mardi 8 janvier 2013

Galaxy's Gamma-Ray Flares Erupted Far From its Black Hole











NASA - Fermi Space Telescope logo.

Jan. 8, 2013

In 2011, a months-long blast of energy launched by an enormous black hole almost 11 billion years ago swept past Earth. Using a combination of data from NASA's Fermi Gamma-ray Space Telescope and the National Science Foundation's Very Long Baseline Array (VLBA), the world's largest radio telescope, astronomers have zeroed in on the source of this ancient outburst.

Theorists expect gamma-ray outbursts occur only in close proximity to a galaxy's central black hole, the powerhouse ultimately responsible for the activity. A few rare observations suggested this is not the case.

The 2011 flares from a galaxy known as 4C +71.07 now give astronomers the clearest and most distant evidence that the theory still needs some work. The gamma-ray emission originated about 70 light-years away from the galaxy's central black hole.


Prior to its strong outbursts in 2011, blazar 4C +71.07 was a weak source for Fermi’s LAT. These images centered on 4C +71.07 show the rate at which the LAT detected gamma rays with energies above 100 million electron volts; lighter colors equal higher rates. The image at left covers 2.5 years, from the start of Fermi’s mission to 2011. The image at right shows 10 weeks of activity in late 2011, when 4C +71.07 produced its strongest outburst. A more frequently active blazar, S5 0716+71, appears in both images. Credit: NASA/DOE/Fermi LAT Collaboration.

The 4C +71.07 galaxy was discovered as a source of strong radio emission in the 1960s. NASA's Compton Gamma-Ray Observatory, which operated in the 1990s, detected high-energy flares, but the galaxy was quiet during Fermi's first two and a half years in orbit.

In early November 2011, at the height of the outburst, the galaxy was more than 10,000 times brighter than the combined luminosity of all of the stars in our Milky Way galaxy.

"This renewed activity came after a long slumber, and that's important because it allows us to explicitly link the gamma-ray flares to the rising emission observed by radio telescopes," said David Thompson, a Fermi deputy project scientist at NASA's Goddard Space Flight Center in Greenbelt, Md.

Located in the constellation Ursa Major, 4C +71.07 is so far away that its light takes 10.6 billion years to reach Earth. Astronomers are seeing this galaxy as it existed when the universe was less than one-fourth of its present age.

At the galaxy's core lies a supersized black hole weighing 2.6 billion times the sun's mass. Some of the matter falling toward the black hole becomes accelerated outward at almost the speed of light, creating dual particle jets blasting in opposite directions. One jet happens to point almost directly toward Earth. This characteristic makes 4C +71.07 a blazar, a classification that includes some of the brightest gamma-ray sources in the sky.


The Very Long Baseline Array is a system of ten radio telescopes spanning 5,500 miles that work together as the world's largest dedicated astronomical instrument. Each station consists of an 82-foot-diameter, 240-ton dish antenna and an adjacent control building. Credit: NASA's Goddard Space Flight Center.

Boston University astronomers Alan Marscher and Svetlana Jorstad routinely monitor 4C +71.07 along with dozens of other blazars using several facilities, including the VLBA.

The instrument's 10 radio telescopes span North America, from Hawaii to St. Croix in the U.S. Virgin Islands, and possess the resolving power of a single radio dish more than 5,300 miles across when their signals are combined. As a result, The VLBA resolves detail about a million times smaller than Fermi's Large Area Telescope (LAT) and 1,000 times smaller than NASA's Hubble Space Telescope.

In autumn 2011, the VLBA images revealed a bright knot that appeared to move outward at a speed 20 times faster than light.

"Although this apparent speed was an illusion caused by actual motion almost directly toward us at 99.87 percent the speed of light, this knot was the key to determining the location where the gamma-rays were produced in the black hole's jet," said Marscher, who presented the findings Monday, Jan. 7, at the American Astronomical Society meeting in Long Beach, Calif.

VLBA and Fermi provided complementary observations of the blazar outburst

Top: During the most intense episode of gamma-ray flaring, VLBA radio maps and polarization measurements, among other observations, linked a bright knot in the jet of 4C +71.07 to variations in brightness in visible and gamma-ray light. The knot appeared to move outward at 20 times the speed of light, an illusion caused by motion almost directly toward us at 99.87 percent the speed of light.

Bottom: The rise and fall of the blazar's gamma-ray brightness as recorded by Fermi's LAT in late 2011 and early 2012. Credit: NASA's Goddard Space Flight Center/A. Marscher and S.Jorstad (BU).

