I Want My NASA TV!

If you’re a Canadian? read this! If you’re not a Canadian, well, still read it… you can help us out. 🙂

I was visiting my Father about 5 years ago, and we were sitting in the kitchen when he said, “hey, it’s time to watch the floaters.” Wha? He turned on the kitchen television, and there was a live broadcast of some astronauts spacewalking outside the shuttle. I couldn’t believe my eyes.

Apparently, my clever Dad had jury-rigged an old satellite dish so that it would receive a television feed from NASA. NASA has a television channel, and it’s all about their space exploration. It could be the greatest thing ever. Okay, it gets a little boring between space launches, but overall, it’s a tremendous channel to have access to.

My Father, on remote Hornby Island, gets NASA television loud and clear. But there’s no way I can get it here in Vancouver. I called my cable company… nope. Then I got a digital satellite dish… nope, sorry.

The only place I can watch NASA TV is on my computer. Ever watched television on your computer? It’s small, blurry, choppy and cuts off all the time. Anyway, I stare enough at computer monitors.

I want my NASA TV.

Well much to my surprise, the Canadian Canadian Radio and Television Commission was actually in discussions to get the cable companies to offer it, but it all fell apart. We get Jerry Springer, but we can’t watch NASA TV. Fortunately, we do get the Daily Show with Jon Stewart, which is about the only thing that gets me to turn my television on these days.

Now there’s hope. The Friends of NASA TV in Canada. It’s a petition to try to convince the CRTC and cable companies to get us the space news we so richly deserve.

If you’re a Canadian, visit their website and sign the petition. Not only that, I want you find as many other Canadians who will do what you say, and get them to sign this. Do it!

If you’re not a Canadian, but you know a Canadian, I want you to send them an email begging them to sign this petition. You got it? Good.

I want my NASA TV.

Fraser Cain, Publisher
Universe Today

New Study of Virgo Galaxy Cluster

Image credit: ESO

New observations from the Japanese 8-m Subaru telescope and the ESO Very Large Telescope (VLT) have revealed new details in the Virgo galaxy cluster – located 50 million light years away. One insight is that massive young stars seem to be able to form in isolation, far away from the brighter parts of galaxies.

At a distance of some 50 million light-years, the Virgo Cluster is the nearest galaxy cluster. It is located in the zodiacal constellation of the same name (The Virgin) and is a large and dense assembly of hundreds of galaxies.

The “intracluster” space between the Virgo galaxies is permeated by hot X-ray emitting gas and, as has become clear recently, by a sparse “intracluster population of stars”.

So far, stars have been observed to form in the luminous parts of galaxies. The most massive young stars are often visible indirectly by the strong emission from surrounding cocoons of hot gas, which is heated by the intense radiation from the embedded stars. These “HII regions” (pronounced “Eitch-Two” and so named because of their content of ionized hydrogen) may be very bright and they often trace the beautiful spiral arms seen in disk galaxies like our own Milky Way.

New observations by the Japanese 8-m Subaru telescope and the ESO Very Large Telescope (VLT) have now shown that massive stars can also form in isolation, far from the luminous parts of galaxies. During a most productive co-operation between astronomers working at these two world-class telescopes, a compact HII region has been discovered at the very boundary between the outer halo of a Virgo cluster galaxy and Virgo intracluster space.

This cloud is illuminated and heated by a few hot and massive young stars. The estimated total mass of the stars in the cloud is only a few hundred times that of the Sun.

Such an object is rare at the present epoch. However, there may have been more in the past, at which time they were perhaps responsible for the formation of a fraction of the intracluster stellar population in clusters of galaxies. Massive stars in such isolated HII regions will explode as supernovae at the end of their short lives, and enrich the intracluster medium with heavy elements.

Observations of two other Virgo cluster galaxies, Messier 86 and Messier 84, indicate the presence of other isolated HII regions, thus suggesting that isolated star formation may occur more generally in galaxies. If so, this process may provide a natural explanation to the current riddle why some young stars are found high up in the halo of our own Milky Way galaxy, far from the star-forming clouds in the main plane.

The Virgo Cluster
The galaxies in the Universe are rarely isolated – they prefer company. Many are found within dense structures, referred to as galaxy clusters, cf. e.g., ESO PR Photo 16a/99.

The galaxy cluster nearest to us is seen in the direction of the zodiacal constellation Virgo (The Virgin), at a distance of approximately 50 million light-years. PR Photo 04a/03 (from the Wide Field Imager camera at the ESO La Silla Observatory) shows a small sky region near the centre of this cluster with some of the brighter cluster galaxies. PR Photo 04b/03 displays an image of a larger field (partially overlapping Photo 04a/03) in the light of ionized hydrogen – it was obtained by the Japanese 8.2-m Subaru telescope on Mauna Kea (Hawaii, USA). The field includes some of the large galaxies in this cluster, e.g., Messier 86, Messier 84 and NGC 4388. In order to show the faintest possible hydrogen emitting objects embedded in the outskirts of bright galaxies, their smooth envelopes have been “subtracted” during the image processing. This is why they look quite different in the two photos.

