MAGIC Telescope

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Prospects for DARK MATTER searches with the
MAGIC Telescope
Josep Flix for MAGIC Collaboration Institut de
Física dAltes Energies (IFAE) Barcelona
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The Fact is...
gt95 if the Composition of the Universe is
still unknown
0.095 lt WCDMh2 lt 0.131
The major unresolved question in astrophysics and
cosmology nowadays !
Embarrassing baryons (i.e. stars, planets,
ourselves...) only account for 5 ...
Determination of DM nature is one of the biggest
challenges by far in present-day fundamental
science.
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Good candidates for Cold Dark Matter
In Standard Cosmological scenario Cold Dark
Matter is favoured (Structure formation) CDM in
form of Weakly Interacting Massive Particles
WIMPs Neutral Weak interaction Stable Massive N
ON-BARYONIC! Various proposed particle
candidates for non-baryonic CDM ? Theoretically
most appealing candidate SUSY-WIMPs
especially neutralino.
more in literature! KK-Particles, ...
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Indirect search for Relic Neutralinos
Annihilations taking place in celestial bodies
where cs have been accumulated. High
density regions (?? (WIMP density)2 )
cc
Search for excess components in cosmic rays
(DIFFUSION)
keep directionallity
cores of DM halos
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The MAGIC Telescope I

• Up-to-date largest Imaging Air Cherenkov
  Telescope for ?-ray astronomy.
• (17 m mirror dish)
• - low design energy threshold
• E? 30 GeV
• fast repositioning
• tRlt30 sec

Canary Island La Palma (2200 a.s.l)
September 2004 Start of regular data-taking
MAGIC is a successful pioneering telescope for
low energy gamma ray astronomy producing first
results ( hints for E lt 100 GeV g-ray detections
) See D. Mazin, N. Tonello and M. López talks

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g-rays from Neutralino self-annihilations I
ph cm-2 s-1GeV-1
?? angle between pointing direction and
center of (sub)halo.
Cesarini et al, astro-ph/0305075
ph cm3 s-1 GeV-3 sr-1
ltsannvgt averaged annihilation cross
section over the halo velocity distribution.
Spectra Sum over all final (f) states, with
proper BRs ? g-yield
m?200 GeV
g-lines are loop suppressed
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g-rays from Neutralino self-annihilations II
ph cm-2 s-1GeV-1
GeV2 cm-5 sr
Geometry dependence l.o.s integration accounts
for neutralino distribution within the halo
Given a telescope qPSF, we integrate over the
aperture DW
Normally, in literature is found the Averaged
l.o.s integral, as
GeV2 cm-5
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Evaluation of fluxes from c annihilations
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FSUSY - mSUGRA Example parameter Scan
Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004)
DarkSUSYISAJET
WMAP allowed
107 input Models 18 UNPHYS 6 EXCL. BY
ACC. 1.6 with Wh2 lt 0.127 0.24 with Wh2 in
WMAP range
MAGIC
5 orders of magnitude
Coannihilations are important! Resonances to
Higss Boson A!
Includes Focus Point, Bulk region... Higgsinos
and Gauginos (No Winos)
FSUSY differs by several orders of magnitude
Integrated
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Galactic Center Motivations

• From distance and DM density criteria, the
  Galactic Center is a priori the
• best candidate place for indirect searches for
  Dark Matter.

BUT

• Other g-ray sources in the FOV,
• i.e. SNR Sgr A East

• g-rays from GC have several plausible
• origin scenarios in competition...

• From MAGIC site, the Galactic Center
• cuminates at 60 degrees.
• This affects to the Ethr ? 700 GeV
  conservative

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Halo modelization - The Galactic Center I
Baryons role during galaxy formation?
Baryonic infall during galaxy formation results
in an increase of the central density of Dark
Matter.
ADIABATIC COMPRESSION EFFECT
Indeed, we know that halos in hierarchical
structure formation scenarios grow via multiple
violent mergers and accretion along filaments...
and particle orbits in halos are highly
eccentric...
STANDARD PRESCRIPTION Response of Dark Matter to
the condensation of baryons was usually
calculated using the model of adiabatic
contraction, which assumes spherical symmetry
halos and circular orbits of infalling
particles...
Blumenthal et al, 1986
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Halo modelization - The Galactic Center II
We used detailed models of our Milky Way galaxy
and applied modified Adiabatic contraction to
model the GC DM distribution. This prescription
gives reasonable accuracy compared to Gnedin et
al 2004 analytical approx. from high-resolution
simulation (10).
Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004)
The standard adiabatic prescription
systematically overpredicts the increase of Dark
Matter density in the inner part of halos (?lt
0.05rvir )...

• Detailed mass model of our Galaxy
• extensive data on the solar neighborhood.
• motion of stars and HII regions in the outer MW
  part .
• Motion of satellites and globular clusters in
  our halo...