The knot passed through a bright stationary feature of the jet, which the astronomers refer to as its radio "core," on April 9, 2011. This occurred within days of Fermi's detection of renewed gamma-ray flaring in the blazar. Marscher and Jorstad noted that the blazar brightened at visible wavelengths in step with the higher-energy emission.

During the most intense period of flaring, from October 2011 to January 2012, the scientists found the polarization direction of the blazar's visible light rotated in the same manner as radio emissions from the knot. They concluded the knot was responsible for the visible and the gamma-ray light, which varied in sync.

This association allowed the researchers to pinpoint the location of the gamma-ray outburst to about 70 light-years from the black hole.

The astronomers think that the gamma rays were produced when electrons moving near the speed of light within the jet collided with visible and infrared light originating outside of the jet. Such a collision can kick the light up to much higher energies, a process known as inverse-Compton scattering.

Fermi Space Telescope

The source of the lower-energy light is unclear at the moment. The researchers speculate the source may be an outer, slow-moving sheath that surrounds the jet. Nicholas MacDonald, a graduate student at Boston University, is investigating how the gamma-ray brightness should change in this scenario to compare with observations. "The VLBA is the only instrument that can bring us images from so near the edge of a young supermassive black hole, and Fermi's LAT is the only instrument that can see the highest-energy light from the galaxy's jet," said Jorstad.

NASA's Fermi Gamma-ray Space Telescope is an astrophysics and particle physics partnership. Fermi is managed by NASA's Goddard Space Flight Center. It was developed in collaboration with the U.S. Department of Energy, with contributions from academic institutions and partners in France, Germany, Italy, Japan, Sweden and the United States.

The VLBA is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

Related Links:

"Active Galaxies Flare and Fade in Fermi Telescope All-Sky Movie" (04.03.09): http://www.nasa.gov/mission_pages/GLAST/news/flare_fade.html

"NASA's Fermi Mission, Namibia's HESS Telescopes Explore a Blazar" (03.18.09): http://www.nasa.gov/mission_pages/GLAST/news/blazar.html

Active Galaxies and Quasars on NASA's "Imagine the Universe!": http://imagine.gsfc.nasa.gov/docs/science/know_l1/active_galaxies.html

The Very Long Baseline Array (VLBA): http://www.nrao.edu/index.php/about/facilities/vlba

Images, Text, Credits: NASA / J. D. Harrington / Goddard Space Flight Center / Francis Reddy / Lynn Chandler.

Cheers, Orbiter.ch

NASA's NuSTAR Catches Black Holes in Galaxy Web












NASA - NuSTAR Mission patch.

Jan. 8, 2013


This new view of spiral galaxy IC 342, also known as Caldwell 5, includes data from NASA's Nuclear Spectroscopic Telescope Array, or NuSTAR. Image credit: NASA/JPL-Caltech/DSS.

NASA's Nuclear Spectroscopic Telescope Array, or NuSTAR, set its X-ray eyes on a spiral galaxy and caught the brilliant glow of two black holes lurking inside.

The new image is being released Monday along with NuSTAR's view of the supernova remnant Cassiopeia A, at the American Astronomical Society meeting in Long Beach, Calif.

"These new images showcase why NuSTAR is giving us an unprecedented look at the cosmos," said Lou Kaluzienski, NuSTAR program scientist at NASA headquarters in Washington. "With NuSTAR's greater sensitivity and imaging capability, we're getting a wealth of new information on a wide array of cosmic phenomena in the high-energy X-ray portion of the electromagnetic spectrum."

Launched last June, NuSTAR is the first orbiting telescope with the ability to focus high-energy X-ray light. It can view objects in considerably greater detail than previous missions operating at similar wavelengths. Since launch, the NuSTAR team has been fine-tuning the telescope, which includes a mast the length of a school bus connecting the mirrors and detectors.

The mission has looked at a range of extreme, high-energy objects already, including black holes near and far, and the incredibly dense cores of dead stars. In addition, NuSTAR has begun black hole searches in the inner region of the Milky Way galaxy and in distant galaxies in the universe.

Among the telescope's targets is the spiral galaxy IC342, also known as Caldwell 5, featured in one of the two new images. This galaxy lies 7 million light-years away in the constellation Camelopardalis (the Giraffe). Previous X-ray observations of the galaxy from NASA's Chandra X-ray Observatory revealed the presence of two blinding black holes, called ultraluminous X-ray sources (ULXs).

How ULXs can shine so brilliantly is an ongoing mystery in astronomy. While these black holes are not as powerful as the supermassive black hole at the hearts of galaxies, they are more than 10 times brighter than the stellar-mass black holes peppered among the stars in our own galaxy. Astronomers think ULXs could be less common intermediate-mass black holes, with a few thousand times the mass of our sun, or smaller stellar-mass black holes in an unusually bright state. A third possibility is that these black holes don't fit neatly into either category.