Clusters of galaxies are believed to have formed because of the strong gravitational pull from dark and luminous matter. The Virgo cluster is considered to be a relatively young cluster, because studies of the distribution of its member galaxies and X-ray investigations of hot cluster gas have revealed small “subclusters of galaxies” around the major galaxies Messier 87, Messier 86 and Messier 49. These subclusters are yet to merge to form a dense and smooth galaxy cluster.

The Virgo cluster is apparently cigar-shaped, with its longest dimension of about 10 million light-years near the line-of-sight direction – we see it “from the end”.

Stars in intracluster space
Galaxy clusters are dominated by dark matter. The largest fraction of the luminous (i.e. “visible”) cluster mass is made up of the hot gas that permeates all of the cluster. Recent observations of “intracluster” stars have confirmed that, in addition to the individual galaxies, the Virgo cluster also contains a so-called “diffuse stellar component”, which is located in the space between the cluster galaxies.

The first hint of this dates back to 1951 when Swiss astronomer Fritz Zwicky (1898-1974), working at the 5-m telescope at Mount Palomar in California (USA), claimed the discovery of diffuse light coming from the space between the galaxies in another large cluster of galaxies, the Coma cluster. The brightness of this intracluster light is 100 times fainter than the average night-sky brightness on the ground (mostly caused by the glow of atoms in the upper terrestrial atmosphere) and its measurement is difficult even with present technology. We now know that this intracluster glow comes from individual stars in that region.

Planetary nebulae
More recently, astronomers have undertaken a new and different approach to detect the elusive intracluster stars. They now search for Sun-like stars in their final dying phase during which they eject their outer layers into surrounding space. At the same time they unveil their small and hot stellar core which appears as a “white dwarf star”.

Such objects are known as “planetary nebulae” because some of those nearby, e.g. the “Dumbbell Nebula” (cf. ESO PR Photo 38a/98) resemble the disks of the outer solar system planets when viewed in small telescopes.

The ejected envelope is illuminated and heated by the very hot star at its centre. This nebula emits strongly in characteristic emission lines of oxygen (green; at wavelengths 495.9 and 500.7 nm) and hydrogen (red; the H-alpha line at 656.2 nm). Planetary nebulae may be distinguished from other emission nebulae by the fact that their main green oxygen line at 500.7 nm is normally about 3 to 5 times brighter than the red H-alpha line.
Search for intracluster planetary nebulae

An international team of astronomers [2] is now carrying out a very challenging research programme, aimed at finding intracluster planetary nebulae. For this, they observe the regions between cluster galaxies with specially designed, narrow-band optical filters tuned to the wavelength of the green oxygen lines.

The main goal is to study the overall properties of the diffuse stellar component in the nearby Virgo cluster. How much diffuse light comes from the intracluster space, how is it distributed within the cluster, and what is its origin?

Because the stars in this region are apparently predominantly old, the most likely explanation of their presence in this region is that they formed inside individual galaxies, which were subsequently stripped of many of their stars during close encounters with other galaxies during the initial stages of cluster formation. These “lost” stars were then dispersed into intracluster space where we now find them.

The Subaru observations
Japanese and European astronomers used the Suprime-Cam wide-field mosaic camera at the 8-m Subaru telescope (Mauna Kea, Hawaii, USA) to search for intracluster planetary nebulae in one of the densest regions of the Virgo cluster, cf. PR Photo 04b/03. They needed a telescope of this large size in order to select such objects and securely discriminate them from the thousands of foreground stars in the Milky Way and background galaxies.

In particular, by observing in two narrow-band filters sensitive to oxygen and hydrogen, respectively, the planetary nebulae visible in this field could be “separated” from distant (high-redshift) background galaxies, which do not have strong emission in both the green and red band. It is very time-consuming to observe the weak H-alpha emission and this can only be done with a big telescope.

Some 40 intracluster planetary nebulae candidates were found in this field which had the expected oxygen/H-alpha line intensity ratios of 3 – 5, such as those depicted PR Photo 04d/03. Unexpectedly, however, the data also showed a small number of star-like emission objects with oxygen/H-alpha line ratios of about 1. This is more typical of a cloud of ionized gas around young, massive stars – like the so-called HII regions in our own galaxy, the Milky Way.

However, it would be very unusual to find such star formation regions in the intracluster region, so follow-up spectroscopic observations were clearly needed for confirmation.

The VLT measurements
The only way to make sure that these unusual objects are actually powered by young stars is by a detailed spectroscopical study, analyzing the emitted light over a wide range of wavelengths. One of the objects was observed in this way in April 2002 with the FORS2 multi-mode instrument at the 8.2-m VLT YEPUN telescope at the ESO Paranal Observatory (Chile).

This was a most challenging observation, even for this very powerful facility, requiring several hours of exposure time. The brightness of the faint object (the flux of the oxygen [OIII 500.7]-line) was comparable to that of a 60-Watt light bulb at a distance of about 6.6 million km, i.e., about 17 times farther than the Moon.

