TY - JOUR
T1 - Radio Signal by Galactic Dark Matter
AU - Borriello, E.
AU - Cuoco, A.
AU - Miele, G.
N1 - Funding Information:
G.M. acknowledges supports by the Spanish MICINN (grants SAB2006-0171 and FPA2005-01269) and by INFN–I.S.Fa51 and PRIN 2006 “Fisica Astroparticellare: Neutrini ed Universo Primordiale” of Italian MIUR.
PY - 2009/5
Y1 - 2009/5
N2 - An interesting strategy for indirect detection of Dark Matter comes through the amounts of electrons and positrons usually emitted by DM pair annihilation. The e+ e- gyrating in the galactic magnetic field then produce secondary synchrotron radiation. The radio emission from the galactic halo as well as from its expected substructures if compared with the measured diffuse radio background can provide constraints on the physics of WIMP's. In particular one gets the bound of 〈 σA v 〉 = 10- 24 cm3 s- 1 for a DM mass mχ = 100 GeV even though sensibly depending on the astrophysical uncertainties.
AB - An interesting strategy for indirect detection of Dark Matter comes through the amounts of electrons and positrons usually emitted by DM pair annihilation. The e+ e- gyrating in the galactic magnetic field then produce secondary synchrotron radiation. The radio emission from the galactic halo as well as from its expected substructures if compared with the measured diffuse radio background can provide constraints on the physics of WIMP's. In particular one gets the bound of 〈 σA v 〉 = 10- 24 cm3 s- 1 for a DM mass mχ = 100 GeV even though sensibly depending on the astrophysical uncertainties.
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U2 - 10.1016/j.nuclphysbps.2009.03.087
DO - 10.1016/j.nuclphysbps.2009.03.087
M3 - Article
AN - SCOPUS:65749088140
SN - 0920-5632
VL - 190
SP - 185
EP - 190
JO - Nuclear Physics B - Proceedings Supplements
JF - Nuclear Physics B - Proceedings Supplements
IS - C
ER -