This new view of the historical supernova remnant Cassiopeia A, located 11,000 light-years away, was taken by NASA's Nuclear Spectroscopic Telescope Array, or NuSTAR. Image credit: NASA/JPL-Caltech/DSS.

"High-energy X-rays hold a key to unlocking the mystery surrounding these objects," said Fiona Harrison, NuSTAR principal investigator at the California Institute of Technology in Pasadena. "Whether they are massive black holes, or there is new physics in how they feed, the answer is going to be fascinating."

In the image, the two bright spots that appear entangled in the arms of the IC342 galaxy are the black holes. High-energy X-ray light has been translated into the color magenta, while the galaxy itself is shown in visible light.

"Before NuSTAR, high-energy X-ray pictures of this galaxy and the two black holes would be so fuzzy that everything would appear as one pixel," said Harrison.

The second image features the well-known, historical supernova remnant Cassiopeia A, located 11,000 light-years away in the constellation Cassiopeia. The color blue indicates the highest-energy X-ray light seen by NuSTAR, while red and green signify the lower end of NuSTAR's energy range. The blue region is where the shock wave from the supernova blast is slamming into material surrounding it, accelerating particles to nearly the speed of light. As the particles speed up, they give off a type of light known as synchrotron radiation. NuSTAR will be able to determine for the first time how energetic the particles are, and address the mystery of what causes them to reach such great speeds.

Artist's view of the NuSTAR spacecraft

"Cas A is the poster child for studying how massive stars explode and also provides us a clue to the origin of the high-energy particles, or cosmic rays, that we see here on Earth," said Brian Grefenstette of Caltech, a lead researcher on the observations. "With NuSTAR, we can study where, as well as how, particles are accelerated to such ultra-relativistic energies in the remnant left behind by the supernova explosion."

For more information about NuSTAR and to view the new images, visit: http://www.nasa.gov/nustar .

NuSTAR is a Small Explorer mission led by Caltech and managed by NASA's Jet Propulsion Laboratory in Pasadena for NASA's Science Mission Directorate in Washington. Orbital Sciences Corporation of Dulles, Va., built the spacecraft. Its instrument was built by a consortium including Caltech; JPL; the University of California (UC) Berkeley; Columbia University; NASA's Goddard Space Flight Center in Greenbelt, Md.; the Danish Technical University in Denmark; Lawrence Livermore National Laboratory in Livermore, Calif.; and ATK Aerospace Systems of Goleta, Calif.

NuSTAR's mission operations center is at UC Berkeley, with the Italian Space Agency providing an equatorial ground station located at Malindi, Kenya. The mission's outreach program is based at Sonoma State University in Rohnert Park, Calif. Goddard manages NASA's Explorer Program. Caltech manages JPL for NASA.

You can follow JPL News on Facebook at: http://www.facebook.com/nasajpl and on Twitter at: http://www.twitter.com/nasajpl . Caltech manages JPL for NASA.

Images (mentioned), Text, Credits: NASA / J.D. Harrington / JPL / Whitney Clavin.

Best regards, Orbiter.ch

lundi 7 janvier 2013

NASA's Kepler Mission Discovers 461 New Planet Candidates












NASA - Kepler Mission patch.

Jan. 7, 2013


Size of Kepler Planet Candidates: Since the last Kepler catalog, the number of candidates discovered in the Kepler data has increased by 20 percent and now totals 2,740 potential planets orbiting 2,036 stars.

NASA's Kepler mission Monday announced the discovery of 461 new planet candidates. Four of the potential new planets are less than twice the size of Earth and orbit in their sun's "habitable zone," the region in the planetary system where liquid water might exist on the surface of a planet.

Based on observations conducted from May 2009 to March 2011, the findings show a steady increase in the number of smaller-size planet candidates and the number of stars with more than one candidate.

"There is no better way to kickoff the start of the Kepler extended mission than to discover more possible outposts on the frontier of potentially life bearing worlds," said Christopher Burke, Kepler scientist at the SETI Institute in Mountain View, Calif., who is leading the analysis.

Since the last Kepler catalog was released in February 2012, the number of candidates discovered in the Kepler data has increased by 20 percent and now totals 2,740 potential planets orbiting 2,036 stars. The most dramatic increases are seen in the number of Earth-size and super Earth-size candidates discovered, which grew by 43 and 21 percent respectively.

The new data increases the number of stars discovered to have more than one planet candidate from 365 to 467. Today, 43 percent of Kepler's planet candidates are observed to have neighbor planets.

