Artificial Gravity Will Help Astronauts Handle Spaceflight

The Short Radius Centrifuge will test human’s ability to withstand gravity. Image credit: NASA. Click to enlarge.
NASA will use a new human centrifuge to explore artificial gravity as a way to counter the physiologic effects of extended weightlessness for future space exploration.

The new research will begin this summer at the University of Texas Medical Branch (UTMB) at Galveston, overseen by NASA’s Johnson Space Center (JSC) in Houston. A NASA-provided Short-Radius Centrifuge will attempt to protect normal human test subjects from deconditioning when confined to strict bed rest.

Bed rest can closely imitate some of the detrimental effects of weightlessness on the body. For the first time, researchers will systematically study how artificial gravity may serve as a countermeasure to prolonged simulated weightlessness.

“The Vision for Space Exploration includes destinations beyond the moon,” said Dr. Jeffrey Davis, director of JSC’s Space Life Sciences Directorate. “This artificial gravity research is an important step in determining if spacecraft design options should include artificial gravity. The collaboration between NASA, the National Institutes of Health (NIH), UTMB and Wyle Laboratories demonstrates the synergy of government, academic and industry partnerships,” he added.

For the initial study this summer, 32 test subjects will be placed in a six-degree, head-down, bed-rest position for 21 days to simulate the effects of microgravity on the body. Half that group will spin once a day on the centrifuge to determine how much protection it provides from the bed-rest deconditioning. The “treatment” subjects will be positioned supine in the centrifuge and spun up to a force equal to 2.5 times Earth’s gravity at their feet for an hour and then go back to bed.

“The studies may help us to develop appropriate prescriptions for using a centrifuge to protect crews and to understand the side effects of artificial gravity on people,” said Dr. Bill Paloski, NASA principal scientist in JSC’s Human Adaptation and Countermeasures Office and principal investigator for the project. “In the past, we have only been able to examine bits and pieces. We’ve looked at how artificial gravity might be used as a countermeasure for, say, cardiovascular changes or balance disorders. This will allow us to look at the effect of artificial gravity as a countermeasure for the entire body,” he added.

The research will take place in UTMB’s NIH-sponsored General Clinical Research Center. The study supports NASA’s Artificial Gravity Biomedical Research Project.

“Physicians and scientists from all over the world will travel to UTMB to study the stresses that spaceflight imposes on cardiovascular function, bone density, neurological activity and other physiological systems,” said Dr. Adrian Perachio, executive director of strategic research collaborations at UTMB. “This is an excellent example of collaboration among the academic, federal and private sectors in research that will benefit the health of both astronauts and those of us on Earth,” he added.

The centrifuge was built to NASA specifications by Wyle Laboratories in El Segundo, Calif. It was delivered to UTMB in August 2004 and will complete design verification testing, validation of operational procedures and verification of science data this spring. The centrifuge has two arms with a radius of 10 feet (3 meters) each. The centrifuge can accommodate one subject on each arm.

Paloski has assembled a team of 24 investigators who designed the study. The first integrated research program is expected to end in the fall of 2006.

Original Source: NASA News Release

Eta Aquarid Meteor Shower Peaks on May 6

Look towards the Aquarius constellation in the early morning on May 6. Image credit: NASA. Click to enlarge.
The eta Aquarid meteor shower peaks on May 5th and 6th. The best time to look, no matter where you live, is during the hours before local sunrise on both days.

This is mainly a southern hemisphere shower, but northern observers can see it, too. In the United States, for example, observers far from city lights might see 5 to 10 meteors per hour. In Australia or South America, rates are better, between 15 and 60 meteors per hour.

This year (2005) the eta Aquarid meteors will be streaming from a point in the sky coincidentally close to Mars. The red planet, which is approaching Earth for a close encounter in October 2005, is already eye-catching.

Eta Aquarid meteors come from the most famous comet of all: Halley’s Comet. Our planet passes close to the orbit of Halley’s Comet twice a year. Although the comet itself is very far away [diagram] tiny pieces of Halley are still moving through the inner solar system. They’re leftovers from the comet’s many close encounters with the Sun. Each time Halley returns (every 76 years) solar heating evaporates about 6 meters of ice and rock from its nucleus! Debris particles called meteoroids, usually no bigger than grains of sand, gradually spread along the comet’s orbit forming an elongated stream of space dust. Earth passes through the debris stream once in May and again in October.

The eta Aquarids are named after a star in the constellation Aquarius. The star has nothing to do with the meteor shower except that the shower’s radiant happens to lie nearby. (The radiant of a meteor shower is a point in the sky from which the meteors appear to stream.) The eta Aquarid’s sister shower in October is called the Orionids, after the constellation Orion.

The eta Aquarid radiant never climbs very far above the horizon in the northern hemisphere. That’s why it is a better shower south of the equator. Most years northerners count about 10 eta Aquarid meteors per hour, while southerners see 3 to 6 times that many.

