EPS 2003, Aachen, 17. Juli, 2003 Outlinedeboer/html/Talks/talk_eps2003.pdf · Halo Models Halo models 10-2 10-1 1 10 0 2 4 6 8 10 12 14 16 18 20 Radius [kpc] ρ CDM [GeV cm-3] DB4d

A Global Fit of Super symmetric Dark Matterto the Flux es of Galactic Positr ons, Antipr otons and Gamma Rays

or

Is Dark Matter Super symmetric?

Wim de Boer

IEKP, Univer sity Karlsruhe

Wim.de [email protected] h http://home .cern.c h/˜deboe rw

EPS 2003, Aachen, 17. Juli, 2003

OutlineProblems with galactic models?

What if we inc lude Dark Matter?

Predictions from Minimal Super symmetr y

Global Fits to Gammas, Antipr otons and Positr ons

Summar yW. de Boer Aachen, Juli, 2003 1

Model of our Galaxy

Primar y par tic les by superno vae explosions, pulsar s, ...

Secondar y par tic les nuclear interactions.

Diffusion parameter s determined from sec./prim. ratios, e.g. B/C ratio

Halo size determined from radioactive isotopes, e.g

ratio(

yr)

Best diffusion parameter s for nuclear spectra yield:too few hard gammas, too few antipr otons and too few hard positr ons!

W. de Boer Aachen, Juli, 2003 2

Diffuse contin uum gamma rays from the GalaxyA. W. Strong (MPE), I. V. Moskalenk o (NASA), O. Reimer (MPE)Astr oph ys.J . 537 (2000) 763-784; Erratum-ibid. 541 (2000) 1109

Models based on locall y measured electr on and nucleon spectra andsync hrotr on constraints are consistent with gamma-ra y measurements in

the 30-500 MeV rang e, but outside this rang e excesses are apparent...Possib le solutions: local hard electr on or hadr on component...

x x

Challenging cosmic ray propagation with antipr otons. Evidence for a“fresh” nuclei component?

Author s: I. V. Moskalenk o (NASA), A. W. Strong (MPE), S. G. Mashnik(LANL), J. F. Ormes (NASA);

Astr oph ys.J . 586 (2003) 1050-1066

Matching both the secondar y to primar y nuclei ratio and the antipr otonflux requires artificial breaks in the diffusion coefficient and the primar yinjection spectrum sug gesting the need for other appr oaches. Using the

measured antipr oton flux AND B/C ratio to fix the diffusion coefficient, wesho w that the spectra of primar y nuclei in the heliosphere may contain a

fresh local “unpr ocessed” component in the Local Bubb le...


Nuclear Abundance in our Univer se

1

10

100

1000

5 10 15 20 25

Rel

ativ

e ab

unda

nces

(O

=10

3 )

Nucleus charge, Z

42.2–111347

Elemental abundancesat 7.5 GeV/nucleon

CalculationsΙ HEAO-3

Φ = 800 MV

Ratio of radioactive/non-radioacti ve isotopes fix es halosiz e to

4 kpc.


B/C and Antipr otons in our Univer se

0

0.1

0.2

0.3

0.4

0.01 0.1 1 10 100 1000

Kinetic energy, GeV/nucleon

B/C

Phi = 450 MV

Voyager

Ulysses

ACE

HEAO-3

0.001

0.01

0.1

0.1 1 10

Flu

x, 1

/(m

^2 s

sr

GeV

)

Kinetic energy, GeV

ANTIPROTONS

Phi = 550 MVBESS 95-97

MASS91

CAPRICE98

Tertiary

B/C fix es diffusion, whic h yields too few antipr otons.


Gamma Rays and Positr on Fraction

0.5<l< 30.0 , 330.0<l<359.0

-5.0<b< 5.0

10-3

10-2

10-1

1

1 10 102

positron energy [GeV]

e+ /(e+ +

e- )

frac

tion

b b–

τ+ τ-

bg+175•signal χ2=25.1

bg (ep-scaling=0.86)

bg only fit χ2=48.0

HEAT 94/95/2000

AMS 01

tanβ=50; m0= 500; m1/2= 500

B/C fix es diffusion, whic h yields too few hard gamma rays and too few hard positr ons.


Is DM supersymmetr ic?

