|
|
First Peek at Spitzer's Lega
…
| Title |
First Peek at Spitzer's Legacy: Mysterious Whirlpool Galaxy |
| Description |
NASA's Spitzer Space Telescope has captured these infrared images of the "Whirlpool Galaxy," revealing strange structures bridging the gaps between the dust-rich spiral arms, and tracing the dust, gas and stellar populations in both the bright spiral galaxy and its companion. The Spitzer image is a four-color composite of invisible light, showing emissions from wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8.0 microns (red). These wavelengths are roughly 10 times longer than those seen by the human eye. The visible light image comes from the Kitt Peak National Observatory 2.1m telescope, and has the same orientation and size as the Spitzer infrared image, measuring 9.9 by 13.7 arcminutes (north up). Also a four-color composite, the visible light image shows emissions from 0.4 to 0.7 microns, including the H-alpha nebular feature (red in the image). The light seen in the images originates from very different sources. At shorter wavelengths (in the visible bands, and in the infrared from 3.6 to 4.5 microns), the light comes mainly from stars. This starlight fades at longer wavelengths (5.8 to 8.0 microns), where we see the glow from clouds of interstellar dust. This dust consists mainly of a variety of carbon-based organic molecules known collectively as polycyclic aromatic hydrocarbons. Wherever these compounds are found, there will also be dust granules and gas, which provide a reservoir of raw materials for future star formation. Particularly puzzling are the large number of thin filaments of red emission seen in the infrared data between the arms of the large spiral galaxy. In contrast to the beady nature of the dust emission seen in the arms themselves, these spoke-like features are thin and regular, and prevalent in the gaps all over the face of the galaxy. Also of interest is the contrast in the distributions of dust and stars between the spiral and its faint companion. While the spiral is rich in dust, bright in the longer infrared wavebands, and actively forming new stars, its blue companion shows little infrared emission and hosts an older stellar population. The spectacular whirlpool structure and star formation in M51 are thought to be triggered by an ongoing collision with its companion. Understanding the impact on star formation by the interaction of galaxies is one of the goals of these observations. The targeted galaxy is known by various names: M51 from its Messier catalog designation, and also as NGC 5194. M51 was one of the original discoveries of Charles Messier, found in October 1773 while he was observing a faint comet. The Messier catalogue of galaxies is named after him. Colloquially, M51 is also known as the "Whirlpool Galaxy", or "Rosse's Galaxy," after Lord Rosse, who first detected galaxy spiral structure in his observations of M51. The companion, NGC 5195, was discovered in 1781 by Pierre Mechain. The Whirlpool galaxy is a favorite target for amateur and professional, astronomers, alike, and was the first light target for the Infrared Space Observatory. Found in the constellation Canes Venatici, M51 is 37 million light-years away. The Spitzer observations of M51 are part of a large 500-hour science project, known as the Spitzer Infrared Nearby Galaxy Survey, which will comprehensively study 75 nearby galaxies with infrared imaging and spectroscopy. From these data, astronomers will probe the physical processes connecting star formation to the properties of galaxies. This information will provide a vital foundation of data, diagnostic tools, and astrophysical inputs for understanding the distant universe, ultraluminous galaxies, and the formation and evolution of galaxies. |
|
First Peek at Spitzer's Lega
…
| Title |
First Peek at Spitzer's Legacy: Mysterious Whirlpool Galaxy |
| Description |