Northern sky watchers sometimes spot spectacular “Earth grazers,” while the active eta Aquarid radiant is low on the horizon. These are meteors that skim horizontally through the upper atmosphere. “Earth grazers” are typically slow and dramatic, streaking far across the sky. The best time to look for Earthgrazers is 2:00 to 2:30 a.m. local time.

Middle-latitude sky watchers in both hemispheres will see the eta Aquarid radiant rise over the eastern horizon at approximately 2:30 a.m. local time. Aquarius is a fairly dim constellation. The nearest bright star is 1st magnitude Fomalhaut in the constellation Piscis Austrini. Fomalhaut is a good finder star for sky watchers in the south, but it’s not much use to northerners because of its low altitude. In Sydney, Australia, for example, Fomalhaut will be visible at 4 a.m. at an elevation of +25 degrees, just above and westward of the shower’s radiant.

Experienced meteor watchers suggest the following viewing strategy: Dress warmly. Bring a reclining chair, or spread a thick blanket over a flat spot of ground. Lie down and look up somewhat toward the east. Meteors can appear in any part of the sky, although their trails will tend to point back toward the radiant.

Original Source: NASA Spaceweather

High Resolution Global Map in Development

Envisat will build up the most detailed map of the entire Earth. Image credit: ESA. Click to enlarge.
The most detailed portrait ever of the Earth’s land surface is being created with ESA’s Envisat environmental satellite. The GLOBCOVER project aims at producing a global land cover map to a resolution three times sharper than any previous satellite map.

It will be a unique depiction of the face of our planet in 2005, broken down into more than 20 separate land cover classes. The completed GLOBCOVER map will have numerous uses, including plotting worldwide land use trends, studying natural and managed ecosystems and modelling climate change extent and impacts.

Envisat’s Medium Resolution Imaging Spectrometer (MERIS) instrument is being systematically used in Full Resolution Mode for the project, acquiring images with a spatial resolution of 300 metres, with an average 150 minutes of acquisitions occurring daily.

The estimate is that up to 20 terabytes of imagery will be needed to mosaic together the final worldwide GLOBCOVER map ? an amount of data equivalent to the contents of 20 million books. The image acquisition strategy is based around regional climate patterns to minimise cloud or snow cover. Multiple acquisitions are planned for some regions to account for seasonal variations in land cover.

Other Envisat sensors will work in synergy with MERIS. The Advanced Synthetic Aperture Radar (ASAR) instrument will be used to differentiate between similar land cover classes, such as wetlands and humid tropical rainforests. And information from the satellite’s Advanced Along Track Scanning Radiometer will be used to correct for atmospheric distortion and to perform ‘cloud masking’, or the elimination of cloud pixels.

An international network of partners is working with ESA on the two-year GLOBCOVER project, which is taking place as part of the Earth Observation Data User Element (DUE).

Participants include the United Nations Environment Programme (UNEP), the Food and Agriculture Organisation (FAO), the European Commission’s Joint Research Centre (JRC), the International Geosphere-Biosphere Programme (IGBP) and the Global Observations of Forest Cover and Global Observations of Land Dynamics (GOFC-GOLD) Implementation Team Project Office.

“UNEP anticipates being able to put the GLOBCOVER map to good use within its programme of assessment and early warning of emerging environmental issues and threats, particularly those of a trans-boundary nature,” said Ron Witt of UNEP. “Changes in land cover patterns, effects of environmental pollution and loss of biodiversity often do not respect national or other artificial boundaries. “An updated view of such problems – or their effects – from interpreted space imagery should offer a large boost to UNEP’s effort to monitor the health of the planet and our changing environment.”

Located at Friedrich-Schiller University in Jena, Germany, the GOFC-GOLD Implementation Team Project Office is responsible for developing international standards and methodology for global observations, and is advising GLOBCOVER on classification issues.

The GLOBCOVER classification system is being designed to be compatible with the Global Land Cover map previously produced for the JRC for the year 2000, a one-kilometre resolution map produced from SPOT-4 Vegetation Instrument data and known as GLC 2000.

GLOBCOVER will also serve to update and improve the European Environment Agency’s CORINE 2000 database, a 300-metre resolution land cover map of the European continent based on a combination of updated land cover maps and satellite imagery.

Once worldwide MERIS Full Resolution coverage is achieved, there will actually be two GLOBCOVER maps produced. The first, GLOBCOVER V1, will be produced automatically by mosaicking images together in a standardised way.

The JRC is then utilising its GLC2000 experience to produce the more advanced GLOBCOVER V2 in the second year, taking a regionally-tuned approach to the data. Some 30 teams worldwide will participate in analysing and validating GLOBCOVER products.

Acquired in a standardised 15 bands, the MERIS images are going to be processed with an upgraded algorithm that includes an ortho-rectification fool, correcting for altitude based on a digital elevation model (DEM) derived from the Radar Altimeter-2 (RA-2), another Envisat instrument.

