Deep Space Station 53, or DSS-53, is a new 34-meter (111-foot) beam waveguide antenna that went online in February 2022 at the Madrid ground station of NASA's Deep Space Network (DSN). DSS-53 is the fourth of six antennas being added to expand the DSN's capacity and meet the needs of a growing number of spacecraft. When the project is complete, each of the network's three ground stations around the globe will have four beam waveguide antennas. The Madrid Deep Space Communications Complex is the first to have completed its build-out as part of project. Construction on DSS-53 began in 2016. https://photojournal.jpl.nasa.gov/catalog/PIA25137

This artist's concept shows what Deep Space Station-23, a new antenna dish at the Deep Space Network's complex in Goldstone, California, will look like when complete in several years. DSS-23 will communicate with NASA's deep space missions using radio waves and lasers. Retractable covers will be able to fan out across the mirrors at the center of the dish to protect them from the elements. https://photojournal.jpl.nasa.gov/catalog/PIA23617

Deep Space Station 53, or DSS-53, is a new 34-meter (111-foot) beam waveguide antenna that went online in February 2022 at NASA's Deep Space Network's ground station in Madrid. DSS-53 is the fourth of six antennas being added to expand the DSN's capacity and meet the needs of a growing number of spacecraft. When the project is complete, each of the network's three ground stations around the globe will have four beam waveguide antennas. The Madrid Deep Space Communications Complex is the first to have completed its build-out as part of project. Construction on DSS-53 began in 2016. https://photojournal.jpl.nasa.gov/catalog/PIA25136

This sunset photo shows Deep Space Station 14 (DSS-14), the 230-foot-wide (70-meter) antenna at the Goldstone Deep Space Communications Complex near Barstow, California, part of NASA's Deep Space Network. The network's three complexes around the globe support communications with dozens of deep space missions. DSS-14 is also the agency's Goldstone Solar System Radar, which is used to observe asteroids that come close to Earth. https://photojournal.jpl.nasa.gov/catalog/PIA26150

In the early morning of Dec. 18, 2024, a crane looms over the 112-foot-wide (34-meter-wide) steel framework for Deep Space Station 23 (DSS-23) reflector dish, which will soon be lowered into position on the antenna's base structure. Located at the Deep Space Network's Goldstone Space Communications Complex near Barstow, California, DSS-23 is a multi-frequency beam waveguide antenna that will boost the DSN's capacity and enhance NASA's deep space communications capabilities for decades to come. In the background are, from left to right, the beam waveguide antennas DSS-25 and DSS-26, and the decommissioned 85-foot (26-meter) Apollo antenna. https://photojournal.jpl.nasa.gov/catalog/PIA26456

Deep Space Station 56, or DSS-56, is a powerful 34-meter-wide (112-foot-wide) antenna that was added to the Deep Space Network's Madrid Deep Space Communications Complex in Spain in early 2021 after beginning construction in 2017. Deep Space Network (DSN) radio antennas communicate with spacecraft throughout the solar system. Previous antennas have been limited in the frequency bands they can receive and transmit, often being restricted to communicating only with specific spacecraft. DSS-56 is the first to use the DSN's full range of communication frequencies. This means DSS-56 is an "all-in-one" antenna that can communicate with all the missions that the DSN supports and can be used as a backup for any of the Madrid complex's other antennas. With the addition of DSS-56 and other 34-meter antennas to all three DSN complexes, the network is preparing to play a critical role in ensuring communication and navigation support for upcoming Moon and Mars missions and the crewed Artemis missions. https://photojournal.jpl.nasa.gov/catalog/PIA24163

Asteroid 1998 WT24 left in December 2001, right on December 11, 2015 taken by NASA the 230-foot 70-meter DSS-14 antenna at Goldstone, California.

The antenna of the Deep Space Network's Deep Space Station 43 (DSS-43) in Canberra, Australia, spans 70 meters (230 foot) and stands 73 meters (239 foot), dwarfing workers as they perform upgrades on the central cone that contains sensitive transmitters and receivers. A giant crane assisted with the replacement of parts that had been operating on the antenna for over 40 years. One of several antennas located at the Canberra Deep Space Network station, DSS-43 is the largest and responsible for transmitting commands to NASA's Voyager 2 spacecraft. Since early March 2020, DSS-43 has been offline for the upgrades, which are expected to continue until January 2021. https://photojournal.jpl.nasa.gov/catalog/PIA23795

