Table of contents

The 15^th edition of the International Conference on Topics in Astroparticle and Underground Physics (TAUP 2017) was held from July 24 through 28, 2017 in Sudbury, Ontario Canada. It was organized and hosted by Laurentian University and SNOLAB with sponsorship and other support from the City of Greater Sudbury, IOP Publishing, the Institute of Particle Physics, the International Union of Pure and Applied Physicists, and Vale.

The meeting attracted 350 participants from around the world: 31 countries were represented. The topics discussed at the meeting included Cosmology, Dark Matter, Neutrino Physics and Astrophysics, Gravitational Waves, High-Energy Astrophysics and Cosmic Rays, New Technologies, and the intersection of these fields. We were particularly pleased to open the meeting with a discussion of education, outreach, and inclusion and to have these themes continue throughout the week.

List of TAUP 2017 Organizing Committee, TAUP-2017 International Advisory Committee, TAUP Steering Committee, Conference Schedule: Monday, July 24, Conference Schedule: Tuesday, July 25, Conference Schedule: Wednesday, July 26, Conference Schedule: Thursday, July 27, Conference Schedule: Friday, July 28, Poster Session, Monday Parallel Sessions: 1:00 PM - 3:00 PM, Monday Parallel Sessions: 3:30 PM - 5:30 PM, Tuesday Parallel Sessions: 1:00 PM - 3:00 PM, Tuesday Parallel Sessions: 3:30 PM - 5:30 PM, Wednesday Parallel Sessions: 1:00 PM - 3:00 PM, Wednesday Parallel Sessions: 1:00 PM - 3:00 PM, Wednesday Parallel Sessions: 3:30 PM - 5:30 PM, Wednesday Parallel Sessions: 3:30 PM - 5:30 PM, Thursday Parallel Sessions: 1:00 PM - 3:00 PM, Thursday Parallel Sessions: 3:30 PM - 5:30 PM are available in the pdf.

All papers published in this volume of Journal of Physics: Conference Series have been peer reviewed through processes administered by the proceedings Editors. Reviews were conducted by expert referees to the professional and scientific standards expected of a proceedings journal published by IOP Publishing.

The realization of multimessenger astrophysics is opening up a new field of exploration of the most energetic phenomena in the universe. Astrophysical messengers associated with each of the four fundamental forces reach detectors buried deep underground or underwater, spread across wide swaths of land, and orbiting high above us in space. Recent detection of coincident real-time signals amongst these experiments heralds the birth of high-energy multimessenger astronomy and enables us to begin exploring and understanding their astrophysical sources. The Astrophysical Multimessenger Observatory Network (AMON) is currently linking multiple current and future high-energy neutrino, cosmic ray, gamma ray and gravitational wave observatories into a single virtual system, facilitating real-time coincidence searches for multimessenger astrophysical transients. AMON will generate alerts that will enable rapid follow-up of potential electromagnetic counterparts. We present the science case, design elements, partner observatories, and status of AMON.

CUORE (Cryogenic Underground Observatory for Rare Events) is a ton-scale experiment aiming to the search of neutrino-less double beta decay in ¹³⁰Te with a projected sensitivity on the Majorana effective mass close to the inverted hierarchy region. The CUORE detector consists of a segmented array of 988 TeO₂ bolometers, organized in 19 towers and operated at a temperature of about 10 mK thanks to a custom cryogenic system which, besides the uncommon scale, observes several constraints from the radio-purity of the materials to the mechanical decoupling of the cooling systems. The successful commissioning of the CUORE cryogenic system has been completed early in 2016 and represents an outstanding achievement by itself. The installation of the detector proceeded along 2016 followed by the cooldown to base temperature at the beginning of 2017. The CUORE detector is now operational and has been taking science data since Spring 2017. With the first ~3 weeks of collected data, we present here the most stringent constraint on the ¹³⁰Te half-live for the neutrino-less double beta decay.

Deep Underground Laboratories are multidisciplinary infrastructures to carry out research on rare events, such as neutrino interactions, proton decay, and dark matter, on geophysics, general relativity, and biology. There are 12 such infrastructures deployed in the north hemisphere. Three new Laboratories are underway, two in the south hemisphere. In the paper some characteristics of the Underground Laboratories are discussed. Synergy between Laboratories is reviewed.

If dark matter annihilates to light quarks in the core of the Sun, then a flux of 236 MeV neutrinos will be produced from the decay of stopped kaons. We consider strategies for DUNE to not only observe such a signal, but to determine the direction of the neutrino from the hadronic recoil. We show that this novel strategy can provide a better handle on systematic uncertainties associated with dark matter searches.

The GERmanium Detector Array (Gerda) experiment located at the INFN Gran Sasso Laboratory (Italy), is looking for the neutrinoless double beta decay of ⁷⁶Ge, by using high-purity germanium detectors made from isotopically enriched material. The combination of the novel experimental design, the careful material selection for radio-purity and the active/passive shielding techniques result in a very low residual background at the Q-value of the decay, about 10⁻³ cts/(keV-kg-yr). This makes GERDA the first experiment in the field to be background-free for the complete design exposure of 100 kg-yr. A search for neutrinoless double beta decay was performed with a total exposure of 46.7 kg-yr: 23.2 kg-yr come from the second phase (Phase II) of the experiment, in which the background is reduced by about a factor of ten with respect to the previous phase. The analysis presented in this paper includes 12.4 kg-yr of new Phase II data. No evidence for a possible signal is found: the lower limit for the half-life of ⁷⁶Ge is 8.0 • 10²⁵ yr at 90% CL. The experimental median sensitivity is 5.8 • 10²⁵ yr. The experiment is currently taking data. As it is running in a background-free regime, its sensitivity grows linearly with exposure and it is expected to surpass 10²⁶ yr within 2018.

The Galactic Center is visible from the South Pole throughout the year, at an inclination of 61°. High energy gamma-rays arriving at the South Pole from this direction, will produce inclined air showers in the atmosphere. Since radio emission of inclined showers leaves a large footprint on the ground, a measurement of the electromagnetic shower component using the radio technique is possible. It is already known that radio detection of air showers helps in the reconstruction of the shower maximum and the energy of the air shower with a very good accuracy. Using radio detectors along with particle detectors enhances the detection accuracy of the air shower events and helps in separating the gamma-ray induced events. IceCube-Gen2, the proposed extension of the IceCube Neutrino Observatory, will enhance both the surface and in-ice capabilities of the facility. Ideas for adding surface radio antennas are under discussion in addition to the upgrade and extension of the IceTop surface array using scintillator detectors. While the scintillators will primarily be used for improving the calibration and lowering the veto energy threshold for distinguishing cosmic ray from astrophysical neutrino events, they can also be used with radio antennas to search for photons of PeV energies from the Galactic Center. Using such a setup at the South Pole can help in the identification of the Galactic Center as a PeVatron. In particular, the key for such a search is to use frequencies higher than the standard frequencies used by air-shower radio experiments, which thereby lowers the energy threshold.

Horizon-T is an innovative detector system constructed to study temporary structure of Extensive Air Showers (EAS) in the energy range above ~10¹⁶ eV coming from a wide range of zenith angles (up to 80°). The system, located at Tien Shan high-altitude Science Station at approximately 3340 meters above the sea level, consists of eight charged particle detection points separated by the distance up to one kilometer. The time resolution of charged particles passage of the detector system is a few ns. This level of resolution allows conducting research of atmospheric development of individual EAS. The total of ~8500 Extensive Air Showers (EAS) with the energy above 10¹⁶ eV has been detected during the ~4000 hours of Horizon-T detectors system operations since October 24, 2016 to April 21, 2017. A notable number of events has a spatial and temporary structure that showed the pulses with several maxima (modals or modes) from several detection points of the Horizon-T at the same time as described further in this work. These modes are separated in time from each other starting from tens to thousands of ns. Some are further classified as unusual event with common structure.

Calorimeters are the key detectors for future space based experiments focused on high-energy cosmic rays spectra measurements. Thus it is extremely important to optimize their geometrical design, granularity and absorption depth, with respect to the total mass of the apparatus, which is among the most important constraints for a space mission. CaloCube is a homogeneous calorimeter whose basic geometry is cubic and isotropic, so as to detect particles arriving from every direction in space, thus maximizing the acceptance; granularity is obtained by filling the cubic volume with small cubic scintillating crystals. A prototype, instrumented with CsI(Tl) cubic crystals, has been constructed and tested with particle beams.

Galactic Cosmic ray (CR) origin is still a mystery. Measuring the knees of the CR spectra for individual species is a very important approach to solve the problem. ARGO-YBJ and LHAASO-WFCTA[1] combined experiment made the first step by measuring the spectrum of hydrogen plus helium nuclei and finding the knee around 0.7 PeV[2]. A significant boost is expected by using LHAASO experiment[3] to measure the spectra and their knees for pure proton and other species in few years. The key is to separate the specific species from all CR samples. In this paper, a multi variate analysis (MVA) approach for the CR composition analysis in LHAASO experiment is discussed. Preliminary results of the analysis and expectations are presented.

The detection of a gravitational wave signal in September 2015 by LIGO interferometers, announced jointly by LIGO collaboration and Virgo collaboration in February 2016, opened a new era in Astrophysics and brought to the whole community a new way to look at - or "listen" to - the Universe. In this regard, the next big step was the joint observation with at least three detectors at the same time. This configuration provides a twofold benefit: it increases the signal-to-noise ratio of the events by means of triple coincidence and allows a narrower pinpointing of GW sources, and, in turn, the search for Electromagnetic counterparts to GW signals. Advanced Virgo (AdV) is the second generation of the gravitational-wave detector run by the Virgo collaboration. After a shut-down lasted 5 years for the upgrade, AdV has being commissioned to get back online and join the two advance LIGO (aLIGO) interferometers to realize the aforementioned scenario. We will describe the challenges and the status of the commissioning of AdV, and its current performances and perspectives.

A few lines wil be also devoted to describe the latest achievements, occurred after the TAUP 2017 conference.

VERITAS has been observing the northern sky at TeV energies with full sensitivity since 2007. Consisting of a ground based array of four 12 m imaging atmospheric Cherenkov telescopes, sited in southern Arizona, it is one of the world's most sensitive detectors of gamma-rays between 85 GeV to 30 TeV. VERITAS maintains a broad scientific programme in many areas of astroparticle physics, including, but not limited to: studies of the acceleration, propagation and indirect measurements of cosmic rays and their spectra; searching for indirect detection signatures of dark matter candidates; and tests of fundamental physics, such as setting constraints on Lorentz invariance violation. There is also an active multi-messenger programme with partners in the electromagnetic, neutrino, and gravitational wave sectors. We review here the current status and some recent results from VERITAS and examine the prospects for future studies.

The High Altitude Water Cherenkov (HAWC) observatory is an air shower detector designed to study very-high-energy gamma rays. In this proceeding we report the most recent scientific results by HAWC that include the detection of 39, point and extended, gamma-ray sources (already known and new) as well as their physical properties. Also HAWC monitors the flux from the Crab Nebula and two nearby active galactic nuclei, Markarian 421 and Markarian 501, every day as well as searching for transient on various timescales from other sources.

The OPERA experiment, designed to search for ν_μ→ν_τ oscillations, reached its main goal by observing the appearance of ν_τ in the CNGS ν_μ beam. Thanks to its location in the underground Gran Sasso laboratory, under 3800 m.w.e., it has also been exploited as an observatory for TeV muons produced by cosmic rays in the atmosphere. In this paper the preliminary measurement of the annual modulation of the atmospheric muon flux with the OPERA detector is reported.

KAGRA is a 3-km interferometric gravitational wave telescope located in the Kamioka mine in Japan. It is the first km-class gravitational wave telescope constructed underground to reduce seismic noise, and the first km-class telescope to use cryogenic cooling of test masses to reduce thermal noise. The construction of the infrastructure to house the interferometer in the tunnel, and the initial phase operation of the interferometer with a simple 3-km Michelson configuration have been completed. The first cryogenic operation is expected in 2018, and the observing runs with a full interferometer are expected in 2020s. The basic interferometer configuration and the current status of KAGRA are described.

From the experimental point of view, very little is known about the gravitational interaction between matter and antimatter. In particular, the Weak Equivalence Principle, which is of paramount importance for the General Relativity, has not yet been directly probed with antimatter. The main goal of the AEgIS experiment at CERN is to perform a direct measurement of the gravitational force on antimatter. The idea is to measure the vertical displacement of a beam of cold antihydrogen atoms, traveling in the gravitational field of the Earth, by the means of a moiré deflectometer. An overview of the physics goals of the experiment, of its apparatus and of the first results is presented.

