DM M Sear earch C ch Compl omplem ement entarity E Empl - - PowerPoint PPT Presentation
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.
1
Cahill ill-Row
ey,
Cotta tta, , A. D . Drlic ica-Wagner gner, S.
Funk, , J. . Gain iner, J. Hewett tt, , A. I . Ismail il, ,
Wood,
G.R. R.
5/ 5/25 25/15 15
.
2
3
188 ± 0.0010 010 (why hy?) ?)
eutral al’, color
nglet et
non-rel elat ativistic during ng struc uctur ure for
now too)
At most weakly-int nter erac acting ng w/ SM ←
baryoni
ery lon
ed ≈ stabl able
Self-ints. are e cons nstraine ned
d be com
plex ex
The usual ual ν’s ar are e hot hot ↔ ∑ mν < ~ ~ 0. 0.25 25 eV eV X
Heav eavy neut neutrinos
→ via the Z.. many orders of magnitude too large !
4
e don don’t kno now if the he SM & DM tal alk to
each ot
her non non-gr grav avitat ational
thi his is an an assum umpt ption(
pe)…ot
herwise e we’re e sunk unk (or not not….) ..and and the he list kee eeps gr growing !
Of c cour
DM may ay be be made of ade of m many any differ erent nt compon
ents--
jus ust one
T.T T.Tait
5
<σv> > ≈ 2. 2.8 x 8 x 10 10-26 cm cm3 sec c -1
1 → MDM DM ~ 0.
0.1-1 T 1 TeV eV f for E
ngs !
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In real ality this ‘relat ations
hip’ p’ is not not so
“SM” may ay be be di different in n the differ eren ent direc ection
Ther ere are e sev ever eral al ways to des describe the he ins nside of
he bl blob
EFTs, Simpl plified ed Model dels, or UV compl plet ete e scenar enarios
each with h thei heir
n good
d aspec pects
7
Tim im T Tait it
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ll SM par particles hav have e SUSY spa partners wit ith spin pin of
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
his tal alk this his is the he ligh lightest neut neutralino (next t slide) de)
is br brok
by a a lar large set et of
ass ter erms (~10 100!) gene generated in in som
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
be agno agnostic.. Try t to be unpr
Bino,
gsinos nos mix when en SUSY is brok
en..the he lightes est can an be the LSP
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ut w wai ait! Isn’ n’t S SUSY dead dead ?? ?? Does
he lac ack of
any appar apparent sig igns o
SUSY at the L LHC HC im imply ly t that t there is is no SUSY SUSY and/ and/or the he mot
n for
SUSY has has been l been los
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
the he SM coupl
gs t to
unify’ at at a a hi high gh scal ale (iii) I It hel helps ps to
educe t the he fine ne-tun uning ng ( (FT FT) & hi hier erar archy pr probl
nly her here i e is ther here s som
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
any signal gnal FT FT inc ncrea eases es ?
muc uch FT h FT is too
uch? We’ll hav have t e to
at thes hese s e sear earche hes mor
e critically
11
In n SUSY, t the S he SM gauge c gauge coupl
ngs UNI UNIFY near near ~ ~10 1016
16 GeV
V but but t thi his does does not not happen happen if w we e onl
have t e the he SM SM p partic icle les. .
Energy gy ( (GeV) V) 1019 1016 103 10-18 Solar S Syst ystem Gravity ty Weak ak GUT UT Pla Planck desert
LHC HC All o ll of know nown ph physics
δmH
2 ~
~ αMPl
Pl 2
δmH
2 ~
~ -αMPl
Pl 2
bo boson fermi mion
~ ~ α|M2
boson – M2 fer ermion | log
PL /mH)
) Lar Large quadr adrat atic loop p effec ects canc ncel el
der by order der bet between the he fer ermions & bos bosons in n PT lea eaving onl
he log
terms… … →→ this canc ncel ellat ation
ed as the he mas ass spl plitting gr grows
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→→ Neutralinos right out of the box with arbitrary masses do NO NOT gi give t the he righ ght r rel elic dens density
inos don’ don’t anni annihilate enou enough.. wino inos & Higg iggsinos too
uch h unle unless they hey ar are e ~3( 3(1) 1) TeV eV
inos need need to
annihilate thr hru u a funnel/resonance (Z,h,..) or via ia a a co-anni annihi hilati ation
ess wit ith anot anothe her near nearby spar particle
arious adm admix ixtures of
ates wil ill als also wor
if the he mas asses & mix ixings ar are e pr prop
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
using ng the pM he pMSSM !!
