TAUP 2019

Sep 8, 2019, 8:00 AM → Sep 14, 2019, 6:00 PM Japan

Toyama International Conference Center

The biennial TAUP series covers recent experimental and theoretical developments in astroparticle physics by invited plenary review talks and parallel workshop sessions of invited and contributed presentations. The conference is hosted by ICRR, The Univ. of Tokyo, and supported by Kavli IPMU, The Univ. of Tokyo and Univ. of Toyama.

Monday, September 9

1 Welcome and Opening remarks

Speaker: Prof. Masayuki Nakahata (Kamioka Observatory, ICRR, Univ. of Tokkyo)

Slides Web_TAUP2019-welcome-address.pdf

2 Latest gravitational wave observation results

Speaker: Dr Patricia Schmidt (Radboud Univ)

Slides Web_Plenary_I_PSchmidt.pdf

3 Gravitaional wave detectors

Speaker: Dr Fulvio Ricci (Rome University)

Slides Web_Plenary_I_FulvioRicci.pdf

4 Binary black hole formation senarios

Speaker: Dr Sterl Phinney (Caltech.)

Slides Web_PLENARY_I_PHINNEY.pdf

10:30 AM Coffee break

5 Compact binary coalescence physics

Speaker: Dr Yuichiro Sekiguchi (Toho Univ.)

Slides Web_Plenary_II_Sekiguchi.pdf

6 Multimessenger signature of compact binary coalescense

Speaker: Dr Masaomi Tanaka (Tohoku Univ.)

Slides Web_PLENARY_II_Tanaka.pdf

7 Dark matter candidates and strategies for future

Speaker: Dr Hitoshi Murayama (UC Berkeley, Kavli IPMU Univ. Tokyo)

Slides TAUP_2019.pdf

DM1: Axion and Axion-Like Dark Matter I

Convener: Moriyama

8 Current Results and R&D Efforts for Higher Frequency Axion Searches with HAYSTAC

Axions represent a leading class of dark matter candidate that has gained considerable interest in recent years. In order to probe the largely unexplored axion parameter space across multiple frequency decades, new experimental techniques are required. The HAYSTAC (Haloscope At Yale Sensitive To Axion Cold dark matter) experiment is a tunable microwave cavity experiment searching for axions, which also serves as an R&D testbed for new technologies in the 10-100𝜇eV mass range. HAYSTAC phase 2 will utilize Josephson parametric amplifiers to create squeezed states for the first time in a haloscope measurement. Evading the quantum noise can lead to an increase of up to a factor of two in the spectral scan rate. In this talk, I will review the phase 1 results, discuss the current phase 2 efforts and describe the latest R&D efforts currently underway to further expand the sensitivity and reach of the HAYSTAC experiment.

Speaker: Dr Alexander Leder (UC Berkeley)

Slides TAUP 2019 - HAYSTAC talk

9 MADMAX: A QCD Axion Direct-Detection Experiment

Axions emerge naturally from the Peccei-Quinn (PQ) mechanism which addresses the absence of CP violation in the strong interaction, and they can make up the cold dark matter in the universe. If PQ symmetry breaking had occurred before inflation, the axion mass would likely range from $\sim40 ~\mu$eV to $\sim1$ meV, which is yet to be explored experimentally. We present a new experiment dedicated to the direct detection of QCD axion dark matter in the mass range of 40 to 400 $\mu$eV — the MAgnetized Disc and Mirror Axion eXperiment (MADMAX). Multiple dielectric discs and a mirror are placed in a strong magnetic field to utilize the axion-induced coherent electromagnetic emissions from each disc surface and the resonance effect therein, such that the axion-induced signal can be boosted to a level detectable by state-of-the-art low noise amplifiers. We will discuss the motivation, design and sensitivity of MADMAX; ongoing R&D studies and the project roadmap will also be presented.

Speaker: Dr Xiaoyue Li (Max Planck Institute for Physics)

Slides taup2019_madmax_li_xiaoyue.pdf

10 The Dark Matter Radio: Searching for QCD Axion Dark Matter Below 1 Micro-eV Abstract

One of the most enduring mysteries in particle physics is the nature of the non-baryonic dark matter that makes up 85% of the matter in the universe. The QCD axion, which solves the strong CP problem and the hierarchy problem, is also one of the most strongly motivated dark matter candidates. After recent theoretical work, it has become clear that the QCD axion can be naturally produced in the observed dark matter abundance over its entire mass range down to ~peV. The Dark Matter Radio is an experiment that searches for QCD axions with mass below ~micro-eV through their coupling to a lumped-element electromagnetic resonators. The operating principles of DM Radio have been demonstrated in two pathfinder experiments: ABRA-10cm, and the DM Radio Pathfinder. Building on these two demonstrations, the combined DM Radio team is progressing towards the ultimate realization - DM Radio Cubic Meter (DMRadio-m3), which will probe the QCD axion over a large mass range, with sensitivity to the KSVZ and DFSZ benchmark axion models. We will describe the science goals and optimization of DMRadio-m3. We will also describe how the science reach of DMRadio-m3 can in the future be enhanced by the use of quantum sensing to achieve sensitivity to DFSZ axions to a factor of 250 in mass, from ~4 neV to ~1 micro-eV.

Speaker: Prof. Kent Irwin (Stanford University)

Slides IrwinTAUPv3.pdf

11 DANCE: Dark matter Axion search with RiNg Cavity Experiment

Axion is a hypothetical particle originally introduced to solve the strong CP problem in QCD, and a plentitude of axion-like particles (ALPs) are predicted by high energy physics such as string theory. Also, ALPs which have a mass smaller than eV are cosmologically well-motivated candidates of dark matter. Recently, we proposed a new experiment to search for axion dark matter by measuring the phase velocity difference between two circular-polarizations of the laser beam using an optical ring cavity. With our ring cavity, sensitivity to axion-photon coupling constant can reach several orders of magnitude better than the current bound for axion mass m < 10^{-10} eV [Phys. Rev. Lett. 121, 161301 (2018)]. In this talk, we present the principles and the status of DANCE (Dark matter Axion search with RiNg Cavity Experiment) project.

Speaker: Dr Yuta Michimura (University of Tokyo)

Slides TAUP2019_michimura.pdf

12 Updates from the Second Run of the ABRACADABRA-10 cm Axion Dark Matter Search

The presence of dark matter provides some of the most tangible evidence for the existence of physics beyond the Standard Model. Separately, long standing problems within the Standard Model point to new feebly interacting particles to help explain away unnatural fine-tunings. The axion was originally proposed to explain the Strong-CP problem, but was subsequently shown to be a uniquely elegant candidate for explaining the dark matter abundance of the Universe. ABRACADABRA is an experimental program to search for ultralight axion-like dark matter in the sub-$\mu$eV mass range all the way down to the QCD coupling range. The ABRACADABRA-10 cm prototype took first data in 2018 and demonstrated an important proof-of-principle of the detection approach. In this talk, I will present early results from the second run of the ABRACADABRA-10 cm prototype, which aims to improve the sensitivity by an order of magnitude and explore never-before tested regions of the axion-like dark matter parameter space.

Speaker: Dr Jonathan Ouellet (Massachusetts Institute of Technology)

Slides ABRA_TAUP_2019_09_Ouellet.pdf

DM2: WIMP Dark Matter I

Convener: moriyama

13 The XENONnT experiment

To further increase the WIMP discovery potential, the XENON collaboration is building the XENONnT detector with a target xenon mass of about 8 ton. The large target mass combined with an approximately $10\times$ lower background than in its predecessor XENON1T, will increase the sensitivity by an order of magnitude to $2\cdot 10^{-48}\mbox{cm}^2$ for a spin-independent WIMP-nucleon cross section. In this talk, I will focus on the XENONnT physics program as well as its design and construction, with special attention to the major challenges in the radioactive background reduction needed to achieve the required increase in sensitivity. Key to success will be the new liquid xenon circulation system, a new neutron veto surrounding the detector, and a new continuous radon distillation system.

Speaker: Auke Colijn (Nikhef)

Slides XENONnT_TAUP2019.pdf

14 Low Mass Wimp Result with DarkSide-50 and Prospects for Future Experiments using LAr

The DarkSide-50 apparatus is a dual phase Liquid Argon TPC, filled with low-radioactivity underground Argon and installed at the Laboratory Nazionali del Gran Sasso (LNGS) of INFN. In this presentation we will present the results of an analysis, dedicated to the search of WIMPs with masses below 20 GeV/c^2, that uses solely the ionisation signal for which DarkSide-50 is fully efficient starting from 0.1 keVee. The observed rate in the detector at 0.5 keVee is about 1.5 events/keVee/kg/day. We obtain a 90% C.L. exclusion limit above 1.8 GeV/c^2 for the spin-independent cross section of dark matter WIMPs on nucleons, extending the exclusion region for dark matter below previous limits in the range 1.8-6 GeV/c^2. The perspectives for larger LAr detectors, such as the DarkSide 1ton prototype and DarkSide-20k, in the search of low-mass WIMPs will also be discussed.

Speaker: Prof. Sandro De Cecco (Sapienza University &amp; INFN Rome, Italy)

Slides DarkSide_LowMass_TAUP2019_De_Cecco.pdf

15 The LUX-Zeplin Dark Matter Experiment

The nature and origin of Dark Matter are among the most compelling mysteries of contemporary science. For over three decades, physicists have been trying to detect Dark Matter particles via collisions on target nuclei, with little success. The LZ collaboration is building a massive Dark Matter detector, which is currently being installed at the 4850 level of the Sanford Underground Research Facility in Lead, South Dakota. This detector features 7 active tons of target nuclei and use the established liquid xenon TPC technology to achieve unprecedented sensitivity to a wide range of Dark Matter candidates. In this talk, I will review the status of the LZ construction and installation, together with the physics reach of the experiment.

Speaker: Alden Fan (SLAC)

Slides AFan_LZstatus_TAUP2019.pdf

16 Results from PICO 60 and status of the PICO 40L experiment

The PICO 2L and PICO 60 bubble chambers have advanced the sensitivity of searches for spin dependent dark matter interactions significantly in recent years. The second data set from the PICO 60 detector was analyzed using new calibration data. The new data also includes operation at lower thresholds that enhance the parameter space for PICO towards lower dark matter mass. PICO 60 was ultimately background limited and therefore decommissioned in 2017. PICO 40L has taken its place at SNOLAB and we will present the status of the experiment and show the first signals from the new chamber.

Speaker: Prof. Carsten Krauss (University of Alberta)

Slides TAUP_2019_CBKrauss_PICO_40_Status_Sept_09_2019_.pdf

17 Recent Results from the PandaX-II Experiment

The PandaX is a series xenon-based experiments searching for dark matter candidates in the China Jinping underground Laboratory (CJPL). PandaX-II, with a 580-kg liquid xenon TPC, has recently finished its data taking, with a total exposure of more than 400 live-day. In this talk, I will present an overview of the project and discuss the recent results from PandaX-II.

Speaker: Dr Xiaopeng Zhou (Beihang University, Beijing, China)

Slides PandaX-II_results_@_TAUP2019_jianglai_V1.pptx

Gravitational Wave #1

18 Overview of KAGRA

KAGRA, laser interferometer with arm-length 3km, aims at detecting gravitational waves and developing gravitational wave astronomy. KAGRA has two features, the underground site and the cryogenic mirrors. In April 2019, most of the installation activities for KAGRA had been completed. After about a half of year commissioning work, KAGRA will join the international gravitational wave observation with LIGO and Virgo, O3. I will talk about the current status of KAGRA.

Speaker: Prof. Masatake Ohashi (ICRR)

Slides KAGRA_TAUP2019.pdf

19 Cryogenic system at underground site for Large-scale Cryogenic Gravitational Wave Telescope, KAGRA

Large-scale cryogenic gravitational wave telescope in Japan, KAGRA, an interferometer having 3 km in length of arms to detect gravitational waves. The notable features of KAGRA are four main mirrors of the interferometer are cooled down below 20 K in order to reduce thermal noise, and installed underground in a mine to isolate it from seismic activities on the ground. A cryo-payload consisting of the mirror and its suspension system is connected with two very-low-vibration cryo-cooler units as cooling devices, and is surrounded by the thermal radiation shield around 20K in a cryostat. Installation works for the four cryo-payloads into the cryostats were completed on the end of February 2019, and started to cool down to 20K after check. One month after, three cryo-payloads were reached around 20 K, and kept required design temperature. The interferometer with cryo-mirrors is now undergoing commissioning work to join O3. Status of the cryogenic system for KAGRA and its performance including troubleshooting at the underground site will be presented in the conference.

Speaker: Prof. Nobuhiro KIMURA (ICRR)

Slides 20190909_TAUP2019_Final.pptx

20 Vibration Isolation System for the Cryogenic Mirrors in KAGRA

KAGRA is a laser interferometric gravitational wave telescope constructed in an underground site in Japan. Gravitational wave events of more than ten from compact binary coalescences have been observed by LIGO and Virgo that brought us observational evidences about astrophysics in strong gravity. Participation of KAGRA in the gravitational wave detector network can improve accuracy of the source localization and isotropy of the network sensitivity, leading to further understandings of the physical properties of the sources. One of the most critical issue in building a gravitational wave detector is reduction of the instrumental noises. Mirrors in a ground-based laser interferometer are subject to seismic disturbances that cause fluctuation of the mirror position and hence a noise source in gravitational wave observation. In the case of KAGRA, underground environment has small seismic motions of about $10^{-10}$ m/Hz$^{1/2}$ at 10 Hz in the spectrum that is by 1-2 orders of magnitude smaller than ones in other detector sites. However, observing gravitational wave strains in KAGRA requires an extremely small displacement noise of the mirrors that must be less than $10^{-19}$ m/Hz$^{1/2}$ at 10 Hz. Thus, additional schemes of reducing the mirror displacement noise is necessary. We present a vibration isolation system used for the cryogenic mirrors in KAGRA. This system, called Type-A suspension, isolates the mirrors from seismic motions by using a pendulum as a second-order low-pass filter in vibration transmission. The Type-A suspension is a nine-stage pendulum with the height of 13.5 m based on the second floor of the underground mine. The top of the suspension has a pre-isolation stage supported by three inverted pendulum legs. The following suspension chain consists of cascaded geometric anti-spring filters. These mechanical components show a negative-stiffness behavior that reduces their effective stiffness and results in low-frequency mechanical resonances. The bottom four stages including the sapphire mirror are called cryogenic payload and cooled down to about 20 K in order to reduce thermal noises. The whole of this suspension realizes seismic attenuation by $\sim10^{-21}$ in the horizontal direction and $\sim10^{-11}$ in the vertical direction at 10 Hz. Whereas its superior seismic attenuation performance, the suspension system has a negative aspect of amplifying the mirror fluctuation at its resonant frequencies. The excess of the mirror displacement even at an out-of-band frequency disturbs stable operation of the interferometer. Therefore, we need to implement local control of the mirror and its suspension in order to make the system sufficiently robust against external disturbances. Although a large gain of the control can stabilize the mass position more robustly, it will contaminate the control loop with the intrinsic sensor noise that deteriorates suppression of the mirror displacement noise in a stationary state. Hence, design of the local control of the suspension is an important issue to compromise stability of the interferometer operation with less control noise. This talk addresses the details of the Type-A suspension and its control strategy. KAGRA is under the commissioning campaign towards the participation of the 3rd observation run conducted by the gravitational wave observatories in operation. The control demonstration of the Type-A suspension regarded as the first ten-meter-scale underground suspension system with cryogenic components are of importance not only for KAGRA but for the future plans and upgrades of gravitational wave detectors.

Speaker: Dr Koki Okutomi (ICRR, University of Tokyo)

Slides taup2019_okutomi.pdf

21 Interferometer control of KAGRA

KAGRA is a gravitational wave (GW) detector under construction in Japan. The world-wide gravitational detector network started the third observation run (O3) in April 2019, and KAGRA construction is proceeding to join O3 as soon as possible. An interferometric GW detector, such as KAGRA, observes GWs by measuring the distance fluctuation between two free-masses. To measure this distance fluctuation, the optical interferometer is used. The basic configuration of the interferometer is a Michelson interferometer. In addition to it, four optical cavities are composited with the Michelson interferometer to enhance GW signals. For GW detection, the relative positions of the mirrors composing the interferometer have to be controlled on the operation point. The difficulty of the interferometer control is to control 5 degrees of freedom (DoFs) simultaneously within the sub-nm order residual motion. In KAGRA, most of the hardware is installed and they are being integrated to control the interferometer stably. In this presentation, we will report the status of the interferometer control in KAGRA.

Speaker: Dr Masayuki Nakano (Toyama Univ.)

Slides main.pdf

22 Global control using a laser strainmeter for KAGRA

KAGRA is a large scale laser interferometric gravitational wave (GW) telescope constructed in an underground in Japan. Comparing to GW telescopes on the ground surface, the underground telescopes such as KAGRA and the planned Einstein Telescope have an advantage of substantially reduced seismic noise above 1 Hz. However, even in underground, seismic motions at low frequencies such as the microseism (~ 100 mHz) and earthquakes ( > 10 mHz), could degrade the stability of GW telescope. In the current design, these disturbances are conventionally suppressed by feedback control with inertial sensors such as seismometers and geophones. However, suppression with this control method is limited by the insufficient sensitivity and tilt-holizontal coupling of the sensors at low frequency. In KAGRA, this problem can be solved by using a laser strainmeter called Geophysics Interferometer (GIF) which is installed in the KAGRA tunnel and have a good sensitivity bellow 100 Hz with no tilt coupling issues. We propose a new real-time control method using GIF to realize further stability of interferometer operation.

Speaker: Mr Koseki Miyo (Institute for Cosmic Ray Research, University of Tokyo)

Slides 2019Sep09_TAUP.pdf

23 Construction and the operation of the interferometer control system and the DAQ system for KAGRA

Advanced LIGO and advanced Virgo started the 3rd observing (O3) run from April 2019. KAGRA will join O3 run from the end of 2019. We completed the construction of KAGRA and now conduct the commissioning test. The interferometer control system and the DAQ system was also constructed. KAGRA provides more than 100,000 channels and stored data rate reaches more than 10MB/s. These data is transferred from internal Kamioka mine to Kashiwa and the other data analysis site. I will report the current status and the O3 plan of the KAGRA computer systems.

Speaker: Dr Takahiro Yamamoto (ICRR, The University of Tokyo)

Slides taup2019_yamat.pdf

HECR #1

Convener: Prof. Yoshiki Tsunesada (Osaka City University)

24 Neutrino Oscillations in ultralong gamma ray bursts

We study high-energy neutrino production in collimated jets inside blue supergiant (BSG) progenitors of gamma-ray bursts (GRBs). Assuming ultralong GRBs, cosmic ray acceleration and neutrino production at the point where collimation begins, we use a semi-analytic approach to calculate the neutrino injection spectrum. These are then propagated through simulations, taking into account charged and neutral current interactions with matter, to find the observed neutrino fluxes and flavor ratios on Earth. We observe a smooth transition in the flavor ratio from 1:0.85:0.85 to 1:1.58:1.53 for injections close to the progenitor's edge in the 100TeV-1PeV region. For neutrino production deeper in the progenitor, we find oscillations in the flavor ratio around the 1:1:1 mark for energies between 1TeV and 10TeV. This behavior may be useful, in future neutrino detectors with precise flavor ratio measurements, to obtain information about the progenitor. Assuming typical values for ultralong GRB parameters, we see that jet luminosities $\sim 10^{45}$ erg s$^{-1}$ and uncollimated jet Lorentz factors $\sim 50$ provide a good explanation to the IceCube event spectrum up to 1 PeV. Our method can be applied to quantitative tests of GRB neutrinos and impact the allowed GRB parameter space.

Speaker: Mr Jose Carpio (Pennsylvania State University)

Slides Neutrino_Oscillations_in_Ultralong_GRBs.pptx

25 Neutrino Distributions for a Rotating Core-collapse Supernova with a Boltzmann-neutrino-transport

We simulate the collapse of a rotating core of the progenitor with 11.2 solar mass with the Boltzmann-radiation-hydrodynamics code, which solves the Boltzmann equations for neutrino transfer directly. We pay particular attention to the neutrino distribution in phase space, which is affected by the rotation. By solving the Boltzmann equations directly, we can assess the rotation-induced distortion of the angular distribution in momentum space, which gives rise to the rotational component of the neutrino flux. We compare the Eddington tensors calculated both from the raw data and from the M1-closure approximation. We find that the difference in the Eddington factors reaches $\sim20\%$ in our simulation. This is due to the different dependence of the Eddington and flux factors on the angular profile of the neutrino distribution function, and hence modification to the closure relation is needed.