NASA's Spitzer Space Telescope has captured these infrared images of the "Whirlpool Galaxy," revealing strange structures bridging the gaps between the dust-rich spiral arms, and tracing the dust, gas and stellar populations in both the bright spiral galaxy and its companion. The Spitzer image is a four-color composite of invisible light, showing emissions from wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8.0 microns (red). These wavelengths are roughly 10 times longer than those seen by the human eye. The visible light image comes from the Kitt Peak National Observatory 2.1m telescope, and has the same orientation and size as the Spitzer infrared image, measuring 9.9 by 13.7 arcminutes (north up). Also a four-color composite, the visible light image shows emissions from 0.4 to 0.7 microns, including the H-alpha nebular feature (red in the image). The light seen in the images originates from very different sources. At shorter wavelengths (in the visible bands, and in the infrared from 3.6 to 4.5 microns), the light comes mainly from stars. This starlight fades at longer wavelengths (5.8 to 8.0 microns), where we see the glow from clouds of interstellar dust. This dust consists mainly of a variety of carbon-based organic molecules known collectively as polycyclic aromatic hydrocarbons. Wherever these compounds are found, there will also be dust granules and gas, which provide a reservoir of raw materials for future star formation. Particularly puzzling are the large number of thin filaments of red emission seen in the infrared data between the arms of the large spiral galaxy. In contrast to the beady nature of the dust emission seen in the arms themselves, these spoke-like features are thin and regular, and prevalent in the gaps all over the face of the galaxy. Also of interest is the contrast in the distributions of dust and stars between the spiral and its faint companion. While the spiral is rich in dust, bright in the longer infrared wavebands, and actively forming new stars, its blue companion shows little infrared emission and hosts an older stellar population. The spectacular whirlpool structure and star formation in M51 are thought to be triggered by an ongoing collision with its companion. Understanding the impact on star formation by the interaction of galaxies is one of the goals of these observations. The targeted galaxy is known by various names: M51 from its Messier catalog designation, and also as NGC 5194. M51 was one of the original discoveries of Charles Messier, found in October 1773 while he was observing a faint comet. The Messier catalogue of galaxies is named after him. Colloquially, M51 is also known as the "Whirlpool Galaxy", or "Rosse's Galaxy," after Lord Rosse, who first detected galaxy spiral structure in his observations of M51. The companion, NGC 5195, was discovered in 1781 by Pierre Mechain. The Whirlpool galaxy is a favorite target for amateur and professional, astronomers, alike, and was the first light target for the Infrared Space Observatory. Found in the constellation Canes Venatici, M51 is 37 million light-years away. The Spitzer observations of M51 are part of a large 500-hour science project, known as the Spitzer Infrared Nearby Galaxy Survey, which will comprehensively study 75 nearby galaxies with infrared imaging and spectroscopy. From these data, astronomers will probe the physical processes connecting star formation to the properties of galaxies. This information will provide a vital foundation of data, diagnostic tools, and astrophysical inputs for understanding the distant universe, ultraluminous galaxies, and the formation and evolution of galaxies. |
|
First Peek at Spitzer's Lega
…
| Title |
First Peek at Spitzer's Legacy: Mysterious Whirlpool Galaxy |
| Description |
NASA's Spitzer Space Telescope has captured these infrared images of the "Whirlpool Galaxy," revealing strange structures bridging the gaps between the dust-rich spiral arms, and tracing the dust, gas and stellar populations in both the bright spiral galaxy and its companion. The Spitzer image is a four-color composite of invisible light, showing emissions from wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8.0 microns (red). These wavelengths are roughly 10 times longer than those seen by the human eye. The visible light image comes from the Kitt Peak National Observatory 2.1m telescope, and has the same orientation and size as the Spitzer infrared image, measuring 9.9 by 13.7 arcminutes (north up). Also a four-color composite, the visible light image shows emissions from 0.4 to 0.7 microns, including the H-alpha nebular feature (red in the image). The light seen in the images originates from very different sources. At shorter wavelengths (in the visible bands, and in the infrared from 3.6 to 4.5 microns), the light comes mainly from stars. This starlight fades at longer wavelengths (5.8 to 8.0 microns), where we see the glow from clouds of interstellar dust. This