PAMELA (Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics) is a satellite-borne experiment. It was launched on June 15th 2006 from the Baikonur space centre on board the Russian Resurs-DK1 satellite. For about 10 years PAMELA took data, giving a fundamental contribution to the cosmic ray physics. It made high-precision measurements of the charged component of the cosmic radiation challenging the standard model of the mechanisms of production, acceleration and propagation of cosmic rays in the galaxy and in the heliosphere. PAMELA gave results on different topics on a very wide range of energy. Moreover, the long PAMELA life gives the possibility to study the variation of the proton, electron and positron spectra during the last solar minimum. The time dependence of the cosmic-ray proton and helium nuclei from the solar minimum through the following period of solar maximum activity is currently being studied. Low energy particle spectra were accurately measured also for various solar events that occurred during the PAMELA mission. In this paper a review of main PAMELA results will be reported.

The Pierre Auger Observatory has been designed to investigate the origin and nature of Ultra High Energy Cosmic Rays. The combination of information from a surface array, measuring the lateral distributions of secondary particles at the ground, and fluorescence telescopes, observing the longitudinal profile, provides an enhanced reconstruction capability and opens the way for a multi-messenger approach. A review of selected results is presented, covering the measurement of energy spectrum, arrival directions, and chemical composition. Finally, the motivation and the status for the ongoing major upgrade of the Observatory, AugerPrime, will be discussed with the emphasis given to future perspectives.

The KM3NeT Collaboration aims at the observation of high neutrino sources in the Universe and at the determination of the neutrino mass hierarchy. This talk is focused on ARCA. The deployment of the first Detection Units at 3500 m depth offshore CapoPassero (Italy) started and two are in operation. ARCA will made of two buildings blocks made of 115 Detection Units corresponding to an instrumented volume of about 1 km3 and will provide a very large coverage of the neutrino sky - 87% for up going muon neutrinos). The superior angular resolution, 0.1°at energy higher of 10 TeV, will be important for source search. In this talk the detector technology, status and perspectives for detection of high energy neutrinos signals from different candidate sources are discussed.

SNOLAB is one of the deepest underground laboratory in the world with an overburden of 2092 m. The SNO+ detector is designed to achieve several fundamental physics goals as a low-background experiment, particularly measuring the Earth's geoneutrino flux. Here we evaluate the effect of the 2 km overburden on the predicted crustal geoneutrino signal at SNO+. A refined 3D model of the 50 χ 50 km upper crust surrounding the detector and a full calculation of survival probability are used to model the U and Th geoneutrino signal. Comparing this signal with that obtained by placing SNO+ at sea level, we highlight a 1.4^+1.8_-0.9 TNU signal difference, corresponding to the ~5% of the total crustal contribution. Finally, the impact of the additional crust extending from sea level up to ~300 m was estimated.

The ANTARES deep sea neutrino telescope has been continuously taking data for more than ten years. Thanks to its excellent angular resolution in both the muon channel and the cascade channel, ANTARES offers unprecedented sensitivity for neutrino source searches in the Southern sky in the TeV-PeV energy range, so that already valuable constraints have been set on the origin of the cosmic neutrino flux discovered by the IceCube detector. This document highlights recent results obtained by ANTARES in the search for high energy cosmic neutrinos coming from point or extended sources, from multi-messenger analyses of transient sources, and from indirect searches for Dark Matter.

The SNO+ experiment is located at SNOLAB in Sudbury, Ontario, Canada. It will employ 780 tonnes of liquid scintillator loaded, in its initial phase, with 1.3 tonnes of¹³⁰Te (0.5% by mass) for a low-background and high-isotope-mass search for neutrino-less double beta decay. SNO+ uses the acrylic vessel and PMT array of the SNO detector with several experimental upgrades and necessary adaptations to fill with liquid scintillator. The SNO+ technique can be scaled up with a future high loading Phase II, able to probe to the bottom of the inverted hierarchy parameter space for effective Majorana mass. Low backgrounds and a low energy threshold allow SNO+ to also have other physics topics in its program, including geo- and reactor neutrinos, supernova and solar neutrinos. This will describe the SNO+ approach for the double-beta decay program, the current status of the experiment and its sensitivity prospects.

The Majorana Collaboration has assembled an array of high purity Ge detectors to search for neutrinoless double-beta decay in ⁷⁶Ge with the goal of establishing the required background and scalability of a Ge-based next-generation ton-scale experiment. The Majorana Demonstrator consists of 44 kg of high-purity Ge (HPGe) detectors (30 kg enriched in ⁷⁶Ge) with a low-noise p-type point contact (PPC) geometry. The detectors are split between two modules which are contained in a single lead and high-purity copper shield at the Sanford Underground Research Facility in Lead, South Dakota. Following a commissioning run that started in June 2015, the full detector array has been acquiring data since August 2016. We will discuss the status of the Majorana Demonstrator and initial results from the first physics run; including current background estimates, exotic low-energy physics searches, projections on the physics reach of the Demonstrator, and implications for a ton-scale Ge-based neutrinoless double-beta decay search.

The KArlsruhe TRItium Neutrino (KATRIN) experiment is a large-scale experiment with the objective to determine the effective electron anti-neutrino mass with an unprecedented sensitivity of 0.2 eV/c² at 90% C.L. in a model-independent way. The measurement method is based on precision β-decay spectroscopy of molecular tritium. The experimental setup consists of a high luminosity windowless gaseous tritium source, a magnetic electron transport system with differential and cryogenic pumping for tritium retention, and an electro-static spectrometer section for energy analysis, followed by a segmented detector system for counting transmitted β-electrons. The experiment was constructed at the Karlsruhe Institute of Technology in Germany and is currently in the final commissioning phase before the commencement of tritium operation.

This proceedings will give an overview of the KATRIN experiment and its current status. Furthermore, initial results of recent commissioning measurements of the completed KATRIN beamline will be presented.

The Project 8 collaboration aims to measure the absolute neutrino mass scale using cyclotron radiation emission spectroscopy on the beta decay of tritium. The second phase of the project will measure a continuous spectrum of molecular tritium beta decays and extract the tritium endpoint value with an eV or sub-eV scale precision. Monoenergetic electrons emitted by gaseous ^83mKr atoms are used to determine the relationship between cyclotron frequency and electron energy. This study allows us to optimize both the event reconstruction algorithm and the hardware configuration, in preparation for measuring the tritium beta decay spectrum. Phase II will benefit from a gas system of krypton and tritium that will allow measurement of and offline correction for magnetic field fluctuations. We present the recent progress in understanding the electron kinematics and implementing the magnetic field calibration.

The MAJORANA DEMONSTRATOR is an experiment constructed to search for neutrinoless double-beta decays in germanium-76 and to demonstrate the feasibility to deploy a ton-scale experiment in a phased and modular fashion. It consists of two modular arrays of natural and ⁷⁶Ge-enriched germanium detectors totaling 44.1kg (29.7kg enriched detectors), located at the 4850' level of the Sanford Underground Research Facility in Lead, South Dakota, USA. Data taken with this setup since summer 2015 at different construction stages of the experiment show a clear reduction of the observed background index around the ROI for 0νββ- decay search due to improvements in shielding. We discuss the statistical approaches to search for a धνββ-signal and derive the physics sensitivity for an expected exposure of 10kg· y from enriched detectors using a profile likelihood based hypothesis test in combination with toy Monte Carlo data.

Double electron capture is a rare nuclear decay process in which two orbital electrons are captured simultaneously in the same nucleus. We have conducted an improved search for two-neutrino double electron capture on ¹²⁴Xe and ¹²⁶Xe using 800.0 days of the XMASS-I data. As a result of fitting the observed energy spectra with the expected signal and background, no significant signal is found. Therefore, we set the most stringent lower limits on their half-lives at 2.1 × 10²² years for ¹²⁴Xe and 1.9 × 10²² years for ¹²⁶Xe at 90% confidence level. The limits get improved by a factor of 4.5 compared to the previous result.

ORCA is the low-energy branch of KM3NeT, the next-generation research infrastructure hosting underwater Cherenkov detectors in the Mediterranean Sea. ORCA's primary goal is the determination of the neutrino mass hierarchy by measuring the matter- induced modifications on the oscillation probabilities of few-GeV atmospheric neutrinos. The technical design of the ORCA detector foresees a dense configuration of optical modules, optimised for the study of interactions of neutrinos in the energy range of 3–30 GeV. The first ORCA detection string was successfully deployed on 22nd September 2017 and is providing high-quality data since then.

With an instrumented mass of 8 Mton for the full-size ORCA detector, it will be possible to probe with a high-statistics neutrino sample a wide range of energies and baselines through the Earth. This allows to detmerine the neutrino mass hierarchy with 3 σ after 3–4 years of operation, to probe the unitarity assumption of 3-neutrino mixing with a high-statistics measurement of tau-neutrino appearance in the atmospheric neutrino flux, and to improve the measurement precision on other oscillation parameters.

The NEMO-3 experience was dedicated to the search for neutrinoless double beta decays (0νββ) and to the precise measurements of the two neutrino double beta decays (2νββ). The detector was installed at Laboratoire Souterrain de Modane (LSM) and investigated ββ decays among seven isotopes from 2003 to 2011. Its unique approach combining a calorimetric and a tracking measurement allows to fully reconstruct the ββ event topology with a very low background level. This feature also permits original searches such as the investigation of the hypothetical quadruple beta decay (0ν4β). Its successor, SuperNEMO, is currently under construction at LSM and will extend the sensitivity of the 0νββ search. The latest results from NEMO-3 concerning the ¹⁵⁰Nd and ¹¹⁶Cd isotopes are presented as well as the installation status of the first SuperNEMO module.

The measurement of the Neutrino Mass Ordering (NMO), i.e. the ordering of the neutrino mass eigenstates, is one of the major goals of many future neutrino experiments. One strategy is to measure matter effects in the oscillation pattern of atmospheric neutrinos as proposed for the PINGU extension of the IceCube Neutrino Observatory. Already, the currently running IceCube/DeepCore detector can explore this type of measurement. Albeit with lower significance, such a measurement can contribute to the current understanding. Furthermore, such an analysis exercises the measurement principle and evaluation of systematic uncertainties and thus prototypes future analyses with PINGU. We present a likelihood analysis spanning multiple years of IceCube data searching for indications of the NMO with a data sample reaching to energies below 10 GeV.

Nuclear power reactors account for a small fraction of the Earth's total antineutrino $(\bar{\nu })$ luminosity. Past experiments, with baselines between ~10 m and ~1000 km, have successfully measured the rate and spectrum of reactor-born ${\bar{v}}_{e}\text{S}$. Additionally detecting the incident direction of reactor $(\bar{\nu })$ luminosity. Past experiments, with baselines between ~10 m and ^1000 km, have successfully measured the rate and spectrum of reactor-born ${\bar{v}}_{e}\text{S}$ would constitute an important milestone in the development of reactor monitoring for nuclear non-proliferation since this information could aid in identifying undeclared nuclear reactors. Here we examine the prospects of using low-background, direction-sensitive tracking detectors to remotely monitor nuclear reactors. For an experiment sited at SNOLab, we calculate that an exposure of 56-78 (31-46) tonne-months is needed to detect the flux of ${\bar{v}}_{e}\text{S}$ produced by a 3758-MW reactor at a distance of 13 km at 95% (90%) confidence level.

Neutrinos are elementary particles in the standard model of particle physics. There are 3 flavors of neutrinos that oscillate among themselves and their oscillation can be described by a 3×3 unitary matrix, containing three mixing angles θ₁₂, θ₂₃, θ₁₃, and one CP phase. Both θ₁₂ and θ₂₃ are known from previous experiments. The Daya Bay experiment gave the first definitive non-zero value in 2012. Daya Bay use the 1230 days data to obtain the most precise measurement of sin²2θ₁₃ =0.08421±0.0027(stat.)±0.0019(syst.) and = (math) × 10⁻³eV². Experiment has measured the flux and spectrum of the reactor antineutrino. Flux is consistent with previous short baseline experiments and spectrum different from prediction with significance 4.4σ in 4-6 MeV energy region. Experiment also measure the IBD yield per fission from individual isotopes (²³⁵U, ²³⁹Pu, ²³⁸U, ²⁴¹Pu) and found that IBD yield of ²³⁵U is 7.8% lower than prediction. For light sterile neutrino serach, there are no hint of light sterile neutrino observed from Daya Bay data and give the most stringent limit for (math) <0.2eV².