Speaker: Dr Akira Harada (ICRR)

Slides TAUP2019Harada.pptx

26 Supernova neutrinos in the proto-neutron star cooling phase and nuclear matter

A proto-neutron star (PNS) is a newly formed compact object in a core collapse supernova. Using a series of phenomenological equations of state (EOS), we have systematically investigated the neutrino emission from the cooling process of a PNS. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. As a result, the cooling timescale evaluated from the neutrino light curve is found to be longer for the EOS models with small neutron star radius. We discuss how to extract the properties of a PNS (such as mass and radius) and the nuclear EOS.

Speaker: Dr Ken'ichiro Nakazato (Kyushu Univ.)

Slides 190909toyama.pdf

27 Neutrino Flavor Evolution in Dense Neutrino Media

Neutrino flavor evolution in dense neutrino media is a very nonlinear and rich phenomenon. Such dense neutrino media could be found in, but not limited to, core-collapse supernovae (CCSNe). It is of great importance to study neutrino flavor oscillations in CCSNe due to its important consequences for the matter composition, the SN dynamics and also for the observed neutrino spectra on earth. In this talk, I will discuss how a recently discovered phenomenon, the so-called "fast modes", could impact neutrino flavor evolution in CCSNe.

Speaker: Dr sajad abbar (APC, Paris)

Slides PARALLEL-SESSION-HECR#1-Abbar.pdf

Neutrino #1

Convener: Dr Itaru Shimizu (Tohoku University)

28 Accuracy improvement of the atmospheric neutrino flux prediction using observed muon spectra at mountain altitude

We have studied the low energy atmospheric neutrino and atmospheric muon to improve the precision of the atmospheric neutrino flux prediction at low energies by the comparison of observed and calculated muon fluxes. We find the study using the muon flux observed at ~4,000 m A.S.L. is most effective to improve the precision of the low energy atmospheric neutrino flux prediction.

Speaker: Dr Morihiro Honda (ICRR university of Tokyo)

Slides honda-190909.pdf

29 Standard Oscillation Physics with Deepcore and IceCube

The IceCube neutrino observitory is a cubic km neutrino telescope located at the geographic South Pole. DeepCore is an infill array of the IceCube Neutrino Observatory and enables observations of atmospheric neutrinos with energies as low as 5 GeV. These lower energy atmospheric neutrinos allow for a broad range of particle physics including the measurement of standard neutrino oscillations. In this talk I will discuss the recent oscillation results from IceCube/DeepCore and go over the future prospects of oscillation physics at the South Pole.

Speaker: Prof. Juan Pablo Yanez (University of Alberta)

Slides yanez_icecube_taup19_std_oscillations.pdf

30 Probing BSM physics via neutrino oscillations with IceCube DeepCore

Since 2010 DeepCore, the more densely instrumented portion of the IceCube Neutrino Observatory array, has been detecting atmospheric neutrino interactions via Cherenkov radiation in the optically clear, deep ice at the South Pole. Analysing only three years of data has yielded the most precise measurements of the atmospheric neutrino oscillation parameters above 5 GeV. Measuring oscillations at these high energies, well above the tau-production threshold, and over extremely long baselines, provides strong constraints on new, Beyond Standard Model physics in a region of phase space uniquely accessed with atmospheric neutrinos. This talk will report the most recent searches for non-standard atmospheric neutrino oscillations with IceCube DeepCore.

Speaker: Dr Summer Blot (DESY)

Slides SBlot_BSM_osc_IceCube.pdf

31 High-energy particle physics with IceCube

While the Standard Model has experienced great predictive success, the neutrino sector still holds opportunities for surprises. Numerous ongoing and planned experiments exist to probe neutrino properties at low energies. The IceCube Neutrino Observatory, comprised of over 5000 photomultiplier tubes (PMT) situated in a cubic-kilometer of ice at the geographic South Pole, lies in a unique position to measure neutrinos at energies of a TeV and higher. The IceCube collaboration first published evidence of astrophysical neutrinos in 2013 and recently found compelling evidence of an astrophysical source. In this talk, I discuss several exciting particle physics measurements using IceCube data. In particular, I will highlight a new neutrino cross section measurement using the high-energy starting event (HESE) sample and the first detection of an event at the Glashow resonance energy.

Speaker: Tianlu Yuan (University of Wisconsin Madison)

Slides hep_ic.pdf

32 Using IceCube to search for time-dependent neutrino emission from blazars

In September 2017, IceCube observed a high energy neutrino event in spatial coincidence with a known blazar that was undergoing an episode of enhanced gamma-ray emission monitored by Fermi. Additionally, analysis of archival neutrino data found an approximately 6-month-long period of neutrino excess between September 2014 and March 2015, while the gamma-ray flux remained low. Taken together, these two independent results hint that blazars are contributing sources to the high-energy astrophysical neutrino flux measured by IceCube. As a follow-up to this analysis, we search a large sample of blazars for further evidence of neutrino emission without assuming a temporal correlation with gamma-ray emission. A time-dependent search for a statistically significant excess of astrophysical neutrinos is performed at the location of each blazar in the Fermi 3LAC catalog. This allows us to identify the most significant candidate neutrino flares found among the blazar population.

Speaker: Erin O'Sullivan (Stockholm University)

Slides TAUP2019_eosullivan.pdf

Neutrino #2

Convener: Dr Itaru Shimizu (Tohoku University)

33 Neutrino masses beyond the minimal seesaw

Majorana neutrino masses can be generated in a variety of ways. The simplest possibility is to open the d=5 Weinberg operator at tree-level. This leads to the three well-known variants of the seesaw mechanism. However, the smallness of the observed neutrino masses can also be understood, if neutrino masses are generated by higher-dimensional operators and/or at higher loop level. In this talk I will summarize recent work on higher-dimensional and radiative neutrino mass modeling from a general point of view. In particular the complete 3-loop classification scheme, published in JHEP 1810 (2018) 197, will be discussed.

Speaker: Martin Hirsch (IFIC (CSIC, Universidad de Valencia))

Slides MHirsch_TAUP19.pdf

34 Leptogenesis with scalar triplets and right handed neutrinos

Leptogenesis is believed to be contributing to the baryon asymmetry of the Universe through baryogenesis. We consider a simple framework to understand the same with the extension of standard model with $S_3$ and $Z_2$ symmetry. We add two scalar triplets and right-handed neutrinos to explain the neutrino data. Moreover, we consider both type-I and type-II seesaw framework with scalar triplets and right-handed neutrinos to give us the required lepton asymmetry which can account for the observed baryon asymmetry of the universe. In doing so, we consider different mass scales for the scalar triplets and solve the Boltzmann equations to obtain the desire results. We also comment on the LFV and g-2 in the current framework.

Speaker: Anjan Giri (IIT Hyderabad)

Slides Toyama-2019-Giri.pdf

35 Entropy production from decay of GeV scale right-handed neutrinos and the primordial gravitational wave

Right-handed neutrinos are particles beyond the SM introduced in the seesaw mechanism that can explain tiny neutrino masses. We revisit the entropy production from the decay of right-handed neutrinos with the GeV scale masses. This additional production of entropy dilutes the DM and baryon abundances. Furthermore, we estimate the effect on the primordial gravitational wave spectrum. Primordial gravitational waves are closely related to the thermal history of the universe. Therefore, the modified history by right-handed neutrino is imprinted in the gravitational wave spectrum. We then evaluate the influence on the spectrum and the sensitivity in future experiments.

Speaker: Mr Hisashi Okui (Niigata University)

Slides HOkui_TAUP2019.pdf

36 Dark matter stability and Dirac neutrinos using only Standard Model symmetries

Neutrino masses and Dark matter both inarguably point to presence of new physics beyond SM and are topics of active theoretical and experimental research. In this talk we aim to discuss a framework based on anomaly free U(1)B-L symmetry to obtain stable dark matter along with naturally small Dirac neutrino masses generated at the loop level.

Speaker: Dr eduardo peinado (Instituto de Fisica, Universidad Nacional Autonoma de Mexico)

Slides PeinadoTaup2019.pdf

37 Phenomenological Study of Texture Zeros in Lepton Mass Matrices of Minimal Left-Right Symmetric Model

We consider the possibility of texture zeros in lepton mass matrices of minimal left-right symmetric model (LRSM) where light neutrino mass arises from a combination of type I and type II seesaw mechanisms. Based on the allowed texture zeros in light neutrino mass matrix from neutrino and cosmology data, we make a list of all possible allowed and disallowed texture zeros in Dirac and heavy neutrino mass matrices which appear in type I and type II seesaw terms of LRSM. For the numerical analysis we consider those cases with maximum possible texture zeros in light neutrino mass matrix $M_{\nu}$, Dirac neutrino mass matrix $M_D$, heavy neutrino mass matrix $M_{RR}$ while keeping the determinant of $M_{RR}$ non-vanishing, in order to use the standard type I seesaw formula. The possibility of maximum zeros reduces the free parameters of the model making it more predictive. We then compute the new physics contributions to rare decay processes like neutrinoless double beta decay, charged lepton flavour violation. We find that even for a conservative lower limit on left-right symmetry scale corresponding to heavy charged gauge boson mass 4.5 TeV, in agreement with collider bounds, for right handed neutrino masses above 1 GeV, the new physics contributions to these rare decay processes can saturate the corresponding experimental bound.

Speaker: Ms Happy Borgohain (Tezpur University)

Slides TAUP_2019_HAPPYBORGOHAIN.pdf TAUP_2019_HAPPYBORGOHAIN.zip

Neutrino #3

Convener: Dr Itaru Shimizu (Tohoku University)

38 Status of Sterile Neutrino Global Fits

A number of short-baseline neutrino oscillation experiments have observed anomalous results which are consistent with the existence of a high mass-squared splitting $\Delta m^2 ≈ 1~\mathrm{eV}^2$ in the neutrino sector. This would require the existence of at least one additional, sterile, neutrino. At the same time, other experiments have seen null results that strongly constrain the parameters space for the simplest sterile neutrino model. This 3+1 $\nu$ model thus faces incompatibilities between these various experiments. We will discuss some recent results in the field of short-baseline oscillation experiments and how they fit into the overall global picture. We will then introduce other models into the global fits, and discuss how they affect the tensions seen.

Speaker: Mr Alejandro Diaz (Massachusetts Institute of Technology)

Slides Diaz-2019TAUP.pptx

39 How likely is a light sterile neutrino signal even if no sterile neutrinos exist?

A vast experimental program has been mounted in the last decade for the search of a sterile neutrino with the mass at the eV scale. In this talk, we will review and compare the statistical methods used to search for short-baseline neutrino oscillations. Reconstructed confidence regions and sensitivities are found to change significantly among the statistical methods used in the field, preventing a direct comparison of the results and performance of different experiments. The differences can be traced back to the choice of the test statistic. Finally, we discuss the asymptotic properties of the test statistics and how they can lead to a positive signal even though no sterile neutrino exists.

Speaker: Birgit Neumair (Technical University of Munich)

Slides taup2019_neumair_short.pdf

40 Sum rules and asymptotic behaviors of neutrino mixing and oscillations in matter

When a neutrino beam travels in a medium, its electron-flavor component undergoes some forward coherent scattering with the electrons in this medium, leading to some nontrivial modifications of the pattern of neutrino mixing and the behaviors of neutrino oscillations. We have recently studied this kind of Mikheev-Smirnov-Wolfenstein (MSW) matter effect along a new line of thought, and obtained some new and parametrization-independent results. First of all, we derive a set of novel, exact but simple formulas (sum rules) for the moduli of the effective PMNS neutrino mixing matrix in matter and for the sides of its unitarity triangles in the complex plane. The well-known Naumov relationship between the matter-corrected and genuine Jarlskog invariants of CP violation can easily be reproduced from our sum rules. Second, we analytically unravel the asymptotic behaviors of neutrino mixing in very dense matter by using the sum rules, and establish a direct "dual" relationship between the PMNS matrix in vacuum and that in very dense matter because the latter depends only on the fundamental PMNS parameters in the limit that the matter parameter approaches infinity. Our results can elegantly interpret the asymptotic phenomena of the effective neutrino mixing and oscillation paramters evolving with the matter paramter, which have been observed in some previous numerical calculations. As a by-product, we also apply our sum rules to the example of antineutrino oscillations in a very low density matter environment --- the JUNO experiment, and illustrate why the terrestrial matter effect is comparable in magnitude with the experimental sensitivity to the neutrino mass ordering. We affirm the previous observation that such matter effects should be carefully taken into account in the JUNO experiment.

Speaker: Prof. Zhi-zhong XING (Institute of High Energy Physics, Chinese Academy of Sciences)

Slides 2019Toyama.pdf

41 Precision Neff Calculation

We revisit a previous calculation of the well-known Standard Model prediction for the effective number of neutrinos in the early universe, $N_{\rm eff}=3.046$, motivated by recent discrepant results from $1512.02205$, who found $N_{\rm eff}=3.052$. We find errors in the latter calculation, stemming from a slight misunderstanding of the implementation of FTQED corrections to the plasma, and confirm that the procedure of $0111408$ were correct. After clarifying the common pitfalls, we seek to improve upon the calculation by including higher order pressure corrections that had previously been excluded, and find that they have non-negligible effects on $N_{\rm eff}$. We concentrate on the approximation whereby neutrinos decouple instantaneously at some temperature $T_d$. In this scenario, our corrections will decrease the SM prediction of $N_{\rm eff}$ by $0.001$ as compared to excluding them. This decrease is the same size as the effects due to the inclusion of neutrino oscillations. Therefore, we argue that these higher-order corrections should be included in a full calculation of $N_{\rm eff}$ with a full treatment of energy transport. Finally, we estimate anew the electron-neutrino decoupling temperature $T_d$ by using a non-equilibrium QFT approach, finding a $10%$ change in $T_d$ from the standard literature. We use this to argue the importance of including neutrino transport in the full calculation.

Speaker: Mr Jack J. Bennett (UNSW)

Slides JBennett_Towards_the_SM_N_eff.pdf

Underground Labs. #1

42 Deep Science at Boulby Underground Laboratory.

An Update of facilities and science in the UK's deep underground science facility. For more than three decades astro-particle physicists have been operating experiments to search for Dark Matter 1100m below ground in a purpose-built 'low-background' facility at Boulby mine in the North East of England. This facility - the Boulby Underground Laboratory - is one of just a few places in the world suited to hosting these and other science projects requiring a 'quiet environment', free of interference from natural background radiation. The race to find Dark Matter continues and Boulby currently supports the DRIFT/CYGNUS directional dark matter detector programme and operates a growing suite of high sensitivity Germanium detectors for material screening for future Dark Matter detectors (inc. LZ) and other rare-event studies. In the meantime the range of science projects looking for the special properties of deep underground facilities is growing and new projects operating at Boulby range from astro & particle physics to studies of geology/geophysics, climate, the environment, life extreme environments on Earth and beyond. This talk will give an overview of the Boulby Underground Laboratory, the science currently supported and plans for science at Boulby in the future.

Speaker: Prof. Sean Paling (STFC Boulby Underground Lab)

Slides Boulby_TAUP_2019_compressed.pdf

43 Low radioactivity and Multi- disciplinarily Underground Laboratory of Modane (LSM)

The Modane Underground Laboratory (LSM) is located 1700 m (4800 m.w.e) below Fréjus peak (Alpes chain) mountain in the middle of the Fréjus tunnel between France/Italy. The LSM is a multi-disciplinary platform for the experiments requiring low radioactivity environment. Several experiments in Particle and Astroparticle Physics, low-level of High Purity of Germanium gamma ray spectrometry, biology and home land security hosted in the LSM. It’s equipped by Anti-Radon facility where all of the detectors are under Radon depleted Air. I’ll present the LSM structure and briefly reviewed of all experiments are installed in.

Speaker: Dr Ali DASTGHEIBI FARD (CNRS_UGA/LPSC_LSM)

Slides DastgheibiFardTaup2019.pdf

44 Sagnac gyroscopes and GINGERINO

Sagnac Gyroscopes attached to the Earth surface are sensitive to the gravitomagnetic fields, and in principle the confrontation with independent measurements of the Earth rotation rate gives the possibility to measure the Lense Thirring effect without the necessity to map the gravitational field, and independently from the space measurements. It has been also pointed out that this kind of test provides accurate measurement of the angular moment of the planet, this property can be used in the future to investigate the existence of near by rotating Dark Matter. This kind of apparatus id highly multidisciplinary since it provides important data for geophysics and geodesy. Ring laser gyros are at present the most powerful Sagnac gyros, the results of the prototype GINGERINO are discussed.

Speaker: Mrs Angela Di Virgilio (INFN Sezione di Pisa)

Slides TAUP_DiVirgilio_2.pdf

45 Characterization of the Sos Enattos site for the Einstein Telescope

In this talk we report the ongoing characterization of the Sos Enattos former mine (Sardinia, Italy), one of the two canditate sites for the Einstein Telescope (ET), the European third-generation interferometric detector of Gravitational Waves. This observatory will be realized in an underground infrastructure: indeed, since either anthropogenic or natural seismic vibrations are dominated by Rayleigh waves, their amplitude decreases rapidly with depth, improving the detector sensitivity at low frequencies. The Sos Enattos site lies on a crystalline basement free of horizontal crustal movements, made up with micaschist, quartzite, ortogneiss and granitoids rocks. All these rocks show good geo-mechanical parameters. The absence of groundwater (due to the low porosity of these rocks) is confirmed by the mine drainage, evaluated in about 1 L/s along ~50 km of galleries. In addition, the site is located in a very stable area from the geological point of view, showing low seismicity due to the absence of active tectonics. Finally, the area has a low population density, resulting in a reduced anthropic noise. A long-term seismic noise measurement was performed between 2012 and 2015 at a depth of about 110m. More recently, in March 2019, a new network of surface and underground seismometers was deployed at the site and is currently monitoring the seismic noise. Most of the energy carried by the seismic waves is due to the microseisms, showing a strong correlation with the waves of the Tyrrhenian sea. Above 1 Hz the seismic noise in the underground levels of the mine approaches the Peterson's low noise model. Horizontal-to-Vertical spectral ratios indicate the lack of significant site amplification effects related to shallow impedance contrasts. Finally, using data recorded during an underground mine blast, we also evaluate the P-waves propagation velocity, the decay distance of the peak ground velocity, and an estimate of the shallow shear-wave velocity profile from the inversion of the Rayleigh-wave dispersion function.

Speaker: Dr Luca Naticchioni (INFN Roma)

Slides Characterization_of_the_Sos_Enattos_site_for_the_Einstein_Telescope.pdf

DM3: Directional Searches & Annual Modulation

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

46 CYGNUS

A directional signal is expected to provide clear evidence of direct dark matter detection. In addition to the characteristic anisotropy signal, directional detection can potentially extend the search below the so-called neutrino-floor where neutrino-nucleus coherent scatterings make serious background. This method is useful for the low mass WIMPs search with particle identification. After the discovery, the nature of the dark matter and it's motion in the galactic halo can be studied. Among a number of technological approaches proposed so far, gaseous-time-projection chambers have been studied most widely and several experimental efforts are ongoing. Since large mass (typically more than O(100kg) ) detectors are required for dark matter detection, we are proposing an international collaboration named CYGNUS. In the talk, the CYGNUS science case and technological studies are presented.

Speaker: Prof. Kentaro Miuchi (Kobe University)

Slides miuchi_201909_TAUP_wbu.pdf

47 Directional Dark Matter searches and the CYGNO project

We are going to discuss the physics reach and the experimental challenges of directional WIMP-like Dark Matter searches, illustrating the concept of the CYGNUS-TPC international collaboration and how the CYGNO (a CYGNus TPC module with Optical readout) effort fits into it. The most innovative CYGNO's features are the exploitation of sCMOS cameras and PMTs, to optically readout the GEMs amplification of an He:CF4 gas mixture at atmospheric pressure. Compared to other approaches, these choices provide an improved signal/noise ratio (thanks to the 1-2 e-/pixel noise of sCMOS and high GEMs gains) combined with full 3D reconstruction including head-tail, and sensitivity to both Spin Independent and Spin Dependent coupling in the low < 10 GeV WIMP mass region. We will illustrate the R&Ds results obtained with 10 L detector prototype, demonstrating 3D tracking, particle identification capabilities and O(keV) energy threshold over 20 cm drift distance. We will discuss CYGNO's synergies with the ERC Consolidator Grant project INITIUM, together with the experiment timeline and expected sensitivity, also in the context of Solar Neutrinos measurements.