Original Source: ESA News Release

History of the Earth’s Atmosphere Written in Rocks

The Earth and its atmosphere today. Image credit: NASA. Click to enlarge.
Washington, D.C. ?CSI-like? techniques, used on minerals, are revealing the steps that led to evolution of the atmosphere on Earth. President of the Mineralogical Society of America, Douglas Rumble, III, of the Carnegie Institution?s Geophysical Laboratory, describes the suite of techniques and studies over the last five years that have led to a growing consensus by the scientific community of what happened to produce the protective ozone layer and atmosphere on our planet. His landmark paper on the subject appears in the May/June American Mineralogist.

?Rocks, fossils, and other natural relics hold clues to ancient environments in the form of different ratios of isotopes?atomic variants of elements with the same number of protons but different numbers of neutrons,? explained Rumble. ?Seawater, rain water, oxygen, and ozone, for instance, all have different ratios, or fingerprints, of the oxygen isotopes 16O, 17O, and 18O. Weathering, ground water, and direct deposition of atmospheric aerosols change the ratios of the isotopes in a rock revealing a lot about the past climate.? Rumble?s paper describes how geochemists, mineralogists, and petrologists are studying anomalies of isotopes of oxygen and sulfur to piece together what happened to our atmosphere from about 3.9 billion years ago, when the crust of our planet was just forming and there was no oxygen in the atmosphere, to a primitive oxygenated world 2.3 billion years ago, and then to the present.

The detective work involves a pantheon of scientists who have analyzed surface minerals from all over the globe, used rockets and balloons to sample the stratosphere, collected and studied ice cores from Antarctica, conducted lab experiments, and run mathematical models. The synthesis from the different fields and techniques points to ultraviolet (UV) light from the Sun as an important driving force in atmospheric evolution. Solar UV photons drive the production of ozone in the atmosphere and yield ozone that is enriched in 17O and 18O, thereby leaving a tell-tale isotopic signature. The ozone layer began to form as the atmosphere gained oxygen, and has since shielded our planet from harmful solar rays and made life possible on Earth?s surface.

The discovery of isotope anomalies, where none were previously suspected, adds a new tool to research on the relationships between shifts in atmospheric chemistry and climate change. Detailed studies of polar-ice cores and exposed deposits in Antarctic dry valleys may improve our understanding of the history of the ozone hole.

Original Source: Carnegie Institution News Release

Watching Gamma Rays from the Safety of Earth

Two of the four H.E.S.S. telescopes in Namibia. Image credit: HESS. Click to enlarge.
Our planet is exposed to almost four dozen octaves of electro-magnetic radiation from the Universe around us. Of those, half-a-dozen octaves can be detected from the Earth’s surface. During the 1990’s several extraordinary new octaves were added with the advent of high-sensitivity CCD imagers and modern computing systems. Today we can track super-high energy gamma rays back to their sources in space ? even while safely ensconced in the Earth?s protective mantle of air.

Well before the turn of the third millennium, it was realized that high-energy photons penetrating the air causes a secondary form of light known as Cherenkov Radiation (CR). CR was first observed by Pierre and Marie Curie when investigating radioactivity at the turn of the 20th century. It wasn’t until the mid-1930s that the hauntingly beautiful “blue-white” glow given off by glass in the presence of radioactivity was studied in detail.

CR was first fully investigated by the Russian experimentalist P. A. Cherenkov in 1936. Cherenkov found that whenever high-energy photons (or particles) pass through a transparent gas, liquid, or glass at velocities greater than the speed of light for that substance, a shower of secondary light is created. In terms of the Earth’s atmosphere, such showers typically occur as gamma rays approach within 10 km’s of sea level and the resulting luminosity projects a light cone (or “light pool”) roughly 250ms in diameter.

Enter the Max Plank Institute of Physics (MPIK) of Heidelberg, Germany in the early 1990s.

In 1992 MPIK tested the first in a series of prototypes intended to develop a full scale IACT (Imaging Atmospheric Cherenkov Telescopes) system. That instrument (CT1) proved that CR showers could be detected using CCDs. It also showed that computers could accurately log a CR shower’s time and position in the sky. A later instrument (CT2) increased CR sensitivity and resolution by adding aperture. Meanwhile improvements were made to associated imaging, data processing, and sky sensing components. By combining four CT2-class instruments together, the first full IACT system was developed in 1995 (CT3). Because of this progress, MPIK’s own website could later say that “Ground-based Imaging Atmospheric Cherenkov Telescopes have become the most efficient experimental technique for the observation of cosmic gamma rays in the TeV energy range.”

IACT systems monitor for CR showers using two or more widely spaced light-collecting mirror assemblies pointed at the same part of the sky. Because CR originates in the Earth’s atmosphere – not well-off in the Universe itself – each mirror sees a shower from a different perspective. The resulting “stereoscopic vision” works like eye and brain to precisely determine the path a gamma ray takes after entering the atmosphere. Based on that data – along with laws governing the way photons move – computers calculate the location of gamma ray source in space. Each ray effectively acts like a luminous finger pointing back toward a distant cosmic source.

By 1998 the first purely astronomical IACT (HEGRA – High Energy Gamma Ray Astronomy) was put into service by MPIK on La Palma in the Canary Islands. HEGRA confirmed dozens of high energy gamma ray sources – many hurling photons of more than 1 terra-electron-volts of energy (the amount of force stored in a single electron accelerated by a trillion volts of electricity). Among them were the Crab Nebula pulsar in Taurus and the giant elliptical galaxy M87 – regent of the Coma-Virgo galaxy cluster.

