 So the next speaker will be Yahya Tayyadati. He's from Morocco in Rabat University and also based at CERN currently. So it'll be more of an experimental talk as you can see on your side and so please start Yahya. Hello, do you hear me? Yes, we hear you. Excellent. So good afternoon everybody. I'm Yahya Tayyadati from the University of Muhammad 5 in Rabat. Please allow me to thank first the organizer and Professor Ali Hassan Ali who gives me this opportunity to present some of our activity in this African Physics Society meeting. So this is the outline of my talk. I will first present one of our recent activity with the atlas collaboration which concerned the search of light by light scattering. After that I will move to the some of our recent activity on astro particle side with the entire collaborations and the search for exotic physics, exotic particles with neutrino telescope. And before to conclude I will also discuss some of the hardware projects we initiated recently in Morocco for both high energy physics and astro particles. So with our group I'm talking on behalf of these people. I'm supervising five PhD students Hassan Al-Jerari who is based at CERN in Geneva leading the activity of search of dark matter in the Higgs ZDK. Hassan Hamdawi almost done with his PhD and he was involved on heavy ion physics. On the bottom we have Jihad on astro particle side. He is working on monopoles with Antares telescope and leading the hardware activity in Rabat. About a year ago we have been joined by Miriam and Ahmed working for Kaimtrinet telescope. Miriam is studying the efficiency of detection of supernova and the demo we will continue with the search of mining in the monopole on the Kaimtrinet telescope. So as you can see we are trying to I try to do our best in order to respect the balance gender. So let's start now with the health activities as you know the light by light scattering is processed which is completely forbidden in classical electrodynamics but it appears in quantum electrodynamics in this diagram with loops with a contribution from quark and and lepton at low energy while we have W boson would dominate the contribution at high at high energy but this process is extremely rare you can see the cross section is proportional to alpha fourth alpha is the fine constant structure which which make it extremely difficult to detect there were many devices proposed to to probe this process but without success but when colliding when considering ultra peripheral collision of the ions the cross section gets in hand since the electromagnetic since the the due to the dependency of the electromagnetic field on the charge of collided ions so which give an opportunity to to observe this for example at the LHC so a very simple topology of the signal you have two scattered for them and the final state the the heavy ions escape the collision with possibility of excitation in the final state at the detection level we will have only the activity of the photons at the level of the calorimeter while the rest of the detection will will behave silent with no activity what what make this since professor Khalil Shaban has discussed dark matter and so on what make this process interesting is not only to probe for a process which is predicted by stonder model but these photons could couple to any new particle and we have here a clean way to probe new physics beyond the stonder model okay in fact atlas has already presented using data from 2015 ultra peripheral collision of lead lead at five at five dev the equivalent of luminosity of 0.48 nano barn inverse they have already provided the first evidence for for the light by light scattering you can see here the basic selections and they they have observed 13 event when we were expecting glee on events being at that time as the first evidence 4.4 sigma for this for this challenging process we our group in rabat has participated to the new analysis which turned the the data from run to sorry data of 2018 we have three more ultra peripheral collision data from lead lead collision at five dev with major improvement as you can see here in term of the trigger efficiency and the identification of photon which is now based on neural network technique and with better rejection of the background on the top you have the trigger efficiency for the old analysis compared to the new one in the bottom one can see that we have the major improvement here especially at low energy you can see that we we reach already the 60 percent of efficiency at about the 5 gv okay this is the sample we use super sheen in order to simulate the signal we have two major background the one the first one is the exclusive the electron production gamma gamma two pair of electrons they were simulated with star light and we have simulated the contribution and the central explosive production photon from gluon with super sheen all the other background coming from electronic noise and from cosmic and so on are negligible and we're not considered in in this analysis so here's some forces on the left you can see the photon reconstruction efficiency which has been derived from gamma gamma to electron positron which is a background for this study but is also used to to calibrate for calibration and so on photons here comes from bremstra long we consider event gamma gamma two ee when one electron emit hard bremstra long radiation due to the interaction with the matter on the right side you can see the the performance in term of the identification of which is uh pension early based on shower shape variable and neural network technique we are using here photon background photons derived from data and also we compute we train the the we train the soft on the Monte Carlo samples so here I present the cut flow basically we require two photon each one with at least three gv this card it's on order to separate prompt photon from fake photon from cosmic and and and so on and from the electronic noise also which which have low energy we are exclude the transition zone of the calorimeter is also exclude for that reason and on the bottom you can see we require no activity especially no reconstructed of any charged particle and we have one of one efficient cut on the aqua planarity which reduce the central exclusive production and the contribution which come from glue one okay so here the new result using data from 2018 as you can see uh represented here in term of the aqua planarity on the left and in fact as interpreted also in in mass invariant mass of the two photons represented here for the the background and from gamma gamma in two pair of electron in blue and for the central exclusive production of photons from gluon and the expected signal in red and the data with the black dots at last