The 230-foot 70-meter DSS-14 antenna at Goldstone, Ca. obtained these radar images of asteroid 2015 TB145 on Oct. 31, 2015. Asteroid 2015 TB145 is depicted in eight individual radar images collected on Oct. 31, 2015 between 5:55 a.m. PDT (8:55 a.m. EDT) and 6:08 a.m. PDT (9:08 a.m. EDT). At the time the radar images were taken, the asteroid was between 440,000 miles (710,000 kilometers) and about 430,000 miles (690,000 kilometers) distant. Asteroid 2015 TB145 safely flew past Earth on Oct. 31, at 10:00 a.m. PDT (1 p.m. EDT) at about 1.3 lunar distances (300,000 miles, 480,000 kilometers). To obtain the radar images, the scientists used the 230-foot (70-meter) DSS-14 antenna at Goldstone, California, to transmit high power microwaves toward the asteroid. The signal bounced of the asteroid, and their radar echoes were received by the National Radio Astronomy Observatory's 100-meter (330-foot) Green Bank Telescope in West Virginia. The images achieve a spatial resolution of about 13 feet (4 meters) per pixel. http://photojournal.jpl.nasa.gov/catalog/PIA20043

In a delicate operation, a 400-ton crane lifts the new X-band cone into the 70-meter (230-foot) Deep Space Network's Deep Space Station 43 (DSS-43) dish in Canberra, Australia. The new cone houses upgraded receiver and transmitter equipment for the 48-year-old antenna. One of several antennas located at the Canberra site, DSS-43 is the largest and responsible for transmitting commands to NASA's Voyager spacecraft. Since early March 2020, DSS43 has been offline for upgrades, which are expected to continue until January 2021. https://photojournal.jpl.nasa.gov/catalog/PIA23796

On Feb. 11, 2020, NASA, JPL, military and local officials broke ground in Goldstone, California, for a new antenna in the agency's Deep Space Network, which communicates with all its deep space missions. When completed in 2 ½ years, the new 112-foot-wide (34-meter-wide) antenna dish will include mirrors and a special receiver for optical, or laser, communications from deep space missions. https://photojournal.jpl.nasa.gov/catalog/PIA23618

A crane lowers the 112-foot-wide (34-meter-wide) steel framework for the Deep Space Station 23 (DSS-23) reflector dish into position on Dec. 18, 2024, at the Deep Space Network's Goldstone Space Communications Complex near Barstow, California. A multi-frequency beam waveguide antenna, DSS-23 will boost the DSN's capacity and enhance NASA's deep space communications capabilities for decades to come. Once online in 2026, DSS-23 will be the fifth of six new beam waveguide antennas to be added to the network, following DSS-53, which was added at the DSN's Madrid complex in 2022. After the reflector skeleton was bolted into place, engineers placed what's called a quadripod into the center of the structure. A four-legged support structure weighing 16 ½ tons, the quadripod is fitted with a curved subreflector that will direct radio frequency signals from deep space that bounce off the main reflector into the antenna's pedestal where the antenna's receivers are housed. Next steps: to fit panels onto the steel skeleton of the parabolic reflector to create a curved surface to collect radio frequency signals. The DSN allows missions to track, send commands to, and receive scientific data from faraway spacecraft. It is managed by NASA's Jet Propulsion Laboratory in Southern California for the agency's Space Communications and Navigation (SCaN) program, which is located at NASA Headquarters within the Space Operations Mission Directorate. https://photojournal.jpl.nasa.gov/catalog/PIA26454

A crane lowers a four-legged support structure called a quadripod onto the steel framework of the Deep Space Station 23 (DSS-23) reflector dish on Dec. 18, 2024. The reflector framework was bolted into place earlier in the day, and the quadripod, which weighs 16 ½ tons, was the last major component to be installed that day. The reflector dish will be fitted with panels to create a curved surface to collect radio frequency signals. The quadripod features a curved subreflector that will direct radio frequency signals from deep space that bounce off the main reflector into the antenna's receiver in its pedestal, where the antenna's receivers are housed. The new 112-foot-wide (34-meter-wide) dish is located at the Deep Space Network's Goldstone Space Communications Complex near Barstow, California. A multi-frequency beam waveguide antenna, DSS-23 will come online in 2026, boosting the DSN's capacity and enhance NASA's deep space communications capabilities for decades to come. It is the fifth of six new beam waveguide antennas to be added to the network, following DSS-53, which was added at the DSN's Madrid complex in 2022. The DSN allows missions to track, send commands to, and receive scientific data from faraway spacecraft. It is managed by NASA's Jet Propulsion Laboratory in Southern California for the agency's Space Communications and Navigation (SCaN) program, which is located at NASA Headquarters within the Space Operations Mission Directorate. https://photojournal.jpl.nasa.gov/catalog/PIA26455

