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Should the Square Kilometre Array telescope be shared between South Africa and Australasia?

By James Dacey

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Since 2006, South Africa has been battling it out with Australasia for the right to host the Square Kilometre Array (SKA). This €1.5bn radio-astronomy telescope, consisting of 2000 to 3000 linked antennas, will probe the first 100 million years after the Big Bang for clues about galaxy evolution, dark matter and dark energy. Last Friday – after months of deliberation – the SKA committee finally reached its decision, which came as a surprise to many outside of the astronomy community: a split-site solution whereby part of the array will be constructed in South Africa and the other part in Australia and New Zealand.

It appears that in reaching this decision a certain degree of politics has been involved. A report submitted by the SKA Site Advisory Committee last February concluded that, while both sites were suitable, South Africa was the preferred choice. But the SKA members also received advice from a separate working group that was set up to consider the dual-site option. We want you to let us know what you think about the decision by taking part in our poll.

Should the Square Kilometre Array telescope be shared between South Africa and Australasia?

Yes, it is a good compromise
No, it should be built exclusively in South Africa
No, it should be built exclusively in Australia and New Zealand

Have your say by visiting our Facebook page. As always, please feel free to explain your response by posting a comment on the Facebook poll.

In last week’s poll we shifted away from current events all the way back to ancient Greece. We asked you to select the famous thinker whom you considered to have made the most important contributions to natural philosophy. The most highly regarded among our list of seven ancient Greeks was Archimedes, who picked up 45% of the vote. Second place went to Aristotle (23%) and third place went to Euclid with 11%.

Given the magnitude and diversity of these philosophers’ contributions, the poll naturally attracted debate among voters. For instance, Jonas Persson voted for Archimedes but he appears to have been somewhat torn: “Difficult to answer with one person and without a discussion. For modern science, I would say Archimedes. But the influence of Plato is one of the main reasons for the Copernican revolution. Aristotle was more into biology. Thales was the first, so hard to say,” he wrote. Alan Saed, who opted for Euclid, was more forthright in his opinion: “Aristotle should not be up there in the list at all! He held back scientific progress for more than a millennia.”

Thank you for your participation and we look forward to hearing from you in this week’s poll.

DNA tiles pave the way

This image may look like a collection of novelty spaghetti shapes but these detailed figures are in actual fact made from assemblies of DNA strands as imaged by an atomic force microscope (AFM). It is the demonstration of a pioneering technique, developed at Harvard University in the US, for engineering complex nanoscale structures from a set of DNA “tiles”.

The concept of fashioning nanoscale structures out of individual strands of DNA has been developed over the past three decades. The field has gathered momentum since the emergence in 2006 of a technique known as “DNA origami”, which enables scientists to fold long single strands of DNA into a wide range of predetermined shapes. These resulting nanostructures can be used as scaffolding or as miniature circuit boards for precisely assembling components such as carbon nanotubes and nanowires.

But despite early applications and the great promise of the origami technique, there are limitations with the production process relating to time and expense. In coercing DNA into folding, scientists must attach several hundred staples to the area surrounding the single strands. Each shape requires a different set of staples, which cost approximately £640 each, and the entire process from design through to fabrication typically takes a week.

Molecular canvas

In this latest research, Peng Yin and colleagues at Harvard University have developed an alternative technique for DNA engineering, based on an earlier manipulation approach that dates back to the 1990s. Instead of starting with one long strand of DNA and folding it, Yin’s team takes a number of shorter single strands of DNA and arrange them into a “molecular canvas” by controlling their local interactions.

It works because the DNA has been programmed to have specific sequences of bases: each single strand comprises 42 bases divided into four sequences of 10 or 11 bases. Single strands are then folded up into rectangles, or “tiles”, that are mixed together with other tiles in an environment where each sequence will only be attracted to one other complementary sequence. In this way, researchers can create specific shapes through the selection of sequences.

Reporting its findings in Nature, Yin’s group demonstrates its technique by presenting these AFM images of 100 distinct shapes including the capital letters of the Latin alphabet, emoticons and astrological symbols, with each shape taking just one hour to produce. These images have been enlarged and their real sizes are 150 nm × 150 nm. Each image was created by selecting a subset of DNA strands from a set of 310, where a further 1396 strands were required for seal the edges of the shapes to prevent them from aggregating. This set of tiles cost roughly £4500, but the researchers estimate that it could make 2 × 1093 possible shapes.

Drug delivery

“Strands are programmed to have sequences that encode local interactions – like every one of them remembers which one is to its left, right, top and bottom – with this, strands can easily find their position within the big molecular canvas, collectively,” Yin told physicsworld.com. Yin thinks that the technique could be applied to a large number of possible applications, including the creation of nanoscale drug-delivery vehicles. In the longer term, Yin believes that the technique could be used to build scaffolds and machinery inside the body that would interact with proteins and other cellular components in a more programmable fashion.

