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USLHC | USA

Tilt!

Anna Phan
Friday, April 13th, 2012

The LHC has restarted this year, with a couple of differences, the most obvious being the energy change from 3.5 TeV per beam to 4 TeV per beam. However there are lots of more subtle changes between this year’s and last year’s running. One of these is the collision setup at Point 8, where LHCb is located.

I should probably pause here to warn you that this post is going to be a little technical. But hopefully you’ll get something out of it, even if it’s only that the LHC is a very complicated machine.

In most of the LHC, there are two separate beam pipes, one for the clockwise beam one and one for the anticlockwise beam two. These two beam pipes can be seen in the above image. However, since we want to collide the two beams, there are sections of the LHC where there is only one beam pipe. As seen below, these naturally are at each of the points where the experiments are located. In these regions, the beams are kept physically separated using magnets (horizontally at CMS and LHCb and vertically at ATLAS and ALICE) and brought into collision at a finite crossing angle to avoid unwanted collisions.

This is where it starts getting more complicated… As I’ve mentioned earlier, each experiment has some sort of magnet system, which could affect the trajectory of the circulating beams. The LHCb dipole magnet produces a deflection of around 180 μrad at the top energy of 7 TeV per beam. The field direction is in the vertical plane and the deflection therefore in the horizontal plane. This deflection must be compensated for to ensure beam stability. The situation can be seen in the image below.

For our physics analyses, we would like to take data with our dipole magnet in both directions (the N pole at the top and S pole at the bottom, and vice versa). We would also ideally like the crossing angle between the two beams to remain the same in both situations to reduce the errors on our results.

The problem here is that both the LHCb dipole compensation and the beam separation and crossing are in the horizontal plane. For the LHC, the beam exchange should always occur in the same direction, that is, the clockwise traveling beam one (the blue one) should always cross from the outside beam pipe to the inside at LHCb. This means that when we change our dipole polarity, we can’t ask the LHC to switch the beams around so we get the same crossing angle in both directions.

So for the 2010 and 2011 LHC runs, we’ve been running with different crossing angles when we switch magnet polarities. This year however, a new scheme has been proposed, where instead of horizontally separating the beams at the LHCb collision point, the beams will be vertically separated. With the vertical separation, and the horizontal compensation, this actually creates a tilted crossing plane, which you can see in the image below.

Now when we change the direction of our dipole magnet, we just change the direction of the tilted crossing plane (from NE-SW to NW-SE), but the crossing angle remains the same. So this year’s results will be even better than last year’s!

More Multitasking

Seth Zenz
Friday, April 13th, 2012

I fell out of practice at multitasking at the end of grad school. For the final six months, almost all of my work went into finalizing how to present my analysis results. There were two versions of the presentation: the paper and my thesis, but the general direction of work was all the same. The previous tasks I had worked on, geared toward keeping ATLAS running, were all long since “done,” at least as far as I was concerned.

Starting a postdoc means a sudden change of gears, with more multitasking than ever before. I’ve started many new projects from scratch at the same time, and because I’m new to CMS, every one of those tasks involves tools and procedures that I don’t know. It’s easy to lose track of some of those tasks at any given time, or simply to want to focus on one thing until I understand it, but the job doesn’t work that way. Being succesful as a postdoc will mean significant contributions to the running and understanding of the detector and significant contributions to keeping my group’s analysis running and starting a new analysis (sub)channel of my own. None can be dropped, and most of the things I’m doing have deadlines in the next few months.

So I’m having to remember and improve my multitasking skills, quickly. Step one is bringing this post to a close, and asking you to wish me luck, and getting back to work!

Grad School Confidential

Flip Tanedo
Wednesday, April 11th, 2012

Later this week another generation of academics will finalize their decisions about which graduate programs to attend next year—many congratulations to all of you soon-to-be grad students who will join us in the trenches at the frontier of human knowledge.

Unlike undergraduate life which has a well-known idealization in Animal House (or the TV series Greek), grad school doesn’t get much publicity other than the sardonic (and delightful) PhD comics. I wanted to take a moment to share some observations of what graduate school is actually like, with the usual caveat that this is just my personal perspective—each person has their own experience. (Grads and former grads: feel free to add to the discussion in the comments section.)  Without further ado, here are five observations about grad school.