Speaker: Dr Elisabetta Baracchini (Gran Sasso Science Institute)

Slides Baracchini_CYGNO_TAUP_2019.pdf

48 Directional Dark Matter Search with Nuclear Emulsion

A variety of experiments have been developed over the past decades, aiming to detect Weakly Interactive Massive Particles (WIMPs) via their scattering in a detector medium. The sensitivity of these experiments has improved with a tremendous speed due to a constant development of the detectors and analysis methods. Detectors that are able to reconstruct the direction of the nucleus recoiling against the scattering WIMP are opening a new frontier to possibly extend Dark Matter searches beyond the neutrino background. Exploiting directionality would also give a proof of the galactic origin of dark matter making it possible to have a clear and unambiguous signal to background separation. The NEWSdm experiment, based on nuclear emulsions, is proposed to measure the direction of WIMP-induced nuclear recoils. We discuss the potentiality, both in terms of exclusion limits and potential discovery, of a directional experiment based on the use of a solid target made by newly developed nuclear emulsions and read-out systems reaching sub-micrometric resolution. We also report results of the test exposure conducted in Gran Sasso last year.

Speaker: Dr Osamu Sato (Nagoya University)

Slides TAUP2019-NEWSdm-Sato.pptx

49 Results of directional dark matter search from the NEWAGE experiment

NEWAGE is a directional dark matter search experiment using a micro-TPC. We marked the best direction-sensitive limit in 2015. Meanwhile, the substrate of μ-PIC was found to be the dominant background source. We developed a new readout device, namely a low alpha-ray emitting μ-PIC (LAμ-PIC). The U/Th contamination of the LA μ-PIC was found to be 100 times less than that of the conventional μ-PIC. A large LAμ-PIC whose detection area was 30x30 cm$^2$ was installed in the Kamioka Observatory. A dark matter search with a live time of 108 days was conducted. We have analyzed nuclear recoil events in the 50-400keV energy range with the recoil angle distribution. We found no significance signal of the dark matter and derived the most stringent direction-sensitive limit on the spin-dependent WIMP-nucleon interaction cross section for WIMP masses above 20GeV. An improvement of several times would make a search in the DAMA region with a directional method possible. We will report these results in detail.

Speaker: Mr Tomonori Ikeda (Kobe Univ.)

Slides TAUP2019_Ikeda.pdf

50 The COSINUS experiment - A cryogenic direct dark matter search with NaI target

Today, the situation in direct dark matter (DM) detection is controversial: The DAMA/LIBRA experiment observes an annual modulation signal at high confidence which is perfectly compatible with a galactic halo of DM particles which interact in their NaI target crystals. However, in the standard scenario on DM halo and DM interaction properties, the DAMA signal contradicts numerous other null-results. The new experiment COSINUS aims for a model-independent cross-check of the DAMA signal. Such a cross-check is absent up to now and requires the use of the same target material (NaI). While several experimental efforts are planned or already ongoing, COSINUS is the only one operating NaI as cryogenic detector which yields distinctive advantages: Discrimination between electronic interactions and nuclear recoils off Na and I on event-by-event basis, a lower nuclear recoil energy threshold and a better energy resolution. We will review the prototype measurements performed so far, present the plans for the new underground facility foreseen to be installed at LNGS and give an outlook on the COSINUS timescale.

Speaker: Florian Reindl (HEPHY and TU Vienna)

Slides TAUP_COSINUS_Reindl.pdf

51 The SABRE Proof of Principle

SABRE is a dark matter direct detection experiment, based on NaI (Tl) scintillating crystals as target material. A primary goal of the experiment is to test the dark matter interpretation of the DAMA/LIBRA annual modulation signal. To reach its purpose, SABRE features arrays of ultra-low background NaI (Tl) crystals immersed in a liquid scintillator active veto system and twin experiments, one in the Northern hemisphere at Laboratori Nazionali del Gran Sasso, Italy (LNGS) and the other, first of its kind, in the Southern Hemisphere, in the Stawell Underground Physics Laboratory (SUPL). We have successfully developed a NaI (Tl) single crystal with a potassium contamination of the order of 4 ppb, measured by inductively coupled plasma mass spectroscopy (ICP-MS). This is about 3 times lower compared to DAMA/LIBRA crystals. The first phase of the experiment is the SABRE Proof of Principle (PoP): a single detector to be operated inside a liquid scintillator veto at LNGS, with the goal of running in 2019 and performing in situ background measurement of SABRE crystals. In this talk, I will present an overview of the detector design followed by the recent progresses on the development of low radioactivity NaI (Tl) crystals and the status of detector commissioning at LNGS.

Speaker: Mr Simone Copello (GSSI - INFN)

Slides SABRE_TAUP2019_SimoneCopello_(1).pdf

DM4: Backgrounds in Dark Matter Experiments I

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

52 Material Assay and Cleanliness for the LUX-ZEPLIN Experiment

The LZ collaboration has concluded one of the most comprehensive and wide-ranging assay and cleanliness programmes to date for an experiment of its type. This included assays for fixed contaminants through gamma-ray and mass- spectrometry, assays for mobile contaminants through radon emanation and assays for surface contamination through a variety of (radio-metric and optical) techniques. The cleanliness programme has ensured the minimisation of any additional sources of contaminants other than those intrinsic to detector materials in the fabrication and assembly of the detector. This talk will review the overall assay and cleanliness efforts of the LZ collaboration which began back in 2013 and has included measurements of over well over 1000 individual items. We will present assays of raw materials and finalized components that highlights the success of commercial and collaboration manufacturing efforts.

Speaker: Dr Alvine Kamaha (University at Albany, State University of New York)

Slides Material_Assay_and_Cleanliness__for_the_LUX-ZEPLIN_Experiment.pdf

53 Backgrounds and Simulations for the LUX-ZEPLIN Experiment

LUX-ZEPLIN (LZ) will search for dark matter with a dual-phase xenon time projection chamber. Backgrounds that can affect the experiment’s sensitivity must be well understood. Material selection, xenon purification and passive shielding are critical in achieving a radiopure environment. Fiducialization and active vetoing will be employed to help discriminate background events. Simulations are used to assess the impact of all of these factors through the development of a background model, analysis and background mitigation strategies. This talk will discuss the main backgrounds in LZ and their simulation, which ultimately informs the projected sensitivity to WIMP dark matter.

Speaker: Dr Amy Cottle (University of Oxford)

Slides TAUP_Cottle.pdf

54 Background Controls for the DAMIC-M Dark Matter Search

The DAMIC-M detector will use fully-depleted silicon charge-coupled devices (CCDs) to search for low mass dark matter. The detector will combine the excellent understanding of CCD backgrounds from DAMIC at SNOLAB with ongoing developments in the single electron resolution of skipper amplifiers to provide unprecedented sensitivity to light dark matter particles. The DAMIC-M program takes advantage of the unparalleled capability to reject events from radioactivity in the CCDs by exploiting spatial coincidences within a decay chain over timescales as long as months. This, combined with aggressive controls over detector design and material selection, will allow DAMIC-M to probe new models of light dark matter.

Speaker: Daniel Baxter (University of Chicago)

Slides damic_backModel.pdf

55 Measuring cosmogenic activation rates in active detector material

Long-lived radioactive isotopes produced by cosmogenic activation are a major source of background for rare event searches such as dark matter and neutrinoless double beta decay. Understanding the production rates of these cosmogenic isotopes is extremely important for determining the total allowable surface residence time of detector materials during fabrication, storage, and transportation. However, experimentally measuring the production rate is difficult due to low specific activities and because several of the decays of interest produce low energy electrons and x-rays that are not easily detectable. I will discuss a measurement technique that uses a high intensity neutron beam (with a spectrum similar to cosmic ray neutrons) in conjunction with low-background self-counting methods to determine production rates in active detector materials. Based on this technique I will present results from the first experimental measurement of 39Ar and 37Ar cosmogenic production rates in argon, ongoing work on the first measurement of cosmogenic tritium production in silicon, and possible applications to other detector materials.

Speaker: Dr Richard Saldanha (Pacific Northwest National Laboratory)

Slides Saldanha_Cosmogenic_2019_09_09.pdf

56 Calculation of ($\alpha$,n) yields for low background experiments using Geant4

The neutron production induced by ($\alpha$,n) reactions is important in various scenarios. One of the most relevant ones is the direct search of WIMP-like dark matter in underground experiments, like DarkSide-20k, where the neutrons produced by the $\alpha$-decay from radioactive contaminants in the detector materials can produce an irreducible background, limiting the sensitivity of the experiment. A precise estimate of the background due to these neutrons is crucial for the experiments currently taking data and for the design of the next generation of detectors. In this work we present new functionalities that allow to read ($\alpha$,n) data libraries in ENDF-6 format in Geant4 and prove that this tool can be used to calculate such neutron yields and energy spectra. First, we study the best set of parameters to optimize the simulation process while preserving accuracy. Then, we review the different databases available, showing the differences and similarities between them, and we compare several Geant4 neutron production yields and spectra with experimental data and other codes. Finally, we show the improvements associated with this approach for the estimation of the neutron yield in the case of DarkSide-20k. These improvements are associated with the possibility of implementing more complex geometries and intrinsically calculating the effect of surface contamination for the yield in surrounding materials.

Speaker: Dr Vicente Pesudo (CIEMAT)

Slides VPesudo_alpha_n.pdf

57 Understanding neutrino background implications in LXe-TPC dark matter searches using 127Xe electron captures

Dark matter searches using dual-phase xenon time projection chambers (LXe-TPC) rely on the discrimination between electronic recoils (background) and nuclear recoils (signal) based on the ratio of ionization electrons to scintillation photons produced by the interaction in the liquid xenon. This discrimination is calibrated at low energies using tritium $\beta$-decays. However, neutrino and Compton scatters from inner-shell electrons of xenon atoms result in the emission of Auger electrons and x-rays in addition to the primary recoiling electron, and thus have a different event topology than $\beta$-decays and valence-shell electron recoils. Due to their low kinetic energy and large numbers, these secondary particles can deposit large amounts of energy within a small radius, which is uncharacteristic of valence electron recoils and is more akin to nuclear recoils. This effects the profile of the neutrino-electron scattering background in a way that is, so far, uncalibrated and unaccounted for in LXe-TPC dark matter searches, and presents the possibility of a false discovery claim. To investigate the significance of this effect, electrons capture decays of $^{127}$Xe are used to simulate the vacancies produced by inner-shell $e^-$-$\nu$ scatters in the Xenon Electron-recoil L-shell Discrimination Analyzer (XELDA) detector. The $^{127}$Xe source produces a high-purity sample of inner-shell vacancies accompanied by an Auger cascade that can easily be isolated from the prompt $\gamma$'s emitted in the decay. In this talk, I will present the results of a cross-calibration of the XELDA detector using both $^{127}$Xe EC-decays and $^{3}$H $\beta$-decays, and discuss the implications this result has on the rejection capability of neutrino-induced electron recoils in large-scale LXe-TPC dark matter searches, such as LUX-ZEPLIN.

Speaker: Mr Dylan Temples (Northwestern University)

Slides Temples_TAUP2019_final.pdf

Gravitational Wave #2

58 Small scale ring laser gyros as environmental monitors

At present, large area ring laser gyros are the most sensitive inertial sensors to measure angular rotation rate, with sensitivity well below tenths of nrad/s in 1 second and with excellent response at very low frequency. In principle this kind of apparatus would be useful for gravitation wave antennas, as environmental monitors or to improve the test mass suspension isolation. The question is whether it is possible to built small size ring laser with nrad/s sensitivity. So far, the sensitivity has been limited by the so called backscatter problem, which basically locks the two counter propagating modes and makes the device un-usefull. We will show that the backscatter problem can be handled with proper analysis of the data, and the results of the prototype GP2 will be discussed.

Speaker: Mrs Angela Di Virgilio (INFN Sezione di Pisa)

Slides TAUP_DiVirgilio_1.pdf

59 The amorphous mirror coatings research to improve the sensitivity of the future GW detectors

The sensitive volume of the gravitational waves advanced detectors are limited by the thermal noise of the test masses. In particular, the high mechanical losses of the multilayer reflecting coating deposited on the mirror surface is accounted for the main contribution of the thermal noise, limiting the sensitivity in the mid-frequency region of the detection band. Several European laboratories committed on the Virgo Collaboration, have joined their efforts to improve the coating mechanical performances. The research lines of this collaboration are all focused on amorphous coatings, which represent a viable solution for all the future GW detector generations. Research activity involves: 1) the synthesis of samples using different materials and mixtures, deposition techniques and post-deposition treatments; 2) the microscopical and macroscopical characterization of the samples; 3) the modelling of the static and dynamic properties of materials. The main objective is to find a way to reduce of a factor three the mechanical losses of the coating for the next generation of room temperature operating detectors. Some activities are also meant to be relevant for cryogenic operations. The status of this collaborative work will be described as well as the last results of the different research lines.

Speaker: Francesco Piergiovanni (University of Urbino - INFN Firenze)

Slides PARALLEL_SESSION_GW2_Piergiovanni.pdf PARALLEL_SESSION_GW2_Piergiovanni.pptx

60 Study and experiment on the alternative technique of frequency–dependent squeezing generation with EPR entanglement for Virgo.

Current Gravitational-Wave (GW) detectors implement squeezed light injection, as a method for the Quantum Noise (QN) reduction. The sensitivity of present detectors is affected mostly by the high–frequency component of QN as the dominant in the low–frequency region Radiation Pressure Noise (RPN) is covered by technical noises. This situation fosters Frequency-Independent Squeezing (FIS) technique to be used. On-going work on Virgo detector upgrade will soon lower the technical noises till the level when RPN also becomes limiting. One can obtain a Frequency-Dependent Squeezing (FDS) by applying an external Filter Cavity (FC), which performs squeezing angle rotation, to FIS technique. Another method has been recently proposed to achieve a broadband reduction of quantum noise in GW detectors using a pair of squeezed Einstein Podolsky Rosen-entangled (EPR) beams to produce FDS. This method promises to achieve a frequency-dependent optimization of the injected squeezed light fields without the need for an external filter cavity. Although suitable filter cavities can be designed, the additional cavity adds further complexity to the interferometer. FDS with EPR-entanglement offers an attractive solution to this by harnessing the quantum correlations generated between a pair of EPR-entangled beams and effectively exploiting the interferometer itself as a filter cavity, thereby achieving a similar response with minimal additional optical components. In the implementation, a pair of squeezed EPR-entangled optical fields can be generated by means of a Non-degenerate Optical Parametric Oscillator (NOPO). By properly choosing the detuning of the pumping field from the OPO resonance, one can generate two entangled photons, named signal and idler. The two entangled vacuum fields are injected into the interferometer; signal field is kept resonant with arm cavities, while idler field is far detuned and experiences a frequency-dependent quadrature rotation, which can be optimized by adjusting with respect to the lengths of interferometer cavities. In reflection from the interferometer, the two fields are separated and measured by two independent homodyne detectors. Output signals are combined using an optimal filter to retrieve the squeezing of the quantum noise on the signal channel. In this talk, I will summarize the present work on the EPR proof-of-principle experiment for Virgo and Virgo subsystem proposal for frequency-dependent squeezing, obtained with a compact apparatus and without the costs required by the infrastructure for the filter cavity. Bibliography: Ma Y, Miao H, Pang BH, Evans M, Zhao C, Harms J, et al. Proposal for gravitational-wave detection beyond the standard quantum limit through EPR entanglement. Nature Physics. Springer Science and Business Media LLC; 2017 May 15;13(8):776–80. Available from: http://dx.doi.org/10.1038/nphys4118 1 INFN Sezione di Perugia, I-06123 Perugia, Italy 2 Laboratoire AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris Cedex 13, France 3 Università di Padova, Dipartimento di Fisica e Astronomia, I-35131 Padova, and INFN Sezione di Padova, Italy 4 Università di Napoli “Federico II”, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, and INFN Sezione di Napoli, Italy 5 Università degli Studi di Genova, Dipartimento di Fisica, I-16146 Genova, Italy 6 INFN Sezione di Genova, I-16146 Genova, Italy 7 Università di Roma “La Sapienza”, I-00185 Roma,Italy 8 Università di Roma Tor Vergata, I-00133 Roma, Italy 9 INFN Sezione di Roma “Tor Vergata”, Italy 10 INFN Sezione di Pisa, I-16146 Pisa, Italy 11 Gran Sasso Science Institute, I-67100 L’Aquila, Italy 12 INFN Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy 13 INFN Sezione di Roma “ La Sapienza”, Italy 14 Università di Trento, Dipartimento di Fisica, I-38123 Povo, Trento, and INFN Sezione di Trento, Italy

Speaker: Dr Mateusz Bawaj (INFN, Sezione di Perugia, I-06123 Perugia, Italy)

Slides Bawaj_TAUP2019.pdf

HECR #2

Convener: Prof. Yoshiki Tsunesada (Osaka City University)

61 Turbulence Particle Acceleration and UHECR

The standard model to produce non-thermal particles is the particle acceleration at shocks. However, the photon spectra in high-energy objects, such as blazars, frequently show very hard feature, which seems inconsistent with the standard shock acceleration theory. The alternative model is the particle acceleration by turbulence. Here, we propose the particle acceleration by large scale compressible MHD waves, where the transit time damping (TTD) is a key mechanism. We find that the acceleration efficiency is higher than previously considered. This model leads to a hard-sphere-like acceleration, in which the acceleration timescale is independent of the particle energy. The electron energy distribution based on this model is consistent with blazar photon spectra. If adopt this model to the deceleration phase of gamma-ray burst jets, ultra high-energy cosmic-rays can be produced. The resultant spectrum is harder than other models, so that the secondary neutrino production in their propagation is relatively suppressed.

Speaker: Dr Katsuaki Asano (Institute for Cosmic Ray Research, The University of Tokyo)

Slides TAUP19.pptx

62 Diffusive shock acceleration of cosmic rays in low mach galaxy cluster shocks.

Astrophysical shocks are known to accelerate particles to high relativistic velocities. This process requires the particles to repeatedly cross the shock, a process that can only occur if the particle is reflected by the local magnetic field. Such particles are observed on Earth as cosmic rays. This phenomenon has been studied in considerable detail for high-Mach shocks, such as the shocks that occur in colliding stellar winds and supernova explosions, but remains relatively unexplored for low-Mach shocks, such as the shocks of colliding clusters of galaxies. Recent simulations using the particle-in-cell (PIC) method have shown that, depending on the exact Mach number, even low-Mach shocks can accelerate charged particles to the point where they start to deviate from the thermal velocity distribution. However, the computationally intensive nature of the PIC calculations makes it difficult to continue the simulations to determine whether the particles can reach relativistic speeds. We now present new simulations, using a combined PIC and magnetohydrodynamics (MHD) technique. This model, which takes advantage of the computational efficiency of MHD, allows us to simulate a much larger physical volume and study the behaviour of the particles over a longer period of time in order to determine to what extent the acceleration process continues and whether these shocks are capable of contributing to the cosmic ray spectrum

Speaker: Prof. Allard Jan van Marle (Ulsan National Institute of Science and Technology)

Slides Taup2019_vanMarle.pptx

63 Chiral transport and turbulence in core-collapse supernovae

The conventional transport theory for core-collapse supernovae misses one key property of elementary particles, the chirality. We show that the chiral transport phenomena due to the chirality of elementary particles that have been neglected so far can reverse the turbulent cascade direction from direct to inverse cascade, which would impact the hydrodynamic evolution of the supernova core toward explosion.

Speaker: Prof. Naoki Yamamoto (Keio University)

Slides Yamamoto_TAUP.pdf

64 A new source type of Galactic Cosmic Rays

Presently the explosions of supernovae are considered as sources of Galactic cosmic rays up to energies of $\sim 10^{17}$ eV. But, the experimental data obtained with Pamela, Fermi, AMS-02, spectrometers require the existence of nearby sources of cosmic rays at the distances less than one kpc. These sources could explain the growth of the ratio of galactic positrons to electrons with an increase of their energy, the complex dependence of the exponent of the proton and alpha spectra from the energy of these particles, the appearance of anomaly component in cosmic rays. We consider active dwarf stars as possible sources of galactic cosmic rays in the energy range up to $\sim 10^{14}$ eV. These stars produce powerful stellar flares sometimes with energy release more than $10^{36}$ erg. The generation of high-energy cosmic rays should be accompanied by high-energy gamma-ray emission, which may be detected. Here we present the SHALON long-term observation data aimed to search for gamma-ray emission above 800 GeV from the active red dwarf stars: V962 Tau, V780 Tau, V388 Cas, V1589 Cyg and GL 851.1. The TeV gamma-ray emission mostly of flaring type from these sources was detected. This result confirms that active dwarf stars are also the sources of high-energy galactic cosmic rays.