Ebbe Sloth Andersen, a biophysicist at Aarhus University in Denmark, agrees that the ability to create multiple shapes from the same set of DNA provides a distinct advantage for this technique over DNA origami. “The technique will, in general, accelerate the research field of DNA nanotechnology by making the design of DNA nanostructures cheaper, faster and easier than before,” he says. Anderson has concerns, however, about the reliability of the technique in its current state. “The main limitation is the yield of the new technique in the 6–40% range, which does not compare with that of DNA origami where 95% yield is regularly obtained.”

Double gongs for discoverers of Kuiper belt

By Margaret Harris

It’s been a good week for the astronomers David Jewitt and Jane Luu.

On Tuesday, the pair – whose discovery of the Kuiper belt of small, icy objects back in 1992 quickly reshaped our understanding of the outer solar system – learned that they had won this year’s Shaw Prize in Astronomy. This is a pretty big deal. The nine-year-old Shaw prizes are a relatively new kid on the scientific-awards block, but the astronomy prize already has a prestigious track record: previous winners include both last year’s dark-energy Nobel laureates (Saul Perlmutter, Adam Riess and Brian Schmidt) and the exoplanet pioneers Geoff Marcy and Michael Mayor. Oh yes, and each Shaw prize is also worth a cool $1m, which is a fair whack even in this age of inflation and economic uncertainty.

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But Jewitt and Luu’s week wasn’t over yet. Earlier today, Norway’s Kavli Foundation announced that Jewitt and Luu had also won its big astro gong: the Kavli Prize in Astrophysics. They’ll share this honour – and its attendant $1m prize pot – with a third astronomer, Michael Brown, who followed up on Jewitt and Luu’s Kuiper-belt observations by discovering some of the region’s largest objects, including the Pluto-sized body known as Eris.

So what happens when you win two major science prizes in a week? I contacted Jewitt and Luu shortly after the prizes were announced, and although neither had much time to talk – “I am not being snooty, it’s just that all the deadlines are converging right now,” Luu explained in an e-mail – Jewitt said it was “very flattering” that two independent prize committees had come to the same decision about their work. Their long and ultimately successful search for objects beyond Neptune’s orbit had, he added, triggered an “explosion” of research into planet formation and the evolution of the outer solar system. For example, subsequent studies of the Kuiper belt have shown that it is the source of most of the comets that pass the Earth, since the proximity of Neptune’s gravitational well alters the trajectory of nearby objects and scatters them into the inner solar system.

As for what the pair plan to do with the prize money, Luu – who began her award-winning work as a PhD student at the Massachusetts Institute of Technology and is now a technical member of staff at the institute’s Lincoln Laboratory – said that was a tough question, and winning a second prize made it even tougher. However, she added that “it is a good problem to have, so I am certainly not complaining”.

Jewitt, who was Luu’s PhD advisor and is now a professor at the University of California, Los Angeles, took a slightly more direct view. “Like many people, I’m massively in debt,” he told physicsworld.com. “The prize[s] might help there, but I haven’t decided yet.”

Frequency combs to join the hunt for exoplanets

A method that uses laser frequency combs to calibrate astronomical spectrographs to unprecedented accuracies has been developed and successfully tested by researchers in Europe. The method could be used to find Earth-sized exoplanets by detecting their tiny influence on the motions of their companion stars. The comb was tested on the European Southern Observatory’s High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph at the La Silla Observatory in Chile.

Astronomical spectrographs separate light according to wavelength and the spectra that they produce play important roles in many aspects of astronomy. As a result, astronomers are constantly looking at ways to make their spectrographs more accurate, stable and precisely calibrated. Currently, the best spectrographs, such as HARPS, use thorium-argon lamps or iodine cells for calibration – however, these do not deliver the precision to detect the tiny shifts in the wavelength of starlight caused by the presence of an exoplanet.

These shifts in wavelength correspond to changes in the radial velocity of a star – which, in turn, could be caused by the gravitational influence of any exoplanets that may be orbiting the star. Radial-velocity changes are derived from shifts in the parent star’s spectral lines caused by the Doppler effect. While this method works very well for enormous planets that orbit very close to their parent stars, the accuracy needed to measure the tiny shifts caused by an Earth-sized planet orbiting within the habitable zone of a Sun-like star cannot be achieved today.

The idea of using a frequency comb to calibrate a spectrograph has been discussed for several years, but this is the first time that the technique has been tested and verified, thanks to the efforts of Tobias Wilken of the Max-Planck-Institute for Quantum Optics in Munich and colleagues in Germany and Spain, in collaboration with scientists at the European Southern Observatory (ESO). Wilken is part of a research group headed by Theodor Hänsch, who shared the 2005 Nobel Prize for Physics for his development of frequency combs.

