08:02:31 Okay, I think we're ready to start.
08:02:34 Welcome to the second day of our novel experiments conference on behalf of Josephine, Anna Maria and myself.
08:02:42 For the first session this morning we're going to go to particle accelerators we're double experiments are also being done. The first talk is joint with a high energy precision 21 program at KITPB Jamie Boyd on a novel set of detectors the fire detectors
08:02:58 at the LHC Jamie, the floor is yours.
08:03:02 Okay, thanks a lot. So thanks for the invitation to give this talk, and as Doug said I'll be talking about a set of mostly proposed new experiments that can be added to the LSC physics program in order to try and increase the sensitivity for new physics
08:03:18 searches at the existing Alexi facility.
08:03:22 So just to set the scene a little bit so as you know there's been excellent performance of the LHC accelerator and also the detectors, but yet the Alexey experiments have not found any evidence of new physics.
08:03:38 And this is of course frustrating.
08:03:56 So beyond the Standard Model Long live particles, theoretically well well motivated and less well, in some sense, less well searched for scenario, and so they may be one of the best remaining options for a new physics discovery at the LHC so this is a
08:03:58 little bit work. These experiments I talked about is interested in.
08:04:03 And so the current existing and he experiments the big experiments like Atlas and CMS are putting an increasing emphasis on searches for these things that long lived bsm particles.
08:04:13 But there's also a number of dedicated proposals for new dedicated long the particle search experiments at the agency.
08:04:20 And this would be to try and increase the coverage for theoretically motivated, new scenarios.
08:04:25 So in some sense these new experiments could be considered good value for money because although they will of course costs money themselves they would be increasing the scientific output from the LSC hopefully increasing the chances of discovery, and
08:04:37 yet he was of course something it was extremely expensive to build and it's expensive to operate. So we should try and squeeze as much physics out of it as we can.
08:04:45 Most of these new experiments are searching for neutral Long live particles, which then decay into charge Standard Model particles and this mean that they all follow us sort of similar principle in how they would try and do this.
08:04:57 But the proposals do cover a wide range of detector sizes and costs. And so even though they mostly rely on the same sort of principle. There's a really big variety and that sort of size and cost of these different experiments and so that means there's
08:05:11 also a big range in sort of where the proposals are in terms of getting approval to be installed, where they are in terms of funding and readiness for being installed.
08:05:22 So yeah, I'm just having one smooth issue with my zoom so yeah this is sorry for this.
08:05:30 Okay, so moving to the next slide. So just to briefly motivate why we should search for new long new particles in general and that the legacy so this is a plot which is shown in many of these types of talks which try to meet this, this is showing the
08:05:44 lifetime of particles in the standard model as a function of their mass. And what you can see is that even in the Standard Model there's a huge range of lifetimes, that particles have from basically stable particles to strongly decaying particles which
08:05:58 have extremely short lifetimes. And what causes this spread in the lifetime to these particles is mostly coming from an approximate symmetries which would if they were true symmetries would make the particle stable, but since the symmetry is an approximate
08:06:18 symmetry. This means that instead the particle has its decay is suppressed and this leads to having some finite overtime. So of course the same type of thing can happen in the on the standard model of physics theories.
08:06:27 And, in fact, lonely particles can very naturally occur in many of the bsm theory. So to give you an example of different ways this can happen. You can have weak couplings so for example in supersymmetry you can have weak couplings associated with the
08:06:41 weakness of gravity or with apparently violating couplings. You can have the keys which are suppressed because of the face space of the final state particles, or you can have the keys which have to go through very heavy mediated particles, which then
08:06:55 also suppresses the, the case. So that's an example that happens in Split Susie which is a type of model.
08:07:03 And in fact, maybe more relevant for most of the detectives that I'll talk about today, the dark sectors which are, of course, sort of new sets of particles which are associated with dark matter.
08:07:15 And so when you have a Dark Sector with light mediators in them. This naturally gives you weak couplings. So this is all because the mixing between the duck sector particles and the standard model is three processes which, if you read couplings.
08:07:29 And in fact, if your dog sector mediator is going to give you the dark low correct Dark Matter Vedic density that's been observed, and the dark matter particle is light, then this also naturally implies that you have a weak coupling so you can see that
08:07:45 in this sort of sketch here which I stolen from Jonathan thing.
08:07:48 And so this is showing interaction strength, versus the mass of a dogmatic particle. And if you have very low masses, then in order to get the right amount of dark matter you need to have low, very low couplings.
08:08:02 And once you go to heavier masses, the kinds of masses that the LHC was originally designed to discover new particles that have ordered TV, then you have all the one couplings.
08:08:12 So that was the top right of this party is kind of what the traditional hc experiments were expecting to find and these are the one couplings means that the particles are not long lived but they decay promptly.
