LHC searches for dark matter.! Uli Haisch

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1 LHC searches for dark matter! Uli Haisch

2 Evidence for dark matter Velocity Observed / 1 p r Disk 10 5 ly Radius Galaxy rotation curves

3 Evidence for dark matter Bullet cluster Mass density contours 10 7 ly X-ray image Gravitational lensing

4 Evidence for dark matter 10 9 ly Structure formation

5 Content of Universe Ordinary matter Dark matter Dark energy

6 But what is dark matter? As a particle physicist I want to know how dark matter (DM) fits into a particle description What do we know about it? - Dark (neutral) - Massive - Still around today (stable or with a lifetime exceeding the age of the Universe) Nothing in the Standard Model of particle physics fits the profile Standard Model (SM)

7 DM questionnaire Mass: Spin: Lifetime: Couplings: Gravity Weak interaction? Higgs? Quarks/gluons? Leptons? Thermal relic? Yes No

8 Particle probes of DM Fermi telescope χ DM particles SM particles χ Indirect detection The common theme of searches for DM is that all methods are determined by how the DM particles interact with the SM

9 Particle probes of DM LUX detector χ Direct detection DM particles χ SM particles The common theme of searches for DM is that all methods are determined by how the DM particles interact with the SM

10 Particle probes of DM χ χ LHC at CERN SM particles DM particles Collider searches The common theme of searches for DM is that all methods are determined by how the DM particles interact with the SM

11 Resid. (σ) Fermi-LAT Has DM already been seen? Energy (GeV) CDMS II Events / 5.0 GeV (c) P7_REP_CLEAN R3 2D E = GeV γ = 17.8 evts = evts n sig s local = 3.3 σ n bkg Γ bkg = 2.76 DM? Resid. (σ) Energy (GeV) Energy (GeV) DM? a line near 130 GeV in R3: (a) at 130 GeV in the P7CLEAN data using the 1D energy dispersion model t 133 GeV in the P7REP CLEAN data again using the 1D model; (c) same as (b), but using the 2D energy e Sec. IV). The solid curve shows the average model weighted using the P E distribution of the fitted events. were unbinned; the binning here is for visualization purposes, and also that the x-axis binning in (a) is tive to (b) and (c). Claims for DM discovery have been made based on the results of indirect and direct detection experiments. Since the backgrounds in both cases are large and uncertain (and given that we have no control over the signal), claims remain unsubstantiated

12 DM production at the LHC If DM particles are sufficiently light and couple to quarks or gluons, we should be able to produce them at the LHC By studying DM production in proton-proton collisions, we are testing the inverse of the process that kept DM in thermal equilibrium in the early Universe LHC may allow us to produce other states of dark sector, which are no longer present in the Universe today ATLAS detector 46 m 25 m, 7000 t, 3000 km of cables,

13 How to see the invisible? The DM particles interact so weakly that they are expected to pass out of the detector components without any significant interaction, making them effectively invisible (much like neutrinos) χ χ One way to see DM particles nonetheless, works by looking for missing momentum and additional SM radiation Visible radiation SM particles Missing momentum

14 How to see the invisible?

15 How to see the invisible? Missing momentum Missing momentum

16 χ χ How to see the invisible? Second way to try to detect SM, based on production of partner particles that decay to DM and SM particles Partner particles SM particle SM particles Missing momentum SM particle

17 Bump hunting for the Higgs The di-photon decay of the Higgs leads to a nice bump in the invariant mass distribution

18 Bump hunting for the Higgs To see the bump for the Higgs decaying to two Z bosons, one does not even have to zoom in

19 Tail surgery to find DM SM background dn/det, miss [events/gev] DM signal Overwhelming SM background, that arises in the case of monojet searches from Z + jet production with the Z boson decaying to neutrinos E T, miss [GeV]

20 Tail surgery to find DM 10 4 dn/det, miss [events/gev] SM background SM background DM signaldm signal The presence of DM manifests itself in a small enhancement in the tail of the missing energy distribution E T, miss [GeV]

21 A big challenge indeed How well can I measure the few events sitting in the tail? How well can I calculate these small numbers? Experimentalist Theorist

22 Precision QCD predictions Proton Parton distribution functions

23 Precision QCD predictions Neutrino Neutrino Hard scattering process Gluon Z Proton Parton distribution functions

24 Precision QCD predictions Neutrino Neutrino Hard scattering process Parton shower evolution Gluon Z Proton Parton distribution functions

25 Precision QCD predictions Neutrino Clustering, hadronisation and decays Neutrino Pions, leptons and photons Hard scattering process Parton shower evolution Gluon Z Proton Parton distribution functions

26 But we also need a DM theory The three main search strategies perform quite different measurements. Without a theoretical model of DM, we cannot compare the results Direct detection χ Indirect detection If evidence for DM is found in one type of search, we can predict in a given model the signals that should be seen in other searches Collider searches