reported 59 event this time where we were expecting only two event from the background this has been interpreted as an observation at eight sigma of the light by light scattering similar result has been also presented by by cms we have also measured the cross section of this process and you can see the value observed are close to uh withening of course the error are close to what is expected in theories okay so let's move now to uh before to go to as for particle physics let me show you one of the event this is the most energetic event we have atlas has registered as you can see we have just back to back scattered photon and no activity in the rest of the of the data i will skip this but the data from 2015 and 2018 has been combined in order to proper for new physics here we considering the possible coupling of the two photon to action like particle which are good candidate for dark matter we have computed atlas has computed the limit upper limit on the cross section and the coupling and you can see on the right with this with data with the combined data from 2015 and 2018 similar analysis compared to the light by light scattering we are pushed here on bottom in blue atlas has pushed the exclusion to a new a new best limit so this is important as halil mentioned when we are searching for new physics beyond the standard model okay let's start with some recent activity on astro particles as you probably know morocco has joined the antarisk collaboration since 2011 when first with the university mohammed one in wujda where i got my first position at that time and later on by uh also my actual university university mohammed five robot has uh has has joined and we managed to transform morocco in cluster which include also our national center of nuclear technique nester in rabat and also the university of of marrakech uh since this is a schematic view of the uh antastelescope so the collaboration managed to deploy successfully uh and since 2008 uh 12 lines each one about 400 meter containing 25 floor and each floor contained three optical module which will detect the sharing of light emitted by millions from induced by by neutrinos in rabat we took the all the responsibility concerned the search of exotic particles the first analysis i will present here concerned the search of magnetic molecules so this analysis relies on two parameters on the on the right we have the brightness of the of the event in green you can see that monopole emit more light compared to what we get from muons represented here in red or what we get from the from neutrino in blue here also comparison to that are represented with the black dots the second you can look at the end here as the number of fired fired optical modules on the left we have a second important variable which is just uh the reconstructed quality uh weighted with the brightness of the event and we have here the number of parameter fitted in order to uh to find the track of uh of the monopoles represented of course here with green for fast monopole blue for neutrino and atmospheric muons in red compared to what we get in data so we we the optimized parameters one can as you can see here one can isolate monopoles from atmospheric million than neutrinos we need to optimize a cut on the brightness of in the event which is represented here in function of the quality of reconstruction of the of the of monopoles this is work quite fine for fast monopole for slow monopole we have an extra cut on the velocity which is reconstructed and should be for slow monopole different from the still flight for millions and neutrinos so we have presented in the last neutrino 2020 meeting a new update for the sensitivity for magnetic monopoles you can see what we get with about with data up to two thousand the equivalent of two thousand four hundred eighty days of data taking here in red it's you can see that exploring the optical property of water we are providing a better and competitive up limits on magnetic monopoles sensitivity I should mention that we have also using about one the equivalent of one thousand twelve days data we have published also a result here in red which was at that time competitive for of the limits from ice cube at at high velocity and fast monopoles so a second it's a performed collaboration with guys put the PhD students in university at university of ujda supervised by my colleague musab illa I remind you that nuclei it was being it's stable part to lose quarter good on the day or so for the light also on two volumes we have on the right the brightness like the part of the event represented for nuclear with different energy in red major and green uh 40 you mass for 10 to 14 gv up to 10 to 16 ev we have more light compared to what we get from atmospheric millions in blue and uh black solid line correspond to me the measured data we uh this is the first variable and the second one is profit from the fact that nuclear right transit the telescope in quite long duration it take like about 200 milliseconds for a nuclear to transit in the telescope compared to a blue line here for the transit time for millions is about two microseconds so we have these two key variable for this analysis but one can see that by optimizing a cut on the brightness and the the time of transit of nuclear rights in the telescope one can perfectly isolate nuclear rights from from atmospheric million represented here in blue this optimization has been done following the Feldman Cousin approach and we have provided new sensitivity you can see we here in red which has been presented in the last conference neutrino 2020 and you can see we push forward the limit compared here to what we get for example from macro macro experiment before to conclude i i think i have a two two minutes to present some hardware activity morocco has joined recently the kaim 3 net collaboration which aim to build new generation of neutrino telescope similar to antares but at big scale we are talking about kilometer network telescope in fact we have two sides one close to orca one close to france and the other one to italy orca is dedicated to low energy activity while orca will will deal with high energy neutrinos so quite promising physics this is the program and what is expected from kaim 3 net low energy will study the neutrino oscillation the problem of hierarchy and so on and orca will will study the the source of cosmic rays and and so on we have some exotic activity in medium energy okay so we have convinced the collaboration uh to build uh to set up a dom sign integration site which will be uh dedicated to the production of digital optical module for this telescope it's really uh here you can see the the lab is now well furnished and you can see on the bottom left the our