Comet ISON swoops around the sun and through Scorpius. This composite merges an SDO AIA 171 sun image (Nov. 28, 2214 UT), SOHO C2 (2036 UT) and C3 (2030 UT) images, and a DSS view of the sky in northern Scorpius. Credit: NASA/ESA/SOHO, NASA/SDO, DSS, and Francis Reddy <b><a href="http://www.nasa.gov/audience/formedia/features/MP_Photo_Guidelines.html" rel="nofollow">NASA image use policy.</a></b> <b><a href="http://www.nasa.gov/centers/goddard/home/index.html" rel="nofollow">NASA Goddard Space Flight Center</a></b> enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. <b>Follow us on <a href="http://twitter.com/NASA_GoddardPix" rel="nofollow">Twitter</a></b> <b>Like us on <a href="http://www.facebook.com/pages/Greenbelt-MD/NASA-Goddard/395013845897?ref=tsd" rel="nofollow">Facebook</a></b> <b>Find us on <a href="http://instagram.com/nasagoddard?vm=grid" rel="nofollow">Instagram</a></b>

Deep Space Station 13 (DSS-13) at NASA's Goldstone Deep Space Communications Complex near Barstow, California – part of the agency's Deep Space Network – is a 34-meter (112-foot) experimental antenna that has been retrofitted with an optical terminal (the boxy instrument below the center of the antenna's dish). Since November 2023, DSS-13 has been tracking the downlink laser of the Deep Space Optical Communications (DSOC) experiment that is aboard NASA's Psyche mission, which launched on Oct. 13, 2023. In a first, the antenna also synchronously received radio-frequency signals from the spacecraft as it travels through deep space on its way to investigate the metal-rich asteroid Psyche. The laser signal collected by the camera is then transmitted through optical fiber that feeds into a cryogenically cooled semiconducting nanowire single photon detector. Designed and built by JPL's Microdevices Laboratory, the detector is identical to the one used at Caltech's Palomar Observatory, in San Diego County, California, that acts as DSOC's downlink ground station. Goldstone is one of three complexes that comprise NASA's Deep Space Network, which provides radio communications for all of the agency's interplanetary spacecraft and is also utilized for radio astronomy and radar observations of the solar system and the universe. NASA's Jet Propulsion Laboratory, a division of Caltech in Pasadena, California, manages the DSN for the agency. https://photojournal.jpl.nasa.gov/catalog/PIA26148

On the left is a radar image of asteroid 1998 WT24 taken in December 2001 by scientists using NASA's the 230-foot (70-meter) DSS-14 antenna at Goldstone, California. On the right is a radar image of the same asteroid acquired on Dec. 11, 2015, during the asteroid's most recent Earth flyby. The radar images from 2001 (on the left), have a resolution of about 60 feet (19 meters) per pixel. The radar image from 2015 (on the right) achieved a spatial resolution as fine as 25 feet (7.5 meters) per pixel. The 2015 radar image was obtained using the same DSS-14 antenna at Goldstone to transmit high-power microwaves toward the asteroid. However, this time, the radar echoes bounced off the asteroid were received by the National Radio Astronomy Observatory's 100-meter (330-foot) Green Bank Telescope in West Virginia. The next visit of asteroid 1998 WT24 to Earth's neighborhood will be on Nov. 11, 2018, when it will make a distant pass at about 12.5-million miles (52 lunar distances). http://photojournal.jpl.nasa.gov/catalog/PIA20216

Dornier Satelliten Systeme (DSS) workers place the back cover of the Huygens probe under its front heat shield in the Payload Hazardous Servicing Facility (PHSF) at KSC. The spacecraft was returned to the PHSF after damage to thermal insulation was discovered inside Huygens from an abnormally high flow of conditioned air. Internal inspection, insulation repair and a cleaning of the probe were required. Mission managers are targeting a mid-October launch date after the Cassini spacecraft, aboard which Huygens will be launched, returns to the pad and is once again placed atop its Titan IVB expendable launch vehicle at Launch Pad 40 at Cape Canaveral Air Station