27 No lack of theoretical models MSSM R-parity violating NMSSM Hidden Sector DM Self-Interacting DM WIMPless DM msugra pmssm Gravitino DM Supersymmetry Dark Photon Technibaryons Asymmetric DM Dirac DM R-parity Conserving Q-balls Light Force Carriers Dynamical DM Extra Dimensions Warm DM Solitonic DM UED DM Sterile Neutrinos Quark Nuggets 6d 5d Warped Extra Dimensions Axion DM? T-odd DM RS DM QCD Axions Little Higgs T Tait Axion-like Particles Littlest Higgs

28 No lack of theoretical models MSSM R-parity violating NMSSM Hidden Sector DM Self-Interacting DM WIMPless DM msugra pmssm Gravitino DM Supersymmetry Dark Photon Technibaryons Asymmetric DM Dirac DM R-parity Conserving Q-balls Light Force Carriers Sterile Neutrinos Warm DM Theories of Dark Matter Solitonic DM Quark Nuggets Dynamical DM UED DM 6d 5d Extra Dimensions Warped Extra Dimensions Axion DM? T-odd DM RS DM QCD Axions Little Higgs T Tait Axion-like Particles Littlest Higgs

29 Spectrum of DM theory space Less complete Dipole interactions Effective field theories Simplified models Z boson Dark photon Minimal supersymmetric SM Contact Interactions Higgs portal Squarks Complete models Models Sketches of models Little Higgs More complete Universal extra dimensions

30 Complete DM theories

31 Complete = complicated All complete DM models add more particles to the SM, most of which are not viable DM candidates g c t H d The classical example is the MSSM, in which each SM particle gets its own superpartner u τ s b γ In the case of the MSSM there are 20 additional parameters that can be relevant for DM physics W μ e Z νi Minimal supersymmetric SM (MSSM)

32 One way to produce DM in MSSM Proton Top squark Top quark χ χ Gluon Top quark

33 LHC limits on DM mass in MSSM

34 LHC limits on DM mass in MSSM Range of DM masses unexplored by the first LHC run 250 GeV

35 LHC limits on DM mass in MSSM Range of DM masses unexplored by the first LHC run 250 GeV 175 GeV Masses of all the SM particles: top quark, Higgs, Z boson,

36 LHC limits on DM mass in MSSM 600 GeV Ultimate reach of the LHC 250 GeV Excluded by the first LHC run

37 DM effective field theories

38 Effective = easy At the other end of complexity are models in which the DM particles are the only new states that can be produced at the LHC In such cases, effective field theory allows us to describe the DM-SM interactions mediated by all heavy particles in a simple and universal way Mass 5 TeV 1 GeV Z2 Very heavy states with DM-SM interactions q χ Z3 Z1

39 Effective field theory primer q q Z 1 X g 2 = X p 2 MZ 2 ( q q)( X X) 1 p = p q + p q = p X + p X

40 Effective field theory primer q q Z 1 X g 2 = X p 2 MZ 2 ( q q)( X X) 1 p = p q + p q = p X + p X p 2 M 2 Z 1 g 2 M 2 Z 1 ( q q)( X X)

41 Effective field theory primer q q Z 1 X X = g 2 p 2 M 2 Z 1 ( q q)( X X) p 2 M 2 Z 1 1 M 2 q q X X = g 2 M 2 Z 1 ( q q)( X X)

42 Effective field theory primer Mass Information on heavy states encoded in a single coupling Z2 Z3 Z1 1 M 2 = g2 M 2 Z 1 5 TeV 1 GeV q χ q q X X Independent of heavy physics

43 LHC limits on suppression scale [GeV] * Suppression scale M Operator D5, SR3, 90%CL Expected limit (± 1 ± 2σ exp ) Observed limit (± 1σ theory ) Thermal relic ATLAS Preliminary s=8 TeV Ldt = 10.5 fb -1 effective theory not valid 700 GeV Excluded by the first LHC run WIMP mass m χ [GeV] 3

44 Comparison with direct detection - [ - ] Spin-independent interactions LHC excluded - Direct detection excluded - [ ] The LHC constraints are strongest at low DM mass, where direct detection is challenging due to the small nuclear recoil

45 Comparison with direct detection - [ - ] - Spin-dependent interactions - - Direct detection excluded LHC excluded - - [ ] The LHC is superior to any spin-dependent search for all DM masses, since DM-nucleon scattering is incoherent in this case

46 Simplified DM models

47 Simplified = in-between Another interesting option is to consider models that contain DM and the most important state mediating its interactions with the SM Unlike the effective field theories, these simplified models can describe the full kinematics of DM production at the LHC Simplified DM models have typically a few parameters Mass 5 TeV 1 GeV q Z2 State with DM-SM interactions that can be produced at the LHC χ Z3 Z1