Speaker: Dr Vera Y. Sinitsyna (P.N. Lebedev Physical Institute, RAS)

Slides RedDwarfs_Sinitsyna2019.pdf

65 Equation of state for quark matter with strong magnetic field and hybrid stars

Neutron stars have many interesting physical features, such as the high-density, strong magnetic field, cooling, rapidly rotation, and glitches. Among them, the strong magnetic field has been a focus of constant attention. In particular, the behavior of high density matter in strong magnetic fields is an important issue in studies about EOS and it has been discussed in many literatures for hadron matter or quark matter. We also consider the effect of magnetic field on the EOS especially for quark matter. Due to the existence of strong magnetic field, one may have to take into account the Landau levels for quark matter. Quark matter in the lowest Landau level makes the equation of state much stiff and the mass of the hybrid star easily over the $2M_\odot$. Including of higher Landau levels may make equation of state softer. In this study we take into account the second Landau level to see this tendency. As a result, we find that the equation of state is still stiff enough for sustaining the heavy star like $2M_\odot$.

Speaker: Tomoki Endo (Osaka Sangyo University)

Slides TAUP2019_endo.ppt

Neutrino #4

Convener: Dr Itaru Shimizu (Tohoku University)

66 Tackling the astrophysical neutrino flux between 5TeV and 100TeV with veto-based methods in IceCube

The groundbreaking discovery of astrophysical neutrinos by IceCube was made above 100TeV where the population becomes easier to distinguish from the atmospheric neutrino background. At high energies above 1PeV more data is needed, and the nature and origin of this astrophysical flux remains largely unknown. Presently we have the capability to obtain a high-purity sample of astrophysical neutrinos between 5TeV and 100TeV with improved veto-based methods. However, correctly predicting background contributions in these samples requires expensive simulation and is limited by systematics. In this talk we summarize current knowledge of the astrophysical neutrino flux, present two methods of obtaining a high purity sample of astrophysical neutrinos between 5TeV and 100TeV, outline modeling challenges and solutions, and discuss plans for the next year with the goal of providing a definitive measurement of the astrophysical flux below 100TeV.

Speaker: Mr Austin Schneider (University of Wisconsin Madison)

Slides TAUP2019_Schneider.pdf

67 Angular power spectrum analysis on current and future high-energy neutrino data

To constrain the contribution of source populations to the observed neutrino sky, we consider isotropic and anisotropic components of the diffuse neutrino data. We simulate through-going muon neutrino events by applying statistical distributions for the fluxes of extra-galactic sources and investigate the sensitivities of current (IceCube) and future (IceCube-Gen2 and KM3NeT) experiments. I will show that the angular power spectrum is a powerful probe to assess the angular characteristics of neutrino data and demonstrate that we are already constraining rare and bright sources with current IceCube data. In addition, I will investigate the decay and annihilation of very heavy dark matter as a potential neutrino source, as suggested by the observed excess in the High-Energy Starting Event dataset. We apply our angular power spectrum analysis to this HESE data for different channels, allowing us to interpret the observed neutrino sky and perform a sensitivity forecast.

Speaker: Ms Ariane Dekker (GRAPPA, University of Amsterdam)

Slides Presentation_Final.pdf

68 Physics Potential of the IceCube Upgrade

The IceCube Neutrino Observatory is a cubic-kilometer Cherenkov detector at the South Pole. The planned Upgrade project, which consists of seven new strings, will be deployed with densely spaced optical modules to improve the neutrino detection capability at a few GeV level. The goal of IceCube Upgrade is to make competitive measurements on neutrino oscillations parameters, and serve as a R&D platform for the future IceCube-Gen2 experiment. The new generation of optical modules will provide improved detection efficiency and directional resolution for Cherenkov photons. Several new calibration devices will provide a better understanding of the detector, and thereby reduce the detector systematic uncertainties. In this talk, the IceCube Upgrade project as well as the new instrumentations will be outlined, and the physics program of the detector will be discussed.

Speaker: Wing Yan Ma (DESY)

Slides TAUPtalk_190908_v2.pdf

69 KM3NeT/ORCA: status and prospects

The KM3NeT collaboration is currently building the next generation of large-volume water-Cherenkov neutrino telescopes in the Mediterranean Sea abysses. ORCA, the denser of the two detectors under construction, will instrument about 6 Mton of sea water. It is optimised for the detection of atmospheric neutrinos with energies above ∼1 GeV. The main research target of the ORCA detector is the measurement of the neutrino mass ordering and atmospheric neutrino oscillation parameters, while the detector is also sensitive to a wide variety of other physics topics, such as dark matter, non-standard interactions and sterile neutrinos. The presentation will provide an overview of the ORCA detector and introduce its research programme. The projected sensitivity of the detector to the neutrino mass ordering will be shown, alongside prospects for early analyses of data collected with a small sub-array of the detector during construction phase.

Speaker: Dr Ronald Bruijn (University of Amsterdam/Nikhef)

Slides Talk_TAUP2019_ORCA_Bruijn.pdf

70 Neutrino CP Violation with the European Spallation Source neutrino Super Beam project

After measuring in 2012 a relatively large value of the neutrino mixing angle θ13, the door is now open to observe for the first time a possible CP violation in the leptonic sector. The measured value of θ13 also privileges the 2nd oscillation maximum for the discovery of CP violation instead of the usually used 1st oscillation maximum. The sensitivity at this 2nd oscillation maximum is about three times higher than for the 1st oscillation maximum inducing a lower influence of systematic errors. Going to the 2nd oscillation maximum necessitates a very intense neutrino beam with the appropriate energy. The world’s most intense pulsed spallation neutron source, the European Spallation Source, will have a proton linac with 5 MW power and 2 GeV energy. This linac, under construction, also has the potential to become the proton driver of the world’s most intense neutrino beam with very high potential to discover a neutrino CP violation. The physics performance of that neutrino Super Beam in conjunction with a megaton underground Water Cherenkov neutrino detector installed at a distance of about 500 km from ESS has been evaluated. In addition, the choice of such detector will extent the physics program to proton–decay, atmospheric neutrinos and astrophysics searches. The ESS proton linac upgrades, the accumulator ring needed for proton pulse compression, the target station optimization and the physics potential are described. In addition to neutrinos, this facility will also produce at the same time a copious number of muons which could be used by a muon collider. The ESS neutron facility will be fully ready by 2023 at which moment the upgrades for the neutrino facility could start. This project is supported by the COST Action CA15139 "Combining forces for a novel European facility for neutrino-antineutrino symmetry-violation discovery" and the European Union’s Horizon 2020 research and innovation program under grant agreement No 777419.

Speaker: Dr Eirik Gramstad (Researcher)

Slides taup19_gramstad.pdf

71 Search for nucleon decay with Super-Kamiokande

The Super-Kamiokande (SK) detector, a large water Cherenkov detector, is well-suited to proton decay searches, with $7.5 \times 10^{33}$ protons in the 22.5 kiloton fiducial volume. SK has been carried out searches for proton (nucleon) decay via many decay modes, like $p \rightarrow e^{+}\pi^{0}$, $p \rightarrow \mu^{+}\pi^{0}$, $p \rightarrow \bar{\nu}K^{+}$, and many other decay modes. This talk will overviews the recent experimental results and prospects of proton decay searches with Super-Kamiokande.

Speaker: Dr Hide-Kazu TANAKA (ICRR, University Of Tokyo)

Slides tanaka_20190909_taup_sk_ndk_v1.pdf

Neutrino #5

Convener: Dr Itaru Shimizu (Tohoku University)

72 Observation of two-neutrino double electron capture in Xe-124 with XENON1T

Two-neutrino double electron capture ($2\nu$ECEC) is a second-order Weak process with predicted half-lives that surpass the age of the Universe by many orders of magnitude. Indications for $2\nu$ECEC decays have only been seen for two isotopes, $^{78}$Kr and $^{130}$Ba, and instruments with very low background levels are needed to detect them directly with high statistical significance. The $2\nu$ECEC half-life provides an important input for nuclear structure models and its measurement represents a first step in the search for the neutrinoless double electron capture processes ($0\nu$ECEC). A detection of the latter would imply the existence of lepton number violation and the Majorana nature of neutrinos. The XENON1T dark matter experiment located at Laboratori Nazionali del Gran Sasso recently achieved the first direct observation of the Standard Model $2\nu$ECEC in $^{124}$Xe. The significance of the signal is $4.4\sigma$ and the corresponding half-life $T_{1/2}^{2\nu\rm{ECEC}} = (1.8\pm 0.5_{\rm{stat}}\pm 0.1_{\rm{sys}})\times 10^{22}\;\rm{yr}$ is the longest ever measured directly [[XENON Collaboration. Nature 568, 532-535 (2019)]][1]. This demonstrates that the low background and large target mass of xenon-based Dark Matter detectors make them well suited to measuring other rare processes and it highlights the broad physics reach for the next-generation of experiments currently under construction. This talk will give a general introduction to XENON1T. It will then shift to double electron capture processes, their signatures, and their connection to nuclear theory as well as neutrino physics. It will present all analysis steps with a focus on energy calibration and background modelling, and discuss prospects for future $0\nu$ECEC searches. The work of the author is supported by Deutsche Forschungsgemeinschaft (DFG) through the Research Training Group *GRK 2149: Strong and Weak Interactions - from Hadrons to Dark Matter*. [1]: https://www.nature.com/articles/s41586-019-1124-4

Speaker: Mr Christian Wittweg (WWU Münster)

Slides dec_taup2019_wittweg.pdf

73 Results of the \textsc{Majorana Demonstrator}'s Search for Double-Beta Decay to Excited States

The \textsc{Majorana Demonstrator} is studying double-beta decay in $^{76}$Ge using a modular array of high purity Germanium detectors. The experiment is constructed using low-background materials and is currently operating at the '4850 level of the Sanford Underground Research Facility. The experiment consists of two modules with 29~detectors each, consisting of 44.8~kg of germanium detectors, 29.7~kg of which are enriched to 88\% in $^{76}$Ge. The \textsc{Demonstrator} is searching for double-beta decay of $^{76}$Ge to three different excited states (E.S.s) of $^{76}$Se. The E.S. decays have a clear event signature consisting of a $\beta\beta$-decay with the prompt emission of one or two $\gamma$-rays, resulting in with high probability in a multi-site event. The granularity of the \textsc{Demonstrator} detector array enables powerful discrimination of this event signature from backgrounds. This talk will present the results of \textsc{Majorana Demonstrator}'s search for $\beta\beta$-decay to excited states. This material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics, the Particle Astrophysics and Nuclear Physics Programs of the National Science Foundation, and the Sanford Underground Research Facility.

Speaker: Ian Guinn (University of North Carolina at Chapel Hill)

Slides 20190909_Guinn_BBES.pptx

74 Search for triple and quadruple beta decay of 150Nd

Triple beta decay of 150Nd to the ground and excited states of 150Eu and quadruple beta decay of 150Nd to the excited states of 150Gd have been studied using a 400 cm3 low-background HPGe detector and an external source consisting of 3046 g of natural Nd2O3 powder. A half-life limit for the quadruple beta decay to the 01+ state of 150Gd was found to be T1/2 (0ν+4ν) > 8.7x10^20 yr (90% C.L.). This is ~ 5 times more strong limit than previous result [Phys. Rev. C 98 (2018) 055501]. For other (0ν+4ν) transitions to the 2_1^+, 3_1^-, 4_1^+, 2_2^+ and 2_3^+ excited states limits for the first time have been obtained at the level of ∼ 6.1-9.5x10^20 yr (90% C.L.). We report here also the results for the first search for triple beta decay to the ground and excited final states of 150Eu. We find no evidence of this decay and set lower limits on the half-life in the range T1/2 (0ν+3ν) > (0.04-4.8)x10^20 yr (90% C.L.). Possible future experiments with more higher sensitivity are discussed.

Speaker: Dr Alexander Barabash (NIC «Kurchatov Institute» - ITEP, B. Cheremushkinskaya 25, 117218 Moscow, Russia)

Slides Barabash_TAUP2019.pdf

75 Search for double capture 2νEC/EC of Cd-106 on a TGV-2 spectrometer

The search for double capture 2νEC/EC in Cd-106 is performed on the TGV-2 spectrometer, located in the underground laboratory (LSM, Modane, France, 4800 m.w.e.). The TGV-2 spectrometer consists of 32 planar detectors with a total active surface of about 400 cm3. The detectors are arranged in pairs, and 16 Cd-106 foils (with an enrichment of 99.57% of Cd-106 and a total mass of ~ 23.2 g) are placed between the pairs of face-to-face detectors. Recent interest to the study of double capture 2νEC/EC has been increased due the announcement of discovery of this extremely rare process by the XENON1T collaboration (https://doi.org/10.1038/s41586-019-1124-4). This result requires further confirmation in other experiments, on other isotopes and using other methods. The TGV-2 spectrometer provides such a unique alternative method taking data since February 2014. The results of analysis of data taken during 29,000 h will be presented with sensitivity level up to T1/2(2νEC/EC, g.s.) ~ 1 × 10^22 y at 90% C.L. compatible with the results given by the XENON1T.

Speaker: Dr Ekaterina Rukhadze (IEAP CTU in Prague)

Slides taup2019_ERukhadze1.pdf

Neutrino #6

Convener: Dr Itaru Shimizu (Tohoku University)

76 First measurement of the neutron-argon cross section between 100 and 800 MeV

Neutral particle production in (anti-)neutrino interactions biases neutrino energy reconstruction, and of the neutral particles, neutron interactions in liquid argon are the least constrained by data. The mini-CAPTAIN LArTPC measured neutron interactions on argon from a neutron beam at Los Alamos National Laboratory in order to address this issue specifically. Using data from a low intensity beam intensity run, first measurement of neutron cross section at the 100-800 MeV range was made, and the energy averaged neutron cross-section was determined to be 0.91±0.10 (stat.)±0.09 (sys.) barns. This will be useful for the future of DUNE, as DUNE will determine the neutrino mass ordering and explore leptonic CP violation by measuring the electron (anti-)neutrino appearance from the mostly muon (anti-)neutrino beam produced at Fermilab. I describe the measurement and discuss future plans.

Speaker: Mr Scott Locke (University of California, Irvine)

Slides locke_taup_minicaptain.pdf locke_taup_minicaptain.pptx

77 Recent neutrino-Argon scattering results from MicroBooNE

MicroBooNE is an 85-ton active mass liquid argon time projection chamber located on the Booster Neutrino Beam at Fermi National Accelerator Laboratory. The primary goal of MicroBooNE is to investigate the excess of low-energy electromagnetic events observed by the MiniBooNE experiment, and determine whether they are photon-like or electron-like. Situated on a muon neutrino beamline with a mean neutrino energy of 800 MeV, the MicroBooNE detector also provides the opportunity to study neutrino-Argon scattering cross-sections in order to probe neutrino-nucleus interactions. In this talk, I will present the most recent cross-section physics results from the MicroBooNE collaboration. Particular focus will be placed on the selection and reconstruction of electromagnetic final states, as these measurements are crucial in resolving the electron or photon-like nature of the MiniBooNE result.

Speaker: Ms Supraja Balasubramanian (Yale University)

Slides taup2019_balasubramanian_sept09.pdf

78 Characterizing Beam-Correlated Neutron Backgrounds in the ANNIE detector

The Accelerator Neutrino Neutron Interaction Experiment (ANNIE) will provide new insights on neutrino-nucleus interaction physics by measuring the neutron yield as a function of neutrino energy for muon-neutrino interactions with nuclei. Such insights will lead to better control of systematic uncertainties in long-baseline neutrino oscillation experiments, as well as potentially improving signal-background discrimination in future neutrino detectors. The ANNIE detector currently under construction uses roughly 30 tons of pure water, doped with gadolinium to enhance the neutron-capture cross-section and instrumented with a combination of conventional photomultipliers and novel Large Area Picosecond Photodetectors (LAPPDs). In 2017, before the addition of either the LAPPDs or the gadolinium, a movable neutron capture volume containing gadolinium-doped liquid scintillator was used to characterize the beam-correlated neutron background as a function of position within the ANNIE tank. We report here on this background measurement and the implications for the ANNIE physics program.

Speaker: Prof. Amanda Weinstein (Iowa State University)

Slides TAUP_ANNIEPhaseI_2019.pdf

79 Study of Charged-Current neutrino interactions on water with nuclear emulsion in the NINJA experiment

Neutrino-nucleus interaction is one of the major sources of the uncertainty for neutrino oscillation experiments. The NINJA experiment aims to measure neutrino-water interactions containing low momentum secondary particles using a nuclear emulsion detector. Since nuclear emulsion has sub-micron position resolution, it allows us to observe the interaction vertices clearly, and is one of the most effective ways to measure low momentum secondary particles. Short proton tracks down to 200MeV/c momentum are expected to be measured which are hardly reconstructed in plastic scintillator based detectors. A series of test experiments has been carried out with prototype detectors at J-PARC. The latest run has $0.7\times10^{21}$ POT of anti-neutrino exposure on 4 kg water-target. More than 100 events of Charged-Current interactions on water are expected to be observed. Comparison between data and Monte Carlo simulation including track multiplicity and momentum distribution of secondary particles will be shown.

Speaker: Ms Ayami Hiramoto (Kyoto University)

Slides TAUP2019_hiramoto_v3.pdf

80 Study of neutrino charged current interactions on iron in the NINJA experiment

Understanding of neutrino-nucleus interactions for energies around 1 GeV is of great importance to us because one of the major systematic uncertainties in current neutrino oscillation experiments comes from nuclear effects in those interactions. The NINJA collaboration aims to study neutrino-nucleus interactions in the energy range of hundreds of MeV to a few GeV by using emulsion-based detector. Nuclear emulsion is well suited for precise measurement of positions and angles of interacting particles since it has sub-micron spatial resolution. It is capable of detecting slow protons as low as 200 MeV/c, which is its advantage over other detectors. Data presented in this talk were taken from the exposure of a 60kg iron target in 2016 to the neutrino and the anti neutrino beam corresponding to integrated POT $0.40\times10^{20}$ and $ 3.53\times10^{20}$, respectively. Based on a few hundred events of neutrino-iron charged current interactions in the target, the number of protons and charged pions in the final state of each event, their emission angles and momenta were measured and compared with Monte Carlo simulation.

Speaker: Mr Hitoshi Oshima (Toho University)

Slides TAUP_oshima_v3.pdf

Underground Labs. #2

81 Baksan large volume scintillation telescope: a current status

A current status of the project of a large volume scintillation telescope at the Baksan neutrino observatory is presented. The main research activities of the BLVST are low-energy neutrino physics, astrophysics and geophysics. To detect geoneutrinos, large-scale new-generation scintillator detectors located at large depths in the regions with a low background level from nuclear reactors are required. The Baksan Neutrino Observatory is geographically located in one of these places. Recently resumed R&D activities are aimed at the creation of new-generation telescope with a target mass of 10 kt at a depth of 4800 m.w.e. A small scale prototype is already under construction.

Speaker: Prof. Valeriy Petkov (Institute for Nuclear Research of the Russian Academy of Sciences)

Slides Petkov_DetGeoNu_TAUP-19.pdf Petkov_DetGeoNu_TAUP-19.ppt

82 Radioassay and Purification for Experiments at Y2L and Yemilab in Korea

Two major rare-decay search experiments, COSINE-100 for WIMP dark matter and AMoRE for neutrinoless double beta decay, have been running at the Yangyang underground laboratory (Y2L) in Korea for about four years. In order to measure radio-activities of materials in both experiments, a number of ultra-low radioactivity measurement detectors have been developed and are now operational. For radioassays of raw materials and detector components, an ICP-MS, an argon gas ionization counter, and a number of HPGe detectors are being used. Three silicon PIN diode-based radon chamber detectors have been either upgraded or constructed for accurate measurements of radon in the airs from a radon reduction system or experimental rooms. A fourteen HPGe detectors array was installed in 2016 for more sensitive measurement with bigger samples than those could be tested in two single crystal HPGe detectors. As the Y2L space is too small to accommodate the next phases of both of these experiments, a new underground laboratory, called Yemilab, is being constructed in Jeongseon, Korea with a factor of ten more space (~2,800 m2) and ~1,100 m overburden compared to ~200 m2 and ~700 m at Y2L. The future experiments require detector materials with even lower background levels than those in the current ones. Various types of scintillating crystals such as CaMoO4, Li2MoO4, and NaI(Tl) are being grown with purification methods specifically developed for the raw materials. A summary on radioassay and purification results for experiments at Y2L and Yemilab in Korea will be presented.

Speaker: Dr Moo Hyun Lee (IBS)

Slides Underground_Labs#2_MHLEE.pdf

83 Rare physics searches at the China Jinping Underground Laboratory

China Jinping underground laboratory (CJPL) has been an ideal site for rare-event experiments such as dark matter, neutrinoless double beta decay, solar neutrino experiment and so on, based on its deepest rock overburden of about 2400m and large internal space. This presentation will give an overview of conditions, status and future plan of the laboratory. Main experiments and scientific activities carried out at CJPL will be presented including dark matter and neutrinoless doubel beta decay experiments such as CDEX and PandaX, and other experiments including Jinping underground nuclear astrophysics program (JUNA), Jinping neutrino experiment and so on.

