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Neutrino Astrophysics Astrophysics and Astronomy Neutrino Astrophysics and Astronomy Madhurima Pandey Astroparticle Physics and Cosmology Division Saha Institute of Nuclear Physics, HBNI, Kolkata WHEPP XVI, IIT Guwahati Wednesday, December 4, 2019 WHEPP XVI 1 Wednesday, December 4, 2019 WHEPP XVI 2 Solar Neutrino Wednesday, December 4, 2019 WHEPP XVI 3 Solar Neutrino Neutrino and antineutrino production mechanism [1] Rates proportional to , and - depend on specific processes, and - effective coupling constants for vector and axial – vector interaction. Antineutrinos can be probed at the Earth detector in KeV energy range. [1] E. Vitagliano et al., JCAP 12, 010 (2017) Wednesday, December 4, 2019 WHEPP XVI 4 Solar Neutrino sterile neutrinos in KeV range - 1. capture on a stable isotope of dysprosium if > 2.83 KeV [2] 2. slightly heavier sterile neutrinos include unstable isotopes[3] coherent inelastic scattering on atoms [4] and electron scattering [5] CP violation MSW effect [2] T. Lasserre et al., arXiv:1609.04671, [3] Y.F. Li et al., Phys. Lett. B 695 (2011) 205, [4] S. Ando et al., Phys. Rev. D 81 (2010) 113006, [5] M.D. Campos et al., Phys. Rev. D 94 (2016) 095010 Wednesday, December 4, 2019 WHEPP XVI 5 Atmospheric(ATM) Neutrino ATM neutrinos at Super Kamiokande (SK) experiment confirmed neutrino flavour oscillation – established the existence of neutrino masses and mixing Discovery of flavour oscillation of ATM neutrinos in 2015 Cosmic ray particles collide with the nuclei in the Earth’s atmosphere, producing pions and kaons which decay into neutrinos First observations of ATM neutrinos in 1965 at kolar Gold experiment in India and simultaneously led by Fred Reines in South Africa – looking for proton decay – the discrepancy was resolved by the SK experiments Wednesday, December 4, 2019 WHEPP XVI 6 ATM Neutrino ATM neutrino detector – 1. Hyper Kamiokande – megaton-class water Cherenkov detector, fiducial volume ~ 20 times that of SK 2. ICAL detector at India-based Neutrino Observatory – 50 Kton magnetised iron calorimeter, charge identification efficiency 3. PINGU – low energy extension of IceCube 4. ORCA proposal – low energy extension of KM3NeT detector Physics Goals - 1. and 2. 3. neutrino mass hierarchy 4. octant of 5. Non-standard interactions 6. probing sterile neutrino 7. CPT violation studies Wednesday, December 4, 2019 WHEPP XVI 7 PINGU (The Precision IceCube Next Generation Upgrade) Low energy infill 17 strings × 125 sensors + Upgrade strings, 24m inter-string spacing Effective mass – 6Mton ice Energy threshold – few GeV sample of over 60 000 atmospheric neutrinos per year PINGU will make highly competitive measurements of neutrino oscillation parameters in an energy range over an order of magnitude higher than long- baseline neutrino beam experiments. It is embedded within the IceCube DeepCore Wednesday, December 4, 2019 WHEPP XVI 8 PINGU (DeepCore Topview) Wednesday, December 4, 2019 WHEPP XVI 9 PINGU Wednesday, December 4, 2019 WHEPP XVI 10 PINGU Scientific Goals – Augmenting the low-energy program of the upgrade. ~60k up-going atmospheric neutrinos per year Neutrino mass ordering appearance – test of the unitarity of (3 × 3) PMNS matrix octant anomaly Wide breadth of other science: 1. Dark matter searches 2. Earth tomography 3. Supernovae Neutrinos (SN) 4. ........ Ref – M.G. Aartsen et al., JPG 44, 054006 (2017) Wednesday, December 4, 2019 WHEPP XVI 11 High Energy Neutrino Astronomy Neutrinos are an ideal messenger for astrophysics Neutrino telescope - 1. ANTARES and KM3NeT in the Mediterranean sea 2. GVD in Lake Baikal 3. IceCube buried in the ice of the South Pole Instrument a large volume of water or ice -> detect the cherenkov radiation ->consequence of a neutrino interaction with the detector IceCube contains 5160 DOMs within a volume of 1 km3 Number of color points and their size - amount of light - relate to the energy of the incident neutrino Color code - >information about the timing -> reconstruct the direction of the produced muon -> estimate the position of the source Spatial distribution of the hits or rather the topology of the event - flavour of the neutrino Three neutrino sources - the sun, the supernovae SN1987A and the blazar TXS 0506 + 056 High energy part of the astrophysical energy spectrum, extending from GeV to PeV energies Wednesday, December 4, 2019 WHEPP XVI 12 IceCube Collaboration In 2013, IceCube announced first detection of High energy astrophysical neutrinos - these events are called HESE events Recent HESE analysis- 7.5 years of icecube data with 103 neutrino events ( out of which 60 events are above 60 TeV) Best fit energy spectrum is a single power law with spectral index , all flavour flux Normalization In 2018, IceCube reported the first multi-messenger evidence of a flaring blazar in coincidence with the high energy neutrino event IC - 170922A A possible source candidate could be TXS 0506+056. 