Dornier Satelliten Systeme (DSS) workers place the back cover of the Huygens probe under its front heat shield in the Payload Hazardous Servicing Facility (PHSF) at KSC. The spacecraft was returned to the PHSF after damage to thermal insulation was discovered inside Huygens from an abnormally high flow of conditioned air. Internal inspection, insulation repair and a cleaning of the probe were required. Mission managers are targeting a mid-October launch date after the Cassini spacecraft, aboard which Huygens will be launched, returns to the pad and is once again placed atop its Titan IVB expendable launch vehicle at Launch Pad 40 at Cape Canaveral Air Station

Dornier Satelliten Systeme (DSS) workers lift the front heat shield of the Huygens probe in the Payload Hazardous Servicing Facility (PHSF) at KSC. The spacecraft was returned to the PHSF after damage to thermal insulation was discovered inside Huygens from an abnormally high flow of conditioned air. Internal inspection, insulation repair and a cleaning of the probe were required. Mission managers are targeting a mid-October launch date after the Cassini spacecraft, aboard which Huygens will be launched, returns to the pad and is once again placed atop its Titan IVB expendable launch vehicle at Launch Pad 40 at Cape Canaveral Air Station

This image of an asteroid that is at least 3,600 feet (1,100 meters) long was taken on Dec. 17, 2015, by scientists using NASA's 230-foot (70-meter) DSS-14 antenna at Goldstone, California. This asteroid, named 2003 SD2020, will safely fly past Earth on Thursday, Dec. 24, at a distance of 6.8 million miles (11 million kilometers). At the time this image was taken, the asteroid was about 7.3 million miles (12 million kilometers) from Earth. In 2018, this asteroid will fly past Earth at a distance of 1.8 million miles (2.8 million kilometers). http://photojournal.jpl.nasa.gov/catalog/PIA20279

Dornier Satelliten Systeme (DSS) workers lift part of the Huygens probe aft cover assembly in the Payload Hazardous Servicing Facility (PHSF) at KSC. The spacecraft was returned to the PHSF after damage to thermal insulation was discovered inside Huygens from an abnormally high flow of conditioned air. Internal inspection, insulation repair and a cleaning of the probe were required. Mission managers are targeting a mid-October launch date after the Cassini spacecraft, aboard which Huygens will be launched, returns to the pad and is once again placed atop its Titan IVB expendable launch vehicle at Launch Pad 40 at Cape Canaveral Air Station

Dornier Satelliten Systeme (DSS) workers lift the heat shield of the Huygens probe in the Payload Hazardous Servicing Facility (PHSF) at KSC. The spacecraft was returned to the PHSF after damage to thermal insulation was discovered inside Huygens from an abnormally high flow of conditioned air. Internal inspection, insulation repair and a cleaning of the probe were required. Mission managers are targeting a mid-October launch date after the Cassini spacecraft, aboard which Huygens will be launched, returns to the pad and is once again placed atop its Titan IVB expendable launch vehicle at Launch Pad 40 at Cape Canaveral Air Station

Dornier Satelliten Systeme (DSS) workers lift the heat shield of the Huygens probe in the Payload Hazardous Servicing Facility (PHSF) at KSC. The spacecraft was returned to the PHSF after damage to thermal insulation was discovered inside Huygens from an abnormally high flow of conditioned air. Internal inspection, insulation repair and a cleaning of the probe were required. Mission managers are targeting a mid-October launch date after the Cassini spacecraft, aboard which Huygens will be launched, returns to the pad and is once again placed atop its Titan IVB expendable launch vehicle at Launch Pad 40 at Cape Canaveral Air Station

Six iROSA solar arrays in the planned configuration will augment the power drawn from the existing arrays on the International Space Station. Power channels shown are 1A, 2B, 3A, 3B, 4A, and 4B.

This composite image contains data from Chandra (purple) that provides evidence for the survival of a companion star from the blast of a supernova explosion. Chandra's X-rays reveal a point-like source in the supernova remnant at the location of a massive star. The data suggest that mass is being pulled away from the massive star towards a neutron star or a black hole companion. If confirmed, this would be only the third binary system containing both a massive star and a neutron star or black hole ever found in the aftermath of a supernova. This supernova remnant is found embedded in clouds of ionized hydrogen, which are shown in optical light (yellow and cyan) from the MCELS survey, along with additional optical data from the DSS (white).