Speaker: Prof. Qian Yue (Tsinghua University)

Slides 20190909-YueQ-Rare_physics_searches_at_CJPL.pdf (Protected)

84 Low Background & Large Scale Electronic Circuit Substrate for CDEX-2 Experiment

The primary design for CDEX-2 Experiment will put 100kg HPGe into a big tank of liquid nitrogen with 13m diameter and 13m height. One of the most important problems is how to obtain low background & large scale Flexible Copper Clad Laminate (FCCL) for electronic circuit substrate. Regarding the copper clad, high purity oxygen-free copper will be used, and for the flexible laminate, PTFE and PEN are good choices for tests. Better than compression technology with rolled copper foil which can only provide limited dimension for substrate(e.g. 9”×9” panel), our solution is using ion beam implantation & deposition technology with roll to roll style (Metal Vapor Vacuum Arc, Filtered Cathodic Vacuum Arc) which can increase the adhesion strength for FCCL obviously with no length restriction(510 mm wide, any length). The results for adhesion strength test show that hydrophilic angle was decreased from 75 degree to 40 degree, and other systematically tests demonstrate that all of the performances for FCCL, such as voltage resistance, stability under high humidity and etc. meet the national standards. ( e.g. IPC-6013B, IPC-TM-650 2.6.25, JIS C 6471,JIS C 6471-1995, etc.)

Speaker: Prof. YUANYUAN LIU (Key Laboratory of Beam Technology of Ministry of Education, College of Nuclear Science and Technology, Beijing Normal University, Beijing 100875, China Beijing Radiation Center, Beijing 100875, China)

Slides 20190909_TAUP_F.pptx

85 Measurement of ambient neutrons in an underground laboratory at Kamioka Observatory

Ambient neutron is one of the most serious backgrounds for underground experiments searching for rare events (e.g., neutrinoless double beta decay and dark matter). Ambient neutron flux in an underground laboratory of Kamioka Observatory was measured using a He-3 proportional counter with various moderator setup. Since the detector response largely depends on the spectrum shape, energy spectra of neutrons transported from the rock to the laboratory are estimated by Monte-Carlo simulations. The ratio of thermal neutron flux to the total one was found to depend on the thermalizing efficiency in the rock. Therefore, the ratio of the count rate without a moderator to that with a moderator was used to determine this parameter. As a result, the most-likely neutron spectrum predicted by the simulations with the parameters determined by the experimental results was obtained (published, PTEP 2018 123C01). The result suggests an interesting spectrum shape in high energy region (-MeV), which has not been indicated in previous studies. To clarify this spectrum structure, low background liquid scintillator is prepared. This detector is sensitive to the interest energy region. The new results will be reported.

Speaker: Mr Keita Mizukoshi (Kobe University)

Slides taup_mzks_2019.pdf

86 Radon monitoring in the Kamioka Observatory

Radioactivity from radon is one of the main backgrounds for low energy experiments, like the Super-Kamiokande and the other experiments hosted in the Kamioka Observatory. In addition, it is an issue for the safety of the researchers and technicians working in underground laboratories. In the Kamioka Observatory, a total of 28 1-L radon detectors are deployed in different areas in order to monitor the radon concentration and ensure it stay below a certain limit. In this presentation, we will describe the 1-L radon detector system and their RaspberryPi-based data acquisition system. The evolution of the radon's air concentration over the last 3 years in the tunnels and the experimental area of the Kamioka Observatory will be showned and described. Preliminary measurements of the Hyper-Kamiokande candidate site's radon concentration in the Tochibora Mine will be also presented.

Speaker: Dr Guillaume Pronost (Kamioka Observatory, ICRR, The University of Tokyo)

Slides 2019Sep_TAUP_Rn.pdf

87 Effects of radioactivity on superconducting quantum bits

Superconducting quantum circuits are emerging as one of the leading candidates for the implementation of coherent quantum processors. Despite the booming development in the last decade, one of the main challenges in the up-scaling of superconducting quantum bit (qubit) technology remains their limited quantum coherence. Our goal is to tackle the decoherence induced by quasiparticles. In Aluminium circuits, which currently represent the quasi-totality of superconducting quantum electronics, at the typical operation temperature (20-50 mK), thermal energy is far inferior to the superconducting gap, and we should not measure even a single broken Cooper pair. Nevertheless, there is an abundance of evidence to show that something breaks Cooper pairs and creates non-thermal quasiparticles. Suppressing the detrimental effects of quasiparticles will allow to open new development avenues for superconducting qubits and will largely benefit also the performance of Kinetic Inductance Detectors in Particle Physics and Astrophysics. Our first goal is attacking a source of quasiparticles that has been too long neglected, namely radioactivity: cosmic rays, environmental radioactivity, and contaminants in the materials can all generate phonons of energy sufficient to break Cooper pairs and thus increase the number of quasiparticles. To prove that radioactivity affects the qubits performance, we measured the same chip in an above ground facility, and then in a shielded cryostat located deep underground in the Laboratori Nazionali del Gran Sasso (Italy). We will discuss the results of these measurements and the future steps of our project.

Speaker: Dr Laura Cardani (Istituto Nazionale di Fisica Nucleare)

Slides 2019_TAUP.pdf

88 The SNOLAB Underground Laboratory

SNOLAB is a laboratory 2-km underground with a program focused on rare-event searches enabled by the suppression of cosmic radiation. As these rare-event searches probe unprecedented low background regimes, SNOLAB is developing infrastructure to support and enable these experimental programs. I will describe some of the current capabilities and the developments that will help plan, construct, and analyze future experiments.

Speaker: Jeter Hall (SNOLAB)

Slides JHall_TAUP_9SEPT2019_SNOLAB_0610.pdf

89 Laboratorio Subterráneo de Canfranc

With 9 years of activities in the current phase of the 1600 m2 LSC underground installations, several experiments and services are producing significant results. ANAIS has accumulated two years of data taking to verify DAMA results, while ArDM finished taking data, to be integrated in the Global Argon DM Collaboration this year. Our flagship experiment NEXT has demonstrated Xenon world record energy resolution at double beta endpoint and show the double electron tracks that further reduce The background one order of magnitude. CROSS demonstrator has started this year to take data on Li2MoO4 scintillating bolometers with Al-film assisted pulse shape discrimination of surface events. Several services are operating underground, with dedicated control and characterization of low levels of Radon, material screening of components in experiments at the LSC and outside (SK-Gd). I will discuss the status of the LSC activities and new coming services and experiments.

Speaker: Carlos Peña Garay (Laboratorio Subterraneo de Canfranc)

Slides LSC_CPG_TAUP19.pdf

Tuesday, September 10

90 Multimessenger astronomy with very high energy gamma ray observation

Speaker: Dr Jim Hinton (MPI Kernphysik)

Slides Plenary_III_Hinton.pdf

91 Dark matter signature in Cosmic Ray observation

Speaker: Dr Alessandro Cuoco (Aachen Univ.)

Slides Plenary_III_Cuoco.pdf

92 Origin of ultra high energy cosmic ray and high energy neutrino

Speaker: Dr Kohta Murase (Penn. State Univ.)

Slides Plenary_III_Murase.pdf

10:30 AM Coffee break

93 Very high energy neutrinos from blazars

Speaker: Dr Matteo Cerruti (Universitat de Barcelona)

Slides Plenary_IV_Cerruti.pdf

94 Inflation models and future CMB B-mode observations

Speaker: Dr Kazunori Kohri (KEK / Sokendai)

95 Dark Matter and structure formation

Speaker: Dr Hai-Bo Yu (US Riverside, USA)

Slides Plenary_IV_HaiBoYU.pdf

DM5: Axions and Axion-Like Dark Matter II

96 New Axion Dark Matter Search with Proto-Planetary Disks

We find that the polarimetric observations of protoplanetary disks are useful to search for ultralight axion (ALPs) dark matter. Axion dark matter predicts the rotation of the linear polarization plane of propagating light, and protoplanetary disks are ideal targets to observe it. We show that a recent observation puts the tightest constraint on the axion-photon coupling constant for axion mass m < 10^{−21}eV.

Speaker: Dr Tomohiro Fujita (Kyoto University)

Slides TAUP_Fujita_talk.pptx

97 Dynamics of axion strings and implications for axion dark matter

We present the result of our recent simulation of cosmological axion strings. The QCD axion is one of the best motivated particles beyond the standard model and promising candidate of dark matter (DM). IF the spontaneous breaking of the Peccei-Quinn global U(1) symmetry takes place after inflation, DM axions are predominantly produced from axion strings. However, due to lack of our understanding of global strings, estimated abundance of produced DM axion remains yet uncertain. Based on field theoretic simulation of axion strings, we traced the behavior of cosmic axion strings for the longest term ever. We for the first time found that the number of axion strings per horizon grows logarithmically in time. This indicates the relic abundance of DM axion from strings may be increased significantly from previous estimates. We will discuss implications of our result for direct detection experiments.

Speaker: Dr Toyokazu Sekiguchi (RESCEU, University of Tokyo)

Slides DM5_ToyokazuSekiguchi.pdf

98 A Unique Multi-Messenger Probe of QCD Axion Dark Matter

We propose a multi-messenger probe of the natural parameter space of QCD axion dark matter (DM) based on observations of black hole-neutron star binary inspirals. It is suggested that a dense DM spike may grow around intermediate mass black holes. The presence of such a spike produces two unique effects: a distinct phase shift in the gravitational wave strain during the inspiral period and an enhancement of the radio emission from the resonant axion-photon conversion occurring in the neutron star magnetosphere. Remarkably, the observation of the gravitational wave signal can be used to infer the DM density and, consequently, to predict the radio emission. Given a sufficiently nearby detection with the LISA interferometer and next-generation radio telescope Square Kilometre Array, I will show that such observations can explore the QCD axion in the mass range $10^{−7}$eV to $10^{−5}$eV, potentially providing a striking multi-messenger signature of QCD axion DM.

Speaker: Mr Thomas Edwards (GRAPPA, University of Amsterdam)

Slides Axions_TAUP_Edwards.pdf

99 Detecting axion-like particles at radio frequencies.

Assuming that dark matter is composed by axion-like particles, we investigate the the possibility of detecting their decay into photons at radio frequencies. We discuss different astrophysical targets, such as dwarf spheroidal galaxies, the Galactic Center and halo, and galaxy clusters. The presence of an ambient radiation field leads to a stimulated enhancement of the decay rate, amplifying the photon flux by serval orders of magnitude, depending on the environment and the mass of the axion. For axion-photon couplings allowed by astrophysical and laboratory constraints (and possibly favored by stellar cooling), we find the signal to be within the reach of next-generation radio telescopes such as the Square Kilometer Array.

Speaker: Dr Marco Taoso (Istituto Nazionale di Fisica Nucleare (INFN) Sezione di Torino)

Slides MTaoso_TAUP.pdf

100 DM Radio Pathfinder: A Superconducting Lumped-Element Resonator for Wave-Like Dark Matter

There is compelling evidence that the vast majority of matter in the universe is not explained by the standard model, and interacts only weakly with ordinary matter. However, the identity of dark matter remains a mystery. While weakly interacting massive particles (WIMPs) have been the focus of direct detection searches for several decades, there is growing interest in ultra-light, wave-like dark matter. The Dark Matter Radio (DM Radio) is a sensitive search for axion and hidden photon dark matter covering the peV to $\mu$eV mass range. The DM Radio Pathfinder is a proof-of-concept detector operating in a liquid helium bath. The Pathfinder uses a superconducting, tunable lumped-element LC resonator with dc SQUID readout. The Pathfinder experiment has two main goals: to serve as a technology development platform for the full-sized cubic meter DM Radio, and to search a new portion of hidden photon parameter space. We present the design and preliminary data from the Pathfinder, which will search for hidden photon dark matter between 100 kHz and 10 MHz in its full scan.

Speaker: Stephen Kuenstner (Stanford University)

Slides KuenstnerTAUP2019slides.pdf

DM6: Indirect detection

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

101 Dark matter distribution in the Galactic dwarf spheroidal galaxies

The Galactic dwarf spheroidal (dSph) galaxies are excellent laboratories to shed light on fundamental properties of dark matter. In particular, the dSphs are promising targets for the indirect searches for particle dark matter. In order to set robust constraints on properties of dark matter particles, revealing dark matter distributions in these galaxies is of crucial importance. However, there are various non-negligible systematic uncertainties on the estimate of dark matter distributions in these galaxies. Therefore, it is necessary to address the development of dynamical models considering the effects of these systematic uncertainties. In this talk, we will introduce our constructed dynamical models taking into account these uncertainties and present the inferred dark matter profiles in the classical dSphs using their current kinematic data. In addition, as an intriguing result, we will show that some of dSphs favor cusped dark halo rather than cored one even considering a mass-anisotropy degeneracy. Using these dark matter profiles, we will revisit the core-cusp problem and discuss a possible link between the inner slope of their dark halos and the star formation history.

Speaker: Dr Kohei Hayashi (ICRR, The University of Tokyo)

Slides TAUP_KH20190910.pdf

102 Modeling evolution of dark matter substructure and annihilation boost

Structure of dark matter halo is hierarchical. Among them, small-scale structures in dark matter halo (so-called subhalos,) can enhance dark matter annihilation signals. It is necessary to quantify boost factors by those subhalos to derive the property of dark matter with current/future gamma-ray observations. In order to derive the subhalo boost factors, calculations of halo structure covering more than 20 orders-of-magnitude in the halo mass up to redshift of ~10 are required. This is beyond the capability of the current state-of-art cosmological N-body simulation which is a widely-adopted method to study the halo structure. In this talk, I introduce our analytical approach for the formalism of subhalo evolutions and the resultant boost factors. I show that the constraints on the annihilation cross-section obtained by isotropic gamma-ray observations can be updated by several factors by taking the contribution from subhalos into account.

Speaker: Dr Nagisa Hiroshima (RIKEN)

Slides TAUP2019_hiroshima.pdf

103 Particle dark matter searches through cross-correlations between gamma-rays and neutral hydrogen intensity mapping

Dark matter in cosmic structures is expected to produce signals originated from its particle physics nature, among which the electromagnetic emission represents a relevant opportunity, whose intensity is directly linked to the amount of dark matter in galaxies and clusters. On the other hand, this emission is very faint, thus contributing only at the unresolved level. These unresolved radiation backgrounds are isotropic at first order, but must exhibit a degree of anisotropy since they originate from clustered dark matter haloes. This fact implies also that the anisotropies in the radiation fields should be correlated to the same matter distribution in the Universe. In this talk we propose to exploit this correlation by using the intensity mapping of the 21cm emission line of neutral hydrogen as the tracer of matter distribution, and gamma-rays as the tracer of particle dark matter annihilation. Intensity mapping has the advantage of not being flux limited in the measurement of the matter distribution (as instead galaxy catalogs are) since it does not need to identify individual galaxies, and offers excellent redshift information being a line emission. We show the expected level for this cross-correlation signal and we derive forecasts for the study of this novel signature through the combination of Fermi-LAT gamma-rays data and SKA intensity mapping capabilities.

Speaker: Ms Elena Pinetti (University of Turin)

Slides CrossCorrelations_Pinetti_Elena_TAUP2019.pdf

104 MeV Gamma-ray imaging spectroscopic observation for Galactic Center and Cosmic Background MeV gammas by SMILE-2+ Balloon Experiment

Recently, there appears lots of papers on the possibility of light Dark Matter (DM) in MeV and sub-GeV scale. Until now, only INTEGRAL and COMPTEL provided experimental data of 511keV of galactic center, and two spectra of g Galactic Diffuse MeV gammas (GDMG) and Cosmic Background MeV gammas (CBMG) for indirect detection of light DMs. However except 511keV, those two spectra included large statistical and systematic errors in spite of 10 years observation, since both two instruments suffered from severe background radiation in space. Thus, experimentally its detection seems very difficult. In 2018 April, we (SMILE-project in Comic-ray Group of Kyoto University) have observed MeV gamma rays for southern sky by Electron Tracking Compton Camera (ETCC) using JAXA balloon at Australia during one-day. (SMILE2+ Project) By measuring all parameters of Compton scattering in every gamma, ETCC has achieved for the first time to obtain the complete direction of MeV gammas same as optical telescopes, and also to distinguish signal gammas from huge background gammas in space. In this observation, ETCC with a large Field of View of 3sr observed MeV gammas from 3/5 of all sky including galactic center, a half disk, crab, and most of CBMG By reconstructing the Compton process, we successfully obtained pure comic gammas by reducing background by more 2 orders, which is clearly certificated by the clear enhancement of detected gamma flux with ~30% during galactic center passing through the FoV, which is consistent with the ratio of CBMG and GDMG. Now 511keV gammas GDMG are preliminarily detected with ~5 and >10 sigma respectively around Galactic Center. Also we have obtained near 105events of CBMG in which contains only a few 10% background. Thus we obtained good data for both with high statistics and very low systematics even one day observation due to the dramatic improvement of imaging method. Here we will present the both differential fluxes of CBMG and GDMG with high statistics and very low systematics, which will be a first reliable data for discussing the possibility of light DM.

Speaker: Prof. Toru Tanimori (on behalf of SMILE project, Kyoto University)

Slides TAUP2019v4.pptx

105 The GAPS experiment – a search for cosmic-ray antinuclei from dark matter

The General Antiparticle Spectrometer (GAPS) is a balloon-borne experiment which aims to survey low-energy cosmic-ray antinuclei. A novel detection concept that utilizes the physics of exotic atoms allows GAPS to realize a large sensitive area, a low energy threshold, and a high identification capability for antinuclei. The primary goal is to search for antideuterons in the energy region <0.25 GeV/n, where they are predicted to be background-free probes for dark matter-annihilation or decay in the Galactic halo. GAPS will also measure precise low-energy antiproton spectra, which provide crucial information about the source and propagation of cosmic rays. Three flights on long-duration balloons from Antarctica are planned; the first flight of GAPS is scheduled for late 2021. We will present the scientific motivation, detection concept, development status, and plans for GAPS.

Speaker: Dr Masayoshi Kozai (ISAS/JAXA)

Slides TAUP_GAPS_Kozai_20190905.pdf

DM7: Low Mass Dark Matter I

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

106 Dark matter search results from DAMIC at SNOLAB

The DAMIC experiment uses thick fully-depleted charge-coupled devices (CCDs) to search for the interactions of dark matter particles in the galactic halo with ordinary silicon atoms. Because of their low instrumental noise, DAMIC CCDs are particularly sensitive to the ionization signals expected from low-mass dark matter particles. Since early 2017, DAMIC has collected dark-matter search data with a seven-CCD array (40-gram target) installed in a low radiation environment in the SNOLAB underground laboratory. I will present recent results from the searches for WIMP and hidden-sector dark matter, which cover a wide range of particle masses from ~1 MeV/$c^2$ to ~10 GeV/$c^2$. In particular, we probe—for the first time with the same nuclear target—a large fraction of the parameter space corresponding to the event excess previously observed by the CDMS-II silicon experiment.

Speaker: Prof. Alvaro Chavarria (University of Washington)

Slides Chavarria_DAMIC_TAUP2019.pdf

107 Latest results of CRESST-III’s search for sub-GeV/c² dark matter

The CRESST-III experiment searches for direct interactions of dark matter with ordinary matter at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy. The main event signature would be a nuclear recoil inside one of the scintillating target crystals. Operating the crystals as cryogenic calorimeters at $\mathcal{O}(10\,\mathrm{mK})$ provides in addition a phonon signal as measure of the deposited energy. The simultaneous readout of both a scintillation light and a phonon signal is used to actively discriminate backgrounds. CRESST-III focuses on the sub-GeV/c² mass region where the sensitivity is driven by the threshold. With a $\mathrm{CaWO_4}$ crystal of $24\,\mathrm{g}$ as target an unprecedented low threshold of $30.1\,\mathrm{eV}$ for nuclear recoils was obtained in the first data taking campaign of CRESST-III from 2016-2018. In this contribution, we will report the status of the experiment. We will discuss the latest results, both spin-dependent and spin-independent. Finally, we will give an outlook to future stages of CRESST.

Speaker: Dr Holger Kluck (TU Wien / HEPHY)

Slides Kluck_2019-09-10_TAUP2019.pdf

108 Current Status of SuperCDMS SNOLAB and Results from Sub-GeV Dark Matter with a Reduced Threshold SuperCDMS-Style Detector

The SuperCDMS (Cryogenic Dark Matter Search) SNOLAB experiment will search for dark matter using ultra-sensitive phonon sensors operated at cryogenic temperatures. Currently, we are in the construction phase. We anticipate commissioning and operations next year. In preparation for operations, the readout electronics were commissioned using a reduced-threshold SuperCDMS-style detector in an above-ground test facility to explore the sub-GeV dark matter parameter space. In this talk, I will present the current status of SuperCDMS SNOLAB construction as well as results from this sub-GeV dark matter search.