08:08:22 We didn't see any of these types of particles in the galaxy yet, unfortunately. And so maybe the reason is that actually the new physics is light and weekly coupled, and these are the type of area where the new physics political that the experiments I'm
08:08:34 going to discuss today, become relevant.
08:08:38 Another thing that's of course very important at the LHC is the fact that we can produce Higgs boson, and the Higgs boson has many interesting properties but something that's interesting about it is has extremely narrow width of any for MTV.
08:09:01 And this means that even for sort of things which are weekly coupled to the Higgs they can still have a relatively large punching faction, because of the narrow width of the Higgs so long the particle experiment at the Elysee can be sensitive to the Higgs
08:09:07 decaying too long lived bsm particles, and there's room for this quite a reasonable bunch interaction. So at the moment the limits on the Higgs to invisible decays from Atlas Atlas and CMS the best limit so it's sort of at the 10% level so 10% of the
08:09:22 bunch infection, could be going to be SM particles which wouldn't be seen in the traditional searches, which is what you would expect from these type of Long live particle the case.
08:09:33 So that's a little bit of the theoretical motivation for searching for bsm normally particles. So what are the main ways that we want to design these experiments.
08:09:42 So, since what we're looking for is generally rare. An important thing to do and try and do is to really reduce the background as much as possible and really try to be background free.
08:09:52 And the way that this is done, is by putting in shielding and distance between the interaction points in the galaxy so where the collisions happen, and where these new experiments are.
08:10:03 So by putting in shielding and distance you can suppress the huge rate of standard model particles which are produced in the galaxy collisions, and therefore, try to make a background free type of experiment.
08:10:14 And so most of these experiments are what we call a sort of light shining through all types of experiment and so I tried to draw a sketch here, the bottom.
08:10:21 To give you an idea what this means. So we have the galaxy collision here, which is producing a huge number of particles, I mean the collision rate in the Alexia is extremely high.
08:10:29 But then we have a lot of shielding or a lot of distance or both, such that all of the Standard Model particles absorbed in the shielding and don't make it to a detector.
08:10:39 And then this red dotted line here is trying to suggest that we have a neutral. Long live particles and this is the bsm particle we're looking for. It goes through the shielding, and then it can decay in our detector, and based on the fact that it's got
08:10:53 an exponential decay distribution so we're not forcing it to the cage just the case here because its lifetime. And it decays into in this case to standard model particles and we would look for this.
08:11:02 Nothing in, and two particles out with coming from a common vertex and this would be the signature that we look for.
08:11:08 Now of course it's not really true that none of the Standard Model particles produced in the collision would make it into a detective in this example, but if we have sufficient shielding we can get rid of all the drones.
08:11:18 And basically what the only particles from the standard model that should make it through here, new ones and neutrinos.
08:11:24 And of course, one of the challenges of these types of experiments is then to convince yourself that you really can suppress the new ones and Eugenia related background but it's very important to have the shielding to get rid of all the hedonic background
08:11:36 which is huge at the latency.
08:11:39 So you also want to put your detector at an interesting place in the lifetime parameter space, and in particular they should be complementary to the existing Alexi experiments, so that generally means putting your detector further away than the size of
08:11:53 of the cone, Alex the experiments that listen to us.
08:11:56 And so the experiment I'll talk about between 10s and hundreds of meters away from the interaction point.
08:12:02 On the other hand, of course, because what you're looking for is rare you also want to cover a have a good acceptance for these type of particles to go into your detector so this means you have to cover a substantial part of the solid angle, which is
08:12:13 of course different difficult if you're very far away from the interaction point, and in some cases instead you can place the detector in a specific location which gives you a maximizes the flux of signal particles that will go into your detector.
08:12:26 And finally, possibly most importantly the detector has to be affordable. And so in this case, what people have tried to do is take advantage of existing infrastructure in the LHC complex as much as possible.
08:12:37 So for example using unused tunnels or cabins or galleries, or even spaces on the surface, in order to be able to put your detector in this place without doing special civil engineering work, etc.
08:12:50 You do get some challenges associated with trying to put detectors in places for which weren't originally designed for this but of course it doesn't mean that you can save substantial money and time without having to dig your own detector location.
08:13:04 Okay, and I want to say wanted to highlight that at CERN this this effort called physics beyond colliders which is a study group that's been set up at CERN about five years ago, and this has been extremely helpful in sort of helping to study the proposed
08:13:15 new detectors and push them through. And so, physically and colliders has dedicated resources to look at things like civil engineering installation of services for the detectors integration and safety aspects, and this has really been, I think, fundamental
08:13:31 in being able to get some of these detectors and these experiments up and running and for pushing for a new ones to also be realized.
08:13:39 The final sensitivity. So, what kind of exclusion or discovery potential these experiments have is a really complicated function of their location, the production process which produces the lonely particles that you're searching for how they can reach
08:13:53 reduce the backgrounds and their acceptance so this is something that you can't really easily sketch and you have to add Monte Carlo simulations in order to assess this sensitivity.
