Abstract
We present the Sommerfeld enhanced Dark Matter (DM) annihilation into gamma ray for a class of three-loop radiative neutrino mass models with large electroweak multiplets where the DM mass is in O(TeV) range. We show that in this model, the DM annihilation rate becomes more prominent for larger multiplets and it is already within the reach of currently operating Imaging Atmospheric Cherenkov telescopes (IACTs), High Energy Stereoscopic System (H.E.S.S.). Furthermore, Cherenkov Telescope Array (CTA), which will begin operating in 2030, will improve this sensitivity by a factor of O(10) and may exclude a large portion of parameter space of this radiative neutrino mass model with larger electroweak multiplet. This implies that the only viable option is the model with lowest electroweak multiplets i.e. singlets of SU(2)L where the DM annihilation rate is not Sommerfeld enhanced and hence it is not yet constrained by the indirect detection limits from H.E.S.S. or future CTA.
Highlights
We are yet to identify the mass and particle nature of the Dark Matter (DM) of the universe despite having extensive astrophysical and cosmological observations supporting its existence
The DM, having quantum numbers under the Standard Model (SM) gauge group SU (2)L × U (1)Y and with mass in the TeV range, has come under the focus of Imaging Atmospheric Cherenkov Telescopes (IACT) as gamma ray produced in the DM annihilation at the central region of the Milky Way galaxy is within the detection reach of Imaging Atmospheric Cherenkov telescopes (IACTs) [1,2,3,4]
We have presented the Sommerfeld enhanced DM annihilation cross sections to gamma rays for a class of three loop radiative neutrino mass generation models with large electroweak fermion and scalar multiplets i.e 5-plet and 7-plet under SU (2)L
Summary
We are yet to identify the mass and particle nature of the Dark Matter (DM) of the universe despite having extensive astrophysical and cosmological observations supporting its existence. The DM, having quantum numbers under the Standard Model (SM) gauge group SU (2)L × U (1)Y and with mass in the TeV range, has come under the focus of Imaging Atmospheric Cherenkov Telescopes (IACT) as gamma ray produced in the DM annihilation at the central region of the Milky Way galaxy is within the detection reach of IACTs [1,2,3,4]. On the other hand, such high energy gamma ray interacts with the upper region of the atmosphere and creates a shower of very energetic secondary charged particles which reaches at about 10 km height These particles move faster than the speed of light in the air and emit the faint blue Cherenkov light.
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