Search for Dark Matter with GLAST

1
Search for Dark Matter with GLAST

Aldo Morselli INFN, Sezione di Roma 2
Università di Roma Tor Vergata
2
Neutralino WIMPs
Assume c present in the galactic halo c is
its own antiparticle gt can annihilate in
galactic halo producing gamma-rays, antiprotons,
positrons. Antimatter not produced in large
quantities through standard processes (secondary
production through p p --gt p X) So, any
extra contribution from exotic sources (c c
annihilation) is an interesting signature ie c
c --gt p X Produced from (e. g.) c c --gt q /
g / gauge boson / Higgs boson and subsequent
decay and/ or hadronisation.
3
Propagation Equation for Cosmic Rays in the
Milky Way
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)
4
Propagation parameters uncertainties

• Geometrical and dynamical parameters of the
  propagation
• Pbar and Isotopes Production Cross Section ( 20
  )
• 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)

5
Enveloping curves ofall the good fitsof the
experimental B/C data
B/C ratio
DC
Dashed line Best fit
DR diffusion reacceleration DC
diffusionconvection
In DC model problem with the ACE data at low
energy
DR
A.Lionetto, A.M, V.Zdravkovic astro-ph/0502406,
21 Feb. 05
6
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
diff index
injection indexes
Vc gradient
diff constant
halo size
7
Proton spectra Upper and lower bounds of due to
the uncertainties of propagation parameters
A.Lionetto, A.M, V.Zdravkovic astro-ph/0502406,
21 Feb. 05
8
Positron spectra Upper and lower bounds of due
to the uncertainties of propagation parameters
A.Lionetto, A.M, V.Zdravkovic astro-ph/0502406,
21 Feb. 05
9
Positron spectra PAMELA expectation for DC model
DRB
DC
A.Lionetto, A.M, V.Zdravkovic astro-ph/0502406
10
Antiproton spectra PAMELA expectation for DC
model
Antiproton spectra Pamela expectation for
Diffuse and Convection model
A.Lionetto, A.M, V.Zdravkovic astro-ph/0502406
11
PAMELA Cosmic-Ray Antiparticle Measurements
Antiprotons
MSSM
fd Clumpiness factors needed to disentangle a
neutralino induced component in the antiproton ?ux
A.Lionetto, A.M, V.Zdravkovic astro-ph/0502406
12
PAMELA Cosmic-Ray Antiparticle Measurements
Antiprotons
MSSM
fd Clumpiness factors needed to disentangle a
neutralino induced component in the antiproton ?ux
A.Lionetto, A.M, V.Zdravkovic astro-ph/0502406
13
Estimated reaches with Pamela
MSSM
mt 174 GeV
Clumpiness factors fd needed to disentangle a
neutralino induced component in the antiproton
?ux with PAMELA (c2gt1.8) that still give a good
fit of the present data
region where 0.13 lt ?CDM?h??lt 0.3
region where 0.09 lt ?CDM?h??lt 0.13
Equi-clumpiness factor density in respect to a
NFW
Equi-neutralino mass lines
astro-ph/0502406, 21 Feb. 05
14
EGRET, E gt 1GeV
Mayer-Hasselwander et al, 1998
15
Poin source location for GLAST 5 arcmin
1 pixel 5 arcmin
20 x 20 field IBIS/ISGRI 2040 keV
16
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
17
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
18
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
19
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
20
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
21
Estimated reaches with GLAST and Pamela
MSSM
mt 174 GeV
Clumpiness factors fd needed to disentangle a
neutralino induced component in the antiproton
?ux with PAMELA (c2gt1.8) that still give a good
fit of the present data Equi-clumpiness factor
density in respect to a NFW
GLAST sensitivity (5 s) for a neutralino density
Nc of 104 NFW in a DW10-5 sr region around the
galactic center

