Posted on by Fraser Cain

Gemini Builds Animation of Galactic Core

Image credit: Gemini

The Gemini Observatory located on top of Hawaii’s Mauna Kea has been used to create an animation of the action going on in galaxy NGC 1068. Using a tool called the Integral Field Unit, astronomers have been able to create a 3-dimensional animation of the tremendous jet emanating from the supermassive black hole as it slams into the galactic gas disk.

Astronomers observing with the Gemini North Telescope on Hawaii’s Mauna Kea have a powerful new tool to probe mysterious cosmic caldrons like those at the cores of galaxies and stellar nurseries.

Using the recently commissioned Integral Field Unit (IFU) on the Gemini Multi-Object Spectrograph (GMOS), astronomers at the observatory have recently obtained a complete multi-dimensional picture of the dynamic flow of gas and stars at the core of an active galaxy named NGC 1068 in a single snap-shot. The resulting windfall of data has been transformed into an animation that dramatically reveals the internal gyrations of the galaxy – including the interactions of a pair of galactic-scale jets that spew material for thousands of light years away from the suspected black hole at the galaxy’s core.

“The Gemini data of NGC 1068 reveal one of the lesser know features of galaxy jets,” explains Gemini North Associate Director Dr. Jean-Ren? Roy. “For the first time we were able to clearly see the jet’s expanding lobe as its hypersonic bow shock slams directly into the underlying gas disk of the galaxy. It’s like a huge wave smashing onto a galactic shoreline.”

Dr. Gerald Cecil of the University of North Carolina, recently led an international team to study this particular galaxy using spectra taken with the Hubble Space Telescope and believes that the new Gemini spectra will clarify many patterns revealed by Hubble. “Large ground-based telescopes like Gemini are the perfect complement to Hubble because they can collect so much more light. But it’s critical to use all this light cunningly, and not throw most of it away as standard slit spectrographs do. The GMOS’s integral field capability now enables detailed studies of fundamental physical processes that were previously too time consuming to conduct on faint cosmic sources.” The Hubble findings by Dr. Cecil et al. will appear in the April 1, 2002 issue of the Astrophysical Journal.

“By using Integral Field Spectroscopy we add dimensions to the data and can essentially make a movie with one click of the shutter,” says Dr. Bryan Miller, the Gemini instrument scientist for IFUs. “When we play back our movie of the galaxy NGC1068, we see a 3-dimensional view of the core of this galaxy. It is striking how much easier it is to interpret features with this kind of data. With integral-field data we can determine the mass distributions, the true shapes, and the histories of galaxies more accurately than before.” The Integral Field Spectroscopy findings by Dr. Miller et al. will appear in the Conference Series of the Astronomical Society of the Pacific.

This technology is new to the world of 8-10 meter class telescopes and is especially powerful on new generation telescopes like Gemini that use the latest optical technologies to focus starlight to razor sharpness. “We are very excited by these results and the superb capabilities that the integral field unit has given the GMOS in Hawaii”, notes Dr. Jeremy Allington-Smith, the scientist from the University of Durham in the United Kingdom who managed the construction of the GMOS Integral Field Unit. “In effect we have added an extra dimension to the instrument so that it can map the motion of gas and stars at any point in the image of the object under study. The GMOS IFU will be a powerful new tool for studying the centers of active galaxies that may harbor black holes, as well as the dynamic internal motions of galaxies and star forming regions.” The GMOS IFU findings by Dr. Allington-Smith et al. will appear in the Conference Series of the Astronomical Society of the Pacific.

An Integral Field Unit (IFU) like the one used in the GMOS uses hundreds of tiny optical fibers (each thinner than an human hair) with tiny micro-lenses attached to guide light from the telescope’s 2-D image to a spectrograph. The spectrograph produces one individual spectrum for each fiber for a total of 1500 individual spectra that can each reveal details of the physical conditions and velocity of the gas, dust and stars it studies. This system was the first IFU to be installed on the new generation of 8 and 10m telescopes when it was commissioned on the Gemini-North telescope in 2001.

The Integral Field Spectroscopy capabilities of the Gemini Observatory are still developing. Within the next two years both telescopes will have optical and near-infrared integral field units. Some of these systems will work with adaptive optics to provide the highest spatial resolution images deliverable by the telescopes, including images in the infrared that will be sharper than can be produced by the Hubble Space Telescope at those wavelengths.

