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Aidan Randle-Conde | USLHC | USA

Read Bio

Happy birthday, Richard Feynman!

Friday, May 11th, 2012

Richard Feynman was one of the most influential physicists of the twentieth century. Not only did he revolutionize quantum theory with his development of quantum electrodynamics, but he also revolutionized the way we think about physics and physicists. He spoke to people from all kinds of backgrounds about physics, from lecturing students destined to change the field themselves, to appearing on television to discuss physics and the philosophy of science, to meeting with the greatest minds of the time.

Feynman in the middle of a lecture. (www.richard-feynman.net)

Feynman in the middle of a lecture. (www.richard-feynman.net)

For me, Feyman’s great contribution was the way he thought about physics. His Lectures on Physics are world famous, and rightly so. (In fact, one of the first things I did after landing in San Francisco to work at SLAC was to buy a copy of his lectures from the Stanford bookstore. Shortly afterwards by bank froze my card, suspecting fraud. It was worth the inconvenience!)

As a jaded undergraduate they were a source of inspiration to me. A faint glimmer of hope turned into a roaring inferno after reading his lectures on electromagnetism, and I’ve never looked back since. Finally, here was someone who wanted to discuss the beauty of the subject, as well as the truth. He had no time for obscuring the underlying symmetry of a concept, nor for lying to students in order to make things easier. Inevitably having to unlearn and relearn ideas leaves people confused, disillusioned and unable to trust their tutors. In that spirit, this is how he started his course on electromagnetism:

“We begin now our detailed study of the theory of electromagnetism. All of electromagnetism is contained in the Maxwell equations.

Maxwell’s equations:

\[
\nabla \cdot \vec{E} = \frac{\rho}{\varepsilon_0}
\]
\[
\nabla \times \vec{E} = - \frac{\partial \vec{B}}{\partial t}
\]
\[
c^2\nabla \times \vec{B} = \frac{\partial \vec{E}}{\partial t} + \frac{\vec{j}}{\varepsilon_0}
\]
\[
\nabla \cdot \vec{B} = 0
\]

Don’t worry about trying to understand these equations. The important thing here is that Feynman has given the students the complete truth about electromagnetism. With these four equations he can solve any problem about the shape and nature of electromagnetic fields for any configuration of charges and currents. The equations he provides are not some approximation of the theory, or some equations that only work some of the time, these are the equations that all physicists and engineers use and they are, as far as we know, complete and state of the art. Feynman has shown a level of honesty and respect for his students/readers that was not present when I sat through lectures. My lecturers taught me backwards, Feynman taught me forwards.

(Experts might notice that the Lorentz force law is missing here, but Feynman already mentioned it a few pages before Maxwell’s equations. With the Lorentz force law physicists can relate the electromagnetic fields to the forces on charged particles.)

Feynman continues:

The situations that are described by these equations can be very complicated. We will consider first relatively simple situations, and learn how to handle them before we take up more complicated. The easiest circumstance to treat is one in which nothing depends on time- called the static case. All charges are permanently fixed in space, or if they do move, they move as a steady flow in a circuit (so \(\rho\) and \(\vec{j}\) are constant in time). In these circumstances, all of the terms in the Maxwell equations which are time derivatives of the field are zero. In this case Maxwell’s equations become:

Electrostatics:
\[
\nabla \cdot \vec{E} = \frac{\rho}{\varepsilon_0}
\]
\[
\nabla \times \vec{E} = \vec{0}
\]

magnetostatics:
\[
c^2\nabla \times \vec{B} = \frac{\vec{j}}{\varepsilon_0}
\]
\[
\nabla \cdot \vec{B} = 0
\]

You will notice an interesting thing about this set of four equations. It can be separated into two pairs. The electric field \(\vec{E}\) appears only in the first two, and the magnetic field \(\vec{B}\) appears only in the second two. The two fields are not interconnected. This means that electricity and magnetism are distinct phenomena so long as charges and currents are static.

And he goes on. Immediately at the start of the course he’s pointed out one of the most important and beautiful symmetries in electromagnetism. He also lets us know how the course is going to proceed, with static cases first and the full treatment later. This leaves the student with a wonderful surprise later in the course, when the two fields finally get united again. When this happens Feynman goes on to show us how electromagnetism comes about as a result of special relativity, and if done properly that is one of the most breathtaking moments in physics! This is the way physics should be taught, and I wish I could have been in that lecture hall to see it happen!

The rest of the lectures are a fascinating journey, full of neat little asides, teasers, paradoxes, and it’s all handled with refreshing clarity. He even pokes fun at physics itself from time to time, showing how our mathematical notation is just a trick to make complicated things look simple and how different problems appear to have similar solutions only because we choose to use the same kinds of methods to solve them. Towards the end of his electromagnetism course he even goes out of his way to show how electromagnetism fails in an epic way. The problem of the infinite energy of the field, and the intractable problem of the mass of the electron are two major failings of the classical theory, and he dedicates a lecture to showing us just many questions were left unanswered by the subject.

Feynman with bongos, because some physicists are cool (www.richard-feynman.net)

Feynman with bongos, because some physicists are cool (www.richard-feynman.net)

Feynman gave us a lot to digest, from Nobel prize worthy discoveries, to a view of scientists that was anything but a crusty old professor, and for me what I value most is the lectures he gave, packed with inspiration and clarity. If you have a chance, go read some of the lectures and find out what made this man get out of bed in the morning. You won’t be disappointed. His other books are also excellent (Six Easy Pieces, Six Not So Easy Pieces, QED and Surely You’re Joking, Mr Feynman!) and well worth a read. Put them on your Christmas wish list!

Feynman’s birthday should be a national day of celebration, not just for physics, but for getting people hooked on physics! (I’m just sorry I’m a bit late to the party here, have a great weekend.)

If you want to find out a bit more about Richard Feynman check out this lecture about Feynman from Lawrence Krauss, one of today’s most eloquent speakers and best advocates for physics.