[All illustrations are my own and brought back memories of my failed first-year aspirations of becoming a chalkboard Banksy.]

1. Grad school: more like Zelda than Mario

College is a lot like a Super Mario Bros. video game. You wake up, go to class, do the homework that’s assigned, and study the chapters you were told to, and rock the exam after practicing on past exams. Sure, sometimes you have to try a few times before you can make that jump right at the end of the level, but at each step it was clear what you had to do.

You may have to rethink your measures of success and re-evaluate the tools you need to get there.

Grad school is different. You can’t just wake up in the morning and do all the stuff that you know you have to do—because research is precisely about figuring out what to do when it is not clear at all what the next step is. In this respect grad school is more like playing a Legend of Zelda video game.

Unlike coursework, research is about open questions. Usually these questions are still open for a good reason: they’re hard! You won’t have an answer key in the back of the book or a TA’s office hours to show you the trick. There’s no road map; you need to carve out your own path and figure out what tools you need to develop to move forward. Sometimes there will be dead ends and you’ll have to back-track, but in the end this can be a rewarding experience. You don’t remember Mario Bros. for how hard it was to stomp on Bowser’s head, but you do remember all the time you spent trying to figure out the puzzle to break into that one dungeon so you could rescue Zelda.

2. Get paid to do what you love—just not very much

One of the perks of grad school that often surprises non-academics is that yes, you get paid to do science! (Usually this is associated with doing some teaching.) In a difficult economy and with undergraduate student loans soaring, this is a welcome respite from large tuition bills and reliance on parental support. On the other hand, don’t expect to be drowning in disposable income.

One trick to stretch out your stipend money: lower your standards when treating yourself to something nice.

Just be careful not to fall into the trap of comparing your income to your college friends who got ‘real’ jobs. That being said, you’ll have health insurance, be able afford an apartment and food, and most importantly, you’ll have the freedom to work on what you want and how (and when) you want to.

3. Somewhere between being a kid and a grown up

Maybe it’s just me (and I really hope not), but part of being a grad student is living precipitously on the edge of growing up. My personal experience has been full of office pranks, jokes, and the “child-ish” silliness that sometimes comes with the “child-like” curiosity that is at the heart of being a scientist. At the same time, one has to balance one’s aforementioned budget, keep pushing the less-fun parts of projects, and be responsible for the direction and content of one’s research.

It’s worth mentioning that sometimes it can feel like the rest of the world is growing up way faster than you are. In addition to earning much more than you, your old high school friends will be getting married and starting families—the latter of which is something which can be difficult (though not impossible) as a young academic.

High school reunion can be a reminder that everyone else has "grown up" while you're still in school.

In a larger sense, grad students are fledgling scientists, apprentices to professors who train their academic offspring. And just like biological offspring, it’s often the case that the apple doesn’t fall far from the tree—after all, your grad school mentors are the ones who teach you how to think about your science, how to grapple with hard problems, and (very important) how to interact with other scientists.

4. Sometimes the next step is a step back

Whatever discipline you’re in, and no matter how smooth things seem to be going for the other students, graduate school is hard. (So are professional schools and real grown up life, for that matter.) Sure, most people are prepared to spend their PhD working on hard research questions. What people don’t usually expect is that often it’s actually everything else that makes a PhD hard: balancing your work with the rest of your life.

“Rest of your life?” It’s a cliche that grad students don’t have lives outside of their labs, and it’s completely wrong. The most successful students—both in undergrad and grad school—are often the ones who have something else that they’re passionate about and that is totally unrelated to their work. Maybe music or art, maybe a particular sport, or a social activity (blogging?)… something to dive into and keep you sane when work isn’t going well—and there will be times when work is not going well.

In many ways the defining moments in graduate school aren’t when research is going well, but rather those times when it feels like everything is crumbling beneath you. Those moments when you feel like you should chain yourself to your desk until everything works? Those are usually the times when the best thing you can do is to take a step back for a bit and relax.

It’s crucially important to recognize that things will not go as smoothly as you plan. Consider the following very-scientific graph of happiness over time.

Actually, the pointy curves come from something I've been working on (with different labels).