This composite image contains data from Chandra (purple) that provides evidence for the survival of a companion star from the blast of a supernova explosion. Chandra's X-rays reveal a point-like source in the supernova remnant at the location of a massive star. The data suggest that mass is being pulled away from the massive star towards a neutron star or a black hole companion. If confirmed, this would be only the third binary system containing both a massive star and a neutron star or black hole ever found in the aftermath of a supernova. This supernova remnant is found embedded in clouds of ionized hydrogen, which are shown in optical light (yellow and cyan) from the MCELS survey, along with additional optical data from the DSS (white).

This mosaic shows NASA's radar observations in one-minute increments of asteroid 2024 MK, a 500-foot-wide (150-meter-wide) near-Earth object, made June 30, 2024, a day after it passed our planet from a distance of only 184,00 miles (295,000 kilometers). The Deep Space Network's 230-foot (70-meter) Goldstone Solar System Radar, called Deep Space Station 14 (or DSS-14), was used to transmit radio frequency signals to the asteroid, and the 114-foot (34-meter) DSS-13 received the reflected signals. The result of this "bistatic" radar observation is a detailed image of the asteroid's surface, revealing concavities, ridges, and boulders about 30 feet (10 meters) wide. The observations were made just before 5:55 a.m. UTC June 30 (10:55 p.m. PDT June 29). The asteroid's close approach occurred at 13:49 UTC June 29 (6:49 a.m. PDT June 29). Close approaches of near-Earth objects the size of 2024 MK are relatively rare, occurring about every couple of decades, on average, so scientists at NASA's Jet Propulsion Laboratory in Southern California sought to gather as much data about the object as possible. The Goldstone Solar System Radar Group is supported by NASA's Near-Earth Object Observations Program within the Planetary Defense Coordination Office at the agency's headquarters in Washington. Managed by NASA's Jet Propulsion Laboratory, the Deep Space Network receives programmatic oversight from Space Communications and Navigation program office within the Space Operations Mission Directorate, also at NASA Headquarters. Animation available at https://photojournal.jpl.nasa.gov/catalog/PIA26383

On March 21, 2021, the large asteroid 2001 FO32 made a close approach with our planet, passing at a distance of about 1.25 million miles (2 million kilometers) — or 5 1/4 times the distance from Earth to the Moon. While there was no risk of the near-Earth asteroid colliding with Earth as its orbit is very well known, scientists at NASA's Jet Propulsion Laboratory in Southern California took the opportunity to capture these radar images of the asteroid as it tumbled past. Using NASA's 34-meter (111.5-feet) Deep Space Station 13 (DSS-13) radio antenna at the Deep Space Network's Goldstone Deep Space Communication Complex near Barstow, California, radio signals were transmitted to 2001 FO32. The signals then bounced off the surface of the asteroid and were received by the 100-meter (328-feet) Green Bank Telescope in West Virginia. Such radar observations can offer additional insight into the asteroid's orbit, provide a better estimate of its dimensions and rotation rate, and help glimpse surface features (like large boulders or craters). Other radar observations were carried out by scientists using the 34-meter DSS-43 antenna at the Deep Space Network's Canberra Deep Space Communication Complex in Australia. Along with the Commonwealth Scientific and Industrial Research Organisation's Australia Telescope Compact Array near Narrabri in New South Wales, both antennas worked together to track 2001 FO32. Asteroid 2001 FO32 was discovered in March 2001 by the Lincoln Near-Earth Asteroid Research (LINEAR) program in Socorro, New Mexico, and had been estimated, based on optical measurements, to be roughly 3,000 feet (1 kilometer) wide. In more recent follow-up observations by NEOWISE, 2001 FO32 appears to be faint when observed in infrared wavelengths, which suggests the object is likely less than 1 kilometer in diameter. Analysis by the NEOWISE team shows that it is between 1,300 to 2,230 feet (440 to 680 meters) wide. Further analysis of data from the radar campaign will better refine the size of the asteroid and increase the precision of its orbital calculations. For more information about 2001 FO32 and observing campaign, read: https://www.jpl.nasa.gov/news/asteroid-2001-fo32-will-safely-pass-by-earth-march-21 https://photojournal.jpl.nasa.gov/catalog/PIA24561

