DM M Sear earch C ch Compl omplem ement entarity E Empl mployi oying ng pMSSM SSM SU SUSY SY . M. C Cahill ill-Row owley, ey, R. C Cotta tta, , A. D . Drlic ica-Wagner gner, S. S. Fu Funk, , J. . Gain iner, J. Hewett tt, , A. I . Ismail il, , 1 5/ 5/25 25/15 15 M. W Wood, od, T.G. G.R. R.
Dark m ark mat atter er exi exists at at al all scales . es .. …& it i int ntera racts with us vi h us via grav a gravity But WHA WHAT is is it ? it ? 2
What hat do do we k e know now ? • Ω h 2 = 0.1188 188 ± 0.0010 010 (why hy?) ?) Non on-bar baryoni onic (BBN) • • Dark = Electrically ‘neut eutral al’, color or singl nglet et Ver ery lon ong-lived ed ≈ stabl able • • Col old = non non-rel elat ativistic during ng struc uctur ure Self-ints. are Se e cons nstraine ned for ormation (& now now too) oo) • It coul ould d be com ompl plex ex ng w/ SM ← • At At most weakly-int nter erac acting • X X SM ? ?? The us ual ν ’s ar The usual are e hot hot ↔ ∑ m ν < ~ ~ 0. 0.25 25 eV eV Heav eavy neut neutrinos os? → via the Z.. many orders of magnitude too large ! NOT th OT the S SM ! ! 3
No o shor shortag age of of i idea deas… T.Tait T.T Of c cour ourse D DM may ay be be made of ade of m many any ..and and the he list kee eeps gr growing ! differ erent nt compon onent ents-- --not j jus ust one one We e don don’t kno now if the he SM & DM tal alk to o eac each ot othe her non non-gr grav avitat ational onally – • thi his is an an assum umpt ption( on( = hope) pe)…ot othe herwise e we’re e sunk unk (or not not….) 4
χχ ↔ SM SM SM SM Fami amiliar Ther ermal WI WIMP P idea: ea: → < σ v> > ≈ 2. 2.8 x 8 x 10 10 -26 cm cm 3 sec c -1 1 → M DM DM ~ 0. 0.1-1 T 1 TeV eV f for E or EWK coupl oupling ngs ! 5
Compl omplem emen entar arity : y : Anot nother her F Fami amiliar ar P Picture In real ality this ‘relat ations onshi hip’ p’ is not not so o trivial ! “SM” may ay be be di different in n ← the differ eren ent direc ection ons Ther ere are e sev ever eral al ways to des describe the he ins nside of of the he bl blob ob: EF EFTs, Simpl plified ed Model dels, or UV compl plet ete e scenar enarios os eac each with h thei heir own n good od & bad d aspec pects 6
Tim im T Tait it 7
Supers upersymmetry: a a canon canonical U UV-com compl plete t e theo heory • All ll SM par particles hav have e SUSY spa partners wit ith spin pin of offset by by ½. ½. R-par parity ins insures a a stab able LS LSP whi hich mus ust be be neut neutral & colorles ess. . For or this his tal alk this his is the he ligh lightest neut neutralino (next t slide) de) • SUSY is is br brok oken by by a a lar large set et of of sof oft mas ass ter erms (~10 100!) gene generated in in som ome e hidd hidden sec ector at at a a hi high gh scale. Spe pecific scen enarios (the here ar are e many any) wil ill int inter-rel elate ate these e parameter eters. . But ut whic hich? We’d We’d lik like to o be be agno agnostic.. Try t to be unpr o be unprejudiced… 8
Ne Neut utral S SUS USY Particles Bino, o, wino o & Higgs gsinos nos mix when en SUSY is brok oken. en..the he lightes est can an be the LSP
• But ut w wai ait! Isn’ n’t S SUSY dead dead ?? ?? Does oes the l he lac ack of of any any appar apparent sig igns o of SUSY SUSY at the L LHC HC im imply ly t that t there is is no SUSY SUSY and/or the and/ he mot otivation n for or S SUSY has has been l been los ost? • What hat do do we e want ant from SUSY SUSY ? (i) It gi gives es us us a a pl plaus ausibl ble W WIMP D DM candi andida date as e as abov above. (ii) I It al allow ows t the he SM coupl ouplings gs t to o ‘uni unify’ at at a a hi high gh scal ale (iii) I It hel helps ps to o reduc educe t the he fine ne-tun uning ng ( (FT FT) & hi hier erar archy pr probl oblems . Onl nly her here i e is ther here s som ome ( e (the heoretical?) i issue ue.. as as SUSY sear earches es i inc ncreas ase i in n streng ngth w h w/o o any any signal gnal ? ? How FT FT inc ncrea eases es ow m muc uch FT h FT is too oo muc uch? We’ll hav have t e to o look ook at at thes hese s e sear earche hes mor ore c e critically 10