Frequency ruler

The team installed a laser frequency comb to calibrate HARPS over two test runs carried out in November 2010 and January 2011. The comb delivers a series of equally spaced spectral lines that act as a “frequency ruler” against which the light emitted from distant stars can be measured. Wilken told physicsworld.com that complex adaptions had to be made to the comb before it could be used. Spectrographs that can detect exoplanets do so by looking at light in the 400–700 nm range. But Wilken uses a fibre laser as his comb because it is “very robust against thermal variations or acoustic vibrations that are bound to occur when the comb is permanently attached to a working spectrograph”. The problem is that the comb operates in the 1000–1500 nm range.

Also, he explains that with fibre lasers, the length of the laser cavity is directly proportional to the line spacing – that is, with a longer time between each laser pulse, the pulse frequency is lowered. The pulse frequency also determines the line spacing, so for a low frequency there is low spacing. But to accurately resolve a spectral line, very high spacing is required. So the team had to increase the laser line spacing. This was done using Fabry–Pérot cavities – highly reflecting parallel mirrors. “They transmit only a small portion of the light, increasing the spacing,” explains Wilken.

For the entire system to work, two channels (fibres) send light to the spectrograph – one channel guides the calibration light; the other channel, starlight – through the grating and prism set-up, from where the light is detected by a CCD camera, showing a very high-resolution spectrum. “The comb actually has 10,000 lines, which appear as several rows of dots in the CCD image, and you see the calibration lines directly beneath the starlight spectra, so you can constantly compare them and check for any inaccuracies,” says Wilken. For example, there might be a slight expansion of the spectrograph caused by heat, which would be detectable thanks to the calibration lines, and thus the instrumental error can be measured and removed.

Calibration light

For its initial tests, the team used calibration light in both channels, so that the researchers could ensure that the calibration was working accurately. “This way, if you have the same source, any changes should be seen in both spectra. So then, with different sources, all shifts are down to instrumental effects and so can be corrected for,” Wilken explains. “And finally, after that any shifts you see are caused by astronomical stellar effects, like a planet,” he says.

The team also used the calibrated spectrograph to make eight measurements of the radial velocity of the star HD 75289, known to have an exoplanet, to ensure that it could be detected. They observed the system for five nights and “this was done mainly to show that the comb can do night-by-night observations, as this was previously doubted by the astronomical community, who felt that the method was complex and too futuristic for now,” says Wilken.

Despite this success, the comb is not quite ready to be installed permanently. The company that produces the frequency combs, Menlo, set up by Hänsch and colleagues and a spin-off from the Max-Plank-Institute, is now perfecting the combs for permanent long-time use. More durable combs should be ready for use in a year’s time.

Unexpected drifting

During testing on HARPS, the team also saw some unexpected drifting of the spectral lines. This allowed astronomers to identify a previously unknown problem with the HARPS instrumentation. “We need to identify where these irregularities are coming from at HARPS, so that the comb can identify the shifts, characterize them and then correct for them, so improving the stability of HARPS,” says Wilken.

Wilken also points out that the combs could help in designing more accurate and stable instruments in the future. These include the ESPRESSO spectrograph that will look for rocky exoplanets and is due to be installed in 2015 on ESO’s Very Large Telescope.

Zoe Leinhardt, from Bristol University in the UK, who heads a group studying planet formation and evolution, is “very impressed” by the work and believes it could prove to be very useful in detecting Earth-mass exoplanets. “If the method is perfected, and can stably reproduce previous data, it could be hugely beneficial for radial-velocity measurements,” she says. As well as pushing radial-velocity measurements closer to the detection of Earth-sized planets, she also believes that the detection process could be faster than conventional techniques.

The research is published in Nature.

The quantum game of life

Suppose you are at a dinner party in a fancy French restaurant. As soon as there is a lull in the conversation, the person on your right – a friend of a friend – leans over and asks “What do you do for a living?”.

Now suppose that you, like us, belong to the first generation of scientists who have studied for PhDs in quantum information. This interdisciplinary field combines aspects of computer science, mathematics and physics, and naturally, you find it absolutely fascinating. However, launching into an explanation of how all of these things come together seems a little risky during dinner. The last time you tried it, the other guests ended up enduring a five-minute lecture – not a good empirical result. You can do better this time. So you offer a short, to-the-point answer: “I’m a theoretical physicist.”

“Really! But what do you do, exactly?”.

Experience has taught you that the most effective answer to this question is one that involves travelling to conferences in exotic countries. But on this occasion, your subconscious rebels. You find your brain filling with concepts such as quantum cellular automata, quantum lambda-calculus and different models of computation. These things are the core of your work. They are what get you out of bed in the morning. So instead, you blurt out something like “Models of quantum computation and the consequences for theoretical physics.” From the look on your companion’s face, you know that you messed up again.

Information focused

The importance of quantum computation for theoretical physics is not a subject that fits neatly into a dinner-party conversation. Yet it is an idea that is increasingly having its day, as a number of world-renowned physicists – including Seth Lloyd, Lee Smolin, Gerard ‘t Hooft and Anton Zeilinger – have argued that physics should shift away from “matter” and focus instead on “information”. In their view, phenomena such as particle interactions, scattering and forces should take a back seat to concepts such as entropy, observation and information exchanges between systems.