Naively, one might imagine that grad school is a period where you just keep learning more and more about something you enjoy until you steadily become the world expert on something really important. What actually happens is that you spend most of your time grappling with the frustrating problems that prevented other people from doing this research before you. Then, with some luck, there are brief moments of ecstatic clarity where you make progress: you’ll remember why you’re doing a PhD and all will be right in the world… for maybe a day or two, at which point you’ll come up to the next hurdle that you’ll have to struggle with.

This perpetual struggle at the heart of research can be hard to swallow, especially for those to whom undergraduate coursework came fairly naturally. The feelings of self-doubt that often arise are so common that it even has a name, impostor syndrome, wherein people feel like their struggles indicate that they are not ‘good enough’ to be a PhD student and their university made a big mistake accepting them to such a program. Just remember: all this is normal! (See Zelda analogy above.)

Footnote: Not every PhD becomes an academic!

I wanted to address something related to this: not every grad student goes on to become an academic, and that this is okay. Somehow it’s almost taboo to talk about going off into industry after grad school instead of continuing to become a postdoc and then a faculty member somewhere—even though there are clearly fewer postdoc positions than grad students, and fewer still faculty hires. (I think it’s great that Burton’s mentioned this in recent posts.)

While there is something special about spending your life pursuing fundamental science, but that doesn’t mean it’s the right path for everyone. And this is not to say that some people “aren’t cut out” for research or that their PhD was not well spent: I’ve seen some truly special and talented individuals with bright academic futures decide that they would be happier applying the skills they developed on something else. And that’s great—one of the reasons why our country invests in fundamental research is to support a highly skilled workforce doing exciting things outside of the ivory tower.

I’ve had difficult conversations with multiple young academics who have struggled to weigh their passion for science against pragmatism: what if they can’t find a job sufficiently close to their spouse? What if they want to settle down and start a family rather than having to bounce between temporary grad and postdoc positions? What if they need to take care of ailing parents and cannot hold off until the indeterminate future to secure that kind of financial stability?

Fortunately, a PhD is something which generally translates into marketable skills “in the real world,” and I think it’s important for those in academia to recognize that sometimes good people will leave the field for good reasons.

5. How to be a good graduate student

I’d like to wrap up by once again addressing the next generation of grad students with some unsolicited advice from someone crawling towards the light at the end of his own PhD tunnel.

1. Find good mentors. Your adviser will have a big impact on your PhD and career, but you should also make a point to find mentors in the form of other faculty, postdocs, and graduate students. Learn as much as you can from the people around you, especially when they can offer advice that they had to learn the hard way.

2. Persistence and enthusiasm goes a long way. You can expect to run into setbacks and roadblocks. One of the most useful things you can develop is an enthusiasm for your work and the persistence to keep pushing even when things feel futile. Persistence and enthusiasm can make up for a lot of things: lost sleep, raw intelligence (when you feel like everyone else is smarter than you), gaps in your problem-solving toolbox, etc.

3. Learn how to communicate. One of the cornerstones of science is being able to effectively communicate your work to others. Learn how to effectively read and write papers, and learn how to give good talks about your research.

4. Use your freedom wisely. For the most part, people won’t tell you how to spend your time. It’ll be up to you to work on what you want, when you want to, and however you think will best solve the problem. Just be careful that you’re not using all of this extra rope to hang yourself. Find the right balance of work and play that works for you.

5. Science is social. There is synergy in academia. People wonder what theorists do all day long since it seems like all we do is to think up silly ideas—we spend most of the day talking to each other. Ideas are meant to be bounced off of one another: revised, refined, and re-assessed. Don’t fall into the bad habit of hiding in a hole in the ground until you find the answer—make use of the community around you!

Science is a team sport, it helps to figure this out earlier rather than later.

While we’re on this note—take time to be part of the science community in your field. There are some scientists who develop their best ideas while hiking with friends or at a pub after a conference.

6. Let it be fun. Despite all the things one has to struggle with from research to personal life and everything in-between, grad school is a special time in your life; enjoy it.

Expectations for a new LHC year

Ken Bloom
Thursday, April 5th, 2012

As has been reported elsewhere, the LHC is off and running again. Yesterday we saw the first stable beam collisions of the year. So far, collision rates are extremely small, and the detectors are just being roused from their winter slumber, so there is certainly no physics news to report yet. Over the next few days and weeks, the LHC will, fill by fill, increase the number of proton bunches circulating in the machine, and thus the collision rates. Meanwhile, the experiments will check that all of the detector elements are functioning and calibrated, which will allow us to get back to our full menu of work.

