Aldo Morselli INFN, Sezione di Roma 2

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Dark Matter WGStato delle attivita'

Aldo Morselli INFN, Sezione di Roma 2
Università di Roma Tor Vergata
Milano, 1 Dic. 2004

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Items Principali in questo momento

• Studio del background
• linee ( Lionetto)

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sono quasi pronti i proceedings di Frontier
Science (500 pagine ) su http//people.roma
2.infn.it/aldo/frontier04.pdf
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Towards High Energy Astroparticle Physics
European network
In view of the
preparation of a new I3 proposal a plenary
meeting on High Energy Astroparticle Physics will
be held in  Paris December 16-17, 2004.
relevant documents concerning the preparation
of European proposals can be found on the web
                         http//crnet.in2p3.fr
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Propagation Equation for Cosmic Rays in the
Milky Way
a)Studio del background
diffusion coefficient in the impulse
space, quasi-linear MHD
convection velocity field that corresponds to
galactic wind and it has a cylindrical symmetry,
as the geometry of the galaxy. Its z-component
is the only one different from zero and increases
linearly with the distance from the galactic plane
loss term fragmentation
loss term radioactive decay
diffusion coefficient is function of rigidity
primary spectra injection index
implemented in Galprop ( Strong
Moskalenko, available on the Web)
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Propagation parameters uncertainties

• Geometrical and dynamical parameters of the
  propagation
• Pbar and Isotopes Production Cross Section ( 20
  ) and pp-gt p0 Cross Section
• Gas distribution in the galaxy
• Secondary to primary CR ratios are the most
  sensitive quantities to parameters changing B/C
  are measured with the highest statistic
• Good fits of B/C experimental data constrain
  possible variations of the unknown parameters
  consistency wit the other prim/sec CR ratios
• Standard statistical test

Heliospheric modulation z (depends on rigidity)

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Gas distribution in the galaxy
Nakanishi Sofue (2004)
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B/C Ratio Enveloping curves of all the good fits
of the experimental B/C data
B/C ratio
DC
(diffusionconvection)
(In DC problem with the ACE data at low energy)
DR and DRB
(DiffusionReacceleration) (DiffusionReaccelerati
onBreak)
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Allowed values for the propagation parameters
for DR propagation
prim spec injection index
halo size
diffusion constant
diff index
Alfven velocity
Allowed values for the propagation parameters
for DC propagation
upper diff index
injection indexes
Vc gradient
diff constant
halo size
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Allowed values for the propagation parameters
for DRB propagation
injection indexes Elt10 GV Egt10 GV
Alfven velocity
diffusion constant
diff index
halo size
Allowed values for the propagation parameters
for DC propagation
diff index Egt4GV
injection indexes Elt20GV Egt20GV
Vc gradient
diff constant
halo size
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Sub Fe/Fe
(ScTiV)/Fe spectra that corresponds to the
best fit of B/C
DC
DR and DRB
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positron spectra for DC and DRB models
DRB
DC
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Total uncertainty of antiproton fluxes and
spectra that correspond to the parameters of the
best B/C fit for DC and DRB models
DC
DRB
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new s model for pp-gt p0
T.Kamae et al. astro-ph/0410617
new s model
GALPROP with the conventional cosmic ray spectra
(Strong et al. 2004)
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EGRET data Susy models
EGRET data
Nb1.82 1021 Nc8. 51 104
Typical Nc values NFW Nc 104 Moore Nc
9 106 Isotermal Nc 3 101
Annihilation channel WW- Mc 80.3 GeV
background model(Galprop)
WIMP annihilation (DarkSusy)
Total Contribution
2 degrees around the galactic center
A.Morselli, A. Lionetto, A. Cesarini, F. Fucito,
P. Ullio, astro-ph/0211327
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GLAST Expectation Susy models
Nb1.82 1021 Nc8.51 104
Typical Nc values NFW Nc 104 Moore Nc
9 106 Isotermal Nc 3 101
2 degrees around the galactic center, 2 years
data
Annihilation channel WW- Mc 80 GeV
(Galprop)
(one example from DarkSusy)
astro-ph/0305075
A.Cesarini, F.Fucito, A.Lionetto, A.Morselli,
P.Ullio, Astroparticle Physics, 21, 267-285,
June 2004 astro-ph/0305075
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EGRET, E gt 1GeV
Mayer-Hasselwander et al, 1998
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Poin source location for GLAST 5 arcmin
1 pixel 5 arcmin
20 x 20 field IBIS/ISGRI 2040 keV
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20 x 20 field EGRET, E gt 1GeV
Poin source location for GLAST 5 arcmin
20 x 20 field IBIS/ISGRI 2040 keV
1 pixel 5 arcmin
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Estimated reaches with GLAST
Minimal Supersymmetric Standard Model with A0
0, ??gt 0, mt 174 GeV
region where 0.13 lt ?CDM?h??lt 1
region where 0.09 lt ?CDM?h??lt 0.13
GLAST sensitivity (5 s) for a neutralino density
Nc of 104 in a DW10-5 sr region around the
galactic center
if GLAST do not see Supersymmetry this region is
excluded for a NFW halo
mh0 lt114.3 GeV GeV
Typical Nc values for DW10-5 sr NFW Nc
104 Moore Nc 9 106 Isotermal Nc 3 101
A.Cesarini, F.Fucito, A.Lionetto, A.Morselli,
P.Ullio, Astroparticle Physics 21, 267-285, June
2004 astro-ph/0305075
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Estimated reaches with GLAST
Minimal Supersymmetric Standard Model with A0
0, ??gt 0, mt 174 GeV
region where 0.13 lt ?CDM?h??lt 1
region where 0.09 lt ?CDM?h??lt 0.13
GLAST sensitivity (5 s) for a neutralino density
Nc of 104 in a DW10-5 sr region around the
galactic center
if GLAST do not see Supersymmetry this region is
excluded for a NFW halo
mh0 lt114.3 GeV GeV
Typical Nc values for DW10-5 sr NFW Nc
104 Moore Nc 9 106 Isotermal Nc 3 101
A.Cesarini, F.Fucito, A.Lionetto, A.Morselli,
P.Ullio, Astroparticle Physics 21, 267-285, June
2004 astro-ph/0305075