 Thank you. Okay. Yes, it's working. So I also would like to thank the organizer for the invitation to talk here It's always a pleasure to be back in Trieste and I will talk about gravitino and decaying dark matter at LHC In this work based on collaboration with many people you see them written here George Arcadi Federico Dradi Marco Nardecchia Alexandra Albrey Marco Battaglia Jastor hasn't come and And So I will try to cover everything it's a little bit well a lot of material we'll see how much I Get through so I will start to give us a few short introduction trying to convince you that Apart from the wind mechanism There is also other mechanism which can produce the dark matter in the right abundance and they can give you also Rise of two in interinterinteresting ferruminology and then I will go and discuss two scenarios of this kind One is connected to the gravitino the gravity of course has a kind of well a very interesting and very special role in theories with supersymmetry since it is the gauge fermion of Supergravity and it is in some sense a particle which has also characteristic which are just determined by the symmetry and So it is in some sense one I think of the supersymmetric particle, which is really very interesting to explore And I will discuss here different scenarios of gravity in a dark matter and their phenomenology at the LHC in Particular in the case of a stop and LSP what happens instead if you have a neutrality no NLSP in the PM SSM And then if I have time a short connection to the case of biogenesis in the case of gravity in a dark matter And then in the last part I will instead move to a scenario, which is not supersymmetric But and it's a very simple scenario which we wrote down in some sense to try to capture the basic ingredients of these Connection of thimp and superwimp without having a full model if you want to full ultraviolet Complete model the characteristic of this model is that you have very minimal set of parameters And you can nevertheless also explain the dark matter density and have also interesting phenomenon Okay, so let me start with this introduction and try to convince you indeed that we have actually something more interesting or as At least as interesting as the wind to study And this is practically the idea of the superwimp or the fimp paradigms And the idea here is in some sense to try to produce the dark matter not from thermal equilibrium But from a particle which used to be or was in thermal equilibrium so the classical picture is that you have a wimp and The simplest scenarios are where you just add a small decay channel of the wimp into some other particle And the wimp of course can decay into this particle where while it is still in equilibrium So in this period and at the same time it will decay then eventually after it freezes out and In these two very different epochs it will at the same time produce the particle the daughter particle in the decay and These mechanisms are usually called fimp in this equilibrium regime and superwimp in the final regime Notice that in this case these two mechanism in some sense are both present if you have a particular decay channel and the characteristic to be in some sense very Well they are effective especially if you have very small couplings so that the decay time is actually very long And we will see therefore also later that this is usually connected to a particle with a long lifetime Now what which one of these two mechanism actually dominates in the production of dark matter depends on the parameters here for example We are changing the mass of the Heavy field which decays and this as you see depending on the mass you could have either the Superwimp contribution dominating other than or the fimp contribution dominating and in some sense both of them can actually Give rise to the right density to have a dark matter The right relic density for dark matter So and as I said they are actually connected always they can be connected to the same coupling and therefore They are in some sense usually present at the same time in a particular model Now what does that this have as consequences for phenomenology? well, of course he has a Well it changes in some sense the WIMP connection that we are usually used to to something like a fimp or super WIMP connection So in that sense there you would have still these early universe production from a WIMP in some sense with this leakage into dark matter That's I just talked about But at the same time you cannot use the similar diagram to get phenomenology at colliders or in indirect detection at colliders again, you can produce these Modern particle these which I call here WIMP and these as I said will actually result usually to have a long lifetime and therefore Bring about this place vertices or even metastable particle at the LHC that you could try to measure and to disentangle What is this decay length? On the other hand the dark matter in this scenarios is coupling very very weakly because this is actually very very slow decay And therefore in general you don't really need a symmetry to make the dark matter stable You usually have naturally dark matter particles with lifetime which are much longer than the age of the universe Actually, we will see later. We have lifetimes of the order of 10 to the 28 seconds And this means that well if you are lucky the dark matter particle could decay Actually now in our galaxy and you could be able to observe the decay product of the dark matter decay and these in some sense will also give you another information on of the dark matter couplings to the visible sector and In the simplifying model, I will talk at the end It's actually these couplings are related and therefore you can really also cross-check and in some sense try to measure all the parameters of the model Now these the decaying dark matter is actually more general So here is just the my usual plot to show you what is the flux that you would expect from a decaying dark matter candidate This is of course proportional to the density instead of the density square and the decay rate depends of course on the On the lifetime of the particle notice here the again the spectrum the spectrum in some sense It can be the same spectrum you would expect also for annihilation And in particular you could also have lines and