The Gemini Observatory is an international collaboration that has built two identical 8-meter telescopes. The telescopes are located at Mauna Kea, Hawaii (Gemini North) and Cerro Pach?n in central Chile (Gemini South), and hence provide full coverage of both hemispheres of the sky. Both telescopes incorporate new technologies that allow large, relatively thin mirrors under active control to collect and focus both optical and infrared radiation from space. Gemini North began science operations in 2000 and Gemini South began scientific operations in late 2001.

The Gemini Observatory provides the astronomical communities in each partner country with state-of-the-art astronomical facilities that allocate observing time in proportion to each country’s contribution. In addition to financial support, each country also contributes significant scientific and technical resources. The national research agencies that form the Gemini partnership include: the US National Science Foundation (NSF), the UK Particle Physics and Astronomy Research Council (PPARC), the Canadian National Research Council (NRC), the Chilean Comisi?n Nacional de Investigaci?n Cientifica y Tecnol?gica (CONICYT), the Australian Research Council (ARC), the Argentinean Consejo Nacional de Investigaciones Cient?ficas y T?cnicas (CONICET) and the Brazilian Conselho Nacional de Desenvolvimento Cient?fico e Tecnol?gico (CNPq). The Observatory is managed by the Association of Universities for Research in Astronomy, Inc. (AURA) under a cooperative agreement with the NSF. The NSF also serves as the executive agency for the international partnership.

Original Source: Gemini News Release

Posted on by Fraser Cain

NASA Showcases its Airbag System

Image credit: NASA

It was a bit of a rough ride, but Pathfinder arrived on the surface of Mars back in 1997 in perfect condition. It was the innovative (and unproven) airbag system that helped slow the lander’s descent, so NASA is planning to employ the system again for the 2003 Mars Exploration Rover missions. These rovers have a different mass than Pathfinder, so NASA engineers have gone back to the drawing board to figure out how to make airbags that inflate seconds before touchdown and can withstand an impact at freeway speeds.

Just one of the many problems in landing on another planet, after it’s been determined where to land and the method to get there, is landing safely. For JPL, a safe landing is “the name of the game,” as engineers work to prepare two rovers for the journey to Mars.

The Mars Exploration Rovers scheduled for launch in 2003 are using the same type airbag landing system that Mars Pathfinder used in 1997. The airbags must be strong enough to cushion the spacecraft if it lands on rocks or rough terrain and allow it to bounce across Mars’ surface at freeway speeds after landing. To add to the complexity, the airbags must be inflated seconds before touchdown and deflated once safely on the ground.

“The 2003 rovers have a different mass [than Sojourner, the Pathfinder rover], so we’ve made changes in the airbag design,” said John Carson, cognizant engineer. “Our requirement is to be able to land safely on a rock extending about a half-meter (about 18 inches) above the surface. Extensive testing gives us a process for trial and error before the final design.”

How to Build a Better Airbag
While most new automobiles now come with airbags, spacecraft don’t. The fabric being used for the new Mars airbags is a synthetic material called Vectran that was also used on Mars Pathfinder. Vectran has almost twice the strength of other synthetic materials, such as Kevlar, and performs better at cold temperatures.

Denier is a term that measures the diameter of the thread used in the product. There will be six 100-denier layers of the light but tough Vectran protecting one or two inner bladders of the same material in 200-denier, according to Dara Sabahi, mechanical systems architect. Using the 100-denier means there is more actual fabric in the outer layers where it is needed, because there are more threads in the weave.

Each rover uses four airbags with six lobes each, which are all connected. Connection is important, since it helps abate some of the landing forces by keeping the bag system flexible and responsive to ground pressure. The fabric of the airbags is not attached directly to the rover; ropes that crisscross the bags hold the fabric to the rover. The ropes give the bags shape, which makes inflation easier. While in flight, the bags are stowed along with three gas generators that are used for inflation.

Testing, Testing, Testing
Since the airbags are composed of many layers, some tearing in the outer layers is acceptable and even expected. Engineers test the bags to make sure there will be no catastrophic problems that would prevent a safe landing.

Mars airbag testing is done in world’s largest vacuum chamber at the Plum Brook Station of NASA’s Glenn Research Center in Ohio. “The Plum Brook facility is pretty impressive, along with all the people who operate it,” said Carson.