Arguably, this focus on information is not new. After all, entropy (a measure of information) is a fundamental component of thermodynamics, while observers and measurements (respectively, the receivers of information and the means of gaining it) are central to relativity and quantum mechanics. Moreover, the information-centred approach has already led to significant breakthroughs in our understanding of fundamental quantum phenomena such as entanglement (the “spooky” correlation at a distance that quantum particles have under certain conditions) and decoherence (the reason why nobody has ever seen a real cat in a superposition of dead and alive). So, to a large degree, modern physics is already “informational”. However, there is a growing opinion that in the future, physics will be computational as well.

To understand what this means, we need to start by going back to the 1970s, when scientists including Edward Fredkin, Norman Margolus, Tommaso Toffoli and Stephen Wolfram first proposed that the universe could be modelled as a giant parallel computer. In this “digital physics” view, particles should be treated as patterns of information moving across a vast grid of microprocessors, rather than material bodies colliding and scattering – much like a tennis ball can be thought of as a pattern of pixels moving across your TV screen during the Wimbledon final, rather than a lump of rubber ricocheting off a grassy surface. Digital physicists, for their part, are like characters in a video game who are desperately trying to understand the rules.

A striking result to come out of this 1970s work on digital physics was Robin Gandy’s argument that the universe can be simulated by a classical computer with unbounded memory. Gandy was a British mathematician, logician and student of Alan Turing, and he began his argument by noting that physicists agree on certain principles. One is that the laws of physics are homogeneous: they remain the same everywhere and at all times. If they did not, they would not deserve to be called “laws”. Another principle states that the laws of physics are causal: information has a bounded speed of propagation, c, meaning that events occurring at time t + Δt have their causes at time t lying within a disc of radius cΔt. Finally, and somewhat more controversially, Gandy stated that it is reasonable for physicists to believe that any finite volume of space can only contain a finite amount of information (a similar principle has been articulated by the Israeli theorist Jacob Bekenstein, although his bound also involves the energy of the system being considered).

From these three principles, it follows that if space is divided into cubes, each cube can be fully described by the finite information it contains. Moreover, the state of each cube at time t + 1 is a function of the state of the neighbouring cubes at time t; in other words, the state is obtained by applying what information theorists call a “local rule”. Finally, it follows that this local rule is the same everywhere and at all times. Thus, the state of the entire universe at time t + 1 can be computed by applying some fixed local rule everywhere in space.

The effect of this argument is to reduce the universe to a type of parallel computer known as a cellular automaton. Many readers have probably played with a simple cellular automaton before, in the form of John Conway’s “Game of Life”. The classic Game of Life consists of a 2D grid of cells in which each cell can be either “alive” or “dead” (figure 1). Once the user has decided which cells will be alive initially, the state of any given cell at a later time step will be determined by that cell’s state at the previous time step and the states of its eight immediate neighbours, according to rules that simulate the effects of underpopulation, overcrowding and reproduction. These rules are very simple, yet it has been shown that the Game of Life is universal, meaning that it can be made to compute any known classical algorithm – in the same way that one can use simple logic gates and wires to perform any computation using a more conventional computer.

But is there any chance that the real universe we see and experience could be such a simple game?

Back to the table

The problem for Gandy’s model – and the reason why the original digital-physics project was doomed to failure – boils down to one thing: quantum physics. To understand why, let us return to our dinner party at the French restaurant, where the food is getting cold.

Against your better judgement, you launched into an explanation of quantum theory using the knives and forks on the table. Now you hear yourself saying “Pick a system that can be one of two things – like this item of cutlery, which can be either a knife or a fork.” You place the knife and fork on the table with their handles touching at a right angle, forming the x and y axes of a 2D space. “Well, in quantum theory, this one piece of cutlery does not have to be one or the other. The possible states are the entire table. For instance, it can be here,” you say, jabbing your finger at the table. But although you are clearly touching the tablecloth at the point representing the 1/√2 |knife〉 + 1/√2 |fork〉 superposition state, you sense that your audience may not be grasping the full implications. You ponder the wisdom of an alternative explanation involving salt and pepper mills, but before you can begin, your waiter arrives with the dessert menu.

The reason we do not encounter superpositions of knives and forks on a daily basis is that as soon as one observes a quantum system, it becomes classical again. This means that the smallest unit of quantum information, referred to as a “qubit”, can only store a single bit of classical information: 0 or 1, knife or fork. In that sense, Gandy’s principle of finite information density remains compatible with quantum theory. However, as we saw in the restaurant, before one observes a qubit, it is allowed to be in any superposition of states. Hence, it is no longer the case that each cube of space can be fully described by the finite information stored in it, and this is where Gandy’s argument falls down.