(Quotes taken from “The Feyman Lectures on Physics, The Definitive Edition Volume II”, Feynman Leighton and Sands, ISBN 0-8053-9047-2)

A sigma here, a sigma there…

Wednesday, May 9th, 2012

Whenever we come across a new result one of the first things we ask is “How many sigma is it?!” It’s a strange question, and one that deserves a good answer. What is a sigma? How do sigmas get (mis)used? How many sigmas is enough?

The name “sigma” refers to the symbol for the standard deviation, σ. When someone says “It’s a one sigma result!” what they really mean is “If you drew a graph and measured a curve that was one standard deviation away from the underling model then this result would sit on that curve.” Or to use a simple analogy, the height distribution for male adults in the USA is 178cm with a standard deviation of 8cm. If a man measured 170cm tall he would be a one sigma deviation from the norm and we could say that he’s a one sigma effect. As you can probably guess, saying something is a one sigma effect is not very impressive. We need to know a bit more about sigmas before we can say anything meaningful.

The term sigma is usually used for the Gaussian (or normal) distribution, and the normal distribution looks like this:

The normal distribution

The normal distribution

The area under the curve tells us the population in that region. We can color in the region that is more than one sigma away from the mean on the high side like this:

The normal distribution with the one sigma high tail shaded

The normal distribution with the one sigma high tail shaded

This accounts for about one sixth of the total, so the probability of getting a one sigma fluctuation up is about 16%. If we include the downward fluctuations (on the low side of the peak) as well then this becomes about 33%.

If we color in a few more sigmas, we can see that the probability of getting two, three, four and five sigma effect above the underlying distribution is 2%, 0.1%, 0.003%, and 0.00003%, respectively. To say that we have a five sigma result is much more than five times as impressive as a one sigma result!

The normal distribution with each sigma band shown in a different color.

The normal distribution with each sigma band shown in a different color. Within one sigma is green, two sigma is yellow, three sigma is... well can you see past the second sigma?

When confronted with a result that is (for example) three sigma above what we expect we have to accept one of two conclusions:

  1. the distribution shows a fluctuation that has a one in 500 chance of happening
  2. there is some effect that is not accounted for in the model (eg a new particle exists, perhaps a massive scalar boson!)

Unfortunately it’s not as simple as that, since we have to ask ourselves “What is the probability of getting a one sigma effect somewhere in the distribution?” rather than “What is the probability of getting a one sigma effect for a single data point?”. Let’s say we have a spectrum with 100 data points. The probability that every single one of those data points will be within the one sigma band (upward and downward fluctuations) is 68% to the power 100, or \(2\times 10^{-17}\), a tiny number! In fact, we should be expecting one sigma effects in every plot we see! By comparison, the probability that every point falls within the three sigma band is 76%, and for five sigma it’s so close to 100% it’s not even worth writing out.

A typical distribution with a one sigma band drawn on it looks like the plot below. There are plenty of one and two sigma deviations. So whenever you hear someone says “It’s an X sigma effect!” ask them how many data points there are. Ask them what the probability of seeing an X sigma effect is. Three sigma is unlikely for 100 data points. Five sigma is pretty much unheard of for that many data points!

A typical distribution of simulated data with a one sigma band drawn.

A typical distribution of simulated data with a one sigma band drawn.

So far we’ve only looked at statistical effects, and found the probability of getting an X sigma deviation due to fluctuations. Let’s consider what happens with systematic uncertainties. Suppose we have a spectrum that looks like this:

A sample distribution with a suspicious peak.

A sample distribution with a suspicious peak.

It seems like we have a two-to-three sigma effect at the fourth data point. But if we look more closely we can see that the fifth data point looks a little low. We can draw three conclusions here:

  1. the distribution shows a fluctuation that has a one in 50 chance of happening (when we take all the data points into account)
  2. there is some effect that is not accounted for in the model
  3. the model is correct, but something is causing events from one data point to “migrate” to another data point

In many cases the third conclusion will be correct. There are all kinds of non-trivial effects which can change the shape of the data points, push events around from one data point to another and create false peaks where really, there is nothing to discover. In fact I generated the distribution randomly and then manually moved 20 events from the 5th data point to the 4th data point. The correct distribution looks like this:

The sample distribution, corrected.

The sample distribution, corrected.

So when we throw around sigmas in conversation we should also ask people what the shape of the data points looks like. If there is a suspicious downward fluctuation in the vicinity of an upward fluctuation be careful! Similarly, if someone points to an upward fluctuation while ignoring a similarly sized downward fluctuation, be careful! Fluctuations happen all the time, because of statistical effects and systematic effects. Take X sigma with a pinch of salt. Ask for more details and look at the whole spectrum available. Ask for a probability that the effect is due to the underlying model.

Most of the time it’s a matter of “A sigma here, a sigma there, it all balances out in the end.” It’s only when the sigma continue to pile up as we add more data that we should start to take things seriously. Right now I’d say we’re at the point where a potential Higgs discovery could go either way. There’s a good chance that there is a Higgs at 125GeV, but there’s also a reasonable chance that it’s just a fluctuation. We’ve seen so many bumps and false alarms over the years that another one would not be a big surprise. Keep watching those sigmas! The magic number is five.

Shifting expectations

Saturday, April 14th, 2012

It’s 2012. We have stable beams. We’re at 8TeV. We’re taking data and I’m sitting in the ATLAS Control Room again. Fans of my blog will remember my previous on-shift posts and, yes, today I had an awesome breakfast of roasted duck (a special treat from a visiting professor).

So ATLAS Control Room, we meet again...

So ATLAS Control Room, we meet again...

The last time I took shifts was about 6 months ago, and since we’ve had a shutdown. Both the LHC and ATLAS have used this break as an opportunity to make substantial improvements and move things around a bit. The change to 8TeV came at the same time as a change in the luminosity calibration. For some reason it looks like CMS are getting about 10% more collisions than ATLAS is. That’s a little unnerving.