Speaker: Dr Tsuguo Aramaki (SLAC)

Slides TAUP2019_CDMS_TsuguoAramaki.pdf

109 Recent results from EDELWEISS Dark Matter searches

The EDELWEISS collaboration is performing direct searches for light Dark Matter particles using cryogenic germanium detectors equipped with a charge and thermal signal readout. This versatile and highly performing technology opens new possibilities for searches for signals involving either electrons or nuclear recoils. This is attested to by results on Axion-Like Particles in the keV range, and by the attainment of the first sub-GeV spin-independent dark matter limit based on a germanium target. The search has been extended to Strongly Interacting Particles (SIMP) down to 45 MeV by exploiting the Migdal effect. New results on SIMPs with spin-dependent interactions will also be presented.

Speaker: Prof. Jules Gascon (Lyon University and IN2P3/CNRS)

Slides Edelweiss-taup2019.pdf

110 NEWS-G : search for low mass Dark Matter with light targets

NEWS-G (New Experiments With Spheres-Gas) is an experiment searching for dark matter using the Spherical Proportional Counter (SPC) technique. Such detectors can operate significant mass of target, of order of kgs with meter size spheres, while keeping single ionization electron detection sensitivity and can be filled with gaseous targets of low atomic mass such as hydrogen, helium, and neon. NEWS-G aspires to extend the sensitivity of direct dark matter searches to the mass range from 0.1 GeV to few GeV, opening a window to non-standard model physics. The talk will cover principle of operations and results obtained with a 60 cm diameter prototype detector, operated in the underground laboratory of Modane (LSM, France) with neon as target nucleus, which allowed to exclude at 90% confidence level cross-sections above 4.4・10-37 cm2 for a 0.5 GeV/c2 WIMP. As well will be presented the status and projected sensitivity of the 140 cm diameter full-scale detector with compact shielding. It will be installed in SNOLab (Canada) at the beginning of 2020 and is currently being tested in LSM. Another contribution to this conference describes the R&D activities led within the collaboration to optimize detector operation and sensitivity for Dark Matter searches.

Speaker: Dr Gilles Gerbier (Queen's University)

Slides NEWSG_TAUP_sep19_GG.pptx

Gravitational Wave #3

111 Inference on the massive black hole binary population from pulsar timing array searches for gravitational waves

Massive black holes reside at the centre of most galaxies. During galaxy mergers, the massive black holes at the centres of each galaxy are believed to form binaries, which can emit gravitational waves in the nano-Hertz frequency band. Pulsar timing arrays are being used to search for the gravitational wave background from many massive binary black hole binaries throughout cosmic time. No detection has yet been made, however pulsar timing arrays are placing upper limits on the strength of the gravitational wave background from these sources. As upper limits improve with sensitivity, we can make comparisons to astrophysical models of the population of massive black hole binaries. A lack of detection could indicate that either these binaries stall before reaching gravitational wave emission or are accelerated through the band. Using Bayesian hierarchical modelling we consider implications of this upper limit for a range of astrophysical scenarios, without invoking stalling, nor more exotic physical processes (Nat. Comm 9, 537, 2018). We find these models to be consistent so far, however as sensitivity improves the most optimistic predictions will become disfavoured.

Speaker: Dr Hannah Middleton (University of Melbourne)

Slides HMiddletonTAUPToyama2019.pdf

112 Astrophysical numerical relativistic simulations: Hypermassive Neutron stars and Core-collapse Supernovae

The inner structures and equations of state inside neutron stars/ proto-neutron star formed by core-collapse supernovae (CCSN) are mysterious. Particularly, by using a new multidimensional general relativistic hydrodynamics simulation code with neutrino schemes to investigate the pulsations/oscillations of proto-neutron stars(formed from CCSN) and Hypermassive neutron stars(formed from Binary neutron stars merger), we present the evolution of neutron stars, the various oscillation modes, and gravitational-wave.

Speaker: Mr HO YIN NG (The Chinese University of Hong Kong)

Slides taup2019ppt.pdf

113 Binary black holes originating from globular clusters as sources of gravitational waves

Stellar mass binary black holes are the most important sources of gravitational waves for ground based interferometric detectors. We analyze about a thousand globular cluster (GC) models simulated using the MOCCA Monte Carlo code for star cluster evolution to study black hole - black hole interactions in these dense stellar systems that can lead to gravitational wave emission. We extracted information for all coalescing binary black holes (BBHs) that merge via gravitational radiation from these GC models and for those BHs that collide due to 2-body, 3-body and 4-body dynamical interactions. By obtaining results from a substantial number of realistic star clusters evolution model, that cover different initial parameters (masses, metallicities, densities etc) we have an extremely large statistical sample oftwo black holes which merge or collide within a Hubble time. We determine the astrophysical properties and local merger rate densities for coalescing binary black holes (BBHs) originating from globular clusters. The existence of Intermediate Mass Black Hole strongly influences the results. I will discuss the importance of BBH originating from GC for gravitational waves observations.

Speaker: Prof. Dorota Rosinska (University of Warsaw)

Slides Rosinska_TAUP2019.pdf

114 Formation of binary black holes in star clusters as gravitational wave sources

Direct detections of gravitational wave suggest that $\sim 30$ solar mass binary black holes (BBHs) commonly exist in the Universe. One possible formation scenario of such BBHs is dynamical three-body encounters in a dense core of globular clusters, which consist of millions of stars. Compared to globular clusters, open clusters are less dense and less massive but more populous. Because of their shallow potential, they have not been considered to be a formation site of merging BBHs. However, we found a new channel for the formation of BBHs, which is dominant in open clusters. We performed direct N-body simulations of open clusters with a mass of $10^3$ -- $10^4$ solar mass for metallicity of $Z/Z_\odot = 0.1$. The core-collapse time of open clusters is much shorter than that of globular clusters. Therefore, massive main-sequence stars can form binaries before they evolve to BHs. These main-sequence binaries experience mass transfer evolution, and some of them evolve to BBHs merging within the Hubble time. From our simulations, we estimated the merger rates of BBHs originated from open clusters and found that it is comparable to that of globular clusters if we take a cluster mass function into account. Thus, open clusters can be a dominant formation site of BBHs as gravitational wave sources.

Speaker: Dr Jun Kumamoto (The University of Tokyo)

Slides slide.pptx

115 Stochastic gravitational wave background mapmaking using regularised deconvolution

Obtaining a faithful source intensity distribution map of the sky from noisy data demands incorporating known information of the expected signal, especially when the signal is weak compared to the noise. We introduce a widely used procedure to incorporate these priors through a Bayesian regularisation scheme in the context of map-making of the anisotropic stochastic GW background (SGWB). Specifically, we implement the quadratic form of regularizing function with varying strength of regularization and study its effect on image restoration for different types of the injected source intensity distribution in simulated LIGO data. We find that regularization significantly enhances the quality of reconstruction, especially when the intensity of the source is weak, and, most importantly, dramatically improves the stability of deconvolution. I will talk more about this method, and it's advantages in this presentation.

Speaker: Dr Jishnu Suresh (ICRR, the University of Tokyo)

Slides Jishnu_TAUP19.pdf

HECR #3

116 IceCube Search for Galactic Sources of High-Energy Neutrinos based on HAWC Observations

Galactic cosmic rays reach energies of at least several PeV, and their interactions should generate gamma rays and neutrinos from the decay of secondary pions. Therefore, Galactic sources are guaranteed to contribute to the total high-energy cosmic neutrino flux observed by IceCube. We present a search in IceCube data for neutrino emission from Galactic TeV gamma-ray sources detected by the HAWC Gamma Ray Observatory. HAWC serves as an excellent instrument to complement IceCube, with its energy range extending to very high energies. Assuming that the highest energy photons originate from the decay of pions, the very high energy gamma-rays observed by HAWC are expected to be correlated with neutrinos. Using eight years of IceCube data, we report two different analyses to test for this possible neutrino-gamma ray correlation. The first is a stacked analysis of identified HAWC point sources and the second is a template method that accounts for the full morphology of HAWC sources, including extension.

Speaker: Ali Kheirandish (University of Wisconsin-Madison)

Slides taup2019_alikheirandish.pdf

117 CALET results after three years on the International Space Station

The CALET (CALorimetric Electron Telescope) space experiment, which is currently conducting direct cosmic-ray observations onboard the International Space Station (ISS), uses an all-calorimetric instrument with total vertical thickness of 30 radiation lengths and fine imaging capability. The instrument is optimized for cosmic-ray electron measurements by achieving large proton rejection and excellent energy resolution well into the TeV energy region. In addition, very wide dynamic range of energy measurements and absolute charge identification capability of the instrument enable us to measure proton and nuclei spectra as well as electron and gamma-ray spectra. The CALET mission goals include the investigation of acceleration and propagation of galactic cosmic rays, of possible nearby sources, and of potential signature of dark matter. During a mission life of five years (or more), the CALET experiment will be measuring the flux of cosmic-ray electrons (including positrons) to 20 TeV, gamma-rays to 10 TeV and nuclei with Z=1 to 40 up to 1,000 TeV for the more abundant elements. Since the start of observation in October 2015, smooth and contiunous operations have taken place. In this contribution, we will give a brief summary of the CALET observation: 1) electron energy spectrum, 2) proton and nuclei spectrum, 3) gamma-ray observation including transient search.

Speaker: Dr Yoichi Asaoka (WISE, Waseda University)

Slides 190910TAUP-CALET-asaoka-upload.pdf

118 The GRAMS Project: Dual MeV Gamma-Ray and Dark Matter Observatory

GRAMS (Gamma-Ray and AntiMatter Survey) is a novel project that can simultaneously target both astrophysical observations with MeV gamma rays and an indirect dark matter search with antimatter. The GRAMS instrument is designed with a cost-effective, large-scale LArTPC detector surrounded by plastic scintillators. With more than an order of magnitude improved sensitivity, GRAMS can measure gamma-ray lines in the poorly explored MeV energy band, which is the key to understand the nucleosynthesis, including possible gamma-ray emission from neutron star mergers for multi-messenger astronomy. GRAMS will also be a next-generation experiment beyond the GAPS project for antimatter survey. In particular, low-energy antideuterons will provide essentially background-free dark matter signatures and GRAMS could fully investigate the parameter space suggested by the possible dark matter detection by Fermi and AMS-02. The project is working towards the development of a balloon experiment, which will become a milestone for a future satellite mission. In this talk, I will present an overview of the GRAMS project, focusing on the detection concept and science goals.

Speaker: Dr Tsuguo Aramaki (SLAC)

Slides TAUP2019_GRAMS_TsuguoAramaki.pdf

Neutrino #7

Convener: Dr Itaru Shimizu (Tohoku University)

119 Experimental studies of axial-vector weak couplings for double beta decays and astro neutrinos.

Nuclear matrix elements (NMEs) and the axial-vector weak coupling $g_A$ are crucial for double beta decays(DBDs) and astro neutrino studies, but theoretical calculations for them are hard. We report experimental studies for them by using charge exchange ($^3$He,t) reactions and muon capture reactions. We show for the first time that single-beta NMEs and the coupling $g_A$ are quenched uniformely by a factor $g_A^{eff}$/$g_A^{free}$ = 0.5-0.6 with respect to the pnQRPA model calculations in the wide multipolarities of $J^{\pm}$ and the momentun transfers of 20-120 MeV/c. These are just the regions of DBD and astro neutrino interests. The quenching is due to non-nucleonic correlations such as $\Delta$ isobar and nuclear medium effects. The impact of the quenching for DBD and astro neutrinos is discussed. H. Ejiri, J. Suhonen and K. Zuber 2019, Physics Report 791 1. H. Ejiri, Frontiers in Physis 2019, 10.3389/fyhs. 2019.00030. I. Hashim, H. Ejiri et al. 2018, Phys. Rev. C 97 014617.

Speaker: Prof. Hiroyasu Ejiri (RCNP Osaka University)

Slides Ejiri_TAUP19.pptx

120 Recent Results and Status of EXO-200

The EXO-200 Collaboration has been searching for neutrinoless double beta decay ($0\nu\beta\beta$) using a liquid xenon time projection chamber filled with ~150kg of enriched Xe$^{136}$. EXO-200 began data taking in September 2011 and has now completed operations as of December 2018. The inclusion of advanced analysis techniques that maximize the topological discrimination between $0\nu\beta\beta$ signal and gamma backgrounds, along with hardware upgrades that have improved the resolution over the last data taking run have allowed EXO-200 to provide one of the most sensitive searches for 0vBB. This talk will present the most recent results from the collaboration including the analysis of the full dataset.

Speaker: Mr Michael Jewell (Stanford University)

Slides exo200_taup2019_jewell_final.pptx

121 Results and post-upgrade performance of GERDA Phase II

Excellent spectroscopic performance, event topology information and outstanding radiopurity are unique properties of High Purity Germanium (HPGe) detectors that facilitate the search for neutrinoless double beta (0$\nu\beta\beta$) decay of $^{76}$Ge. A detection of this process would shed light onto physics beyond the standard model as it would reveal the Majorana nature of neutrinos. The Germanium Detector Array (GERDA) experiment employs 44.2 kg of HPGe detectors with an isotopic fraction of 87% $^{76}$Ge in a liquid argon active shield at Laboratori Nazionali del Gran Sasso (LNGS) in Italy. The combination of an ultra-low background environment with active background rejection techniques allows the exploration of 0$\nu\beta\beta$ half-lives beyond 10$^{26}$ yr. No signal has been found in 58.9 kg$\cdot$yr of data in 2018, from which the most stringent limit on 0$\nu\beta\beta$ decay of $^{76}$Ge has been derived. More than one year of additional data has been collected after an upgrade of the Phase II experimental setup. The latest results, as well as an insight into the performance of GERDA after this upgrade, will be presented in this talk.

Speaker: Christoph Wiesinger (Technische Universität München)

Slides 20190910_TAUP_GERDA.pdf

122 Majorana Demonstrator Updated 0vBB Search and Background Characterization

The Majorana Demonstrator neutrinoless double-beta decay experiment comprises modular germanium detector arrays comprising 44.8 kg of germanium, 29.7 kg of which have been fabricated from germanium enriched to 88% in germanium-76 with the aims of probing neutrinoless double-beta decay, searching for new physics beyond the standard model, and demonstrating backgrounds sufficiently low to justify and inform a future ton-scale experiment. The Demonstrator's detectors are operated within a pair of vacuum cryogenic modules constructed primarily from underground-electroformed ultra-pure copper and low-background plastic materials, housed in a compact lead, copper and polyethylene radiological shield located at the 4850-ft level of the Sanford Underground Research Facility. The Demonstrator's detector modules have been operating since 2016. Optimization of background-reducing analysis techniques is expected to yield improved background rejection; new results from an improved analysis applied to a subset of the total collected exposure to date will be presented. A model of the Majorana Demonstrator observed backgrounds, key to informing the design and background expectations in the next-generation LEGEND experiment, will be discussed.

Speaker: Prof. Matthew Green (North Carolina State University &amp; Oak Ridge National Laboratory)

Slides 2019_09_TAUP_MGreen_MajoranaDemonstrator.pdf

Neutrino #8

Convener: Dr Itaru Shimizu (Tohoku University)

123 Modular invariance approach to masses and mixing of neutrino flavors

I present the new approach of flavor symmetry, which is based on modular invariance. I discuss the phenomenological implications of the modular symmetry $\Gamma(3) \simeq A_4$ of lepton flavors facing recent experimental data of neutrino oscillations. The mass matrices of neutrinos and charged leptons are essentially given by fixing the expectation value of modulus $\tau$, which is the only source of modular invariance breaking. I also discuss the quark sector by the modular symmetry.

Speaker: Dr Morimitsu Tanimoto (Niigata University)

Slides TAUP2019-tanimoto.pdf

124 New Physics and (vector, scalar, dark) Non-Standard Interactions in Neutrino Oscillation

The neutrino oscillation can probe not only the neutrino mass matrix but also the neutrino interactions. In other words, it provides two possible ways of determing the new physics beyond the SM. A commonly discussed example is the vector non-standard interactions (NSI) by vector mediators other than W & Z. We introduce another two possibilities of the scalar & dark NSIs. The scalar NSI is an analogy of the vector one with scalar mediator instead but has totally different phenomenological consequences. With the effect of vector NSI depends linearly on the neutrino energy, the scalar NSI is energy independent and introduces direct correction to the neutrino mass term. The dark NSI is even more interesting. In the absence of any extra mediator, the neutrino mass squared term can be modified by the matter potential of neutrinos propagating through the dark matter (DM) medium and it violates the CPT violation without breaking the CPT symmetry at the fundamental Lagrangian. The neutrino oscillation experiment provides another way of testing DM.

Speaker: Dr Shao-Feng Ge (T.D.Lee Institute, Shanghai Jiao-Tong University)

Slides 190910_TAUP.pdf

125 Constraints on Nonstandard Neutrino Interaction from Neutrino Electron Scattering

Neutrino electron scattering is a purely leptonic fundamental interaction and therefore provides an important channel to test Standard Model especially at the low energy-momentum transfer regime. Constraints on neutrino non-standard interactions (NSI) couplings depending on model independent approaches, which are described by a four-Fermi point like interaction, are derived. The upper limits and the allowed regions of vectorial, scalar, pseudo-scalar and tensorial NSI couplings of neutrinos are derived at 90% confidence level in both one-parameter and two-parameter analysis. In addition, constraints on couplings of several Beyond Standard Model (BSM) physics scenarios are placed via neutrino electron scattering channel to test Standard Model at low energy-momentum transfer regime which are mediated by massive intermediate particles which include: (1) Extra Z-prime, (2) New Light Spin-1 Boson, (3) Dark Photon, and (4) Charged Higgs Boson. Bounds to coupling constants of Flavor Conserving and Flavor Violation New Light Spin-1 Boson, Dark Photon, and Charged Higgs Boson with respect to different mass of mediators are placed. The relevant parameter spaces are extended by allowing light mediators. New lower mass limits for extra Z-prime gauge boson models are placed. Data on neutrino and anti-neutrino electron scattering from the TEXONO and LSND experiments, respectively, are used.