Unific ficatio tion: : Su Supersy rsymmet etry ry In n SUSY, t the S he SM gauge c gauge coupl oupling ngs UNI UNIFY near near ~ ~10 10 16 16 GeV V but t but thi his does does not not happen happen if w we e onl only hav have t e the he SM SM p partic icle les. . 11
The he Hierar erarchy P Probl roblem: Su Supersym ersymmet etry ry Energy gy ( (GeV) V) Lar Large quadr adrat atic loop p effec ects canc ncel el 10 19 Pla Planck orde der by order der bet between the he fer ermions 10 16 GUT UT & bos bosons in n PT lea eaving onl only the he log og terms… … desert bo boson ~ α M Pl 2 δ m H 2 ~ Pl 10 3 Weak ak LHC HC fermi mion on ~ - α M Pl 2 δ m H 2 ~ Pl All o ll of ~ ~ α |M 2 boson – M 2 ermion | log og (M PL PL /m H ) ) know nown fer ph physics →→ this canc ncel ellat ation on is more tuned ed as Solar S Syst ystem the he mas ass spl plitting gr grows 10 -18 Gravity ty
Take ake a a Step B ep Back ack: neu neutralinos as D as DM →→ Neutralinos right out of the box with arbitrary masses do NO NOT gi give t the he righ ght r rel elic dens density Bino inos don’ don’t anni annihilate enou enough.. • wino inos & Higg iggsinos too oo muc uch h unle unless they hey ar are e ~3( 3(1) 1) TeV eV Bino inos need need to o anni annihilate thr hru u • a funnel/resonance (Z,h,..) or Baer aer via ia a a co-anni annihi hilati ation on proces ess wit ith anot anothe her near nearby spar particle Var arious adm admix ixtures of of stat ates wil ill als also wor ork if if the he mas asses & mix ixings • ar are e pr prop oper erly chos hosen, e. e.g. g., ‘well ll-tem temper ered ed’ neutr tral alinos nos We e can an study dy al all thes hese c e cas ases es s simul ultane neou ously us using ng the pM he pMSSM !! 13
The p( he p(henomenol henomenologi ogical cal)MSSM • General eneral CP CP-cons onser erving ng MSS MSSM wi with h R-pari parity • MFV a V at the he TeV eV s scal ale (F (Flav avor or=CKM) M) • Li Light ghtes est neut neutral ralino o is the he LS LSP. • 1 st st /2 /2 nd generat generation s on sfer ermion ons degenerat degenerate e 50 GeV ≤ |M 1 | ≤ 4 TeV • Ignore 1 gnore 1 st st /2 /2 nd generat generation A on A-ter erms & &Yukawa’ wa’s. . • No No as assumpt ption ons wrt wrt SUSY SY-br brea eaking ng 100 GeV ≤ |M 2 , μ| ≤ 4 TeV • The neut he neutral ralino no not not nec neces essar arily the he onl only DM DM 400 GeV ≤ M 3 ≤ 4 TeV 1 ≤ tan β ≤ 60 100 GeV ≤ M A , l, e ≤ 4 TeV the he pMSSM SSM wit with 19 19 param amet eter ers 400 GeV ≤ q 1 , u 1 , d 1 ≤ 4 TeV 200 GeV ≤ q 3 , u 3 , d 3 ≤ 4 TeV ‘ Thr Throw ow dar darts’ int nto t o thi his s spac pace.. l look ook at at |A t,b,τ | ≤ 4 TeV the v he var ariou ous pr predi ediction ons -- --the hen k keep eep poi point nts t tha hat s sur urvive al e all cons onstraints & & study dy t them em Sev ever eral s studi udies es.. 14
Rel elic den density con onstraint sat atisfied but but mos ost mod odels lie e far ar bel below it ←Planck 15
Wel ell-tem empered ed neut neutral alino no Bino c no co-an anni nihilat ation on N O T heav heavy wino H I L N G E P 1 1 TeV eV H Higgs ggsino no H/A r reson onant ant a annihi hilat ations ns Bino annihilation through h/Z funnels 16
40 0 30 0 Z pMSSM SSM 45 5 60 0 50 0 70 70 f-o now now f-o o ↑ 17 Scales up up & dow down w n with th Higgs ggsino con onte tent
Γ ( Z →χχ ) < < 2 Me 2 MeV LEP EP Bo Bound ↓ ↑ ! Inc ncreas asing g rel elic dens density Clear early LSP masses es below ow ~30 30 GeV eV woul ould be be exclud uded ed IF we e sat aturate the he rel elic den density or lie ie below it pMSSM model pM odels w w/ rel relic densi density sat saturated 18
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