DM annihialtion in Karlsruhe

1
DM annihialtion in Karlsruhe
Historical introduction 06.2003
Simultaneous consideration of DM annihilation
components gamma, antiprotons, positrons. Good
agreement for the NFW(1,3,1,) in DarkSusy
10.2003 Reconstruction of the DM profile from the
EGRET gamma angular distributions and GALPROP
prediction. Isothermal like profile, rings, fit
in DarkSusy. 12.2003 Implementation of DM
annihilation in GALPROP. Large
antiprotons(positrons) contribution for 'EGRET'
profile. 05.2004 Trying to reduce DM
antiprotons by GALPROP parameters, first scans.
Implimentation of anisotropic diffusion in R,
convection in z, new XCO, source distribution.
Difficulties to find solution for all components
(gamma, pb,ep) 10.2004 Start GALPROP version
with more flexible algorithms(not finished)
10.2005 GALPROP scans, trying to find a solution
with less antiprotons. 12.2005 'Boosting' of
pb annihilation in the gas to reduce CR pb. CR
pb are less than DM, but can be used as a
constraint of the gas clustering. 02.2006
L.Bergstrom at al. Realized the pb excess.
02.2006 LocalBubbleColdCloud magnetic wall.
Also affects protons. 03.2006 Cross check
GalProp, DarkSusy good agreement. 04.2006
Attempt to reduce DM pb region.Anisotropic
diffusion in Z, small box. 04. 05.2006
Todays discussion.
2
What is the problem?
Annihilation yields and fluxes for NFW(2,2,0)
Yield Ypb is the loweset Yg/Ypb30 , but
flux(and SNR) is the largest Fpb/Fg(2GeV)gt30 Ov
erestimation of DM pb flux with effective
isothermal like annihilation profile (not DM
profile)
nosolarmod
Factor of 100 !
3
Why?
Propagation efficiency of charges in diffusion
model is very high. Gamma F1/4p
Collection distance (99) for CR species
Heavier CR -gt smaller collection distance
(Diffp/z) B/C, Be are from 2 kpc
Diffusion only smears source function! Fragmentati
on losses are small lt10 Escapes only from the
box boundaries
Gas


DM clump propagation efficiency in the Galactic
plane F R 2
CR sources
4
Can the propagation efficiency be changed?
The DM profile and Gas/Source distributions for
CR are at the same places (almost)
Gas
Sources
DM
The DM antiprotons does not differe from CR
'Free' propagation parameters D,Z(zsqrt(Dt)),
Va, Vc...
-gt Will affect all CR species! Changes in
antiprotons will cause inavoidable changes in all
secondaries B, Be, Al, etc. Have to look not
only on ratios (B/C, Be19/Be9,) but also absolute
fluxes! To restore secondaries -gt change
injection of primary mothers. But injection is
fixed by data (FmeasFinjDiff) if Diff. is
fixed. (Same valid for the LocalBubble
effects) Problem just moved to the primaries,
etc.
CR primaries p, CNO...
DM ann.
propagation
CR secondaries pb, B,Be,...
DM pb
Can not decouple dmpb propagation from other
species.
5
Change the collection areas.
Free propagation parameters D,Z, Va, Vc Can we
use the D,Z degeneracy? In ideal case uniform
leaky box zsqrt(D t), can reduce the Z without
changing most of CR parameters
CR chi2 of exp.data D-Z scans
gamma
B/C
DM halo
Initial box
Small box
protons
Can reduce collection area from DM. But in
reality Z2 not D due to - nonuniform
gas/source distribution - non linearity for
narrow boxes when Dgtgtz Not trivial to get
solution.
fBe
pb
fep
Be10/Be9 breaks degeneracy since t Will be the
main problem.
6
Change the collection area
How much we can gain? Use the 'EGRET' DM
profile, slice it in r,z Contribution to the
local spectrum from different DM components.
Local region r(/-2kpc), z(/-0.5 kpc)
gamma15 pb30 (need 1!) Can be not enough!
The Be10/Be9 problem can be worser.
Gamma angular profile latitudinal profiles are
wrong Has to introduce larger box- 2- zone
diffusion etc. Need to take into account escaping
particles, or convection zone. Not done in
GALPROP.
Typical decay length Be10 300 pc, size of
LocalBubble where is no gas-gt free decay of
unstable -gt Be10/Be9 even smaller! All short
lived isotopes are smaller. Not in GALPROP.
Small Z
Z , kpc
7
Reducing DM pb
It is not trivial to get solution with the small
collection zone. The diffusion Galactic model
(not only Galprop, also Annecy group) is very
constrained (within 20), especially for
secondaries(B/C). Complications (spiral arms,
anisotropies, etc) still not decouple DMpb from
CR. What else? - Relax the DM profile -gt
probably bad idea, loose main observation (rotatio
n curves and gamma angular correlations) Which
freedom we have to reduce the local DM density?
(NFW(1,3,1) profile is OK!) - Select another DM
candidate. But to get continious gamma needs
jets. i.e Ypb/Yg 0.03 holds. Some exotics with
extra gamma production..? -