08:14:04 Ok so now I just want to flush through a few of these proposed detectors starting with fazer. So fazer is a very small experiment which is situated in the very forward region of the collisions in Atlas.
08:14:16 You can see in this sketch here so this is a sort of schematic of the LHC where IP is the collision pointing Atlas, and the LSC goes in a straight line here for 270 meters, and then it starts to slowly bend away from the this straight line the condition
08:14:31 access in order of course to complete circle in 27 kilometers, which is the circumference of the galaxy.
08:14:39 When you were about 480 meters away from this interaction point that the collision axis is about five meters away from the LSC machine, and it crosses this unused tunnel called to 12 that you can see in the bottom of this sketch.
08:14:51 And so this tunnel is where phase was positioned and this allows the detector to be centered on this collision axis. And it turns out that this is a very good location for looking for certain types of new long lives new physics particle.
08:15:04 This TI 12 tunnel was an old injection tunnel. When lap. When the Alexi was tunnel was used for the left collider This is how they injected electrons intellect, but when they built the LHD they used a different injection tunnel.
08:15:16 So to 12 is unused and Faiza takes advantage of the fact that this collision axis crosses this to 12 tunnel.
08:15:22 So this is about 500 meters from Atlas and it's a detective that's looking for a long live particle light particles that are produced in means on decay in the very Ford region.
08:15:33 So, in order to realize this detector, we measured particle rates and radiation in this tunnel during 2018 running up the LHC and found that these are compatible with putting an experiment there.
08:15:43 And what's kind of nice here is that a particle from the interaction points of phase that goes through 100 meters of rock.
08:15:49 So this provides the shielding from the Standard Model particles.
08:15:53 And what you actually see in fazer is a really low rate of standard model particles.
08:15:58 So what's nice about phase two is it covers such a small, it's only 10 centimeters radius in the transverse plane so it covers a tiny fraction of the solid angle two times 10 to the minus 6% of the solid angle, but 2% of the pie zero is produced in the
08:16:12 galaxy collisions produced in the angular acceptance of faith and this is just because of the way that the collisions work you get a huge flux of standard model particles produced along the collision access.
08:16:23 the bottom here which is showing the angle which with pions are produced with respect to the beam line as a function of the energy of these pions, and you can see the face of acceptance which is shown here.
08:16:35 This is for one invest at Arbonne. So in the one three of the galaxy we expect 150 investments of bonds. And this means we expect about 10 to 15 pie zeros which are produced in the angular acceptance of phases detector.
08:16:49 And so even if you had a very rare decay of a Pi Zero into a dark photon or similar Dark Sector particle. So we're looking at punching fractions of order 10 to the minus 10, you would still get a substantial number of these particles which would go be
08:17:07 pointing towards fazer and could decay inside the phases detector. So another thing that you can notice from this plot at the bottom here is that the Pisces which are produced in the face of acceptance have very high energies, this is one TV of energy.
08:17:17 So this gives them a big boost and it means that the detector being 500 meters away from the interaction point.
08:17:22 Still have sensitivity to interesting lifetimes and couplings of these dark feet on so in this plot on the right here you can see the sensitivity for different luminosity values as a function of the mass of the dark feet on and it's coupling.
08:17:38 So the lifetime is increasing when you go down in coupling. And you can see even with one investment amount of data you get unique coverage in this case on premise space.
08:17:46 And with the full run three data set of 150 interest empty bones, you get quite a decent region of unique coverage from fazer.
08:17:55 So this is just a quick sketch of phases so the particles are coming in from the right here, they decay inside this decay volume which is inside a permanent magnet.
08:18:04 And then you have a tracking spectrometer, and the perimeter at the back.
08:18:08 And this can search for dark feet on signal, if the dark futon is now coming in from the left at the keys inside this first magnet into an E plus a minus pair.
08:18:16 These are separated by the magnetic field and track through the spectrometer and then leave their energy in the kilometer at the back of the detector.
08:18:23 What's the challenge here is that this photon that's coming in has a mass of about 100 MEV in a momentum of about a TV. So the E plus minus are really produced on top of each other, and the magnet is needed to separate the so that you can see them as
08:18:39 two separate particles inside the detector. So just to flush a few photos of the progress of phases so here you can see the perimeter and the tracking detector.
08:18:45 This is the magnet under construction. So phase, it was able to move very quickly because it uses spare parts from other experiments there's kind of limited modules from Alex Eb and the tracking silicon detectors are from Atlas.
08:18:57 And what you can see at the bottom right here is the phase of detector installed in this to 12 tunnel, which was the installation was completed in March, 2021.
08:19:05 And so Phase I went from an idea in a theorists paper in summer 2017 to an extort installed experiment. A few months ago. And all of this took about three and a half years so this is that that does demonstrate that these experiments can be implemented
08:19:18 fairly quickly, and when things go well.
