Dark Matter annihilation in Draco: new considerations of
the expected gamma flux 1
Miguel A. Sánchez-Conde
Instituto de Astrofisica de Andalucia (CSIC), E-18008, Granada, Spain
Abstract. A new estimation of the γ-ray flux that we expect to detect from SUSY dark matter annihilation from the Draco
dSph is presented using the DM density profiles compatible with the latest observations. This calculation takes also into
account the important effect of the Point Spread Function (PSF) of the telescope. We show that this effect is crucial in the way
we will observe and interpret a possible signal detection. Finally, we discuss the prospects to detect a possible gamma signal
from Draco for MAGIC and GLAST.
Keywords: cosmology: dark matter — galaxies: dwarf — gamma-rays: theory
PACS: 95.35.+d; 95.55.Ka; 95.85.Pw; 98.35.Gi; 98.52.Wz
INTRODUCTION
The Draco galaxy, a satellite of the Milky Way, represents one of the best suitable candidates to search for DM outside
our galaxy [1], since it is near (80 kpc) and it has probably more observational constraints than any other known DM
dominated system. This fact becomes crucial when we want to make realistic predictions of the expected observed
γ-ray flux due to DM annihilation.
The expected total number of continuum γ-ray photons received per unit time and per unit area, from a circular
aperture on the sky of width σt (which represents the resolution of the telescope) observing at a given direction Ψ0
relative to the centre of the dark matter halo is given by:
F(E > Eth) =
fSUSY ·U(Ψ0), with fSUSY =
Nγ 〈σv〉
, U(Ψ0) =
J(Ψ)B(Ω)dΩ (1)
where the factor fSUSY encloses all the particle physics, and the factor U(Ψ0) involves all the astrophysical properties
such as the dark matter distribution, geometry considerations and telescope performances like the PSF, this one directly
related to the angular resolution (for a detailed explanation of each of these terms, see e.g. [2]).
DRACO γ-RAY FLUX PROFILES AND THE EFFECT OF THE PSF
We assumed that the dark matter distribution in Draco can be approximated by the formula ρd(r) = Cr−α exp(− rrb )
proposed by [3], which was found to fit the density distribution of a simulated dwarf dark matter halo stripped during
its evolution in the potential of a giant galaxy. Here we will consider two cases, the profile with a cusp α = 1 and a core
α = 0. The calculated γ-ray flux profiles are shown in left panel of Fig.1. For both cusp and core DM density profiles,
the flux values should be very similar for the inner region of the dwarf, where signal detection would be easier. It is
also necessary to take into account the role of the PSF in the calculations. Its effect on gamma ray flux profiles, usually
neglected, may be crucial to correctly interpret a possible signal in the telescope, as it can be clearly seen in right panel
of Fig. 1.
1 Poster presented at the First GLAST Symposium, Stanford University, USA, 5-8 February 2007
http://arxiv.org/abs/0704.0222v1
FIGURE 1. Left panel: Draco flux predictions for the core (red line) and cusp (blue line) DM density profiles, computed using
a PSF= 0.1◦. A value of fSUSY = 10
−33GeV−2cm3s−1 was used (the most optimistic case given by particle physics at 100 GeV).
Right panel: Flux predictions for the cusp density profile and using a PSF=0.1◦ (blue line), PSF=1◦ (red) and without PSF (green).
FIGURE 2. Draco flux profile detection prospects for GLAST (red lines) and MAGIC (blue lines), and for the cusp density
profile using a PSF=0.1◦. Values of fSUSY = 10
−33GeV−2cm3s−1 at 100 GeV and fSUSY = 4 10
−33GeV−2cm3s−1 at 10 GeV were
used for MAGIC and GLAST respectively (the most optimistic scenarios given by particle physics at those energies.
DETECTION PROSPECTS
We carried out some calculations concerning the possibility to detect a γ-ray signal coming from DM annihilation in
Draco for MAGIC and GLAST (Fig.2). According to these calculations, a detection of the gamma ray flux profiles
seems to be very hard. We computed also the prospects for an excess signal detection, i.e. we are not interested in the
shape of the gamma ray flux profile, only in detectability (Table. 1). According to the results we reached there is no
chance to detect a γ-ray signal (flux profiles or just an excess) coming from Draco with current experiments, at least
with the preferred particle physics and astrophysics models (for a more detailed study, see the complete work [4]). It
will be necessary go a step further with IACTs that join a large field of view with a high sensitivity.
TABLE 1. Prospects of an excess signal detection for MAGIC
and GLAST. For FDraco, the most optimistic and pessimistic values
are given in the form FDraco,min - FDraco,max. Fmin represents the
minimum detectable flux for each instrument. All values refer to the
inner 0.5◦ of the dwarf.
FDraco (ph cm
2 s−1) Fmin (ph cm
2 s−1)
MAGIC 1.6 10−19 - 4.0 10−16 4.4 10−11 (250 h, 5σ )
GLAST 1.6 10−19 - 1.6 10−15 3.9 10−10 (1 yr, 5σ )
REFERENCES
1. Evans N. W., Ferrer F. and Sarkar S., 2004, Physical Review D, 69, 123501
2. Prada F., Klypin A., Flix J., Martínez M. and Simonneau E., 2004, Phys. Rev. Letters, 93, 241301
3. Kazantzidis S., Mayer L., Mastropietro C., Diemand J., Stadel J., Moore B., 2004, ApJ, 608, 663
4. Sánchez-Conde M.A., Prada F. Łokas E.L., Gómez M.E., Wojtak R. Moles M., 2007, submitted to JCAP, [astro-ph/0701429]
http://arxiv.org/abs/astro-ph/0701429
	Introduction
	Draco -ray flux profiles and the effect of the PSF
	Detection prospects

  A new estimation of the gamma-ray flux that we expect to detect from SUSY
dark matter annihilation from the Draco dSph is presented using the DM density
profiles compatible with the latest observations. This calculation takes also
into account the important effect of the Point Spread Function (PSF) of the
telescope. We show that this effect is crucial in the way we will observe and
interpret a possible signal detection. Finally, we discuss the prospects to
detect a possible gamma signal from Draco for MAGIC and GLAST.

Introduction
	Draco -ray flux profiles and the effect of the PSF
	Detection prospects