Hopes that digital physics might be resurrected in some form rose in the early 1980s, when Richard Feynman proposed that the blatant gap between the power and information content of quantum theory and that of classical computers might be bridged by a new type of computer. His idea was born out of frustration at seeing classical computers take weeks to simulate quantum-physics experiments that happen faster than a blink of an eye. Intuitively, he felt that the job of simulating quantum systems could be done better by a computer that was itself a quantum system.

Like their classical counterparts, quantum computers consist of circuits. To construct quantum circuitry you need quantum wires, which are analogues of real wires carrying conventional bits (as voltages), except they carry qubits. There are many different ways of implementing qubits and wires experimentally; one example is to use the two spin states of a spin-half atomic nucleus as the qubit states, and manipulate them using nuclear magnetic resonance. But you also need quantum gates that can be applied to these wires. For instance, one can imagine that it might be useful to transform a qubit in state |0〉 into the 1/√2 |0〉 + 1/√2 |1〉 superposition state mentioned earlier. A device that performs this operation is called a Hadamard gate. You also need at least one two-qubit gate; one example is the controlled π/8 gate, which causes a universal phase change if both qubits are in state |1〉 and leaves them unchanged otherwise. These two-qubit gates are universal: by combining them, one can compute any quantum algorithm – just as one can use classical gates such as the two-bit NAND gate (which always returns a value of “true” unless both inputs are true) to compute any classical algorithm.

Towards quantum cellular automata

Over the past decade or so, experimentalists in many groups around the world have successfully implemented quantum wires and one-qubit gates such as the Hadamard gate described above. The true difficulties lie with precision two-qubit gates and with protecting many wires from the environment – remember, if the environment “observes” the quantum wires, they become classical again.

Working with Gilles Dowek, and building on previous research results with Vincent Nesme and Reinhard Werner, one of us (PA) developed a version of Gandy’s hypotheses that accounts for the complexities of quantum mechanics. Mainly, this means replacing Gandy’s finite-density principle with the hypothesis that a finite volume of space can contain only a finite number of qubits. Considering the implications of the three updated principles led us to a vision of the universe that behaves like a quantum version of the cellular automaton discussed earlier.

A quantum cellular automaton is very much like a classical cellular automaton, except that now the cells of the grid contain qubits. The time evolution from time t to t + 1 in this model is obtained by applying a quantum gate operation to neighbourhoods of cells repeatedly, across space. However, there are some subtleties to quantum cellular automata that cannot be explained quite so easily in a picture. For example, the cells can now be in a superposition of states, and they can also be entangled with any other cell.

A good example of a quantum cellular automaton is our proposed 3D “Quantum Game of Life”, which takes its name from Conway’s famous original. In this quantum cellular automaton, each cubic cell can be |empty〉, |full〉 or any superposition of these two qubit states, such as 1/√2 |full〉 – 1/√2 |empty〉. The behaviour of the system as it evolves in time can be obtained by applying a quantum gate to a 2 × 2 × 2 grid of cubes (figure 2). This local quantum gate defines the “rule of the game”.

There is, of course, a big gap between constructing a “toy-model” quantum cellular automaton and applying the lessons learned from it to the real world. But if the updated versions of Gandy’s hypotheses hold true – and we can indeed describe the universe as a gigantic quantum cellular automaton – then studying physics becomes a game of attempting to deduce the “program” of the vast, parallel quantum computer that we live in.

The conventional approach to deducing the program is, of course, not to use cellular automata or anything like them, but to probe the “rules of the game” with increasingly refined physics experiments, such as those performed using the Large Hadron Collider at the CERN particle-physics lab. We believe, however, that there is an alternative computer-science-oriented method, one that attempts to find the rules deductively.

We can begin this deductive process by discarding rules that are too simple, on the grounds that we live in a complex universe. Next, we note that all sufficiently complex rules can be made to simulate each other. In other words, if the rule of a particular quantum cellular automaton is complex enough, then it can simulate all other quantum cellular automata, even when the other automata have rules that are horrendously complicated. A quantum cellular automaton that can perform such a simulation is said to have intrinsic universality, a concept we have developed in the quantum setting. Hence, if we can find the simplest, intrinsically universal rule for a quantum cellular automaton, we can use it to find the simplest and most “natural” (in the sense of being how nature does it) way of implementing or simulating physical phenomena.

Beyond quantum digital physics

The Quantum Game of Life we have described is a minimal, intrinsically universal quantum cellular automaton, but it remains to be seen whether all physical phenomena can be encoded using the concepts developed here. Many difficulties lie ahead for those of us who are trying to answer the question “How does nature compute itself?”. One problem is that models of quantum cellular automata are typically not isotropic. For example, on a square grid, signals can generally propagate faster in the four cardinal directions than they can diagonally, so grid-type models cannot easily simulate ripple-like wavefronts. Another problem is that, just as classical digital physics did not integrate the radical features of quantum theory, and thus needed to be updated, quantum digital physics does not integrate general relativity, so it will have to be updated, too. Some members of the quantum-gravity community, including Alioscia Hamma, Fotini Markopoulou, Simone Severini and Lee Smolin, have already been making some attempts in this direction, so we may well be on the verge of a trend towards a new, relativistic, quantum digital physics.

