Author: Fraser Cain

Image credit: Sea Launch

The Odyssey Launch Platform and Sea Launch Commander set sail from their port in Los Angeles on Wednesday in preparation to launch the Thuraya-2 satellite on board a Zenit 3SL rocket. The ship and launch platform will reach the launch site, located in the Pacific Ocean at the Equator, and then begin a 72-hour countdown for launch – the 44-minute launch window begins June 10 at 1356 GMT (9:56am PDT). The Thuraya-2 satellite will provide communications in the Middle East, Europe, Africa and Asia.

The Odyssey Launch Platform and the Sea Launch Commander departed Sea Launch Home Port this week, for the launch of the Thuraya-2 satellite. Liftoff is scheduled for June 10, in a 44-minute launch window that opens at 6:56 am PDT (13:56:00 GMT).

The two Sea Launch vessels will travel from Sea Launch Home Port, in the Port of Long Beach, to the launch site on the Equator at 154o West Longitude, where a 72-hour countdown will begin upon arrival. Once the platform is ballasted to launch depth, the team will perform final tests on the rocket and spacecraft, and prepare for launch operations. The 200-foot Zenit-3SL rocket will lift the 5177 kg (11,413 lb) Thuraya-2 satellite to geosynchronous transfer orbit with a liftoff thrust of 1.6 million lbs.

Thuraya-2 was built by Boeing [NYSE:BA] for the Thuraya Satellite Telecommunications Company, of United Arab Emirates, and shipped from its satellite manufacturing facility in El Segundo, Calif. The GEO-Mobile (GEM) model satellite uses a Boeing 702 body-stabilized design and integrates a ground segment and user handsets to provide a range of cellular-like voice and data services over a vast geographic region. Sea Launch successfully inserted the first Boeing GEM model, Thuraya-1, to orbit in October 2000. It is the heaviest commercial spacecraft launched successfully to date.

Thuraya-2 will enable Thuraya Satellite Telecommunications to continue to grow and expand its successful business, providing communications services to the people of 100 nations in the Middle East, Europe, North and Central Africa, and South and Central Asia. Thuraya?s advanced satellite telecommunications provides blanket border-to-border coverage to nearly one third of the globe. Based in Abu Dhabi, Thuraya offers uninterrupted and seamless services that link urban and rural areas, and ensure call continuity over regions with fragmented conventional telecommunication networks.

Sea Launch Company, LLC, headquartered in Long Beach, Calif., is a world leader in providing heavy-lift commercial launch services. This multinational partnership offers the most direct and cost-effective route to geostationary orbit. With the advantage of a launch site on the Equator, the proven Zenit-3SL rocket can lift a heavier spacecraft mass or provide longer life on orbit, offering best value plus schedule assurance. Sea Launch has a current backlog of 16 firm launch contracts. For additional information, visit the Sea Launch website at: www.sea-launch.com

Original Source: Boeing News Release

Image credit: NASA

A team of astronomers have weighed a group of planets orbiting a pulsar by precisely measuring their orbits. So far, two of the system’s three planets have been weighed, and they’re 4.3 and 3.0 times the mass of the Earth. What’s unusual is that the spacing between the planets almost exactly match the spacing of Mercury, Venus and Earth – making this bizarre system the most similar to our own Solar System so far discovered. The pulsar, 1257+12, was discovered 13 years ago using the Arecibo radio telescope.

For the first time, the planets orbiting a pulsar have been “weighed” by measuring precisely variations in the time it takes them to complete an orbit, according to a team of astronomers from the California Institute of Technology and Pennsylvania State University.

Reporting at the summer meeting of the American Astronomical Society, Caltech postdoctoral researcher Maciej Konacki and Penn State astronomy professor Alex Wolszczan announced today that masses of two of the three known planets orbiting a rapidly spinning pulsar 1,500 light-years away in the constellation Virgo have been successfully measured. The planets are 4.3 and 3.0 times the mass of Earth, with an error of 5 percent.

The two measured planets are nearly in the same orbital plane. If the third planet is co-planar with the other two, it is about twice the mass of the moon. These results provide compelling evidence that the planets must have evolved from a disk of matter surrounding the pulsar, in a manner similar to that envisioned for planets around sun-like stars, the researchers say.

The three pulsar planets, with their orbits spaced in an almost exact proportion to the spacings between Mercury, Venus, and Earth, comprise a planetary system that is astonishingly similar in appearance to the inner solar system. They are clearly the precursors to any Earth-like planets that might be discovered around nearby sun-like stars by the future space interferometers such as the Space Interferometry Mission or the Terrestrial Planet Finder.