The recorded (long-slit) spectrum (PR Photo 04e/03) is indeed that of an HII region, with characteristic emission lines from hydrogen, oxygen and sulphur, and with underlying blue “continuum” emission from hot, young stars. This is the first concrete evidence that some of the ionized hydrogen gas in the intracluster medium near NGC 4388 is heated by massive stars, rather than radiation from the nucleus of the galaxy.

Comparing the spectrum with simple starburst models showed that this HII region is “powered” by one or two hot and massive (O-type) stars. The best-fitting starburst model implies an estimated total mass of young stars of some 400 solar masses with an age of about 3 million years. The object is obviously very compact – it is indeed unresolved in all the images. The inferred radius of the HII region is about 11 light-years.

Young stars form far from galaxies
This compact star-forming region is located about 3.4 arcmin north and 0.9 arcmin west of the galaxy NGC 4388, corresponding to a distance of some 82,000 light-years (projected) from the main star-forming regions in this galaxy. The small cloud is moving away from us with an observed velocity of 2670 km/sec. This is considerably faster than the mean velocity of the Virgo cluster (about 1200 km/sec) but similar to that of NGC 4388 (2520 km/sec), indicating that it is probably falling through the Virgo cluster core together with NGC 4388, but it cannot have moved far during the comparatively short lifetime of its massive stars.

It is not known whether it once was or still is bound to NGC 4388, or whether it only belonged to the surroundings that fell into the Virgo cluster with this galaxy. In any case, the existence of this HII region is a clear demonstration that stars can form in the “diffuse” outskirts of galaxies, if not in intracluster space.

Because of internal dynamical processes, the stars in this object cannot remain forever in a dense cluster. Within a few hundred million years they will disperse and mix with the diffuse stellar population nearby. This isolated star formation is therefore likely to contribute to the intracluster stellar population, either directly, or after having moved away from the halo of NGC 4388.

This mode of isolated star formation does not contribute much to the total intracluster light emission – at the current rate it can explain only a small fraction of the diffuse light now observed in this region. However, it may have been more significant in the past, when protogalaxies and proto-galaxy groups, rich in neutral gas and with gas clouds at large distances from their centers, fell into the forming Virgo cluster for the first time.

Prospects
The existence of isolated compact HII regions like this one is important as a very different site of star formation than those normally seen in galaxies. The massive stars born in such isolated clouds will explode as supernovae and enrich the Virgo intracluster medium with metals.

Other possible – but not yet spectroscopically verified – compact HII regions in the halos of both Messier 86 and Messier 84 have been detected during this work. This finding thus also calls into question the current use of emission-line planetary nebulae luminosities as a distance indicator; to obtain the best possible accuracy, it will henceforth be necessary to weed out possible HII regions in the samples.

If compact HII regions exist generally in galaxies, they may possibly be the birthplaces of some of the young stars now observed in the halo of our Milky Way galaxy, high above the main plane. Observational programmes with both the Subaru and VLT telescopes are now planned to discover more of these interesting objects and to explore their properties.

Original Source: ESO News Release

Hubble Offers a Clear View of a Quasar

Image credit: Hubble

The Hubble Space Telescope has provided the clearest view of nearby Quasar 3C 273 ever taken in visible light. The image was taken by using the newly installed Advanced Camera for Surveys (ACS), which is able to block the brightest light to show the dimmer parts of the object. Features in the galaxy surrounding the central quasar are clearly visible.

NASA Hubble Space Telescope’s new Advanced Camera for Surveys (ACS) has provided the clearest visible-light view yet of the nearby quasar 3C 273. The ACS’ coronagraph was used to block the light from the brilliant central quasar, revealing that the quasar’s host galaxy is significantly more complex than had been suggested in previous observations. Features in the surrounding galaxy normally drowned out by the quasar’s glow now show up clearly. The ACS reveals a spiral plume wound around the quasar, a red dust lane, and a blue arc and clump in the path of the jet blasted from the quasar. These details had never been seen before. Previously known clumps of hot gas and the inner blue optical jet are now resolved more clearly.

The power of the ACS coronagraph is demonstrated in this picture. The Hubble image on the left, taken with the Wide Field Planetary Camera 2, shows the brilliant quasar but little else. The diffraction spikes demonstrate the quasar is truly a point-source of light (like a star) because the black hole’s “central engine” is so compact. Once the blinding “headlight beam” of the quasar is blocked by the ACS (right), the host galaxy pops into view. Note that the ACS’ occulting “finger” and other coronagraphic spot are seen in black near the top of the ACS High Resolution Channel image.

Quasars (also known as QSOs ? short for quasi-stellar objects) were discovered in the early 1960s, but at least two decades passed before astronomers had observational evidence that they reside in galaxies. They now are commonly accepted to be supermassive black holes accreting infalling gas and dust. Using the ACS, astronomers want to learn what activities in a quasar’s host galaxy feed the black hole, allowing it to “turn on” as a quasar.