test bench completely set up with our phd student so this project will bring uh some high-level training for our students and will give more visibility to morocco and it's kind of uh it works trans uh technology transfer to to our country uh another site will be uh has been approved by the collaboration and will be installed to the university of ujda it will be dedicated to the integration of base module you can look at base module like a router which will collect uh optical signal from four lines of the detection very nice activity again will ensure the good training high-level training for phd student and uh knowledge transfer to to to our country uh on her side after a long discussion with management board of atlas discussion initiated by my colleague rashid mazini from academy kassinika myself we convene the collaboration to approve a project which will involve in elegant way the participation of morocco to the upgrade so since couple of weeks morocco uh represented by masir its technological foundation we have in rabat has joined the atlas collaboration as associate institute and we will participate to the constructions and the assembly of the high granularity timing detection uh this is one of the major upgrade of atlas since they want to uh will the 4d detection providing information opposition and also on on timing the it's explore the you know this elgad low gain avalanche detection technique and the the goals is to reach a resolution of about 30 picosecond in time okay this uh technological and 60 percent which is extremely important 60 percent of this high granularity timing detection will be produced in morocco since morocco has been chosen as six sites for this uh for the assembly of uh this uh nice and and challenging the device okay so i reached my conclusion to say that we are active in uh in both high energy physics and astro particles for high energy physics i didn't have time i i just presented our activity our activities in with the hivions groups we we we have observed we participated to the observation of light by light scattering so the lhc worked perfectly as a collider of photons and we we are also very active on the astro particle side with antares collaboration and the search for exotic particle like magnetic monopoles and nuclearite and we have initiated some hardware project in morocco which will give more visibility to our country and we we we will ensure of course high level training of our ut and i hope via morocco also we can share these expertise with other african country thanks a lot thank you very much for for such a comprehensive talk you're here uh and for sticking to time do we have any quick questions from the audience i don't see any questions in the text but maybe somebody uh maybe okay hasan please go ahead Ali so thank you thank you yeah here so you know i'm not a high energy physicist so um but i just wanted to ask you uh do you have any uh do you already have some contact with the people at ictp? yes we are in contact with booby akaria for example and yeah and i should mention that ictp supports also some of our students yes i am the director of a group it's a kind of affiliated center to the ictp yes okay okay that's not right so i just want i guess yeah so one of one of the reasons why it was very nice for you to be here is also for the other people in the african community to see what's what's going on and and to try to build some some networks and collaborations so uh so yeah thank you very good um another question when is uh and taurus expected to start taking data and taurus was running since 2008 and uh it's still it started in 2008 and still running yeah so what i presented it was i think you mean k3 net uh i guess the new generation of telescope yeah for k3 net we we managed to deploy a few lines we have six lines in the orca we started to taking data okay but the goal is to have a complete uh detection unit about which is 115 lines for orca for example and for arca we will have two detection units each with 115 lines okay very good um i don't see any more questions from the audience so just one quick question so my question is about the magnetic monopoles what's the prospects for detection of magnetic monopoles and then what will this mean for charge quantization i mean as i showed what we have we didn't find the magnetic monopole you can see here we just uh this is our last real result you see in green we have just set an upper limit on the magnetic monopole flux yes okay so we're almost certain it doesn't exist yeah i could not say that maybe the flux is less than this experimental limit okay okay so i guess we can stop here thank you very much i have also a question please um i'll i'll leave it to have a question should we stop here i think i think you can go ahead and ask it's fine okay that will be the last question of the session thanks okay okay uh please is there any way to get the light by light startering theoretically regarding the femur diagram i didn't get exactly what you mean like what's there if there is another possibility to to get the light by light scattering another way up to now yeah regarding the femur diagram yeah up to now you can see here the cross section is very weak due to the cathode fourth there were many devices based on laser and so on and for the moment the only way is with colliding heavy ions okay thank you so much because in order to enhance these cross sections okay so thank you so much so when uh how long do you expect we will observe those magnetic monopoles perhaps it could solve the problem of losing masses of universe it's it's like the question before i think i cannot answer it depends you know okay i i think what we are doing in antares uh and i think with the huge telescope like i'm treating it we will have more sensitivity and we can definitively decide on the existence of monopole form but right now with small antares telescope it's almost impossible has an alip just allow me to to to add one thing we we are in discussion with senegal a discussion with senegal in order to join antares k etrinat and atlas we have also uh we made contact with with university and we concretize an adhesion of which to to k etrinat and we are willing to discuss with any other country and help them in order to be involved in this international efforts i will be very happy if if we can help at that level okay thank you thank you very much um okay so i think we have to close this session to an end it's been a very busy day uh thank you shoaib and marcello uh for chairing this last session uh thank you to all the speakers and thank you all we'll see you tomorrow morning at 10 a.m for the poster session of course virtually so have a very good evening and thank you thanks bye bye thank you