we will get perhaps to that at the end And if you have lines that the advantage of course is that it's a very Smoking-gun signature on one point and secondly the position of the line will tell you immediately. What is the mass of the dark matter? So let me go now to the case of the gravity, no The gravity, no, of course has a long history and it has been studied in cosmology since many many many years and The usual thing is actually that is very famous is the so-called gravity no problem and the gravity no problem Well, I will actually talk to it in the next slide But the point is that usually the gravity knows if it is not stable It is very long-lived and this can cause troubles in cosmology but assuming it is stable the densities of gravity knows can be set both by Equilibrium computation so in the case of the equilibrium density you get that the Gravitino couples are usually very weakly and the couples when it is still relativistic so that it has actually the right Density at the corresponding to masses which are very small and therefore It's usually a warm or even hot dark matter which is now more or less excluded and this one was discussed in the 80s already It was actually I think the first supersymmetric dark matter candidate discussed and Of course, so so this scenario is actually nowadays not the best scenario from structure formation And therefore we will concentrate on the second scenario where you have the gravity knows never intermolecule equilibrium But you produce them slowly both through this film and super wheel mechanism I discussed above before but actually in the case of the gravity no you also have dimension 5 Scatterings which gives you also contribution which is proportional to the heat temperature and depending on the height How large the heat temperature is this is actually very often the dominant contribution if you see here This is for example in this case the one part of the contribution is coming from the gay genus So here you have a dependence on the gay genome masses square and inversely proportional to the gravity no mass And this will be important later on in the in the discussion So in through this production you see that if you have reheating temperatures sufficiently large You can produce in some sense the right number densities for masses of the super partners in the GV TV range Now the problems I was talking about is actually here It's the the fact that if the gravity no it's not stable or not very very long-lived as we will discuss later If you just it is not the LSP Then it can decay into other supersymmetric particles with a lifetime which is long It is in it is of the order of 10 to the 7 seconds for example, but not long enough so 10 to the 7 seconds is actually after nucleosynthesis and well, it's approximately one year if you want to translate that and if you have a Large population of gravity no decaying after nucleosynthesis. This can actually destroy the abundances of light elements and then destroy the predictions of nucleosynthesis and From this plot you can see some of the limits you can pose in the scenario Depending in this case again on the reheating temperature exactly because the density is here assumed to be proportional to the reheating temperature And you it turns out that if you want to be completely safe You have to really have a very heavy gravity no above something like 40 TV or Otherwise you have to live with a small reheat temperature of the order of 10 to the 5 or lower So in that sense these changes if you want the cosmology the presence of gravity no which is not the LSP In the scenario I was discussed instead that will take the gravity no to be the LSP and I will then have the limits on BB and not on the LSP which is in some as either stable or Sufficiently stable not to decay during nucleosynthesis But on the NLSP and these NLSP will be in this case for example in the first study actually the stop We will take the stop as the NLSP for two reasons one of course It is the fact that you have naturally a very low density of stops in the early universe because it's a particle Which interacts strongly and therefore you are hoping that the limits on BB and nucleosynthesis are actually weaker because you Have a low density on the other hand You have also you probably all know for naturality reasons a light stop. It's actually preferred by the To in order to have a light Hicks. So in this case, of course It will be the lightest stop there. The other one can be much heavier now in this scenario we have looked at the BBN constraints and There are still a region which is excluded by BBN also for the case of stop Even if the density is very low you have actually bounced state effects which cause actually a change in the abundance of light elements And therefore you see the regions here above is actually excluded because the lifetime of the stop would be too long It's after the order 100 seconds or so on the other hand if you want to have the right density of Gravitinos you have actually to be more or less on this line depending on the reheat temperature So in this plot I'm taking something like 10 to the 7 GB And you see therefore that you have just the white region where if you are on the yellow line You are exactly at the right density and in the white region. You would be below the density But of course changing the heat temperature You can move the yellow line about in this plane and of course lower heat temperature would move the line down And allow you to have also lower gravity no masses, which are in the other axis But in general at a certain point this yellow line will cross in the in the practically Red region here and this one is actually telling you the Maximum reheat temperature you can actually have and this is plotted here as you see you are in the range of 10 to the 7 Gv also before you are really hit the BBN constraints or so for a stop NLSP Notice that these bounds are actually avoided if you just switch on a small Variation of our parity and this is also the other scenario we will discuss This was observed a few years ago So if you have a small evaluation of our parity actually in the concrete couplings in the region between 10 to the minus 12 and 10 to the Minus 6 you are actually in a region which cosmological is very favorable Because on one hand you can avoid