"The large number of multi-candidate systems being found by Kepler implies that a substantial fraction of exoplanets reside in flat multi-planet systems," said Jack Lissauer, planetary scientist at NASA's Ames Research Center in Moffett Field, Calif. "This is consistent with what we know about our own planetary neighborhood."


The Kepler space telescope identifies planet candidates by repeatedly measuring the change in brightness of more than 150,000 stars in search of planets that pass in front, or "transit," their host star. At least three transits are required to verify a signal as a potential planet.

Scientists analyzed more than 13,000 transit-like signals to eliminate known spacecraft instrumentation and astrophysical false positives, phenomena that masquerade as planetary candidates, to identify the potential new planets.

Candidates require additional follow-up observations and analyses to be confirmed as planets. At the beginning of 2012, 33 candidates in the Kepler data had been confirmed as planets. Today, there are 105.

"The analysis of increasingly longer time periods of Kepler data uncovers smaller planets in longer period orbits-- orbital periods similar to Earth's," said Steve Howell, Kepler mission project scientist at Ames. "It is no longer a question of will we find a true Earth analogue, but a question of when."

The complete list of Kepler planet candidates is available in an interactive table at the NASA Exoplanet Archive. The archive is funded by NASA's Exoplanet Exploration Program to collect and make public data to support the search for and characterization of exoplanets and their host stars.

Kepler space telescope

Ames manages Kepler's ground system development, mission operations and science data analysis. NASA's Jet Propulsion Laboratory (JPL) in Pasadena, Calif., managed Kepler mission development. Ball Aerospace and Technologies Corp. in Boulder, Colo., developed the Kepler flight system and supports mission operations with JPL at the Laboratory for Atmospheric and Space Physics at the University of Colorado in Boulder.

The Space Telescope Science Institute in Baltimore archives, hosts and distributes the Kepler science data. Kepler is NASA's 10th Discovery Mission and is funded by NASA's Science Mission Directorate at the agency's headquarters in Washington.

JPL manages NASA's Exoplanet Exploration Program. The NASA Exoplanet Archive is hosted at the Infrared Processing and Analysis Center at the California Institute of Technology.

For information about the NASA Exoplanet Archive, visit: http://exoplanetarchive.ipac.caltech.edu/index.html

For information about the Kepler Mission, visit: http://www.nasa.gov/mission_pages/kepler/main/index.html

Images, Text, Credits: NASA / Ames Research Center / Michele Johnson.

Best regards, Orbiter.ch

LEON: The Space Chip That Europe Built












ESA - European Space Agency patch.

7 January 2013

 Layout of the LEON2-FT chip, alias AT697

Just like home computers, the sophisticated capabilities of today’s space missions are made possible by the power of their processor chips. ESA’s coming Alphasat telecom satellite, the Proba-V microsatellite, the Earth-monitoring Sentinel family and the BepiColombo mission to Mercury are among the first missions to use an advanced 32-bit microprocessor – engineered and built in Europe.

All of them incorporate the new LEON2-FT chip, commercially known as the AT697. Engineered to operate within spacecraft computers, this microprocessor is manufactured by Atmel in France but originally designed by ESA.

To give an idea of the kind of complex factors involved in its design, the ‘FT’ in its name stands for ‘fault tolerant’, meaning it can withstand the random memory ‘bit flips’ due to space radiation (for more information, see the link: LEON: The making of a microprocessor for space).

Alphasat

This year's Proba-V microsatellite – surveying daily vegetation growth on a daily basis for a community of scientists previously served by the Spot satellites – will use the AT697 processor in its main flight computer.

And while Alphasat employs an older ERC32 chip in its main flight computer, LEON2-FT will be operating an experimental star tracker aboard the satellite as well as the payload computer.

Also with ERC32-based flight computers, ESA’s Sentinels, the first of which will also be launched in the coming year, will similarly harness LEON2-FT chips in their GPS receivers and startrackers for navigation.

BepiColombo heading towards Mercury

ESA’s 2014 IXV Intermediate eXperimental Vehicle for testing atmospheric reentry will control its avionics with a LEON2-FT chip. And 2015’s BepiColombo mission to Mercury and 2018’s Gaia star-mapper are both using the same design.

The underlying LEON design has also been made available to Europe’s space industry as the basis for company-owned ‘system-on-chip’ microprocessors optimised for dedicated tasks. For instance, Astrium is using it to create a space-based GPS/Galileo satnav receiver.

Innovating for Independence

LEON2-FT chip within Proba-2's computer

How did ESA end up designing computer chips in the first place? As one of the only bodies worldwide to deal with the entire range of space activities, the Agency is as concerned with the internal components used to put together missions as the design of the missions themselves.