The test chamber used for the tests is a little over 30 meters (100 feet) across and about 37 meters (120 feet) high — big enough that three railroad tracks go through it. A test spacecraft and airbag system weighing about 535 kilograms (about 1,180 pounds) are accelerated with a bungee cord system onto a platform with rocks that approximate the Mars surface. The drop is at landing speed, about 20 to 24 meters (yards) per second.

Tests are documented thoroughly with high-speed and video cameras, in addition to visual inspections. Engineers even built a clear dome, studded with rocks, that has a camera that documents tests from a rock’s-eye view. During testing, a crew from ILC Dover, the airbag’s manufacturer, stands by to make quick repairs and to note any changes required.

“We do extensive testing,” said Tom Rivellini, deputy mechanical systems architect. “We want to break the bag on Earth, not on Mars. If we see a tear that is unexpected or goes too deep, we can make changes now [before the final design].”

Carson added, “We’ll go over all the data we’ve accumulated so far, do some more testing, and decide on a design configuration.”

And then on to Mars in 2003!

Posted on by Fraser Cain

Galileo Navigation System is a Go

European transport ministers have approved a plan to develop Galileo, a satellite navigation system. Galileo, which is due to come online in 2008, is expected to cost $3.15 billion US and will consist of 30 satellites deployed in three circular Medium Earth Orbits at an altitude of 23,616 km. Although the system will compete with the US-built Global Positioning System, the designers say the two networks will be compatible and provide redundancy.

Posted on by Fraser Cain

Hubble Reveals Blue Galaxy Ablaze with Star Formation

A new photo released from the Hubble Space Telescope shows how galaxy NGC 7673 is teeming with hot star nurseries. Located 150 million light years away in the constellation of Pegasus, each cluster in this new photograph contains thousands of infant stars burning at incredibly high temperatures. Astronomers aren’t sure why this galaxy is so active, but it could be because the galaxy collided with another millions of years ago.

Posted on by Fraser Cain

NASA Classifies Shuttle Launch Times

NASA officials have decided to keep the exact time of launch of the next space shuttle a secret until 24 hours before liftoff to guard against terrorist attack. So, the launch of the space shuttle Atlantis, on a mission to continue assembly of the International Space Station, will occur at some point on the afternoon of April 4th.

Posted on by Fraser Cain

New Evidence of the Universe’s Expansion

A team of UK and Australian astronomers have come up with independent evidence that the expansion of the universe is accelerating. Three years ago astronomers stunned the scientific community when they announced their evidence of an accelerating universe (they calculated the velocity of supernovas in distant galaxies). This team came to the same conclusion after measuring the position of 250,000 galaxies and plotted their movement compared it to the structure of the early universe.

Posted on by Fraser Cain

Asteroid Discovered After a Near Miss

Astronomers discovered a new asteroid, four days after it made a near miss of the Earth. The object, now called 2002 EM7, was between 40 and 80 metres across and missed the planet by a distance of only 480,200 kilometres – the 9th-closest brush ever recorded; roughly the distance from the Earth to the moon. Had it actually hit the Earth, it could have flattened a city and caused thousands of deaths.

Posted on by Fraser Cain

Six Telescopes Acting as One

Image credit: USNO

Astronomers from several US observatories announced that they have successfully merged the light from six independent telescopes to form a single, high-resolution image of a distant multi-star system. To create an image with this level of detail, a single telescope would need to be 50-metres across – bigger than anything that currently exists. This technique, called interferometry, has been done with pairs of telescopes before, but never with as many as six.

Astronomers from the U.S. Naval Observatory (USNO), the Naval Research Laboratory (NRL), and Lowell Observatory announced today that they have successfully combined the light from six independent telescopes to form a single, high-resolution image of a distant multiple-star system. This is the first time that this has ever been accomplished in the optical region of the electromagnetic spectrum. The Navy Prototype Optical Interferometer (NPOI) at Lowell Observatory’s Anderson Mesa site near Flagstaff, Arizona observed the triple star system Eta Virginis, located about 130 light-years away from Earth.

“This development makes it possible to ‘synthesize’ telescopes with apertures in excess of hundreds of meters,” says Dr. Kenneth Johnston, Scientific Director of the Naval Observatory. “It will lead to the direct imaging of the surfaces of stars and of star spots, analogous to the sunspots on the Sun. This technology can also be applied to space systems for remote sensing of the Earth and other objects in the solar system, as well as stars and galaxies.”