Baer aer
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The p(
eneral CP CP-cons
erving ng MSS MSSM wi with h R-pari parity
V at the he TeV eV s scal ale (F (Flav avor
M)
Light ghtes est neut neutral ralino
he LS LSP.
st/2
/2nd generat generation s
ermion
degenerate e
gnore 1st
st/2
/2nd generat generation A
erms & &Yukawa’ wa’s. .
No as assumpt ption
wrt SUSY SY-br brea eaking ng
he neutral ralino no not not nec neces essar arily the he onl
DM
the he pMSSM SSM wit with 19 19 param amet eter ers
50 GeV ≤ |M1| ≤ 4 TeV 100 GeV ≤ |M2, μ| ≤ 4 TeV 400 GeV ≤ M3 ≤ 4 TeV 1 ≤ tan β ≤ 60 100 GeV ≤ MA, l, e ≤ 4 TeV 400 GeV ≤ q1, u1, d1 ≤ 4 TeV 200 GeV ≤ q3, u3, d3 ≤ 4 TeV |At,b,τ| ≤ 4 TeV
‘Thr
Throw
darts’ int nto t
his s spac pace.. l look
at the v he var ariou
predi ediction
hen k keep eep poi point nts t tha hat s sur urvive al e all cons
& study dy t them em Sev ever eral s studi udies es..
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←Planck
Rel elic den density con
atisfied but but mos
e far ar bel below it
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Bino annihilation through h/Z funnels Bino c no co-an anni nihilat ation
Wel ell-tem empered ed neut neutral alino no heav heavy wino 1 1 TeV eV H Higgs ggsino no H/A r reson
ant a annihi hilat ations ns
L E P
N O T H I N G
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f-o now now
pMSSM SSM Scales up up & dow down w n with th Higgs ggsino con
tent
60 50 45 5 40 30 70 70
Z
f-o
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LEP EP Bo Bound
Clear early LSP masses es below
~30 30 GeV eV woul
be exclud uded ed IF we e sat aturate the he rel elic den density
ie below it
Inc ncreas asing g rel elic dens density
↑ !
19
Com
plem ement entar arity: We
e need need many any ex exper periments t to
er t thi his lar arge par ge param ameter er s spac pace & & under understand nd any any di discov
e can an find LS nd LSPs ev even i en if they hey don’ don’t mak ake e up up al all the D he DM ! !
7/8 T TeV eV LH LHC MET ET & & non non-ME MET → 13/ 13/4 T TeV eV
CE3
3
nations
What do do thes hese dif different exper eriments ents say about ut the he LS LSP & the he pM pMSSM in in gene general ? What What par param ameter rang anges do
hey pr probe
What happe happens when hen they hey ar are e com
→ We take these each in turn..
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The LH LHC (her here A ATLA TLAS) has has per performed ed num numer erous us S SUSY searche hes and w and we e can us an use t e the he pM pMSSM to c
ne them hem & iden dentify any any par parameter s spac pace hol e holes es & & sear earch c h cav avea eats
There e hav have been 2 e been 2 studi udies es @ 8 8 TeV TeV : : by by us & AT & ATLAS AS it itself…
enerate ~few ew 10 105 pts in n pM pMSSM space OK with h al all ot
her con
Gener nerate e MC ‘event ents’ for eac ach pt pt & run un the hem thr hru SUSY & relat ated ed sear earche hes & see e which h sur urvive e or are kill lled CPU PU intensive ! ~1014
4 evts
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Our
ur A Anal nalyses
ATLA
TLAS A Anal nalyses es Cer ertai ainl nly A ATLA TLAS c can an per perform t thei heir
n analyses es bette tter than w han we e can an but but t the he res esults are quit ite s sim imila ilar given t en the he sligh ghtly di differen ent assum umptions ns m made ade
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quarks & & gl glui uinos nos c can an be be light ghter t than i han indi ndicated ed by by the s he simpl plified m d model
analyses
This i is one
any suc uch h exampl ples es:
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24
25
8 TeV V ATLAS S SUSY USY sear arches hes impa pact ct on DM M most
at l low
LSP masse asses
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SI DD is extremel ely power erful ul over er much of the par aram ameter er spac ace e (as as we’ e’ll see ee) but but SD has has a a bi bit les ess impac pact due e to smal aller er σ’s pred edicted ed
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Xen enon 2011 2011 Xen enon 2012 2012 LUX UX Xenon 1 non 1T LZ ν ‘F ‘Flo loor’
Many ny model dels with h ‘pur ure’ e’ state e χ ‘s ‘s pre redict low ra rates
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LZ SD
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entiona nally, I IDM s sear earches es as assume t e tha hat WIMPs anni annihi hilate int nto onl
nal s state & quot quote a a cros
sec ection l n limit bas based on ed on the c e cor
ding f g flux ux l limit
FERMI
ever er in n the pM he pMSSM the he LSP p SP propertie ies & & SUSY m SUSY mass spec pectra ar are e mor
e com
so
hat m mul ultipl ple f e final nal s states will cont
e to
he γ flu lux
Thus t the he flux ux l limit itself lf is t the he quant quantity of
int nter erest & & mus ust be be cal alcul ulated ed f for
each model
30
31
The FE FERMI D Dwar arfs ar are e jus ust begi beginni nning ng t to
probe t
his s set et of
model
TA @ 5 5 yrs w will hav have ac e acces ess to a a reas easonab able f e fraction
thes ese m model
FERMI FERMI CTA ~18. 18.8%
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mi (Dwarfs) sensitive to
bino no-Higgsino adm admixtures and and a a few ew bi bino no- li like LSPs SPs that co-an anni nihi hilat ate
A (GC) sens ensitive e to heav avy winos nos and d Higgs ggsinos nos, many ny bino no-Higg ggsino no adm admixtures and and a a few ew bi bino nos.