“One of the main reasons for ESA to exist is to ensure the independence of Europe’s space industry,” said Roland Weigand of ESA’s microelectronics section. 

“If we are too dependent on parts from outside Europe whose supply could be restricted at any time then the competitiveness, even the long-term viability, of our space sector comes into question. That’s become a real concern with foreign export controls and related regulations.

Proba-2

“ESA first became motivated to get involved with microprocessor development back in the 1990s as they became more central to the performance of space missions.

“Independence from non-European parts is also a driver of our European Components Initiative, in place for the last decade, which is working with European industry to bring new components to market.”

Leading up to LEON: ESA'S First Microprocessors

 Computing performance of ESA's standard microprocessors

ESA engineers began by taking existing designs and adapting them for space use. This process began with the Agency’s MA31750 16-bit microprocessor, designed in the early 1990s.

Manufactured in the UK, this microprocessor is sold internationally and still in widespread use in the satellite telecommunications sector, as well as serving ESA missions, including comet-chaser Rosetta.

For its next attempt the Agency adopted the SPARC (Scalable Processor Architecture) open industry standard, resulting in the ERC32 design.

An initial three-chip set (each chip containing part of the microprocessor) was developed in the mid-1990s. Commercialised by Atmel as the TSC691/692/693, it was employed by several computers of the International Space Station, by the Automated Transfer Vehicle supply truck and by ESA’s highly automated Proba-1 Earth observation microsatellite.

 Rosetta, running on ESA's MA31750 chip

Its second generation, developed in the late 1990s, merged these three chips into one: the ERC32 ‘single chip’, subsequently commercialised by Atmel as the TSC695. This product has been at the heart of European space systems for more than a decade.

Notable adopters include the inertial units guiding the flight of Ariane 5 launchers and the Herschel and Planck space observatories, among other ESA science missions.

“About 3500 ERC32 single-chip flight units have been sold, and it remains on sale to this day, valued in the space industry as a mature, reliable product,” Roland added.

Starting Over

Then, for ERC32’s follow-on microprocessor came the concept of starting over from scratch.

“The idea in the second half of the 1990s was not just to rely on this existing SPARC open architecture but to take full control of the functionality, which meant making our own design,” explained Roland.

Development of the LEON microprocessor was initiated by two then ESA staff André Pouponnot and Jiri Gaisler, in coordination with their division head, Richard Creasey.

ERC32-based ISS flight computer

Not that the small ESA team did everything themselves: by initially releasing a reduced version of the LEON design as open source code to a worldwide community of users, including many universities, they crowdsourced valuable debugging feedback ahead of manufacturing (for more information, see the link: LEON: The making of a microprocessor for space).

Boasting a five-fold performance improvement on the ERC-32, ESA’s LEON2-FT is once more manufactured by Atmel. Features are etched onto its underlying semiconductor at 180 nanometre scale, compared to the single-chip ERC32’s 500 nm. The smaller the scale, of course, the more computing power can be crammed onto an individual chip.

Ariane 5 runs on single version ERC32 chip

To give an idea of scale, an individual atom measures a few nanometres across while a typical human hair is about 60 000 nm to 100 000 nm wide. Manufacturing at such a scale sounds impressive but the commercial semiconductor industry is typically operating several generations ahead of the space industry.

LEON'S First Flights

The AT697 (LEON2-FT) flew for the first time in 2008, launched to ESA’s Columbus module on the Space Station within a prototype computer payload called the ERNObox.

Global ship traffic detection from ISS based on AIS signals

This served to gather data on the internal Station environment before being converted into an experimental system detecting Automatic Identification System (AIS) signals from orbit – the maritime equivalent of air traffic control signals – to build up a global picture of oceangoing traffic.

The following year a second LEON2-FT chip ran the flight computer of ESA’s Proba-2 microsatellite, a technology demonstration mission focused on solar and space weather monitoring.

LEON2-FT-based ERNObox

Both chips remain fully functional to this day, achieving the all-important flight heritage essential for broader market acceptance.

“About 400 flight units have been sold in the almost four years that the LEON has been on sale,” Roland added.

“It is a general-purpose microprocessor, so it can serve in a main computer to run the satellite platform, but can also be used for payload computers to oversee particular experiments.”

An Intangible Asset

And the LEON’s versatility extends beyond the physical microprocessor itself. ESA also has full rights to reuse its ‘IP core’ (Intellectual Property core), meaning the underlying code that describes the circuit, the key input needed, after several design steps, to embed the circuit onto a real chip.

 Venus Express

Existing separately from the manufactured circuit, this LEON ‘source code’ therefore can be applied to various different platforms, such as becoming part of a dedicated ‘system on a chip’ with specialised peripheral functions, such as data compression or encoding and decoding.