Within this trend, the concepts discussed here, namely those of quantum cellular automata and intrinsic universality, are likely to prove key in finding simple, minimal and universal “toy models” to work on. From a computer-science point of view, reaching this goal will amount to understanding the nature of the ultimate parallel and relativistic quantum computer. Yet we are obliged to conclude with a word of caution: these ideas may not be all that helpful in a restaurant conversation. Attempting to explain them may, in fact, end with the other diners deciding that you are the best person to call the next time their (classical) computer breaks down. But on a more positive note, if we can find the rules, everyone will be a winner in this game of life.

Two new surprises for three-body physics

Physicists in the US have calculated that a new class of three-body bound states should exist for atoms that experience long-range interactions – even though the interactions themselves are too weak to bind pairs of the same atoms. Such states have previously been seen in bosonic atoms affected by short-range interactions, but the team says that this latest phenomenon is very different, particularly because it can also occur for fermions. Although the researchers have not yet seen the new states, these could be revealed in experiments on ultracold atomic gases.

The idea that three atoms can form a loosely bound quantum state – even if any two of the atoms on their own cannot bind together – was first predicted by the Russian physicist Vitaly Efimov in the early 1970s. Now known as Efimov three-body bound states, they were first spotted in 2006 in a gas of caesium atoms that was cooled to just 10 nK by a team led by Hanns-Christoph Nägerl of Innsbruck University in Austria. Efimov states only occur for atoms that are bosons; that is, atoms that have integer, rather than half-integer, values of spin.

The long and the short of it

One important feature of Efimov states is that the interactions between the atoms are short ranged – in other words, they are described by an attractive potential that falls off faster than the inverse square of the distance between atoms. If the potential has a longer range, then Efimov’s calculations do not apply and Efimov states do not exist. Of course, if these long-range potentials happen to be strong, then there will be an infinite number of three-body bound states – but these are not Efimov states.

Until now, however, it has not been clear if three-body bound states exist when the potential is so weak that it does not bind together pairs of atoms. What Brett Esry and colleagues at Kansas State University have found is that bound states of three atoms should occur when they are attracted to each other by a very weak inverse-square potential. The team came to this conclusion by studying numerical solutions to the three-body Schrödinger equation for three identical bosons.

Esry does it

Esry and colleagues then turned their attention to fermions and obtained a second surprising result. When the spins of all three atoms point in the same direction, three-body bound states occur even when atoms in pairs repel each other.

Esry told physicsworld.com that it may be possible to see the new states in lab experiments. “Given that they are very weakly bound – much like Efimov states – ultracold gases are the most likely candidates for seeing them,” he says. “The most likely scenario for seeing our states is in a mixture of heavy bosonic atoms interacting with light fermionic atoms.”

In this scenario, the fermions act as force mediators resulting in an effective attractive inverse-square potential between the bosons. While Esry believes that the effect could reveal itself in a gas of bosonic caesium and fermionic lithium, more ideal candidate systems should have a larger mass ratio between the boson and fermion. Possible systems include ytterbium–hydrogen or erbium–hydrogen, although Esry points out that hydrogen is particularly difficult to work with so lithium might be a better choice of fermion.

Nägerl says he “would not have expected” this result, adding that it is “surprising how rich the [inverse square] case is”. However, Nägerl believes that it may be difficult to persuade experimentalists to try to confirm the theoretical result because of the challenges associated with tooling up their labs to create and study an appropriate boson–fermion combination.

The work is described in Physical Review Letters.

Tuna carry Fukushima isotopes to California

Pacific bluefin tuna off the California coast have been found to contain levels of radioactive caesium isotopes that are around 10 times higher than expected. It is believed that the fish ingested the caesium following a discharge of radioactive material into the ocean near the earthquake- and tsunami-damaged Fukushima Daiichi nuclear power plant in March 2011.

“Our work suggests that Pacific bluefin tuna were exposed to enough radioactivity off Japan to measure it months later in California,” Dan Madigan of Stanford University in the US told physicsworld.com. “This means that bluefin and other migratory animals may carry this signal if they have come from Japan in recent months. This suggests the use of these radioactive isotopes as tracers of movement in the Pacific Ocean on a large scale.”

Madigan and colleagues from Stony Brook University, US, found caesium-134 and caesium-137 in 15 two-year-old Pacific bluefin tuna (Thunnus orientalis) that were caught near San Diego in August 2011. The fish spawns in the western Pacific; some juveniles stay in Japanese waters, while others swim east to the California Current Large Marine Ecosystem, generally when they are around a year old. That means all two-year-old Pacific bluefin caught during summer in the eastern Pacific must have migrated recently.