Original Source: Hubble News Release

Rosetta Will Have to Be Dismantled

Now that Rosetta has been delayed indefinitely from its original mission to visit Comet Wirtanen, technicians have to dismantle the spacecraft and return each scientific instrument to the researchers who built them. The mission was cancelled because a recent report indicated that the Ariane 5 rocket was unsafe to launch. Rosetta’s original target was Comet Schwassmann-Wachmann 3, then Comet Wirtanen, so now planners are considering Comets Finlay, Brooks 2 and Wild 2. There’s no scheduled launch date, though.

Columbia Launches on Science Mission

Image credit: NASA

The Space Shuttle Columbia lifted off from Cape Canaveral yesterday, carrying the first Israeli astronaut and six crewmates on a scientific mission. Columbia blasted off at 1539 GMT (10:39 am EST) and reached orbit 9 minutes later. The astronauts have a total of 80 experiments to perform over the next 16 days.

Columbia lifted off from the Kennedy Space Center this morning on the first shuttle mission of the year, carrying the first Israeli astronaut into orbit along with six crewmates on a marathon international scientific research flight.

Commander Rick Husband, Pilot Willie McCool, Mission Specialists Dave Brown, Kalpana Chawla and Laurel Clark, Payload Commander Mike Anderson and Payload Specialist Ilan Ramon of the Israel Space Agency blasted off at 9:39 a.m. CST from Launch Pad 39-A. Less than nine minutes later, Columbia settled into an orbit inclined 39 degrees to the equator.

The seven astronauts will divide their duties into two teams working 12-hour shifts to conduct round-the-clock science. Aboard Columbia more than 80 experiments dealing with astronaut health and safety, advanced tehnology development and Earth and space sciences.

Husband, Chawla, Clark and Ramon comprise the Red team which will work in the pre-dawn and daytime hours, while McCool, Brown and Anderson make up the Blue team, working the evening and overnight hours.

Once in orbit, the crewmembers will begin to unstow gear and prepared for the opening of Columbia’s payload bay doors, before activating hardware and experiments in a double Spacehab research module housed in the shuttle’s cargo bay, which contains the lion’s share of the mission’s science. Other experiments housed in the cargo bay also will be activated, along with a special pallet of cryogenic fuel tanks at the rear of the cargo bay which will provide Columbia and its experiments sufficient electrical power for the duration of the flight.

Having shifted their sleep schedule to accommodate the dual-shift operations, McCool, Brown and Anderson will begin an abbreviated six-hour sleep period at 1:39 p.m. CST and will be awakened at 7:39 p.m. while Red team counterparts continue the early stages of experiment activation. Husband, Chawla, Clark and Ramon will begin an eight-hour sleep period at 8:39 p.m. and will be awakened Friday at 4:39 a.m. to handover work from the Blue team which will be continuing the initial phase of scientific studies overnight.

As Columbia was launched, the Expedition 6 crew aboard the International Space Station was orbiting over the northern Pacific Ocean south of the Aleutian island chain. Commander Ken Bowersox, Flight Engineer Nikolai Budarin and NASA ISS Science Officer Don Pettit are in their 54th day in space, their 52nd day on board the station.

The next STS-107 mission status report will be issued this evening, or earlier if events warrant.

Original Source: NASA News Release

NASA Announces Shuttle Launch Time

NASA announced the official launch time of the Space Shuttle Columbia on Wednesday, as part of its new policy of keeping the time secret until 24 hours before launch. If all goes well, the shuttle will lift off from Florida’s Cape Canaveral at 1539 GMT (10:39 am EST). The shuttle won’t dock with the International Space Station this mission, so there is a long launch window of 2.5 hours. The weather looks excellent for launch.

QuikScat Captures Images of Melting Ice Shelf

Image credit: NASA

An instrument on board NASA’s Quick Scatterometer spacecraft has detected the earliest melting in Antarctica’s Larsen Ice Shelf. This huge plate of glacier-fed ice has been disintegrating since 1995, losing nearly 10-percent of its size (more than two trillion tonnes of ice), and the most recent chunk disappeared due to a cyclone that sent warm weather into the area.

An international research team using data from NASA’s SeaWinds instrument aboard the Quick Scatterometer spacecraft has detected the earliest yet recorded pre-summer melting event in a section of Antarctica’s Larsen Ice Shelf. This huge, nearly 200 meter (656 foot) thick plate of glacier-fed floating ice, which in the late 1980s was about as large as Indiana, experienced dramatic disintegration events beginning in 1995 that have reduced its area by nearly 10 percent, or more than two trillion tons of ice.

Researchers Dr. Mark Drinkwater of the European Space Agency, Dr. David Long of Brigham Young University and Dr. Steve Harangozo of the British Antarctic Survey used near real time Quick Scatterometer (QuikScat) data to document a rapid, extensive melting of the Larsen C Ice Shelf in Antarctica’s Weddell Sea from Oct. 27 to Oct. 29, 2002. The melting, which extended to 68 degrees south, was triggered by a mid-latitude cyclone that delivered warm air to the region. The same storm is believed to have also caused a noticeable recession in the sea-ice margin to the west of the Antarctic Peninsula. The QuikScat images are available at: http://photojournal.jpl.nasa.gov/catalog/PIA03894

Air temperatures in the region typically exceed freezing for a few days on or after November 1 each year-a precursor to sustained summer melting that normally sets in several weeks later at these latitudes. The cumulative duration of these annual summer melting events is likely to have increased substantially over the past 50 years as summer average air temperatures on the eastern side of the Antarctic Peninsula have warmed appreciably (approximately two degrees Celsius, or 3.6 degrees Fahrenheit). Scientists believe these events are responsible for the previous breakups of Larsen and other ice shelves. Therefore, the ability to observe such events in near real time using scatterometers is of great interest to researchers, since they may provide invaluable clues to the fate of other, much larger Antarctic ice shelves.