Borexino has provided an updated upper limit on the effective neutrino magnetic moment of solar neutrinos μ_βα < 2.8 x 10⁻¹¹μ_औ at 90% C.L. This result represents nearly a factor of two improvement with respect to the previous result based on 192 days of the Phase-I data. The current analysis has been performed using 1291.5 days exposure of the Phase-II data, characterized by a further improved level of radio-purity of liquid scintillator. Another key ingredient of the new analysis, lowering the threshold from 260 to 186 keV, was possible thanks to a better understanding of the detector-response function at low energies. The global spectral fit was preformed up to 2970 keV energy, using constraints on the sum of the solar neutrino fluxes implied by the radiochemical gallium experiments. From the limit for the effective neutrino magnetic moment, new limits for the magnetic moments of the neutrino flavour states were derived.

The reactor antineutrino energy spectra and flux were reevaluated during the preparation of the recent experiments devoted to the measurement of θ₁₃. Consequently some discrepancies between data and the theoretical predictions in reactor antineutrino experiments at short distances were observed when using the new predicted flux and spectra. This problem has been called the Reactor Antineutrino Anomaly (RAA), which together with the gallium anomaly, both show discrepancies with respect to the expectations at the ∼ 3 σ level. Oscillations into a light sterile neutrino state (Δm² ~ 1eV²) could account for such deficits. The SoLid experiment has been conceived to give an unambiguous response to the hypothesis of a light sterile neutrino as the origin of the RAA. To this end, SoLid is searching for an oscillation pattern at short baselines (6-9 m) in the energy spectrum of the (math)'s emitted by the SCK • CEN BR2 reactor in Belgium. The detector uses a novel technology, combining PVT (cubes of 5×5×5 cm³) and ⁶LiF:ZnS (sheets ∼ 250 μm thickness) scintillators. It is highly segmented (modules of 10 planes of 16×16 cubes), and it's read out by a network of wavelength shifting fibers and SiPMs. The fine segmentation and the hybrid technology of the detector allows the clear identification of the neutrino signals, reducing significantly backgrounds. Thus, a high experimental sensitivity can be achieved. A 288 kg prototype was deployed in 2015, showing the feasibility of the detection principle. A full scale detector (1.6 tons) is currently under construction, the data taking with the first detector modules is expected by the end of 2017. In this proceeding, the status of the construction and the first results of the calibration of the first SoLid planes are presented.

Borexino is a 300 ton sub-MeV liquid scintillator solar neutrino detector which has been running at the Laboratori Nazionali del Gran Sasso (Italy) since 2007. Thanks to its unprecedented radio-purity, it was able to measure the flux of ⁷Be, ⁸B, pp, and pep solar neutrinos and to detect geo-neutrinos. A reliable simulation of the detector is an invaluable tool for all Borexino physics analyses. The simulation accounts for the energy loss of particles in all the detector components, the generation of the scintillation photons, their propagation within the liquid scintillator volume, and a detailed simulation of the electronics chain. A novel efficient method for simulating the external background which survives the Borexino passive shield was developed. This technique allows to reliably predict the effect of the contamination in the peripheral construction materials. The techniques developed to simulate the Borexino detector and their level of refinement are of possible interest to the neutrino and dark matter communities, especially for current and future large-volume liquid scintillator experiments.

The OPERA experiment reached its main goal by proving the appearance of tau-neutrinos in the CNGS muon-neutrino beam. A total sample of 5 candidates fulfilling the analysis defined in the proposal was detected with a S/B ratio of about ten allowing to reject the null hypothesis with a significance of 5.1 σ. The search was extended to ½_T-like interactions failing the kinematical analysis defined in the experiment proposal, to obtain a statistically enhanced, lower purity, signal sample. One such interesting neutrino interaction showing a double vertex topology with a high probability of being a tau-neutrino interaction with charm production will be reported. Based on the enlarged data sample the estimation of (math) in appearance mode is presented. The search for ½_e interactions has been extended over the full data set with a more than twofold increase in statistics with respect to published data. The analysis of the ν_μ → ν_e channel is updated and the implications of the electron-neutrino sample in the framework of the 3+1 sterile model is discussed. An analysis of the ν_μ → ν_τ oscillations in the framework of the sterile neutrino model has also been performed.

Super-Kamiokande (SK), a 50 kton water Cherenkov detector in Japan, is observing neutrinos and searching for proton decay and dark matter. The installation of new front-end electronics in 2008 marks the beginning of the 4th phase of SK (SK-IV). With the improvement of the water circulation system, calibration methods, reduction cuts, this phase achieved the lowest energy threshold thus far: 3.5 MeV kinetic energy. SK studies the effects of both the solar and terrestrial matter density on neutrino oscillations: a distortion of the solar neutrino energy spectrum would be caused by the edge of the Mikheyev-Smirnov-Wolfenstein resonance in the solar core, and terrestrial matter effects would induce a day/night solar neutrino flux asymmetry. SK observed solar neutrino interactions for more than 20 years. This long operation covers about ∼2 solar activity cycles. An analysis about a possible correlation between solar neutrino flux and 11 year activity cycle will be presented.

Super-Kamiokande (SK) is a 50 kiloton water Cherenkov detector aiming for the detection of several physics such as solar, atmospheric, astrophysical neutrinos, proton decay, WIMP dark matter, etc. It has been running over 20 years since 1996, and achieved several remarkable outcomes in the field of the particle and astrophysics, one of which is the discovery of the neutrino oscillation, bringing the Nobel Prize in physics 2015. SK still accumulates a large number of neutrino events, and simultaneously the physic target and its sensitivity are extended along with the improvement of the analysis method, such as event reconstruction and background rejection. One of the strong motivations for the atmospheric neutrino oscillation measurement is to measure the mass ordering (hierarchy) between ½₂ and ½₃. The atmospheric neutrino is sensitive to the mass hierarchy with help of the matter effect which is given when passing through the Earth. We have performed a detailed analysis to discriminate small signature of the mass hierarchy due to the matter effect. Proton decay is a direct signature anticipated by the grand unified theory (GUT) which is the physics beyond the standard model. Though the major decay modes and GUT models are excluded by the past searches, the efforts to search a glimpse of the proton decay signal are being continued with better event reconstruction and analysis method. In this paper the recent results of the atmospheric neutrino measurement and proton decay search using the most updated dataset taken until 2017 spring are described.

Project 8 is a tritium endpoint neutrino mass experiment utilizing a phased program to achieve sensitivity to the range of neutrino masses allowed by the inverted mass hierarchy. The Cyclotron Radiation Emission Spectroscopy (CRES) technique is employed to measure the differential energy spectrum of decay electrons with high precision. We present an overview of the Project 8 experimental program, from first demonstration of the CRES technique to ultimate sensitivity with an atomic tritium source. We highlight recent advances in preparation for the first measurement of the continuous tritium spectrum with CRES.

Investigation of double beta decay processes (β+EC, EC/EC) of ⁵⁸Ni was performed at the Modane underground laboratory (LSM, France, 4800 m w.e.). A sample of natural nickel, containing ∼68% of ⁵⁸Ni and a mass of ∼21.7 kg, was measured using ultra low-background HPGe detector Obelix (sensitive volume of 600 cm³) during ∼143.8 days. New experimental limits on 2νβ+EC decay of ⁵⁸Ni to the ground 0⁺ and (math), 811 keV excited state of ⁵⁸Fe, and 2νEC/EC decay of ⁵⁸Ni to (math), 811 keV and (maht), 1 675 keV excited states of ⁵⁸Fe were obtained in this measurement. There are -T_1/2(β+EC, 0+ → 0+) > 1.7 × 10²² y; (math), (math), (math). For resonant neutrino-less radiative EC/EC decay with energy of 1 918.3 keV a new experimental limit of T_1/2 (0νEC/EC – res, 1918KeV) > 4.1 ×10²² y was also obtained. All limits are at 90 % CL.

In the recent years, major milestones in neutrino physics were accomplished at nuclear reactors: the smallest neutrino mixing angle θ₁₃ was determined with high precision and the emitted antineutrino spectrum was measured at unprecedented resolution. However, two anomalies, the first one related to the absolute flux and the second one to the spectral shape, have yet to be solved. The flux anomaly is known as the Reactor Antineutrino Anomaly and could be caused by the existence of a light sterile neutrino eigenstate participating in the neutrino oscillation phenomenon. Introducing a sterile state implies the presence of a fourth mass eigenstate, while global fits favour oscillation parameters around sin²(2θ) = 0.09 and Δm² = 1.8eV².

The Stereo experiment was built to finally solve this puzzle. It is one of the first running experiments built to search for eV sterile neutrinos and takes data since end of 2016 at ILL Grenoble, France. At a short baseline of 10 metres, it measures the antineutrino flux and spectrum emitted by a compact research reactor. The segmentation of the detector in six target cells allows for independent measurements of the neutrino spectrum at multiple baselines. An active-sterile flavour oscillation could be unambiguously detected, as it distorts the spectral shape of each cell's measurement differently.

This contribution gives an overview on the Stereo experiment, along with details on the detector design, detection principle and the current status of data analysis.

T2K is a long-baseline neutrino oscillation experiment built to measure ν_μ disappearance and ν_e appearance using the J-PARC neutrino beam and the Super-Kamiokande detector. Presented here are the first results in the search for CP violation in neutrino oscillations with a combined analysis of appearance and disappearance channels using data from both neutrino- and antineutrino-mode beams. The data included in this analysis comprises 7.48×10²⁰ protons on target in neutrino mode, giving 37 electron-like and 135 muon-like events at the far detector, and 7.47 × 10²⁰ protons on target in antineutrino mode, giving 4 electron-like and 66 muon-like events. Including a constraint on sin²(2θ₁₃) from reactor measurements, the 90% confidence interval for δ_CP spans the range [-2.95, -0.44] for the normal mass hierarchy.

Super-Kamiokande (SK) will be upgraded to Super-Kamiokande Gd (SK-Gd). This modification will enable it to identify low energy anti-neutrinos for the world's first observation of the Diffuse Supernova Neutrino Background (DSNB). On average, there is one core-collapse supernova somewhere in the universe each second. The neutrinos emitted from all of these supernovae since the onset of stellar formation have suffused the universe. The flux of the DSNB is expected to be several tens per square centimeter per second. Theoretical models vary, but as many as five diffused supernova neutrinos per year above 10 MeV are expected to interact in SK. However, in order to separate these signals from the much more common solar and atmospheric neutrinos and other backgrounds, we need a new detection method. In 2015, the Super-Kamiokande Collaboration approved the SK-Gd project. It is the upgrade of the SK detector via the addition of water-soluble gadolinium (Gd) salt. Since then, we have been conducting many dedicated studies and developments for deploying Gd to SK.

RENO (Reactor Experiment for Neutrino Oscillation) is the first reactor neutrino experiment which began data-taking in 2011 with two identical near and far detectors in Yonggwang, Korea. Using 1500 live days of data, sin²2θ₁₃ and |Δm²_ee| are updated using spectral measurements: sin²2θ₁₃ = 0.086 ± 0.006 (stat.) ± 0.005 (syst.) and |Δm²_ee| = 2.61⁺⁰¹⁵_-016 (stat.) ± 0.09 (syst.) (×10⁻³ eV²). The correlation between the 5 MeV excess rate and the reactor thermal power is again clearly observed with the increased data set.

The goal of the NEXT experiment is the observation of the neutrinoless double beta decay in ¹³⁶Xe using a gaseous xenon TPC with electroluminescent amplification and specialized photodetector arrays for calorimetry and tracking. After a prototyping period (2009-2014) where the technique was demonstrated, the Collaboration has completed the construction and started the operation of its first phase (NEXT-White or NEW) in the Laboratorio Subterraneo de Canfranc, in the Spanish Pyrenees, with the objectives of measuring in-situ the NEXT background model and the two-neutrino mode of the double beta decay under a radiopure regime. After running NEW, the Collaboration will operate a bigger detector, NEXT-100, which will look for the neutrinoless decay mode.

There is a short overview on the selected issues of neutrino electromagnetic properties with focus on existed experimental constraints and on the effect of neutrino spin precession in the transversal magnetic field and transversal matter current.

In this work we summarize the current status of global neutrino oscillation analyses in the three-neutrino framework. We first describe the different data samples included in the global fit, emphasizing the role of each of them in constraining a given set of parameters. Next, we discuss the main improvements obtained thanks to the consideration of the latest experimental data. The status of the yet-unknown parameters, such as the true neutrino mass ordering, the Dirac CP-violating phase and the octant of the atmospheric mixing angle is also commented. Finally, we discuss some scenarios where the measurement of the reactor mixing angle or the CP violation phase could be significantly affected by the presence of neutrino physics beyond the Standard Model.

