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PoS(PLANCK 2015)054 http://pos.sissa.it/ ∗ [email protected] Speaker. We studied the interplay between theand direct mass detection experiments. reach The for lack electroweakinos of newsplit at phenomena future at scenarios the LCH with motivates colliders different us electroweakino tomay focus spectra. on reach A masses 100 up TeV hadron to collider 3Moreover, TeV in in scenarios models where of the anomaly lightestinterplay mediation between with collider is searches long-lived not and thermal the direct Winos. detection onlyparameter experiments space. dark might cover large component, part the of the ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 18th International Conference From the Planck25-29 Scale May to 2015 the Electroweak Scale Ioannina, Greece SISSA - International School for AdvancedVia Studies, Bonomea 265, I-34136 Trieste, Italy INFN - Sezione di Trieste, via Valerio 2, I-34127 Trieste, Italy E-mail: G. Grilli di Cortona Searching SUSY from below PoS(PLANCK 2015)054 β m (2.1) , tan µ ]. 1 , 3 TeV respec-  ∼ . Depending on 2 2 G. Grilli di Cortona β ˜ µ m 1 or + 1 ∼ is the mass, ˜  2 ) / β 3 2 m − we show the interplay between , the higgsino parameter 4 2 tan / 3 + m 1 (  ln 2 state. are related by the value of the Higgs mass, µ ] the leading contribution to comes β ˜ 4 W β its beta function, + / , i ˜ 2 tan 3 B 2 ˜ β m , µ ) ) 2 1 2 µ and tan + + β m 2 2 ˜ m or a mixed ( tan ( ˜ W 2 , / π 1 ˜ h 2 α . However ˜ + 2 m / 3 we present the reach at future hadron colliders for split SUSY models m 3 2 2 , , 1 1 g β we describe the properties of the spectra in split SUSY models with anomaly = 2 2 , 1 M is the corresponding gauge coupling, i g In split SUSY with anomaly mediation [ After the discovery of the Higgs , the ATLAS and CMS experiments have constrained In SUSY models higgsino or Wino might have mass up to In Sect. direct detection and collider searches.simplified Details models and for the this interplay scenario, betweensplit reach collider SUSY at searches models and future with direct colliders universal detection for experiments masses other for are described in the original2. work [ Split SUSY with anomaly mediation from one-loop anomaly mediation effects.contribution from However threshold the effects: Bino and Wino masses receive a further where and the scalar mass-scale ˜ bringing the number of free parameters to two once we fixed a value for tan mediation. In Sect. with anomaly mediation with long-lived Winos, while in Sect. is the scalar mass-scale and theeffect. second The model term is in entirely the described right by hand the side gravitino mass of the equation is the threshold the contribution of the higgsino,higgsinos the the nature higgsino of itself the is dark theheavier matter LSP, than candidate with the changes. Wino Wino. NLSP. Winos The Indeed can threshold forthey be corrections light lead the dominate to when LSP a the if higgsinos Bino the areand higgsino LSP. Bino therefore very is heavy it dark and has matter, to however, coannihilate wouldhiggsino, with be a a overproduced pure Wino. in Wino, Therefore the a the mixed early dark universe matter candidate can be a pure several beyond the Standardsions Model of scenarios. the In thethe particular, lack spectrum, of in excluding discovery supersymmetric squarks of new and (SUSY)bounds coloured on exten- states with electroweakinos put are masses strong much below weaker, constraints constraining about on about Binos, 1 few Winos hundred and TeV. On higgsinos GeV. These the to be constraints othertion below might hand, of be supersymmetry: read scenarios as with in heavymodels. tension scalars and with light While a electroweakinos natural giving favours implementa- split upother SUSY on potential the problems such idea as ofover, FCNCs, the solving CP successful the violation unification hierarchy and of fast problem, thea gauge split dark decay. couplings matter SUSY candidate. and It ameliorates the maintains, lightest more- supersymmetric as Searching SUSY from below 1. Introduction tively, not directly accessible at the LHC.33 This motivates TeV the or exploration of 100 higher TeV energiesfuture hadron through hadron colliders. colliders and to Therefore show itexperiments the can complementary is play. roles important collider to searches and study direct the detection physics potential of PoS(PLANCK 2015)054