Today even more advanced IACT systems collect CR. One of the most sophisticated instruments (H.E.S.S – High Energy Stereoscopic System) was developed by MPIK along with a consortium of European scientific and educational organizations. Currently HESS consists of four separate 12m diameter IACTS gathering faint CR light in the dark skies above the 1.8km high Khomas Highlands of Namibia, Africa.

Named after Nobel Prize winning physicist Victor Hess (who discovered cosmic rays in 1912), HESS uses an array of four IACT mirror systems. Each spherical IACT mirror consists of 382, 60cm diameter individually-adjustable sub-mirrors reflecting CR light into a large electronic “camera”. Light focused on the camera is detected by a honeycomb of 960 “smartpixel” photo-multiplier tubes (PMTs). The four IACTs are placed in a square and spaced by 120 meters to give an optimally stereoscopic view of the sky within the 250m light pool caused by a CR event.

Each HESS IACT is ten times more sensitive than its corresponding HEGRA unit – and has to be, for the total amount of CR light in the sky is 10 stellar magnitudes fainter than starlight. HESS IACTS can resolve CR showers caused by photons as “weak” as .1 TeV while discriminating between high-energy particles and photons. Using a pair of IACTS, gamma ray sources can be isolated to less than 5 arc-minutes of angular resolution – roughly 1/6th the apparent size of the full moon. To simplify detection, HESS IACTS can scan 5 degrees of the sky at a time.

One of the fundamental questions before astrophysicists is to determine just how nature manages to pack so much punch into those mass-less, charge-less photons. Currently no terra-electron-volt particle accelerators are on line – and such devices only work with charged particles – not photons. It may fall to IACTS like HESS to lead the way.

In a paper entitled “Observation of the giant radio galaxy M87 at TeV energies using H.E.S.S”, M Beilicke of the Institute for Expermental Physics, Hamburg Germany and associates have used HESS to determine that the giant elliptical galaxy M87 is a strong and possibly periodically variable source of high-energy gamma ray photons.

According to the paper, “M87 is of particular interest for observations of TeV energies. The large jet angle makes it different from the so far observed TeV emitting AGN of the blazar type.” Using HESS, the team determined that high-energy photons originate from a point source centered in the midst of M87 – precisely where it’s AGN is thought to be. Unlike blazars however, M87’s relativistic jets do not point at the Earth.

Meanwhile the team may have also discovered that gamma ray output from M87’s AGN is variable “on time scales of years.” According to M. Bielecke et al, “Such a result would be very important since various models for the TeV gamma-ray production in M87 could be ruled out.” The team goes on to say that “Mechanisms correlated with cosmic rays, large scale jet structures, and exotic dark matter particle annihilation could not explain variability in the TeV gamma ray emission on these time-scales.”

As in many areas of contemporary astronomical investigation, observing M87 across a wide-range of the em band may be essential to understanding how those tiny mass-free wave-particles of light can carry so much ?weight?. There is no doubt that capturing the ‘blue-white” glow of Cherenkov radiation put off by our Earth’s very own atmosphere will play a critical role in making this possible.

Written by Jeff Barbour

Did Life Arrive Before the Solar System Even Formed?

Image credit: NASA
Things seem to start simple then get more complex. Life is like that. And perhaps nowhere is this notion truer than when we investigate the origins of life. Did the earliest single cell life-forms coalesce from organic molecules here on Earth? Or is it possible that – like dandelions wafting spore above spring grass – cosmic winds carry living things from world to world later to take root and flourish? And if this is the case, how precisely does such a “dia-spora” occur?

450 years before the common era, Greek philosopher Anaxagoras of Ionia proposed that all living things sprung from certain ubiquitous “seeds of life”. Today’s notion of such “seeds” is far more sophisticated than anything Anaxagoras could possibly envision – limited as he was to simple observations of living things such as budding plant & flowering tree, crawling & buzzing insect, loping animal or walking human; not too mention natural phenomena like sound, wind, rainbows, earthquakes, eclipses, Sun, and Moon. Surprisingly modern in thought, Anaxagoras could only guess as to the details…

Some 2300 hundreds years later – during the 1830s – Swedish chemist J?ns Jackob Berzelius confirmed that carbon compounds were found in certain meteorites “fallen from the heavens”. Berzelius himself however, held that these carbonates were contaminates originating with the Earth itself – but his finding contributed to theories propounded by later thinkers including the physician H.E. Richter and physicist Lord Kelvin.

Panspermia received its first real treatment by Hermann von Helmholtz in 1879, but it was another Swedish chemist – 1903 Nobel Prize winning Svante Arrhenius – who popularized the concept of life originating from space in 1908. Perhaps surprisingly, that theory was based on the notion that radiation pressure from the Sun – and other stars – “blew” microbes about like tiny solar sails – and not as the result of finding carbon compounds in stony meteorite.