08:19:23 quickly, and when things go well. Okay, there's an idea to extend fazer in the future to give it a bigger radius. So at the moment the radius of the text is only 10 centimeters by increasing this to one meter, you would significantly increased sensitivity
08:19:35 to new physics particles that could be produced in heavy needs on the key. So the decay of things like B and D Nissan's. This is because the end means on the more spread out with respect to the beam, when they're produced, as you can see in this block
08:19:47 here. And that means that new physics models which were the new physics particles coming the decay of these heavy Nissan's you get much better sensitivity.
08:19:56 If you have this bigger detector than this r equals 10 centimeter fazer. And so there's a possible future upgrade to fazer to try and increase the acceptance in this way.
08:20:07 Okay, so now moving to kind of the opposite of phases and this is a very big proposed detected called Methuselah. You can see a sketch of how this looks here so this is the CMS detector in the bottom here on the Galaxy beam line and Methuselah is a big
08:20:20 experiment that would be installed basically on the surface, it's actually dug into a trench which is 20 meters deep. and the whole detector is 29 meters high and hundred by 100 meters in the kind of transverse plane.
08:20:33 So it's a huge detector, and it covers about 5% of the solid angle. And the idea here is that you could get neutral Longley particles which would be produced in the interactions in CMS they would go through 60 meters or more of rock which acts as a shield.
08:20:45 And then they put the key inside the decay volume of Methuselah, and the tracks that they produce with NBC and by the detector.
08:20:53 So this is of course sensitive to particles were very long lifetimes, because of the large distance between the interaction point and the Methuselah detector.
08:21:03 So you can see him a sketch of different types of background that you would expect for these this type of experiment. So you can have new ones from the LSC which can then scatter you can have neutrinos interacting in the air in the decay volume of cosmic
08:21:15 rays or you can have neutrinos coming through the earth.
08:21:19 And people have studied this and by combining very precise timing and also position resolution of the measurements of these charged particles, you can reduce the background to a very low level of about one background event, per year.
08:21:31 The current idea for the detector is to use us inflatables with wavelength shifting fibers, a couple of to Silicon pm.
08:21:38 And so with each bar is five meters by four centimeters by two centimeters, where you read out at both ends and this gives the required resolution of about a centimeter in space and very good resolution sub nanosecond resolution in time.
08:21:52 The Methuselah team have produced this test and you can see here which has been put on the surface above Atlas and taking data while at the end he was running as this is 2.5 by 2.5 by 6.8 meters high.
08:22:04 And here they could measure them you're in flux, you can see here the angle of the new ones, and the orange here is new ones coming from the collisions, and the blue is in fact, new ones coming from cosmic rays which are bouncing off the ground and then
08:22:15 going upwards. And you can see that the data agrees fairly well with the expectation.
08:22:20 The way that the materials that could be realized is in this sketch here so this is 100 modules, each module is nine by nine meters in this plane, and about 29 meters high.
08:22:31 And it has tracking layers at the bottom, and then at the top with the decay volume in the middle.
08:22:35 This has about 700,000 channels and the idea is that the trigger could be combined with CMS blue, which could mean that you could use CMS as an active veto.
08:22:44 So when you see an event in Methuselah you could see if there was any big activity that was pointing in CMS towards with you so and you could veto on this if you wanted to reduce your backgrounds.
08:22:54 The problem with Miss Isa is because it's such a huge detector 100 meters by 100 meters, that you really have to minimize the cost of the detective components in order to keep the cost under control and that's something that is being studied at the moment.
08:23:07 You can see here the sensitivity for an interesting physics major This is a Higgs became too too long live particles as I mentioned, this is something you can only do it the LLC.
08:23:15 And here you can see the sensitivity as a function of the lifetime. And you can see that Methuselah has a significantly better sensitivity than the current best sensitivity from the LSD experiments which is from Atlas.
08:23:26 Here you gain about three orders orders of magnitude insensitivity and in lifetime so this is really a big improvement.
08:23:33 So, a new idea called a new base is a similar idea to Methuselah, but here the idea is to make the detective smaller by inserting it into the shaft, which is above Atlas, so this is the shaft which is used to lower down the components about this during
08:23:47 the construction. It's 18 meters in diameter and 56 six meters high. From the top of the cabin, to the surface. And by instrumentalists with tracking detectors, you would cover something like only 1% of the size of Methuselah, but still have a pretty
08:24:03 good sensitivity to new fit the similar new physics models, and again you could use Atlas as an active veto by looking activity in the ATLAS detector that's pointing in the direction of this newest detector.
08:24:16 When you see a signal signal like event inside the nucleus.