SUSY:Unif icat ionElectroweak SBNeutralino Annihilat ion

Cosmology:Inf lat ionAcoust ic PeaksDark Matter

Electroweak Data LEP H iggs limitsAnomalous Magnet ic Momentb−>s gamma

Astrophysics:B/C rat io, nucleiAnt iprotonsPositronsGammas

Nuclear Interact. and Galaxy propagation: GALPROP (Moskalenk o,Str ongNeutrino Annihilation: DarkSusy: Edsj o, Ullio, Bergstr om


mSUGRA Spar tic le Spectrum

From RGE equations:

0

200

400

600

800

1000

0 2 4 6 8 10 12 14 16 18

log10(Q/GeV)

mas

ses

[GeV

]

g~

w~

b~

m1

m2

τ~

r

τ~

l

t~

r,b~

l,r

t~

l

m0

m1/2

√m02+µ2

Characteristic MSSM Features:Squarks and gluinos heavy thr oughstr ong rad. corr .Gaugino from U(1) (=Bino) LightestNeutral SUSY Partic le (LSP)(if not too large w.r.t. )Mass terms in Higgs potential drivennegative by Yukawa couplings

EWSB(determines )Higgs mixing parameter usuall y largecompared with

Consequentl y:Pseudoscalar Higgs and hig gsinosheavy

light Higgs SM-hig gs-likeLSP bino-like , since no mixing withheavy hig gsinos

very good DARKMATTER candidate


Relic Density

! "

#%$& ' () # $& ' )

250

500

750

1000

250 500 750 1000m0

m1/

2

Neutralino not LSP

tachyonic particle

mh < 114.6 GeV

250

500

750

1000

250 500 750 1000m0

m1/

2

Neutralino not LSP

tachyonic particle

mh < 114.6 GeV

Ω h 2=0.113(8)

Light blue regions pref erred by WMAP*+ , - . /0 - *1 , 243 5

for

687 9 : ; <=

(if no coannih.)


Main Diagrams for Neutralino Annihilation

>?@

@

A??

BC

C

DEE

FG

G

HII

J KL M KNK OPN J QRS T M KNVUKW X KLKY Z []\_^ \a` bc degfh i4j kl U m KN%nQR S T J KN M KLK Oo \ [` bc d

p qsrp

p

t qtu

vwv

v

xx

J ^^ y b KzL | ~ KL d O4 b KW ~ KL d O ka | k m k | k

To Note: Dominant diagrams Fermionmass squared(Light fermion pair s suppressed dueto Pauli-Principle) for

#%$& ' ) quark pair s domina-

te, since Higgs exchang e suppres-sed for top quarks at large

#%$& ' )

Interf erences enhance in additionb-quarks over t-quarks(Z-t-channel negative and A-t-channel positive interf erence)


Helicity suppression for light final states

at low neutralino momenta

g

¡ ¢

£ ¤£

¦¥ £¥ £

££

§ ¨©ª «

¬ ®

¯ ° ¯ °²± ³ ´³

µ¶ ·¶ ¸¶¹zº» ¼

½ ¶¾ ¿½ ¶¾ µ

¶ÁÀ ¶ ½¶ À ½

½½ ¶

Â ÃÄÅÆ

ÇÉÈÊÌË ÍÎË Ï

) Ð ÑÓÒ Ô ( ) ÕÖ Ð ÑÒ ×ÙØ Ú () Ð ÑÒ ×ÜÛ Ú Ð Ñ


Pseudoscalar Higgs exchang e vs

Ý²Þ ß

à à × à à × Ô Ô

á âäã á âÌå æå ç è ç

éê ëê ìVíî ï

ð ê ñð ê òó ôõ

ö ÷ ø ùûú ø ùü ýü þ ÿþ

à à × dominates at large

#%$& '

.


