First Science Data from LRO; ‘Tantalizing’ Hints of Water

This image shows daytime and nighttime lunar temperatures recorded by Diviner. Credit: NASA/UCLA

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The Lunar Reconnaissance Orbiter has successfully completed its testing and calibration phase and is now in its science and mapping orbit of the moon. Already, the spacecraft has made significant progress in creating the most detailed atlas of the moon’s south pole, and Thursday mission scientists reported some of the early science results, including “tantalizing” hints of water at the Moon’s south pole. So far, the data returned from LRO’s seven instruments “exceed our wildest expectations,” said Richard Vondrak, LRO project scientist at NASA Goddard Space Flight Center . “We’re looking at the moon now with new eyes.”

Last Tuesday, a final maneuver put LRO 50 km (31 miles) above the Moon, closer than any previous orbiter. LRO has already proved its keen eyes, imaging fine details of the Apollo landing sites earlier this summer with the LROC, the Lunar Reconnaissance Orbiter Camera.

Coldest place in the solar system

According to the first measurements from the Diviner instrument, which has infrared radiation detectors, LRO found that temperatures at about 35 Kelvin, or -238º Celsius deep in some permanently shaded regions. Vondrak said that these bitterly cold regions at the south pole “are perhaps the coldest part of the solar system.” With such cold temperatures, volatiles like water ice could be present, preserved for billions of years.

This image shows neutron flux detections around the lunar south pole from LEND. Credit: NASA/Institute for Space Research (Moscow)
This image shows neutron flux detections around the lunar south pole from LEND. Credit: NASA/Institute for Space Research (Moscow)

And indeed, first results from LRO’s Lunar Exploration Neutron Detector, or LEND instrument found hallmarks of hydrogen—a potential marker of water— not only in deep, dark craters, but in unexpected places as well.

“What it also seems to indicate is that the hydrogen is not confined to permanently shadowed craters,” said Vondrak. “Some of the permanently shadowed craters do indeed contain hydrogen. Others, on the other hand, do not appear to have hydrogen. And in addition, there appears to be concentrations of hydrogen that are not confined to the permanently shadowed regions.”


Surface topography

This mosaic shows altitude measurements from the LOLA instrument. Credit: NASA's Goddard Space Flight Center
This mosaic shows altitude measurements from the LOLA instrument. Credit: NASA's Goddard Space Flight Center

Data from LRO’s Lunar Orbiter Laser Altimeter, or LOLA, give scientists a detailed look at the topography of the lunar south pole, shown here. Red regions are high altitude, and blue regions are low altitude.

Some of the first results have turned up fresh craters, unknown boulders, and smooth sites that would be good landing sites for future humans or robotic missions. However, most regions are filled with rough terrain, which will make in situ exploration difficult. The roughness is probably a result of the lack of atmosphere and absence of erosion from wind or water, according to David Smith, LOLA principal investigator.

Another instrument, LRO’s Cosmic Ray Telescope for the Effects of Radiation instrument is exploring the lunar radiation environment and its potential effects on humans during record high, “worst-case” cosmic ray intensities accompanying the extreme solar minimum conditions of this solar cycle, showing damaging amounts of radiation at various points.

This Mini-RF image shows radar imagery of the lunar south pole. Credit: NASA/APL/LPI
This Mini-RF image shows radar imagery of the lunar south pole. Credit: NASA/APL/LPI

The Mini RF Technology Demonstration on LRO has confirmed communications capability and produced detailed radar images of potential targets for LRO’s companion mission, LCROSS, the Lunar Crater Observation and Sensing Satellite, which will impact the moon’s south pole on Oct. 9.

LRO’s prime science mission will last a year.

“The LRO instruments, spacecraft, and ground systems continue to operate essentially flawlessly,” said Craig Tooley, LRO project manager at Goddard “The team completed the planned commissioning and calibration activities on time and also got a significant head start collecting data even before we moved to the mission’s mapping orbit.”

“There’s still an awful lot to be done,” says Michael Wargo, chief lunar scientist at NASA Headquarters in Washington, D.C. “And the maps will only get better.”

See more information, including more images and flyover videos here.

