“The galaxy, a spiral beauty called Messier 94, is located about 17 million light-years away. In this image from NASA’s Spitzer Space Telescope, infrared light is represented in different colors, with blue having the shortest wavelengths and red, the longest.

How many rings do you see in this new image of the galaxy Messier 94, also known as NGC 4736? While at first glance one might see a number of them, astronomers believe there is just one. This image was captured in infrared light by NASA’s Spitzer Space Telescope.

Historically, Messier 94 was considered to have two strikingly different rings: a brilliant, compact band encircling the galaxy’s core, and a faint, broad, swath of stars falling outside its main disk.

Astronomers have recently discovered that the outer ring, seen here in the deep blue glow of starlight, might actually be more of an optical illusion. A 2009 study combined infrared Spitzer observations with those from other telescopes, including ultraviolet data from NASA’s Galaxy Evolution Explorer, now operated by the California Institute of Technology, Pasadena; visible data from the Sloan Digital Sky Survey; and shorter-wavelength infrared light from the Two Micron All Sky Survey (2MASS). This more complete picture of Messier 94 indicates that we are really seeing two separate spiral arms, which, from our perspective, take on the appearance of a single, unbroken ring.

The bright inner ring of Messier 94 is very real, however. This area is sometimes identified as a “starburst ring” because of the frenetic pace of star formation in the confined area. Starbursts like this can often be triggered by gravitational encounters with other galaxies, but in this case might be caused by the galaxy’s oval shape.”

See the full article here.

Jet Propulsion Laboratory (JPL) is a federally funded research and development center and NASA field center located in the San Gabriel Valley area of Los Angeles County, California, United States. Although the facility has a Pasadena postal address, it is actually headquartered in the city of La Cañada Flintridge [1], on the northwest border of Pasadena. JPL is managed by the nearby California Institute of Technology (Caltech) for the National Aeronautics and Space Administration. The Laboratory’s primary function is the construction and operation of robotic planetary spacecraft, though it also conducts Earth-orbit and astronomy missions. It is also responsible for operating NASA’s Deep Space Network.

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Brookhaven Lab

Approach could be useful in fabricating new kinds of materials with engineered properties

May 16, 2013
Contacts: Karen McNulty Walsh, (631) 344-8350 or Peter Genzer, (631) 344-3174

“Scientists at the U.S. Department of Energy’s Brookhaven National Laboratory have discovered that DNA “linker” strands coax nano-sized rods to line up in way unlike any other spontaneous arrangement of rod-shaped objects. The arrangement—with the rods forming “rungs” on ladder-like ribbons linked by multiple DNA strands—results from the collective interactions of the flexible DNA tethers and may be unique to the nanoscale. The research, described in a paper published online in ACS Nano, a journal of the American Chemical Society, could result in the fabrication of new nanostructured materials with desired properties.

DNA-tethered nanorods link up like rungs on a ribbonlike ladder—a new mechanism for linear self-assembly that may be unique to the nanoscale.
‘This is a completely new mechanism of self-assembly that does not have direct analogs in the realm of molecular or microscale systems,’ said Brookhaven physicist Oleg Gang, lead author on the paper, who conducted the bulk of the research at the Lab’s Center for Functional Nanomaterials (CFN).

Alexei Tkachenko, the CFN scientist who developed the theory to explain the exceptional arrangement, elaborated: ‘Remarkably, the system has all three dimensions to live in, yet it chooses to form the linear, almost one-dimensional ribbons. It can be compared to how extra dimensions that are hypothesized by high-energy physicists become hidden, so that we find ourselves in a 3-D world.’

Schematic of how gold nanorods link up when complementary strands of DNA attached to each rod (A, A’)—or DNA linker strands with ends complementary to two different types of DNA tethers on adjacent rods (B, C)—are used as “glue.”

See the full article here. There is much more.

One of ten national laboratories overseen and primarily funded by the Office of Science of the U.S. Department of Energy (DOE), Brookhaven National Laboratory conducts research in the physical, biomedical, and environmental sciences, as well as in energy technologies and national security. Brookhaven Lab also builds and operates major scientific facilities available to university, industry and government researchers. Brookhaven is operated and managed for DOE’s Office of Science by Brookhaven Science Associates, a limited-liability company founded by Stony Brook University, the largest academic user of Laboratory facilities, and Battelle, a nonprofit, applied science and technology organization.

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May 16, 2013
Mike Ross

“The US Senate has unanimously confirmed MIT physics professor Ernest Moniz as the next Secretary of Energy.

Ernest Moniz

Ernest Moniz, an MIT physics professor with extensive experience with particle accelerators and national energy policies, has been confirmed in a unanimous vote by the US Senate as the next Secretary of Energy.

The Department of Energy is the single largest supporter of particle physics, and of basic research in the physical sciences, in the United States.