The writing's on the wall, literally.  CMS have more collisions than we do.

The writing's on the wall, literally. CMS have more collisions than we do.

As the beam conditions changed, so has the Trigger Shifter’s desk. Performing the checks used to take me about 20 minutes, but with the new layout it took me one hour. Hopefully as I get used to the new system it will be quicker! Since I’m supposed to perform these checks about once an hour I could spend my whole shift staring at one set of histograms! That’s the kind of environment that leads to simple mistakes which could cost data.

Just when things were going well I heard a sound over the intercom and all my trigger rates dropped to 0Hz. There were no error messages, nothing seemed to be wrong with the detector and every system seemed to be working fine. After discussing the situation with colleagues in the Control Room I realized that it was a scheduled beam dump. A scheduled beam dump. We don’t get those often, and the training doesn’t include an MP3 file of the “scheduled beam dump” sound. But then again it’s 1:00am and it’s been 6 months since I was last on shift, so I think I can be forgiven for forgetting what a scheduled beam dump sounds like.

Discussing the beam dump with the other shifters.

Discussing the beam dump with the other shifters.

I’ll be on shift for the tonight and the next two night, racking up credit for SMU and keeping the trigger alive. If all goes well it’s a good chance to catch up on work, write a few blog posts and get some time to ponder the bigger challenges in my analyses. For a few days I’m essentially free from all meetings and distractions, giving me the time and space to sort out all the little problems that have built up in the past few weeks. The broken code, the old E-mails, the unasked questions. Shifts are great.

If you liked this post you might also like:
On shift
The best and worst moment on shift

Physicists discover large body orbiting Earth!

Sunday, April 1st, 2012

After gathering a huge amount of data the physicists at the Ice Cube experiment in Antarctica have come to an inescapable and startling conclusion. There is a massive body orbiting the Earth, and the scientists can see its “shadow” in their data. They can even trace its path across the sky.

This body is called “Luno” by some scientists and it seems to be cross the sky once every 29.5 days. The mass of Luno is estimated to be quite staggering- about 1% of the mass of the Earth! Despite its large size there seems to be little danger posed by this body, It seems to be orbiting happily, showing no sign deviating from its course. Taking a look at the data once the movement of Luno is taken into account gives a striking pattern, confirming that its orbit is indeed stable over long periods of time:

The position of neutrinos in the sky respect to Luno (Ice Cube)

The position of neutrinos in the sky respect to Luno (Ice Cube) (Link to pdf)

The Ice Cube experiment is a neutrino observatory that searches for high energy neutrinos from outer space. These are thought to be given off by gamma ray bursts, neutron stars and alien TV broadcasts. (Some controversial theories also state that we can expect high energy neutrinos from malfunctioning microwave ovens and vacuum cleaners. But it would have to be some extreme form of malfunction.) As the neutrinos cosmic rays hit Luno they interact and the associated neutrinos don’t make it to Ice Cube. This is how Ice Cube see the “shadow” of Luno:

Schematic of the shadow of Luno (Ice Cube)

Schematic of the shadow of Luno (Ice Cube) (Link to pdf)

Other observations of Luno

This is not the first time that a particle physics experiment has speculated about a massive extra terrestrial body. The experiments at LEP postulated the existence of a massive body outside the Earth that changed their centre of mass energies. The assumptions went as far as to say that Luno was responsible for huge tidal forces that changed the shape of the Earth subtly around LEP. Then again, the LEP experiments were also sensitive to the TGV train timetables and meetings of the CERN Yoga Club.

Scientists at NASA have been studying Luno and they have come to some interesting conclusions. The most striking prediction is that Luno should be visible to the naked eye. Luno should reflect electromagnetic radiation from the sun, making it particularly visible at night. It is also thought that Luno is largely responsible for the tides we see in the seas and oceans across the world, a phenomenon which had been a mystery for centuries. Luno could even block the line of sight between the sun and the Earth, causing nightfall for a brief period of time. This could cause panic for people from scientifically illiterate cultures, nocturnal animals and biochemists. After much study there have been a number of artist’s impressions to help with identification of Luno:

Artist's impression of Luno to aid identification (NASA)

Artist's impression of Luno to aid identification (NASA)

Ancient prophecy

Although Ice Cube has only discovered Luno recently, there are several examples of prophecy of Luno in various forms. Several ancient civilizations drew pictograms that represented Luno in some way with some examples, such as the Tarot deck, surviving to the present day. Some cultures even had a Luno deity, such as Khonsu of the ancient Egyptians. His pictogram includes a large figure, which carries Luno. Given the size of Luno, we should be able to see the large figure as well, but all searches have been fruitless. Some people think that this figure may be even harder to find than SUSY, or even extra dimensions (outside of the Terry Pratchett universe.)

Khonsu (discovered portions shown in gray) (Wikipedia)

Khonsu (discovered portions shown in gray) (Wikipedia)

Whatever Luno is, it should be heralded as one of the greatest discoveries of 2012, and I wouldn’t be surprised if it won the Nobel Prize!

Ramping up

Tuesday, March 27th, 2012

At the moment the LHC is making the transition from no beams to stable beams. It’s a complicated process that needs many crosschecks and calibrations so it takes a long time (they have already been working on the transition since mid February.) The energy is increasing from 7TeV to 8TeV, and the beams are being squeezed tighter, and this means more luminosity, more data, and better performance. As the LHC prepares for stable beams, so do the experiments. I can only see what is happening within ATLAS, but the story will be the same for CMS and LHCb.

As the LHC moves through its checks and changes its beam parameters the experiments have an opportunity to request special beam setup. We can ask that the LHC “splashes” the detector with beam in order to calibrate our hardware. This is similar to the famous first beam plots that we saw in 2008. In addition to splashes we can also request very low pileup runs to test our simulation. “Pileup” refers to the average number of events we expect to get every time the beams collide in the detectors, and by increasing the pileup we cram as many events as we can into the limited periods of time available to us. For 2011 our pileup was about 15, and this is going to increase in 2012 to about 20-30. This meant I was surprised to find out that we can use pileup of 0.01 for some of our simulation calibrations!