dels with res esonan
anni nihi hilat ations
e very low pres esent nt-day day anni nihi hilat ation
ates & ar are mos
not ac accessible
Fermi CTA
* Extension of previous analysis w/ KIPAC- FERMI on Dwarfs
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ept up up by by the s he sun un can an col
ect & & then hen pai pair-an anni nihi hilat ate i e in the s he sol
ar cor
thus hus pr produ
g hi high gh-E neut neutrinos from t the dec he decay ay
the he cor
pondi ding anni g annihi hilation pr produ
gain, n, s sinc nce t e the LS he LSP pr prope
pectra var ary w widel dely in n the pM he pMSSM t the pot he poten ential al f flux ux mus ust be be cal alcul ulated ed for
each h model
eparatel ely & & then c hen com
pared w d with t h the he ex expec pected ed limit
not l leadi eading ng t to an
equilibr brium i in n capt apture/an annihi hilation n rate f e for
DM in n the s he sun un (the ~ e ~ 47% 47% !) ar are e not not w wel ell-pr probe bed by d by IC ICE3 . It is is mostly ly mix ixed b bin ino-Higgs gsino LS
bina nation
that ar are v e visibl ble & & thes hese e hav have l e lar arge ge r rel elic dens densities.
34
c/o R
andy C Cot
35
1601. 1601.006 0653
ICE CE3
3 probes
bes inter eres esti ting ng range e of DM mas asses but but is is som
ewhat sens ensitive to t
he nat natur ure of
the S he SM fina inal as as w well ell as as equi equilibrium bein being reac eached in in the he sun un
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~ ~ fe few % %
FERMI+CTA LZ CO COUP UPP 5 500
WMAP satur urated ed red=bino, no, b bl=wino gr = Higgs gsino no , , magent enta= a=highl ghly m mixed
→ → →
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38
39
40
41
42
Bino annihilation through h/Z funnels Bino c no co-an anni nihilat ation
Wel ell-tem empered ed neut neutral alino no heav eavy wino 1 1 TeV eV H Higgs ggsino no H/A anni nihi hilat ation
43
Wel ell-tem empered ed neut neutral alino no heav eavy wino 1 1 TeV eV H Higgs ggsino no H/A anni nihi hilat ation
Bino c no co-an anni nihilat ation
Bino annihilation through h/Z funnels
44
Of cou
he LH LHC is now now run unning at at highe her ener ergies es..cons
aini ning ng scena enarios
com
n from
he low
de.. The he LH LHC itself will ne never get get to
1.6-2 2 TeV V LSPs SPs → 100 TeV ??
45
1 @ 14
Onl nly co-an anni nihi hilat ating ng or lucky funnel nel binos
emai ain n at ful ull rel elic den density…
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DD = LZ both SI + SD ID = FERMI + CTA 11. 11.4% 4% 29. 29.2% 2% 7. 7.2% 2% 27. 27.5% 5% 24. 24.7% 7%
47
1 @ 14 T
48
Thermal al WIMP DM rem emains ns an an at attractive s e scena enario . .. but but there ar e are e now now many any c com
petitors
There ar e are e sev ever eral appr approac aches es t to
describe be D DM phy physics: EF EFTs, Sim Simpli lifie ied M Models ls & & UV UV-comple lete p pic ictures a all ll wit with pl plus uses es & & minus nuses.