dust consists mainly of a variety of carbon-based organic molecules known collectively as polycyclic aromatic hydrocarbons. Wherever these compounds are found, there will also be dust granules and gas, which provide a reservoir of raw materials for future star formation. Particularly puzzling are the large number of thin filaments of red emission seen in the infrared data between the arms of the large spiral galaxy. In contrast to the beady nature of the dust emission seen in the arms themselves, these spoke-like features are thin and regular, and prevalent in the gaps all over the face of the galaxy. Also of interest is the contrast in the distributions of dust and stars between the spiral and its faint companion. While the spiral is rich in dust, bright in the longer infrared wavebands, and actively forming new stars, its blue companion shows little infrared emission and hosts an older stellar population. The spectacular whirlpool structure and star formation in M51 are thought to be triggered by an ongoing collision with its companion. Understanding the impact on star formation by the interaction of galaxies is one of the goals of these observations. The targeted galaxy is known by various names: M51 from its Messier catalog designation, and also as NGC 5194. M51 was one of the original discoveries of Charles Messier, found in October 1773 while he was observing a faint comet. The Messier catalogue of galaxies is named after him. Colloquially, M51 is also known as the "Whirlpool Galaxy", or "Rosse's Galaxy," after Lord Rosse, who first detected galaxy spiral structure in his observations of M51. The companion, NGC 5195, was discovered in 1781 by Pierre Mechain. The Whirlpool galaxy is a favorite target for amateur and professional, astronomers, alike, and was the first light target for the Infrared Space Observatory. Found in the constellation Canes Venatici, M51 is 37 million light-years away. The Spitzer observations of M51 are part of a large 500-hour science project, known as the Spitzer Infrared Nearby Galaxy Survey, which will comprehensively study 75 nearby galaxies with infrared imaging and spectroscopy. From these data, astronomers will probe the physical processes connecting star formation to the properties of galaxies. This information will provide a vital foundation of data, diagnostic tools, and astrophysical inputs for understanding the distant universe, ultraluminous galaxies, and the formation and evolution of galaxies. |
|
Visible-Infrared Whirlpool
| Title |
Visible-Infrared Whirlpool |
| Description |
This animation transitions from the more familiar visible light image of the "Whirlpool Galaxy" to the dramatic new view captured by NASA's Spitzer Space Telescope. Revealed are strange structures bridging the gaps between the dust-rich spiral arms, and tracing the dust, gas and stellar populations in both the bright spiral galaxy and its companion. The visible light image comes from the Kitt Peak National Observatory 2.1m telescope, and is a four-color composite showing light from 0.4 to 0.7 microns, including the H-alpha nebular feature (red in the image). The Spitzer image is a four-color composite of invisible light of wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8.0 microns (red). These wavelengths are roughly 10 times longer than those seen by the human eye. The light seen in the images originates from very different sources. At shorter wavelengths (in the visible bands, and in the infrared from 3.6 to 4.5 microns), the light comes mainly from stars. This starlight fades at longer wavelengths (5.8 to 8.0 microns), where we see the glow from clouds of interstellar dust. This dust consists mainly of a variety of carbon-based organic molecules known collectively as polycyclic aromatic hydrocarbons. Wherever these compounds are found, there will also be dust granules and gas, which provide a reservoir of raw materials for future star formation. In the transition from the visible to the infrared view, the dust lanes seen as dark streaks to the human eye become vivid filaments of red emission seen in the infrared data between the arms of the large spiral galaxy. In contrast to the beady nature of the dust emission seen in the arms themselves, these spoke-like features are thin and regular, and prevalent in the gaps all over the face of the galaxy. Also of interest is the contrast in the distributions of dust and stars between the spiral and