Abstract
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.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 185-190 |
| Number of pages | 6 |
| Journal | Nuclear Physics B - Proceedings Supplements |
| Volume | 190 |
| Issue number | C |
| DOIs | |
| State | Published - May 1 2009 |
| Externally published | Yes |
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ASJC Scopus subject areas
- Atomic and Molecular Physics, and Optics
- Nuclear and High Energy Physics
Cite this
Radio Signal by Galactic Dark Matter. / Borriello, Enrico; Cuoco, A.; Miele, G.
In: Nuclear Physics B - Proceedings Supplements, Vol. 190, No. C, 01.05.2009, p. 185-190.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Radio Signal by Galactic Dark Matter
AU - Borriello, Enrico
AU - Cuoco, A.
AU - Miele, G.
PY - 2009/5/1
Y1 - 2009/5/1
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.
UR - http://www.scopus.com/inward/record.url?scp=65749088140&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=65749088140&partnerID=8YFLogxK
U2 - 10.1016/j.nuclphysbps.2009.03.087
DO - 10.1016/j.nuclphysbps.2009.03.087
M3 - Article
VL - 190
SP - 185
EP - 190
JO - Nuclear and Particle Physics Proceedings
JF - Nuclear and Particle Physics Proceedings
SN - 2405-6014
IS - C
ER -