08:24:21 And here again you can see the sensitivity, it's a little bit worse than Methuselah but it's much smaller, of course, and the sensitivity picks up slightly shorter lifetimes, which is what you would expect since it's closer to, to the interaction point.
08:24:34 And here's another proposed experiment called Codex B which is in some sense a little bit in between Methuselah and phase so it sits in the seat This is plan to be situated in the LLC, an interaction points so it's about 25 meters from the interaction
08:24:49 point in LXEB, where there's a room which is currently full of the LGBT DAC system, and this is being moved to the surface. During the covenant shutdown of the legacy.
08:24:59 And so this room is being freed up and you could put along the particle detector here which is called Codex be here the idea would be a 10 times 10 times 10 meter detector.
08:25:09 And you would put an active and passive shielding between the IP, and this detector in order to reduce the Standard Model backgrounds.
08:25:17 Here, the concept is to use our PC detectors with very good timing resolution, in order to be able to see these neutral and normally particles became the standard model particles, and because this is so close to LA TV, it would be really integrated into
08:25:31 the Elite Series, out, in a way, such as another galaxy be detected which would give additional advantages.
08:25:37 So here at the top you can see the sensitivity, this again this is for a Higgs became too dark photons with different dark fetal masses and light one on the left and heavier one here, you can see the Codex be sensitivity compared to Atlas is much better.
08:25:51 It's not as strong as Methuselah and, and you can see that it can cover both light and heavy cases of these questions.
08:26:01 So the status of Codex be at the moment is that they tried proposing to install a small demonstrator in this location so 120 fifth of the final size of the detector, which would allow them to measure backgrounds and to test it detected technology and
08:26:14 the reconstruction.
08:26:16 And the idea would be to install this during 2022 and take data during part of the, the next Elysee run already they've measured background rates in this proposed location by installing some simulator based detectors and this plot you see here is looking
08:26:29 at the rate of hits in the simulators, as a function of the beam time in a, in a collision fill in LA cb. And what this shows actually is that the simulation is the results of fairly conservative with respect to the simulation so they see less backgrounds
08:26:45 and they were expecting which is encouraging for this type of detecting.
08:26:50 Okay. And the last detector I wanted to mention in a little bit of detail is Millie can, so this is a detective which is a bit different than the ones I said before because this isn't really looking for a neutral Long live particle which then decays instead
08:27:02 it's looking for a particle with a very low electric charge so electric charges in the range, sort of tend to the minus three to 10 to the minus one of the electric charge, and with masses in the range of 10 MEV to 10s of gv.
08:27:16 So such particles can be produced in models such as dark QED three processes which you see on the right here so it's kind of drill young production process where you can produce these many charged particles.
08:27:27 And you can see the cross sections which are used in these studies in this plot at the bottom as a function of the mass.
08:27:34 And here the detector is basically relies on simulator bars which are pointing at the interaction point. And when you have a really charged particle going through these inflatables it releases of course a very low amount of simulation light, and these
08:27:48 integration photons can be detected. And by having bars that are pointing at the IP you can control the backgrounds which mostly come from cosmic rays and the dark rate from the PMT.
08:27:59 And so this detector is being placed in an unused drainage gallery close to the CMS cabin so it's kind of above CMS about 33 meters from the interaction point.
08:28:09 And again shielded by 17 meters of rock so you can see in all of these cases there's a good shielding between the new detector, and where the particles are produced.
08:28:18 So here on the right you can see this is what the final mini can detect which is hoping to look like so it's made up of these. And since later bars with p amp t on them here there's three sets of simulator bars and their angle to point towards interaction
08:28:32 point in a detector that's final detectors one meter by meter by three meters.
08:28:38 And, in fact, the team installed a small demonstrator detector which you can see in the picture here, which is just made up of a few of these bars, 1% of the final detector.
08:28:48 This was installed for LHD running in 2018 and it was exposed to 35 investment tons of data. And this is really useful for understanding the backgrounds and how you would use this detector to do physics, but it was actually also able to make a physics
08:29:03 measurement. And you can see here, this is the sensitivity that you can see in terms of the charge of the particle and its mass. And this red line here is the result which came from this demonstrators it is 1% of mini cam that was installed in 2018.
08:29:19 You can see it does have some regions where it's the most sensitive results, compared to the existing limits, which are the other colored curves here.
08:29:27 And then what you can see in green here is the expected sensitivity for the detector which they would install for run three of the galaxy. And then also the final sensitivity in the green dash line, which they expect to be able to achieve with the full
08:29:41 home last year he did set of 3000 investment funds. So this is a nice improvement over the existing constraints.
08:29:50 So this slide just tries to compare and contrast the different proposals which I've mentioned in terms of where they are from the IP, the size that they are, and also then you can calculate the approximate solid angle that they cover which ranges from
08:30:03 times 10 to the minus 6% for phase two 5% for Methuselah which interaction point there in so most of them are in either Atlas or CMS interaction points which will both see 3000 investment bonds in the university LLC Codex be would only see 300 investment
08:30:19 bonds because the luminosity in LHEB, it's about a factor of 10 less than in the, the big experiments.