While scientists used to believe there was no connection between recent Antarctic Peninsula warming and the natural cycle of deglaciation, recent field measurements provide some evidence to suggest the frequency of summer melting, and the resulting quantities of melt water penetrating ice shelves, may be connected with the accelerated disintegration of Larsen and other Antarctic ice shelves.

“The water is believed to penetrate cracks and fissures in the ice and refreeze at depth, where the ice is relatively colder,” said Drinkwater. “As the ice expands, this process effectively drives a wedge into existing cracks to accelerate the natural fracture process.”

Scatterometers operate by transmitting high-frequency microwave pulses to Earth’s surface and measuring the “backscattered,” or echoed, radar pulses bounced back to the satellite. Moshe Pniel, scatterometer projects manager at NASA’s Jet Propulsion Laboratory, Pasadena, Calif., which developed and manages the instruments, said scatterometers such as SeaWinds on QuikScat and a similar SeaWinds instrument on Japan’s recently launched Advanced Earth Observing Satellite 2 (Adeos 2), are proving to be increasingly important in monitoring land and ice processes.

“Scatterometers can effectively and quickly detect the difference between melting and dry surfaces,” he said. “They provide an important new tool in our capability to monitor climate change impacts on the Antarctic ice cover on a daily basis. These scatterometer data are vital in the southern hemisphere because near real time synthetic aperture radar data is not available there on a frequent, uninterrupted basis. QuikScat measurements being compiled and archived in the Scatterometer Climate Record Pathfinder study by Long and Drinkwater (http://www.scp.byu.edu) enable critical assessments of the links between changes taking place in global ice cover and associated changes in important elements of Earth’s closely-linked ocean-atmosphere climate system.”

QuikScat measurements and image data developed by Long are processed and distributed in near real time by the National Oceanic and Atmospheric Administration, providing scientists at the British Antarctic Survey and elsewhere with rapid access to low-resolution radar data that can be used to report melt events. The British Antarctic Survey compiles and distributes Antarctic Meteorological Station data in near real time.

More information about SeaWinds is available at: http://winds.jpl.nasa.gov/index.html.

NASA’s Earth Science Enterprise is a long-term research effort to understand and protect our home planet. The California Institute of Technology in Pasadena manages JPL for NASA.

Original Source: NASA/JPL News Release

Where Should the Next Martian Rovers Land?

Image credit: NASA

With only a few months to go before NASA launches its next two rovers to Mars, mission planners need to pin down exactly where they want the robot explorers to touch down. The twin Mars Exploration Rovers are scheduled for launch in May and June of 2003, and they currently have four candidate landing locations picked out – each of which offers unique terrain to explore. The final decision will be made in April.

The launch dates for the two Mars Exploration Rovers are getting closer and so is the need to pick a place for them to land.

Adventurous travelers might spin a globe and pick a vacation based on whichever spot their finger finds. But scientists and engineers working on NASA’s newest rover mission cannot be as casual about landing site choices for the twin rovers that will launch in May and June of this year.

Last week, team members and others from the scientific community met for a final chance to discuss and fine-tune the pros and cons of each of the four landing site contenders.

Images and data from two other NASA spacecraft currently orbiting the red planet — Mars Global Surveyor and Mars Odyssey — have provided invaluable information on possible landing sites.

“This is a unique period where we have orbital missions that can help us make the selection,” said Dr. Matt Golombek, JPL landing site scientist. “We want to go to sites with terrains that will challenge our minds but not the safety of the rovers.”

Since the rovers do not have the luxury of landing on a well-paved runway, JPL geologists and engineers must carefully choose an area without large rocks that could damage the rovers’ airbag landing system. Also, an area that is too densely populated with rocks of any size could prevent the rover from moving freely. Winds in the lower atmosphere are also an important consideration, as are the slopes the airbag-clad lander impact against.

Adequate exposure to the sun is vital for the solar-powered rovers. Geologists have chosen sites near the equator where there is sufficient sunlight. The sites are also relatively free of accumulations of iron-oxide dust particles that can coat solar panels and interfere with the rovers’ mobility.

Like the final four in any competition, each of the four Mars candidates is a potential winner.

“Three of the sites, Terra Meridiani, known as the Hematite site, Gusev, and Isidis show evidence for surface processes involving water. These sites appear capable of addressing the science objectives of the rover missions: to determine if water was present on Mars and whether there are conditions favorable to the preservation of evidence for ancient life,” said Golombek.