Moniz succeeds Steven Chu, also a physicist, who served during the Obama administration’s first term and who announced Feb. 1 that he would be stepping down. After the transition, Chu will be joining the faculty of Stanford University.

Coincidentally, Moniz also has a Stanford connection. He earned his PhD in theoretical nuclear physics there in January 1972.

After postdoctoral research stints in Saclay, France, and the University of Pennsylvania, Moniz joined MIT’s physics faculty in 1973. He was director of the DOE-funded Bates Linear Accelerator Center from 1983 to 1991. In the 1990s, Moniz became more active in the national energy policy discussion. He served the Clinton Administration as associate director for science in the White House’s Office of Science and Technology Policy (1995-97) and then as DOE undersecretary (1997-2001). In 2006, he was named director of the MIT Energy Initiative and the Laboratory for Energy and the Environment.

‘Taken together, these roles have given me a deep appreciation of DOE’s importance to American leadership in science,’ Moniz said in his April 9 written statement to the Senate committee reviewing his nomination. ‘DOE is the lead funder of basic research in the physical sciences and provides the national research community with unique research opportunities at major facilities for nuclear and particle physics, energy science, materials research and discovery, large-scale computation and other disciplines. DOE operates an unparalleled national laboratory system and partners with both university and industry at the research frontier.

‘The Secretary of Energy has the responsibility for stewardship of a crucial part of the American basic research enterprise. If confirmed, I will work with the scientific community and with Congress to assure that our researchers have continuing access to cutting-edge research tools for scientific discovery and for training the next generation.’

With a 21-1 vote, the committee approved Moniz’s nomination on April 18.”

See the full article here. Best of luck to the new Secretary and to us here in the embattled scientific community.

Symmetry is a joint Fermilab/SLAC publication.

Fermilab is an enduring source of strength for the US contribution to scientific research world wide.

Friday, May 17, 2013
Don Lincoln

“The world of particle physics and cosmology is full of invisible phenomena like dark matter, neutrinos and that latest spiffy object predicted by the theory of the week. When you think about it, it’s really quite hard to measure some of the properties of these invisible particles. So scientists had to come up with some clever ways to determine things like the mass of something that cannot be detected directly. One such way involves careful accounting of the energy observed in the experiment.

When scientists were first studying beta decay, they expected the electron to be emitted with a single unique energy, as depicted in red. However, they measured instead a range of energies for the emitted electron, shown in yellow, all lower than the expected energy, which the electron would carry if neutrinos didn’t exist. In the lower right hand corner, we see a closeup of the spectrum near the expected energy. The dashed line is what we see if the neutrino has no mass, while the magenta curve is what we’d see if the neutrino had a small but non-zero mass. CMS scientists employed this technique to study top quark production to validate the method.

This technique has been used in the past. A type of radioactivity called beta decay occurs when a neutron in the nucleus of an atom converts to a proton and emits an electron. Following the principle of energy conservation, scientists predicted the electron to be emitted with a single energy, but measurements showed that the energy of the electron can have many different values. In fact, it turned out that the predicted value of the electron’s energy was actually the maximum it could be. The measured values were always lower.

In 1930 Wolfgang Pauli proposed a solution to this curious situation: Not only were a proton and an electron emitted in beta decay, but a neutrino was emitted as well. Neutrinos are particles that interact only via the weak nuclear force and are therefore very, very hard to detect. Clyde Cowan and Frederick Reines showed the idea to be correct in 1955 when the neutrino was detected.

See the full article here.

Fermi National Accelerator Laboratory (Fermilab), located just outside Batavia, Illinois, near Chicago, is a US Department of Energy national laboratory specializing in high-energy particle physics.

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“Already celebrated for bringing the world news of the Higgs boson, the Large Hadron Collider is only beginning its long journey of discoveries. Yet scientists are already planning the next big machine, the International Linear Collider [read Linear Collider, from the linear Collider Collaboaration], to study the LHC’s discoveries in more detail.

So what’s the difference between the LHC and the proposed ILC? Why do we need both?

LHC

Linear Collider.

For one thing, the ILC would accelerate particles along a straight line some 30 kilometers long while the LHC accelerates them along a circular path 27 kilometers in circumference. But that just skims the surface of their differences.

The two types of machine provide very different types of information because they collide different kinds of particles. The LHC collides protons, which themselves are made up of quarks and gluons. The ILC, in contrast, would collide electrons and positrons, point-like particles that have no known internal structure. Proton collisions are messy, allowing scientists to discover new particles and new processes, while linear-collider experiments are cleaner, allow scientists to explore these new particles and new processes without the complicated debris present at the LHC.

Not clear? Maybe this image helps. The protons in the LHC aren’t just single particles; they are each made of a list of ingredients (up quarks, a down quark and gluons)…That’s why the LHC produces the mind-boggling number of collisions that it does.

