzer space telescope shows stars in blue, gas in green, star formations in red - orange. Red dots are distant galaxies. In infrared, the galaxy appears larger than visible light, revealing cold gas and dust that spread around the galaxy. Also known as M33 or NGC 598, the Triangulum Galaxy is part of the Local Group of galaxies, which includes the Andromeda Galaxy (M31) and our galaxy, the Milky Way. M33 is over thirty thousand light - years across, and more than two million light - years away. Viewed here with Spitzer's infrared eyes, this elegant spiral galaxy sparkles with color and detail. Stars appear as glistening blue gems (several of which are actually foreground stars in our own galaxy), while dust rich

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