So what can we expect in the year to come? Here are a few things that I could think of.

  • The standard model, again. The LHC has increased the collision energy from 7 to 8 TeV, meaning that once again we have the highest-energy collisions ever created in a controlled experimental environment. One of the first things that happened when we started taking 7 TeV data was a full exploration of the production of known particles, to see that the rates etc. matched the predictions of the well-established and well-tested standard model. Now that we’re at 8 TeV, we’re going to do it all over again. This isn’t going to be making the front page of the newspaper, but it is critical work that must be done; if you can’t show that you understand the “known” physics, you can’t argue that you are seeing any kind of new physics.
  • OK, so is there a Higgs boson or not? This one will make the front page of the newspaper! As we last saw, CMS and ATLAS (and the Tevatron experiments) have results that suggest that we might be just on the edge of observing the long-awaited Higgs boson. Or perhaps not; everyone agrees that these results might be fluctuations that could well disappear when a larger dataset is analyzed. The expected production rate for a Higgs boson is greater with 8 TeV collisions than 7 TeV, and we hope to record at least three times as much data as we did last year. By the end of 2012, we should finally have an answer to the Higgs question.
  • The race for Bs. Here is another place where CMS, LHCb and perhaps ATLAS are just on the edge of making a discovery. The decay of the Bs meson to a pair of muons is expected in the standard model at a very low rate. This decay is particularly sensitive to effects from physics beyond the standard model, which could cause the rate to be either higher or lower than that predicted by the SM. It won’t take that much more data for each of the experiments to be able to observe the decay at the predicted rate…if that is indeed what happens. This could well come down to who can process and analyze data most quickly.
  • How’s that pileup thing working for you? To get more data this year than last year, the LHC will be colliding more protons at a time. Every collision of interest will be accompanied by debris from additional uninteresting collisions. This puts a strain on just about every aspect of the experiment — the volume of the data that must be read out, the complexity of event reconstruction, the requirements on computing resources, and the sophistication of the final data analyses. The sensitivity of many analyses can be degraded by this “pileup” of additional collisions. The experiments will have to be able to control all of these factors to get results out.
  • Will we ever find anything? It’s true; every search for new particles at the LHC has come up dry so far. We’ll try again this year, with a lot more going for us. Just like with the Higgs, pretty much any new particle will be produced at a higher rate at the higher collision energy, and we’ll also have much more data to look at. And with 2012 being the last year of LHC operations before a two-year long shutdown, we’ll be pulling out all the stops in the searches.
  • What will be ready for “summer” conferences? The next big public landmark for presenting new results will be the 2012 International Conference on High Energy Physics, which starts on July 4 in Melbourne, Australia. (This is traditionally a summer conference, but in the Southern Hemisphere it will be a winter conference, although it seems winter is mild in Melbourne, at least by Nebraska standards.) There will be about three months of LHC operations before then. What sort of results will be ready in time to show at that forum? Will anyone be able to produce a discovery by that time. I think it’s going to be very challenging, but who knows? (I got asked to co-organize one of the ICHEP parallel tracks, so I will be attending — very exciting! I will be sure to blog and tweet as much as I can from there, assuming my computer works when it is upside down.)
  • OK, readers — what are you expecting from the LHC this year? We welcome your comments.

    Conference-going for the almost-graduated

    Burton DeWilde
    Monday, April 2nd, 2012

    I’m currently writing you from Atlanta, GA, where I’ve been attending the APS April Meeting on particle, nuclear, and astro physics (this year’s theme is “100 Years of Cosmic Ray Physics”). Officially I’m here to give a talk on my thesis research (the leptoquark search I’ve been alluding to for some time but still haven’t fully explained — patience, it’s coming!), but really I’m here to network and interact with other physicists re: getting a job post-PhD.

    Self-promotion comes naturally to some people… Not me. I prefer to casually undersell, which is a bit of a problem given that resumes are crafted to formally oversell a person. Still working on my elevator pitch.