Optical interferometers combine the light from several independent telescopes to form a “synthetic” telescope whose ability to make a high-resolution image is proportional to the maximum separation of the telescopes. They are the answer to the prohibitive costs and immense technical difficulties of building extremely large, monolithic single-mirror telescopes. Since the rate at which a giant telescope aperture is synthesized with an interferometer array is equal to the number of combinations between any two telescopes of the array, the combination of the six NPOI telescopes has more than quadrupled NPOI’s capability to collect data over its competitors.

USNO and NRL, in collaboration with Lowell Observatory and with funding from the Office of Naval Research and the Oceanographer of the Navy, joined forces in 1991 to build the instrument. Stellar observations have been conducted with a three-station array since its “first light” in 1996.

However, due to the technical difficulty associated with linking even a small number of separate telescopes, the high-resolution capabilities of optical interferometers have only been used to date on relatively simple stellar sources. Basic questions, such as a star’s apparent diameter or the existence and motions of nearby stellar companions, are easily answered for such sources. However, to increase the spatial resolution and sensitivity to stellar structure, interferometers must link more telescopes together to provide an even sampling of the synthesized aperture. Three combined telescopes provide three mea-surements in the synthesized aperture, but six telescopes provide 15 combinations.

To merge the six beams, the NPOI team has designed a new type of hybrid beam combiner. In addition, new hardware and control systems have been developed to uniquely encode every possible telescope combination in the recorded data so that the information necessary for the alignment and superposition of the starlight wave-fronts and the image reconstruction may be properly decoded.

The field of interferometry is a rapidly developing one, with giants like the twin Keck 10-meter telescopes having achieved “first fringes” last year, and the European Southern Observatory’s VLTI planning to combine the light from four 8-meter telescopes. More modest but versatile imaging interferometers like CHARA, COAST, and IOTA have also been operating for a few years, but NPOI is the first to combine light from a full array of six telescopes.

In the near future, NPOI will be commissioning all of the remaining stations onto which any of the six telescopes can be mounted for a maximum array size of 430 meters, the largest baseline of all current imaging interferometer projects.

Stellar astrophysics will be revolutionized by the capability to directly image stars other than the Sun. Ultimately, when employed in space with the experience collected from ground-based experiments, optical interferometry may develop the capability to image Jupiter-sized planets orbiting distant stars.

“Remember the early days of radio interferometry and look at the world- wide arrays we routinely use today,” says Dr. Johnston. “We’ve gone from simple two-element arrays to continent-sized ones with 10 or more antennas that produce extremely fine-scale images of distant quasars. We are standing on the brink of achieving similar results for visible-light sources.”

Original Source: US Naval Observatory News Release

Posted on by Fraser Cain

Grace Satellites Launched

Image credit: NASA

NASA and the German Center for Air and Space Flight successfully launched the Gravity Recovery and Climate Experiment, or “Grace” today. The twin-satellite mission lifted off on Sunday from Russia’s Plesetsk Cosmodrome on board a Rockot launch vehicle. Once in their final orbit, the satellites will separate to a distance of 220km apart, and will begin producing a high-definition gravity map of the Earth’s surface to help scientists understand some of the factors that affect climate change.

NASA and the German Center for Air and Space Flight today successfully launched the Gravity Recovery and Climate Experiment, or “Grace,” mission into Earth orbit at 1:21:27 a.m. Pacific time from Russia’s Plesetsk Cosmodrome. The mission, comprised of identical twin satellites, will precisely measure Earth’s shifting water masses and map their effects on Earth’s gravity field.

The five-year Grace mission-the first launch of NASA’s Earth System Science Pathfinder program-will be a scientific boon to researchers who study Earth with space-based instruments. The monthly gravity maps generated by Grace will be up to 1,000 times more accurate than those currently in use, substantially improving the accuracy of many techniques used by oceanographers, hydrologists, glaciologists, geologists and other scientists to study phenomena that influence climate. These phenomena range from shallow and deep ocean currents, water movement on and beneath Earth’s surface, and the movement and changing mass of ice sheets, to sea-level heights, sea-level rise and changes in the structure of the solid Earth.