that this BBN constraints because the NLSP decays before Nucleosynthesis on the other hand if the coupling is sufficiently small you don't Practically increase the washout processes which would for example erase the leptone number or the barion number depending on which is the in some sense the mechanism you choose for Biogenesis if you do it of course at a higher temperature and you have still washout processes active you would actually erase This barion asymmetry So you see that you have small couplings, but not incredibly small and in this case Of course you would have that the NLSP would not decay into the Gravitino, but would decay preferentially through our parity violation So well of course if you have a decay at our parity breaking and not only the NLSP decays But also the Gravitino decays But luckily the decay is suppressed by the small our parity violating coupling and by the Planck's K And therefore actually you get very very long lifetime and there are already bounds in particularly from antiproton Which I'm showing here This is one of the recent bounds But given by the Lahaya and Grafe a couple of years ago from the antiprotons And you see that this is the bound which constraints actually these are parity violating parameter to be of the order of 10 to the Minus 9 or so at lower masses here's a large Gravitino mass at lower masses the Fermi constraints take over and They are of the similar order of magnitude. So this means again that these are parity violating parameter has to be small Okay, so in general then we have to study the two scenarios. We can actually study two scenarios at the same time one scenario where you have conservation of our parity and then this NLSP would decay in Gravitino and top and You see here the lifetime. It is quite long 19 seconds for this Parameter chosen But of course, we have also the other choice to have a small our parity violation in this case the decay of the Of the stop will be in bottom and charge left on and the DDK is a little bit smaller So that the if you want the lifetime is a bit shorter But not very short 10 to the minus 4 for collider purposes is actually very long lifetime And this means that in both these cases you actually expect to not prompt decay and either this place vertices Or even metastable particles in particular in the our party conserving more metastable particle And this means that the usual searches which has been done apart from the metastable particle search Which has been already performed do not really apply. So you have to do a dedicated analysis and And this is for example, just the picture what we did with the Federico Dradi was to try really to see where does this stop Decay once you produce it at the LHC So we generated the events with mad graph and we actually simulated also the decay and the decay length And as you see you can actually have depending on the lifetime the case all are in your Possible places in your detector In particular, we will concentrate to look what happens if when the decay are in the pixel or in the tracker Because there we can see the tracks more easily and in some sense you would see that there is a kink in the track or even a vertex And the other thing we will also consider is the case where the decay happens really outside to the detector And then in this case of course a stop which is a charge object could actually add on ice into a charge Hadron And leave a track through the whole detector. So this is also case where you could see something and And what we did here is to explore in the parameter space exactly what is the region which is accessible by the LHC searches And here is this plot we are plotting just the mass of the stop and the lifetime of the stop So these plots actually apply to any scenario so at the moment we are not specifying what is the decay channel and You see exactly we are requiring practically that the sufficient number of events Decay events either in the pixel the tracker or how many at least some events outside the detector And as you see here in the green line actually gives you the curve which corresponds to 10 decays outside So above the green line you have more than 10 decay inside the detector Sorry outside the detector instead of the red and the blue line correspond to to tracker and pixel respectively and Below the line you will have more than 10 decay events either in the pixel or in the tracker So as you see here if you want to cover the whole range of lifetime You need actually to combine both searches metastable particle and pixel or tracker displaced vertices and You have also region which is here We will have it also more often later a region where you could actually do both measurement have both displaced vertices and Metastable particle and in that region in some sense you would have the hope to be to have the better lever arm to measure the parameters notice here in Yellow is the region which is already excluded by the present searches on metastable particles Which of course is very effective for very long lifetime, but it runs out of steam when you have shorter lifetimes Yeah, so this one of course you can interpret in both models either in the our particle serving or in the our party to violating model and here it's the parameter space in the first case Gravitino mass and Stop mass in the other cases are party violating coupling and gain stop mass and you see again that here of course in the case of their party conserving as I was saying for High reheating temperature. You are actually mostly in the metastable particle or a metastable Signal region is instead in the case of the our party to violating you have actually regions Which is also only covered by the by the displaced vertices here above in the in some sense This is the limit from the indirect detection of dark matter Which of course depends one has to say on the mass of the dark matter so on the Gravitino mass So here we have taken one GB So depending on the mass you can move it a little bit around But for this parameter you see immediately that there is a region where you need actually displaced vertices in order to cover The whole parameter space that you it is available Now this one are actually I will have to stress they are for the Ultimate limit of the LHC for three thousand inverse phantom barn. So not really at the