First ATLAS splash from 2008 (ATLAS Collaboration)

First ATLAS splash from 2008 (ATLAS Collaboration)

The timetable for the ramping up the LHC is announced as far in advance as possible, but it’s subject to small changes and delays as new problems arise. In general, the LHC outperforms its expectations, delivering higher luminosities than promised and stable beams for longer than expected, so when we factor in unexpected problems and unexpected higher performance we have to take the timetable with a pinch of salt. We expect to get stable beams around Easter weekend. You can see the timetable in the pdf document provided by the LHC team.

In the meantime the ATLAS hardware has been checked and maintenance performed to get it in good working order for the data taking. The thresholds are fine tuned to suit the new beam conditions and the trigger menu is updated to make the best use of the data available. There are plenty of decisions that need to be made and discussions that need to take place to make sure that the hardware is ready for stable beams. Today I got a glimpse at the checks that are performed for the electromagnetic calorimetry system, the trigger system and some changes to the muon systems. It’s easy to lose sight of how much work goes into maintaining the machine!

The LHC team preparing for beams.

The LHC team preparing for beams.

As the hardware improves, so does the software. Software is often a cause of frustration for analysts, because they develop their own software as a collaboration and the software is sometimes “bleeding edge”. As we learn more about the data and the differences between data and simulation we can improve our software, and that means that we constantly get new recommendations, especially as the conferences approach. There is a detailed version tracking system in place to manage these changes, and it can be difficult to keep up to date with it all. Unfortunately, updated software usually means analyzing the data or simulation again, which is time consuming and headache-inducing in itself. That is how things worked in 2011. This year it looks like we’ve already learned a lot about how the data look, so we can start with much better simulation and we can start with an improved release for all the software. This should make progress much easier for analyses and simpler for everyone (which is a very important consideration, given that we have a large range of experience with software, and a large range of knowledge of physics processes.)

The banks of super computers are ready and waiting...

The banks of super computers are ready and waiting...

Putting all this together we can conclude the following: we will have higher energy beams giving us more data, we’ll have a better functioning detector based on previous experience, we’ll have improved simulation, and we’ll have more stable and simpler software. This is very exciting on the one hand, but a bit intimidating on the other, because it means that the weak link in the chain could be the physicists performing the analyses! There are plenty of analyses which are limited by statistics of the dataset, or by resolution of the detector, or stymied by last minute changes in the software or bugs in the simulation. If we hit the ground running for 2012 we could find ourselves with analyses limited by how often the physicists are willing to stay at work until 3am to get the job done.

I’ve already explained why 2012 is going to be exciting in terms of results in another blog post. Now it looks like it will bring a whole new set of challenges for us. Bring it on, 2012, bring it on.

Cleaning the world’s biggest machine

Tuesday, March 6th, 2012

Today I spent much of my time crawling around on hands and knees, picking pieces of rubbish from the innards of the ATLAS detector. It’s just one of those things that comes with the job and gives you a different view of the experiment (literally.) Before we start taking data we need to make sure that the ATLAS cavern is clean and safe. I call this process “Grooming the Beast”.

We started our shift with a briefing in the ATLAS Control Room.

We started our shift with a briefing in the ATLAS Control Room.

The ATLAS detector is housed in the ALTAS cavern, just behind the Globe at CERN. The journey down is long (more than 100 meters) and convoluted, with all kinds of doorways, locks, passages and elevators. Work has been taking place in the cavern during the winter shutdown to make improvements and sort out minor problems with the detector. Is a piece of the hardware getting damaged by interactions with matter? This is an excellent time to replace it!

Some of the team survey the work ahead of them.

Some of the team survey the work ahead of them.

Cleaning the cavern just as people start to leave it may seem like an unusual thing to do, but it serves a very important purpose. There has been a lot of work to improve the detector during the shutdown, and this leaves some debris. The engineers clear up as much as they can as they go along, but the odd screw or piece of wire goes missing, and over the months this builds up. The real danger to the machine is metal debris. The detector contains large magnets and these can interact with metallic objects lying around. They need to be removed before we turn on and take data!

The problem with photographing ATLAS is that it's just too big and the cavern is too small.

The problem with photographing ATLAS is that it's just too big and the cavern is too small.

The cleaning also serves a milestone in the life of the experiment. It serves as a reminder that the shutdown is over, the repairs are complete and that we need to look forward to the new data that’s going to arrive. It’s no coincidence that at the same time as we clean the cavern, we present our work at the Moriond conferences. (These two weeks are going to be my favorite of this year! So many interesting results, and getting the chance to poke around inside a large detector.)

We got treated to a coffee break halfway through!  (Note the security guard preventing use of the "Goods In" entrance, and the retinal scanners in the green "Pedestrians" entrance.)

We got treated to a coffee break halfway through! (Note the security guard preventing use of the "Goods In" entrance, and the retinal scanners in the green "Pedestrians" entrance.)

As you would expect, health and safety are very important in this process. To get access to the cavern I had to pass 4 levels of safety training, get a dosimeter to monitor radioactive dose, a hardhat with a light, and hard boots. In addition we had to register our names and phone numbers in case anything happened while we were down there. There is an elaborate key system in place as well, which is mainly for safety. We each take a key as we enter, and the beams cannot pass through the cavern until every key is returned. We each get a pass (either on our CERN ID cards or a magnetic key fob) that is linked to our names and dosimeters, so that if a key is not returned we know who is still in the cavern and when they entered. Safety isn’t the only concern though, these systems have the added advantage of protecting the machinery. Everyone who goes down to the cavern has to have safety training and the correct permission, which significantly improves the quality of all the work down there. If we knew we could just pop along at any time to fix a minor problem there would be people down in the cavern all the time!

