J/MNRAS/418/1526 Dark matter in dSph galaxies (Charbonnier+, 2011)
Dark matter profiles and annihilation in dwarf spheroidal galaxies:
prospectives for present and future γ-ray observatories.
I. The classical dwarf spheroidal galaxies.
Charbonnier A., Combet C., Daniel M., Funk S., Hinton J.A., Maurin D.,
Power C., Read J.I., Sarkar S., Walker M.G., Wilkinson M.I.
<Mon. Not. R. Astron. Soc., 418, 1526-1556 (2011)>
=2011MNRAS.418.1526C 2011MNRAS.418.1526C
ADC_Keywords: Models ; Galaxies, peculiar ; Gamma rays
Keywords: astroparticle physics - methods: miscellaneous - galaxies: dwarf -
galaxies: kinematics and dynamics - dark matter - gamma-rays: general
Abstract:
Due to their large dynamical mass-to-light ratios, dwarf spheroidal
galaxies (dSphs) are promising targets for the indirect detection of
dark matter (DM) in γ-rays. We examine their detectability by
present and future γ-ray observatories. The key innovative
features of our analysis are as follows: (i) we take into account the
angular size of the dSphs; while nearby objects have higher
γ-ray flux, their larger angular extent can make them less
attractive targets for background-dominated instruments; (ii) we
derive DM profiles and the astrophysical J-factor (which parametrizes
the expected γ-ray flux, independently of the choice of DM
particle model) for the classical dSphs directly from photometric and
kinematic data. We assume very little about the DM profile, modelling
this as a smooth split-power-law distribution, with and without
subclumps; (iii) we use a Markov chain Monte Carlo technique to
marginalize over unknown parameters and determine the sensitivity of
our derived J-factors to both model and measurement uncertainties; and
(iv) we use simulated DM profiles to demonstrate that our J-factor
determinations recover the correct solution within our quoted
uncertainties.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
cls_car.dat 81 40 Carina dSph clump luminosity
cls_dra.dat 81 40 Draco dSph clump luminosity
cls_for.dat 81 40 Fornax dSph clump luminosity
cls_scl.dat 81 40 Sculptor dSph clump luminosity
cls_sex.dat 81 40 Sextans dSph clump luminosity
cls_umi.dat 81 40 Ursae Minor dSph clump luminosity
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Byte-by-byte Description of file: cls*.dat
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Bytes Format Units Label Eplanations
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1- 12 E12.7 deg alpha Integration angle, αint
14- 25 E12.7 Msun+2/kpc5 J Integration angle dependence,
J(αint) (1)
29- 40 E12.7 Msun+2/kpc3 CL68lo Most-likely, 68% clump luminosity on the
quantity J(αint), lower limit
42- 53 E12.7 Msun+2/kpc3 CL68up Most-likely, 68% clump luminosity on the
quantity J(αint), higher limit
56- 68 E13.7 Msun+2/kpc3 CL95lo Most-likely, 95% clump luminosity on the
quantity J(αint), lower limit
69- 81 E13.7 Msun+2/kpc3 CL95up Most-likely, 95% clump luminosity on the
quantity J(αint, higher limit
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Note (1): J-factor which corresponds to the integration of the dark matter
density sqared along the line of sight and over the solid angle
ΔΩ=2π(1-cosαint).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 23-Jul-2012