The fourth site, Elysium, appears to contain ancient terrain, which may hold clues to Mars’ early climate when conditions may have been wetter.

Over the next several months, geologists and engineers will continue to analyze the viability of each site. The final decision will be made by NASA in April, shortly before the rovers begin their journey to Mars.

Original Source: NASA/JPL News Release

Two Astronauts Go for a Spacewalk

Image credit: NASA

Astronauts Donald Pettit and Kenneth Bowersox enjoyed their first ever walk in space on Wednesday as they performed some maintenance work on the International Space Station. The walk was slightly delayed because of a sticky hatch, but after about 20 minutes they made it outside the station. They spent a total of 6 hours and 51 minutes outside the station.

Expedition 6 Commander Ken Bowersox and NASA Science Officer Don Pettit continued the assembly of the International Space Station today and set the stage for a series of complex shuttle construction flights to the complex later this year during a 6-hour, 51-minute spacewalk staged out of the Quest Airlock.

The spacewalk, which was the first for both Bowersox and Pettit, was the 50th excursion in support of the assembly and maintenance of the ISS, the 25th originated from the Station itself and the 16th conducted from Quest. Russian cosmonaut Nikolai Budarin supported the spacewalk from inside the ISS, acting as the spacewalk choreographer while operating television cameras on the Canadarm2 robotic arm.

After encountering some difficulty opening the airlock hatch due to a strap on the inside of the thermal hatch cover, the hatch finally swung open and Bowersox and Pettit began their spacewalk at 6:50 a.m. Central time by placing their suits on internal battery power. As he did, Bowersox reported a loss of digital data for his suit systems, requiring him to recycle his suit power that cleared up the momentary glitch. Once outside, Bowersox and Pettit quickly set up tools and gear, then moved to the recently installed Port One (P1) Truss segment, where they released ten remaining launch restraints from the truss? radiator system. Eight others had been released when the truss was delivered to the ISS last November on the STS-113 mission.

Flight controllers then sent commands to unfurl the P1?s center radiator, enabling it to extend to its fully deployed length of 75 feet, preparing the system for its activation later this year to provide cooling for station systems. The deployment took only 9 minutes to complete.

After inspecting some hardware on the P1 Truss for engineers on the ground, the two spacewalkers made their way to the Unity connecting node, where Pettit used Kapton tape to dab away small amounts of grit from a sealing ring on the nadir Common Berthing Mechanism, leaving the CBM in a pristine condition for the attachment of the Raffaello Multi-Purpose Logistics Module during the next shuttle flight to the station in March.

Bowersox and Pettit were unable to complete one minor task, the installation of a stanchion and a light fixture on one of two handcarts located on the Starboard One (S1) Truss which future spacewalkers will use to transport themselves up and down the station?s truss system. The stanchion would not release from its stowed position on the truss, apparently because of a pin interfering with its movement, and the task, considered a low priority for today?s spacewalk, was deferred to a future Expedition excursion.

As they neared the end of their spacewalk, Bowersox and Pettit returned to the center of the station, as Pettit retrieved tools from a storage box on the Z1 Truss and conducted a health check on an ammonia reservoir that was delivered to the P6 solar array truss structure in 2001. That ammonia system will be used to partially fill the cooling loops of the P1 Truss on an intricate shuttle assembly flight later this year that will occur in the midst of the reconfiguration of station power systems.

As they reentered the Quest Airlock, Bowersox and Pettit used a scissors to cut away the strap on the hatch cover which interfered with the rotation of the hatch handle at the start of the spacewalk. The hatch closed normally with no further problems expected in the future.

With their work completed, Bowersox and Pettit completed their spacewalk at 1:41p.m. Central time, raising the total spacewalk time for ISS assembly and maintenance to 312 hours and 11 minutes.

Before the spacewalk began, robotic engineers in Mission Control sent commands to move the station?s Mobile Transporter from the far end of the P1 Truss to its normal parking place at the centermost S0 Truss segment to protect its umbilical cable from any potential damage from orbital debris. The Transporter began its move from the P1 Truss to the S0 Truss at 1:53 a.m. Central time, latching itself in place about 20 minutes later.

The transporter is used to maneuver the Canadarm2 space crane up and down the length of the station?s trusses for assembly work. It had been parked on the P1 Truss during the STS-113 mission when it ran into a communication antenna on the truss, delaying its use for one of that flight?s spacewalks. Today, it moved back to its normal parking place uneventfully.

Bowersox, Budarin and Pettit will enjoy an off-duty day Thursday in the wake of today?s spacewalk before resuming their normal complement of scientific experiments and ISS housekeeping on Friday.

Original Source: NASA News Release

Nearest Brown Dwarf Found

Image credit: ESO

A team of European astronomers have located the closest brown dwarf star ever discovered. Epsilon Indi, located only 12 light-years from the Earth, was thought to be a single star, but the ESO team spotted its companion. Epsilon Indi B is 45 times the mass of Jupiter and takes 400 years to orbit the main star.

A team of European astronomers [2] has discovered a Brown Dwarf object (a ‘failed’ star) less than 12 light-years from the Sun. It is the nearest yet known.