48 Outlook Dark matter implies physics beyond the Standard Model An understanding of dark matter thus requires new theoretical concepts. These can be complete models, but it is also fruitful to think about less defined, more hazy sketches of theories Searches at the LHC, in underground experiments and in astrophysical observations naturally target different parts of the dark matter theory space. They complement one another Once we have a detection, only the full suite of techniques will allow us to fully learn what dark matter really is

49 The LHC can bring sketches of dark matter to life!

50 2013 A possible timeline Mass Spin Stable? Couplings: Gravity Weak interaction? Higgs? Quarks/gluons? Leptons? Thermal relic? 2018

51 2013 A possible timeline 2014 LUX sees a handful of elastic scattering events consistent with a DM mass < 200 GeV ? Mass: < 200 GeV Spin Stable? Couplings: Gravity Weak interaction? Higgs? Quarks/gluons Leptons? Thermal relic?

52 2013 A possible timeline LUX sees a handful of elastic scattering events consistent with a DM mass < 200 GeV Fermi observes a faint gamma ray line at 150 GeV from the galactic center Mass: 150 +/- 15 GeV Spin Stable? Couplings: Gravity Weak Interaction? Higgs? Quarks/gluons Leptons? Thermal Relic?

53 2013 A possible timeline LUX sees a handful of elastic scattering events consistent with a DM mass < 200 GeV Fermi observes a faint gamma ray line at 150 GeV from the galactic center 2016 Xenon sees a similar signal Two LHC experiments see a significant excess of leptons plus missing energy Mass: 150 +/- 15 GeV Spin 2017 Stable? Couplings: Gravity? Weak interaction? 2018? Higgs? Quarks/gluons Leptons? Thermal relic?

54 2013 A possible timeline Mass: 150 +/- 15 GeV Spin: > 0 Stable? Couplings: X Gravity Weak interaction Higgs? Quarks/gluons Leptons Thermal relic? Xenon sees a similar signal Two LHC experiments see a significant excess of leptons plus missing energy No jets plus missing energy Fermi observes a faint gamma ray line at 150 GeV from the galactic center Neutrinos are seen coming from the Sun by IceCube

55 2013 A possible timeline LUX sees a handful of elastic scattering events consistent with a DM mass < 200 GeV Fermi observes a faint gamma ray line at 150 GeV from the galactic center Xenon sees a similar signal A positive signal of axion conversion is observed at an upgraded ADMX Two LHC experiments see a significant excess of leptons plus missing energy Mass: 150 +/- 15 GeV Spin: > 0 Stable? Couplings: X Gravity Weak interaction Higgs? Quarks/gluons Leptons Thermal relic? Mass: 20 μev Spin: 0 Neutrinos are seen coming X Stable from the Sun by IceCube. Couplings: Gravity Photon interaction Higgs? Quarks/gluons? Leptons? X Thermal relic?

56 2013 A possible timeline Mass: 150 +/- 0.1 GeV LUX sees Spin: a handful > 0 of elastic scattering events consistent with a DM Stable? mass < 200 GeV. Couplings: X Gravity Weak unteraction Higgs? Xenon sees a similar signal. Quarks/gluons Leptons Thermal relic A positive signal of axion conversion is observed at an upgraded ADMX X Mass: 20 μev Spin: 0 Stable Couplings: X Gravity Photon interaction Two LHC experiments see a Higgs? significant excess of leptons Quarks/gluons? plus missing energy. Leptons? Thermal relic No jets + MET Fermi observes a faint gamma ray line at 150 GeV from the galactic center Neutrinos are seen coming from the Sun by IceCube 2018???? Observation at a Higgs factory indicates that the interaction with leptons is too strong to saturate the relic density

57 2013 A possible timeline ???? Spin: > 0 LUX sees a handful of elastic scattering events consistent Stable? with a DM mass < 200 GeV. Couplings: Xenon sees a similar signal. X A positive signal of axion conversion is observed at an upgraded ADMX Mass: 150 +/- 0.1 GeV Gravity Weak interaction Higgs? Quarks/gluons Leptons Thermal relic Mass: 20 μev Spin: 0 Stable Couplings: Gravity Weak interaction Two LHC experiments Higgs? see a significant excess of Quarks/gluons? leptons plus missing energy. Leptons? X Thermal relic No jets A multi-pronged search strategy identifies a mixture of dark + MET matter which is 50% weakly interacting particle and 50% axion X Observation at a Higgs factory indicates that the interaction with leptons is too strong to saturate the relic density Fermi observes a faint gamma ray line at 150 GeV from the galactic center Neutrinos are seen coming from the Sun by IceCube

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