its faint companion. While the spiral is rich in dust, bright in the longer infrared wavebands, and actively forming new stars, its blue companion shows little infrared emission and hosts an older stellar population. The spectacular whirlpool structure and star formation in M51 are thought to be triggered by an ongoing collision with its companion. Understanding the impact on star formation by the interaction of galaxies is one of the goals of these observations. The targeted galaxy is known by various names: M51 from its Messier catalog designation, and also as NGC 5194. M51 was one of the original discoveries of Charles Messier, found in October 1773 while he was observing a faint comet. The Messier catalogue of galaxies is named after him. Colloquially, M51 is also known as the "Whirlpool Galaxy", or "Rosse's Galaxy," after Lord Rosse, who first detected galaxy spiral structure in his observations of M51. The companion, NGC 5195, was discovered in 1781 by Pierre Mechain. The Whirlpool galaxy is a favorite target for amateur and professional astronomers, alike, and, was the first light target for the Infrared Space Observatory. Found in the constellation Canes Venatici, M51 is 37 million light-years away. The Spitzer observations of M51 are part of a large 500-hour science project, known as the Spitzer Infrared Nearby Galaxy Survey, which will comprehensively study 75 nearby galaxies with infrared imaging and spectroscopy. From these data, astronomers will probe the physical processes connecting star formation to the properties of galaxies. This information will provide a vital foundation of data, diagnostic tools, and astrophysical inputs for understanding the distant universe, ultraluminous galaxies, and the formation and evolution of galaxies. |
|
Titania's Trenches
| Title |
Titania's Trenches |
| Explanation |
British astronomer Sir William Herschel [ http://star.arm.ac.uk/history/herschel.html ] discovered Titania and Oberon in January of 1787. He wasn't reading Shakespeare's [ http://the-tech.mit.edu/Shakespeare/works.html ]"A Midsummer Night's Dream" though, he was making the first telescopic observations of moons of the planet Uranus [ http://seds.lpl.arizona.edu/nineplanets/nineplanets/uranus.html ] (a planet which he himself discovered in 1781 [ http://www-groups.dcs.st-and.ac.uk/~history/ HistTopics/Neptune_and_Pluto.html ]). In January of 1986, nearly 200 years later, NASA's robot explorer Voyager 2 became the only spacecraft to visit the remote Uranian [ http://antwrp.gsfc.nasa.gov/apod/ap990531.html ] system [ http://antwrp.gsfc.nasa.gov/apod/ap971103.html ]. Above is Voyager's highest resolution picture of Titania [ http://photojournal.jpl.nasa.gov/cgi-bin/ PIAGenCatalogPage.pl?PIA00039 ], Uranus' largest moon. The picture is a composite of two images recorded from a distance of 229,000 miles. The icy, rocky world [ http://antwrp.gsfc.nasa.gov/apod/ap960304.html ] is seen to be covered with impact craters. A prominent system of fault valleys, some nearly 1,000 miles long, is visible as trench-like features near the terminator (shadow line). Deposits of highly reflective material which may represent frost can be seen along the sun-facing valley walls. The large impact crater near the top, known as Gertrude [ http://wwwflag.wr.usgs.gov/USGSFlag/Space/nomen/uranus/titacrat.html ], is about 180 miles across. At the bottom the 60 mile wide fault valley, Belmont Chasma [ http://wwwflag.wr.usgs.gov/USGSFlag/Space/nomen/uranus/titachas.html ], cuts into crater Ursula. Titania itself [ http://wwwflag.wr.usgs.gov/USGSFlag/Space/wall/titania.html ] is 1,000 miles in diameter. |
|
M106 in Canes Venatici
| Title |
M106 in Canes Venatici |
| Explanation |
Close to the Great Bear (Ursa Major) and surrounded by the stars [ http://www.enchantedlearning.com/subjects/astronomy/stars/ constellations.shtml ] of the Hunting Dogs (Canes Venatici), this celestial nebula was discovered [ http://www.seds.org/messier/Mdes/dm106.html ] in 1781 by the metric [ http://www.britannica.com/eb/article?eu=52982 ] French astronomer Pierre Mechain [ http://www.seds.org/messier/xtra/history/ pmechain.html ] and later added to the catalog of his friend and colleague Charles Messier as M106 [ http://www.seds.org/messier/m/m106.html ]. Modern deep telescopic views reveal it to be an island universe [ http://antwrp.gsfc.nasa.gov/apod/ap020518.html ] -- a spiral galaxy around 30 thousand