). The right

background no fb L L H D

@ 1 1 - G. Grilli di Cortona 100 10 1 0.1 0.01 ) or keeping fixed the 1 ]. 8 10.0 5.0 , having therefore the possibility to rule òò 1 − D Wino 2.0 TeV @ 3 lived 1.0 òò . Moreover we show that a 100 TeV collider has the wino - 1 m − ], implying that the charged Wino has a lifetime of order 80 GeV), if feasible (dashed lines in figure 7 òò , > 0.5 6 Long TeV TeV , T TeV TeV 5 p TeV shows the luminosity as a function of the mass reach for different 8 14 33 100 200 òò 1 ]. We derived the mass reach rescaling the cut on the transverse 1 1 1 - - - 10 0.2 fb , fb fb 9 300 20.3 3000 0.1 ]. 1 4 5 8 10

100 10 10

1000

fb L background rescaled @ L H D

1 - cm. ) Long-lived Wino. The left axis shows the integrated luminosity for the method explained in the 10 ( O This search is well motivated because a pure Wino is expected to thermally saturate the relic The signature for long-lived Wino searches is one hard jet from initial state radiation, large Anomaly mediation models with Wino LSP can be probed by long-lived searches. The mass reach corresponding to an existing search at a new hadron collider can be obtained ∼ τ momentum of the jet with the mass of the final state (solid lines in figure abundance around 3 TeV. Figure cut used by ATLAS in itsaxis analysis show ( the integrated luminosity requiring 5 events and no background. hadron collider’s centre of mass energy. LHCmasses at 14 up TeV to will be around able 600 to explore GeV scenarios with with 300 Wino fb missing energy and a disappearing trackrelevant background coming is from due the to unidentified decay of andtransverse the charged momentum chargino with as to high well soft mis-reconstructed as . chargedexperiment The already interacting excludes with up the to inner 250 detector. GeV The in ATLAS this scenario [ c 3. Reach at future hadron colliders Heavy higgsinos can produce acharged spectrum Wino, in while all which the the other neutral statesand are Wino at decoupled. is one-loop The highly is mass degenerate around splitting 170 with at MeV tree the [ level is suppressed by computing the production cross sectionto and put requiring the the same original number bound of [ signal events needed Figure 1: text and on the rightcurrent bound axis, from the [ same for having 5 events and no background. The grey shaded area is the potential to probe Wino mass around 3 TeV with 300 fb Searching SUSY from below PoS(PLANCK 2015)054 gluon → → . g g 3 g g gluon gluon (4.2) (4.1) → → Q g g exchange becomes g g Z q/Q µ contribution Q decreases and h 2 W/Z q/Q gluon gluon G. Grilli di Cortona M W/Z 0 Higgs 0 0 0 ˜ ˜ χ χ ˜ ˜ χ χ → → h g W/Z -2 diagram contributes g the sign of g g W/Z (c) Gluon. 0 0 0 0 β ˜ ˜ χ χ ˜ ˜ χ χ diagrams start to be of the Q twist twist-2 axial-tree , q/Q , such that the . The 2 Higgs → | 2 ], while the dashed magenta curve 2 h axial-loop scalar scalar twist-2 W/Z M 12 , → W/Z → 0 0 q q 0 0 ˜ . At large tan ˜ χ χ ˜ ˜ χ . χ twist-2 axial-loop scalar 2 β scalar q q q q + → cm → Z 1 TeV. In this limit the dominant contributions . 