We have studied the neutrino-less double beta decay(0νββ) of ⁴⁸Ca by using CaF₂(pure) scintillators. Analysis for rejection of backgrounds(²¹²Bi→ ²¹²Po events and ²⁰⁸Tl events) was effective to reduce backgrounds in Qββ-value region. No events are observed in the Qββ-value region for the data of 131 days × 86 kg. It gives a lower limit (90% confidence level) of (math) > 6.2 × 10²² year (preliminary) for the half-life of 0νββ of ⁴⁸Ca.

The neutrino flux at Earth is dominated in the keV energy range by the neutrinos produced in the Sun through thermal processes, namely photo production, bremsstrahlung, plasmon decay, and emission in free-bound and bound-bound transitions of partially ionized elements heavier than hydrogen and helium. Such a component of the neutrino flux is conspicuously absent from popular analyses of the all-sources spectrum at Earth, whereas if detected it could be a source of information about solar physics. Moreover, it would be the relevant background for keV-mass sterile neutrino dark matter direct searches.

The Jiangmen Underground Neutrino Observatory (JUNO) is a multi-purpose underground experiment and the largest liquid scintillator (LS) detector going for neutrino mass hierarchy, precise measurement of neutrino oscillation parameters and other rare processes which include but not limited to solar neutrino, geo-neutrino, supernova neutrinos and the diffuse supernova neutrinos background. The 20" PMT system with ∼18000 high quantum efficiency phototubes, including Hamamatsu 20" and newly developed NNVT MCP 20" tubes, is the key component of JUNO experiment for better energy resolution, good detector response etc. This article reports the status of the JUNO experiment.

The Deep Underground Neutrino Experiment (DUNE) experiment, a 40-kton underground liquid argon time-projection-chamber detector, will have unique sensitivity to the electron flavor component of a core-collapse supernova neutrino burst. We present the expected capabilities of DUNE for measurements of neutrinos in the few-tens-of-MeV range relevant for supernova detection and its corresponding sensitivity to both neutrino physics and supernova astrophysics. Recent progress and some outstanding issues are highlighted.

The proposed Hyper-Kamiokande experiment (Hyper-K) is a next generation large water Cherenkov (WC) detector with a broad physics program consisting of neutrino beam measurements in search of leptonic CP violation, astrophysical measurements and a search for proton decay. Hyper-K will act as the far detector to measure the oscillated neutrino flux from the long-baseline beam of 0.6 GeV neutrinos/anti-neutrinos produced by a 1.3 MW proton beam at J-PARC in Japan. To minimise systematic uncertainties, particularly due to flux and cross-section uncertainties, detailed measurements of the unoscillated flux are required with a suite of near detectors. We review the challenges, and present the planned components of the near detector measurement suite, including a new intermediate Water Cherenkov Detector.

Hyper-Kamiokande (Hyper-K) is a proposed next generation underground large water Cherenkov detector. We plan to build two cylindrical water tanks in our experimental period, filled with ultra pure water and surrounded with newly developed photo sensors. In total, it will provide the fiducial volume of 0.19-0.37 Mt. The energies, positions, directions and types of charged particles produced by neutrino interactions are detected using its Cherenkov light in water. Our detector will be located at deep underground to reduce the cosmic muon flux and its spallation products, which is a dominant background for the analysis of the low energy astrophysical neutrinos.

With the fruitful physics research programs planned for the accelerator neutrinos, atomospheric neutrinos and nucleon decay, Hyper-K will play an important role in the next neutrino physics frontier, even in the neutrino astrophysics. It will provide remarkable information for both of particle physics and astrophysics with its large statistics of astrophysical neutrino measurements, i.e., solar neutrino, supernova burst neutrinos and supernova relic neutrino. Here, we will discuss about physics potential of Hyper-K neutrino astrophysics and expected performance of the detector.

In a dedicated run where protons from the Fermilab Booster were delivered directly to the steel beam dump of the Booster Neutrino Beamline (BNB), the MiniBooNE detector was used to search for the production of sub-GeV dark matter particles via vector-boson mediators. The signal searched for was the elastic scattering of dark matter particles off nucleons in the detector mineral oil, with neutrinos being an irreducible background. A review of the experiment, its analysis methods, its results and future perspectives are summarized, demonstrating that beam dump experiments provide a novel and promising approach to dark matter searches.

The ANAIS experiment aims at the confirmation of the DAMA/LIBRA signal at the Canfranc Underground Laboratory (LSC). Several 12.5 kg NaI(Tl) modules produced by Alpha Spectra Inc. have been operated there during the last years in various set-ups; an outstanding light collection at the level of 15 photoelectrons per keV, which allows triggering at 1 keV of visible energy, has been measured for all of them and a complete characterization of their background has been achieved. In the first months of 2017, the full ANAIS-112 set-up consisting of nine Alpha Spectra detectors with a total mass of 112.5 kg was commissioned at LSC and the first dark matter run started in August, 2017. Here, the latest results on the detectors performance and measured background from the commissioning run will be presented and the sensitivity prospects of the ANAIS-112 experiment will be discussed.

This report presents the past results, current status and future plans for DAMIC: a search for low-mass dark matter particles with low-noise CCDs. We summarize the extensive laboratory efforts on the characterization of the CCDs and the calibration of their response to potential dark matter signals and radioactive backgrounds. Recent results include exclusion limits on the spin-independent scattering of WIMPs with silicon nuclei and on the absorption of eV-scale hidden-photon dark matter by valence electrons. A 40 g 7-CCD array started operation in February 2017 and data acquisition is ongoing, with results expected in 2018. We outline the future plans for DAMIC-1K, a 1kg 50-CCD array with an ionization threshold of 2 e⁻.

China JinPing underground Laboratory (CJPL) is located about 2400 m below Jinping mountain, providing a unique feature for studies of low-energy neutrinos. A neutrino experiment has been proposed to perform an in-depth research on solar neutrinos, geo-neutrinos and supernova relic neutrinos at Jinping. The physics motivations, the R&D efforts and the present status are reported for a proposed kilo-ton neutrino detector at Jinping. The future prospects are also given.

In this conference paper, I give an overview of the capabilities of DarkBit, a module of the GAMBIT global fitting code that calculates a range of dark matter observables and corresponding experimental likelihood functions. Included in the code are limits from the dark matter relic density, multiple direct detection experiments, and indirect searches in gamma-rays and neutrinos. I discuss the capabilities of the code, and then present recent results of GAMBIT scans of the parameter space of the minimal supersymmetric standard model, with a focus on sensitivities of future dark matter searches to the current best fit regions.

The SABRE (Sodium Iodide with Active Background REjection) experiment will search for an annually modulating signal from dark matter using an array of ultra-pure NaI(Tl) detectors surrounded by an active scintillator veto to further reduce the background. The first phase of the experiment is the SABRE Proof of Principle (PoP), a single 5 kg crystal detector operated in a liquid scintillator filled vessel at Laboratori Nazionali del Gran Sasso (LNGS). The SABRE-PoP installation is underway with the goal of running in 2018 and performing the first in situ measurement of the crystal background, testing the veto efficiency, and validating the SABRE concept. The second phase of SABRE will be twin arrays of NaI(Tl) detectors operating at LNGS and at the Stawell Underground Physics Laboratory (SUPL) in Australia. By locating detectors in both hemispheres, SABRE will minimize seasonal systematic effects. This paper presents the status report of the SABRE activities as well as the results from the most recent Monte Carlo simulation and the expected sensitivity.

The nature of Dark Matter is one of the fundamental questions to be answered. Direct Dark Matter searches are focussed on the development, construction, and operation of detectors looking for the scattering of Weakly Interactive Massive Particles (WIMPs) with target nuclei. The measurement of the direction of WIMP-induced nuclear recoils is a challenging strategy to extend dark matter searches beyond the neutrino floor and provide an unambiguous signature of the detection of Galactic dark matter. Current directional experiments are based on the use of gas TPC whose sensitivity is strongly limited by the small achievable detector mass. NEWSdm is an innovative directional experiment proposal based on the use of a solid target made by newly developed nuclear emulsion films and read-out systems achieving a position accuracy of 10 nm.

Potassium-40 (⁴⁰K) is a background in many rare-event searches and may well play a role in interpreting results from the DAMA dark-matter search. The electron-capture decay of ⁴⁰K to the ground state of ⁴⁰ Ar has never been measured and contributes an unknown amount of background. The KDK (potassium decay) collaboration will measure this branching ratio using a ⁴⁰K source, an X-ray detector, and the Modular Total Absorption Spectrometer at Oak Ridge National Laboratory.

We discuss a dark family of lepton-like particles with their own "private" gauge bosons व_μ and ध_μ under a local SU'(2) × U'(1) symmetry. The product of dark and visible gauge groups SU'(2) × U'(1) × SU_w(2) × U_Y(1) is broken dynamically to the diagonal (vector-like) subgroup SU(2) × U(1) through the coupling of two fields (math) to the Higgs field and the dark lepton-like particles. This defines a new Higgs portal, where the "dark leptons" can contribute to the dark matter and interact with Standard Model matter through Higgs exchange.

The EDELWEISS experiment is a direct search for Weakly Interacting Massive Particles (WIMP) dark matter using an array of twenty-four 860 g cryogenic germanium detectors equipped with a full charge and thermal signal readout. The experiment is located in the ultra-low radioactivity environment of the Modane underground laboratory in the Frejus tunnel. WIMP limits, background rejection factors and measurements of cosmogenic activation recorded in long exposures are used to assess the performance of the third generation of EDELWEISS detectors in view of the search for WIMPs in the mass range from 1 to 20 GeV/c². The developments in progress to pursue this goal in the coming years are also presented.

There are a number of papers that calculate how the limits or positive results of current experiments would be if some specific twist is applied to the standard interpretation framework (e.g., SI interactions with f_p = f_n). These works are usually not performed by members of the experiments, and therefore make very simple assumptions on experimental details like efficiencies. Nevertheless, it is possible to retain this type of information without actually knowing it, by starting from the final exclusion plots and working backwards. This possibility is discussed and exemplified.

Despite several large-scale direct detection experiments operating worldwide, dark matter remains elusive. Not favoured by supersymmetric theories, the low Weakly Interacting Massive Particle (WIMP) mass regime (less than few GeV) has been largely ignored. The NEWS-G project builds on the experience gathered with the operation of the SEDINE detector at the Laboratoire Souterrain de Modane (France). The goal is to construct a 140cm diameter low-background Spherical Proportional Counter (SPC) capable of holding up to 10 bar of gas and to be operated at the SNOLAB underground facility (Canada). The use of low-Z target materials such as Ne, He and H, together with a strict selection of low activity materials will provide sensitivity to WIMP masses down to 0.1 GeV/c2. The detector is expected to be deployed in 2018.

The China Dark Matter Experiment (CDEX) aims at direct searches of light Weakly Interacting Massive Particles (WIMPs) at the China Jinping Underground Laboratory (CJPL) with an overburden of about 2400m rock. Results from a prototype CDEX-1 994 g p-type Point Contact Germanium(pPCGe) detector are reported. Research programs are pursued to further reduce the physics threshold by improving hardware and data analysis. The CDEX-10 experiment with a pPCGe array of 10 kg target mass range is being tested. The evolution of CDEX program into "CDEX-1T Experiment" with ton-scale germanium detector arrays will also be introduced in this study.

Kaluza-Klein (KK) axions produced in the Sun have been proposed to explain several astrophysical anomalies. We searched for the decay of such solar KK axions using 832 × 359 kg • days XMASS-I data. No significant event rate modulation is found, and we set the first experimental constraint on KK axion photon-coupling of 4.8 × 10"¹² GeV⁻¹ for a KK axion number density of (math) = 4.07 × 10¹³ m³ at 90% C.L.

The ANKOK project is a dark matter search experiment using an argon detector specialized for the low mass (∼ 10 GeV/c²) WIMP detection. We are currently proceeding with R&D efforts to understand the background sources, develop and apply new photo sensor that is directly sensitive to 128 nm argon scintillation light and improve electron recoil type background rejection. In the next few years, we are planning to construct such an argon detector in an underground laboratory with enough sensitivity to detect low mass WIMP.

International Axion Observatory (IAXO) is a new generation axion helioscope aiming to search for solar axions and axion-like particles (ALPs) with a signal to background ratio of about 5 orders of magnitude higher than the one achieved by currently the most sensitive axion helioscope, CAST. IAXO relies on large improvements in magnetic field volume and extensive use of X-ray focusing optics combined with low-background detectors. IAXO will probe a substantial unexplored region of the axion and ALP parameter space which is theoretically and cosmologically motivated, and thus will have significant discovery potential. IAXO could also be used to test models of other proposed particles at the low energy frontier of particle physics, like hidden photons or chameleons. In addition, the IAXO magnet could accommodate new equipment to search for relic axions or ALPs potentially composing the galactic halo of dark matter.