ISS Canadarm2 Grabs Resupply Ship

The station’s robotic arm attaches the unpiloted Japanese H-II Transfer Vehicle (HTV) to the Earth-facing port of the Harmony node. Credit: NASA TV


In a true display of international cooperation, American flight engineer Nicole Stott, using Canada’s Canadarm2, captured the Japanese H-II Transfer Vehicle (HTV), with help from Belgium’s Frank DeWinne and Canada’s Robert Thirsk, under the direction of Russian ISS commander Gennady Padalka. The unpiloted HTV arrived at the International Space Station Thursday and later was attached to the Harmony node at 6:26 p.m. EDT. The HTV launched on Sept. 10, and took seven days to reach the ISS so controllers could run various tests and demonstrations on its maiden voyage.

“We had an amazing time doing this,” said Stott, “and we’re so happy to have this beautiful vehicle here. We look very much forward to going in tomorrow and finding all the supplies that I’m sure you’ve stored there for us.” The crew then offered a toast to the new vehicle with their recycled water drink bags.

Stott only had 99 seconds to latch onto the cargo ship before it moved past the station and into another orbit. It came to with nine meters (30 feet) away from the lab before going into free drift so it could be grabbed by the arm.

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The crew will open up the HTV on Friday afternoon.

The HTV can bring up to six tons of supplies to the ISS, and will be used to dispose of spent equipment, used clothing, and other waste material when it later undocks and burns up the Earth’s atmosphere during re-entry.

The success of the HTV is crucial for station re-supply, especially when the space shuttle is retired.

“After the space shuttle starts to fade away, we will take over responsibility to bring stuff up to the space station. We’re really looking forward to the success of this mission,” Japanese astronaut Soichi Noguchi, who is scheduled to launch to the ISS in December, said before HTV-1’s arrival.

Source: NASA

NASA Has a Little Fun With Buzz

Buzz Lightyear returns from 15 months in the ISS. Credit: NASA. Click for larger image.

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Buzz Lightyear, that is. The action figure returned from space on Sept. 11, aboard space shuttle Discovery’s STS-128 mission after 15 months aboard the International Space Station. Word has it that Disney is quite excited about his return, and will give him a ticker-tape parade on October 2, along with some of his his space station crewmates and the original Buzz, Apollo 11’s Buzz Aldrin, at Walt Disney World in Florida.

So what was Buzz doing on the ISS?

While in space Buzz supported NASA’s education outreach program — STEM (Science, Technology, Engineering and Mathematics)–by creating a series of fun educational online outreach programs. Following his return, Disney is partnering with NASA to create a new online educational game and an online mission patch competition for school kids across America. NASA will fly the winning patch in space. In addition, NASA plans to announce on Oct. 2, 2009, the details of a new exciting educational competition that will give students the opportunity to design an experiment for the astronauts on the space station.

Source: NASA

Searching for Life As We Don’t Know It

Artist's impression of exoplanets around other stars. Credits: ESA/AOES Medialab

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When discussing the possibility of finding life on other worlds, we usually add the phrase “life – as we know it.” But we’ve been surprised at exotic forms of life even on our own world and we need figure out how life might evolve elsewhere with foreign biochemistry in alien environments. Scientists at a new interdisciplinary research institute in Austria are working to understand exotic life and how we might find it.

Traditionally, planets that might sustain life are looked for in the ‘habitable zone’, the region around a star in which Earth-like planets with carbon dioxide, water vapor and nitrogen atmospheres could maintain liquid water on their surfaces. Consequently, scientists have been looking for biomarkers produced by extraterrestrial life with metabolisms resembling the terrestrial ones, where water is used as a solvent and the building blocks of life, amino acids, are based on carbon and oxygen. However, these may not be the only conditions under which life could evolve.

The University of Vienna established a research group for Alternative Solvents as a Basis for Life Supporting Zones in (Exo-)Planetary Systems in May 2009, under the leadership of Maria Firneis.

“It is time to make a radical change in our present geocentric mindset for life as we know it on Earth,” said Dr. Johannes Leitner, from the research group. “Even though this is the only kind of life we know, it cannot be ruled out that life forms have evolved somewhere that neither rely on water nor on a carbon and oxygen based metabolism.”

One requirement for a life-supporting solvent is that it remains liquid over a large temperature range. Water is liquid between 0°C and 100°C, but other solvents exist which are liquid over more than 200 °C. Such a solvent would allow an ocean on a planet closer to the central star. The reverse scenario is also possible. A liquid ocean of ammonia could exist much further from a star. Furthermore, sulphuric acid can be found within the cloud layers of Venus and we now know that lakes of methane/ethane cover parts of the surface of the Saturnian satellite Titan.