48 h − q q q W/Z q 0 0 W/Z 4 gluon ˜ ˜ χ χ twist-2 10 , + 0 0 0 0 decreases and the ˜ ˜ ˜ χ χ ˜ χ χ . h 2 W/Z ]. The light blue area describes the irreducible W/Z axial-loop scalar SI of luminosity would extend the reach to over 3 TeV. scalar N M σ 1 14 (b) Twist-2. 0 0 0 0 Higgs → → , Higgs − ˜ ˜ ˜ | χ χ ˜ χ χ diagrams dominate. The LUX bounds apply in the region of 13 = → q q q q SI N g σ g h Higgs -2 refer to the diagrams of figure W/Z W/Z and the limit for large tan Q 0 0 0 0 β the cross section decreases and the LSP approaches the pure Wino state. ˜ ˜ ˜ χ χ ˜ χ χ , the twist 2 2 -2 diagrams. However a cancellation suppress the spin independent cross M M h and ∼ < 0 0 ˜ twist χ ˜ χ µ µ ]. The yellow, blue and red curves represent respectively the cross section for and gluon 15 , (a) Higgs. q q with small tan ]. The spin independent cross section of the LSP with a N can be expressed as Diagrams that contribute to the neutralino nucleon cross section. The diagrams with µ gluon 11 Higgs h The spin independent cross section that satisfy the relic density constraint is shown in figure While the higgsino mass increases, Direct detection experiments exploit the recoil energy from dark matter particle scattering on 0 0 ˜ χ ˜ χ irrelevant. When shows the projected reach from LZ [ accidentally cancels the othereventually, diagrams. when Continuing alongmaximal the mixing. yellow curve, The threepositive different yellow/blue curve show the cross section for negative and background [ higgsino, Wino and Bino darkcase matter. and We then will discuss describe the behaviour thea as curve pure the starting higgsino higgsino dark from mass matter is the to increased. pureare have The higgsino a the relic mass density around constraints 1 section: where to the amplitude with oppositeaccidental sign cancellation. with respect to the other diagrams and itThe will magenta then area lead represents to the an region excluded by LUX [ same order of the other contributions. There is a value of Searching SUSY from below Figure 2: are relevant only for the Spin Dependent cross section. out anomaly mediation scenarios with longTeV lived collider chargino. or An an increase increase in the inrange: luminosity the a for energy 200 a would TeV 100 collider be with enough 1000 to fb probe the thermal dark matter mass nuclei [ 4. Direct detection interplay PoS(PLANCK 2015)054 (4.3) TeV decreases TeV TeV TeV 16 GeV GeV µ 27 > TeV 100 450 TeV 3 . In the upper > 550 > > 30 30 350 3 4 M 3 3 > , > > > M 3 M M , 3 3 3 , , . In order to have M G. Grilli di Cortona M M M , . The relic density GeV , , , µ -2 contribution and GeV TeV TeV µ TeV 1600 TeV 10 50 TeV TeV diagrams are the only 2900 5 8 7 12 > > > 2 2 2 > > > > > twist Μ Μ Μ Μ Μ M M M 1 2 3 4 5 6 7 8 and Higgs must decrease. When gluon µ 5000 pure plane. The yellow line divides the plane 3 6 wino direct detection and collider searches are . ) àà 2 2 àà 2 µ 2 TeV M TeV = cm TeV TeV , Β 1 47 16 2.8 M − tan 400 100 > 2000 ( 5 > , 0 3 10 > > 3 < M Μ Μ M Μ . àà 1 -2 diagrams are also important. As it was for the pure àà SI diagrams cancel the N 4 5 scenario the direct detection searches are limited due to D σ 1000 µ and represents the area in which the higgsino is the LSP. We twist TeV decreases and the cross section stays constant, this is the top GeV @ 1 TeV µ àà