Now designated Epsilon Indi B, it is a companion to a well-known bright star in the southern sky, Epsilon Indi (now “Epsilon Indi A”), previously thought to be single. The binary system is one of the twenty nearest stellar systems to the Sun.

The brown dwarf was discovered from the comparatively rapid motion across the sky which it shares with its brighter companion : the pair move a full lunar diameter in less than 400 years. It was first identified using digitised archival photographic plates from the SuperCOSMOS Sky Surveys (SSS) and confirmed using data from the Two Micron All Sky Survey (2MASS). Follow-up observations with the near-infrared sensitive SOFI instrument on the ESO 3.5-m New Technology Telescope (NTT) at the La Silla Observatory confirmed its nature and has allowed measurements of its physical properties.

Epsilon Indi B has a mass just 45 times that of Jupiter, the largest planet in the Solar System, and a surface temperature of only 1000 ?C. It belongs to the so-called ‘T dwarf’ category of objects which straddle the domain between stars and giant planets.

Epsilon Indi B is the nearest and brightest T dwarf known. Future studies of the new object promise to provide astronomers with important new clues as to the formation and evolution of these exotic celestial bodies, at the same time yielding interesting insights into the border zone between planets and stars.

Tiny moving needles in giant haystacks
Imagine you are a professional ornithologist, recently returned home from an expedition to the jungles of South America, where you spent long weeks using your high-powered telephoto lenses searching for rare species of birds. Relaxing, you take a couple of wide-angle snapshots of the blooming flowers in your back garden, undistracted by the common blackbird flying across your viewfinder. Only later, when carefully comparing those snaps, you notice something tiny and unusually coloured, flittering close behind the blackbird: you’ve discovered an exotic, rare bird, right there at home.

In much the same way, a team of astronomers [2] has just found one of the closest neighbours to the Sun, an exotic ‘failed star’ known as a ‘brown dwarf’, moving rapidly across the sky in the southern constellation Indus (The Indian). Interestingly, at a time when telescopes are growing larger and are equipped with ever more sophisticated electronic detectors, there is still much to be learned by combining old photographic plates with this modern technology.

Photographic plates taken by wide-field (“Schmidt”) telescopes over the past decades have been given a new lease on life through being digitised by automated measuring machines, allowing computers to trawl effectively through huge and invaluable data archives that are by far not yet fully exploited [3]. For the Southern Sky, the Institute for Astronomy in Edinburgh (Scotland, UK) has recently released scans made by the SuperCOSMOS machine of plates spanning several decades in three optical passbands. These data are perfectly suited to the search for objects with large proper motions and extreme colours, such as brown dwarfs in the Solar vicinity.
Everything is moving – a question of perspective

In astronomy, the `proper motion’ of a star signifies its apparent motion on the celestial sphere; it is usually expressed in arcseconds per year [4]. The corresponding, real velocity of a star (in kilometres per second) can only be estimated if the distance is known.

A star with a large proper motion may indicate a real large velocity or simply that the star is close to us. By analogy, an airplane just after takeoff has a much lower true speed than when it’s cruising at high altitude, but to an observer watching near an airport, the departing airplane seems to be moving much more quickly across the sky.

Proxima Centauri, our nearest stellar neighbour, is just 4.2 light-years away (cf. ESO PR 22/02) and has a proper motion of 3.8 arcsec/year (corresponding to 23 km/sec relative to the Sun, in the direction perpendicular to the line-of-sight). The highest known proper motion star is Barnard’s Star at 6 light-years distance and moving 10 arcsec/year (87 km/sec relative to the Sun). All known stars within 30 light-years are high-proper-motion objects and move at least 0.2 arcsec/year.

Trawling for fast moving objects
For some time, astronomers at the Astrophysical Institute in Potsdam have been making a systematic computerised search for high-proper-motion objects which appear on red photographic sky plates, but not on the equivalent blue plates. Their goal is to identify hitherto unknown cool objects in the Solar neighbourhood.

They had previously found a handful of new objects within 30 light-years in this way, but nothing as red or moving remotely as fast as the one they have now snared in the constellation of Indus in the southern sky. This object was only seen on the very longest-wavelength plates in the SuperCOSMOS Sky Survey database. It was moving so quickly that on plates taken just two years apart in the 1990s, it had moved almost 10 arcseconds on the sky, giving a proper motion of 4.7 arcsec/year. It was also very faint at optical wavelengths, the reason why it had never been spotted before. However, when confirmed in data from the digital Two Micron All Sky Survey (2MASS), it was seen to be much brighter in the infrared, with the typical colour signature of a cool brown dwarf.

At this point, the object was thought to be an isolated traveller. However, a search through available online catalogues quickly revealed that just 7 arcminutes away was a well-known star, Epsilon Indi. The two share exactly the same very large proper motion, and thus it was immediately clear the two must be related, forming a wide binary system separated by more than 1500 times the distance between the Sun and the Earth.