NASA image relase December 13, 2011 Gamma-rays detected by Fermi's LAT show that the remnant of Tycho's supernova shines in the highest-energy form of light. This portrait of the shattered star includes gamma rays (magenta), X-rays (yellow, green, and blue), infrared (red) and optical data. Credit: Gamma ray, NASA/DOE/Fermi LAT Collaboration; X-ray, NASA/CXC/SAO; Infrared, NASA/JPL-Caltech; Optical, MPIA, Calar Alto, O. Krause et al. and DSS To read more go to: <a href="http://www.nasa.gov/mission_pages/GLAST/news/tycho-star.html" rel="nofollow">www.nasa.gov/mission_pages/GLAST/news/tycho-star.html</a> <b><a href="http://www.nasa.gov/audience/formedia/features/MP_Photo_Guidelines.html" rel="nofollow">NASA image use policy.</a></b> <b><a href="http://www.nasa.gov/centers/goddard/home/index.html" rel="nofollow">NASA Goddard Space Flight Center</a></b> enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. <b>Follow us on <a href="http://twitter.com/NASA_GoddardPix" rel="nofollow">Twitter</a></b> <b>Like us on <a href="http://www.facebook.com/pages/Greenbelt-MD/NASA-Goddard/395013845897?ref=tsd" rel="nofollow">Facebook</a></b> <b>Find us on <a href="http://instagrid.me/nasagoddard/?vm=grid" rel="nofollow">Instagram</a></b>

This figure represents the 1,000th near-Earth asteroid (NEA) to be detected by planetary radar since 1968. Being only 65 to 100 feet (20 to 30 meters) wide, asteroid 2021 PJ1 was too small to be imaged in any detail, but the powerful 70-meter (230-foot) Deep Space Station 14 (DSS-14) antenna at the Deep Space Network's Goldstone Deep Space Complex near Barstow, California, was able to measure the Doppler frequency of the radio waves that reflected off the object's surface. The data was recorded for 16 minutes between 2:26 p.m. and 2:42 p.m. PDT on Aug. 14, 2021. The figure shows radar echo signal strength on the vertical axis versus Doppler frequency (in units of hertz, or Hz) on the horizontal axis. The strong spike at a value of minus 70 Hz is the reflected signal (or "echo") from 2021 PJ1; the other, smaller spikes are receiver noise, which is like the static on an AM radio if there aren't any nearby stations. Using this information, scientists at NASA's Jet Propulsion Laboratory in Southern California could more accurately calculate the asteroid's velocity, its distance from Earth and its future motion around the Sun. These observations used a prediction – known as an "ephemeris" – that had relatively large uncertainties because the asteroid had been discovered only a few days earlier. If the original prediction had been perfect, the radar echo would appear at zero Hz. The fact that the radar echo is at minus 70 Hz indicates a correction could be made to the predicted velocity of minus 2.7 miles per hour (minus 1.2 meters per second). This measurement also reduced the uncertainty in the asteroid's distance from Earth from 1,300 miles (2,100 kilometers) to 5.2 miles (8.3 kilometers) – a reduction of a factor of about 250. https://photojournal.jpl.nasa.gov/catalog/PIA24563

Release date: July 1, 2008 This image is a composite of visible (or optical), radio, and X-ray data of the full shell of the supernova remnant from SN 1006. The radio data show much of the extent that the X-ray image shows. In contrast, only a small linear filament in the northwest corner of the shell is visible in the optical data. The object has an angular size of roughly 30 arcminutes (0.5 degree, or about the size of the full moon), and a physical size of 60 light-years (18 parsecs) based on its distance of nearly 7,000 light-years. The small green box along the bright filament at the top of the image corresponds to the dimensions of the Hubble release image. The optical data was obtained at the University of Michigan's 0.9-meter Curtis Schmidt telescope at the National Science Foundation's Cerro Tololo Inter-American Observatory (CTIO) near La Serena, Chile. H-alpha, continuum-subtracted data were provided by F. Winkler (Middlebury COllege) et al. The X-ray data were acquired from the Chandra X-ray Observatory's AXAF CCD Imaging Spectrometer (ACIS) at 0.5-3keV, and were provided by J. Hughes (Rutgers University) et al. The radio data, supplied by K. Dyer (NRAO, Socorro) et al., were a composite from the National Radio Astronomy Observatory's Very Large Array (NRAO/VLA) in Socorro, New Mexico, along with the Green Bank Telescope (GBT) in Green Bank, West Virginia. Data of the supernova remnant were blended on a visible-light stellar background created using the Digitized Sky Survey's Anglo-Australian Observatory (AAO2) blue and red plates. Photo Credit: NASA, ESA, and Z. Levay (STScI) Science Credit: Radio: NRAO/AUI/NSF GBT+VLA 1.4 GHz mosaic (Dyer, Maddalena and Cornwell, NRAO); X-ray: NASA/CXC/Rutgers/G. Cassam-Chenai and J. Hughes et al.; Optical: F.Winkler/Middlebury College and NOAO/AURA/NSF; and DSS To learn more about the Hubble Space Telescope go here: <a href="http://www.nasa.gov/mission_pages/hubble/main/index.html" rel="nofollow">www.nasa.gov/mission_pages/hubble/main/index.html</a> <b><a href="http://www.nasa.gov/centers/goddard/home/index.html" rel="nofollow">NASA Goddard Space Flight Center</a></b> is home to the nation's largest organization of combined scientists, engineers and technologists that build spacecraft, instruments and new technology to study the Earth, the sun, our solar system, and the universe. <b>Follow us on <a href="http://twitter.com/NASAGoddardPix" rel="nofollow">Twitter</a></b> <b>Join us on <a href="http://www.facebook.com/pages/Greenbelt-MD/NASA-Goddard/395013845897?ref=tsd" rel="nofollow">Facebook</a><b> </b></b>