DEAP-3600 is a dark matter WIMP (Weakly Interacting Massive Particles) search experiment, which aims to detect nuclear recoils from WIMP scattering in a liquid argon target. At WIMP masses of 100 GeV, DEAP-3600 has a projected sensitivity of 10⁻⁴⁶ cm² for the spin-independent elastic scattering cross section of WIMPs. The beta emissions from the intrinsic ³⁹ Ar present in the natural Ar target, as well as external calibration sources, can be used to tune the energy calibration and position reconstruction in the energy region of interest (ROI) for WIMP signals. These proceedings will present the techniques used to determine the energy response and position reconstruction in DEAP-3600. Using these techniques, the light yield was found to be LY = (math) (fit syst.) ± 0.22(SPE syst.) PE/keV_ee with a fiducial mass for WIMP detection of 2 223 ± 74 kg for the first data set.

The DEAP-3600 experiment, located at SNOLAB, is searching for dark matter with a single phase liquid argon (LAr) target. For a background-free exposure of 3000 kg·yr, the projected sensitivity to the spin-independent WIMP-nucleon cross section at 100 GeV/c² WIMP mass is 10⁻⁴⁶ cm².

The experimental signature of dark matter interactions is keV-scale argon recoils producing 128 nm LAr scintillation photons which are wavelength shifted and observed by 255 PMTs. To reach the large background-free exposure, a combination of careful material selection, passive shielding, active vetoes, fiducialization and pulse shape discrimination (PSD) is used. The main concept of the background rejection in DEAP-3600 is the powerful PSD, employing the large difference between fast and slow components of LAr scintillation light. The designed background level of DEAP-3600 is less than 0.6 events in a 3000 kg·yr exposure. The experiment was filled in November 2016 and is currently taking dark matter search data.

Axion like particles (ALPs) are fundamental pseudo scalar particles with properties similar to Axions which are a well-known extensions of the standard model to solve the strong CP problem in Quantum Chromodynamics. ALPs can oscillate into photons and vice versa in the presence of an external tranversal magnetic field. This oscillation of photon and ALPs could have important implications for astronomical observations, i.e. a characteristic energy dependent attenuation in Gamma ray spectra for astrophysical sources. Here we have revisited the opportunity to search Photon-ALPs coupling in the disappearance channel. We use eight years of Fermi Pass 8 data of a selection of promising galactic Gamma-ray source candidates and study the modulation in the spectra in accordance with Photon-ALPs mixing and estimate best fit values of the parameters i.e. Photon-ALPs coupling constant (g_ʱγγ) and ALPs mass(m_α). For the magnetic field we use large scale galactic magnetic field models based on Faraday rotation measurements and we have also studied the survival probability of photons in the Galactic plane.

I review results from searches for neutrinos from annihilating or decaying dark matter with the IceCube Neutrino Observatory, using data from the fully deployed detector and new event selection algorithms. So far, no signal has been observed and limits have been put on the dark matter lifetime, spin-dependent interaction cross section of dark matter and nucleons, as well as the velocity-averaged dark matter annihilation cross section. We present competitive limits on the annihilation of Galactic halo dark matter with mass between 10 GeV and 300 TeV, which are rather insensitive to the halo density profile. The limits on the spin-dependent scattering cross section from IceCube searches for dark matter annihilations in the Sun set the strongest such bounds for dark matter of mass above 100 GeV. IceCube has searched for halo dark matter decays and set stringent limits on the life time of particles with mass above 10 TeV.

This work presents indirect searches for dark matter (DM) as WIMPs (Weakly Interacting Massive Particles) using neutrino data collected with the Super-Kamiokande detector from 1996 until 2016. The results of the search for WIMP-induced neutrinos from the Sun, the Earth's core and the Milky Way are discussed. We looked for an excess of neutrinos related to a given source as compared to the expected atmospheric neutrino background. No excess of the WIMP-induced neutrinos is observed in any of the analyses. Limits on the WIMP-nucleon spin-dependent/-independent cross sections (Solar & Earth analysis) and on the WIMP self-annihilation cross section 〈σ_AV〉 (Galactic analysis) are derived assuming various annihilation modes and masses of the relic particles.

The CRESST experiment (Cryogenic Rare Even Search with Superconducting Thermometers), located at Laboratori Nazionali del Gran Sasso in Italy, searches for dark matter particles via their elastic scattering off nuclei in a target material. The CRESST target consists of scintillating CaWO₄ crystals, which are operated as cryogenic calorimeters at millikelvin temperatures. Each interaction in the CaWO₄ target crystal produces a phonon signal and a light signal that is measured by a second cryogenic calorimeter. Since the CRESST-II result in 2015, the experiment is leading the field of direct dark matter search for dark matter masses below 1.7 GeV/c², extending the reach of direct searches to the sub-GeV/c² mass region. For CRESST-III, whose Phase 1 started in July 2016, detectors have been optimized to reach the performance required to further probe the low-mass region with unprecedented sensitivity. In this contribution the achievements of the CRESST-III detectors will be discussed together with preliminary results and perspectives of Phase 1.

The Super Cryogenic Dark Matter Search (SuperCDMS) and its predecessor CDMS have been at the forefront of the search for Weakly Interacting Massive dark matter Particles (WIMPs) for close to two decades. Significant improvements in detector technology have opened up the low-mass parameter space (≲ 10 GeV/c²) where the experiment broke new ground with the CDMS low ionization threshold experiment (CDMSlite). Building on this success, SuperCDMS is preparing for the next phase of the experiment to be located at SNOLAB near Sudbury, Ontario. The new experimental setup will provide space for up to ∼200 kg of target mass in a considerably lower background environment. The initial payload of about 30 kg will be a mix of germanium and silicon targets in the form of both background discriminating iZIP and low-threshold HV detectors, pushing the sensitivity towards WIMPs with even lower masses and improving the cross-section reach of SuperCDMS by more than an order of magnitude. The long-term goal is to reach the neutrino-floor below 10 GeV/c². We present the status of and plans for SuperCDMS at SNOLAB.

Germanium detectors with point contact configuration is an exciting detector technology which provides sub-keV sensitivities as low as 100 eV_ee with kg-scale detector mass. This detector technique offers a unique opportunity to realize experiments on dark matter, to enhance the sensitivity of electromagnetic properties of neutrino and coherent elastic scattering of neutrino nucleus with reactor neutrino source. The TEXONO collaboration have been pursuing this research program at the Kuo-Sheng Neutrino Laboratory (KSNL) in Taiwan. We will highlight our results on neutrino electromagnetic properties, search of sterile neutrinos, as well as studies towards observation of neutrino-nucleus coherent scattering. The detector R&D programs which allow us to experimentally probe this new energy window will be discussed. The efforts set the stage and complement the CDEX dark matter experiment at the new China Jinping Underground Laboratory (CJPL) in China.

The interaction properties of cold dark matter particles candidates are known to lead to the structuring of dark matter on scales much smaller than typical galaxies. This translates into a large population of dark matter subhalos inside our Galaxy, which impacts the predictions for direct and indirect searches. We present a model for this subhalo population that accounts for the gravitational effects experienced by those structures (tidal stripping and disk shocking) while remaining consistent with dynamical constraints. The subhalos mass density and annihilation profiles are derived. The impact of subhalos on indirect searches with cosmic rays antiprotons is evaluated using the latest data from the AMS-02 experiment.

XMASS-I is a single-phase liquid xenon detector located underground in Kamioka Observatory mainly aiming direct detection of dark matter. We performed a WIMP search in a fiducial volume containing 96.5 kg liquid xenon using 705.9 live days of data between November 2013 and March 2016. All events remaining in the fiducial volume after data reduction were consistent with only background prediction from careful evaluation of it. In conclusion, a 90% confidence level upper limit on the spin-independent WIMP-nucleon cross section of 2.2×10⁻⁴⁴ cm² for a WIMP mass of 60 GeV/c² was derived.

Neutron-induced backgrounds are among the dominant backgrounds in many low-background experiments. One of the main processes that produce these neutrons is the (α,n) reaction occurring in detector components. We present NeuCBOT, a new tool for calculating (α,n) yields and neutron energy spectra in arbitrary materials. By combining NeuCBOT calculations with ex situ measurements of the radioactive contamination of detector components, we predict the neutron backgrounds in the DEAP-3600 WIMP detector.

NEWAGE is a direction-sensitive direct dark matter search experiment with a three-dimensional gaseous tracking detector (μ-TPC). Our goals are detection of the dark matter - nucleus scattering signal and the investigation of kinematics of the dark matter in the Galaxy. A dark matter search experiment with the NEWAGE-0.3b' detector was performed from Jul. 2013 to Aug. 2016 (RUN14 to Run17). The total live time is 230.16 days which is about 8 times larger than that of our previous measurement. In the analysis, the event selection was improved and the background was reduced to about 1/3 at 50 keV. This work is important to investigate the properties of the dark matter in the Galaxy in the future dark matter research.

In this work, we conducted annual modulation search for dark matter with 2.7 years of data taking with the XMASS-I detector. A total exposure was 800 live days times 832 kg. When we assume Weakly Interacting Massive Particle (WIMP) dark matter elastically scattering on the xenon target, the exclusion upper limit of the WIMP-nucleon cross section was 1.9×10⁻⁴¹cm² at 8 GeV/c². For model independent case, without assuming any specific dark matter model, we did not find any modulation signal with a p-value of 0.11 in the 1-20 keV energy region for the null hypothesis.

GINGER (Gyroscopes IN General Relativity) is a proposal aiming at measuring the Lense-Thirring effect with an Earth based experiment, using an array of ringlasers, which are the most sensitive inertial sensors to measure the rotation rate of the Earth. The long term stability of the apparatus plays a crucial role for this experiment, and an underground location is advantageous from this point of view. GINGERINO is a single axis ring laser located inside the Gran Sasso laboratory. Gingerino has demonstrated that the very high thermal stability of the underground laboratory allows a continuous operation, sensitivity well below fractions of nrad/s, and with a duty cycle above 90% even in free running operation, without stabilisation of the scale factor of the ring laser.

The former Homestake gold mine in Lead, South Dakota, has been transformed into a dedicated facility to pursue underground research in rare-process physics, as well as offering unique research opportunities in other disciplines. The Sanford Underground Research Facility (SURF) includes two main campuses at the 4850-foot level (4300 m.w.e.) - the Davis Campus and the Ross Campus - that host a range of significant physics projects: the LUX dark matter experiment, the MAJORANA DEMONSTRATOR neutrinoless double-beta decay experiment and the CASPAR nuclear astrophysics accelerator. Furthermore, the BHUC Ross Campus laboratory dedicated to critical material assays for current and future experiments has been operating since Fall 2015. Research efforts in biology, geology and engineering have been underway at SURF for 10 years and continue to be a strong component of the SURF research program. Plans to accommodate future experiments at SURF are well advanced and include geothermal-related projects, the next generation direct-search dark matter experiment LUX-ZEPLIN (LZ) and the Fermilab-led international Deep Underground Neutrino Experiment (DUNE) at the Long Baseline Neutrino Facility (LBNF). SURF is a dedicated research facility with significant expansion capability, and applications from other experiments are welcome.

Experiments currently searching for dark matter and studying properties of neutrinos require very low levels of radioactive backgrounds both in their own construction materials and in the surrounding environment. These low background levels are required so that the current and next generation experiments can achieve the required sensitivities for their searches. This presentation will describe the low background measurement facilities currently operating at SNOLAB and will discuss plans and options to expand these facilities to allow for the increased sensitivity required by the next generation of experiments.

In the VIP2 VIolation of the Pauli Exlusion Principle (PEP) experiment at the Gran Sasso underground laboratory (LNGS) we are searching for possible violations of standard quantum mechanics predictions. With high precision we investigate the Pauli Exclusion Principle and the collapse of the wave function (collapse models). We will present our experimental method of searching for possible small violations of the Pauli Exclusion Principle for electrons, via the search for "anomalous" X-ray transitions in copper atoms, produced by "new" electrons (brought inside a copper bar by circulating current) which could have the probability to undergo Pauli-forbidden transition to the ground state (1 s level) already occupied by two electrons. We will describe the concept of the VIP2 experiment taking data at LNGS presently. The goal of VIP2 is to test the PEP for electrons with unprecedented accuracy, down to a limit in the probability that PEP is violated at the level of 10⁻³¹. We will show preliminary experimental results obtained at LNGS and discuss implications of a possible violation.