    At any rate, the conference has provided a number of opportunities for an almost-graduated job-hunter to explore interesting intellectual avenues and make connections with advice-givers and potential employers. I was fortunate to attend a panel discussion held specifically for grad students on the topic of careers, networking, and carrying out a job search. In addition to providing an occasion for free food, the panel also imparted some very useful wisdom:

    • Create individualized resumes and cover letters for each position you apply to. Whoever reads your application will know if you’ve done your homework or, alternatively, if you’re trying to catch a bunch of different fish with the same net. Heads-up: Most fish will slip through.
    • Communication is essential. You can’t expect employers to infer why it is that they should hire you, you have to tell them, in clear, understandable terms.
    • Networking is also essential. People often get jobs because they “know somebody who knows somebody,” so it is beneficial to your job search to talk about your qualifications and what you’re looking for with as many people as possible. If that sounds obnoxious, well… indeed it is, but don’t let that stop you! :)
    • Maintain interests and passions outside of those in your particular sub-field. Physicsts are “all-arounders” that perform well in a variety of tasks; a surprisingly large fraction of physics PhDs get jobs totally unrelated to their thesis research or, in fact, physics. Being well-rounded is a strength to be valued and emphasized.

    Tonight is the last night of the conference. Earlier today I nailed my talk, even getting a couple general laughs from a room full of physicists (not easy!) so now I just have to find myself an interested future employer or somebody who knows him. I’ll be in the hotel bar, working on my pitch and resumes — let’s chat!

    — Burton

    Tools of the trade: MC4BSM 2012

    Flip Tanedo
    Sunday, April 1st, 2012

    Last week Cornell hosted the sixth “Monte Carlo Tools for Beyond the Standard Model” mini-workshop and I thought it was a terrific success. Here “Monte Carlo” refers to the computer simulation techniques used to solve difficult problems such as the behavior of high energy particles at the LHC. The name is a reference to the famous casino in Monaco since these methods are based on random sampling.

     

    MC4BSM poster: if CMS reminds you of a roulette wheel, you may have a gambling problem.

     

    Playing Dice with the LHC?

    It’s not what it sounds like. At first glance talking about ‘random sampling’ might make it sound like someone doesn’t know what they’re doing. It’s actually quite the opposite. The theory of hadron colliders (which is mostly quantum chromodynamics) is well established, but actual calculation requires compromise.

    I won’t go into details, but the rough sketch is that a high energy collision at the LHC does not look like the nice Feynman diagrams that we’ve been drawing (and that we can calculate easily):

    Nope. In fact, the events look much, much more complicated (from S. Hoeche’s talk):

    Needless to say, this is very difficult to calculate using pen and paper. In fact, the situation is even more difficult than it looks: many of the steps in this calculation require systematic approximations and are non-perturbative (hopeless to calculate in the usual method). There’s more: the above picture is just what happens when there’s a high energy collision in vacuum. We also have to model how all of that interacts with the detector to give a picture more like this:

    It is practically impossible to calculate a closed form expression for the Standard Model prediction for the distribution of detector signatures. On the other hand, what we can do is imagine actually simulate particle production and decay at each step of the process so that the random evolution of the initial collision into the final detector signature follows the probability distribution of the “closed form expression” that we can’t write down. By doing this many times, we can determine the probability distribution simply by looking at the distribution of the Monte Carlo simulation.

    This probably still sounds a little abstract—but it’s the analog of determining the interference pattern of the double slit system by actually doing the experiment with electrons and looking at the distribution of electron hits on the screen. Another nice example is to determine the area of a circle (or the value of π) by Monte Carlo.

     

    Tools of the Trade

    Suffice it to say that Monte Carlo is a very important tool in high energy physics. For example, the results of Monte Carlo studies are used to determine what sorts of events we should be looking at to find the cleanest signals for a Higgs or for new physics—this sort of thing is especially relevant since the rate of high energy events at the LHC is actually much larger than our bandwidth for recording data, so we need to be able to trigger on particular events that we think are worth a closer look.

    On the more theoretical side, Monte Carlo gives us a handle for mapping models of new physics to experimental signatures. For example, if we see a definitive signal of a new particle outside of the Standard Model, how can we begin to determine whether it is a supersymmetric partner, an extra dimensional resonance, or something else?