See the full scintillating article here.

Symmetry is a joint Fermilab/SLAC publication.

Wednesday, May 15, 2013

Craig Hogan, director of the Center for Particle Astrophysics, wrote this column.

“The first great breakthrough of 20th-century physics came just as it dawned, in late 1900, when Max Planck derived from simple quantum principles an exact universal formula for the spectrum, or amount of light at each frequency, emitted by opaque matter.

A related breakthrough in cosmology came many decades later, when it was found that radiation with precisely Planck’s spectrum is found not only in the laboratory, but also coming from all directions in the sky. This simple fact carries a profound message about cosmic history: The entire universe is expanding from a state when matter everywhere was once hot, dense and opaque. The cosmic radiation is left over from the earliest moments of the cosmic expansion—the big bang.

In recent decades, measurements have shown that the cosmic radiation is not at exactly just one temperature, but varies by a tiny amount in different directions—a little colder here, a little hotter there. The early universe was not perfectly uniform, which is a good thing, because those tiny variations eventually led to the formation of galaxies and, of course, us.

Measurements of cosmic background radiation have advanced rapidly in the last year with new high-resolution detectors in Chile and at the South Pole and with the release in March of definitive all-sky data from the Planck satellite. Some of these results offer tantalizing hints of new physics beyond the Standard Model…Fermilab scientists invented many techniques of precision cosmology, helped create the Sloan Digital Sky Survey that defines the state of the art in precision measurement of cosmic structure with galaxies, and are about to start operating a still deeper cosmic mapping project, the Dark Energy Survey. Exciting choices lie ahead as we plan our participation in future experiments, perhaps including measurements of cosmic background radiation.”

See the full and very interesting article here.

Fermi National Accelerator Laboratory (Fermilab), located just outside Batavia, Illinois, near Chicago, is a US Department of Energy national laboratory specializing in high-energy particle physics.

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14 May 2013
Cian O’Luanaigh

“An international team of physicists at the radioactive-beam facility ISOLDE at CERN have for the first time measured the ionization potential of the rare radioactive element astatine.

Part of the resonance ionization laser ion source (RILIS) at ISOLDE (Image: ISOLDE/CERN)

The value for astatine, published today in the journal Nature Communications, could help chemists to develop applications for the element in radiotherapy, and will serve as a benchmark for theories that predict the structure of super-heavy elements.

The ionization potential of an element is the energy needed to remove one electron from the atom, thereby turning it into an ion. This measurement is related to the chemical reactivity of an element and, indirectly, to the stability of its chemical bonds in compounds.

See the full article here.

Meet CERN in a variety of places:

Cern Courier

THE FOUR MAJOR PROJECT COLLABORATIONS

ATLAS

ALICE

CMS

LHCb

LHC

Quantum Diaries

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05.14.2013
Ruth Dasso Marlaire
Public Affairs Office
Ames Research Center, Moffett Field, Calif.
650-604-4789

“Scientists at NASA’s Ames Research Center, Moffett Field, Calif., now have the capability to systematically investigate the molecular evolution of cosmic carbon. For the first time, these scientists are able to automatically interpret previously unknown infrared emissions from space that come from surprisingly complex organic molecules, called polycyclic aromatic hydrocarbons (PAHs), which are abundant and important across the universe.

For the first time, scientists are able to automatically interpret previously unknown infrared emissions from space that come from surprisingly complex organic molecules, called polycyclic aromatic hydrocarbons (PAHs), which are abundant and important across the universe. They use spectra of infrared radiation to identify unknown substances in space. These spectra are as good as fingerprints for identification purposes. Analyzing the PAH bands represents a powerful new astronomical tool to trace the evolution of cosmic carbon and, at the same time, probe conditions across the universe. Image credit: NASA Ames

Between 2003 and 2005, thanks to its unprecedented sensitivity, NASA’s Spitzer Space Telescope, managed and operated by NASA’s Jet Propulsion Laboratory, Pasadena, Calif., created maps of the tell-tale PAH signature across large regions of space, from hot regions of harsh ultraviolet (UV) radiation close to stars, to cold, dark clouds where stars and planets form. By exclusively using their unique collection of authentic PAH spectra, coupled with algorithm-driven, blind-computational analyses, scientists at Ames were able to interpret the cosmic infrared maps with complex organic molecules. They found that PAHs changed significantly in size, electrical charge and structure, to adjust to the different environment at each spot in the map. Carbon is one of the most abundant atoms in space and scientists believe that the spectral changes across these maps trace the molecular evolution of carbon across the universe.

The Spitzer Space Telescope is a NASA mission managed by the Jet Propulsion Laboratory located on the campus of the California Institute of Technology and part of NASA’s Infrared Processing and Analysis Center.

