Feb 18 – 26, 2021
Europe/Rome timezone

Neutrinos as signal and background in the search for dark matter with INO

Feb 26, 2021, 10:20 AM
Room 2 (https://unipd.link/NeuTel-ParallelRoom2)

Room 2


Parallel Contributed Talk Neutrino Telescopes and Multimessenger New Facilities


Deepak Tiwari (PICO, University of Montreal)


Annihilation of Weakly Interacting Massive Particles (WIMPs) in the center of the sun($\odot$), earth($\oplus$) and the galaxy can give rise to neutrino-antineutrino pairs as their final products. We look at the prospects of detecting such neutrinos at the proposed 50-kt Iron Calorimeter (ICAL) detector, to be housed at the upcoming India-Based Neutrino Observatory (INO), wherein the interaction of neutrinos ($\nu_{\mu}/\bar{\nu}_{\mu}$) with detector iron layers will produce $\mu^{-}/\mu^{+}$. The atmospheric neutrinos in GeV range will pose a serious background to such signal neutrinos, which fortunately, can be suppressed considerably by exploiting the excellent angular resolution of the ICAL detector. The expected sensitivity limits for 500 kt-years of ICAL exposure are quite competitive to other neutrino experiments for the WIMP masses $m_{\chi}$) $<$ 100 GeV. The expected 90 % C.L. exclusion sensitivity limits for 500 kt-years exposure for $\tau^{+} \tau^{-}$ channel (100 % branching ratio) for WIMP-nucleon Spin Dependent ($\sigma_{SD}$) and Spin Independent $\sigma_{SI}$) cross-section are found to be $\sigma_{SD,\odot} < 6.87\times 10^{-41}$ cm$^2$ and $\sigma_{SI,\odot} < 7.75\times 10^{-43}$ cm$^2$ for the WIMP mass ($m_{\chi}$) = 25 GeV, and $\sigma_{SI,\oplus} =1.02\times 10^{-44}~\mathrm{cm}^2$ for $m_{\chi}$ =52.14 GeV. For galactic centre searches, the expected 90 % C.L. sensitivity limits on velocity averaged annihilation cross-section $\langle\sigma_{A}v\rangle$ for a 30 GeV WIMP, assuming NFW WIMP profile and 100\% branching ratio for each channel are: $\langle\sigma_{A}v\rangle \leq 1.19\times 10^{-22}~ \mathrm{cm}^3 \mathrm{s}^{-1}$ for the $\mu^{+} \mu^{-}$ channel and \langle\sigma_{A}v\rangle \leq 6.35\times 10^{-23} \mathrm{cm}^3 \mathrm{s}^{-1}$ for the $\nu ~\bar{\nu}$ channel.

Collaboration name INO

Primary author

Deepak Tiwari (PICO, University of Montreal)


Dr Anushree Ghosh (University of Padua) Prof. Sandhya Choubey (Department of Physics, School of Engineering Sciences, KTH Royal Institute of Technology)

Presentation materials