Plan for 3 lectures Introduction. The need for new physics. - PowerPoint PPT Presentation

Plan for 3 lectures � � Introduction. The need for new physics. Portals to new Physics. � Strong CP problem and axion solutions. Searches for axions and axion-like particles. � Weakly interacting massive particles. WIMP interaction with Standard Model particles. Some snapshots of WIMP phenomenology. � Dark mediators. Direct searches of dark mediators at low and medium energies. ��

Plan for 3 lectures � � Introduction. The need for new physics. Portals to new Physics. � Strong CP problem and axion solutions. Searches for axions and axion-like particles. � Weakly interacting massive particles. WIMP interaction with Standard Model particles. Some snapshots of WIMP phenomenology. � Dark mediators. Direct searches of dark mediators at low and medium energies. ��

Plan for 3 lectures U of Pospelou Victorian Maxim � , Perimeter Inst . � Introduction. The need for new physics. Portals to new Physics. � Strong CP problem and axion solutions. Searches for axions and ÷ axion-like particles. � Weakly interacting massive particles. WIMP interaction with Standard Model particles. Some snapshots of WIMP phenomenology. � Dark mediators. Direct searches of dark mediators at low and medium energies. TGU ��

Evidence for New Physics � � Standard Model based on SU(3)*SU(2)*U(1) interactions is a well- F- established paradigm � Evidence for “New Physics” – interactions and particles and fields beyond the SM field content – comes from the neutrino physics and cosmology � These are enormous subjects to cover in 3 lectures – but a lot of reference literature exists. ��

Early cosmology is relatively simple . ⇐ nyw=a#E Parameter Value (68%) +BAO) Parameter Value (95%) ! b h 2 " 0.02207±0.00027 -0.0005±0.0066 ! K " ! c h 2 " 0.1198±0.0026 (is it high?) # m $ (eV) " <0.23 100 # * (acoustic scale at 1.04148±0.00062 (~ 500 parts recombination) per million accuracy) N eff 3.30±0.54 0.091±0.014 (WMAP seeded) Y P " 0.267±0.040 $" ln(10 10 A s ) 3.090±0.025 �� tz - n s 0.9585±0.0070 (<1 at > 5 % )

Dark energy, dark matter to €£→m � stgruatery not forms Chester P€e⇒t Particle physg st. , cosmological ( constant ) Asto tart a- ��

Dark energy, dark matter, dark forces...? last Far � Historic examples : ( ? , A) 1920s force strong heutrouy + ��

Dark energy, dark matter, dark forces...? EM Maxwell theory 1960s � radioctrvity 1898 - 1932-35 neutrons , strong - force -1972-4 neutral Weak - currents of discovery -2012 - fundamental Yukawa force ? ? force 2050 Dark �� -

Nx : Possible types of dark matter � WIMPs (weakly interacting massive particles) Fly abundance X\→SM/ forbidden ← allowed ,±aggyystray§ sm - Xx → . mx.in#tagRCinnad;gFep T3 nr h× Tznnx - - ya " px t - bgpx IEEE - ) ��

Possible types of dark matter � Super-WIMPs (super-weakly interacting massive particles) nxaeri handed gravitionosetc Right neutrinos 's - . bbgpx couplings - L%h¥*i7 #t±eyIw×hgr . rate expansion ��

>n÷ has Possible types of dark matter sub all - particles - � Super-cold DM (axions, any other light bosonic field). - cannot fermion tell mf 0.5 ← < DM , form out it of boy §× , µ , nmx I €Xs↳pir⇐h÷ It ' = slope Zt 1 -3 ¥•m4 tcollectim ' particles of oscillations of classical field �� - or

Energy and intensity frontiers � yeux M= * trxnemxr ( , ) k=e= - t÷mi .pro#gtTnx=G=.6/YIsd.er ( Atlas ,cms ✓ loghx -3k$ ~Mz - iwtewitfowtier ���

Portals to New Physics � Left =Eo±o*d (15+4.5) Http ( h An / book for sBµwFµ WdFFnensm to "@HN7 #rN*¥ sfjeff operators . strength - ���

Portals to New Physics � ) ( Http ( A. Higgs p . kinetic Fio Bµ , $+1.51 mixing p . portal ( LH ) neutrino N portal I vector ( 4- A K4 ) , ¥ jfrsf ) ⇐ portal axiom fa . @k4)(Frx) . - . - . . . . . . ���

Evidence for neutrino portal � IV SM not a- gauge invariant operator .am 417=45 Heavy scale zV÷ V= 246 of My = ; G==1 ZVZ . ���

Evidence for neutrino portal � Natural completion UV 0¥ 'T ' ←*÷n←n E genie .#zn . +y¢H)N simplest a- model for = 7544 ) ? u masses - . ���

Motivation for axion portal � 4- ( rrrst dm=t 75A ) [ strong problem CP , solution axiom ���

Summary of Strong CP problem � SM ) generically ( and QCD more has trivial a non vacuum - due to structure strong dynamics tnstantons and . , >>my for Responsible My .← condition baby Same , to observability term of 0 mxn - . Lazio Lac . otszsttrquaqwa = + totally GZ perturbative is * non . 0 absolute 0+2+3 symmetry * → ��� .

Summary of Strong CP problem � qeuasrmomeutum for the Oacp - fixed configurations with vacuum #=o Winding number h Zueinoln > 10 > = forced introduce We to are because of ' In ) > In ±t 0 → , called thsfantoob transitions , = 382*43×1<94 42*49 '⇐GF¢5 . £ = - EFC =n+ n - ��� .

Summary of Strong CP problem � of QCD Energy vacuum .gs/h.dFays.%ad ¥5,1 e- menoii . ( 0-+942 field that " oehaees " Evacneozmoinac Like a . Superselectiom rule ' > Oofwifmutlo at -86--0 's ���

Summary of Strong CP problem � full targdetmumd SM 5=0 the In freaks CP 5 ← . it decays . Example y 't → : 02 T ~ induces EDMS importantly More , d Es Hint 5 = . |dh/ 53×1526 am Combe made dn= 0hL precise €6417 15 ��� 1<150

Solutions to Strong CP � _ small Why E is so could be When it ' ) " ? chance By I . . -0 ? du mn= J 2 * → be to . →o seems viable refntetao lattice not by , QCD parity Engineer 8=0 cousax 3. . mirror symm models ?0 energies 5=0 hzh at , Axiom solution 4 to strong CP ' ��� understand strong be to not May inter 5 we . .

Axions solve strong CP problem � Lai Laawie Laa → = + . + . ( +1782 a⇒EoEµ € + + . ( 0+afa) (a) Evac operator #dm⇒Euac= at ! Minimum of energy . fa a > < Erac ⇒ 0 to = - vae Effective theta then is < asuae Problem 0 a + = 0 eff # = solved . ��� .

Axions. Mass ~ coupling � ^aYB in Man f. ( ¥gMmMtcmpm⇒ precisely mat more substituting get numbers in we , ' 109611/4 6 mell Ma = × 9 fa " snow . disfavored ( excluded it , oy . - - Very light weakly coupled very ��� , particles

Axions. Need for UV completion � ���

Axion-like particles � ���

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