“Surprisingly, the planetary system around the pulsar 1257+12 resembles our own solar system more than any extrasolar planetary system discovered around a sun-like star,” Konacki said. “This suggests that planet formation is more universal than anticipated.”

The first planets orbiting a star other than the sun were discovered by Wolszczan and Frail around an old, rapidly spinning neutron star, PSR B1257+12, during a large search for pulsars conducted in 1990 with the giant, 305-meter Arecibo radio telescope. Neutron stars are often observable as radio pulsars, because they reveal themselves as sources of highly periodic, pulse-like bursts of radio emission. They are extremely compact and dense leftovers from supernova explosions that mark the deaths of massive, normal stars.

The exquisite precision of millisecond pulsars offers a unique opportunity to search for planets and even large asteroids orbiting the pulsar. This “pulsar timing” approach is analogous to the well-known Doppler effect so successfully used by optical astronomers to identify planets around nearby stars. Essentially, the orbiting object induces reflex motion to the pulsar which result in perturbing the arrival times of the pulses. However, just like the Doppler method, the pulsar timing method is sensitive to stellar motions along the line-of-sight, the pulsar timing can only detect pulse arrival time variations caused by a pulsar wobble along the same line. The consequence of this limitation is that one can only measure a projection of the planetary motion onto the line-of-sight and cannot determine the true size of the orbit.

Soon after the discovery of the planets around PSR 1257+12, astronomers realized that the heavier two must interact gravitationally in a measurable way, because of a near 3:2 commensurability of their 66.5- and 98.2-day orbital periods. As the magnitude and the exact pattern of perturbations resulting from this near-resonance condition depend on a mutual orientation of planetary orbits and on planet masses, one can, in principle, extract this information from precise timing observations.

Wolszczan showed the feasibility of this approach in 1994 by demonstrating the presence of the predicted perturbation effect in the timing of the planet pulsar. In fact, it was the first observation of such an effect beyond the solar system, in which resonances between planets and planetary satellites are commonly observed. In recent years, astronomers have also detected examples of gravitational interactions between giant planets around normal stars.

Konacki and Wolszczan applied the resonance-interaction technique to the microsecond-precision timing observations of PSR B1257+12 made between 1990 and 2003 with the giant Arecibo radio telescope. In a paper to appear in the Astrophysical Journal Letters, they demonstrate that the planetary perturbation signature detectable in the timing data is large enough to obtain surprisingly accurate estimates of the masses of the two planets orbiting the pulsar.

The measurements accomplished by Konacki and Wolszczan remove a possibility that the pulsar planets are much more massive, which would be the case if their orbits were oriented more “face-on” with respect to the sky. In fact, these results represent the first unambiguous identification of Earth-sized planets created from a protoplanetary disk beyond the solar system.

Wolszczan said, “This finding and the striking similarity of the appearance of the pulsar system to the inner solar system provide an important guideline for planning the future searches for Earth-like planets around nearby stars.”

Original Source: Caltech News Release

Image credit: ESO

A team of astronomers based in Hawaii have discovered a distant galaxy 12.8 billion light years away which shows us what the Universe looked like when it was only 900 million years old. They found the galaxy by using a special camera installed on the Canada-France-Hawaii telescope which searches for distant objects in a very specific frequency of light. By uncovering this galaxy, located in the constellation of Cetus, right near the star Mira, the team has developed a new methodology for discovering distant objects which should help future observers look even further into the past.

With improved telescopes and instruments, observations of extremely remote and faint galaxies have become possible that were until recently astronomers’ dreams.

One such object was found by a team of astronomers [2] with a wide-field camera installed at the Canada-France-Hawaii telescope at Mauna Kea (Hawaii, USA) during a search for extremely distant galaxies. Designated “z6VDF J022803-041618”, it was detected because of its unusual colour, being visible only on images obtained through a special optical filter isolating light in a narrow near-infrared band.

A follow-up spectrum of this object with the FORS2 multi-mode instrument at the ESO Very Large Telescope (VLT) confirmed that it is a very distant galaxy (the redshift is 6.17 [3]). It is seen as it was when the Universe was only about 900 million years old.

z6VDF J022803-041618 is one of the most distant galaxies for which spectra have been obtained so far. Interestingly, it was discovered because of the light emitted by its massive stars and not, as originally expected, from emission by hydrogen gas.