Klypin, Zhao et al, 2002
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Halo modelization - The Galactic Center III
Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004)
Detailed mass model of our Galaxy
DENSITY
MASS
NFW Moore
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Halo modelization - The Galactic Center IV
Evaluation of average l.o.s Integral (FCOSMO)
MAGIC qPSF 0.1º DW 10-5 sr
qPSF (MAGIC)
3 orders of magnitude
COMP. NFW
UNCOMP. NFW
q1-order 0.12º q2-orders 0.3º q1-order
0.47º q2-orders gt0.5º
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DRACO dSph Motivations

• The Milky way is surrounded by a number of small
  faint companion galaxies.

Northern source

• These dSph are believed to be the most dominated
  Dark Matter objects.

• Distances and M/L ratios 16 kpc to 250 kpc
  M/L 30-300

• Interesting places to test present theoretical
  predictions of DM profiles.

• Also they play an important role in theories of
  structure formation subhaloes.

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Halo modelization - Draco dSph I
Different Dark Matter modelizations for DRACO
Flix et al., in preparation
Ewans et al. (2004) Kleyna et al 2002 data
Tidal effects included in the model Lokas et al.
(2005) (NFWcut-off) Wilkinson et al 2004 data
2004 Wilkinson
2002 Kleyna
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Halo modelization - Draco dSph II
Evaluation of average l.o.s Integral (FCOSMO)
Flix et al., in preparation
qPSF 0.1º DW 10-5 sr
qPSF (MAGIC)
lt1 order of magnitude
q1-order 0.18º q2-orders 0.39º q1-order
0.20º q2-orders 0.41º q1-order
0.24º q2-orders 0.32º q1-order
0.17º q2-orders 0.47º
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Pros and Cons for MAGIC viable targets
Ethr(0º) 100 GeV Very conservative
Object D kpc ZA deg Ethr GeV ltJgtDW GeV2 cm-5 q1-order deg Contami-nation?
GC(comp) 8.5 60 650 4.41028 .12 Yes
GC(uncomp) 8.5 60 650 1.51025 .47 (ext) Yes
DRACO 80 29 150 7.31023 .18 (ext) No
M31 770 13 110 2.71023 .27 (ext) Yes
FLUX




Dominiks talk
M87
Canis Major dSph ZA 60º - No modeled (Tidally
stripped) Saggitarius dSph ZA 60º - No modeled
(Tidally stripped)
VHE Spectra VHE Upper Limits
ext extended
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A summary (comparative) plot NFW models
Flix et al., in preparation
? Wh2 showed A0 ? 0 (still low sampling) stop
coannihilations! SUSY naturalness violated (
M12gt2 TeV, i.e. ? mc )
M87
M31
DRACO
5s limit curves
GC uncomp.
GC comp.
No substructure enhancement
Ethr(0º) 100 GeV Very conservative Sensitivi
ty from latest MAGIC 04 Crab data
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Enhancement factors and other scenarios
All these putative contributions could enhance
significantly the g-flux
Adiabatic contraction effects (not for
dSph) non-constrained SUSY models Wino-like-Neutr
alinos (1-order mag.) Substructure contribution
(gt1 lt2-order mag.) Quintassence Kination
regime modify expansion rate ? Relic
Density higuer ltsvgt allowed ( 1 to 2-order
magnitude) Q-Balls with high lifetime decay
after freeze-out of c non-thermal c
production higuer ltsvgt allowed (???) other WIMPs?
g-rays
SuperHeavy Dark Matter Kaluza-Klein
Particles Leptonic WIMPs (LIMPs) ...
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Towards Dark Matter Observations with MAGIC
Galactic Center

• GC observable from La Palma at zenith gt60º
• High energy threshold (EthrO(650 GeV),
  conservative).
• Large effective collection area (cut-off
  determination!)
• Contamination from other VHE emitters

HESS Flux _at_ 700 GeV ? MAGIC 5s in 2h
MAGIC observed the GC in September 2004 for 3
hours under test conditions
Proposal for more observations between
April-August 2005
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Towards Dark Matter Observations with MAGIC
DRACO dSph

• DRACO is the most DM dominated dwarf (M/L up to
  300).
• Low Zenith angle observations ? Nominal (low)
  Energy Threshold.
• No known VHE emitters in the FOV.
• Clean target for Dark Matter observations.
• DM modelling of the dwarf SUSY models ? Very
  Small fluxes compared to GC.
• Scenarios with enhancement factors are needed
  and/or other DM particles ? ??.

Proposal for observations between May-June 2005
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Summary
- Conservative c predictions are not that
optimistic (targets are weak sources).

• Window for scenarios that could enhance
  significantly the g-flux.

- Other scenarios which yield g-rays allow higher
fluxes.
Planned Dark Matter inspired observations with
MAGIC for 2005
Near DM clumps high-latitude
? Observations of gt 1 source
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• Where is the sky section?