Armed with a proton pack (I mean a vacuum cleaner) I take on the dirt and debris of the ATLAS cavern!

Armed with a proton pack (I mean a vacuum cleaner) I take on the dirt and debris of the ATLAS cavern!

Most of the actual work involved picking pieces up off the floor and cleaning the areas that others can’t reach. It seems simple, but the shape and size of the detector make it very difficult. Balancing on one foot on a low friction floor as you lean into a crevice to see if that wire is actually attached to anything, while wearing a hard hat that makes your head bigger than usual is exactly as difficult as it sounds! For bonus points you can do this in a dark space with a special tool for grabbing objects in places too small for your hands to reach. Some of the “treasure” I found included a drill bit, a box of screws and tubes (“It’s good, but it’s not the Higgs”), a guide to some important looking apparatus, and some rusted metal in a box of rusty water. When faced with those objects it’s not always obvious what to do. Is it trash? Is it safe to move? Is somebody missing it?

"How can we make the ATLAS cavern even cooler than it already is?" "Put a scorpion like crane in it, of course!"

"How can we make the ATLAS cavern even cooler than it already is?" "Put a scorpion like crane in it, of course!"

This is the first time I’ve seen the ATLAS detector in person and it’s impressive. But on the other hand, I couldn’t relate to it very easily. I saw some piece of the toroid and some piece of the muon system, but from the outside it looked like an amorphous chunk of wires and pipes. My officemate, Julia, pointed out the muon systems, and showed me the sensors they used to calibrate their position. In addition to this, they also have geodetic instrumentation in the cavern so that they can work out the position of any part of the detector. That’s some neat hardware to have 100 meters underground! I’d hoped to be able to recognize a lot more of the detector, but it’s just not that kind of experiment. It’s far too huge to appreciate in a single day.

Is this ATLAS?  Or a space age submarine?  Or the best clubhouse in the world?

Is this ATLAS? Or a space age submarine? Or the best clubhouse in the world?

Towards the end of the day my friend Katie showed me the inside of the detector. At the bottom of the detector there’s a crawl space (mind your head on the muon system!) into a series of chambers and tunnels. These give access to some instruments and hardware so that we make some changes or repairs, and through an intricate set of ladders and tunnels you can actually get quite far into the outer parts of the detector. It’s warm down there, and you can see parts of the famous toroid, which is neat. It was around this time that Katie suggested that it would make the best clubhouse in the world. I can see myself enjoying somewhere like that as a 12 year old boy! (Actually, I can see my self enjoying it as an adult, but that’s just how amazing it looks when you’re inside.)

Right now I’m exhausted, and my throat is a little dry, but it’s been an awesome day and I’m glad to have the chance to share some photos of the ATLAS cavern with you!

But what if they are faster than light?

Friday, February 24th, 2012

This week the OPERA experiment released a statement about their famous “faster than light” neutrino measurement. In September scientists announced that they had measured the speed of neutrinos traveling from CERN to Gran Sasso and they found that they arrived slightly sooner than they should do according to special relativity. There was a plethora of scientific papers, all kinds of rumors and speculation, and most physicists simply refused to believe that anything had traveled faster than light. After months of diligent study, OPERA announced that they may have tracked down two sources of experimental error, and they are doing their best to investigate the situation.

But until we get the results of OPERA’s proposed studies we can’t say for sure that their measurement is right or wrong. Suppose that they reduce the lead time of the neutrinos from 60ns to 40ns. That would still be a problem for special relativity! So let’s investigate how we can get faster than light neutrinos in special relativity, before we no longer have the luxury of an exciting result to play with.

The OPERA detector (OPERA Collaboration)

The OPERA detector (OPERA Collaboration)

Special relativity was developed over a hundred years ago to describe how electromagnetic objects act. The electromagnetic interaction is transferred with electromagnetic waves and these waves were known to travel extremely quickly, and they seemed to travel at the same speed with respect to all objects, no matter how those objects were moving. What Einstein did was to say that the constancy of the speed of light was a fundamental law of nature. Taking this to its logical conclusion meant that the fastest speed possible was the speed of light. We can call the fastest possible speed \(s\) and the speed of light \(c\). Einstein then says \(c=s\). And that’s how things stood for over a century. But since 1905 we’ve discovered a whole range of new particles that could cast doubt on this conclusion.

When we introduce quantum mechanics to our model of the universe we have to take interference of different states into account. This means that if more than one interaction can explain a phenomenon then we need to sum the probabilities for all these interactions, and this means we can expect some strange effects. A famous example of this is the neutral kaon system. There two lightest neutral kaons are called \(K^0\) and \(\bar{K}^0\) and the quark contents of these mesons are \(d\bar{s}\) and \(s\bar{d}\) respectively. Now from the “outside” these mesons look the same as each other. They’ve got the same mass, they decay to the same particles and they’re made in equal numbers in high energy processes. Since they look identical they interfere with each other, and this gives us clues about why we have more matter than antimatter in the universe.

Since we see interference all over the place in the Standard Model it makes sense to ask if we see interference with a photon. It turns out that that we do! The shape of the Z mass peak is slightly asymmetric because of interference between virtual Z bosons and virtual photons. There are plenty of other particles that the photon can interfere with, including the \(J/\psi\) meson, and the \(\rho\) meson. In fact, any neutral vector meson with no net flavor will do. Einstein didn’t know about any of these particles, and even if he did he never really accepted the conclusions of quantum mechanics, so it’s no surprise that his theory would require that the speed of light is the fastest speed (that is, \(c=s\).) But if the photon interferes with other particles then it’s possible that the speed of light is slightly lower than the fastest possible speed (\(c<s\)). Admittedly, the difference in speed would have to be very small!

In terms of quantum mechanics we would have something like this:
\[
|light>_{Einstein} = |\gamma>
\]
\[
|light>_{reality} = a_\gamma |\gamma> + a_{J/\psi} |J/\psi> + a_Z |Z> + \ldots
\]

As you can see there are a lot of terms in this second equation! The contributions would be tiny because of the large difference in mass between the massive particles and the photon. Even so, it could be enough to make sure that the speed of light is ever so slightly slower than the fastest possible speed.