About 25 year ago LUNA (laboratory for Underground Nuclear Astrophysics) opened the era of underground nuclear astrophysics installing a home-made 50 kV ion accelerator under the Gran Sasso mountain. A second machine, with a terminal voltage of 400 kV, was then installed and it is still in operation. Most of the processes so far investigated were connected to the physics of solar neutrinos and hence to the hydrogen burning phase in stars. The interest in next and warmers stages of star evolution (i.e. helium and carbon burning) pushed a new project based on an ion accelerator in the MV range called LUNA-MV. Thanks to a special grant of the Italian Ministry of Research (MIUR), INFN is now building, inside one of the major halls at Gran Sasso, a new facility which will host a 3.5 MV single-ended accelerator able to deliver proton, helium and carbon beams with intensity in the mA range.

Activation of germanium crystals due to cosmic rays becomes a serious limitation for experiments searching for rare events with germanium detectors. Cosmic ray induced activation of the detector components and, even more importantly, of the germanium itself during production, transportation and storage at the Earth's surface, might result in the production of radioactive isotopes with long half-lives, with a possible impact on the expected background. We present a measurement of the cosmogenic activation in the cryogenic germanium detectors of the EDELWEISS III direct dark matter search experiment. The decay rates measured in detectors with different exposures to cosmic rays above ground are converted into production rates of different isotopes. They are compared to model predictions present in literature and to estimates calculated with the ACTIVIA code.

SHiP is a new general purpose fixed target facility, whose Technical Proposal has been recently reviewed by the CERN SPS Committee and by the CERN Research Board. The two boards recommended that the experiment proceeds further to a Comprehensive Design phase in the context of the new CERN Working group "Physics Beyond Colliders", aiming at presenting a CERN strategy for the European Strategy meeting of 2019. In its initial phase, the 400 GeV proton beam extracted from the SPS will be dumped on a heavy target with the aim of integrating 2 × 10²⁰ pot in 5 years. A dedicated detector, based on a long vacuum tank followed by a spectrometer and particle identification detectors, will allow probing a variety of models with light long-lived exotic particles and masses below O(10) GeV/c². The main focus will be the physics of the so-called Hidden Portals, i.e. search for Dark Photons, Light scalars and pseudo-scalars, and Heavy Neutrinos. The sensitivity to Heavy Neutrinos will allow for the first time to probe, in the mass range between the kaon and the charm meson mass, a coupling range for which Baryogenesis and active neutrino masses could also be explained. Another dedicated detector will allow the study of neutrino cross-sections and angular distributions. ν_τ deep inelastic scattering cross sections will be measured with a statistics 1000 times larger than currently available, with the extraction of the F₄ and F₅ structure functions, never measured so far and allow for new tests of lepton non-universality with sensitivity to BSM physics.

The TREX-DM experiment is conceived to look for low mass WIMPs by means of a gas time projection chamber equipped with novel micromegas readout planes at the Canfranc Underground Laboratory. The detector can hold 20 l of pressurized gas up to 10 bar, which corresponds to 0.30 kg of Ar, or alternatively, 0.16 kg of Ne. The micromegas will be read with a self-triggered acquisition, allowing for effective thresholds below 0.4 keV (electron equivalent). The preliminary background model, following a complete material screening program, points to levels of the order of 1-10 counts keV⁻¹ kg⁻¹ d⁻¹ in the region of interest, making TREX-DM competitive. The status of the commissioning, description of the background model and the corresponding WIMP sensitivity will be presented here.

The HOLMES project aims to directly measure the electron neutrino mass using the electron capture decay (EC) of ¹⁶³Ho down to the eV scale. It will perform a precise measurement of the end-point of the ¹⁶³Ho calorimetric energy spectrum to search for the deformation caused by a finite electron neutrino mass. The choice of ¹⁶³Ho as source is driven by the very low Q-value of the EC reaction (around 2.8 keV), which allows for a high sensitivity while keeping the overall activities to reasonable value (O(10²)Hz/detector), thus reducing the pile-up probability. A large array made of thousands of Transition Edge Sensor based micro-calorimeters will be used for a calorimetric measurement of the EC ¹⁶³Ho spectrum. The calorimetric approach, with the source embedded inside the detector, eliminates systematic uncertainties arising from the use of an external beta-source, and minimizes the effect of the atomic de-excitation process uncertainties. The commissioning of the first implanted sub-array is scheduled for the end of 2017. It will provide useful data about the EC decay of ¹⁶³Ho together with a first limit on neutrino mass. In this paper the current status of the main tasks will be summarized: the TES array design and engineering, the isotope preparation and embedding, and the development of a high speed multiplexed SQUID read-out system for the data acquisition.

A liquid scintillator containing ⁹⁶Zr has been developed for ZICOS experiment. We will use 180 tons of liquid scintillator with 64 % photo coverage of 20 inch photomultiplier. In order to reach the sensitivity [math] ≥ 10²⁷ years, we have to achieve 50 % enrichment of ⁹⁶ Zr and reduce 95 % of ²⁰⁸Tl decay backgrounds. Using Monte Carlo simulation, we could reduce 93 % of ²⁰⁸Tl background with 78 % efficiency for 0νββ signal using difference of Cherenkov hit pattern. For the separation of Cherenkov and scintillation signals, we measured the timing pulse shape of Zr loaded liquid scintillator using FADC digitizer, and we found an inconsistent pulse shape at the rising time with the template of scintillation. Also the event rate with an inconsistent pulse shape seems to have a directionality.

The CONUS experiment (COherent elastic NeUtrino nucleus Scattering) aims at detecting coherent elastic neutrino nucleus scattering of reactor antineutrinos on Germanium. The experiment will be set up at the commercial nuclear power plant of Brokdorf, Germany, at a distance of ∼17 m to the reactor core. The recoil of the nuclei hit by the antineutrinos is detected with four high-purity point contact Germanium detectors with a very low threshold and an overall mass of about 4 kg. To suppress the background, the setup is equipped with a shell-like passive shield and an active muon veto system. The shield and the muon veto have successfully been tested at the shallow depth laboratory at Max-Planck-Institut für Kernphysik. Monte Carlo simulations have been performed to reproduce the prompt muon-induced background and to examine the induced neutron spectrum. Currently, the low threshold Germanium detectors are characterized and the experiment is prepared for commissioning.

The PandaX-III (Particle And Astrophysical Xenon Experiment III) experiment will search for Neutrinoless Double Beta Decay (NLDBD) of ¹³⁶Xe at the China Jin-Ping underground Laboratory II (CJPL-II). In the first phase of the experiment, a high pressure gas Time Projection Chamber (TPC) will contain 200 kg, 90% ¹³⁶Xe enriched gas operated at 10 bar. Microbulk Micromegas, a fine pitch micro-pattern gas detector, will be used for charge readout and enable us to reconstruct tracks of NLDBD events with good energy and spatial resolution. With simulation, we demonstrate excellent background suppression capability with tracking information. In this proceeding, we will give an overview of recent progress of PandaX-III, including data taking of a 20 kg scale prototype TPC.

The Micro-X High Resolution Microcalorimeter X-Ray Imaging Rocket is a sounding rocket mission that will observe Supernova Remnants and search for keV-scale sterile neutrino dark matter. Micro-X will combine the excellent energy resolution of Transition Edge Sensor microcalorimeters with the imaging capabilities of a conical imaging mirror to map extended and point X-ray sources with an unprecedented combination of energy and spatial resolution. The payload has been designed to operate in the challenging conditions of a sounding rocket flight and to achieve sensitive results, in a single five-minute exposure, for each of these science goals. Micro-X's unique design considerations are presented here, along with the status of the instrument and projections for the upcoming flights. The first Micro-X flight in 2018 will observe the Puppis A supernova remnant, where it will attain nearly 13,000 counts in the 300 s exposure. The second Micro-X flight will observe the Galactic Center to search for keV-scale dark matter and explore the nature of the unexplained 3.5 keV line observed by X-ray satellites.

In contrast to WIMPs, light Dark Matter candidates have increasingly come under the focus of scientific interest. In particular the QCD axion is also able to solve other fundamental problems such as CP-conservation in strong interactions. Galactic axions, axion-like particles and hidden photons can be converted to photons at boundaries between materials of different dielectric constants under a strong magnetic field. Combining many such surfaces, one can enhance this conversion significantly using constructive interference and resonances. The proposed MADMAX setup containing 80 high dielectric disks in a 10 T magnetic field would probe the well-motivated mass range of 40–400 _μeV, a range which is at present inaccessible by existing cavity searches. We present the foundations of this approach and its expected sensitivity.

The axion is a hypothetical low-mass boson predicted by the Peccei-Quinn mechanism solving the strong CP problem. It is naturally also a cold dark matter candidate if its mass is below ∼1 meV, thus simultaneously solving two major problems of nature. All existing experimental efforts to detect QCD axions focus on a range of axion masses below ∼25 μeV. The mass range above ∼40 μeV, predicted by modern models in which the Peccei-Quinn symmetry was restored after inflation, could not be explored so far. The MADMAX project is designed to be sensitive for axions with masses (40–400) μeV. The experimental design is based on the idea of enhanced axion-photon conversion in a system with several layers with alternating dielectric constants. The concept and the proposed design of the MADMAX experiment are discussed. Measurements taken with a prototype test setup are discussed. The prospects for reaching sensitivity enough to cover the parameter space predicted for QCD dark matter axions with mass in the range around 100 μeV is presented.

Over almost three decades the TAUP conference has seen a remarkable momentum gain in direct dark matter search. An important accelerator were first indications for a modulating signal rate in the DAMA/NaI experiment (today DAMA/LIBRA) reported in 1997. Today the presence of an annual modulation observed by DAMA, which matches in period and phase the expectation for dark matter, is doubtless and supported at > 9σ confidence. Despite the positive evidence from the DAMA experiment the underlying nature of dark matter is still considered an open and fundamental question of nowadays particle physics. No other direct dark matter search experiment could confirm the DAMA claim up to now; moreover, numerous null-results are in clear contradiction with DAMA under so-called standard assumptions for the dark matter halo and the interaction mechanism of dark with ordinary matter. As both bear a dependence on the target material, resolving this controversial situation will convincingly only be possible with an experiment using sodium iodide (NaI) as target, just like DAMA. COSINUS aims to even go a step further by combining NaI with a novel detection approach. DAMA and all other NaI experiments solely measure the scintillation light created by a particle interaction in the NaI crystal. COSINUS aims to operate NaI as a cryogenic calorimeter reading scintillation light and phonon/heat signal. Two distinct advantages arise from this approach, a substantially lower energy threshold for nuclear recoils and particle identification on an event-by-event basis. These key benefits will allow COSINUS to clarify a possible nuclear recoil origin of the DAMA signal with comparatively little exposure of O(100kg days) and, thereby, answer a long-standing question of particle physics. Today COSINUS is in R&D phase; in this contribution we show results from the 2nd prototype, albeit the first one of the final foreseen detector design. The key finding of this measurement is that pure, undoped NaI is a truly excellent scintillator at low temperatures: We measure 13.1% of the total deposited energy in the NaI crystal in the form of scintillation light (in the light detector).

Massive neutrinos demand to ask whether they are Dirac or Majorana particles. Majorana neutrinos are an irrefutable proof of physics beyond the Standard Model. Neutrinoless double electron capture is not a process but a virtual ΔL = 2 mixing between a parent ^AZ atom and a daughter ^A(Z — 2) excited atom with two electron holes. As a mixing between two neutral atoms and the observable signal in terms of emitted two-hole X-rays, the strategy, experimental signature and background are different from neutrinoless double beta decay. The mixing is resonantly enhanced for almost degeneracy and, under these conditions, there is no irreducible background from the standard two-neutrino channel. We reconstruct the natural time history of a nominally stable parent atom since its production either by nature or in the laboratory. After the time periods of atom oscillations and the decay of the short-lived daughter atom, at observable times the relevant "stationary" states are the mixed metastable long-lived state and the short-lived excited state, as well as the ground state of the daughter atom. Their natural population inversion is most appropriate for exploiting the bosonic nature of the observed X-rays by means of stimulating X-ray beams. Among different observables of the atom Majorana mixing, we include the enhanced rate of stimulated X-ray emission from the long-lived metastable state by a high-intensity X-ray beam. A gain factor of 100 can be envisaged in a facility like European XFEL.