The theory that simple forms of life travel in ejecta from other worlds ? embedded in rock blasted from planetary surfaces by the impact of large objects – is the basis for “lithopanspermia”. There are numerous advantages to this hypothesis – simple, hardy forms of life are often found in mineral deposits on Earth in forbidding locales. Worlds – such as our own or Mars – are occasionally blasted by asteroids and comets large enough to hurl rock at speeds exceeding escape velocities. Mineral in rocks can shield microbes from shock and radiation (associated with impact craters) as well as hard radiation from the Sun as stony meteors move through space. The hardiest forms of life also have the ability to survive in a cold vacuum by going into stasis – reducing chemical interactions to zero while maintaining biological structure well enough to later thaw and multiply in more salubrious environs.

In fact several examples of such ejecta are now available on earth for scientific analysis. Stony meteors can include some very sophisticated forms of organic materials (carbonaceous chondrites have been found that include amino and carboxylic acids). Fossilized remnants from Mars in particular – though subject to various non-organic interpretations – are in the possession of institutions such as NASA. The theory and practice of “lithopanspermia” looks very promising – although such a theory can only explain where the simplest forms of life come from – and not how it originated to begin with.

In a paper entitled “Lithopanspermia in Star Forming Clusters” published April 29, 2005, cosmologists Fred C. Adams of the University of Michigan Center for Theoretical Physics and David Spergel of the Department of Astrophysical Sciences of Princeton University discuss the probability of carbonaceous chondrite distribution of microbial life within early star clusters. According to the duo, “the chances of biological material spreading from one system to another is greatly enhanced … due to the close proximity of the systems and low relative velocities.”

According to the authors, previous studies have looked into the likelihood that life-bearing rocks (typically exceeding 10 kgs in weight) play a role in the spread of life within isolated planetary systems and found “the odds of both meteroid and biological transfer are exceedingly low.” However “odds of transfer increase in more crowded environments” and “Since the time scale for planet formation and the time that young stars are expected to live in birth clusters are roughly comparable, about 10 – 30 million years, debris from planet formation has a good chance of being transferred from one solar system to another.”

Ultimately Fred and David conclude “young star clusters provide an efficient means of transferring rocky material from solar system to solar system. If any system in the birth aggregate supports life, then many other systems in the cluster can capture life bearing rocks.”

To arrive at this conclusion, the duo performed “a series of numerical calculations to estimate the distribution of ejection speeds for rocks” based on size and mass. They also considered the dynamics of early star forming groups and clusters. This was essential to help determine rock recapture rates by planets in neighboring systems. Finally they had to make certain assumptions about the frequency of life-encapsulated materials and the survivability of life-forms embedded within them. All this led up to a sense of “the expected number of successful lithopanspermia events per cluster.”

Based on methods used to arrive at this conclusion and thinking only in terms of present distances between solar systems, the duo estimated the probability that Earth has exported life to other systems. Over the age of life on Earth (some 4.0 Byr) Fred and David estimate that the Earth has ejected some 40 billion life-bearing stones. Of the estimated 10 bio-stones per annum, nearly 1 (0.9) will land on a planet suitable for further growth and proliferation.

Most cosmologists tend to address the “hard-science questions” of the origin of the Universe as a whole. Fred says that “exobiology is intrinsically interesting” to him and that he and “David were summer students together in New York in 1981” where they worked on “issues related to planetary atmospheres and climate, issues that are close to questions of exobiology.” Fred also says that he “spends a healthy fraction of research time on problems associated with star and planet formation.” Fred acknowledges David’s special role in thinking “up the idea of looking at panspermia in clusters; when we talked about it, it became clear that we had all the pieces of the puzzle. We just had to put them together.”

This interdisciplinary approach to cosmology and exobiology also led Fred and David to look at the question of lithopanspermia between clusters themselves. Again using methods developed to explore the proliferation of life within clusters, and later applied to the exportation of life from the Earth itself to other non-solar system planets, Fred and David were able to conclude that “a young cluster is more likely to capture life from outside than to give rise to life spontaneously.” And “Once seeded, the cluster provides an effective amplification mechanism to infect other members” within that cluster itself.

Ultimately however, Fred and David can not answer the question of where and under what conditions the first seeds of life took form. In fact, they are willing to admit that “if the spontaneous origin of life were sufficiently common, there would be no need for any panspermia mechanism to explain the presence of life.”

But according to Fred and David, once life gets a foothold somewhere, it manages to get around quite handily.

Written by Jeff Barbour

The Earth Through Rosetta’s Eyes

Rosetta’s view of Earth, taken during its March 2005 flyby. Image credit: ESA. Click to enlarge.
ESA?s comet chaser mission Rosetta took infrared and visible images of Earth and the Moon, during the Earth fly-by of 4/5 March 2005 while on its way to Comet 67P/Churyumov-Gerasimenko.

These images, now processed, are part of the first scientific data obtained by Rosetta. ?The Earth fly-by represented the first real chance to calibrate and validate the performance of the Rosetta?s instruments on a real space object, to make sure everything works fine at the final target,? said Angioletta Coradini, Principal Investigator for the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument.