08:30:25 And here I show what kinds of new particles sensitive to. And I also was brave enough to sort of categorize how expensive these detectors are so I think fazer and many can have fairly cheap and probably cost of order one to 2 million.
08:30:40 I think phase two and codecs be a property in the border five to 10 million bracket and Methuselah. I've never heard a sort of real costing of this but for such a large detector hundred meters by 100 meters.
08:30:52 I imagined this isn't the many 10s of millions and type of area.
08:30:57 One thing I did want to mention is that all of these magnets except all of these experiments except Phase I don't have a magnet, and they just see this neutral particle that came to two charged particles.
08:31:09 And this means that they can't reconstruct the mass of the Long live particle in a reliable way and in some cases, this has been criticized as a weak point of these designs.
08:31:17 The reason there is of course that there's just not enough room to have him on, you can't build a magnet that would be able to see this in a good way.
08:31:25 Okay then I just want to very quickly change tack and mentioned neutrino detectors at the LHC so there's no neutrino detector installed at the LSC at the moment but when we were studying fazer for example we realized that will be a huge flux of standard
08:31:37 model neutrinos that will go along the line of sight, and could be detected with an appropriate detector so here you can see the number of neutrinos that would traverse fazer in one field the lacs I tend to the 11 electron neutrinos tend to the 12 noon
08:31:51 neutrinos and 10 to nine town neutrinos, and by sticking in 1.2 tons of tungsten, we would expect about 1000 electron electron neutrino interactions 20,000 your nutrient interactions and 20 Tower neutrino interactions.
08:32:05 So this is something that's quite interesting and in fact since then fazer has introduced a new sub detected to look for these types of interactions, which was approved in 2019, and there's a new experiment very recently approved called s&d, which is
08:32:19 again an experiment that will look for neutrino interactions, from the galaxy. So for phase that we put in a small emotion based detector which you can see here on the line of sight to the collisions in 2018 running and it was exposed to 12 investment
08:32:33 funds of data. And we've started to analyze this and we see some neutral vertices, you can see some event displays of here, which are likely to be the first neutrino candidates for neutrinos which have been produced in a Collider, the analysis is still
08:32:46 ongoing and these could also be neutral had one interactions.
08:32:49 So I wanted to just very briefly mention a very new idea, which is called the Ford physics facility which is kind of an extension of what phase two is trying to do.
08:32:59 So what we've seen when we studied phase two and phase of new is that there's a lot of interesting physics associated with this very forward region of the galaxy collision so when you're really follow the line of sight of the collisions.
08:33:09 Once the LLC Ben's away.
08:33:11 And at the moment the CERN civil engineering experts are looking at ways that you could do this so you can see in the bottom two ways, things that being considered when he's trying to widen what's called the junction Kevin of the LSC say at in this picture
08:33:29 are we more ambitious proposal was to dig a new cabin so here we would have to take a shaft down something like 80 meters and then a Kevin, which would begin beyond the line of sight of these collisions where we could put new experiments.
08:33:50 So just to give you an idea of what you could do in such a cabin so you could install the neutrino detector that would, if you had a 1010 neutrino detector.
08:33:58 For the full 3000 different bands of the holy meal hc this would expect to get a few thousand high energy town neutrino interactions. Remember there's only about a handful of town neutrino interactions that have ever been recorded.
08:34:10 And so with this you could discover the tower anti nuclear you know you could constrain the towel neutrino EDM and you could study town you tune your interactions with heavy flavor.
08:34:18 This is something that's pretty interesting. There's also an idea to put a liquid on TPC detector in this word physics facility which could have sensitivity to Dark Matter scattering where the dark matter is produced in the NFC collisions.
08:34:31 There's a plot here which shows that this is really quite interesting for probing the thermal relic region of the Dark Matter parameter space for a number of models and.
08:34:40 Another example is if you took the mini cam detector and just moved it to this Ford physics facility to be on the line of sight, you could significantly increase the sensitivity to many charged particles.
08:34:50 This is just by virtue of the location which has a where most of these many charged particles would go.
08:34:55 So this is something that's really quite interesting and it's been studied by stone at the moment.
08:35:00 So just to show.
08:35:12 This is this FPF this forward physics facility. This is a number of theoretical benchmarks which are produced by the physics beyond colliders group at CERN, and the Ford physics facility would have sensitivity to all of these types of model with phase
08:35:17 two, and this liquid argon TPC, and this Ford really charged particle detector.
08:35:23 So that brings me to the end so I hope I prepared presented to you a few proposals for new fire detectors at the LSC fazer Methuselah Codex be and Mindy can.
08:35:34 Unfortunately that I didn't have time to mention everything is a couple more which I threw in the backup.