Consequently, the discussion on potential life and the best strategies for its detection is ongoing and not only limited to exoplanets and habitable zones. The newly established research group at the University of Vienna, together with international collaborators, will investigate the properties of a range of solvents other than water, including their abundance in space, thermal and biochemical characteristics as well as their ability to support the origin and evolution of life supporting metabolisms.

“Even though most exoplanets we have discovered so far around stars are probably gas planets, it is a matter of time until smaller, Earth-size exoplanets are discovered,” said Leitner.

The research group discussed their initial investigations at the European Planetary Science Conference in Potsdam, Germany.

Source: Europlanet

Space Shuttle Flushes the Toilet for All the World To See

Shuttle with water dump. Copyright Clair Perry

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This picture is from last week; September 9, 2009 to be exact, but I still wanted to share it. I just got in touch with photographer Clair Perry from Prince Edward Island, Canada to get his permission to post the image. No, this is not a comet. Pictured is space shuttle Discovery executing a water dump. The shuttle needed to get rid of excess waste water before landing the next day, and jettisoned it overboard via the waste water dump line, creating a spectacular visual effect as sunlight hit the spraying water. This dump occurred just as the shuttle was flying over North America last week, and lots of people witnessed this “toilet flush.” Some reports indicated it was “pristine” water (the shuttle fuel cells’ by-product is water) and other reports said it was “waste water and urine” (the Bad Astronomer called it Constellation Urion). Whatever, it was pretty. NASA said this was an unusually large dump, about 150 pounds (68 kg), because new regulations say no shuttle water dumps can take place while docked to the ISS, so as not to contaminate the outdoor experiments on the Kibo lab.

See below for the spectacular entire image, which also includes the nearby ISS creating a streak in the sky. Thanks to Clair Perry for sharing his images.

Shuttle and ISS on 9/9/09.  Copyright Clair-Perry
Shuttle and ISS on 9/9/09. Copyright Clair-Perry

And if you’re worried about the water ice freezing and becoming projectiles in orbit, NASA says that while waste water usually freezes upon jettison into a cloud of tiny ice droplets, when the sun hits, the ice sublimates directly into water vapor and disperses in space.

I remember the first time I saw a shuttle water dump. It was back in 2000, and I had gotten up early, about 4:45 am, to watch the shuttle pass over. But I saw this strange sight, like something was coming off of the shuttle. I ran inside and turned on NASA TV, just in time to see a view of a golden spray shooting out of the shuttle — the sunlight hitting the water at just the right angle made it look like a shimmering gold spray. Gold, not yellow.

God Particle

The Large Hadron Collider at CERN. Credit: CERN/LHC

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When the media talks about the “god particle”, they’re really talking about a theoretical particle in physics known as the higgs boson. If reality matches the predictions made by theoretical physics, the higgs boson is the particle that gives objects mass. It explains why objects at rest tend to stay at rest and objects in motion tend to stay in motion.

One of the primary goals of the Large Hadron Collider in Switzerland is to search for the so called “god particle”. When it finally gets running, the Large Hadron Collider, or LHC, will run beams of protons around a 27 kilometer circle, slamming them together at close to the speed of light. All the kinetic energy of the protons is instantly frozen out as mass in a shower of particles. Remember Einstein’s famous E=mc2 formula? Well, you can reconfigure the equation to be m = E/c2.

The higgs boson is thought to be a very heavy particle, and so it takes a lot of energy in the collider to create particles this massive. When the LHC starts running, it will collide protons at higher and higher energies, searching for the higgs boson. If it is found, it will confirm a theorized class of particles predicted by the theory of supersymmetry. And even if the higgs boson isn’t found, it will help disprove the theory. Either way, physicists win.

The term “god particle” was coined by physicist Leon Lederman, the 1988 Nobel prize winner in physics and the director of Fermilab. He even wrote a book called the “God Particle”, where he defended the use of the term.

We have written many articles about the Higgs Boson and the Large Hadron Collider here on Universe Today. Here’s an article about how the LHC won’t create a black hole and destroy the Earth. And here’s more on Fermilab’s search for the Higgs Boson.

We have also recorded an episode of Astronomy Cast all about the higgs boson. Listen to it here, Episode 69: The Large Hadron Collider and the Search for the Higgs Boson.

What is Cherenkov Radiation?