same but for Nc of 105 (clumpines factor 10 )
region where 0.13 lt ?CDM?h??lt 0.3
region where 0.09 lt ?CDM?h??lt 0.13
Equi-neutralino mass lines
astro-ph/0502406 and astro-ph/0305075
22
The GLAST Participating Institutions
Italian Team Institutions INFN - Instituto
Nazionale di Fisica Nucleare and Universities of
Bari, Perugia, Pisa, Roma2, Trieste, Udine
ASI - Italian Space Agency IASF-
Milano, Roma American Team Institutions
SU-HEPL Stanford University, Hanson Experimental
Physics Laboratory , , SU-SLAC Stanford
Linear Accelerator Center, Particle Astrophysics
group GSFC-NASA-LHEA Goddard Space Flight
Center, Laboratory for High Energy Astrophysics
NRL - U. S. Naval Research Laboratory, E. O.
Hulburt Center for Space Research, X-ray and
gamma-ray branches UCSC- SCIPP University of
California at Santa Cruz, Santa Cruz Institute of
Particle Physics SSU- California State
University at Sonoma, Department of Physics
Astronomy , WUStL-Washington University, St.
Louis UW- University of Washington , TAMUK-
Texas AM University-Kingsville, Ohio State
University Japanese Team Institutions
University of Tokyo ICRR - Institute for
Cosmic-Ray Research ISAS- Institute for
Space and Astronautical Science Hiroshima
University French Team Institutions CEA/DAPNIA
Commissariat à l'Energie Atomique, Département
d'Astrophysique, de physique des
Particules, de physique
Nucliaire et de l'Instrumentation Associée,
CEA, Saclay IN2P3 Institut National de
Physique Nucléaire et de Physique des Particules,
IN2P3 IN2P3/LPNHE-X Laboratoire de
Physique Nucléaire des Hautes Energies de l'École
Polytechnique IN2P3/PCC Laboratoire de
Physique Corpusculaire et Cosmologie, Collège de
France IN2P3/CENBG Centre d'études
nucléaires de Bordeaux Gradignan Swedish Team
Institutions KTHRoyal Institute of Technology
Stockholms Universitet
total US Collaboration members 161 75 Members
77 43 Affiliated Sci. 67 28 Postdocs 17 4
23
Six Towers in the GRID on Tuesday 14/06/05
24

During the 20th century the quest to broaden our
view of the universe has shown us the vastness of
the Universe and revealed violent cosmic
phenomena and mysteries
25

GLAST Exploring Natures Highest Energy
Processes August 2007 launch
26
the end
27
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)
28
Signal rate from Supersymmetry
gamma-ray flux from neutralino annihilation
J(j)
29
Other hints? WMAP data
Excess microwave emission observed in the inner
Galaxy (1-2 Kpc, 7-14 deg) consistent with
synchrotron emission from highly relativistic e
e- produced by 100 GeV dark matter particle
annihilation.
D. P. Finkbeiner astro-ph/0409027
30
Earth-Mass halos observed in high-resolution
simulations Diemand, Moore Stadel, Nature 433
(2005) 389-391
Z26
M10-6 Msun
0.024 parsecs
.. contact Lidia Pieri
31
Where is the galaxy ?
R.Minchin et al. astro-ph/0502312 16 Feb 2005
VIRGOHI21 contain no stars, a cloud of hydrogen
atoms of 108 solar mass, but it is is thousand
times more massive
32
Mini-Spikes in Mini-Halos Zhao Silk, 2005
IMBH forms by gas accretion, mass 103--104
Solar masses Accretion time-scale longer than
the local dynamical time, Formation of
mini-spike of r-1.5 density Other scenarios
could produce even more massive black holes (mass
105 Msun).
r -1.5
log ?(r)
BH
log (r)
Mini-Spike
Mini-Halo or clump
33
new s model for pp-gt p0
T.Kamae et al. astro-ph/0410617
34
f dark matter fraction concentrated in clumps
d gives the overdensity due to a clumps in
respect to the local halo density. In the
presence of many small clumps the antiproton flux
is given by
35
Energy versus time for X and Gamma ray detectors
36
Sensitivity of g-ray detectors
ARGO
MAGIC 2 (exp)
MAGIC (now)
HESS
High galactic latitudes(Fb2 10-5 g cm-2 s-1 sr
-1 (100 MeV/E)1.1). Cerenkov telescopes
sensitivities (Veritas, MAGIC, Whipple, Hess,
Celeste, Stacee, Hegra) are for 50 hours of
observations.Large field of view detectors
sensitivities (AGILE, GLAST, Milagro, ARGO, AMS)
are for 1 year of observation.
37
GLAST Scheme
Gamma-Ray Large Area Space Telescope
38
GLAST Performance
39
EGRET
AMS Cal
AMS Trk
40
(No Transcript)
41
(No Transcript)
42
(No Transcript)
43
PAMELA scientific program
PAMELA is a magnetic spectrometer which will fly
on a Russian satellite by Fall 2005. Its
scientific scope is the measurement of the
antiproton and positron spectra up to few hundred
GeV, of the proton and electron spectra up to 700
GeV and that of light nuclei.