08:35:39 I think these new detectors are theoretically were made tweeted and they could really be good value for money to increase the physics reach of the LSC, as well as the bsm, and especially dogs acted on the political searches that I talked about these new
08:35:51 new experiments targeting neutrinos producing the galaxy, something quite new. And to date no neutrino produced a collider has ever been detected so this really could open up a new regime in Newtonian physics and neutrinos produced at the link to an unexplored
08:36:05 high energy regime which could make them particularly interesting.
08:36:08 And so this forward physics facility I mentioned is a very recent idea which could allow multiple new experiments to increase sensitivity in several important areas.
08:36:17 And just I leave it there but I leave some references here, I hope I'll be able to post the slides so people can look at these, and if they want to know more.
08:36:28 Oh yes.
08:36:28 Okay, so that's what I had thanks. Oh, thank you for that, inspiring talk, I learned a lot. I'm an outsider but I had no idea these things were going on.
08:36:37 Let's see, I'm sure there will be questions and comments. Let's try raising hands at first and see if that's necessary. So please raise your hand.
08:36:54 while people are doing that, I have a naive question.
08:36:59 How do you suppress the neutrino background in most of the detectors that you described.
08:37:04 Well this is a good question. So, I mean, normally we don't really ever consider neutrino backgrounds in collider physics, this is something which we don't think is normally important and I think fazer is in fact the only because of the location of phase
08:37:32 So our magnets in fazer are filled with air, and there is of course a chance that you can have an interaction of a neutrino in the air, probably there's more chance that you can have an interaction in the simulators which we have.
08:37:35 which is really on this collision axis, this is where the neutrino been in a way it goes. And so, of course, it's hard to suppress but the main thing is to have little material inside your detective volume.
08:37:42 And we, we believe we would be able to control this using the the tracking detectors to see where the activity is coming from.
08:37:48 In fazer we have a calorie meter maid of lead 100 kilos of lead, and we do expect about avoided 1015 neutrino interactions inside the color emitter, which will be something that we need to understand how to suppress.
08:38:02 So, but it to my knowledge that's the first time that a neutrino background is really significant in a collider based experiment so it's kind of a new regime in a way.
08:38:11 Yes.
08:38:16 Okay, Lance.
08:38:18 And how about neutron background.
08:38:22 Yeah, so, neutron backgrounds. I mean the general philosophy, I mean, in fazer for example we have.
08:38:39 So we have a simulator in front of the detector which will take the Milan and studies have shown that basically if you get a new one coming into phase, it will always be associated with this new one.
08:38:47 So we the particles go through hundred meters of rock, and we have high energy new one so any background is effectively associated with these high energy neon beam.
08:38:52 So by vetoing events where we see me on entering the detector. We will also be two events where additional activity associated with the new one is also entering the detector.
08:39:01 So neutrons run the primary interaction point or either thermal eyes by the time they get there, they're just not really a big problem. Yeah, I mean to any of these detectors.
08:39:12 Yeah, well I can I'm a put my cards on the table I work on fazer, and so I can speak strongly for fazer for other detectors This is of course being considered.
08:39:22 But this is what I was trying to mention at the beginning that generally you have a lot of shielding so you have 10s of meters of rock between the interaction point, and your detector.
08:39:33 I think this is suppressing the background thanks primary particles.
08:39:38 Good Stefania.
08:39:41 Okay, hi.
08:40:02 so
08:40:02 yeah so the primary idea for phase and used to measure the nutrient cross section for the three flavors of neutrino in a unprecedented energy regime so this figure here is showing projections of the sensitivity for the cross section so this is the electron
08:40:19 neutrinos the neon neutrino in the town neutrino as a function of energy. And you can see for the electron neutrino so in phase we go up to two above a TV, whereas measurements are basically below 100 GV so we're looking at a really new regime, from your
08:40:34 neutrinos The, the cross section can be measured again between sort of hundred and thousand gv here there is actually measurements from Ice Cube at their multi TV level.
08:40:45 So here they are measurement should be able to sort of fill the gap between accelerator base between a measurements and ice cube and Fatone neutrinos, we expect this relatively large uncertainties but we expect to order 10 interactions.
08:40:58 So there'll be large uncertainties but again this will be unprecedented energies.
08:41:03 I did also include a slide. So this is what s&d which has this kind of rifle experiment to phase A new it situated in and basically the same place as fazer but on the other side of the Atlas interaction points a 500 meters and also close to the collision
08:41:18 access it's slightly offset from the collision axis.
08:41:21 The physics mutations they give s&d is to measure the cross section similar to fazer but also to constrain the glue on PDF at low x. So, this is by measuring electron neutrino interactions in the detector which is basically in their Angular space is coming
08:41:36 from Chandra K. And so somehow this allows you to constrain the glue on PDF.