How the CANGAROO Imaging Cherenkov Air Telescope works

Cherenkov radiation is named after the Russian physicist who first worked it out in detail, in 1934, Pavel Alekseyevich Cherenkov (he got a Nobel for his work, in 1958; because he’s Russian, it’s also sometimes called Cerenkov radiation).

Nothing’s faster than c, the speed of light … in a vacuum. In the air or water (or glass), the speed of light is slower than c. So what happens when something like a cosmic ray proton – which is moving way faster than the speed of light in air or water – hits the Earth’s atmosphere? It emits a cone of light, like the sonic boom of a supersonic plane; that light is Cherenkov radiation.

The Cherenkov radiation spectrum is continuous, and its intensity increases with frequency (up to a cutoff); that’s what gives it the eerie blue color you see in pictures of ‘swimming pool’ reactors.

Perhaps the best known astronomical use of Cherenkov radiation is in ICATs such CANGAROO (you guessed it, it’s in Australia!), H.E.S.S. (astronomers love this sort of thing, that’s a ‘tribute’ to Victor Hess, pioneer of cosmic rays studies), and VERITAS (see if you can explain the pun in that!). As a high energy gamma ray, above a few GeV, enters the atmosphere, it creates electron-positron pairs, which initiate an air shower. The shower creates a burst of Cherenkov radiation lasting a few nanoseconds, which the ICAT detects. Because Cherenkov radiation is well-understood, the bursts caused by gamma rays can be distinguished from those caused by protons; and by using several telescopes, the source ‘on the sky’ can be pinned down much better (that’s what one of the Ss in H.E.S.S. stands for, stereoscopic).

The more energetic a cosmic ray particle, the bigger the air shower it creates … so to study really energetic cosmic rays – those with energies above 10^18 ev (which is 100 million times as energetic as what the LHC will produce), which are called UHECRs (see if you can guess) – you need cosmic ray detectors spread over a huge area. That’s just what the Pierre Auger Cosmic Ray Observatory is; and its workhorse detectors are tanks of water with photomultiplier tubes in the dark (to detect the Cherenkov radiation of air shower particles).

However I think the coolest use of Cherenkov radiation in astronomy is IceCube, which detects the Cherenkov radiation produced by muons in Antarctic ice … traveling upward. These muons are produced by rare interactions of muon neutrinos with hydrogen or oxygen nuclei (in the ice), after they have traveled through the whole Earth, from the Artic (and before that perhaps a few hundred megaparsecs from some distant blazer).

ICAT: imaging Cherenkov Air Telescope
CANGAROO: Collaboration of Australia and Nippon (Japan) for a Gamma Ray Observatory in the Outback
H.E.S.S.: High Energy Stereoscopic System
VERITAS: Very Energetic Imaging Telescope Array System
UHECR: ultra-high-energy cosmic ray

This NASA webpage gives more details of how ICATs work.

Quite a few Universe Today stories are about Cherenkov radiation; for example Astronomers Observe Bizarre Blazar with Battery of Telescopes, and High Energy Gamma Rays Go Slower Than the Speed of Light?.

Examples of Astronomy Casts which include this topic: Cosmic Rays, and Gamma Ray Astronomy.

Sources:
http://en.wikipedia.org/wiki/Cherenkov_radiation
http://abyss.uoregon.edu/~js/glossary/cerenkov_radiation.html

Weekend SkyWatcher’s Forecast – September 18-20, 2009

Greetings, fellow SkyWatchers! It’s an awesome weekend forecast for many of us attending Fall Star Parties, and all over the world we’re looking forward to moonless nights and the fellowship with our brother and sister amateur astronomers. If you’ve never been to a star party, try the Goggle pages for information… you just might find one going on near you! In the meantime, let’s have us a “Snowball” fight, chase some galaxies and ponder double stars! I’ll see you in the night…

Friday, September 18, 2009 – One of the most interesting features of the autumn sky is how slowly the stars and constellations seem to proceed across the heavens. This is only an illusion, since skydark arrives earlier each night (after summer solstice in the Northern Hemisphere), making the progress of the constellations across the sky seems to ‘‘freeze.’’ Tonight, Capella can be seen rising to the northeast just as Antares settles southwest. Four planets—Jupiter, Pluto, Neptune, and Uranus—are still above the horizon, with Jupiter now very low to the west-southwest. Descending to the northwest is Ursa Major, the ‘‘Big Dipper.’’ Across the sky is Piscis Austrinus, and lonely but bright Fomalhaut is beginning its rise. Seven stars of the first magnitude now grace the heavens. Against this backdrop, one of the darkest skies of the month is now upon us. It’s the New Moon…