“In fact, a LEON IP core actually was launched even before the AT697 into space,” said Roland. “A programmable chip based on a radiation-tolerant version of this IP core has been controlling a visual monitoring camera on ESA’s Venus Express mission since 2005.”

LEON's Next Steps

Not that the LEON story ends with the LEON2-FT. Alphasat and Europe’s Galileo navigation satellites both use next-generation LEON3-based reprogrammable chips within payload elements, embedding a new IP core evolved from the previous LEON design by Swedish company Aeroflex Gaisler.

LEON3 spacecraft controller on a chip

Aeroflex Gaisler’s LEON3 is also become the basis of the SCOC3 spacecraft-computer-on-a-chip. Developed by Astrium with ESA support for manufacture by Atmel, this single component has sufficient functionality to operate an entire satellite platform or payload in space. 

The SCOC3 is already flying in orbit, an integral part of missions including France’s Spot-6 Earth observation satellite launched in September and the MISSE-7 materials experiment outside the Space Station.

Spot-6 satellite

And ESA has contracted with Göteborg-based Aeroflex Gaisler to develop the Next Generation Microprocessor (NGMP) for the decade to come, which will be based on the LEON4 microprocessor: four CPUs will serve a comprehensive set of peripherals to provide a further boost in processing performance, reflecting a similar move to multicore processors in terrestrial markets.

The chances are whatever hardware you are reading this on would not cope well with space. Assuming its mechanical structure survived the launch acceleration and vibration, it would then face sustained hard vacuum and temperature extremes. And within a matter of months or even weeks its central microprocessor would doubtless be fried by radiation exposure.

Space is awash with charged particles of various energy levels, either emitted directly from the Sun or the wider Cosmos beyond the Solar System or else confined within Earth’s magnetic field to help form the radiation belts.

Space radiation

When a high-energy particle strikes a computer chip, the consequences can include the random ‘flipping’ of microprocessor memory cells – known as a Single Event Upset – through to transistor gate ruptures up to a complete burn-out, called a ‘latch-up’.

Sustained radiation exposure can also weaken the underlying quality and electrical conductivity of the chip’s semiconductor material, potentially leading to degraded performance or excessive power consumption.

Single Event Effect

“As microprocessor gates become smaller and the absolute levels of power go down, our circuits are becoming more vulnerable to Single Event Upsets,” said Roland Weigand of ESA’s microelectronics section.

“Even terrestrial chip manufacturers are growing more concerned about hardening against radiation – especially for products like network routers or medical applications where reliability needs are absolute.

“For the radiation-heavy space environment the problem is, of course, many orders of magnitudes worse.”

Robustness Through Redundancy

So dedicated microprocessors like ESA’s LEON family are essential for space missions and radiation-hardening is one of the main factors driving their design.

Physical shielding has a role to play, but can only extend so far. Heavy ions can still pass through an aluminium box, or else interact with it to produce a shower of secondary particles that could be almost as harmful.

South Atlantic Anomaly - heightened radiation in Earth orbit

“The key to designing for rad-hardening is really redundancy,” Roland added. “You might duplicate your bits at different sites around the microprocessor or use ‘parity coding’ to add on extra bits that help with detecting errors.

“Or you can triplicate your bits and then use a voting system to detect and correct errors: the result that comes up the most is likely to be right.

LEON2-FT– AT697

“Alternatively you can perform the same calculation multiple times – temporal instead of spatial redundancy.

“Whatever mode of fault tolerance is used, there is a price to pay for that redundancy. Your chip will be larger, run slower and consume more power – in return for its increased reliability. 

“To limit these penalties requires a careful optimisation of the design, striving for compromises with the expected processor timing performance.

LEON2-FT within its container

 “So before introducing radiation tolerance features, the chip designers should ideally have in-depth knowledge of how the processor works. This is a real problem with commercial processors – based on proprietary information – and it is difficult to add in such features after cores have already been designed.

“Instead for the LEON we decided to start from scratch, adding redundancy from the beginning.”

LEON: A New Recipe for Chips

How to go about designing a microprocessor? The first step is to think about what it needs to do, in this case serve as a general purpose processor for space-based computer systems.

The next, having selected the SPARC open standard to work within, was to code the instruction set defined by this standard into a text-based description suitable for translation into an electronic circuit.

Clean room for chip fabrication

“Coding is performed using a hardware description language called VHDL which resembles a software programming language but has specific features to describe an electronic circuit,” Roland explained.