Speaker: Prof. Deniz Muhammed (Dokuz Eylul University)

Slides TAUP_2019_md.pdf

126 Electromagnetic neutrinos: New constraints and new effects in oscillations

We continue our discussions [1-3] of neutrino electromagnetic properties and give a short introduction to the derivation of the general structure of the electromagnetic form factors of Dirac and Majorana neutrinos. Then we consider experimental constraints on neutrino magnetic and electric dipole moments, electric millicharge, charge radii and anapole moments from the terrestrial laboratory experiments (the bounds obtained by the reactor MUNU, TEXONO and GEMMA experiments and the solar Super-Kamiokande and the recent Borexino experiments). A special credit is done to the recent and most severe constraints on neutrino magnetic moments, millicharge and charge radii [4-8]. The world best reactor [4] and solar [5] neutrino and astrophysical [9,10] bounds on neutrino magnetic moments, as well as bounds on millicharge from the reactor [6] neutrinos fluxes are included in the recent issues of the Review of Particle Physics (see the latest Review: M. Tanabashi et al. (Particle Data Group), Phys. Rev. D 98 (2018) 030001). The best astrophysical bound on neutrino millicharge was obtained in [11]. The main manifestation of neutrino electromagnetic interactions, such as: 1) the radiative decay in vacuum, in matter and in a magnetic field, 2) the neutrino Cherenkov radiation, 3) the plasmon decay to neutrino-antineutrino pair, 4) the neutrino spin light in matter, and 5) the neutrino spin and spin-flavour precession are discussed. Phenomenological consequences of neutrino electromagnetic interactions (including the spin light of neutrino [12]) in astrophysical environments are also reviewed. We present results of the recent detailed study [13] of the electromagnetic interactions of massive neutrinos in the theoretical formulation of low-energy elastic neutrino-electron scattering. The formalism of neutrino charge, magnetic, electric, and anapole form factors defined as matrices in the mass basis with account for three-neutrino mixing is presented. Using the derived new expression for a neutrino electromagnetic scattering cross section [13], we further developed studies of neutrino electromagnetic properties using the COHERENT data [7] and obtained [8] new bounds on the neutrino charge radii from the COHERENT experiment. Worthy of note, our paper [8] has been included by the Editors Suggestion to the Phys. Rev. D “Highlights of 2018”. The concluding part of the proposed talk is dedicated to results of our recently performed detailed studies of new effects in neutrino spin, spin-flavour and flavor oscillations under the influence of the transversal matter currents [14] and a constant magnetic field [15, 16]. The discussed two new effects can be summarized as follows: 1) it is shown [14] that neutrino spin and spin-flavor oscillations can be engendered by weak interactions of neutrinos with the medium in the case when there are the transversal matter currents; different possibilities for the resonance amplification of oscillations are discussed, the neutrino Standard Model and non-standard interactions are accounted for; 2) within a new treatment [15] of the neutrino flavor, spin and spin-flavour oscillations in the presence of a constant magnetic field, that is based on the use of the exact neutrino stationary states in the magnetic field, it is shown that there is an interplay of neutrino oscillations on different frequencies; in particular: a) the amplitude of the flavour oscillations νLe↔ νLμ at the vacuum frequency is modulated by the magnetic field frequency μB , and b) the neutrino spin oscillation probability (without change of the neutrino flavour) exhibits the dependence on the neutrino energy and mass square difference Δm2 . The discovered new phenomena in neutrino oscillations should be accounted for reinterpretation of results of already performed experiments on detection of astrophysical neutrino fluxes produced in astrophysical environments with strong magnetic fields and dense matter. These new neutrino oscillation phenomena are also of interest in view of future experiments on observations of supernova neutrino fluxes with large liquid-scintillator detectors like JUNO, for instance. The best world experimental bounds on neutrino electromagnetic properties are confronted with the predictions of theories beyond the Standard Model. It is shown that studies of neutrino electromagnetic properties provide a powerful tool to probe physics beyond the Standard Model. References: [1] C. Guinti and A. Studenikin, “Neutrino electromagnetic interactions: A window to new physics”, Rev. Mod. Phys. 87 (2015) 531-591. [2] C. Giunti, K. Kouzakov, Y. F. Li, A. Lokhov, A. Studenikin, S. Zhou, Electromagnetic neutrinos in laboratory experiments and astrophysics, Annalen Phys. 528 (2016) 198. [3] A.Studenikin, “Neutrino electromagnetic interactions: A window to new physics - II”, PoS EPS-HEP2017 (2017) 137. [4] A. Beda, V. Brudanin, V. Egorov et al., “The results of search for the neutrino magnetic moment in GEMMA experiment”, Adv. High Energy Phys. 2012 (2012) 350150. [5] M. Agostini et al (Borexino coll.), “Limiting neutrino magnetic moments with Borexino Phase-II solar neutrino data”, Phys. Rev. D 96 (2017) 091103. [6] A. Studenikin, “New bounds on neutrino electric millicharge from limits on neutrino magnetic moment”, Europhys. Lett. 107 (2014) 21001. [7] D. Papoulias, T. Kosmas, “COHERENT constraints to conventional and exotic neutrino physics”, Phys. Rev. D 97 (2018) 033003. [8] M. Cadeddu, C. Giunti, K. Kouzakov, Y.F. Li, A. Studenikin, Y.Y. Zhang, “Neutrino charge radii from COHERENT elastic neutrino-nucleus scattering”, Phys. Rev. D 98 (2018) 113010. [9] N. Viaux, M. Catelan, P. B. Stetson, G. G. Raffelt et al., “Particle-physics constraints from the globular cluster M5: neutrino dipole moments”, Astron. & Astrophys. 558 (2013) A12. [10] S. Arceo-Díaz, K.-P. Schröder, K. Zuber and D. Jack, “Constraint on the magnetic dipole moment of neutrinos by the tip-RGB luminosity in ω-Centauri”, Astropart. Phys. 70 (2015) 1. [11] A. Studenikin, I. Tokarev, “Millicharged neutrino with anomalous magnetic moment in rotating magnetized matter”, Nucl. Phys. B 884 (2014) 396-407. [12] A. Grigoriev, A. Lokhov, A. Studenikin, A. Ternov, “Spin light of neutrino in astrophysical environments”, JCAP 1711 (2017) 024 (23 p.). [13] K. Kouzakov, A. Studenikin, “Electromagnetic properties of massive neutrinos in low-energy elastic neutrino-electron scattering”, Phys. Rev. D 95 (2017) 055013. [14] P. Pustoshny, A. Studenikin, "Neutrino spin and spin-flavour oscillations in transversal matter currents with standard and non-standard interactions", Phys. Rev. D98 (2018) no.11, 113009. [15] A. Popov, A. Studenikin, "Neutrino eigenstates and flavour, spin and spin-flavour oscillations in a constant magnetic field ", Eur.Phys.J. C79 (2019) no.2, 144. [16] P. Kurashvili, K. Kouzakov, L. Chotorlishvili, A. Studenikin, “Spin-flavor oscillations of ultrahigh-energy cosmic neutrinos in interstellar space: The role of neutrino magnetic moments”, Phys. Rev. D 96 (2017) 103017.

Speaker: Prof. Alexander Studenikin (Moscow State University & JINR-Dubna)

Slides org_Studenikin_TAUP_10_09_2019.pdf

127 The effects of coherent neutrino mixing modulation by dark matter.

If there was a coupling between neutrinos and Dark Matter, then there could be an induced modulation of the neutrino-mixing spectrum analogous to the one produced by the MSW effect. The possible results of such a modulation have previously been investigated for the case where coherent effects cannot be isolated and the resulting pattern is de-coherent. This presentation is on an investigation that included coherent effects, which are relevant for very high-energy neutrinos as the wave-packets remain coherent over cosmological distances. The investigation found that observable coherent effects are produced by potentials several orders of magnitude smaller than the minimum potential required to produce an observable de-coherent effect, with the amount being baseline dependent. This extends the range of observability down to levels where an interaction is likely to exist, if it exists at all. The significant challenges in making such an observation will be covered.

Speaker: Mr William Marks (School of Fundamental Sciences, Massey University)

Slides The_Effects_of_Coherent_Neutrino_Mixing_Modulation_by.pptx

Neutrino #9

Convener: Dr Itaru Shimizu (Tohoku University)

128 Neutrino physics beyond the Standard Model in DUNE

In the last decades, neutrino physics has experienced great progress. Nowadays, there is no doubt that neutrinos are massive and mix, giving rise to the flavor oscillation mechanism, rather well characterized by current data. However, there are still some uncertainties in the oscillation mechanism that will be addressed by the next generation of neutrino experiments, such as DUNE. Likewise, DUNE will explore the presence of new physics beyond the Standard Model (SM) through its effects in the neutrino signal. In this talk, I will discuss DUNE's sensitivity to some of these scenarios of new physics beyond the SM.

Speaker: Dr Mariam Tórtola (IFIC (CSIC / Universitat de València))

Slides TAUP2019-MTortola.pdf

129 Search for heavy neutrinos with the T2K near-detector ND280

The results from a search for heavy neutrinos with masses in the range 140 < $M_N$ < 493 MeV/c$^2$, using the off-axis near detector ND280 of the T2K experiment, will be reported. These particles can be produced from kaon decays in the standard neutrino beam and then subsequently decay in ND280. The decay modes under consideration are $N \to \ell^{\pm} \pi^{\mp}$ and $N \to \ell^{+} \ell^{-} \nu$. A search for such events has been made using the Time Projection Chambers of ND280, where the background has been reduced to less than two events in the current dataset in all channels. No excess has been observed in the signal region. Upper limits on the mixing elements of heavy neutrinos to electron-, muon- and tau- flavoured currents ($U_e^2$, $U_{\mu}^2$, $U_{\tau}^2$) as a function of the heavy neutrino mass have been computed. These constraints are competitive with the previous experiments such as E949 and PS191.

Speaker: Mr Mathieu Lamoureux (INFN Padova)

Slides 19-09-11_TAUP_HeavyNu.pdf

130 The SHiP experiment at CERN

The SHiP Collaboration has proposed a general-purpose experimental facility operating in beam dump mode at the CERN SPS accelerator with the aim of searching for light, long-lived exotic particles of Hidden Sector models. The SHiP experiment incorporates a muon shield based on magnetic sweeping and two complementary apparatuses. The detector immediately downstream of the muon shield is optimised both for recoil signatures of light dark matter scattering and for tau neutrino physics, and consists of a spectrometer magnet housing a layered detector system with heavy target plates, emulsion film technology and electronic high precision tracking. The second detector system aims at measuring the visible decays of hidden sector particles to both fully reconstructible final states and to partially reconstructible final states with neutrinos, in a nearly background free environment. The detector consists of a 50 m long decay volume under vacuum followed by a spectrometer and particle identification with a rectangular acceptance of 5 m in width and 10 m in height. Using the high-intensity beam of 400 GeV protons, the experiment is capable of integrating $2\times 10^{20}$ protons in five years, which allows probing dark photons, dark scalars and pseudo-scalars, and heavy neutrinos with GeV-scale masses at sensitivities that exceed those of existing and projected experiments. 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 can be explained. The sensitivity to light dark matter reaches well below the elastic scalar Dark Matter relic density limits in the range from a few MeV/c$^2$ up to 200 MeV/c$^2$. The tau neutrino deep-inelastic scattering cross-sections will be measured with a statistics a thousand times larger than currently available, with the extraction of the $F_4$ and $F_5$ structure functions, never measured so far, and allow for new tests of lepton non-universality with sensitivity to BSM physics. Following the review of the Technical Proposal, the CERN SPS Committee recommended in 2016 that the experiment and the beam dump facility studies proceed to a Comprehensive Design Study phase. These studies have resulted in a mature proposal submitted to the European Strategy for Particle Physics Update.

Speaker: Dr Annika Hollnagel (JGU Mainz)

Slides taup_2019_ship_hollnagel_nobackup.pdf

131 Detector physics with MicroBooNE

The MicroBooNE detector is a liquid argon time projection chamber (LArTPC), designed for the short-baseline neutrino physics program in the Booster neutrino beamline at Fermilab. Because of the exceptional calorimetric and tracking capabilities, LArTPCs are employed in many current and future neutrino experiments. MicroBooNE takes a crucial role as an operating physics experiment to characterise the performance of this technology. This talk will provide an overview of detector physics studies in MicroBooNE, including identification and filtration of excess TPC noise, signal calibration, and drift electron attenuation. Furthermore, we will present the measurement of the electric field which is vital for the performance of LArTPCs. The calibration techniques towards extracting the neutrino-physics measurements will aslo be presented.

Speaker: Yifan Chen (University of Bern)

Slides TAUP_Detector_Physics_with_MicroBooNE.pdf

New Technology #1

132 SiPM photosensor development for nEXO

The nEXO collaboration is developing a low-background detector to search for neutrinoless double beta decays in 5 tonnes of liquid xenon enriched in the isotope Xe-136. Both, 175 nm scintillation light and charge signals of events within the detector will be recorded to allow reconstruction of energy and position of each event. The nEXO collaboration identified Silicon Photon Multipliers (SiPMs) as the devices of choice for the detection of scintillation photons. Inside the detector, an area of about 4.5 m$^2$ has to be covered with SiPM devices with an overall light detection efficiency of more than 3%. This requires a SiPM dark-noise rate of less than 50 Hz/mm$^2$, a correlated avalanche rate of <0.2 and a photon-detection efficiency of more than 15% at 175 nm. This is required to achieve the anticipated energy resolution of =<1% with nEXO. Recent measurements of FBK SiPMs demonstrated their suitability for the application in nEXO. Integration of SiPMs into tiles of ~10x10 cm$^2$ area and larger is a focus of ongoing efforts. The development of the nEXO baseline concept with SiPMs is well advanced and results of the development will be presented.

Speaker: Dr Thomas Brunner (McGill and TRIUMF)

Slides 20190910-nEXO-photonsensors-TAUP.pdf

133 Development of low background PMT R13111

For underground low background experiment such as direct dark matter search, lowering the background from detector components is the one of the most important issue, especially for sensors which occupy largest amount of the components in many case. PMTs are used very often by many low background experiments, as a photo sensor, we developed a new low background PMT R13111 which is operable inside liquid xenon. We will report about the developed PMT, the RI amounts reduced less than 1/5 of R10789 used in the XMASS-I detector and the performance, together with explanation of the RI screening facilities in Kamioka observatory.

Speaker: Dr Ko Abe (ICRR, The University of Tokyo)

Slides 2019taup-abe-R13111-v4.pdf

134 Development and performance of the 20” PMT for Hyper-Kamiokande

Hyper-Kamiokande is the next generation water Cerenkov experiment in Japan, scheduled to start construction in 2020. This new experiment will build on the successful strategies developed in the currently running Super-Kamiokande experiment, and be able with unprecedented precision to study the oscillation of neutrinos from different sources and search for proton decay and neutrinos produced by supernovae. This increase in precision comes from the larger size of the detector, providing large statistics, and the use of high performance photo-detectors. In the baseline design, the inner part of the detector will be instrumented with 40000 20” PMTs. Two models are considered for this part: the nominal option is to use the R12860 produced by Hamamatsu Photonics, an improved version of the R3600 used in Super-Kamiodande, and micro-channel plate PMTs produced by North Night Vision Technology Co. are studied as an alternative option. We will present the developments on those two models to match the requirements and challenges of Hyper-Kamiokande: achieving high photon detection efficiency and timing resolution, while maintaining low noise level and being able to sustain the higher pressure coming from the increased water depth of this new detector. We will also report measurements of the performances of those PMTs and of their stability in time.

Speaker: Dr Christophe Bronner (Kamioka Observatory, ICRR, The University of Tokyo)

Slides HK_PMT.pdf

135 Large Area Photo-Detection System using 3" PMTs for the Hyper-Kamiokande Outer Detector

Hyper-Kamiokande, scheduled to begin construction as soon as 2020, is a next generation underground water Cherenkov detector, based on the highly successful Super-Kamiokande experiment. It will serve as a far detector, 295~km away, of a long baseline neutrino experiment for the upgraded J-PARC beam in Japan. It will also be a detector capable of observing --- far beyond the sensitivity of the Super-Kamiokande detector --- proton decay, atmospheric neutrinos, and neutrinos from astronomical sources. An Outer Detector (OD) consisting of PMTs mounted behind the inner detector PMTs and facing outwards to view the outer shell of the cylindrical tank, would provide topological information to identify interactions originating from particles outside the inner detector. Any optimization would lead to a significant improvement for the physics goals of the experiment, which are the measurement of the CP leptonic phase and the determination of the neutrino mass hierarchy. An original setup using small 3” PMTs is being designed for the Hyper-Kamiokande OD. They would give better redundancy, spatial, and angular resolution, as they would be twice or three times more photosensors that the original 8” design proposal of the experiment, and for a reduce cost. Several 3” PMTs candidates considered for the Hyper-Kamiokande OD have been characterized at Queen Mary University London. They all show a very low dark counts and good collection efficiency, which makes them excellent choice to be used in the experiment. In this talk/poster I will introduce the Hyper-K experiment with an emphasis on its sub-detector system. Then, I will show the expected performance of the system using a large array of 3" PMTs which performs better than the previous 8" design. The improvements on event selection with this new design will be discussed and how it affect the mass hierarchy sensitivity.

Speaker: Stephane Zsoldos (Queen Mary University of London)

Slides Zsoldos-Hyper-KOD-TAUP2019.pdf

136 Use of poly(ethylene naphthalate) as a self-vetoing structural material

Poly(ethylene naphthalate), PEN, is a commonly used high-performance industrial polyester plastic which has been observed to scintillate in the blue wavelength region, without the need for additional materials. Combined with measurements of a high intrinsic radiopurity, this has sparked interest in the material for use in low-background experiments. In this presentation, measurements of custom molded PEN tiles, covering a range of scintillation and structural properties will be discussed.

Speaker: Mr Felix Fischer (Max-Planck-Institute for Physics)

Slides PEN-Scintillator-Fischer.pdf

3:40 PM Break

DM10: Low Mass Dark Matter II

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

137 Low Energy Rare Event Searches with the Majorana Demonstrator

The Majorana Demonstrator is sensitive to rare events near its energy threshold, including bosonic dark matter, solar axions, and lightly ionizing particles. It is an array of ultra-low background, P-type point contact (PPC) high-purity germanium (HPGe) detectors, whose surface exposure time was carefully limited to minimize the activation of cosmogenic backgrounds. Significant progress has been made towards understanding the observed backgrounds and in data filtering at low energy, enabling tighter limits to be set on searches for rare events. In this talk I will present the current status of the low energy rare event search and report new results.

Speaker: Clint Wiseman (University of Washington)

Slides Wiseman_TAUP2019.pdf

138 Recent advancements of the NEWS-G experiment

NEWS-G (New Experiments With Spheres-Gas) is an innovative experiment aiming to shine a light on the dark matter conundrum with a novel gaseous detector, the spherical proportional counter. It uses light gases, such as hydrogen, helium, and neon, as targets, to expand dark matter searches to the sub-GeV/c${}^{2}$ mass region. First results obtained with neon target by NEWS-G with a 60 cm diameter detector operated at LSM and the 140 cm project at SNOLAB are described in another presentation at this conference. In this talk, I present developments incorporated in this new detector: a) sensor technologies using resistive materials and multi-anode read-out that allow high gain - high pressure operation, b) gas purification techniques to remove contaminants (H${}_{2}$O, O${}_{2}$) and radon impurities, c) reduction of ${}^{210}$Pb induced background through copper electroforming methods, d) utilisation of UV-lasers for detector calibration, detector response monitoring and estimation of gas related fundamental properties. This next experimental phase of NEWS-G will allow searches for low mass dark matter with unprecedented sensitivity.

Speaker: Dr Ioannis Katsioulas (University of Birmingham)

Slides taup_katsioulas_v2.pdf

139 The Future PICO Dark Matter Search Program with Bubble Chambers and Lower Threshold Capability

The PICO collaboration has been developing ever larger detectors for the direct detection of dark matter using the superheated bubble chamber technology. The use of C3F8 has led to world leading results for spin-dependent dark matter interactions on the proton. The next generation detector, PICO 500, will have an order of magnitude larger active mass and significantly reduced backgrounds. In addition, a new understanding of the detector response to electron recoils will allow the detector to be optimized for lower threshold running. The future dark matter search program with the PICO bubble chambers and lower threshold capability will be presented.

Speaker: Dr Tony Noble (Queen's University: For the PICO Collaboration)

Slides TAUP_PICO_Future_Plans_Noble_2019.pptx

140 The DAMIC-M dark matter experiment

The DAMIC-M experiment –— to be installed at the Laboratoire Souterrain de Modane in France — features a kg-size silicon target consisting of ultra low-noise charge-coupled devices (CCDs). DAMIC-M will probe a broad range of low-mass dark matter particles, particularly from the hidden-sector, with sensitivity improvements of several orders of magnitude beyond current experiments. The CCDs' excellent energy and spatial resolutions, low-energy threshold and unique capability to identify surface and bulk radioactive backgrounds has been demonstrated by a 40 g detector deployed at SNOLAB. DAMIC-M CCDs, thanks to a new specialized skipper readout, have unprecedented single electron resolution resulting in a detection threshold as low as 2 ionized electrons. We will review the key components of the experiment, and also present results from the characterization of our first batch of 24 mega-pixel skipper CCDs, the largest ever built.

Speaker: Prof. Paolo Privitera (University of Chicago)

Slides DAMIC-M-TAUP-2019-Privitera-3.pdf

5:30 PM Closed session

DM8: Axions and Axion-Like Dark Matter III

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

141 Search for dark matter in the form of axion-like particles and hidden photons in the XMASS detector

Weakly Interacting Slim particles, such as Axion-like Particles (ALPs) and Hidden Photons (HPs), are candidates of cold DM. ALPs and HPs are experimentally interesting because both bosons are absorbed by materials through an interaction analogous to a photoelectric effect, transferring the energy equivalent to their rest mass to recoil electrons. XMASS is an experiment aiming at direct detection of dark matter, using single-phase liquid-xenon scintillator at the Kamioka Observatory in Japan. With its low background environment, the XMASS detector has a good sensitivity to the electron recoil signals from ALPs and HPs. Analyzing 800 live-days of XMASS data with 327 kg liquid xenon in the fiducial volume, we set the most stringent upper limits on the coupling constant $g_{Ae}$ of ALPs and the parameter for kinetic mixing $\alpha’/\alpha$ of HPs in the mass range from 40 to 120 keV/$c^2$.

Speaker: Dr Kazufumi Sato (ISEE, Nagoya University)

Slides 190910-sato-TAUP2019-HP-draft_v2.pdf

142 A comprehensive approach to axion dark matter search and hadronic EDMs

The Center for Axion and Precision Physics research (CAPP) of the institute for basic science (IBS) of South Korea aims to search for dark matter axions with high sensitivity reaching all the way down to the hadronic axion models. The frequency range is 1 - 10 GHz using several experiments in parallel and high B-field magnets. CAPP has also developed a high frequency capability using the same magnets to be able to cover the 10 - 20 GHz range again with similar sensitivity. The Center is also involved in selective high precision, accelerator based experiments, muon g-2 and COMET, as well as playing a critical role in developing the storage ring proton electric dipole moment experiment. The proton EDM experiment capable of reaching $10^{-29}\, {\it e} \cdot {\rm cm}$ sensitivity, will reach a new physics scale of hundreds of TeV and will improve the sensitivity to $\theta_{\rm QCD}$ by three to four orders of magnitude, greatly probing the Strong-CP problem.