?Although we were just calibrating VIRTIS during the Earth fly-by last month, we obtained images of Earth and the Moon which have a high scientific content,? she added.

On 4 and 5 March, before closest approach to Earth and from a distance of 400 000 kilometres from our Moon, Rosetta?s VIRTIS took these images with high resolution in visible and infrared light. In these images, only a small portion of the Moon surface was illuminated (between 19% and 32%).

The spectral analysis (chemical ?finger-printing?) gives indications of the mineralogical differences between highlands and ?seas? or ?maria?. For instance, it was possible to see marked differences in the abundance of two kinds of rocks known as pyroxene and olivine.

On 5 March, after the closest approach to Earth, VIRTIS then took a series of high-resolution images of our planet in visible and infrared light from a distance of 250 000 kilometres. Only 49% of the Earth surface was visible from Rosetta.

Once at Comet 67P/Churyumov-Gerasimenko in 2014, VIRTIS will be used to determine the composition and the nature of the solid nucleus and the gases present in the comet?s coma.

In combination with the other Rosetta instruments, it will also help the selection of the ?touchdown? site for the Rosetta lander Philae.

Before then, Rosetta will make more cosmic loops to reach the comet, and its instruments will collect new data about planets, asteroids and comets. The next encounter with Earth is planned for November 2007.

VIRTIS as been developed by a large consortium of European scientists, with major contribution by Italy, France and Germany.

Original Source: ESA News Release

Next Mars Mission Arrives at the Cape

Workers rolling a case containing parts of the Mars Reconnaissance Orbiter equipment into the Payload Hazardous Servicing Facility. Image credit: NASA. Click to enlarge.
A large spacecraft destined to be Earth’s next robotic emissary to Mars has completed the first leg of its journey, a cargo- plane ride from Colorado to Florida in preparation for an August launch. NASA’s Mars Reconnaissance Orbiter is an important next step in fulfilling NASA’s vision of space exploration and ultimately sending human explorers to Mars and beyond.

The spacecraft’s prime mission will run through 2010. During this period, the project will study Mars’ composition and structure, from atmosphere to underground, in much greater detail than any previous orbiter. It will also evaluate possible sites for future martian landings and will serve as a high-data-rate communications relay for surface missions.

“Great work by a talented team has brought Mars Reconnaissance Orbiter to this milestone in our progress toward a successful mission,” said Jim Graf of NASA’s Jet Propulsion Laboratory, Pasadena, Calif., project manager for the mission.

The spacecraft arrived at Kennedy Space Center’s Shuttle Landing Facility on April 30 aboard a C-17 cargo plane and was taken to the Payload Hazardous Servicing Facility to begin processing. It was built near Denver by Lockheed Martin Space Systems. Launch is scheduled for Aug. 10 at 7:53:58 a.m. EDT (4:53:58 a.m. PDT), at the opening of a two-hour launch window.

The spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A test this month will verify the spacecraft’s ability to communicate through NASA’s Deep Space Network tracking stations. A June test will check the deployment of the spacecraft’s high gain communications antenna. Another major deployment test will check out the spacecraft’s large solar arrays.

In July, the spacecraft will be filled with hydrazine fuel for the “Mars orbit insertion” engine burn, which will be used to reduce the velocity of the spacecraft and place it in orbit around Mars. The fuel also will be used for attitude-control propellant. On July 26 the Mars Reconnaissance Orbiter will be encapsulated in the Atlas V fairing prior to being moved to its launch site on Cape Canaveral Air Force Station.

The Lockheed Martin Atlas V arrived at Cape Canaveral Air Force Station aboard an Antonov cargo plane on March 31 and was taken to the high bay at the Atlas Spaceflight Operations Center. The Atlas booster will be transported in May to the Vertical Integration Facility at Space Launch Complex 41 to be erected. The Centaur upper stage will be transported to that facility for hoisting atop the booster in June.

Prelaunch preparations will include a “wet dress rehearsal” in July, during which the Atlas V will be rolled from the Vertical Integration Facility to the launch pad on its mobile launch platform. The vehicle will be fully fueled with RP-1, liquid hydrogen and liquid oxygen, and the team will perform a simulated countdown. The Atlas V will then be rolled back into the Vertical Integration Facility for final launch preparations.

The Mars Reconnaissance Orbiter will be transported from the Payload Hazardous Servicing Facility at Kennedy Space Center to the Vertical Integration Facility on July 29. It will be hoisted atop the launch vehicle to join the Atlas V for the final phase of launch preparations. The spacecraft is scheduled to undergo a functional test on August 1, followed by a final week of launch vehicle and spacecraft closeouts.

The Mars Reconnaissance Orbiter mission is managed by JPL, a division of the California Institute of Technology, Pasadena, for the NASA Science Mission Directorate, Washington. Lockheed Martin Space Systems is the prime contractor for the project. International Launch Services, a Lockheed Martin joint venture, and Lockheed Martin Space Systems are providing launch services for the mission.

Information about Mars Reconnaissance Orbiter is available online at http://marsprogram.jpl.nasa.gov/mro.