The resulting description contained several thousand lines of code: the LEON2-FT VHDL IP core. This VHDL code could then be simulated on computers, to validate it was operating as intended in advance of producing any hardware. A reduced version of the LEON IP core was distributed to the user community to obtain crowdsourced debugging tips.

“The next stage was then to physically translate that code to create a test board hosting a programmable chip called a ‘field programmable gate array’ (FPGA) where the LEON design could be put to work and tested.”

The reprogrammable nature of the FPGA allowed different design configurations to be evaluated before deciding on a definitive version for the final (and expensive) chip manufacturing, when the microprocessor design is etched onto semiconductor chips.

LEON simulation

In the Nanoworld

Conservative space technology tends to lag behind its faster-moving terrestrial equivalent: the LEON2-FT is etched to a resolution of 180 nm, while the forthcoming Next Generation Microprocessor will go down to 90 nm or even 65 nm. For comparison, Intel’s latest CPU is around 32 nm.

These 90 nm and 65 nm technologies, while available in the commercial world for many years, are currently being validated for use in space through a pair of ESA activities called the Design Against Radiation Effects (DARE) and Deep Sub Micron (DSM) initiatives.

This descent into the nanoworld throws up fresh design challenges – such smaller technology is more sensitive to Single Event Upsets, for example – but success would mean that spacecraft designers can go on assuming enhanced processing performance for future missions for many years to come.

Related Links:

European Components Initiative (ECI): http://www.esa.int/Our_Activities/Technology/European_Component_Initiative_ECI

Microelectronics website: http://www.esa.int/TEC/Microelectronics/

Images, Text, Credits: ESA / AOES Medialab / P. Carril / J. Huart / Qinetiq Space Belgium / CNES / Arianespace / FFI / Astrium / SSA / NASA / STMicroelectronics.

Greetings, Orbiter.ch

A Cradle of Stars










ESA / NASA - Herschel patch.

7 January 2013

 W40’s cradle of stars

Six hundred newly forming stars are crowded into intricate filaments of gas and dust that makes up this stellar nursery, seen for the first time by ESA’s Herschel space observatory.

The nebulous area coloured in blue, known as W40 or Sharpless 2-64, is roughly 1000 light-years away in the constellation Aquila, and is about 25 light-years across.

It is a vast cloud of hydrogen gas, illuminated by the radiation streaming out from at least three young massive stars embedded in the cloud.

The nebula is expanding into the surrounding medium, compressing the ambient gas on its way and triggering the formation of a second generation of even younger stars.

In total, around 600 condensations of dust and gas have been estimated in this field of view, the majority of which will eventually collapse to form stars.

Already about 150 objects are in the final stages of forming stars. Once nuclear fusion kicks in, their cores will ignite and they will become fully fledged stars.

ESA’s Herschel space observatory

W40 is part of a giant ring of stars and star-forming clouds known as Gould’s Belt that appears to circle the night sky. These stellar nurseries are key targets for Herschel, allowing astronomers to compare the differences in star formation from region to region and to identify the role of the local environment in the process.

This image is from our archives; it was created from observations by Herschel’s PACS and SPIRE instruments on 24 October 2009 and published on OSHI in 2011.

Related link:

Herschel: http://www.esa.int/Our_Activities/Space_Science/Herschel

Images, Text, Credits: ESA and SPIRE & PACS consortia, Ph. André (CEA Saclay) for Gould’s Belt Key Programme Consortia.

Best regards, Orbiter.ch

samedi 5 janvier 2013

A vast, thin plane of corotating dwarf galaxies orbiting the Andromeda galaxy












Canada France Hawaii Telescope logo.

Jan. 5, 2013

 Andromeda galaxy (M 31)

Dwarf satellite galaxies are thought to be the remnants of the population of primordial structures that coalesced to form giant galaxies like the Milky Way. It has previously been suspected that dwarf galaxies may not be isotropically distributed around our Galaxy, because several are correlated with streams of Hi emission, and may form coplanar groups.

These suspicions are supported by recent analyses. It has been claimed that the apparently planar distribution of satellites is not predicted within standard cosmology, and cannot simply represent a memory of past coherent accretion. However, other studies dispute this conclusion.

Here we report the existence of a planar subgroup of satellites in the Andromeda galaxy (M 31), comprising about half of the population. The structure is at least 400 kiloparsecs in diameter, but also extremely thin, with a perpendicular scatter of less than 14.1 kiloparsecs.


This composite shows the alignment of the satellite dwarf galaxies of the Andromeda galaxy, in relation to the view that we see from Earth (the top left panel shows a true color image of the center of the Andromeda galaxy taken with the Canada France Hawaii Telescope). Credit: Ibata et al.