    In between theory and experiment, there’s a lot of hard work done ‘in the trenches’ to develop better tools (both theoretical and computational) to model quantum chromodynamics. Often times this is under appreciated in the field since the work is not glamorous enough to land in one of Dennis Overbye’s New York Times articles, but recently three of the leaders of this field received the 2012 Sakurai prize—congrats to AltarelliSjostrand, and Webber!

    Theorists will wax poetic about espresso machines and long nights at a chalkboard, experimentalists will tell you what it’s like to jump into the world’s largest scientific apparatus (armed with a vacuum cleaner), but the truth of the matter is that we spent a lot of time running computer simulations. We rely on the subset of the community that develops and maintains these tools, and occasionally we hold workshops (such as MC4BSM) to learn the latest and greatest tools.

    MC4BSM 2012

    Probably the first mystery of the MC4BSM series of workshops is the strange logo:

    Apparently the illustration was done by a professional artist who is a friend of one of the organizers. The interpretation still isn’t clear to me—though it’s been suggested that it represents the “elephant in the room” associated with the lack of training opportunities to learn Monte Carlo techniques. Alternately, it was also pointed out that it’s a different kind of “pink elephant.”

    The workshops are geared toward an audience of theorists who don’t necessarily have a background in Monte Carlo methods. The “big idea” is connecting our models of new physics to experimental data (image from M. Perelstein’s slides):

    The key to doing this efficiently has been to develop a pipeline of Monte Carlo tools which interface with one another and take a theorist’s model to something that can be compared to real data; one example of such a pipeline is (image from C. Duhr’s talk):

    The ovals are different stages of computational tools—the first two or three stages can usually be done by hand by a careful graduate student. From there on out we really rely on the Monte Carlo tools available to us. The red text highlights common programs used to connect each step, while the green-ish text are common languages that are used to provide a standardized language for program to communicate with one another.

    All of these programs are open source (though some depend on commercial software like Mathematica) and are developed by high energy physicists for high energy physicists.

    Tutorial

    The real highlight of the workshop were the two tutorial sessions where attendees had a chance to play with various programs in a hands-on environment. The whole point of the meeting, after all, is to learn how to use these tools. The tutorial session allow attendees to ask questions directly to the program developers and to build their own templates by solving a simple toy problem.

    Unlike previous MC4BSM workshops, the organizers adopted a novel format for the tutorial sessions which I thought worked very well. Each participant brought their own laptop and had a choice choice of which chain of programs they would use to solve the toy problem:

    Instead of having representatives from each program give a short talk about how to install and run their code, users were left to themselves to jump in head first with their colleagues and then flag own experts as needed. (The night before the workshop there was also a group installation session where people could work out kinks in getting specific programs to compile on specific operating systems.)

    Several of the graduate students there got their first taste in going through the entire series of programs, while more senior researchers learned how to use alternate tools than the ones they’re used to.

    The tutorial information is all available online for anyone who wants to follow along on their own. The material will eventually be made available as proceedings for the workshop; I think it will be a valuable resource for anyone interested in learning to use these tools.

    Human vs. Machine

    One of the running jokes at the workshop was that eventually we’d be able to select a few options in a smart phone app to cook up a model of new physics and then send it to a computing cluster to work out the detailed phenomenology—perhaps obviating the need for graduate students. However, one thing that computers cannot yet replace is the value of having face-to-face interactions with one’s colleagues.

    I’ve said many times that physics is a social activity and the field progresses from the collaborative efforts of the entire community. Meetings like MC4BSM are more than just ways to learn new tools, but are also ways to catch up with friends and colleagues and bounce new ideas off one another.

    One bright idea that was promptly shot down was a request to hold the next MC4BSM meeting at the Monte Carlo casino in Monaco.

    Physicists discover large body orbiting Earth!

    Aidan Randle-Conde
    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!

    The great vacuum in the sky

    John Huth
    Thursday, March 29th, 2012

    This is the zone rockets traverse in Thomas Pynchon’s novel Gravity’s Rainbow. I got e-mail from a reader who didn’t understand the concept of the vacuum. The writer didn’t think it possible, and is in good company. Neither Plato, nor Aristotle, nor even Descartes believed that a pure vacuum could exist.