Under partly cloudy, cold skies, the Grace twins lifted off on a Russian Rockot launch vehicle. Riding over 1,500,000 newtons (approximately 350,000 pounds) of thrust, the rocket headed northward over the Arctic Ocean and Alaska, then south across the Pacific Ocean and Antarctica before heading north again over Africa and Europe. At 85 minutes, 38 seconds into the mission-or 2:47 a.m. Pacific time-the satellites separated from the launch vehicle’s third stage above Africa into a polar orbit 500 kilometers (311 miles) above Earth.

Ground controllers successfully acquired the spacecraft’s signal from the German Space Operations Center’s ground tracking station in Weilheim, Germany at 2:49 a.m. Pacific time. Initial telemetry reports received by the Grace team show both satellites to be in excellent health.

Following separation, the leading Grace satellite began pulling away from the trailing satellite at a relative speed of about 0.5 meters (1.6 feet) per second. Over the course of the next four days, the satellites will be spaced 220 kilometers (137 miles) apart- a little more than the distance between Los Angeles and San Diego.

As they race around the globe 16 times a day, the satellites will sense minute variations in Earth’s surface mass below and corresponding variations in Earth’s gravitational pull. Regions of slightly stronger gravity will affect the lead satellite first, pulling it slightly away from the trailing satellite. By measuring the constantly changing distance between the two satellites using an extremely sensitive microwave ranging system and combining that data with precise positioning measurements from Global Positioning System instruments, scientists will be able to construct a precise Earth gravity map.

During the next two and a half weeks, basic satellite operations will be established. During a subsequent three-week commissioning phase, Grace’s science instruments and supporting systems will be powered up, evaluated and calibrated. The performance of the Grace system for measuring Earth gravity will then be validated over the following six months. The mission then enters its observational phase, during which routine operational data products will be made available to scientists.

Additional information about the Grace program is available on the Internet at:

http://www.csr.utexas.edu/grace .

Grace is a joint partnership between NASA and the German Center for Air and Space Flight (Deutsches Zentrum fur Luft und Rumfahrt, or DLR). NASA’s Jet Propulsion Laboratory, Pasadena, Calif., manages the U.S. portion of the project for NASA’s Office of Earth Science, Washington. Science data processing, distribution, archiving and product verification are managed under a cooperative arrangement between JPL and the University of Texas’ Austin-based Center for Space Research in the United States and Germany’s Earth Research Center (or GeoForschungsZentrum).

JPL is a division of the California Institute of Technology in Pasadena.

Original Source: NASA/JPL News Release

Posted on by Fraser Cain

Tightest Binary System Discovered

Image credit: ESO

Astronomers have discovered a pair of white dwarf stars that revolve around each other at a distance of only 80,000km (1/5th the distance between the Earth and the Moon) – the closest binary system ever discovered. The system, known as RX J0806.3+1527, was investigated with the European Southern Observatory’s Very Large Telescope (VLT), and observers noticed that the object dimmed once every five minutes suggesting a binary system.

Observations with ESO’s Very Large Telescope (VLT) in Chile and the Italian Telescopio Nazionale Galileo (TNG) on the Canary Islands during the past two years have enabled an international group of astronomers [1] to unravel the true nature of an exceptional binary stellar system.

This system, designated RX J0806.3+1527, was first discovered as an X-ray source of variable brightness – once every five minutes, it “switches off” for a short moment. The new observations have shown beyond doubt that this period reflects the orbital motion of two “white dwarf” stars that revolve around each other at a distance of only 80,000 km. Each of the stars is about as large as the Earth and this is the shortest orbital period known for any binary stellar system.

The VLT spectrum displays lines of ionized helium, indicating that the presence of an exceedingly hot area on one of the stars – a “hot spot” with a temperature of approx. 250,000 degrees. The system is currently in a rarely seen, transitory evolutionary state.

An amazing stellar binary system
One year is the time it takes the Earth to move once around the Sun, our central star. This may seem quite fast when measured on the scale of the Universe, but this is a snail’s motion compared to the the speed of two recently discovered stars. They revolve around each other 100,000 times faster; one full revolution takes only 321 seconds, or a little more than 5 minutes! It is the shortest period ever observed in a binary stellar system.

This is the surprising conclusion reached by an international team of astronomers led by GianLuca Israel of the Astronomical Observatory of Rome [1], and based on detailed observations of the faint light from these two stars with some of the world’s most advanced telescopes. The record-holding binary stellar system bears the prosaic name RX J0806.3+1527 and it is located north of the celestial equator in the constellation Cancer (The Crab).