A brief history of the early Universe
Most scientists agree that the Universe emanated from a hot and extremely dense initial state in a Big Bang. The latest observations indicate that this crucial event took place about 13,700 million years ago.

During the first few minutes, enormous quantities of hydrogen and helium nuclei with protons and neutrons were produced. There were also lots of free electrons and during the following epoch, the numerous photons were scattered from these and the atomic nuclei. At this stage, the Universe was completely opaque.

After some 100,000 years, the Universe had cooled down to a few thousand degrees and the nuclei and electrons now combined to form atoms. The photons were then no longer scattered from these and the Universe suddenly became transparent. Cosmologists refer to this moment as the “recombination epoch”. The microwave background radiation we now observe from all directions depicts the state of great uniformity in the Universe at that distant epoch.

In the next phase, the primeval atoms – more than 99% of which were of hydrogen and helium – moved together and began to form huge clouds from which stars and galaxies later emerged. The first generation of stars and, somewhat later, the first galaxies and quasars [4], produced intensive ultraviolet radiation. That radiation did not travel very far, however, despite the fact that the Universe had become transparent a long time ago. This is because the ultraviolet (short-wavelength) photons would be immediately absorbed by the hydrogen atoms, “knocking” electrons off those atoms, while longer-wavelength photons could travel much farther. The intergalactic gas thus again became ionized in steadily growing spheres around the ionizing sources.

At some moment, these spheres had become so big that they overlapped completely; this is referred to as the “epoch of re-ionization”. Until then, the ultraviolet radiation was absorbed by the atoms, but the Universe now also became transparent to this radiation. Before, the ultraviolet light from those first stars and galaxies could not be seen over large distances, but now the Universe suddenly appeared to be full of bright objects. It is for this reason that the time interval between the epochs of “recombination” and “re-ionization” is referred to as the “Dark Ages”.

When was the end of the “Dark Ages”?
The exact epoch of re-ionization is a subject of active debate among astronomers, but recent results from ground and space observations indicate that the “Dark Ages” lasted a few hundred million years. Various research programmes are now underway which attempt to determine better when these early events happened. For this, it is necesary to find and study in detail the earliest and hence, most distant, objects in the Universe – and this is a very demanding observational endeavour.

Light is dimmed by the square of the distance and the further we look out in space to observe an object – and therefore the further back in time we see it – the fainter it appears. At the same time, its dim light is shifted towards the red region of the spectrum due to the expansion of the Universe – the larger the distance, the larger the observed redshift [3].

The Lyman-alpha emission line
With ground-based telescopes, the faintest detection limits are achieved by observations in the visible part of the spectrum. The detection of very distant objects therefore requires observations of ultraviolet spectral signatures which have been redshifted into the visible region. Normally, the astronomers use for this the redshifted Lyman-alpha spectral emission line with rest wavelength 121.6 nm; it corresponds to photons emitted by hydrogen atoms when they change from an excited state to their fundamental state.

One obvious way of searching for the most distant galaxies is therefore to search for Lyman-alpha emission at the reddest (longest) possible wavelengths. The longer the wavelength of the observed Lyman-alpha line, the larger is the redshift and the distance, and the earlier is the epoch at which we see the galaxy and the closer we come towards the moment that marked the end of the “Dark Ages”.

CCD-detectors used in astronomical instruments (as well as in commercial digital cameras) are sensitive to light of wavelengths up to about 1000 nm (1 ?m), i.e., in the very near-infrared spectral region, beyond the reddest light that can be perceived by the human eye at about 700-750 nm.

The bright near-infrared night sky
There is another problem, however, for this kind of work. The search for faint Lyman-alpha emission from distant galaxies is complicated by the fact that the terrestrial atmosphere – through which all ground-based telescopes must look – also emits light. This is particularly so in the red and near-infrared part of the spectrum where hundreds of discrete emission lines originate from the hydroxyl molecule (the OH radical) that is present in the upper terrestrial atmosphere at an altitude of about 80 km (see PR Photo 13a/03).

This strong emission which the astronomers refer to as the “sky background” is responsible for the faintness limit at which celestial objects can be detected with ground-based telescopes at near-infrared wavelengths. However, there are fortunately spectral intervals of “low OH-background” where these emission lines are much fainter, thus allowing a fainter detection limit from ground observations. Two such “dark-sky windows” are evident in PR Photo 13a/03 near wavelengths of 820 and 920 nm.