08:41:41 They also want to try and measure electron flavor universality and neutrino interactions and to measure the ratio of neutral to charge current interactions insights neutrino interactions in that detector.
08:41:52 I think phase and you can probably also do some of these things, although. Yeah, I think maybe s&d are a bit more aggressive in what they claim they can do.
08:42:03 Okay, thank you. So maybe you're measuring more than production than you are the, the cross section.
08:42:15 Yes, that the cross sections are theoretically better understood than the, the small x production. This is a very good point. So in fact, we measure something which has in it the production and the cross section and we can kind of choose what we claim we
08:42:23 we measuring and what we had long discussions on they say what we might be able to do is use cross section measurements which overlapping energy with existing cross section measurements to constrain the production, and then use this to extrapolate into
08:42:37 the new energy which in but you're completely correct, but you probably also extrapolating in the production at the same time. Right.
08:42:45 stuff and it does it folds into kickboard QCD. And in fact, interestingly, there's a huge interest from ice cube to for these types of measurements because they can constrain very forward proton charm and interactions which are somehow super relevant
08:43:01 for ice cube in a way that I haven't completely understood but this is there is quite some interesting stuff here So, but you're right for there's definitely there is great to see the overlap with ice cube to.
08:43:12 Yeah, totally different facility.
08:43:13 Yeah. Yeah, exactly. So, it's very interesting actually since we made these plots, we now hope to be able to link the phase A new emotion based detector to the spectrometer in fazer with the new tracking detector, which would allow us to take the charge
08:43:28 of the new one. And so when we made this plot we were looking at the average cross section of neon and anti neon neutrino, but now we hope we would be able to make these two measurements separately by being able to measure the charge of the neon produced
08:43:40 in the interaction so that's a I don't know we have to study if we can really do this but this would allow us to make separate measurements of the neutrino and underneath you know, just for the moon.
08:43:54 Anybody else.
08:43:59 I feel free to speak up if you have any last minute questions here.
08:44:08 I do have another naive question, Jamie.
08:44:11 If you discovered any of these particles, turning up in any of these experiments of course it would be a revolution.
08:44:18 If you discovered a millet charged particle.
08:44:21 That would really upset this whole theoretical apple cart, I think, you know, no more engaged theories, perhaps.
08:44:29 So, what interest and even push back to you get from theorist on the subject of well you'll never find one of those.
08:44:37 Second question I have to say I'm not super expert in this stuff but I think I've seen this mentioned in the, in the context of what they called q CD.
08:45:04 And, which is like these Dark Sector type models. And so I'm not sure exactly how I mean it's for sure revolutionary of course but I'm not sure it's completely something that people push back as being totally impossible to happen. And, but maybe I take
08:45:06 advantage of your question just highlight this point, I mentioned about the magnetic field because when you said if we discover anything, then it would of course be a revolution and that's true.
08:45:16 And I think there is a little bit of doubt about these types of experiments, because you can't measure the mass of the longest popsicle that's being produced.
08:45:25 So, most of these experiments they're looking for nothing coming in. And then you see two particles which point to a common decay vertex, what we call a displace vertex.
08:45:33 And of course what we would like to be able to do is measure the momentum of these two particles such that we could vertex them together and say the parent particle had a certain math, yes I do that and we saw a number of events and they all come from
08:45:56 Yes, one of the limitations of these experiments, is that they can't do that. And I believe if they did see a signal, probably the next step would be to build an experiment that would be able to tell you the mass, and this would probably be needed to
08:46:04 really clear what people could really claim as a robust result. So I don't want to put too much with them from these things but in my mind this is a little bit a weak point.
08:46:16 And of course, the reason is clear because these experiments are big and it's hard to fill a big space with the magnetic field in a, in a reasonable way so that's the issue.
08:46:24 Actually in phase that we do have a magnetic field but I think we still suffer from the same problem because the particles coming in is so high momentum that we don't get sufficient bending, to be able to really measure with a good resume.
08:46:39 Anything else.
08:46:41 So I don't think discovering Millie charged particles necessarily overthrows gauge theory I think it suggests that there is a light, a master list, dark photon, that has some kinetic mixing with our photon, and then things that have a sort of normal charged
08:46:57 under the dark gauge sector can look like they have a small charge under our. Pull it it's just a small mixing angle okay my own a kinetic mixing so you are you can understand it if you have particles heavy particles that are charged under both you draw
08:47:13 one loop graph that turns one photon into another through by coupling to both the pieces right against Molly mixing tank Yeah.
08:47:22 Okay, well, Jamie thanks very much for a great talk, please do up your load your slides and other speakers up your load your slides to.
08:47:39 Yeah, there's also lots of backup sites but I didn't for me it wasn't obvious I'll just send you an email to figure out how to do it offline. Okay, okay, that's fine.
08:47:41 Okay, thanks. Thanks.