At this point we need to make a few remarks about what this small change in speed would mean for experiments. It would not change our measurements of the speed of light, since the speed of light is still extremely fast and no experiment has ever showed a deviation from this extremely fast speed. Unless somebody comes up with an ingenious experiment to show that the difference between the speed of light and the fastest possible speed is non-zero we would probably never notice any variation in the speed of light. It’s a bit unfortunate that since 1983 it’s been technically impossible to measure the speed of light, since it is used in the definition of our unit of length.

Now we know that photons can interfere with other particles it makes sense to ask the same question about neutrinos. Do they interfere with anything? Yes, they can interfere, so of course they do! They mix with neutrinos of other flavors, but beyond that there are not many options. They can interfere with a W boson and a lepton, but there is a huge penalty to pay in the mass difference. The wavefunction looks something like this:
\[
|\nu_e>(t) = a(t)_{\nu_e}|\nu_e> + a(t)_{\nu_{\mu}}|\nu_\mu> + a(t)_{\nu_{\tau}}|\nu_\tau> + a(t)_{We}|We>
\]
(I’ve had to add a time dependence due to neutrino mixing, but it’s essentially no more complicated than what we had for the photon.)

That means that the photon could get slowed down slightly by the interference with other particles (including particles in the vacuum) and that neutrinos could get slowed down more slightly by their interference terms with other particles. And that way we could get neutrinos traveling faster than the speed of light and special relativity could remain intact. (In this description of the universe we can do what used to seem impossible, we can boost into the rest frame of a photon. What would it mean to do that? Well I suppose it would mean that in this frame the photon would have to be an off-shell massive particle at rest.)

The SN 1987 supernova, a rich source of slower than light electron neutrinos (Hubble, ESA/NASA)

Now I’ll sit back and see people smarter than I am pick holes in the argument. That’s okay, this isn’t intended to be a serious post, just a bit of fun! There are probably predictions of all kinds of weird effects such as shock waves and time travel that have never been observed. And there are plenty of bits I’ve missed out such as the muon neutrinos traveling faster than electron neutrinos. It’s not often we get an excuse to exercise our analytic muscles on ideas like this though, so I think we should make the most of it and enjoy playing about with relativity.

Anatomy of an aurora

Thursday, January 26th, 2012

This week the Earth has seen some increased magnetic activity in the upper atmosphere, and that means we got to see aurore! Across Northern Europe and the Northern USA people looked to the skies to see the northern lights. An aurora is one of the most beautiful sights in the natural world, and a phenomenon that actually tells us a lot about the Earth and how it interacts with its environment.

Those who followed me on Twitter (@aidanatcern) may have already seen some of the wonderful images of aurorae. There are dedicated webcams that capture the night sky, and you can see some sample images at the Aurora Webcam archive.

Aurora over Alaska (wikimedia)

Aurora over Alaska (wikimedia)

When charged particles accelerate or decelerate, or recombine in pairs, they emit electromagnetic radiation, and it is this radiation that we see in the aurora. The color of the light depends on the wavelength of the radiation, and the intensity of the light depends on how much radiation is emitted. That means that there is always an aurora above us, but if the energy of the radiation is too low, or the intensity is too weak, we won’t see anything. Once we know how to interpret the light we can learn something about the radiation that is emitted. Usually we see a variety of colors in an aurora and each color corresponds to a different wavelength, so if we can see a region of the sky that is all one color, we know that the wavelength (and hence the energy, ignoring the effects of aberration) must be the same. That means we can “map” the sky and find contours of wavelength.

Since the particles are accelerating, there must be something that causes the acceleration. The Earth’s core is made of (among other materials) molten iron. The rotation of the Earth means that this core is also rotating, and a rotating fluid magnetic medium creates a magnetic dipole, giving the Earth magnetic North and South poles. These poles are aligned near the geographic North and South poles of the Earth, but not exactly. (In fact, magnetic North and South keep moving and from time to time they even swap places. The exact mechanism behind this is not yet fully understood, but geological records show it happens every few hundred thousand years. Simulations suggest that the rotating magnetic fluid is a chaotic system, so the reversals occur at stochastic, or random, intervals of time.)

The sun produces a stream of particles, known as the solar wind, and they create their own electromagnetic field. The two fields, from the Earth and the sun, interact and they force charged particles in the upper atmosphere along curved paths. As the particles move along these paths they accelerate, decelerate and recombine, and that is what produces the aurorae. The most recent increase in magnetic activity can be traced back to a huge coronal mass ejection that arrived from the sun. This video shows the arrival of the flare:

The effect looks impressive, but don’t be scared, solar winds like this are perfectly harmless. Far bigger winds have hit the Earth in the past few billions years and life has continued to flourish in spite of them. Life has adapted to the Earth’s magnetic field and this field protects us from the high energy particles.

It turns out that while looking up at the night sky is a beautiful and moving experience in itself, it is also important to particle physicists. Some of the most important discoveries in the last century came from a different phenomena, cosmic rays. Cosmic rays are very high energy particles (usually protons) that travel huge interstellar distances and rain down on the Earth in much the same way that the solar wind does. They interact with the upper atmosphere to create cascades of particles, and usually the muons are the only detectable particles that reach sea level. Interactions of these cosmic rays gave rise to the discovery of the muon (“Who ordered that?!”), the pion and the kaon, the lightest forms of mesonic matter. It was around this time that large scale accelerators were developed, and we found hundreds of new mesons and baryons. Cosmic rays gave us a very small glimpse into a rich “zoo” of particles that has occupied physicists ever since.