    A ‘vacuum’ in the most common sense is simply the absence of matter in some volume. Early experiments by physicists Torricelli and Boyle with vacuum pumps demonstrated that at least a partial vacuum was possible and could be created on earth. A standard measure of the purity of a vacuum is often expressed in the unit of pressure called a “Torr”, after Torricelli. The pressure at the surface of the earth is 760 Torr. The creation of vacuums of increasingly rarefaction has been possible with more and more powerful pumps. First, there is a mechanical pump, much like a piston engine in a car, which can achieve a pressure of about 10E-5 Torr. Then, there is a turbomolecular pump that uses a high-speed turbine to rid a chamber of gas. Beyond this, there are ion pumps, which trap atoms in a chamber by bombarding them with ionized atoms. At very low temperatures, physicists can take advantage of cryopumping where molecules can be made to stick to cold surfaces.

    Why are vacuums important to the LHC? As you might be aware, we have to cool the magnets to a degree or so above absolute zero. In order to do this, we effectively have to create a giant thermos bottle to help keep the magnets cold. This uses a vacuum as the first stage of insulation from the outside world, which prevents the transmission of heat across the barrier of the vacuum.

    The beam pipes of the LHC must have a very clean vacuum in order to keep protons circulating in the accelerator tubes without colliding with errant gas molecules. To do this, the pipes the protons travel through are typically maintained to a vacuum of 10E-9 Torr. At the interaction points, where the collisions take place in the middle of the detectors, extra care has to be taken to reduce the number of gas molecules even further, so more cryopumping is used to get the vacuum down to a level of 10E-11 Torr.

    To give you some idea of what 10E-11 Torr is like, it’s akin to the pressure in interplanetary space. Present estimates of the vacuum of space far between galaxies is more than 1000 times lower than that, with 6 hydrogen atoms per cubic meter.

    In a sense, these are all ‘partial vacuums’ – meaning that there are still atoms floating around. But, if we were able to make a perfect vacuum pump, would this mean that there’s absolutely nothing but space in such a creation?

    The answer is ‘no’ and somewhat bizarre. In quantum field theory, there is a concept of ‘virtual’ particles, which are always being created and destroyed in empty space. For example, an electron and an anti-electron (called a positron) can be created momentarily in free space and can then fall back together again. If we introduced a free charge to this perfect vacuum, these electron-positron pairs would polarize and tend to screen the charge of the particle.

    Beyond these virtual pairs of particles, there is something even stranger, that we sometimes associate with the Higgs boson, called a ‘vacuum expectation value’. This is to say, in a perfect vacuum we expect that there is some non-zero amount of the Higgs field floating around. Now, one may be quick to dismiss this as just some figment of a theorist’s imagination that has no consequence. Measurements of the rate of expansion of the universe, however, indicate a strange ‘dark energy’ that permeates free space and is forcing the universe to accelerate its expansion. This dark energy appears to be an energy that will inhabit space devoid of any matter whatsoever and is akin to the ‘vacuum expectation value’ in many ways. No one knows why this dark energy exists, but it is permitted by Einstein’s equations describing the large-scale structure of the universe. We just didn’t expect to see it, and it seems to lurk everywhere.

    So, perhaps the ancient philosophers were right: there may not be a pure vacuum in nature after all.

    Not all things are created equally…

    Anna Phan
    Wednesday, March 28th, 2012


    At the end of my last post, I left you all with the above plot (from this ATLAS conference note) without any real explanations. It’s actually quite a nice result, so I thought I might go through it in a little more detail today.

    So what does the plot show? Reading the axes, it shows the lepton charge asymmetry as a function of lepton pseudorapidity of leptonic W events.

    What does this actually mean? To answer this, let’s go back to what a W boson is. On the right here, it’s a cute little plush toy, which you can buy from Particle Zoo. In real life, it’s massive charged elementary particle. This means there is a positive W boson, and a negative W boson, \(W^+\) and \(W^-\) respectively. When a W boson decays into a charged lepton and corresponding neutrino, due to charge conservation, the charge of the lepton must match the charge of the W boson. So the above plot of lepton charge asymmetry is actually a plot of W charge asymmetry, which can be interpreted as a W production asymmetry, \(A_W = \frac{\sigma_{W^+} – \sigma_{W^-}}{\sigma_{W^+} + \sigma_{W^-}} \).