The pM pMSSM pr prov
des a a flex exibl ble pl e plat atform f for
entarity studi dies es
ultiple ex e exper perimen ents can an be be com
bine ned t d to
probe
even en sub ub-Planck d ck density W y WIMPs.
uch of h of the par he param ameter s spac pace will be c be cov
ered d by by pl planned anned ex exper periments.
ully w we e will di discov
DM s soon !
49
50
The pM pMSSM al allow
for
a systematic & & com
ehen ensive survey ey of
he cons
aints on
The pMSSM i is a a val aluabl uable tool
for
all kinds nds of
exper periments: collid lider, DM DM & f & fla lavor
The pMSSM c can gener an generate ‘ ‘coun
exam amples es’ t to t
he us usual ual sea earches es t tha hat ar are us e usef eful ul f for
fut uture s e stud udies
The pM pMSSM teac eaches es us us about about c com
entar arity & & the he man any differ erent ent ways t to a acces ess S SUSY
51
The ther hermal al W WIMP v val alue of ue of <σv> + unitarity constraints (s (s-wav ave!) pl plac aces es an an upper upper l limit on
he DM mas ass of
120 TeV
eutralinos
do not not i int nter eract ‘stron
gly’ aw away ay f from res esona nanc nces so th the ma mass l limi mit i t is mo more re re restrictive.
eld ef effec ects al allow
nos up up to
TeV (1601.04718)
601.04718)
bey beyond
he r reac each of
the he LH LHC but but ac acces essible t e to
TA
To ac acces ess t thi his mas ass r range ange at at a c a col
der we e need a need a hi higher gher ener energy gy m mac achi hine ne
Kamionk
& & Grie iest st ‘90 90
52
uch of
he LH LHC sen ensitivity to
he LS LSP rel elies on
ascade dec decays from squarks and and gl glui
all the he col
ates ar are hea heavy & we e nee need to
es are e ver ery smal all & we need ed a ~100 00 TeV mac achi hine ne to cover this pos
earch h type pe depend pends on the mass splitting w/ the NLSP SP, etc. .
e.g.
: 151 510. 0.03 03460, 1511.064 6495 95, 1 1605.00658
53
54
~2% 2%
→ FERMI+CTA → CO COUP UPP → LZ
55
56
57
58
59
~61% 61% of
exclud uded
60
61
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Thi his ar arises due due to,
e.g. g., the LSP’ SP’s EW EWK K nature, differ erent nt up up & dow down squ quark masses es which h happe ppens ns very infreq equent uently in n the he CMSSM as as wel ell as as from
ggs exchan hanges ges..som
ariat ation
n the he pM pMSSM.
Rem emem ember er thi his is a a log
plot
63
The S The SI c cros
ection i is sens ensitive e to t
he NLS LSP-LSP m P mass spl plitting ng whi hich al h also pr
he LS LSP E EWK c cont
Higgs ggsino
win wino bi bino no
64
0 LSP
65
~23% 3% ~2 ~2%
SD & SI SI DD s DD searches bot both pr probe
regi egions
he pMSSM pa param ameter s spac pace e
The pot poten ential al c cov
erage i e is qui quite signi gnifican ant for
SI sear earche hes bu but l les ess so
n the S he SDcas ase
66
qχ→ qχ χχ→ qq qq qq qq → χχ Snow nowmass 2013 2013
67
SUSY SUSY
pMSSM SM MSSM SSM N= N=1
mSUGRA RA NMSSM SM
Dira rac gaugi ginos nos singl glinos nos
U(1)’ )’
SUSY SY is not not a s singl ngle e model
but a a ver ery lar large ge theor
etical al framewor
68
pM pMSS SSM mode
go qui quite dee deep in n ter terms of SI
sec ections
LU LUX-Zeplin
~50% 50%
Energy gy ( (GeV) V) 1019 1016 103 10-18 Solar S Syst ystem Gravity ty Weak ak GUT UT Pla Planck dese sert
LHC HC All o ll of know nown ph physics
δmH
2 ~
~α MPl
Pl 2
Quant antum um Correc ections
Loop
ects will want nt to ‘drag’ ag’ the he Higg ggs mas ass up up to nea near ~ MPl
Pl
But ut in n SUSY for
every par particle in n the he loop
here’s al also a a spa particle so…
70
ublic D DM codes
(eg, eg, m microM
arkSUSY) ar are e missing ng s som
e impor portan ant i ingr ngred edients f for
both anni annihi hilation
and DD suc uch as h as Som
eld ef d effects as as wel ell as as impor portan ant QCD & EWK l loop
for
both al almos
pure e states es as as wel ell as as in bl n blind di nd direc ections ns
Local al D DM flux ux unc uncer ertainties
71
72
SM
Medi
diat ator
Da
Dark Sector
ediators ar are e ‘heav heavy’ t they hey c can an be be ‘int ntegrated ed’ out
to
produc
hi higher gher di dimens ension oper n operators l link nking t ng the D he DM to
he SM
ere e 5 → 2 parameters : the D he DM mas ass & & the s he scal ale, Λ. What hat coul
d be simpl pler?