Let’s have a look at another fine planetary nebula—NGC 7662. At 9 magnitude, this one is more commonly known as the ‘‘Blue Snowball’’ and can be found about three finger-widths east of Omicron Andromedae, or a little less than a handspan northwest of Alpha Pegasi (RA 23 25 54 Dec +42 32 06).

snowball

Similar in size to M57, even low power with a small scope easily reveals the planetary nature of this very fine study. Power up and you’ll discover that the annulus of this roughly circular planetary is definitely brighter inside than out. Large telescopes will highlight NGC 7662’s blue coloration and reveal a bright inner globe surrounded by a faint outer ring.

Saturday, September 19, 2009 – On this date in 1848, William Boyd was observing Saturn and discovered the planet’s eighth moon, Hyperion. If you’re out before sunset, some lucky stargazers are going to discover that the slender crescent Moon is about to occult Mercury! Check the Resources in this book and IOTA for locations and dates. Then check them both out in binoculars!

Would you like to try for another pair? Then wait until the skies are fully dark and head north for a galaxy and cluster pairing—NGC 6946 (RA 20 34 51 Dec +60 09 18) and NGC 6939 (RA 20 31 30
Dec +60 39 42).

6946

Located in western Cepheus, you’ll find them about a finger-width southwest of Eta.

6939Discovered by William Herschel on September 9, 1798, 10 million-light-year-distant face-on spiral NGC 6946 spreads itself pretty thin in modest instruments. Lacking a bright core, this oval mist orients southwest to northeast. Larger telescopes will reveal traces of rotating spiral arms, especially in the southwest. This galaxy would appear extraordinary if we weren’t looking through Milky Way obscuration to view it! Through smaller scopes, northwestern open cluster NGC 6939 appears like a tight little formation of 11th and 12th magnitude stars similar in pattern to a very small M11. It resolves well in larger scopes.

humboldtSunday, September 20, 2009 – Today we recognize the passing of cosmonaut Gherman S. Titov in 2000; Titov was not only the second human in space but also the youngest! Perhaps when he was orbiting Earth in Vostok 2 he had a chance to see the Moon. Why don’t we join him? Tonight, your lunar mission is to journey to the edge of the east limb and slightly south of central to identify crater Humboldt. Seen on the curve, this roughly 200-kilometer-wide crater holds a wealth of geographical details. Its flat, cracked floor has central peaks and a small mountain range, as well as a radial Rille structure. If libration and steadiness of skies are in your favor, power up and look for dark pyroclastic areas and a concentric inner crater.

betalyraeNow, let’s have a look at Beta and Gamma Lyrae, the lower two stars in the ‘‘Harp.’’ Beta is actually a quick-changing variable, which drops to less than half the brightness of Gamma in about 12 days. For a few days, the pair will seem of almost equal brightness, and then you will notice the star closest to Vega fade away. Beta is one of the most unusual spectroscopic stars in the sky, and it is possible that its eclipsing binary companion may be the prototype of a ‘‘collapsar’’ (yep, a black hole!), rather than a true luminous body.

Enjoy your weekend!!

This week’s awesome images (in order of appearance) are: NGC 7662 (credit—Adam Block/NOAO/AURA/NSF), NGC 6946 and NGC 6939 (credit—Palomar Observatory, courtesy of Caltech), Crater Humboldt (credit—Ricardo Borba) and Beta Lyrae (credit—Palomar Observatory, courtesy of Caltech). We thank you so much!!

IYA (Almost) Live Telescope!

Greetings! In case you weren’t tuned into Galactic TV yesterday… We had us a regular skyfest! Truly pristine dark skies ruled and the IYA “Live” telescope rocked the Aussie night away. For more than 8 hours we went from target to target – and loved every minute of it. While we could have done a lot more than four objects, allowing you time to enjoy them is a worthwhile effort, too. While I’d ordinarily spread this over a couple of days I’m going to post all our objects – M2, M41, M93 and M46 – right now because I’m outta’ here for the Hidden Hollow Star Party. Want to party at your end? Then check out information on our iPhone Galactic TV Weekend Marathon! Enjoy!!