Eventually, when we have exhausted our ability to accelerate particles to higher energies we might need to rely on cosmic rays again. There are proposals to develop ground based detectors to study the interactions of extremely high energy particles from outer space. Those particles have the potential to reach energy regimes we can only dream of at the moment. (Incidentally, this is one of the ways that we know for sure that the LHC cannot destroy the world. The universe creates much more energetic particles than we could ever hope to create in our accelerators, and since the universe seems to be in one piece we can conclude that the LHC is safe on Earth!)

An aurora from above (Expedition 28 on board the International Space Station)

An aurora from above (Expedition 28 on board the International Space Station)

If you’re fortunate enough to see an aurora then take a few moments to think about the huge forces at work, the vast distances involved, and how the colors tell us so much about how the Earth and solar wind behave. It really is one of the most beautiful phenomena in the universe.

Getting layed

Friday, January 20th, 2012

On a past blog post I came across the most wonderful comment from Kelly, one of our readers:

Lay people are far smarter than it is supposed, they are also fickle and quick to get bored or offended if talked down to

This got me thinking about the last time I spoke to an expert in another field about their research, about the last time I got “layed”, if you’ll excuse the awful pun. I also hope you’ll excuse an excursion into biochemistry for one post.

Alex and Kia, relaxing in the sun

Alex and Kia, relaxing in the sun

I was in Manchester for the weekend, spending the evening with Alex and Kia, a couple of friends from undergraduate and we had a lot of catching up to do! They’re both biochemistry graduate students and they work in the same lab, although in different areas. We stayed up all night over tea and biscuits (how British), discussing our research, using analogies, looking at diagrams, and coming up with all sorts of thought experiments to try to understand what was happening. They had a lot of questions about how the detector works, how we reconstruct particles (including the Higgs!) and why it takes so long to find it.

Having a discussion about something technical with an expert is not only lots of fun, but it also tells you a lot about your own skills when it comes to explaining concepts. As Kelly mentioned in her comment, there’s a temptation to talk down to people, but I find it’s more rewarding for all involved if we match our discussion to the intelligence of the audience. I’d like to think that most people who read Quantum Diaries and US LHC Blogs are here because they’re intelligent, they’re not scared of nuance, they want to read more than what a press release will tell them, and they may even be a scientist too. Once we find the right level of discussion for a given audience things get much more rewarding!

From the outside biochemistry is such a wonderful field of research. Their work is instantly relevant to the fight against disease and cancer, the field is expanding so rapidly that what students learn one year may be out of date a couple of years later, and there’s no end to the range of different topics you can research. It’s about as fast paced as you can get! It must have its frustrations, like any area of research, but being a layperson I got a chance to appreciate the concepts without the hard work, and that made it sound amazing.

The watered down version of what they told me went something like this:

HIV and T cells

What HIV looks like (Telegraph)

What HIV looks like (Telegraph)

The HIV virus is extremely dangerous for one reason- it infects the white blood cells (T cells) that fight disease in the body. This in itself isn’t a huge problem, but when a person with HIV have some infection then things become very serious. It’s not so much that the white blood cells don’t function anymore, it’s more that they use so many of their resources building more copies of the virus. The virus attaches itself via a protein, and a small percentage of the population have a different form of the protein, which has a different shape. In principle, if a person could get a complete blood transfusion then they could be given the white blood cells with the other protein and may become immune to HIV. An easier way to do this would be to have a bone marrow transplant from another person, as the bone marrow creates the white blood cells. Naturally there are dangers associated with any procedure like this, so it’s not something to be taken lightly. Still, in the course of an hour or so my friends gave me a wonderful insight into how HIV works and some of the discoveries in the fight against the disease.

Genetic diseases

While on the topic of diseases with risky treatments we also discussed a family of genetic diseases (known as mucopolysaccharide diseases, a name I could not remember) which cause premature aging or degradation of the body. The diseases are associated with the failure of the body to break down certain sugars, so the cells get clogged up, do not function as well and then part of the body ages. The exact type of disease manifests in different ways, and sometimes they can only be identified once the disease has progressed. So I asked why children aren’t just screened for this at birth, as they are for many other diseases. It turns out that the cost of the test isn’t low enough and rate of incidence of the disease isn’t high enough for that to become a realistic option yet. Putting groundbreaking, life saving research in that kind of context is rather chilling. I’m glad physicists don’t have to deal with those kinds of choices!

Kia was kind enough to link to one of the charities, so I could find out more about the disease and how it affects us: The MPS Society.

The immune system

But we weren’t done yet! We also talked about the immune system and cancer. Having heard so much about T cells, I was curious about where they came from and why they only attacked foreign objects in the body. It turns out that T cells spend much of their time in the thymus where they are trained to learn what cells in the body look like. When the T cells are produced there is some shuffling of genes and each T cell ends up a little different. If a T cell latches onto part of the thymus it gets destroyed and isn’t allowed into the rest of the body. Otherwise the T cell is let out into the bloodstream. If it finds a cell it “thinks” is attractive, it latches on and releases chemicals into the blood stream. Other T cells respond to the chemical gradient and they too latch on. After a short while the foreign body is overwhelmed and dies.

A red blood cell, a platelet and a T-cell, side by side (Wikipedia)

A red blood cell, a platelet and a T-cell, side by side (Wikipedia)

Well that’s how it works in principle, and there are many ways in which it can go wrong. Some viruses are adept at mutating so that their appearance changes. (On the subject of mutations, my friends also treated me to a discussion of “frame shifts” and how you can get two proteins from one gene!) If one of these viruses gets identified and overwhelmed, one copy may mutate into another form, and the T cells are back to square one again. Another “nightmare scenario” is when a cancerous growth releases a different kind of chemical which essentially says “All fine over here! Carry on!” to the T cells. If that happens then things can go quite seriously wrong quite quickly. If all that wasn’t complicated enough, T cells can also get “confused” and latch on cells from their host body, giving rise to auto immune diseases. The immune system is so amazingly intricate that you could easily spend a whole evening just scratching the surface of the subject. At the same time it also seems immensely fragile and wonderfully robust. Although the apparatus for making an immune system is inherited, the good work it does fighting disease isn’t. If those ideas doesn’t blow your mind then I don’t know what will!