    So why is there a W production asymmetry? Let’s look at how a W boson is produced in a proton-proton collision. On the left here, we have a Feynman diagram of this process, where you can see that to make a positive W boson, you need a certain combination of quark and antiquark, most often an up quark and an antidown quark. To make a negative W boson, you need the opposite combination, a down quark and an antiup quark.


    The production asymmetry occurs because, as illustrated in the diagram on the right, the proton contain two valence up quarks and one valence down quark in a sea of quark-antiquark paris and gluons. So in a proton-proton collision, there is a higher probability of a up and an antidown quark interacting than an antiup quark and a down quark, and hence more positive W bosons are produced compared to negative W bosons.

    So that’s why there’s a W production asymmetry, but why does it depend on pseudorapidity? And what is pseudorapidity anyway?

    Well, pseudorapidity is a measure of the angle at which the W boson was produced, which depends on the momentum of the two quarks from which the W boson was produced. The quarks and gluons within a proton carry a fraction, \(x\), of the total proton momentum, which is described by a parton density function \(f(x)\). The plot on the left shows the proton parton distribution functions for various types of quarks and anitiquarks, as well as gluons, for a particular proton collision energy scale \(Q\).

    So the momentum of the quarks which produce the W boson varies from collision to collision, depending on their parton density functions, which causes the W production asymmetry, caused by the quark content of the proton, to vary with pseudorapidity. Which is what the plot shows!

    Not just B physics!

    Anna Phan
    Tuesday, March 27th, 2012

    Today, I’m going to be talking about some lesser known LHCb results. In fact, I’m going to discuss physics that some people thought LHCb couldn’t do, given the detector and software design.

    What am I going to be talking about? Electroweak physics. Yes, you read that right, not the heavy quark physics which LHCb was designed and built for, but electroweak physics. In particular, I’m going to discuss some of our new results on Z and W boson cross sections, which will be presented at the DIS workshop in Bonn this week.

    But before I go into the results and why they are interesting, let me quickly introduce the Z and W boson, as found at The Particle Zoo. Theorised in the 60s and discovered in the 80s, they are massive elementary particles that mediate the weak force. Z bosons are neutral and decay into a pair of leptons or quarks. W bosons are charged and decay into either a charged lepton and neutrino or two quarks.

    At the LHC, Z and W bosons are usually identified by their leptonic decays. The signatures that electrons, muons and tauons leave in the detectors are much easier to find and measure than those left by quarks. In LHCb, we are able to detect Z decays to a pair of electrons, or muons or tauons and W decays into a muon and corresponding muon neutrino. Unfortunately, we aren’t able to cleanly identify W decays to electron or tauons and their corresponding neutrinos.

    Above I present a summary of all the Z and W cross sections we have measured so far using data from 2010. On the left are the Z cross sections, given separately for each decay mode, while on the right are the Z and W to muon cross sections and various ratios of them.

    If you are used to seeing LHC results, these may look a little strange. Usually the data is shown as black solid points while the theory is shown as coloured bands. Here the data is shown as the coloured bands, while the predictions of various theoretical models are shown as black open points.

    Why this confusing presentation you ask? Well, that has to do with why we are trying to measure the Z and W production cross sections in LHCb.

    As I’ve mentioned before, LHCb has a unique geometry compared to the other LHC experiments. In particular, with our cone geometry, we cover the forward region of 1.9 < y < 4.9, while ATLAS and CMS cover |y| < 2.5 with their cylindrical geometries.

    In terms of proton-proton collisions and the production of Z and W bosons, this means we are able to probe a complementary region of phase space. The plot on the right illustrates this, where you can see that LHCb is able to explore the low-\(x\), high \(Q^2\) region inaccessible by other experiments (past and present).

    This is important as this is the region where there is the highest uncertainty in the theoretical predictions in the Z and W production cross sections. So ideally, we would like to use experiment to constrain the theoretical predictions.

    I say ideally, as if you look at our current results, we don’t have the experimental precision to do this. But we will in the future, so be on the look out!

    Of course we aren’t the only experiment looking at Z and W production cross sections, ATLAS and CMS are as well, so I feel obliged to show you this plot on the left, which is of the W lepton charge asymmetry as a function of lepton pseudorapidity from ATLAS, CMS and LHCb…