Radial velocity measurements reveal that the satellites in this structure have the same sense of rotation about their host. This shows conclusively that substantial numbers of dwarf satellite galaxies share the same dynamical orbital properties and direction of angular momentum. Intriguingly, the plane we identify is approximately aligned with the pole of the Milky Way’s disk and with the vector between the Milky Way and Andromeda.

This new discovery was made ​​possible by a computer simulation carried out with the programming language Python, programmed by a young college boy (15 years) Neil G. Ibata.

Images, Text, Credits (Contributions, authors):  Nature / Canada France Hawaii Telescope (CFH) / Rodrigo A. Ibata, Geraint F. Lewis, Anthony R. Conn, Michael J. Irwin, Alan W. McConnachie,    Scott C. Chapman, Michelle L. Collins, Mark Fardal, Annette M. N. Ferguson, Neil G. Ibata, A. Dougal Mackey, Nicolas F. Martin, Julio Navarro, R. Michael Rich, David Valls-Gabaud & Lawrence M. Widrow / NASA - ESA Hubble / Orbiter.ch.

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Miracle - A Star









Astronomical Observations.

05/01/2013

As we know from the Gospels preceded the birth of Christ astronomical phenomenon called the star of Bethlehem. Astronomers and historians still can not figure out what it was? Comet or a supernova explosion? The debate about what shone so brightly in the sky for two thousand years ago, is still going on. Every year before Christmas, new hypotheses.

On Christmas Eve, a new hypothesis of the star of Bethlehem. According to American scientists a star that guides the Magi to the infant Jesus, was a unique astronomical phenomenon: the Sun, Moon, Jupiter and Saturn are lined up in a row in the constellation Aries, which is why there was a bright glow.

"Connecting the planets are quite common in 2012, these events took place, will be in 2013, and the planet do not merge, they just come closer to each other ... and this is nothing extraordinary ...." - says senior researcher Oleg IKI Ugolnikov .

The debate about what kind of celestial event happened two thousand years ago, is still going on. Every year just before Christmas a mass of new hypotheses. However, the actual astronomical phenomena, which would provide a bright glow in the sky, even this day, not so much.

In 1604, the great mathematician and astronomer Johannes Kepler observed the supernova explosions. Scientists have suggested that this may well have happened two thousand years ago. Brightest supernova is comparable with glitter galaxy. Its glow can be seen even on a sunny day.

Supernova explosion

"The supernova explosion, a death star, at the end of evolution. Star actually falls on itself and becomes a neutron star with the release of huge amounts of energy. But if at that time there was an outbreak of a supernova, we would have seen her rest ... ", - says Oleg Ugolnikov.

Another popular hypothesis is the star of Bethlehem was a comet. After all, according to scripture, a star moving across the sky. Maybe - it was one of the most mysterious comets - Halley's Comet. Close to the planet it flies every 75 years. The last time it was observed in 1986, following the visit of space pilgrims expected in 2061. With this comet involves a lot of superstitions. If the tail is long, it is to be war. By some accounts, it was Halley's comet, and could be the star of Bethlehem.

"There are comets that come very close to the Sun, and just a few days, it sharply increases its shine ..." - says Oleg Ugolnikov.

Halley's comet

Two thousand years have passed, and the consensus among scientists or not. Each version is available and thus can not be proved.

"The sky has its own book, in his own society, and people try to connect, but it's naive form ... Science and religion are in principle not compatible ...." - explains Professor, Doctor of Physical and Mathematical Sciences Rostislav Polishchuk.

In the temple of Star City prayer. The spiritual mentor of our cosmic detachment father Job prays for the crew, who now has a watch on the International Space Station. Once he also dreamed of flying to the stars, and even acted in flight school, but chose a heavenly way ...

His board books not only theological literature, and scientific works, including the recent astronomical discoveries. At the expense of the star of Bethlehem father Job brief - is a miracle. Even one small statement, which scientists somehow ignored.

Star of Bethlehem: this was (in Russian)

"The Star - it's not easy astronomical phenomenon, a spiritual force, an angel of God, which went before the Magic And this is the proof, you know how to move the star. Neither star is not from the North to the East, but the star was from the North to the East, showing the way the Magi. It shines even in the day "- explains the rector of the church of the Transfiguration in Star City Abbot Job.

Perhaps, indeed, we should not look for any evidence. Especially in these days, like Christmas and New Year, why not believe in miracles. The more that a person has not answered the most important question - how did life on the third planet from the Sun called Earth? Is not that a great miracle!

Original text in Russian: http://www.federalspace.ru/main.php?id=2&nid=19803

Images, Text, Video, Credits: Roscosmos TV Studio / ROSCOSMOS / NASA / Translation: Orbiter.ch Aerospace.

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