Messier 2 or M2 (also designated NGC 7089) is a globular cluster in the constellation Aquarius, five degrees north of the star Beta Aquarii. It was discovered by Jean-Dominique Maraldi in 1746 and is one of the largest known globular clusters.

M2 was discovered by the French astronomer Jean-Dominique Maraldi in 1746 while observing a comet with Jacques Cassini. Charles Messier rediscovered it in 1760 but thought it a nebula without any stars associated with it. William Herschel was the first to resolve individual stars in the cluster, in 1794. M2 is, under extremely good conditions, just visible to the naked eye. Binoculars or small telescopes will identify this cluster as non-stellar while larger telescopes will resolve individual stars, of which the brightest are of apparent magnitude 13.1.

M2 is about 37,500 light-years away from Earth. At 175 light-years in diameter, it is one of the larger globular clusters known. The cluster is rich, compact, and significantly elliptical. It is 13 billion years old and one of the older globulars associated with the Milky Way Galaxy. M2 contains about 150,000 stars, including 21 known variable stars. Its brightest stars are red and yellow giants. The overall spectral type is F4.

Messier 41 (also known as M41 or NGC 2287) is an open cluster in the Canis Major constellation. It was discovered by Giovanni Batista Hodierna before 1654 and was perhaps known to Aristotle about 325 BC.

M41 lies about four degrees almost exactly south of Sirius. It contains about 100 stars including several red giants, the brightest being a spectral type K3 giant near the cluster’s center. The cluster is estimated to be moving away from us at 23.3 km/s. The diameter of the cluster is between 25 and 26 light years. Its age is estimated at between 190 and 240 million years old. M41 is also referred to as NGC 2287.

Messier 93 (also known as M 93 or NGC 2447) is an open cluster in the constellation Puppis. It was discovered by Charles Messier in 1781.

M93 is at a distance of about 3,600 light years from Earth and has a spatial radius of some 10 to 12 light years. Its age is estimated at some 100 million years.

Messier 46 (also known as M 46 or NGC 2437) is an open cluster in the constellation of Puppis. It was discovered by Charles Messier in 1771. Dreyer described it as “very bright, very rich, very large.” M46 is about 5,500 light-years away with an estimated age on the order of several 100 million years.

The planetary nebula NGC 2438 appears to lie within the cluster near its northern edge, but it is most likely unrelated since it does not share the cluster’s radial velocity. The case is yet another example of a superposed pair, joining the famed case of NGC 2818.

M46 is about a degree east of M47 in the sky, so the two fit well in a binocular or wide-angle telescope field.

If you had fun with this, then make sure to tune into your TVU Channel Number 79924 on your iPhone for a weekend marathon of all the best of our IYA Live Telescope! Wishing you all clear skies and a great weekend….

Factual information courtesy of Wikipedia.

Planck First Light

Strips of the sky measured by Planck. Credit: ESA

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One of the newest telescopes in space, the Planck spacecraft, recently completed its “first light” survey which began on August 13. Astronomers say the initial data, gathered from Planck’s vantage point at the L2 point in space, is excellent. Planck is studying the Cosmic Microwave Background, looking for variations in temperature that are about a million times smaller than one degree. This is comparable to measuring from Earth the body heat of a rabbit sitting on the Moon.

The initial survey yielded maps of a strip of the sky, one for each of Planck’s nine frequencies. Each map is a ring, about 15° wide, stretching across the full sky.

The the differences in color in the strips indicate the magnitude of the deviations of the temperature of the Cosmic Microwave Background from its average value, as measured by Planck at a frequency close to the peak of the CMB spectrum (red is hotter and blue is colder).

The large red strips trace radio emission from the Milky Way, whereas the small bright spots high above the galactic plane correspond to emission from the Cosmic Microwave Background itself.

In order to do its work, Planck’s detectors must be cooled to extremely low temperatures, some of them being very close to absolute zero (–273.15°C, or zero Kelvin, 0K).

Routine operations are now underway, and surveying will continue for at least 15 months without a break. In approximately 6 months, the first all-sky map will be assembled.

Within its projected operational life of 15 months, Planck will gather data for two complete sky maps. To fully exploit the high sensitivity of Planck, the data will require delicate adjustments and careful analysis. It promises to return a treasure trove that will keep both cosmologists and astrophysicists busy for decades to come.

Source: ESA