Annihilation Contr . to Gammas

10-5

10-4

10-1

1 10E [GeV]

E2 *

flux

[GeV

cm

-2 s

-1sr

-1]

EGRETbackgroundsignalbg + sig

Boostfaktor: 1.1χ2: 7.3/6χ2 (bg only): 34.5/7

m0 = 500 GeVm1/2 = 350 GeVtan β = 50

bb-

mχ = 143.7 GeV

250

500

750

1000

250500

7501000

0200400600800

100012001400160018002000

m 0

[GeV]m

1/2 [GeV]bo

ost γ

! " " #%$ & '( () * !,+ ! à -/.10 2 " 34 à -/.10 567 78 4 + 2 39


Annihilation Contr . to Positr ons and Antipr otons

10-3

10-2

10-1

1

10-1

1 10 102

E [GeV]

e+/(

e :++

e- )

HEAT 94 / 95 / 00AMS01backgroundsignalbg + sig

Boostfaktor: 1.5χ2: 20/17χ2 (bg only): 59.4/18

m0 = 500 GeVm1/2 = 350 GeVtan β = 50

bb-

mχ = 143.7 GeV

10-8

10-7

10-6

10-1

1 10 102

E [GeV]

p- flux

[cm

-2G

eV-1

s-1sr

-1]

BESS 95/97backgroundsignalbg + sig

Boostfaktor: 1χ2: 6.5/12χ2 (bg only): 27.4/13

m0 = 500 GeVm1/2 = 350 GeVtan β = 50

bb-

mχ = 143.7 GeV

! " " # $ & <; = - 2


Halo Models

Halo models

10-2

10-1

1

10

0 2 4 6 8 10 12 14 16 18 20Radius [kpc]

ρ CD

M [G

eV c

m-3

]

DB4dCRMDB2fDB2dKbSpour model

To Note:Spherical symmetric halo profile (Navar-ro, Frenk, White):

> ?A@ B >C D ? @E BF G HJI K ? @E BL M NO PQ +

We put

R, S I

and T I + U

fora scale E R

kpc. The density > C is ad-justed suc h that the local halo density isin the rang e 0.1-0.7 GeV/cm

V

, as requiredby the rotation cur ve of our galaxy . Notethat the local density is str ongl y correla-ted with halo parameter s, so in the fit thehaloparameter s are fix ed and onl y >C isvaried.


Direct WIMP Detection

030716050600

http://dmtools.berkeley.edu/ Gaitskell&Mandic

101

102

103

10−42

10−40

10−38

10−36

WIMP Mass [GeV]

Cro

ss−

se

ctio

n [

cm2]

(no

rma

lise

d t

o n

ucle

on

)

UKDMC

NAIAD

spin− dependent

χ

m =144GeVχ

m =295GeV

030716050101

http://dmtools.berkeley.edu/ Gaitskell&Mandic

101

102

103

10−45

10−44

10−43

10−42

10−41

10−40

WIMP Mass [GeV]

Cro

ss−

se

ctio

n [cm2] (n

orm

alise

d to

nu

cle

on

)

DAMA I

EDELWEISS I

ZEPLIN 4

spin− independent

ZEPLIN I

CRESST 2

EDELWEISS 2 χ

χ

m =144GeV

m =295GeV

experimental limits

projections


Summar y: what is new?

W Simultaneous fit to antipr otons, positr ons and gammas using Dark-Susy modified to sim ulate backgr ounds and diffusion model fromGALPROP (DS has no diffusive reacceleration!)W Not scanned over MSSM parameter s, but taken appr oximatel y lo-west neutralino mass consistent with WMAP and electr oweak cons-traints, i.e. LSP X Y Z[

GeV, whic h yields “boost factor s” for ALLflux es of order unity .LSP < 300 GeV, if boost factor s required to be belo w 10.

W No freedom in neutralino annhilation, since

\ \final state dominates

in CMSSMW Is Dark Matter super symmetric?Much discussed “Local Bubb le”, fresh components, hard (but un-kno wn) components of electr ons and/or nuclei, unph ysical breaksin diffusion coeff . etc. are much less appealing then Dark Matter an-nihilation, whic h is the ONLY explanation sofar to fix Galaxy Modelproblems SIMULTANEOUSLY.W Including Neutralino annihilation impr oves probability of global fitfrom

Z^] Y [ _ `to 0.53 (about 6 a)


Documents

EPS 2003, Aachen, 17. Juli, 2003 Outlinedeboer/html/Talks/talk_eps2003.pdf · Halo Models Halo models 10-2 10-1 1 10 0 2 4 6 8 10 12 14 16 18 20 Radius [kpc] ρ CDM [GeV cm-3] DB4d