Z’ q χ χ q
73
FTs allo llow t w the ‘SM ‘SM’ ’ (as w wel ell as as t the i he int nteg egrated ed out
ediators) to be be ‘any anything’ g’ inc nclud uding g lept ptons ns, , quar quarks, , gl gluons uons, , W/Z and/ and/or
Hig Higgs
The DM can be an be spi pin-0, ½ ½, 1, 1,… w with h pos possibl bly i indef ndefinite par e parity
e down n all ll oper
ever er-inc ncreas asing ng di dimens ension
e.g.,
1009.0008 9.0008
Tw Two
ampl ples of
any l long
!
1210.0525 0.0525
Lot
74
hile E e EFTs FTs can an ‘al alway ays’ be be us used ed in n DD ex expt pts, t they hey ar are e ‘most stly’ y’ inap napplicabl ble at at t the LH he LHC unl unles ess t the he medi ediator m mas ass i is >~TeV’ V’s
for
unles ess t the he medi ediator i is muc uch heav h heavier t than t han the D he DM or
the S e SM anni annihi hilation
produc
Thi his has has pr prom
d the he mov
e to
plified ed Model
at the LH he LHC t to
hat t thes hese cros
com
parison
can be an be made c ade cor
But ut be be car areful ul of
gauge inv nvar arian ance ! !! They hey A ARE, how howev ever, l les ess gener general al
75
Using ng a simplified model (e.g., the Z’ above) we can n trans nslat ate e LHC sear arches hes for BO BOTH DM & & the he med ediators (lef eft) ont
he DD DD pl plan ane for
both SI SI & & SD SD inter eractions
below
ate e the relic ic den
en we can n compar are e with ID res esul ults from, e.g., FER ERMI. But ut doe does the he simplified model del real ally capt ptur ure all the he UV mod
physics? UV theo heories ar are rat ather comp mplex with lot
parts!
76
DM has has non non-gr gravitational al i int nterac actions ns w with h the S he SM it may ay be be pos possibl ble to s
earch f for
in n mul ultiple w way ays Not
all DM scena enarios
allow
com
entar arity (e.g .g., ., ax axions
but but ot
hers do do (e.g .g., ., WIMP IMPs)
plemen entar arity requi equires es a a theo heoretical al f framework t to
elat ate var arious s sear earche hes : :
SM
Medi
diat ator
Da
Dark Sector
77
FT’s ar are e ‘model
depe pend nden ent’ & & hav have onl e only 2 2 par param ameter ers. Man any pos possibi bilities es & & no no reas eason
to
pref efer any any par particular one.
Li Limited appl d applicabi bility es espec pecially at at lar arge m ge mom
trans nsfers bu but t they hey A ARE int nter eresting ng & & us usef eful.
UV-complete model
are ‘ e ‘real eal wor
d’ s scena enarios but but hav have l e lot
ngred edients & & par parameters m mak aking ng det detai ailed ex d exam amina nation n di difficul
How
ever er, t they hey ar are al e alway ays w widel dely appl applicable.
plified m d model
are e bet better behav behaved ed, hav have a e a few ew par parameters & ar are w e widel dely appl applicabl ble e but but can hav an have gauge i e gauge inv nvar arianc nce & uni unitarity i issues ues. The They f freq eque uently don’ don’t c capt apture al all of
the he phy physics of
he real eal UV-theo heory. Bal alanc nced? d?
78
79
We c e can an al also mak make an an educat ucated ed guess ess at the LHC pMS pMSSM c cov
for
both 0. 0.3 3 & & 3 3 ab ab-1 …
300 pb 300 pb-1 3 3 ab-1
LZ reaches on SI and SD cross- sections for LSP masses below ~80 GeV can be combined to exclude/discover all models (except 1 stau coannihilator) Need annihilation through the Z/h
couplings give SI cross-section, while the Zχχ couplings give SD interactions. mLSP < 80 GeV
Uncons nstrai ained ed Regi gion
81
ICE CE3
3 Proj
Alter ernative S Sear earch P h Planes anes