Considering these aspects, a promising way to search efficiently for the most distant galaxies is therefore to observe at wavelengths near 920 nm by means of a narrow-band optical filter. Adapting the spectral width of this filter to about 10 nm allows the detection of as much light from the celestial objects as possible when emitted in a spectral line matching the filter, while minimizing the adverse influence of the sky emission.

In other words, with a maximum of light collected from the distant objects and a minimum of disturbing light from the terrestrial atmosphere, the chances for detecting those distant objects are optimal. The astronomers talk about “maximizing the contrast” of objects showing emission lines at this wavelength.

The CFHT Search Programme
Based on the above considerations, an international team of astronomers [2] installed a narrow-band optical filter centered at the near-infrared wavelength 920 nm on the CFH12K instrument at the Canada-France-Hawaii telescope on Mauna Kea (Hawaii, USA) to search for extremely distant galaxies. The CFH12K is a wide-field camera used at the prime focus of the CFHT, providing a field-of-view of approx. 30 x 40 arcmin2, somewhat larger than the full moon [5].

By comparing images of the same sky field taken through different filters, the astronomers were able to identify objects which appear comparatively “bright” in the NB920 image and “faint” (or are even not visible) in the corresponding images obtained through the other filters. A striking example is shown in PR Photo 13b/03 – the object at the center is well visible in the 920nm image, but not at all in the other images.

The most probable explanation for an object with such an unusual colour is that it is a very distant galaxy for which the observed wavelength of the strong Lyman-alpha emission line is close to 920 nm, due to the redshift. Any light emitted by the galaxy at wavelengths shorter than Lyman-alpha is strongly absorbed by intervening interstellar and intergalactic hydrogen gas; this is the reason that the object is not visible in all the other filters.

The VLT spectrum
In order to learn the true nature of this object, it is necessary to perform a spectroscopic follow-up, by observing its spectrum. This was accomplished with the FORS 2 multi-mode instrument at the 8.2-m VLT YEPUN telescope at the ESO Paranal Observatory. This facility provides a perfect combination of moderate spectral resolution and high sensitivity in the red for this kind of very demanding observation. The resulting (faint) spectrum is shown in PR Photo 13c/03.

PR Photo 13d/03 shows a tracing of the final (“cleaned”) spectrum of the object after extraction from the image shown in PR Photo 13c/03. One broad emission line is clearly detected (to the left of the center; enlarged in the insert). It is asymmetric, being depressed on its blue (left) side. This, combined with the fact that no continuum light is detected to the left of the line, is a clear spectral signature of the Lyman-alpha line: photons “bluer” than Lyman-alpha are heavily absorbed by the gas present in the galaxy itself, and in the intergalactic medium along the line-of-sight between the Earth and the object.

The spectroscopic observations therefore allowed the astronomers to identify unambiguously this line as Lyman-alpha, and therefore to confirm the great distance (high redshift) of this particular object. The measured redshift is 6.17, making this object one of the most distant galaxies ever detected. It received the designation “z6VDF J022803-041618” – the first part of this somewhat unwieldy name refers to the survey and the second indicates the position of this galaxy in the sky.

Starlight in the early Universe
However, these observations did not come without surprise! The astronomers had hoped (and expected) to detect the Lyman-alpha line from the object at the center of the 920 nm spectral window. However, while the Lyman-alpha line was found, it was positioned at a somewhat shorter wavelength.

Thus, it was not the Lyman-alpha emission that caused this galaxy to be “bright” in the narrow-band (NB920) image, but “continuum” emission at wavelengths longer than that of Lyman-alpha. This radiation is very faintly visible as a horizontal, diffuse line in PR Photo 13c/03.

One consequence is that the measured redshift of 6.17 is lower than the originally predicted redshift of about 6.5. Another is that z6VDF J022803-041618 was detected by light from its massive stars (the “continuum”) and not by emission from hydrogen gas (the Lyman-alpha line).

This interesting conclusion is of particular interest as it shows that it is in principle possible to detect galaxies at this enormous distance without having to rely on the Lyman-alpha emission line, which may not always be present in the spectra of the distant galaxies. This will provide the astronomers with a more complete picture of the galaxy population in the early Universe.

Moreover, observing more and more of these distant galaxies will help to better understand the ionization state of the Universe at this age: the ultraviolet light emitted by these galaxies should not reach us in a “neutral” Universe, i.e., before re-ionization occurred. The hunt for more such galaxies is now on to clarify how the transition from the Dark Ages happened!