This new view of spiral galaxy IC 342, also known as Caldwell 5, includes data from NASA Nuclear Spectroscopic Telescope Array, or NuSTAR. IC 342 lies 7 million light-years away in the Camelopardalis constellation.

This new view of the historical supernova remnant Cassiopeia A, located 11,000 light-years away, was taken by NASA Nuclear Spectroscopic Telescope Array, or NuSTAR. While the star is long dead, its remains are still bursting with action.

The unique ultraviolet vision of NASA Galaxy Evolution Explorer revealed, for the first time, dwarf galaxies forming out of nothing more than pristine gas likely leftover from the early universe.

This sky map shows the location of the star HD 219134 (circle), host to the nearest confirmed rocky planet found to date outside of our solar system. The star lies just off the "W" shape of the constellation Cassiopeia and can be seen with the naked eye in dark skies. It actually has multiple planets, none of which are habitable. http://photojournal.jpl.nasa.gov/catalog/PIA19832

The Ghost of Mirach galaxy is shown in visible light on the left, and in ultraviolet as seen by NASA Galaxy Evolution Explorer on the right. The fields of view are identical in both pictures, with the Ghost of Mirach -— a galaxy called NGC 404.

Hidden behind a shroud of dust in the constellation Cygnus is a stellar nursery called DR21, which is giving birth to some of the most massive stars in our galaxy. Visible light images reveal no trace of this interstellar cauldron because of heavy dust obscuration. In fact, visible light is attenuated in DR21 by a factor of more than 10,000,000,000,000,000,000,000,000,000,000,000,000,000 (ten thousand trillion heptillion). New images from NASA's Spitzer Space Telescope allow us to peek behind the cosmic veil and pinpoint one of the most massive natal stars yet seen in our Milky Way galaxy. The never-before-seen star is 100,000 times as bright as the Sun. Also revealed for the first time is a powerful outflow of hot gas emanating from this star and bursting through a giant molecular cloud. The colorful image (top panel) is a large-scale composite mosaic assembled from data collected at a variety of different wavelengths. Views at visible wavelengths appear blue, near-infrared light is depicted as green, and mid-infrared data from the InfraRed Array Camera (IRAC) aboard NASA's Spitzer Space Telescope is portrayed as red. The result is a contrast between structures seen in visible light (blue) and those observed in the infrared (yellow and red). A quick glance shows that most of the action in this image is revealed to the unique eyes of Spitzer. The image covers an area about two times that of a full moon. Each of the constituent images is shown below the large mosaic. The Digital Sky Survey (DSS) image (lower left) provides a familiar view of deep space, with stars scattered around a dark field. The reddish hue is from gas heated by foreground stars in this region. This fluorescence fades away in the near-infrared Two-Micron All-Sky Survey (2MASS) image (lower center), but other features start to appear through the obscuring clouds of dust, now increasingly transparent. Many more stars are discerned in this image because near-infrared light pierces through some of the obscuration of the interstellar dust. Note that some stars seen as very bright in the visible image are muted in the near-infrared image, whereas other stars become more prominent. Embedded nebulae revealed in the Spitzer image are only hinted at in this picture. The Spitzer image (lower right) provides a vivid contrast to the other component images, revealing star-forming complexes and large-scale structures otherwise hidden from view. The Spitzer image is composed of photographs obtained at four wavelengths: 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange) and 8 microns (red). The brightest infrared cloud near the top center corresponds to DR21, which presumably contains a cluster of newly forming stars at a distance of nearly 10,000 light-years. The red filaments stretching across the Spitzer image denote the presence of polycyclic aromatic hydrocarbons. These organic molecules, comprised of carbon and hydrogen, are excited by surrounding interstellar radiation and become luminescent at wavelengths near 8 microns. The complex pattern of filaments is caused by an intricate combination of radiation pressure, gravity, and magnetic fields. The result is a tapestry in which winds, outflows, and turbulence move and shape the interstellar medium. http://photojournal.jpl.nasa.gov/catalog/PIA05735