Migrating across the Pacific

“After the Fukushima accident, there was a lot of attention to the possibility that fish may accumulate and transport radioactive material,” says Madigan. “Since Pacific bluefin are known to migrate across the Pacific, we chose to test them for two elements of radioactive caesium.”

The team found radioactivity levels of around 4 becquerels per kilogram (Bq/kg) dry weight of 134Cs and roughly 6 Bq/kg of 137Cs in the white-muscle tissue of fish sampled in late summer 2011. Pacific bluefin caught before Fukushima and yellowfin tuna, which tend to stay in Californian waters, contained no 134Cs and only background concentrations of 137Cs.

“Tagging studies of tuna, such as the TOPP [Tagging of Pacific Predators] programme, let us know that young bluefin migrate across the Pacific – making them logical test animals – and that yellowfin in the eastern Pacific tend to be generally residential in the eastern Pacific, making them logical ‘control’ animals to test for uptake of radiocesium in the east Pacific,” says Madigan.

Ten times higher, but safe

The total caesium concentrations in the post-Fukushima fish were roughly 10 times higher than before the leaks. But the levels were low compared with naturally occurring radioactive isotopes of potassium and polonium, and an order of magnitude less than the Japanese safety limit of about 400 Bq/kg dry weight for human consumption. The researchers calculated that the fish lost 1.9% of the caesium from their tissues per day as they migrated – which means they would have contained radiocaesium concentrations 1.5–15 times higher than the measured values before they left Japan.

The two caesium isotopes were released in near-equal amounts at Fukushima. 134Cs (half-life 2.1 years) decays faster than 137Cs, which has a half-life of 30 years. The team used the ratio of 134Cs and 137Cs in the fish caught in California, which was 0.62 on average, to work out that the fish had left Japanese waters four months earlier. This suggests that the fish were exposed to contaminated waters for less than one month.

This is the first time that caesium ratios have been employed to track movements of animal life; the team believes that further investigations will help confirm the accuracy of such calculations.

The team estimates that much less than 1% of the radiocaesium released into Japanese waters has been transported to the California Current Large Marine Ecosystem in tuna that have then been caught.

Tracing migrations

“[The results] demonstrate the ability for migratory animals to transport radioactive material,” says Madigan. “They suggest that these tracers may be of use, for a finite period of time, to study migratory patterns of marine animals that use the waters around Japan and then migrate large distances.”

The researchers believe that loggerhead turtles, salmon sharks, sooty shearwaters, pinnipeds, whales and billfish may also have transported radiation from Fukushima.

“We will be testing more bluefin, of many sizes, in California waters in 2012,” says Madigan. “This will give us an idea of the amount of radioactivity (if any) that these animals are carrying more than a year after the Fukushima disaster. We will also be measuring radiocaesium in other Pacific predators to examine the possibility that other species transported radioactive caesium to other regions, and to gain insight into the movements of the predators themselves.”

Madigan and colleagues will report their work this week in PNAS.

New nanosensors could detect disease earlier

Scientists in the UK and Spain have developed a new biological nanosensor that produces a stronger signal when its target molecules are lower in concentration. The sensor can reliably detect molecules at concentrations that are many orders of magnitude lower than can be detected by the diagnostic tests that are used in hospitals today, and could help to identify diseases in their earliest stages, when, in many cases, they are easier to treat and cure.

Conventional biosensors produce a signal that is in proportion to the concentration of target molecules, so at low concentrations they lose sensitivity and become susceptible to interference from other molecules. For disease biomarkers such as cancer antigens, the ability to differentiate confidently between a zero result and a trace result is critical.

The new sensor developed by Molly Stevens and colleagues at Imperial College London and the University of Vigo, Spain, can detect concentrations that are at least 10 times lower than the best existing ultrasensitive tests. “For many diseases, using current technology to look for early signs can be like finding the proverbial needle in a haystack,” says Stevens. “Our new test can actually find that needle.”

Nurturing nanostars

The team built its sensors out of tiny gold stars (or nanostars) measuring about 50 nm across. These structures host surface plasmons, which are coherent oscillations of the conduction electrons at the gold surface. Attached to their gold surfaces is the enzyme glucose oxidase (GOx), which acts as a biocatalyst to reduce silver ions in solution. At low concentrations of GOx, silver atoms are deposited so that a silver coating grows around each nanostar (see figure). This causes a shift towards higher frequencies (blueshift) of the nanostar’s surface-plasmon resonance. At higher concentrations, the silver crystallizes at a faster rate and tends to nucleate separately in solution, and there is a less pronounced shift of the resonance.

The frequency of the resonance is measured by shining visible/near-infrared light on the nanostars and looking for the frequency where absorbance is greatest. As a result, measuring the frequency before and after GOx is introduced provides a very sensitive measure of the GOx concentration.