Original Source: NASA/JPL News Release

Return to Flight Delayed to July

Crew of STS-114, practicing for their upcoming launch. Image credit: NASA. Click to enlarge.
NASA announced today July 13 to 31 is the new launch planning window for the Space Shuttle Discovery mission. The new window gives the agency time to do additional work to ensure a safe Return to Flight for Discovery and its crew.

Today’s announcement follows Space Shuttle Program reviews over the past two weeks. Managers identified the need to do more work to validate engineering analyses of potential debris hazards and to make some additional modifications to the external fuel tank. NASA officials and program managers agreed late Thursday to take the time to complete the work.

“This is consistent with our overall approach to the STS-114 mission, which is that we’re going to return to flight, we’re not going to rush to flight,” NASA Administrator Michael Griffin said at a morning news conference at NASA Headquarters. “Our intent with this effort is to make certain we are as safe as we know how to be before we launch the Space Shuttle and its crew. We want it to be right.”

“From the beginning we?ve been milestone-driven,” said William Readdy, NASA associate administrator for Space Operations. “This time, the milestones on debris and ice analyses, propulsion system troubleshooting and External Tank modifications drove us to retarget for July. We?ve never been reluctant to adjust the dates as information becomes available.”

The Return to Flight mission will take Shuttle Commander Eileen Collins and six crew members to the International Space Station. The mission is the first of two test flights to evaluate new thermal protection system inspection and repair techniques and to deliver supplies and equipment to the Station. A transcript of today’s news conference and follow-on technical briefing from NASA’s Johnson Space Center is available at: www.nasa.gov/returntoflight

Original Source: NASA News Release

What’s Up This Week – May 2 – May 8, 2005

Galaxy M51. Image credit: Todd Boroson/NOAO/AURA/NSF. Click to enlarge.
Monday, May 2 – If you’re up before dawn today, look closely at the Moon – ruddy Mars will make its appearance less than 3 degrees north of its waning form.

With early evening dark skies, this would be an excellent time for mid-sized binoculars and telescope users to discover anew the fantastic “Whirlpool Galaxy”. Designated as NGC 5194, this impressive face-on spiral galaxy was discovered by Charles Messier in October of 1773 and cataloged as the M51. You can find it easily by heading about three finger-widths southwest of Eta Ursa Majoris (the end star in the handle of “the Big Dipper”) and in the same finderscope of binocular field as faint star 24 Canes Venaticorum.

At around 35 million light years away, the “Whirlpool” is a spiral delight to all optical aid. Binoculars at a dark location will see it as a large, round “haze” with a brightness toward the center. Small scopes will reveal its galactic nature and satellite galaxy, NGC 5195. With large aperture, this galaxy comes alive with detail. 10″ will clearly show spiral arm structure, while at 12.5″ knots, clusters, stellar condensations and dark dustlanes become wonderfully apparent – making the M51 one of the very few deep space objects that look like a photograph in the eyepiece. Absolutely one of the finest in the night sky!

Tuesday, May 3 – During the very early morning hours, take the opportunity that darker skies provide and view the Alpha Scorpiid meteor shower during its peak. The radiant is near Antares. Later in the morning, try using binoculars to locate Uranus as it appears a little more than three degrees north of the Moon.

Tonight’s destination is a very compact and bright little galaxy that can be seen in larger binoculars and is an easy telescope target – M94. Start by identifying past study Cor Caroli (Alpha Canum). About half a fist width to its northwest you will see Beta. Aim your scopes or binocular mid-way between the two and move slightly more than a degree towards the last star in the handle of the Big Dipper – Alkaid. The M94 was discovered in 1781 by my hero, Mechain, and this small galaxy has a powerful central core. At around 20 million light years away, smaller scopes will have difficulty resolving detail, but larger apertures under ideal conditions will pick up on its tightly-wound spiral structure.

Wednesday, May 4 – If you missed your chance to catch a “shooting star” yesterday morning, then why not try again today as the Eta Aquarids reach their peak? With a fall rate of about 21 per hour, this highly dependable annual shower is the offspring of Comet Halley. With far less Moon to interfere, these bright yellow meteors with outstanding trails are well worth looking for. If skies are cloudy, don’t worry. The Eta Aquarid stream stays active for another week.

Tonight let’s further our understanding of distance and how it effects what we see. As you know, light travels at an amazing speed of about 300,000 kilometers per second. To get a grasp on this concept, how many seconds are there in a minute? An hour? A week? A month? How about a year? Ah, you’re beginning to see the light! For every second – 300,000 kilometers. Now, go back to previous study M3 located between Arcturus and Cor Caroli. This great globular cluster is about 40,000 light years away. In terms of kilometers – that’s far more zeros than most of us can possibly understand – yet we can still see this great globular cluster.