This image composite shows two views of a puffy, dying star, or planetary nebula, known as NGC 1514. At left is a view from a ground-based, visible-light telescope; the view on the right shows the object in infrared light from NASA WISE telescope.

This image highlights the hidden spiral arms blue that were discovered around the nearby galaxy NGC 4625 by the ultraviolet eyes of NASA Galaxy Evolution Explorer.

This visible-light view from from NASA Spitzer Space Telescope highlights the bright M17 nebula, as well as the glowing hot gas filling the bubble to its left.

This new composite image of stellar cluster NGC 1333 combines X-rays from NASA's Chandra X-ray Observatory (pink); infrared data from NASA's Spitzer Space Telescope (red); and optical data from the Digitized Sky Survey and the National Optical Astronomical Observatories' Mayall 4-meter telescope on Kitt Peak near Tucson, Arizona. The Chandra data reveal 95 young stars glowing in X-ray light, 41 of which had not been seen previously using Spitzer because they lacked infrared emission from a surrounding disk. http://photojournal.jpl.nasa.gov/catalog/PIA19347

NASA Galaxy Evolution Explorer discovered an exceptionally long comet-like tail of material trailing behind Mira -- a star that has been studied thoroughly for about 400 years.

NASA Spitzer Space Telescope caught a glimpse of the Cepheus constellation, thirty thousand light-years away; astronomers think theyve found a massive star whose death barely made a peep.

This composite of the giant barred spiral galaxy NGC 6872 is 522,000 light-years across, making it about five times the size of the Milky Way.

This composite image is of spiral galaxy M106 NGC 4258; optical data from the Digitized Sky Survey is yellow, radio data from the Very Large Array is purple, X-ray data from Chandra is blue, and infrared data from the Spitzer Space Telescope is red.

This majestic false-color image from NASA's Spitzer Space Telescope shows the "mountains" where stars are born. Dubbed "Mountains of Creation" by Spitzer scientists, these towering pillars of cool gas and dust are illuminated at their tips with light from warm embryonic stars. The new infrared picture is reminiscent of Hubble's iconic visible-light image of the Eagle Nebula, which also features a star-forming region, or nebula, that is being sculpted into pillars by radiation and winds from hot, massive stars. The pillars in the Spitzer image are part of a region called W5, in the Cassiopeia constellation 7,000 light-years away and 50 light-years across. They are more than 10 times in the size of those in the Eagle Nebula (shown to scale here). The Spitzer's view differs from Hubble's because infrared light penetrates dust, whereas visible light is blocked by it. In the Spitzer image, hundreds of forming stars (white/yellow) can seen for the first time inside the central pillar, and dozens inside the tall pillar to the left. Scientists believe these star clusters were triggered into existence by radiation and winds from an "initiator" star more than 10 times the mass of our Sun. This star is not pictured, but the finger-like pillars "point" toward its location above the image frame. The Spitzer picture also reveals stars (blue) a bit older than the ones in the pillar tips in the evacuated areas between the clouds. Scientists believe these stars were born around the same time as the massive initiator star not pictured. A third group of young stars occupies the bright area below the central pillar. It is not known whether these stars formed in a related or separate event. Some of the blue dots are foreground stars that are not members of this nebula. The red color in the Spitzer image represents organic molecules known as polycyclic aromatic hydrocarbons. These building blocks of life are often found in star-forming clouds of gas and dust. Like small dust grains, they are heated by the light from the young stars, then emit energy in infrared wavelengths. This image was taken by the infrared array camera on Spitzer. It is a 4-color composite of infrared light, showing emissions from wavelengths of 3.6 microns (blue), 4.5 microns (green), 5.8 microns (orange), and 8.0 microns (red). http://photojournal.jpl.nasa.gov/catalog/PIA03096