• energy range particles/3 years
• Antiproton flux 80 MeV - 190 GeV gt3 104
• Positron flux 50 MeV 270 GeV gt3 105
• Electron flux up to 400 GeV 6 106
• Proton flux up to 700 GeV 3 108
• Electron/positron flux up to 2 TeV
• Light Nuclei (up to Z6) up to 200 GeV/n
  He/Be/C 4 107/4/5
• AntiNuclei search (sensitivity of 3 10-8 in
  He/He)

• Unprecedented Statistics and new Energy Range in
  Cosmic Rays
• Actual limits antippositrons ? 40 GeV

44
The Satellite Resurs DK1

• Soyuz-TM Launcher from Baikonur
• Launch in 2005
• Lifetime gt3 years
• PAMELA mounted inside a Pressurized Container,
  attached to Satellite
• Earth-Observation- Satellite

45
Helium spectra Upper and lower bounds of due to
the uncertainties of propagation parameters
46
Prim/Sec consistency check
DR uncertanty band
DC uncertanty band
(ScTiV)/Fe Ratio that corresponds to the best
fit of B/C
47
Antiproton spectra Upper and lower bounds of
due to the uncertainties of propagation
parameters
A.Lionetto, A.M, V.Zdravkovic astro-ph/0502406,
21 Feb. 05
48
Estimated reaches with Pamela
MSSM
Clumpiness factors fd needed to disentangle a
neutralino induced component in the antiproton
?ux with PAMELA that still give a good fit of
the present data
region where 0.13 lt ?CDM?h??lt 0.3
region where 0.09 lt ?CDM?h??lt 0.13
Equi-clumpiness factor density in respect to a
NFW
Equi-neutralino mass lines
astro-ph/0502406
49
Estimated reaches with Pamela
Clumpiness factors fd needed to disentangle a
neutralino induced component in the antiproton
?ux with PAMELA that still give a good fit of
the present data
region where 0.13 lt ?CDM?h??lt 0.3
region where 0.09 lt ?CDM?h??lt 0.13
Equi-clumpiness factor density in respect to a
NFW
Equi-neutralino mass lines
astro-ph/0502406
50
Estimated reaches with GLAST and Pamela
MSSM
Clumpiness factors fd needed to disentangle a
neutralino induced component in the antiproton
?ux with PAMELA (c2gt1.8) that still give a good
fit of the present data Equi-clumpiness factor
density in respect to a NFW
GLAST sensitivity (5 s) for a neutralino density
Nc of 104 NFW in a DW10-5 sr region around the
galactic center

same but for Nc of 105 (clumpines factor 10 )
region where 0.13 lt ?CDM?h??lt 0.3
region where 0.09 lt ?CDM?h??lt 0.13
Equi-neutralino mass lines