Epsilon Indi is one of the 20 nearest stars to the Sun at just 11.8 light years [5]. It is a dwarf star (of spectral type K5) and with a surface temperature of about 4000 ?C, somewhat cooler than the Sun. As such, it often appears in science fiction as the home of a habitable planetary system [6]. That all remains firmly in the realm of speculation, but nevertheless, we now know that it most certainly has a very interesting companion.

This is a remarkable discovery: Epsilon Indi B is the nearest star-like source to the Sun found in 15 years, the highest proper motion source found in over 70 years, and with a total luminosity just 0.002% that of the Sun, one of the intrinsically faintest sources ever seen outside the Solar System!

After Proxima and Alpha Centauri, the Epsilon Indi system is also just the second known wide binary system within 15 light years. However, unlike Proxima Centauri, Epsilon Indi B is no ordinary star.

Brown dwarfs: cooling, cooling, cooling …
Within days of its discovery in the database, the astronomers managed to secure an infrared spectrum of Epsilon Indi B using the SOFI instrument on the ESO 3.5-m New Technology Telescope (NTT) at the La Silla Observatory (Chile). The spectrum showed the broad absorption features due to methane and water steam in its upper atmosphere, indicating a temperature of ‘only’ 1000 ?C. Ordinary stars are never this cool – Epsilon Indi B was confirmed as a brown dwarf.

Brown dwarfs are thought to form in much the same way as stars, by the gravitational collapse of clumps of cold gas and dust in dense molecular clouds. However, for reasons not yet entirely clear, some clumps end up with masses less than about 7.5% of that of our Sun, or 75 times the mass of planet Jupiter. Below that boundary, there is not enough pressure in the core to initiate nuclear hydrogen fusion, the long-lasting and stable source of power for ordinary stars like the Sun. Except for a brief early phase where some deuterium is burned, these low-mass objects simply continue to cool and fade slowly away while releasing the heat left-over from their birth.

Theoretical discussions of such objects began some 40 years ago. They were first named ‘black dwarfs’ and later ‘brown dwarfs’, in recognition of their predicted very cool temperatures. However, they were also predicted to be very faint and very red, and it was only in 1995 that such objects began to be detected.

The first were seen as faint companions to nearby stars, and then later, some were found floating freely in the Solar neighbourhood. Most brown dwarfs belong to the recently classified spectral types L and T, below the long-known cool dwarfs of type M. These are very red to human eyes, but L and T dwarfs are cooler still, so much so that they are almost invisible at optical wavelengths, with most of their emission coming out in the infrared. [7].
How massive is Epsilon Indi B?

The age of most brown dwarfs detected to date is unknown and thus it is hard to estimate their masses. However, it may be assumed that the age of Epsilon Indi B is the same as that of Epsilon Indi A, whose age is estimated to be 1.3 billion years based on its rotational speed. Combining this information with the measured temperature, brightness, and distance, it is then possible to determine the mass of Epsilon Indi B using theoretical models of brown dwarfs.

Two independent sets of models yield the same result: Epsilon Indi B must have a mass somewhere between 4-6% of that of the Sun, or 40-60 Jupiter masses. The most likely value is around 45 Jupiter masses, i.e. well below the hydrogen fusion limit, and definitively confirming this new discovery as a bona-fide brown dwarf.

The importance of Epsilon Indi B
PR Photo 03c/03 shows the current census of the stars in the solar neighbourhood. All these stars have been known for many years, including GJ1061, which, however, only had its distance firmly established in 1997. The discovery of Epsilon Indi B, however, is an extreme case, never before catalogued, and the first brown dwarf to be found within the 12.5 light year horizon.

If current predictions are correct, there should be twice as many brown dwarfs as main sequence stars. Consequently, Epsilon Indi B may be the first of perhaps 100 brown dwarfs within this distance, still waiting to be discovered!

Epsilon Indi B is an important catch well beyond the cataloguing the Solar neighbourhood. As the nearest and brightest known brown dwarf and with a very accurately measured distance, it can be subjected to a wide variety of detailed observational studies. It may thus serve as a template for more distant members of its class.

With the help of Epsilon Indi B, astronomers should now be able to see further into the mysteries surrounding the formation and evolution of the exotic objects known as brown dwarfs, halfway between stars and giant planets, the physics of their inner cores, and the weather and chemistry of their atmospheres.

An historical note – the southern constellation Indus
The constellation Indus lies deep in the southern sky, nestled between three birds, Grus (The Crane), Tucana (The Toucan) and Pavo (The Peacock), cf. PR Photo 03d/03.

First catalogued in 1595-1597 by the Dutch navigators Pieter Dirkszoon Keyser and Frederick de Houtman, this constellation was added to the southern sky by Johann Bayer in his book ‘Uranometria’ (1603) to honour the Native Americans that European explorers had encountered on their travels.

In particular, it has been suggested that it is specifically the native peoples of Tierra del Fuego and Patagonia that are represented in Indus, just over two thousand kilometres south of La Silla where the first spectroscopic observations of Epsilon Indi B were made some 400 years later.

In the later drawing by Bode shown here, Epsilon Indi, the fifth brightest star in Indus, is associated with one of the arrows in the Indian’s hand.

Original Source: ESO News Release