next run now of course the best hope would be if you really have a displaced vertices Vertex inside the detector is especially in the tracker or in the pixel Then you would also be able to see the decay the tracks and measure probably the momenta of the decay particles the notice that in the 2d case the visible particles are the same is always a bottom and Yes, so the visible particle as always bottom and left on and these one are invisible in this case And in this case is a just a two-body decay So in some sense from the particle point of view you would see the same thing in the final state But of course the missing energy will gives you a hint And I hope I don't have to ask you which of these two is the our party conserving and which is the our party Violating distribution of momenta, so I think it's pretty clear This one is actually the two-body decay and this one instead is the full body decay So if you would be able to measure the momenta you would actually be able to lead to distinguish if you are our party conservation Or our party violation Okay, so let me go now to the other scenario the scenario where we studied the Gravitino in the PM SSM This was the work done in collaboration with our Baye battalion hasn't come in my movie and in this case We wanted actually to ask especially the question what happens if the NLSP is a neutrality No, and can you really distinguish or see any differences between a neutrality no dark matter and Gravitino dark matter with neutrality no NLSP So we took for the moment they are part of the conserving PM SSM PM SSM is a phenomena larger MSSM with 19 parameters plus one so these plus one is the Gravitino mass in this case and We have imposed also a lot of the constraints which are already there from low energy also have all flavors and also LHC Susie searches and mono jets and the first thing we Know you can you can notice immediately is actually the composition of the neutrality no NLSP The composition here is given in Hixino, Bino and Wino and as you see in the case of Gravitino LSP You don't really care. What is the composition of the? Neutralino you have actually nearly one-third one-third one-third in all the three different types Instead if you require the gravity the Neutralino to be really the dark matter and you want to produce the dark matter density through the WIMP mechanism You are actually nowadays constrained to be mostly in the Hixino region And this is just because the limit of LHC have excluded most of the Bino Space and so you still you have some regions where you have you can arrange to have the right density with Bino But the most of the time actually you are in the Hixino region and very very rarely in In the Wino region so in this sense you have really a completely different composition of the Neutralino in the two cases and These of course gives you also Differences in what you expect here is one plot where we try to compare with the signals in direct detection of dark matter So in this case is the Gravitino case This one is the Neutralino case in this case of course Gravitino the dark matter so this signal is actually not there So even if you see points which are above the line You shouldn't care because the Gravitino you cannot see in direct detection But you notice in the color is instead what can be excluded by LHC at least the infraction of points So you see that the LHC would actually be very sensitive to the blue point and the dark blue in particular and will exclude mostly the light If you want an LSP mass This instead is the case where you have really Imposed also a constraint that the Neutralino makes up the whole dark matter and that you see immediately in this case You have actually that the you well you have in some kind of limit of the cross section You cannot go very much Lower instead in case of the Gravitino you can actually be all over the place is in this case of course they The way to disentangle it would be to have a signal where the parameters look like is be already Excluded by the direct detection and this will already tell you that the Neutralino you're seeing at collider is not really the dark matter Now the other important thing is the production of Gravitino's as we have seen the production of Gravitino Is mostly dominated by the heat temperature and also by the spectrum of the particles and the Giginos in particular And this one is actually shown in these plots where we first of all This is the are the points which are already more or less excluded by the present searches And this one would be in the next the run at 14 TV with 300 inverse phantom bar so we see here and we are plotting here the Yeah, the logarithm of the heat temperature. Sorry. No, that's yeah as a function of the mass of the NLSP so the in this case is the again always the Neutralino and we see here clearly that the Well, we have already some constraints, but there are actually also white regions of very small Neutralino mass So therefore that is a still a possibility and on the other hand in the future We will be able to exclude Neutralino masses at least well depends how well but even in these dark blue regions you exclude 80% of the points up to one TV More or less of the Neutralino mass Here what I wanted to show you is that in principle you can have Gravitino dark matter for any reheat temperature as you see here There are blue points all over the point. They are highly heat temperature Points are here and they are actually more easily tested by LHC because in that region in order to have highly heat temperature You need low gegino masses if you remember the formula it was proportional to the gegino masses square and the reheat temperature and On the other hand you have also regions where the heat temperature is very small and in this region below here actually the superwind mechanism is instead playing a role in the production of gravitas and Due to this connection with the gravitino mass and between the Gravitino energy density and the gluino mass and the reheat temperature We can actually say that the next LHC run will be able to probe this high reheat temperature region and Possibly exclude reheat temperature of the order of 10 to the 9 4 10 to the 9 or something like that So this one is the gluino mass which will nominally be probably excluded in the next run a little bit