Now let’s locate M53. Roughly halfway between Arcturus and Denebola is faint star Alpha Comae. Aim your binoculars or telescopes there and you will find the M53 about a degree northeast. This very rich, magnitude 8.7 globular cluster is almost identical to the M3, but look at what a difference an additional 25,000 light years can make to how we see it! Larger telescopes will enjoy the compact bright core as well as resolution at the cluster’s outer edges. As a bonus for scopes, look one degree to the southeast for peculiar round cluster NGC 5053. Classed as a very loose globular, this magnitude 10.5 grouping is one of the least luminous objects of its type due to low stellar population and wide separation of members – yet its distance is almost the same.

Thursday, May 5 – Today in 1961, astronaut Alan Shepard made history as he became the first American in “space”. Onboard the Mercury craft, Freedom 7, Shephard spent 15 minutes in a sub-orbital ride of a lifetime. By today’s standards this is considered “shallow space”, but your chance to view something far more distant and every bit as history making is now here.

If you did not get an opportunity to view Comet 9/P Tempel 1 last week, then try again as it will be about two degrees west/southwest of Epsilon Virginis. Projected magnitudes show that Tempel 1 should be around magnitude 10 at this time and recent observing reports indicate that it is condensing well and will be easily distinguishable as cometary. In two months time, the “Deep Impact” mission will have reached Tempel 1 and the result of its experimentation may make the comet flare brightly enough to be seen with the unaided eye. Stay tuned!

Friday, May 6 – Looking for your chance to spot Mercury? Then let the Moon be your guide as the two will appear just before dawn. The swift inner planet will appear about 3 degrees south of the slender crescent Moon for most observers.

Tonight let’s have a little bit of fun. For binocular users, we’re going to visit a large star cluster and a small galaxy. Our beginning destination is Melotte 111, a large hazy patch of stars visible to the unaided eye in Coma Berenices. Known as the “Queen’s Hair”, this five degree span of 5th to 10th magnitude stars is wonderfully rich and colorful. As legend has it, Queen Berenices offered her beautiful long tresses to the gods for the King’s safe return from battle. Touched by her love, the god’s took Berenices’ sacrifice and immortalized it in the stars.

While our next destination isn’t quite so romantic, I think you’ll enjoy getting a “Blackeye”. Located 1 degree east/northeast of 35 Comae, this small bright galaxy can be caught in the same wide binocular field northwest of previous study – M53. Originally discovered by Bode about a year before Messier cataloged it, the M64 is about 25 million light years away and holds the distinction of being one of the more massive and luminous of spiral galaxies. Telescope users will find this particular galaxy most endearing for its namesake – a very wide dark dustlane to the northeast side of the galaxy’s bright core. Power up and enjoy this very unusual treasure!

Saturday, May 7 – Tonight at at about 11:03 p.m. PDT for western United States observers in a rough line between Sacramento to Barstow and San Diego, CA (including Yuma, AZ and northern Mexico), a unique opportunity arrives to help contribute to science. A magnitude 11.7 star is being occulted by a large, and possible binary asteroid named Ophelia. According to Dr. Raoul Behrend of Geneva Observatory, “The recent lightcurve of asteroid (171) Ophelia, shows strong similarities with other binary asteroids.” While the dual nature of this asteroid is still being debated, only radar and observations during an occultation can help to help confirm it, and a single-body theory is not ruled out. “We are working on the interpretation of the lightcurve using various models:
– a single body – a pear which can reproduce the lightcurve, but with departure which seem to be significative – a single body with a huge crater (like Mathilde) – which seems to be ruled out, and
– two bodies – the most difficult to model, but preliminary results are nice. So, as we can’t exclude the single body (at 2/3 level), our preference goes actually to the binary system.” The work with Ophelia’s light curve continues further in this working document which explores sizes in the event of binarity. In a call to observers, Dr. Behrend says, “Good occultations by Ophelia are extremely rare; the last one for *many years* is around 2005-05-08 at 6h UT, over California, Arizona, and Mexico”. If Ophelia should prove to be a binary asteroid, the resulting separation would be near a maximum as predicted by Behrend’s lightcurve. “Every positive, every negative observation is important to determine the binarity state (yes or no), and the size(s). If binarity if confirmed, then the mass, scale, density, albedo and other important physical parameters could be determined with an impressive precision.”

For further information on this event, view the prediction by Steve Preston. If you are in the path of the occultation and wish further information on how to view, record and time the event, please contact Derek Breit or access this page for further instructions.

For the rest of us, we can still have lots of fun viewing another asteroid. In a matter of hours, Ceres will reach opposition and an admirable magnitude of 7. You can spot it easily tonight just northwest (and in the same binocular field) as Beta Librae. Best of luck!

Sunday, May 8 – Tonight is New Moon and time to dish you up a very special galactic treat. Located just a little less than two degrees east of 17 Comae, the NGC 4565 is one of the largest and most beautiful of edge-on galaxies. For the small telescope, it will appear as a very thin scratch of light. As aperture progresses, so does the view. With mid-sized scopes, this impressive galaxy becomes a bright, needle-like silver scratch with a small, almost stellar nucleus. For larger scopes and the trained eye, you will see perfect edge-on form with a dark dissecting dustlane. This is one extremely fine galaxy… Enjoy!

Until next week? May all your journeys be at Light Speed! ….~Tammy Plotner