Original Source: ESO News Release

Image credit: NASA

NASA’s RHESSI satellite may have uncovered new clues about the most powerful explosions in the Universe when it accidentally caught an image of a gamma-ray burst while capturing images of solar flares on the Sun. What RHESSI discovered is that the light coming from the burst is polarized, which indicates that a powerful magnetic field could be the cause. When a giant star becomes a rapidly spinning black hole, it could twist up the magnetic field so much that the whole object explodes like an uncoiled spring.

NASA’s RHESSI satellite may have uncovered one of the most important clues yet obtained on the mechanism for producing gamma-ray bursts, the most powerful explosions in the universe. This was the result of a chance observation by a satellite designed to study the Sun.

The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) satellite was snapping pictures of solar flares on December 6, 2002, when it caught an extremely bright gamma-ray burst in the background, over the edge of the Sun, revealing for the first time that the gamma rays in such a burst are polarized. The result indicates intense magnetic fields may be the driving force behind these awesome explosions.

Solar flares are tremendous explosions in the atmosphere of the Sun, powered by the sudden release of magnetic energy. Gamma-ray bursts are remote flashes of gamma-ray light that pop off about once a day randomly in the sky, briefly shining as bright as a million trillion suns. Recent observations suggest they may be produced by a special kind of exploding star (supernova), but not all supernovae generate gamma-ray bursts, so the physics of how a supernova explosion can produce a burst of gamma-rays is unclear.

The findings are being presented in a press conference at the American Astronomical Society meeting in Nashville, Tenn., by two University of California, Berkeley, researchers: Dr. Wayne Coburn, a postdoctoral fellow at UC Berkeley’s Space Sciences Laboratory, and Dr. Steven Boggs, assistant professor of physics. They are authors of a paper about this discovery published in the May 22 issue of Nature.

“RHESSI was sent into space to uncover the secrets of solar flares, the largest explosions in our Solar System, so I am delighted that it has been able to serendipitously provide new information about gamma-ray bursts, the largest explosions in the whole universe,” said Dr. Brian Dennis, RHESSI Mission Scientist at NASA’s Goddard Space Flight Center, Greenbelt, Md.

“Curiously, magnetic fields seem to be driving both the local solar flares and the distant gamma-ray bursts, two immensely powerful events,” added Dennis.

The strong polarization measured by RHESSI provides a unique window on how these bursts are powered, according to Boggs. He interprets the measurements to mean that the burst originates from a region of highly structured magnetic fields, stronger than the fields at the surface of a neutron star – until now, the strongest magnetic fields observed in the universe. “The polarization is telling us that the magnetic fields themselves are acting as the dynamite, driving the explosive fireball we see as a gamma-ray burst,” he said.

The gamma rays measured by RHESSI were about 80 percent polarized, consistent with the maximum possible polarization from electrons spiraling around magnetic field lines. The spiraling causes electrons to produce light by “synchrotron radiation”. Polarized light, familiar to most of us as the reflected light blocked by Polaroid sunglasses, is light with its magnetic and electric fields vibrating primarily in one direction, not randomly. Such coherence implies an underlying physical symmetry, in this case, aligned magnetic fields.

Though the electrons are probably accelerated to nearly the speed of light in shock waves, the fact that the gamma rays are maximally polarized implies that the shock waves themselves are driven by an underlying strong magnetic field.

“The amount of polarization they found is so intense, that it looks like it’s pure synchrotron radiation and nothing else, and all the other theories are going to have to bite the dust now,” said Dr. Kevin Hurley, a UC Berkeley gamma-ray burst physicist who since 1990 has operated the Third Interplanetary Network (IPN3) of six satellites linked together to pinpoint gamma-ray bursts and immediately alert astronomers. However, for such a novel measurement, further independent confirmation is crucial, Boggs added.

The discovery of polarization reveals how a gamma-ray burst is powered – through the generation of a strong, large-scale magnetic field. The next question is: Why do some supernovae lead to a strong, organized magnetic field? This might be a question we can only address through theory, but the pieces of evidence are in place for theorists to unravel, Boggs said.

Though he leaves it to theorists to work out how such strong magnetic fields could be generated, Boggs said that the burst is probably preceded by the core collapse of a massive star directly to a black hole. A black hole itself has no magnetic field, but the local magnetic field can thread through the black hole. If rapidly spinning, the black hole will wind up the local field like a string on a top. The energy density in the tightly wound, compressed field would eventually get so high that the field would rebound outward in a massive fireball, dragging matter with it.

Original Source: NASA News Release