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NASA Chandra

“A giant black hole in the center of the galaxy 4C+29.30 is generating two powerful jets of particles. By combining X-rays (blue), optical (gold), and radio (pink) data, astronomers get a full picture of what is happening. The X-rays reveal superheated gas swirling around the black hole, some of which may eventually be consumed by it. The black hole at the center of 4C+29.30 is thought to be about 100 million times more massive than our Sun.

Composite

X-ray

Optical

Radio

Credit X-ray: NASA/CXC/SAO/A.Siemiginowska et al; Optical: NASA/STScI; Radio: NSF/NRAO/VLA
Release Date May 15, 2013

This composite image of a galaxy illustrates how the intense gravity of a supermassive black hole can be tapped to generate immense power. The image contains X-ray data from NASA’s Chandra X-ray Observatory (blue), optical light obtained with the Hubble Space Telescope (gold) and radio waves from the NSF’s [NRAO] Very Large Array (pink).

This multi-wavelength view shows 4C+29.30, a galaxy located some 850 million light years from Earth. The radio emission comes from two jets of particles that are speeding at millions of miles per hour away from a supermassive black hole at the center of the galaxy. The estimated mass of the black hole is about 100 million times the mass of our Sun. The ends of the jets show larger areas of radio emission located outside the galaxy.

The X-ray data show a different aspect of this galaxy, tracing the location of hot gas. The bright X-rays in the center of the image mark a pool of million-degree gas around the black hole. Some of this material may eventually be consumed by the black hole, and the magnetized, whirlpool of gas near the black hole could in turn, trigger more output to the radio jet.

See the full article here.

Chandra X-ray Center, Operated for NASA by the Smithsonian Astrophysical Observatory

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15 May 2013
Contacts

Amelia Stutz
Max Planck Institute for Astronomy
Heidelberg, Germany
Tel: +49 6221 528 412
Email: stutz@mpia.de

Thomas Stanke
ESO
Garching bei München, Germany
Tel: +49 89 3200 6116
Email: tstanke@eso.org

Richard Hook
ESO Public Information Officer
Garching bei München, Germany
Tel: +49 89 3200 6655
Cell: +49 151 1537 3591
Email: rhook@eso.org

“This dramatic new image of cosmic clouds in the constellation of Orion reveals what seems to be a fiery ribbon in the sky. This orange glow represents faint light coming from grains of cold interstellar dust, at wavelengths too long for human eyes to see. It was observed by the ESO-operated Atacama Pathfinder Experiment (APEX) in Chile.

Clouds of gas and interstellar dust are the raw materials from which stars are made. But these tiny dust grains block our view of what lies within and behind the clouds — at least at visible wavelengths — making it difficult to observe the processes of star formation.

This is why astronomers need to use instruments that are able to see at other wavelengths of light. At submillimetre wavelengths, rather than blocking light, the dust grains shine due to their temperatures of a few tens of degrees above absolute zero. The APEX telescope with its submillimetre-wavelength camera LABOCA, located at an altitude of 5000 metres above sea level on the Chajnantor Plateau in the Chilean Andes, is the ideal tool for this kind of observation.

This spectacular new picture shows just a part of a bigger complex called the Orion Molecular Cloud, in the constellation of Orion (The Hunter). A rich melting pot of bright nebulae, hot young stars and cold dust clouds, this region is hundreds of light-years across and located about 1350 light-years from us. The submillimetre-wavelength glow arising from the cold dust clouds is seen in orange in this image and is overlaid on a view of the region taken in the more familiar visible light.

A picture of Barnard’s Loop, which is a primary component of the nebula complex. Also seen in the image are the locations of other nebulae in the complex such as M42.

The large bright cloud in the upper right of the image is the well-known Orion Nebula, also called Messier 42. It is readily visible to the naked eye as the slightly fuzzy middle “star” in the sword of Orion. The Orion Nebula is the brightest part of a huge stellar nursery where new stars are being born, and is the closest site of massive star formation to Earth.

The APEX observations used in this image were led by Thomas Stanke (ESO), Tom Megeath (University of Toledo, USA), and Amelia Stutz (Max Planck Institute for Astronomy, Heidelberg, Germany). APEX is a collaboration between the Max Planck Institute for Radio Astronomy (MPIfR), the Onsala Space Observatory (OSO) and ESO. Operation of APEX at Chajnantor is entrusted to ESO.”

See the full article here.

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THE BASIC TOOLS OF E.S.O.

Paranal Platform The VLT

NTT – New Technology Telescope

La Silla

ALMA Atacama Large Millimeter/submillimeter Array

The European Extremely Large Telescope
VISTA (the Visible and Infrared Survey Telescope for Astronomy)

Atacama Pathfinder Experiment telescope (APEX)

ESO, European Southern Observatory, builds and operates a suite of the world’s most advanced ground-based astronomical telescopes.

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