The scientists also find that the two partners in this hectic dance are most likely a dying white dwarf star, trapped in the strong gravitational grip of another, somewhat heavier star of the same exotic type. The two Earth-size stars are separated by only 80,000 kilometers, a little more than twice the altitude of the TV-broadcasting satellites in orbit around the Earth, or just one fifth of the distance to the Moon.

The orbital motion is very fast indeed – over 1,000 km/sec, and the lighter star apparently always turns the same hemisphere towards its companion, just as the Moon in its orbit around Earth. Thus, that star also makes one full turn around its axis in only 5 minutes, i.e. its “day” is exactly as long as its “year”.

The discovery of RX J0806.3+1527
The visible light emitted by this unusual system is very faint, but it radiates comparatively strong X-rays. It was due to this emission that it was first detected as a celestial X-ray source of unknown origin by the German ROSAT space observatory in 1994. Later it was found to be a periodically variable source [2]. Once every 5 minutes, the X-ray radiation disappears for a couple of minutes. It was recently studied in greater detail by the NASA Chandra observatory.

The position of the X-ray source in the sky was localised with sufficient accuracy to reveal a very faint visible-light emitting object in the same direction, over one million times weaker than the faintest star that can be seen by unaided eye (V-magnitude 21.1). Follow-up observations were carried out with several world class telescopes, including the ESO Very Large Telescope (VLT) at the Paranal Observatory in Chile, and also the Telescopio Nazionale Galileo (TNG), the Italian 4-m class observatory at the Roche de Muchachos Observatory on La Palma in the Canary Islands.

The nature of RX J0806.3+1527
The observations in visible light also showed the same effect: RX J0806.3+1527 was getting dimmer once every 5 minutes, while no other periodic modulation was seen. By observing the spectrum of this faint object with the FORS1 multi-mode instrument on the 8.2-m VLT ANTU telescope, the astronomers were able to determine the composition of RX J0806.3+1527. It was found to contain large amounts of helium; this is unlike most other stars, which are mainly made up of hydrogen.

“At the outset, we thought that this was just another of the usual binary systems that emit X-rays”, says Gianluca Israel. “None of us could imagine the real nature of this object. We finally solved the puzzle by eliminating all other possibilities one by one, while we kept collecting more data. As the famous detective said: when you have eliminated the impossible, whatever remains, however improbable, must be the truth!”.

Current theory predicts that the two stars, which are bound together by gravity in this tight system, produce X rays when one of them acts as a giant “vacuum cleaner”, drawing gas off its companion. That star has already lost a significant fraction of its mass during this process.

The incoming matter impacts at high speed on the surface of the other star and the corresponding area – a “hot spot” – is heated to some 250,000 ?C, whereby X rays are emitted. This radiation disappears for a short time during each orbital revolution when this area is on the far side of the accreting star, as seen from the Earth.

A very rare class of stars
Our Sun is a normal star of comparatively low mass and it will eventually develop into a white dwarf star. Contrary to the violent demise of heavier stars in a glorious supernova explosion, this is a comparatively “quiet” process during which the star slowly cools while losing energy. It shrinks until it finally becomes as small as the Earth.

The Sun is a single star. However when a solar-like star is a member of a binary system, the evolution of its component stars is more complicated. During an initial phase, one star continues to move along an orbit that is actually inside the outer, very tenuous atmospheric layers of its companion. Then the system rids itself of this matter and develops into a binary system with two orbiting white dwarf stars, like RX J0806.3+1527.

Systems in which the orbital period is very short (less than 1 hour) are referred to as AM Canis Venaticorum (AM CVn) systems, after first known binary star of this rare class. It is likely that such systems, after having reached a minimum orbital period of a few minutes, then begin to evolve towards longer orbital periods. This indicates that RX J0806.3+1527 is now at the very beginning of the “AM CVn phase”.

Gravitational waves
With its extremely short orbital period, RX J0806.3+1527 is also a prime candidate for the detection of the elusive gravitational waves, predicted by Einstein’s General Theory of Relativity. They have never been measured directly, but their existence has been revealed indirectly in binary neutron star systems.

A planned gravitational wave space experiment, the European Space Agency’s Laser Interferometer Space Antenna (LISA) that will be launched in about 10 years’ time, will be sufficiently sensitive to be able to reveal this radiation from RX J0806.3+1527 with a high degree of confidence. Such an observational feat would open an entirely new window on the universe.

Original Source: ESO News Release