The next step is to use the nanosensor to measure the concentration of a biological molecule of interest – in this case a biomarker of prostate cancer called a prostate specific antibody (PSA). To do this, the researchers first coat the gold nanostars with an antibody that grabs the PSA out of the solution. Then, a second antibody – which is bound to the GOx – latches on to the PSA on the nanostar surfaces. Finally, the presence of the GOx initiates the silver-reduction step and shifts the surface-plasmon resonance, which is then measured.

Using this technique, the team could detect PSA at concentrations as low as 10–18 g/ml. This is a billion times more dilute than the limit of the enzyme-linked immunosorbent assay (ELISA) test that is widely used in hospitals.

“Our sensor generates the highest signal at the lowest concentration,” says Stevens, “therefore the presence of the target molecule at ultra-low concentrations can be detected with the highest confidence.”

“A really neat trick”

The new strategy has made a positive impression on David Duffy, who is head of research at Quanterix – a company developing single-molecule protein-detection technologies that is based in Boston, USA. “It seems like a really neat trick and a different way of approaching it,” he says. “It definitely made me stop and think.”

A sensitive test for PSA is important because after surgery for prostate cancer, PSA should no longer appear in the body – unless the cancer has spread or if the surgeon has left any affected tissue.

“[Ultra-low levels of PSA] have never been detectable previously, so current diagnostics miss it. All patients are basically in the same boat – they do not know if the surgery was successful in the long term for them,” explains Duffy. “Definitely from the gold standard, which is ELISA, this [new method offers] a big jump in sensitivity.”

Next step

David Fermín, a nanostructures and electrochemistry expert at the University of Bristol in the UK, agrees that the new results constitute “a very impressive piece of work”.

The next step, he suggests, should be a close investigation of how well tiny concentrations of biomarkers can be picked out in the presence of potential interferences. “The researchers mention it briefly in the article, but I think [it will] be a very important aspect to investigate. I am sure that there is a clever chemistry that could be done to make it very specific, so this is an exciting development,” he says.

So far, the researchers have only tested the PSA biomarker, but, says Stevens, “We are confident that the test can be adapted to identify many other diseases at an early stage.” Of particular interest is p24, a protein related to HIV infection the detection of which could help in diagnosing the infection in its infancy.

The research is published in Nature Materials.

Five questions for SKA

SKA

An artist’s impression of the Square Kilometre Array.
(Courtesy: SKA organization/Swinburne Astronomy)


By Michael Banks

After months of political wrangling, a decision finally emerged on Friday afternoon about where the €1.5bn Square Kilometre Array (SKA) will be built.

SKA is a massive next-generation radio-astronomy facility consisting of about 2000 to 3000 linked antennas that will probe the first 100 million years after the Big Bang for clues about galaxy evolution, dark matter and dark energy.

For more than five years, two rival bids have been going head-to-head to host the telescope: one led by Australia and the other by South Africa.

On Friday at a meeting in Amsterdam, the SKA organization opted to split the project between the two hosts, with South Africa building a long-baseline high-resolution telescope and Australia constructing a lower-resolution array but one that can survey a wider field.

Yet, while all this seems like good news – and that was certainly the message from the dozens of press releases that appeared after the announcement – it does throw up some interesting questions.

So here are my five burning questions for SKA officials.

1. Why did the SKA organization not follow the recommendation by the independent SKA Site Advisory Committee that the project would best be built in South Africa?

2. If a split-site option was such a good solution in the first place, why was there not a solid case made for it from the start, thus potentially eliminating the need for a drawn-out site-selection process?

3. When SKA is fully complete, the South Africa bid will get the majority of the antennas – was this just a weak political decision to give the Australian-led bid some part of the project?

4. Is there a risk that SKA now effectively devolves into two separate and thus distinct projects?

5. How much will this decision increase the cost of the SKA project, given the need for more infrastructure to develop two sites; in a time of austerity could this hinder the overall plan?

We will be tackling these questions in detail for an in-depth report in the July issue of Physics World.

If you have any comments, e-mail pwld@iop.org.

Ringed molecule honours sporting event

Olympicene


By Hamish Johnston

In honour of a certain event in London this summer, researchers at the Royal Society of Chemistry (RSC), the University of Warwick in the UK and IBM Research – Zurich have used “clever synthetic chemistry and state-of-the-art imaging techniques” to create a molecule that’s reminiscent of the five rings that symbolize the event.

What have they called it? Olympicene, of course, and it’s already made its way onto the RSC’s chemical database.

“Alongside the scientific challenge involved in creating olympicene in a laboratory, there’s some serious practical reasons for working with molecules like this,” says David Fox of the University of Warwick.

“The compound is related to single-layer graphite, also known as graphene, and is one of a number of related compounds that potentially have interesting electronic and optical properties. For example, these types of molecules may offer great potential for the next generation of solar cells and hi-tech lighting sources such as LEDs,” he says.

The image shown here was obtained by the Physics of Nanoscale Systems Group at IBM Research. It claims to have achieved “unprecedented resolution using a complex technique known as non-contact atomic force microscopy”. A single molecule is just 1.2 nm in width.

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