The PhD problem

To round off the evening we also discussed how our PhDs had progressed. Biochemistry seems less forgiving than physics, and they told me that between them and two other mutual friends, two of them had to find new topics, new funding and new institutions. Sometimes, when a research idea doesn’t work out and the funding disappears, even if it’s through no fault of the student, the student has no choice but to start again. I faced a similar situation with my own PhD, as funding for the experiment was cut short and I suddenly found myself with 18 months left, no research topic and no service task. My colleagues rallied round, asked questions, contacted people and helped me find a new topic and a new service task on the same experiment. I finished about 9 months later than expected (but still within four years!) with a decent thesis and some glowing letters of recommendation. Once again, I was glad to be in the cozy realm of physics! It’s differences like these that aren’t at all obvious, and make us realize just how much we have to learn from each other. (My friends were also amazed to find I had about a hundred papers with my name on!)

PhDs are elastic... (PhD Comics)

PhDs are elastic... (PhD Comics)

When did you last get layed?

So for a few hours I was a layperson with two experts at my disposal, and it was one of the most entertaining evenings I’ve had in a long time. So to the lay people reading this blog, if you don’t find the term “layperson” pejorative, it would be great to hear about your experiences. What discussions particularly excited you? How you deal with being patronized or, perhaps worse, overwhelmed with ideas? Or for that matter, if you’re an expert in another area, what are your experiences telling other people about your work? In short, tell us happened last time you got “layed”.

A new year, a new outlook

Saturday, December 31st, 2011

2011 has been a year of change and excitement. We’ve had plenty of good news and bad news to deal with. The new year doesn’t mean just another calendar on the wall, it means a new way of looking at physics. There’s no better way to bring in the new year than watching the fireworks in central London, surrounded by friends. There’s usually a fantastic display, because London is not only one of the most important cities in the world, but it’s also home of universal time. With the Greenwich Meridian running through the capital, we’re reminded of the role that timekeeping has played in the development our history and our science. But this year was even more special, since London is literally inviting the world to its streets this year for the Olympics. So I got caught up in the excitement of it all my thoughts turned to what we’ve seen in the world of physics, and where we’re going next.

New year fireworks in London (New York Times)

New year fireworks in London (New York Times)

2011 got off to a start with ATLAS announcing a startling asymmetry in the jet momenta in heavy ion collisions. However, the joy was tainted by a leaked abstract from an internal document. That document never made it through internal review and should never have been made public. We were faced with several issues of confidentiality, ethics and biases, and how having several thousand people, all armed with the internet and with friends on competing experiments makes the work tough for all of us. In the end we followed the right course, subjected all the analyses to the rigors of internal and external review, and presented some wonderful papers.

There was more gossip over the CDF dijet anomaly presented at Blois. CDF saw a bump, and D0 didn’t. Before jumping to any conclusions it’s important to remember why we have two experiments at Tevatron in the first place! These kinds of double checks are exactly what we need and they represent the high standard of scientific research that we expect and demand. The big news for Tevatron was, of course, the end of running. We’re all sad that the shutdown had to happen and grateful for such a long, productive run, but lets look to the future in the intensity frontier.

Meanwhile both ATLAS and CMS closed in on the Higgs boson, excluding the vast majority of the allowed regions. The combinations and results just got better and better, until eventually on December 13th we saw the result of 5fb-1 from each experiment. The world watched as the presentations were made and quite a few people were left feeling a little deflated. But that’s not the message we should take away. If the Higgs boson is there (and it probably is) then we’ll see by the end of the year. There’s no more of saying “Probably within a year, if we’re lucky”, or “Let’s not get ahead of ourselves”. This time we can be confident that this time next year we’ll have uncovered every reasonable stone. The strategies will change and we narrow the search. We may have new energies to explore, and we’ll tweak our analyses to get more discriminating power from the data. Now is the time to get excited! The game has changed and the end is definitely in sight.

Raise a glass as we say farewell to a great year of physics, and welcome another

Raise a glass as we say farewell to a great year of physics, and welcome another

It’s been a good year for heavy flavor physics as well. LHCb has gone from strength to strength, probing deeper and deeper into the data. We’ve seen the first new particle at the LHC, a state of bottomonium. Precision measurements of heavy flavor physics give some of the most sensitive tests of new physics models, and it’s easy to forget the vital role they play in discover.

ALICE has been busy exploring different questions about our origins, and they’ve studied the quark gluon plasma in great detail. The findings have told us that the plasma acts like a fluid, while showing unexpected suppression of excited bottomonium states. With even more data from 2011 being crunched we can expect even more from ALICE in 2012.

The result that came completely out of left field was the faster than light neutrinos from OPERA. After seeing neutrinos break the cosmic speed limit, OPERA repeated the measurements with finer proton bursts and got the same result. Something interesting is definitely happening with that result. Either it’s a subtle mistake that has eluded all the OPERA physicists and their colleagues across the world, or our worldview is about to be overturned. I don’t think we’ll get the answers in the immediate future, so let’s keep an eye out for results from MINOS and OPERA.

Finally it’s been an incredible year for public involvement. It’s been a pleasure to have such a responsive audience and to see how many people all across the world have been watching CERN and the LHC. A couple of years ago I would not have thought that the LHC and Higgs boson would get so much attention, and it’s been a of huge benefit to everyone. The discoveries we share with the world are not only captivating us all, they’re also inspiring the next generation of physicists. We need a constant supply of fresh ideas and new students to keep the cutting edge research going. If we can reach out to teenagers in schools and inspire some of them to choose careers in science then we’ll continue to answer the most fascinating, far reaching and beautiful questions about our origins.

So when you a raise a glass to the new year, don’t forget that we’ve had an incredible 2011 for physics, and that 2012 is going to deliver even more. We don’t even know what’s out there, but it’s going to be amazing. To physics!