Neutrino fluxes could arise due to annihilation of Weakly Interactive Massive Particles (WIMPs) in the center of the sun. We study the prospects of search for muon events due to such neutrinos at the upcoming Iron CALorimeter (ICAL) detector to be housed at India-based Neutrino Observatory (INO). Although the atmospheric neutrinos will pose a serious background to the signal neutrinos produced through WIMP annihilation, the former could be supressed significantly by using the directional property of signal neutrinos. For 50kt×10 years of ICAL running and WIMP masses (m_χ) between 3-100 GeV, we perform a χ² analysis and present expected exclusion regions in the σ_βख़ — m_x and σ_βι — m_x plane, where σ_βख़ and σ_βι are the WIMP-nucleon Spin-Dependent (SD) and Spin-Independent (SI) scattering cross-sections, respectively. For m_x = 25 GeV, the expected 90 % C.L. exclusion limit on σ_βख़ are σβॄ < 7.82 x 10⁻⁴¹cm² for τ+τ⁻ channel and σ_βख़ < 1.23 10⁻³⁹cm² for 66 channel. For same m_×, the expected 90 % C.L. exclusion limits on σ_βι are σβι < 8.97 × 10⁻⁴³cm² for τ +τ⁻ channel and σβι < 1.43×10⁻⁴¹cm² for 66 channel.

This outreach workshop explains why narrative structure matters in communicating science to the public. It demonstrates the technique by converting a piece of textbook style introduction to an experiment of underground physics (SNO+'s Double Beta Decay study with ¹³⁰Te) into a story for the general public.

The large datasets and often low signal-to-noise inherent to the raw data of modern astroparticle experiments calls out for increasingly sophisticated event classification techniques. Machine learning algorithms, such as neural networks, have the potential to outperform traditional analysis methods, but come with the major challenge of identifying reliably classified training samples from real data. Citizen science represents an effective approach to sort through the large datasets efficiently and meet this challenge. Muon Hunter is a project hosted on the Zooniverse platform, wherein volunteers sort through pictures of data from the VERITAS cameras to identify muon ring images. Each image is classified multiple times to produce a clean dataset used to train and validate a convolutional neural network model both able to reject background events and identify suitable calibration data to monitor the telescope performance as a function of time.

The origin of recently discovered PeV neutrinos is an unsolved problem. In this work we consider a hadronic scenario to produce PeV neutrinos from a region around giant lobes of Centaurus A. Although ultrahigh-energy cosmic rays (UHECRs) are accelerated and confined by giant lobes, they can escape to be later injected in the inter-group medium where galaxies near the giant lobes provides the condition to confine them. UHECRs interact with low-energy photons and protons producing high-energy photons and neutrinos. We found that although the IC35 event cannot be generated inside the giant lobes, this PeV neutrino might be created in galaxies close to the Lobes of Cen A.

Borexino experiment is located at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy, and its primary goal is detecting solar neutrinos, in particular those below 2 MeV, with unprecedentedly high sensitivity. Its technical distinctive feature is the ultra-low radioactive background of the inner scintillating core, which is the basis of the outstanding achievements obtained by the experiment (fluxes of ⁷Be, pep, pp, and limit on CNO). A spectral fit in the whole energy range from 200 keV up to 2 MeV has been performed for the first time, allowing to obtain simultaneously fluxes of all the solar neutrino components. To make such a fit possible, one requires the exact shapes of neutrino signals and backgrounds, as seen in the detector. Therefore, the transformation of the spectra from the original energy scale to the scale of the desired energy estimator, such as the number of hit PMTs or photoelectrons, is one of the key steps of the analysis. This conversion accounts for the energy scale non-linearity and the detector's energy response, and can be performed using two approaches: the Monte Carlo simulation and the use of analytical models. The details and advantages of the analytical approach are presented in this contribution.

CALIOPE, or CP(T) Aberrant Leptons in ortho-Positronium Experiment, is a tabletop search for fundamental symmetry violations, including CP- and CPT-violation, in ortho-positronium (o-Ps). We use a tagged ²²Na source adjacent to a cylinder of aerogel to generate o-Ps at the center of a cylindrical array of 24 NaI(Tl) bars. We search for CPT - violating angular correlations in the gamma rays emitted in the decay of o-Ps. With an angular acceptance of 75% of 4π, and the ability to acquire statistics over a longer period of time, CALIOPE will improve upon the limit set by previous experiments. The experimental setup can also be used in a search for CP-violation in o-Ps with the addition of an electromagnet. We describe the design of the experiment, results from a characterization of the systematics for the CPT- and CP-violating measurements, and a demonstration of the DAQ.

Some neutrino experiments reveal anomalous results which can make room for new physics beyond the three-flavor neutrino oscillation model. These hints suggest the existence of sterile neutrinos with mass m <eV. SOX will be a short-baseline disappearance experiment aiming to test this hypotesis, performed with the liquid scintillator detector Borexino at Gran Sasso National Laboratory in Italy [1]. Due to the good energy and position resolution, a light sterile neutrino can create an oscillatory pattern in the signal. The SOX sensitivity, the related analysis and systematics will be briefly discussed.

The SNO+ experiment has a varied neutrino physics program that includes a neutrino-less double beta decay experiment in addition to reactor, solar, and geoneutrino measurements. SNO+ uses the architecture of SNO, using an acrylic vessel filled with scintillator as its neutrino target suspended in a water volume. At this time data is being collected with the acrylic vessel filled with water in preparation for the scintillator phase. An essential component to the successful execution of this physics program is a calibration of the optical and energetic response of the detector. Calibrations are underway using a laser-driven light source and radioactive gas sources, such as Nitrogen-16, that are to be lowered into the detector vessel on an umbilical. The position can be manipulated in 1-D using the umbilical retrieval mechanisms (URM) or in 2-D using ropes to guide the source off-axis. The sources and drive systems will be presented here with the goals of the calibration in the context of its impact on the SNO+ physics program.

Borexino has performed the first direct, high-precision, wideband solar neutrino spectroscopy of the solar neutrino spectrums main components, including improving the knowledge of the CNO ν flux. Its next-generation short-baseline ¹⁴⁴Ce-¹⁴⁴Pr (math) source program (CeSOX) intends to unambiguously measure or disprove signs of anomalous oscillatory behavior in the low L/E regime. Both programs rely on the detector's unprecedented and record-setting background levels, which are tightening its requirement for background stability. Aiming to minimize background fluctuations (particularly ²¹⁰Po), a new Temperature Monitoring and Management System was deployed. Computational Fluid Dynamics (CFD) simulations are also being developed in order to model, characterize and ultimately predict the subtle fluid currents that might be a hindrance for the required background stability.

The Borexino collaboration has recently released the first simultaneous measurement of the interaction rates of pp, ⁷Be and pep solar neutrinos. This result was made possible by the unprecedented low background of the scintillator during Phase-II, together with new data analysis techniques. We present the data selection strategy of the Borexino solar neutrino analysis: we describe how we select the neutrino-like scintillation events according to event-based cuts which eliminate most of the external and cosmogenic backgrounds. We describe also how the spatial distribution of events and a β+/β⁻ pulse shape discrimination variable are used in a multivariate fit approach to additionally constrain the residual cosmogenic ¹¹C and external backgrounds.

SNO+ is a multipurpose neutrino physics experiment, located 2 kilometers underground in the SNOLAB facility in Sudbury, Canada. It is the successor of the SNO experiment, replacing the heavy water in the Acrylic vessel (AV) with 780 tons of liquid scintillator, Linear Alkyl Benzene (LAB). The AV is surrounded by 7000 tons of ultrapure light water, which shields the detector from naturally occurring radioactivity in the surrounding rock, PMTs, and PSUP. To achieve the radiopurity requirements, the water should be very clean and levels of U and Th contamination in the shielding water must be carefully controlled. A water assay technique, based on the capture of Ra and Th radioisotopes using Hydrous Titanium Oxide (HTiO), was developed by the SNO experiment. Ra sensitivities equivalent to ²³²Th: 4×10⁻¹⁶ gTh/D₂O and ²³⁸U: 3×10⁻¹⁶ gU/g D₂O were achieved with this technique [1]. The HTiO technique will be used in SNO+ to monitor ²³⁸U and ²³²Th contamination levels in the shielding water and the performance of the water purification system.

For the lower energy measurements of interest to SNO+, radon daughter radioisotopes, especially ²¹⁰Po and ²¹⁰Bi supported by ²¹⁰Pb, are also important. Since water will be used in the purification of both the liquid scintillator and tellurium that will be chemically loaded in SNO+ to search for neutrinoless double beta decay, a technique to assay for ²¹⁰Pb in water was desirable. The SNO+ collaboration has extended the HTiO assay technique to allow measurement of ²¹⁰Pb in the water. This technique is capable of measuring 0.4 +/- 0.13 mBq/m³ of ²¹⁰Pb for a 10 tonne assay. The method developed and results of initial ²¹⁰Pb measurements are presented.

Sn-124 is one of the double beta decay isotopes where no measurement of the 2νββ decay rate has been performed. The abundance of the isotope is 5.79%, fairly low, however it can be compensated for by the high loading potential of the natural isotope up to 10% into liquid scintillator without significant light quenching. This work presents results of the LAB based tin loaded liquid scintillator: stability, light yield and possible purification techniques.

The SOX (Short distance Oscillations with boreXino) experiment aims to investigate possible anomalous oscillatory behaviours in neutrinos, including the existence of sterile neutrinos, by exploiting the very low radioactive background of the Borexino detector. A calibration campaign is crucial to achieve a deeper understanding of the energy response and the spatial reconstruction accuracies of the detector. It will be performed with a suite of low-activity radioactive sources which will map the whole active volume, especially nearby the inner vessel. The calibration points at the border of the active zones will be extremely important to study the neutron detection efficiency. The calibration system, already used in Borexino Phase-I, allows the insertion of the sources without perturbing the radio-purity of the detector. The calibration campaign will take place a few months before the beginning of the SOX experiment. In this work, we describe in detail both the calibration hardware and the calibration strategy.

CUORE, the Cryogenic Underground Observatory for Rare Events, is an experiment searching for the neutrinoless double-beta decay of ¹³⁰Te. The first CUORE dataset was acquired in May and June 2017 and consisted of 10.6 kg-yr of TeO₂ exposure, with several days of calibration data before and after the physics dataset. We discuss here the initial performance of the CUORE detector and cryostat in this first dataset.

A thermal calorimetric apparatus was designed, built and calibrated for measuring the activity of the artificial ¹⁴⁴Ce —¹⁴⁴ Pr antineutrino source. This measurement will be performed at the Laboratori Nazionali del Gran Sasso in Italy, just before the source insertion in the tunnel under the Borexino detector and a precision better than 1% is required for a disappearance technique measurement in the SOX (Short distance neutrino Oscillation with BoreXino) project. In this work the apparatus is described and the most important results from the calibration measurements are shown, where the final precision of few per thousand is demonstrated.

A spectral fitter based on the graphics processor unit (GPU) has been developed for Borexino solar neutrino analysis. It is able to shorten the fitting time to a superior level compared to the CPU fitting procedure. In Borexino solar neutrino spectral analysis, fitting usually requires around one hour to converge since it includes time-consuming convolutions in order to account for the detector response and pile-up effects. Moreover, the convergence time increases to more than two days when including extra computations for the discrimination of ¹¹C and external γs. In sharp contrast, with the GPU-based fitter it takes less than 10 seconds and less than four minutes, respectively. This fitter is developed utilizing the GooFit project with customized likelihoods, pdfs and infrastructures supporting certain analysis methods. In this proceeding the design of the package, developed features and the comparison with the original CPU fitter are presented.

The Jiangmen Underground Neutrino Observatory (JUNO) is a 20 kton liquid scintillator detector currently under construction near Kaiping, China. It is located 650 m underground with a baseline of 53 km to two nuclear power plants. The reactor neutrinos are measured via inverse beta decay in order to determine the neutrino mass hierarchy. Muons that cross the detector create a correlated background for this measurement. A set of sub-detectors and sophisticated reconstruction algorithms are presented to achieve an efficient veto of cosmogenic backgrounds while keeping a high exposure. On a sample of through-going muons with the expected mean energy of 215 GeV a spatial bias of less than 10 cm and an angular bias better than 0.5 ° can be reached. There is only 1% additional loss in exposure compared to a perfect tracking.