below 2000 GV and as I said these are the curves which give you the Lowest gravitino mass which is still compatible with the energy density of the dark matter Okay, so let me go to the bariogenesis connection The idea here is of course since we have our parity violation Then the one idea could be also to try to do also bariogenesis with it And actually the idea was already a few years ago by Sundram Kui and Kui later And the idea would be to produce the body in a symmetry true in this case the be violating coupling Arparity coupling and the decay of a beano Which is freezing out in songs after for his pros out These are the diagrams which contributed to the CP a symmetry and in order to have an unvarnishing CP a symmetry You need usually a supersymmetric particle lighter than the beano in this case It is the gluino which is here and you have practically to consider this scenario In this scenario you can very easily embed also gravity in a dark matter through the same decay And this is explained shortly here the idea of course is that when you produce the violin a symmetry from the density For example of the beano you have a large suppression coming from the epsilon CP, which is a small number In the case of dark matter production You would get a large suppression in the case of gravity no especially because the branching fraction of decay into the Gravitino is very small and in this scenario is not Difficult to get an epsilon CP of the same order of this branching fraction so that in some sense You are able to explain the order of magnitude Equality or if you want a similarity between the density of variance and density of dark matter Just by assuming that these branching fraction and epsilon are of the same order notice that at the end this ratio is independent on the mother particle density and You just need to have in some sense the right epsilon CP and the right branching fraction Unfortunately the scenario is not as simple and this is because there are also washout processes if you look Things more in detail as we are still doing you get a lot of contribution and the effects from washout That actually moves the scale especially of the scalar particle to quite a high scale of the order of 10 to the 7 gb So the scenario is still working But you need larger masses of the scalar particle larger masses of the beano Which is also beyond the LHC if you want Will ever probe and in this scenario will also have the possibility to have the the right arc matter density But again due to the suppression through the large scalar masses you need also to push the gravitino mass high So this is not surprising all the scales goes up So it could also be natural to have a heavier gravitino and you can go also to one TV or three TV gravitino in this case the One good news is that the gravitino lifetime is in the ballpark what it will be tested by AMS Especially because in this case the gravity no wood decay also in antiprotons through the our parity violating coupling which is also bio Okay, oh I have zero seconds So I showed just one plot on this So we will look to also these more gen this more simple scenario where you have just two couplings and two masses To parametrize actually these mother particle and daughter particle So the man the dark matter here is psi and sigma is the particle which produces the dark matter and in this case You can have of course the decay of the dark matter again And you have actually a possibility to have both indirect detection and the production of dark matter in the right ballparks With coupling of the order of 10 to the minus 11 or so and we try to look at what it is are the the prospects for Detection at collider and what we found is again that is the same picture as even with the stop You could produce it and in principle have both this place vertices and the metastable tracks And there is still also room to have this double at the traction both in this place vertices and metastable But of course the indirect detection constraints depending on the dark matter mass are in some sense cutting off part of this region if you would be in this region you could be able probably to measure both couplings the mass of the dark matter and Possibly also them. Well the mass of sigma. So in that sense the in this case that would be the Best case scenario where you could be able to reconstruct the full model Okay, so I am to have to finish you can also explain the line But I don't want to spend time on here in the line in case of the line You don't have displaced vertices, but prompt decay And here I leave you my conclusion since I run out of time you can probably read it yourself I hope I convinced you that there are in some sense alternative to the wind mechanism. Thank you If super symmetry will be discovered at LHC, what can you say about the mass of Gravitina and how it is related to the vanishing cosmological constant if we See this picture in the cosmological setting Well, I mean the Gravitino mass is in this case scenarios is not directly measured at the LHC So in this case you would measure only the NLSP only if you are able to also measure the decay The lifetime and you are sure that is an our party conserving case Then you would get a hint of the Gravitino mass Yeah, I'm I do not mean the measuring I mean the theoretical conclusion of discovery What would it imply for Gravitino mass? What are options? Well, I mean of course as you all know, I mean as you know it depends of course on the mediation mechanism What is the size of the Gravitino mass and in this scenario? We are not looking at a particular scenario. I mean a particular Mediation mechanism we are using just the Gravitino mass as a free parameter as you see from the plots Usually we are looking more at GV or 100 GV mass of the Gravitino Which seems to be the the region where you can have higher heat temperature which in some sense We like from the perspective of cosmology in order to have also the Leptogenesis or baryon asymmetry production, but in these scenarios you could also leave with smaller Gravitino mass as long as it is heavier than 100 KV So it is sufficiently cold dark matter. You would actually from cosmological perspective be fine So you will need some mechanism of mediation, which is compatible. Yes. Yes No more questions. Let's thank the speaker again