Higgs LZ 1.4 2 M -2 diagrams: and -2 contributions accidentally cancel suppressing the cross section: higgsino LSP 39 AMSB Β , = > m Β µ > 3 500 tan Μ M pure tan twist twist planes for both negative (left) and positive (right) , gluon ) 0 2 > large and and Μ M the , 8 such that the 2 µ ( M µ gluon gluon 200

dominated  7 µ

Bino Neutrino

background LUX Spin independent nucleon-neutralino cross section in a split SUSY with anomaly mediation model 100 48 50 52 42 44 46 ------

The interplay between collider and direct detection searches is shown in figure

10 10 10 10 10 10

cm D @ Σ

2 SI constraint excludes the blue region. Thefor bounds at long-lived LHC8 Winos and searches projected reach arebelow at shown a the by 100 TeV grey the collider dark linesgluino and is light pair excluded green searches. by area LHC8 In respectively.the the suppression or The of negative area it the may cross section, be while probed for positive at a 100 TeV collider through complementary. The bottom panel describes the the correct relic density, the Bino mustmass coannihilate scale with and the maintain Wino and the in rightthe order splitting cross to for decrease section coannihilation, the increases. LSP panels there are the Figure 3: (the red curve describe a Bino-likematter LSP, candidate). the yellow The curve magenta a areareach higgsino-like is of and the the LZ. actual blue The bound one neutrino bythe a background right LUX, Wino-like is dark panel. the shaded dashed in magenta light line blue. is The the numbers projected are explained in the legendIn on the region in two region with opposite sign of Searching SUSY from below there is a value of the cross section vanishes.dominated by When the the higgsino and the Bino are decoupled the cross section is Increasing further the value of contributions to the cross section and they are suppressed by the large value of higgsino case, the flat edge of the blue rectangle. Once the Bino becomes the LSP, the PoS(PLANCK 2015)054 G. Grilli di Cortona ], we presented also mass reach for 1 0 ) in the left (right) panel. The bottom > µ 0 ( < µ 6 ) for 2 M , µ ). Direct Detection, collider constraints and future reach are also shown. 2 M , 1 M The parameter space region allowed by the requirement that the neutralino relic abundance does The fact that the LHC excludes electroweakinos up to few hundred GeV, wellIn below this the talk, inter- we presented the mass reach for long lived searches in split SUSY models with Figure 4: not exceed the relic density in the plane ( esting case of SUSY dark matter, motivates studies of mass reach atanomaly future mediation hadron at future colliders. hadron colliders, thetarity implications with for direct dark detection matter experiments. and In the the complemen- original paper [ Searching SUSY from below panel shows the plane ( have to notice how long-livedspace, Wino leaving searches unexplored regions would corresponding be to able the to pure Wino probe and large higgsino part cases. 5. of the Conclusion parameter PoS(PLANCK 2015)054 . , 9812 31 ]. (1999) 79 JHEP , 557 Phys. Rev. D G. Grilli di Cortona ]. , ]. of luminosity. Long-lived ]. s= 8 TeV with the ATLAS 1 Nucl. Phys. B . − √ , ]. arXiv:1310.8214 Aspects of ]. ]. Discovering SUSY at the Tevatron in wino Gaugino mass without singlets -jets and leptons) and Bino LSP, with Bino b (2014) 091303, [ arXiv:1110.0103 ]. Generic and chiral extensions of the supersymmetric ,[ hep-ph/9904250 112 7 hep-ph/9904378 hep-ph/9811316 arXiv:1310.3675 [hep-ex] Phenomenological consequences of SUSY with anomaly Search for charginos nearly mass degenerate with the lightest , arXiv:1412.5952 [hep-ph] First results from the LUX dark matter experiment at the Sanford β (1999) 27 [ (1999) 1731 [ (1999) 47 [ ]. Phys.Rev.Lett. Detectability of Certain Dark Matter Candidates 83 , 559 543 hep-ph/0409232 Out of this world supersymmetry breaking (2013) 11, 112006 [ (2015) 035 [ 88 ]. http://collider-reach.web.cern.ch Collider reach Hunting electroweakinos at future hadron colliders and direct detection After LUX: The LZ Program 1505 , (2005) 3 [ Nucl. Phys. B Nucl. Phys. B Phys. Rev. Lett. , , et al. , 709 [ATLAS Collaboration], JHEP hep-ph/9810442 , Phys. Rev. D , et al. hep-th/9810155 standard model induced masses (1985) 3059. Nucl. Phys. B Underground Research Facility LSP scenarios https://gsalam.web.cern.ch/gsalam/talks/repo/2014-02-FHC-PU-collider-reach.pdf experiments (1998) 027 [ detector neutralino based on a disappearing-track signature in pp collisions at [ In conclusion we showed how future hadron colliders can explore the neutralino dark mat- In anomaly mediation scenarios, the ratio between the and the Wino mass is large, [5] H. C. Cheng, B. A. Dobrescu and K. T. Matchev, [6] J. L. Feng, T. Moroi, L. Randall, M. Strassler and S. f.[7] Su, T. Gherghetta, G. F. Giudice and J. D. Wells, [8] G. Aad [9] G. Salam, A. Weiler, [1] G. Grilli di Cortona, [3] G. F. Giudice, M. A. Luty, H. Murayama and R. Rattazzi, [4] N. Arkani-Hamed, S. Dimopoulos, G. F. Giudice and A. Romanino, [2] L. Randall and R. Sundrum [10] G. Salam, A. Weiler, [11] M. W. Goodman and E. Witten, [12] LUX Collaboration, D. Akerib et al., [13] D. C. Malling ter parameter space in splitbeyond SUSY the LHC. with anomaly mediation, addressing the necessity of colliders References Winos set strong mass reach inare regions weak: of the the parameter interplay spacelarge where between areas direct of collider detection the and experiments parameter direct space of detection neutralino experiments dark may matter. be able to cover making Wino searches more powerful. Indeeddark a matter 100 (and TeV indirectly collider gluinos may heavier be than able 20 to TeV) with reach 3000 pure fb Wino NLSP decaying to andW gravitino and in gauge with mediation higgsino models.and NLSP Moreover direct decaying we detection presented to experiments interplay gravitino for between models and collider of Z searches split or SUSY with universal gaugino masses. Searching SUSY from below scenarios with Wino NLSPs decaying to leptons (or PoS(PLANCK 2015)054 G. Grilli di Cortona , (2014) 023524 89 Phys. Rev. D , Implication of neutrino backgrounds on the reach of 8 ]. ]. Working Group Report: WIMP Dark Matter Direct Detection , et al. arXiv:1310.8327 arXiv:1307.5458 [ next generation dark matter direct detection[ experiments B. Cabrera [15] J. Billard, L. Strigari and E. Figueroa-Feliciano, Searching SUSY from below [14] P. Cushman, C. Galbiati, D. N. McKinsey, H. Robertson, T. M. P. Tait, D. Bauer, A. Borgland and