13 5 neutrino excess found in 2014-2015 over 110 days in addition to the event detected in 2017. Wednesday, December 4, 2019 WHEPP XVI 13 IceCube Probing a four flavour vis-a-vis three flavour neutrino mixing for ultrahigh energy neutrino signal at a 1 Km2 detector M. Pandey et al., Phys. Rev. D 97, 103015 (2018) Wednesday, December 4, 2019 WHEPP XVI 14 From the analysis of the high-energy starting events (HESE) data (the IceCube Collaboration), they calculated a best fit power law for the neutrino flux as [ICRC2017 (2017) 981] .....2.....20) For a one component fit the neutrino flux , with the index We have computed for this flux as well and the energy range 60 TeV is to be considered for such calculations. Table 2: Same as Table 1, but here we consider the diffuse flux of UHE neutrinos obtained from the recent analysis of the IceCube (HESE) data. Figure 1: Variation of with and for (a) = 1◦ and (b) = 4◦ (the recent IceCube HESE data). IceCube Mass and Life time of heavy dark matter decaying into IceCube PeV neutrinos M. Pandey et al., Phys. Lett. B 797, 134910 (2019) Wednesday, December 4, 2019 WHEPP XVI 16 Introduction The source of other UHE neutrino events at IceCube is by and large unknown. These also include the track events for the neutrinos in and around PeV region. We explore an alternative possibility that these neutrinos could have been created by the rare or long lived decay of superheavy dark matter in the Universe. The superheavy dark matter could be created during a spontaneous symmetry breaking in Grand Unified scale and thus they were never in thermal equilibrium with the Universe. Thus their production is nonthermal in nature. They can also be created by the process of gravitational production. Here in this work, we consider the decay of the super heavy dark matter to interpret the neutrinos in and around the PeV region recorded by IceCube that includes the best fit region for muon neutrino track events given by IceCube in the same regime. In the whole process one needs to consider two decay channels, one is the hadronic decay channel while the other is the leptonic decay channel. We try to estimate the best fit value of the mass ( ) and the decay lifetime ( )of the dark matter, which undergoes a decay via the hadronic channel. Also for the fixed value of the dark matter mass we calculate the best fit value of the dark matter decay lifetime ( ) when both hadronic and leptonic channel are considered. Wednesday, December 4, 2019 WHEPP XVI 17 IceCube IceCube Data and Fit [PoS(ICRC2017)981] Wednesday, December 4, 2019 WHEPP XVI 18 Formalism [M. Pandey et al., Phys. Lett. B 797, 134910 (2019)] The neutrino spectrum from the decay of such dark matter can be written as ..... (1) where and the functions are taken from the reference [1] ...... (2) is the dimensionless energy fraction transferred to the hadron. [1] S.R. Kelner et al., Phys. Rev. D 74, 034018 (2006); Erratum: Phys. Rev. D 79, 039901 (2009). Wednesday, December 4, 2019 WHEPP XVI 19 Formalism [M. Pandey et al., Phys. Lett. B 797, 134910 (2019)] The neutrino flux can be of two type; extragalactic and galactic - The isotropic extragalactic neutrino flux from the decay of such a heavy dark matter with mass is given as ....... (3) Hubble radius The cosmological dark matter density at the present epoch is describes the neutrino energy spectrum, obtained from the decay of super heavy dark matter and this neutrino spectrum is a function of the neutrino energy at redshift The galactic neutrino flux from similar decay is described by ..... (4) is the dark matter density and we consider Navarro-Frenk-White (NFW) profile. defines the neutrino spectrum decaying from the super heavy dark matter , where , are the galactic coordinate . The total flux is obtained as ...... (5) Wednesday, December 4, 2019 WHEPP XVI 20 Calculation and Results We have consider the UHE region in the energy range GeV to PeV. [2] [2] The IceCube Collaboration, 35th International Cosmic Ray Conference, ICRC2017, PoS ICRC2017 (2017) 981. Ref - [M. Pandey et al., Phys. Lett. B 797, 134910 (2019)] Wednesday, December 4, 2019 WHEPP XVI 21 Calculation and Results Wednesday, December 4, 2019 WHEPP XVI 22 Calculations and Results The for our fit ...... (6), where is the number of chosen points (Table 1) are the energies of the chosen points. is the theoretical flux obtained from Eq. (5). corresponding to experimental data are given in Table 1. is the error of chosen experimental points (Table 1). Figure The best fit value is (only hadronic channel is considered for dark matter decay) 23 Wednesday, December 4, 2019 WHEPP XVI Calculations and Results We make one parameter analysis (using Eq. (6) for all set of points given in Table 1) and obtained the best fit value of for the best fit value of (Figure 2) when both the hadronic and the leptonic channels are considered.
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