The MAJORANA DEMONSTRATOR is a ⁷⁶Ge-based neutrinoless double-beta decay (0νββ) experiment. Staged at the 4850 ft level of the Sanford Underground Research Facility, the DEMONSTRATOR operates an array of high-purity p-type point contact Ge detectors deployed within a graded passive shield and an active muon veto system. The present work concerns the two-neutrino double-beta decay mode (2νββ) of ⁷⁶Ge. For Ge detectors, having superior energy resolution (0.1%), this mode poses negligible background to the 0νββ mode, even for a ton-scale experiment. However, the measurement of the 2νββ mode allows for careful systematics checks of active detector mass, enrichment fraction, and pulse shape discrimination cuts related to both the 0νββ and 2νββ decay modes. A precision measurement of the 2νββ shape also allows searches for spectral distortions, possibly indicative of new physics, including 0νββχ. Work is underway to construct a full experimental background model enabling a Bayesian fit to the measured energy spectrum and extraction of a precise 2νββ spectrum and half-life.

An interplay between electromagnetic properties of massive neutrinos and neutrino oscillation phenomena is discussed. The role of neutrino oscillations in the search of neutrino magnetic moments in experiments on low-energy elastic neutrino-electron scattering is emphasized. A general treatment of neutrino spin-flavor oscillations in a magnetic field is presented. An impact of neutrino electromagnetic interactions on Majorana neutrino fluxes from supernovae is pointed out.

In this paper we discuss the possibility of SLν radiation by a neutrino moving in dense matter of a neutron star. We determine a set of conditions inside neutron stars for which the radiation is possible and might have a considerable efficiency.

Electron energy and angular distributions in the process of low-energy elastic neutrino-electron scattering are treated in the free-electron approximation. The effects of the millicharges, magnetic, electric, and anapole moments of massive neutrinos along with the flavor change of neutrinos travelling from the source to the detector are taken into account under the assumption of three-neutrino mixing. The footprints of neutrino electromagnetic interactions in the electron energy and angle distributions are discussed.

We consider the construction of interval estimates for the parameters with one-sided constraints. We show that the so-called method of sensitivity limit yields a correct solution of the problem. Derived are the solutions for the cases of a continuous distribution with non-negative estimated parameter and a discrete distribution, specifically a Poisson process with background. For both cases, the best upper limit is constructed that accounts for the a priori information. Particular applications to the neutrino mass measurements, rare processes (neutrinoless double beta-decay etc.) searches and cosmic ray studies are discussed.

Euclid is an ESA mission designed to understand why the expansion of the Universe is accelerating and what is the nature of the dark energy responsible for this acceleration. By measuring two cosmological probes simultaneously, the Weak Gravitational Lensing and the Galaxy Clustering (BAO and Redshift-Space distorsions), Euclid will constrain dark energy, general relativity, dark matter and the initial conditions of the Universe with unprecedented accuracy. Euclid will be equipped with a 1.2 m diameter SiC mirror telescope feeding 2 instruments: the visible imager and the Near-Infrared Spectro-Photometer. Here the Euclid's observation probes and main aims are recalled, and the NISP instrument and expected performances are presented.

The MAJORANA DEMONSTRATOR is an experiment constructed to search for neutrinoless double-beta decays in germanium-76 and to demonstrate the feasibility to deploy a large-scale experiment in a phased and modular fashion. It consists of two modular arrays of natural and 76 Ge-enriched germanium detectors totalling 44.1 kg, located at the 4850' level of the Sanford Underground Research Facility in Lead, South Dakota, USA. Any neutrinoless double-beta decay search requires a thorough understanding of the background and the signal energy spectra. The various techniques employed to ensure the integrity of the measured spectra are discussed. Data collection is monitored with a thorough set of checks, and subsequent careful analysis is performed to qualify the data for higher level physics analysis. Instrumental background events are tagged for removal, and problematic channels are removed from consideration as necessary.

The energy spectra of galactic cosmic rays carry fundamental information regarding their origin and propagation, but, near Earth, cosmic rays are significantly affected by the solar magnetic field which changes over time. The time dependence of proton and electron spectra were measured from July 2006 to December 2009 by PAMELA experiment, that is a ballooon-borne experiment collecting data since 15 June 2006. These studies allowed to obtain a more complete description of the cosmic radiation, providing fundamental information about the transport and modulation of cosmic rays inside the heliosphere. The study of the time dependence of the cosmic-ray protons and helium nuclei from the unusual 23rd solar minimum through the following period of solar maximum activity is presented.

The High-Energy Particle Detector (HEPD) is one of the payloads of the CSES space mission. The HEPD is built by the Italian Limadou collaboration and has different goals. It will study the temporal stability of the inner Van Allen radiation belts, the precipitation of trapped particles in the atmosphere and the low energy component of the cosmic rays (5-100 MeV for electrons and 15 - 300 MeV for protons). It has been tested at the Beam Test Facility of the INFN National Laboratory of Frascati, for electrons, and at the Proton Cyclotron of Trento, for protons. Here is presented a study of the performance of the apparatus to separate electrons and protons and identify nuclei up to iron.

In this paper we considered semiclassical neutrino spin precession in a transversal matter current and quantum case of the neutrino spin oscillations in the mass and flavor bases induced by a moving media. In the first part we have verified, that even without presence of an electromagnetic field, in presence of a matter, when the transverse matter term is not zero, the neutrino spin oscillations can be induced. In the second part there were some calculations, that in the end led us to the evolution equations which include an effective Hamiltonian of the weak interactions. From these equations one can see the influence of the transverse component of a matter velocity on a spin oscillations and of the longitudinal component of a matter velocity on the neutrino energy spectrum.

The SNO+ detector main physics goal is the search for neutrinoless double-beta decay, a rare process which if detected, will prove the Majorana nature of the neutrinos and provide information on the absolute scale of the neutrino absolute mass. Additional physics goals of SNO+ include the study of solar neutrinos, anti-neutrinos from nuclear reactors and the Earth's natural radioactivity as well as Supernovae neutrinos. Located in the SNOLAB underground physics laboratory (Canada), it will re-use the SNO experiment infrastructure with the 12 m diameter spherical volume filled with 780 tons of Te-loaded liquid scintillator. A short phase with the detector completely filled with water has started at the end of 2016. It will be followed by a scintillator phase expected to start at the end of this year. Continual careful monitoring of the detector state such as its hardware configuration, slow control information, data handling and triggers is required to ensure the quality of the data taken. Several automatic checks have been put in place for that purpose. This information serves as input to higher level run selection tools that will ultimately perform a final decision on the goodness of a run for a given physics analysis.

The excellent energy resolution and low threshold of cryogenic detectors have brought them to the forefront of the search for low-mass Weakly Interacting Massive Particles. The next generation of large cryogenic detectors for dark matter search promises further improvements in sensitivity, yet it is difficult and in some cases impossible to test and fully characterize these detectors in an unshielded environment. Therefore, the Queen's SuperCDMS team is installing a well shielded Cryogenic Underground detector TEst facility (CUTE) at SNOLAB to support detector testing and characterization for SuperCDMS and future cryogenic rare event search experiments. Significant effort is put into achieving a very low background environment which may open the door for early science results with the first set of SuperCDMS detectors during the time the main experimental apparatus is being installed. We discuss some of the challenges and solutions implemented in the design of this facility as well as the status and schedule for the start of operations underground at SNOLAB.

The MAJORANA DEMONSTRATOR is an experiment constructed to search for neutrinoless double-beta decays in germanium-76 and to demonstrate the feasibility to deploy a ton-scale experiment in a phased and modular fashion. It consists of two modular arrays of natural and 76Ge-enriched germanium p-type point contact detectors totaling 44.1 kg, located at the 4850' level of the Sanford Underground Research Facility in Lead, South Dakota, USA. The DEMONSTRATOR uses custom high voltage cables to bias the detectors, as well as custom signal cables and connectors to read out the charge deposited at each detectors point contact. These low-mass cables and connectors must meet stringent radiopurity requirements while being subjected to thermal and mechanical stress. A number of issues have been identified with the currently installed cables and connectors. An improved set of cables and connectors for the MAJORANA DEMONSTRATOR are being developed with the aim of increasing their overall reliability and connectivity. We will discuss some of the issues encountered with the current cables and connectors as well as our improved designs and their initial performance.

The SNO+ experiment is a large-scale liquid scintillator-based experiment, adapting the Sudbury Neutrino Observatory (SNO) detector located at SNOLAB, Canada. The main physics goal is to investigate the Majorana nature of neutrinos through the search for the neutrinoless double-beta decay of ¹³⁰Te. The camera system of SNO+ is designed to photograph calibration sources and triangulate their locations with an accuracy of a couple of centimeters. This will lead to better calibrations and more accurate physics measurements in SNO+. The camera system, when operated in a special mode with underwater lights turned on, also allows monitoring of the physical state of the detector. The optical calibration source was deployed in the water filled SNO+ detector in the summer of 2017. Pictures of the deployed source were taken using the camera system while the underwater lights were turned on. The triangulation analysis of the pictures gave us an opportunity to test the position accuracy of the deployed source in SNO+ using the camera system.

Neutrino oscillations in a constant magnetic field are considered. The backward influence of neutrinos on the environment is accounted for using the density matrix formalism. The entanglement of neutrinos with the magnetic field can destroy quantum coherent superposition of different neutrino states and thus lead to the suppression of neutrino oscillations. The master equation for the neutrino density matrix accounting for the effects of quantum decoherence due to entanglement with the magnetic field is derived.

We investigate new gram-scale cryogenic detectors, 1-2 orders of magnitude smaller in size than previous devices. These are expected to reach unprecedentedly low energy thresholds, in the 10 eV-regime and below. This technology allows new approaches in rare-event searches, including the search for MeV-scale dark matter, detection of solar neutrinos and a rapid discovery of coherent neutrino-nucleus scattering (CNNS) at a nuclear reactor. We show a simple scaling law for the performance of cryogenic calorimeters, allowing the extrapolation of existing device performances to smaller sizes. Measurement results with a 0.5 g sapphire detector are presented. This prototype reached a threshold of 20 eV, which is one order of magnitude lower than previous results with massive calorimeters. We discuss an experiment, called ν-cleus, which enables a 5-σ discovery of CNNS within about 2 weeks of measuring time at 40 m distance from a power reactor. In a second stage, this experiment enables precision measurements of the CNNS cross-section and spectral shape for new physics within and beyond the Standard Model.

CDEX (China Dark Matter Experiment) is now upgraded to about 10 kg HPGe (High Purity Germanium) detectors and new dedicated readout electronics is in operation. The readout system is interfaced to the front preamplifiers, which have two "slow" outputs with typical 20 μs shaping time and two "fast" output with typical 200 ns shaping time. 8 channels 14-Bit 100 MSPS FADC and 2 channels 12Bit 2000 MSPS FADC are embedded in the readout 6U prototype board. The RAIN1000Z2 readout module based on ZYNQ SoC is used for readout with Gigabit Ethernet.

COSINE-100, a direct detection WIMP dark matter search, is using 106 kg of NaI(Tl) crystals to definitively test the DAMA collaboration's claim of WIMP discovery. In the context of most standard models of WIMP dark matter, the DAMA result is in conflict with other direct detection experiments. To resolve this tension, COSINE-100 seeks to independently test the DAMA observation using a detector of the same target material as DAMA, thus definitively confirming or refuting their claim of WIMP discovery. Here, we present the current status and projected sensitivity of COSINE-100, along with the projected sensitivity of COSINE-200, a possible next phase of the experiment.

At the end of a massive star's life, a violent explosion known as a supernova occurs and releases 99% of the star's gravitational binding energy in the form of neutrinos. Although the explosion generates a huge burst of neutrinos, the large distance to earthbound detectors, low cross sections, and flavour changing oscillations can make detection and analysis challenging. Only one neutrino burst from a supernova has ever been detected, but neutrino detectors have been waiting patiently for another. The SNO+ detector at SNOLAB can be used as a supernova detector during both regular operation and calibrations by measuring the burst of neutrinos from a supernova. We present the neutrino detection method and analysis of potential galactic supernova with the SNO+ detector.

A newly completed (Oct. 2016) detector system of Extensive Air Showers (EAS) called Horizon-T (HT) is a part of Tien Shan high-altitude Science Station of Lebedev Physical Institute of the Russian Academy of Sciences, which is located 32 km from Almaty at the altitude of 3340 meters above the sea level. Horizon-T is constructed to study Extensive Air Showers in the energy range above ∼10¹⁶ eV coming from a wide range of zenith angles (0° - 85°). The system currently has eight working and two under construction charged particle detection points separated by the distance more than a kilometer. The ability to record each detector response with accuracy of 2 ns gives HT ability to study the temporary structure of EAS disk and apply the results to the event reconstruction. The reconstruction is therefore based on chronotron (< 0.5 ns), spatial and temporary distribution of charged particles within the detected EAS event. In this paper, we will show the simulated time distribution of charged particles in the EAS disk vs. distance from the axis and the correspondence to the data. A flow of the reconstruction of standard EAS events and the event display is presented as well as recent HT results.