light-years across located only about 21 million light-years beyond the stars of the Milky Way. Youthful blue star clusters and reddish stellar nurseries trace the striking spiral arms of M106. Seen so clearly in this beautiful image [ http://www.noao.edu/outreach/aop/observers/m106.html ], the galaxy's bright core is also visible across the spectrum [ http://www.ipac.caltech.edu/Outreach/Multiwave/ ] from radio to x-rays, making M106 a nearby example of the Seyfert class [ http://antwrp.gsfc.nasa.gov/apod/ap981023.html ] of active galaxies. The bright core of a Seyfert galaxy is believed to be powered by matter falling into a massive central black hole [ http://csep10.phys.utk.edu/astr162/lect/active/ smblack.html ]. |
|
M106 in Canes Venatici
| Title |
M106 in Canes Venatici |
| Explanation |
Close to the Great Bear (Ursa Major) and surrounded by the stars [ http://www.enchantedlearning.com/subjects/astronomy/stars/ constellations.shtml ] of the Hunting Dogs (Canes Venatici), this celestial nebula was discovered [ http://www.seds.org/messier/Mdes/dm106.html ] in 1781 by the metric [ http://www.britannica.com/eb/article?eu=52982 ] French astronomer Pierre Mechain [ http://www.seds.org/messier/xtra/history/ pmechain.html ]. Later, it was added to the catalog of his friend and colleague Charles Messier as M106 [ http://www.seds.org/messier/m/m106.html ]. Modern deep telescopic views reveal it to be an island universe [ http://antwrp.gsfc.nasa.gov/apod/ap020518.html ] -- a spiral galaxy around 30 thousand light-years across located only about 21 million light-years beyond the stars of the Milky Way. Youthful blue star clusters and reddish stellar nurseries trace the striking spiral arms of M106. Seen so clearly in this beautiful image [ http://www.noao.edu/outreach/aop/observers/m106.html ], the galaxy's bright core is also visible across the spectrum [ http://coolcosmos.ipac.caltech.edu/cosmic_classroom/ multiwavelength_astronomy/multiwavelength_astronomy/ ] from radio to x-rays, making M106 a nearby example of the Seyfert class [ http://antwrp.gsfc.nasa.gov/apod/ap981023.html ] of active galaxies. The bright core of a Seyfert galaxy is believed to be powered by matter falling into a massive central black hole [ http://csep10.phys.utk.edu/astr162/lect/active/ smblack.html ]. |
|
Los Angeles from Space
PIA02679
Sol (our sun)
ASTER
| Title |
Los Angeles from Space |
| Original Caption Released with Image |
This ASTER image was acquired on July 23, 2001 and covers an area of 64 x 72 km. The data were processed to create a simulated natural color image. From its start as a sleepy Spanish pueblo in 1781, LA and its metropolitan area has grown to become an ethnically diverse, semitropical megalopolis, laying claim as the principal center of the western US and the nation's second largest urban area. The city's economy is based on international trade, aerospace, agriculture, tourism, and filmmaking. LA provides a glimpse of the typically cosmopolitan and global city of the future. Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) is one of five Earth-observing instruments launched December 18, 1999, on NASA's Terra satellite. The instrument was built by Japan's Ministry of International Trade and Industry. A joint U.S./Japan science team is responsible for validation and calibration of the instrument and the data products. Dr. Anne Kahle at NASA's Jet Propulsion Laboratory, Pasadena, Calif., is the U.S. Science team leader, Moshe Pniel of JPL is the project manager. ASTER is the only high resolution imaging sensor on Terra. The primary goal of the ASTER mission is to obtain high-resolution image data in 14 channels over the entire land surface, as well as black and white stereo images. With revisit time of between 4 and 16 days, ASTER will provide the capability for repeat coverage of changing areas on Earth's surface. The broad spectral coverage and high spectral resolution of ASTER will provide scientists in numerous disciplines with critical information for surface mapping, and monitoring dynamic conditions and temporal change. Example applications are: monitoring glacial advances and retreats, monitoring potentially active volcanoes, identifying crop stress, determining cloud morphology and physical properties, wetlands Evaluation, thermal pollution monitoring, coral reef degradation, surface temperature mapping of soils and geology, and measuring surface heat balance. |
|
|