Speaker: Prof. Yannis Semertzidis (IBS and KAIST)

Slides YkS_TAUP_Axion_Dark_Matter_pEDM_2019_0910.pdf

143 Axion Dark Matter Search with Interferometric Gravitational Wave Detectors

Axion dark matter differentiates the phase velocities of the circular-polarized photons. In this work, we present a scheme to measure its phase difference by using a linear optical cavity. We applied this scheme to the Fabry-Perot arm of gravitational wave detectors such as aLIGO, KAGRA, CE, and DECIGO. We found that their potential sensitivities to the axion-photon coupling constant, g_{aγ}, can reach beyond the current limit of CAST with several orders of magnitude, at a wide axion mass range 10^{-16}eV < m < 10^{-9} eV. Our sensitivity can be achieved without loosing any sensitivity to gravitational waves. This work is based on our recent paper [arXiv: 1903.02017].

Speaker: Dr Ippei Obata (ICRR)

Slides TAUP2019.pdf

144 Dark matter axion search experiments using 18T HTS magnet

The presence of dark matter had profound consequences on the evolution of the Universe. The Standard Model does not accommodate a suitable dark matter candidate. Therefore, the existence of dark matter is a crucial phenomenological evidence for physics Beyond the Standard Model. The pressing goal of current and future dark matter experiments is to answer the question of whether dark matter interacts with normal matter other than gravity; i.e. if dark matter is detectable. Among the plethora of dark matter candidate particles, the Weakly Interacting Massive Particles (WIMPs) and the Axions are the most outstanding contender. In this talk, we will present the dark matter axion search projects at the Center for Axions and Precision Physics Research at CAPP/IBS, especially focused on the CAPP18T axion dark matter search experiment which utilizes a 18T High Temperature Superconducting solenoid magnet.

Speaker: Byeongsu Yang (Institue for Basic Science)

Slides 20190906_yang_TAUP_v1_submit.pptx

145 Status and plans for NA64

The NA64 experiment at the CERN North Area searches for dark matter production via both visible and invisible decays of sub-GeV vector mediators, such as the dark photon A’. In a first data taking period from 2016-2018, A’ generation from the reaction e−Z → e−ZA′ and subsequent decays A’→χχ and A’ → e+e− was studied with the help of an active dump set-up using 100 GeV/c electrons. Recently, an extension of the performed searches was proposed using a 150 GeV/c muon beam, available at the M2 beam line at CERN. These measurements would allow for additional coverage of parameter space towards higher A’ masses and would open the possibility for searches for a possible Zµ that would couple only to second and third generation leptons. We will present both the analysis of the available NA64 data as well as future plans for searches with muon and electron beams that are proposed within the “Physics Beyond Colliders” framework at CERN, including optimisation of the M2 optics and integration studies for implementing NA64µ in the EHN2 experimental area.

Speaker: Dr Johannes Bernhard (CERN)

Slides NA64_TAUP2019.pdf NA64_TAUP2019.pptx

DM9: Astrophysical probes of dark matter

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

146 Towards closing the window of primordial black holes as dark matter: The case of large clustering

The idea of dark matter in the form of primordial black holes has seen a recent revival triggered by the LIGO detection of gravitational waves from binary black hole mergers. In this context, it has been argued that a large initial clustering of primordial black holes can help alleviate the strong constraints on this scenario. In this work, we show that, on the contrary, with large initial clustering the problem is exacerbated and constraints on primordial black hole dark matter become overwhelmingly strong.

Speaker: Mr Paul Frederik Depta (DESY)

Slides PBHlimits_taup_2019_FDepta.pdf

147 Observable signatures of dark photons from supernovae

A dark photon is a well-motivated new particle which, as a component of an associated dark sector, could explain dark matter. One strong limit on dark photons arises from excessive cooling of supernovae. We point out that even at couplings where too few dark photons are produced in supernovae to violate the cooling bound, they can be observed directly through their decays. Supernovae produce dark photons which decay to positrons, giving a signal in the 511 keV annihilation line observed by SPI/INTEGRAL. Further, prompt gamma-ray emission by these decaying dark photons gives a signal for gamma-ray telescopes. Existing GRS observations of SN1987a already constrain this, and a future nearby SN could provide a detection. Finally, dark photon decays from extragalactic SN would produce a diffuse flux of gamma rays observable by detectors such as SMM and HEAO-1. Together these observations can probe dark photon couplings several orders of magnitude beyond current constraints for masses of roughly 1 - 100 MeV.

Speaker: William DeRocco (Stanford University)

Slides taup_2019.pdf

148 Detection of cross-correlation between DES Y1 shear and the extra-galactic gamma-ray background: implications for Dark Matter

Dark Matter (DM) Weakly Intercactive Massive Particles (WIMPs) are expected to produce a gamma-ray emission via annihilation; on the other hand this signal should trace the matter distribution being originated from DM structures evolved from primordial perturbations. The anisotropies of the unresolved component of the extra-galactic gamma-ray background (UGRB) hosts valuable information on the faint astrophysical sources and can hide a long-sought DM signal. In order to extract information from this faint emission, a cross-correlation with gravitational tracers of matter in the Universe has been predicted to be a powerful tool. We report the first statistically-significant detection of cross-correlation between the Dark Energy Survey (DES) Y1 cosmic shear catalogue and the gamma-ray sky measured by the Fermi-LAT. Being mostly localized at small angular scales and high gamma-ray energy, the most likely interpretation is that the signal originates from blazar emission. The possibility of a DM contribution at the degree scale will be discussed.

Speaker: Dr Simone Ammazzalorso (University of Turin &amp; INFN)

Slides TAUP2019_DESxFermi_Ammazzalorso.pdf

5:10 PM Closed session

Gravitational Wave #4

149 Prompt and accurate sky localization of gravitational-wave sources

Accurate, precise and prompt sky localization of gravitational-wave sources is essential to the success of multi messenger astronomy. One of the most accurate sky localizations we can obtain is from full signal parameter estimation obtained with the LIGO-Virgo LALInference software [1], done after a quick initial sky localization with the Bayestar software [2]. While more accurate, the improved analysis takes on the order of a day to complete for a binary neutron star event. In that time-scale, an optical counterpart signal has a high chance of being missed. In order to speed up that process, we designed a new automation scheme and improved significantly the speed of LALInference parameter estimation. For the automation, we integrated LALInference parameter estimation with an infrastructure for automatic follow ups on gravitational-wave alerts, GWCelery [3]. Currently, it starts within less than 10 minutes after the detection of gravitational waves, and includes optimised choices for parameter estimation settings. For the acceleration, we formulated a technique to restrict prior ranges of source parameters before parameter estimation utilizing the preliminary information provided by the detection pipelines. We found that the parameter estimation is sped up by an order of magnitude with this technique, delivering an improved sky localization in potentially less than an hour. In this talk, I will explain the detail of the automatic infrastructure and our technique to speed up the parameter estimation, and I will also summarize the current status of the development of the infrastructure for the accurate and precise sky localization. [1]: J. Veitch et al., "Parameter estimation for compact binaries with ground-based gravitational-wave observations using the LALInference software library", Phys. Rev. D 91, no. 4, 042003 (2015). [2]: L. P. Singer and L. R. Price, "Rapid Bayesian position reconstruction for gravitational-wave transients," Phys. Rev. D 93, no. 2, 024013 (2016). [3]: https://git.ligo.org/emfollow/gwcelery .

Speaker: Mr Soichiro Morisaki (The University of Tokyo)

Slides TAUP2019.pdf (Protected)

150 Investigation of the environment influence for the underground and cryogenic gravitational wave detector, KAGRA.

KAGRA is the 2nd generation large gravitational wave detector, which is placed in Japan. There are two characteristic features, underground and cryogenic detector. Toward joining the international network observation, called O3 run, KAGRA must operate with the better sensitivity. For this purpose, we installed the various environmental monitors, such as accelerometer, seismometer, magnetometer, microphone and so on. We will report the investigation of the KAGRA environmental influence to the gravitational wave strain signal. Also, those two features are important technology for the future detectors. We will also investigate the environmental influence toward the future gravitational detectors.

Speaker: Dr Takaaki Yokozawa (Institute for Cosmic Ray Research, University of Tokyo)

Slides TAUP2019_yokozawa_ver2.pdf

151 Detector Characterization for the underground-based gravitational-wave detector, KAGRA

The underground gravitational-wave detector, KAGRA, is rapidly being commissioned and integrated towards the joint observation run with LIGO and VIRGO. The laser-interferometer type of the gravitational-wave detectors are based on very complicated optical systems, with numerous feedback control loops at an extreme high precision. Since the interferometer is so complex, there are many possible states of the operation, with different levels of noise contributions. Furthermore, the interferometer is affected by the environmental perturbations such as earthquakes and tidal waves of the ocean, through various noise coupling mechanisms. The goal of the detector characterization (DetChar) is to understand the behavior of the interferometer, states of the environment, and various noise coupling mechanisms to the gravitational-wave channel. The study includes the software developments as well as instrumental experiments. The obtained insights of the interferometer are crucial both from the following three aspects: (i) Data analysis. For when the gravitational-wave channel is analyzed for the event search, Detchar provides the state information of the interferometer which are based on the study of the interferometer behavior. The gravitational-wave channel data is avoided when the bad state so that the efficient searches can be performed and so to avoid false alerts of the gravitational-wave events. (ii) Instruments. By studying the noise sources and their coupling routes, some of them are identified. When possible, those noises will be mitigated and the interferometer performance will be improved. (iii) Commissioners. DetChar provides software tools also to present the status of the interferometer and environmental information. With such tools, specific plots of the instruments and DetChar results are easily accessible for the commissioners (and anyone in the collaboration) so the noise hunting will be done quicker and more efficiently. Thus, detector characterization will serve as a "brigade" between the instruments and data analysis studies. In this talk, the status of the KAGRA detector characterization towards O3, and the prospects will be presented.

Speaker: Dr Keiko Kokeyama (ICRR, University of Tokyo)

Slides main_kokeyama.pdf

152 Newtonian noise from the underground water

KAGRA is the world first large scale underground gravitational wave telescope and one of the advantages of being built under the ground is to be isolated from gravity gradient fluctuation, or so-called Newtonian noise. According to a well-established theoretical models, the seismic-driven or atmospheric-driven Newtonian noise level in KAGRA is lower than other ground based telescopes, but one concern is that we have underground water flowing violently near the test masses and it may cause Newtonian noise. We would like to present our recent study on water-driven Newtonian noise to show its influence in the sensitivity of KAGRA.

Speaker: Prof. Kentaro Somiya (Tokyo Institute of Technology)

Slides Somiya190910.pptx

153 KAGRA Data Tiers

KAGRA is a laser interferometric gravitational wave detector that is placed underground Kamioka-mine, Gifu, Japan. KAGRA is planning to have observational operation in late 2019. Since the data is obtained in the KAGRA tunnel, it have to be transfered, stored and processed at Off-site facilities where have enough computing environment. We have been constructed KAGRA's data transfer and storage system. We also constructing data distribution Tiers. On the other hand, data sharing of the international network of the gravitational wave detectors with very low latency as like less 10 seconds is important for the event search and follow-up observations. In this talk, we will display an overview of KAGRA's data tiers, low latency data transfer and these constructions.

Speaker: Prof. Nobuyuki Kanda (Graduate School of Science / NITEP, Osaka City University)

Slides TAUP2019_kanda_v4.pdf

154 Overview of KAGRA Data Analysis

KAGRA is planning to start the observation run in 2019. If it is realized, it is done during LIGO's and Virgo's 3rd Observation run. KAGRA data analysis group has been preparing for this observation. Gravitational wave signals are categorized based on the property of signals. Those property include the duration of the signal, predictability of waveforms, and statistical nature (deterministic or stochastic). Data analysis of gravitational waves depends on these property. Now in KAGRA, there are several groups are working for establishing the data analysis system of KAGRA. Those include four gravitational wave search groups (Compact Binary Coalescense, Burst, Continuous Waves, and Stochastic Background). Other groups are Detector Characterization which is working for noise characterization, Calibration group, and Computing and Software group which is managing the infrastructure for computing and software libraries. In this talk, I will present the overview of the current activities of KAGRA data analysis group.

Speaker: Hideyuki Tagoshi (ICRR, The University of Tokyo)

Slides 20190910TAUP2019_Tagoshi_v1.1.pdf

HECR #4

155 Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the ISS

Precision measurements by AMS of the fluxes of cosmic ray positrons, electrons, antiprotons, protons and light nuclei as well as their ratios reveal several unexpected and intriguing features. The presented measurements extend the energy range of the previous observations with much increased precision. The new results show that the positron flux rises from ∼10 GeV above the rate expected from cosmic ray collisions with interstellar gas and at energies ~300 GeV exhibits behavior consistent with a new source of high energy positrons. In the absolute rigidity range ∼60 to ∼500 GV, the antiproton, proton, and positron fluxes are found to have nearly identical rigidity dependence and the electron flux exhibits different rigidity dependence. Below 60 GV, the antiproton-to-proton, antiproton-to-positron, and proton-to-positron flux ratios each reaches a maximum. Particular emphasis is made on new observations of the properties of elementary particles in the rigidity range above 500 GV.

Speaker: Dr Zhicheng TANG (Institute of High Energy Physics, Chinese Academy of Sciences)

Slides taup-ztang.pdf

156 Anisotropy of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the ISS

Analysis of anisotropy of the arrival directions of galactic protons, electrons and positrons has been performed with the Alpha Magnetic Spectrometer on the International Space Station. These results allow to differentiate between point-like and diffuse sources of cosmic rays for the explanation of the observed excess of high energy positrons. The AMS results on the dipole anisotropy are presented along with the discussion of implications of these measurements.

Speaker: Dr Miguel Angel Velasco Frutos (CIEMAT)

Slides MAVelasco_TAUP.pdf

157 New Properties of Primary Cosmic Rays Measured by AMS on ISS

New properties of the primary cosmic rays from Z=1 to Z=16 measured by Alpha Magnetic Spectrometer on ISS will be presented.

Speaker: Dr Valerio Formato (Univesity of Perugia, ITALY)

Slides vformato_-_primaries.pdf

158 New properties of secondary cosmic rays measured by AMS

New properties of secondary cosmic rays Li, Be and B measured by AMS will be discussed.

Speaker: Dr Mercedes Paniccia (Université de Genève)

Slides TAUP2019_-_New_Properties_of_Secondary_Cosmic-Rays_measured_by_AMS__-_M.Paniccia.pdf

159 Cosmic Ray Isotopes measured by AMS

The properties of cosmic ray isotopes of H, He and Li, measured by AMS will be presented.

Speaker: Dr Francesca Giovacchini (CIEMAT. Spain)

Slides FGiovacchiniTAUP2019.pdf

160 Observation of Complex Time Structures in the Cosmic-Ray Electron and Positron Fluxes by the Alpha Magnetic Spectrometer on the ISS

We present high-statistics, precision measurements by AMS of the detailed time and rigidity dependence of the primary cosmic-ray electron, positron, proton and helium fluxes over 79 Bartels rotations from May 2011 to May 2017 in the energy range from 1 to 50 GeV. For the first time, the charge-sign dependent modulation during solar maximum has been investigated in detail by leptons alone. We report the observation of short-term structures on the timescale of months coincident in all the fluxes. These structures are not visible in the positron-to-electron flux ratio. The precision measurements across the solar polarity reversal show that the ratio exhibits a smooth transition over ~800 days from one value to another.

Speaker: Dr Valerio Vagelli (Agenzia Spaziale Italiana - Unità di Ricerca Scientifica)

Slides TAUP2019_Vagelli_AMSelepostime.pdf

Neutrino #10

Convener: Dr Itaru Shimizu (Tohoku University)

161 Status of 48Ca double beta decay search and its future prospect in CANDLES

The observation of neutrino-less double beta decay (0nbb) is considered to be the most practical way to prove the Majorana nature of the neutrino and lepton number violation. CANDLES (CAlcium fluoride for the study of Neutrinos and Dark matters by Low Energy Spectrometer) is the experiment to search for the 0nbb of 48Ca with CaF2 scintillator. The advantage of 48Ca is that it has the highest Q-value (4.3 MeV) among all isotope candidates for 0nbb. It enables us to measure signals with very low background condition. The CANDLES detector is installed at Kamioka underground observatory, Japan and it consists of 96 pure CaF2 crystals (300kg). These crystals are immersed in liquid scintillator as an active shield. We have been taking data for several years. And we have analyzed them with some analytical techniques. In this presentation, we report on the latest result obtained by the data of several hundred days. In addition, we present the strategy for future CANDLES experiment.

Speaker: Mr Konosuke Tetsuno (Osaka University)

Slides TAUP2019_Ver3_Tetsuno.pdf

162 New results from the CUORE experiment

The Cryogenic Underground Observatory for Rare Events (CUORE) is the first bolometric experiment searching for neutrinoless double beta decay (0νββ) that has been able to reach the one-ton scale. The detector, located at the Laboratori Nazionali del Gran Sasso in Italy, consists of an array of 988 TeO2 crystals arranged in a compact cylindrical structure of 19 towers. The construction of the experiment was completed in August 2016 with the installation of all towers in the cryostat. Following a cooldown, diagnostic, and optimization campaign, routine data-taking began in spring 2017. In this talk, we present the updated 0νββ results of CUORE from examining the total available TeO2 exposure. An update of the CUORE background model is also discussed. The detector performance is then reviewed. We finally present an update of the measurement of the 130Te 2νββ half-life.

Speaker: Dr Stefano Pozzi (University of Milano Bicocca and INFN Milano Bicocca)

Slides TAUP19_Pozzi.pdf

163 Final results of the CUPID-0 Phase I experiment

A convincing observation of neutrino-less double beta decay (0$\nu$DBD) relies on the possibility of operating high-energy resolution detectors in background-free conditions. Scintillating cryogenic calorimeters are one of the most promising tools to fulfill the requirements for a next-generation experiment. Several steps have been taken to demonstrate the maturity of this technique, starting form the successful experience of CUPID-0. The CUPID-0 experiment collected 10 kg*y of exposure, running 26 Zn$^{82}$Se crystals during two years of continuous detector operation. The complete rejection of the dominant alpha background was demonstrated, measuring the lowest counting rate in the region of interest for this technique. Furthermore, the most stringent limit on the Se-82 0$\nu$DBD was established. In this contribution we present the final results of CUPID-0 Phase I, including a detailed model of the background and the measurement of the 2$\nu$DBD half-life.

Speaker: Dr Nicola Casali (INFN-Roma1)

Slides TAUP_Cupid0.pdf

164 First results of KamLAND-Zen 800

KamLAND-Zen is a neutrinoless double beta decay ($0\nu\beta\beta$) search experiment using xenon 136 and ultra-low background environment of KamLAND (Kamioka Liquid scintillator Anti-Neutrino Detector). The previous project KamLAND-Zen 400 set the most strict lower limit on the half-life of $0\nu\beta\beta$ in $^{\rm 136}$Xe, and it was terminated in 2015. KamLAND-Zen collaboration has prepared the upgrade project KamLAND-Zen 800 with increased xenon amount and cleaner container (mini-balloon) for xenon loaded liquid scintillator. The new mini-balloon production was started in May 2017 and KamLAND-Zen 800 data acquisition was started in January 2019. In this presentation, we will explain the KamLAND-Zen 800 project and report the detector condition, data quality, the first analysis results, and the prospects. We also mention the next project KamLAND2-Zen and related research and developments.

Speaker: Dr Yoshihito Gando (Research Center for Neutrino Science, Tohoku University)

Slides TAUP2019YoshihitoGando_v5.0.pdf

165 A Bayesian Approach to Neutrinoless Double Beta Decay Analysis in KamLAND-ZEN

Neutrinoless Double Beta Decay(0νββ) is one of the major research interests in neutrino physics. The discovery of 0νββ would answer persistent puzzles in the standard model. KamLAND-ZEN experiment is one of the leading efforts in the search of 0νββ. The data is taken from 380kg of Xe136 isotopes, and analyzed by a Frequentisit likelihood analysis to set limit on 0νββ lifetime. In addition to the well-established Frequentist approach, we conduct a Bayesian analysis with a Markov Chain Monte Carlo(MCMC). The Bayesian approach allows us to use modern statistical tools and serves as a cross check of the Frequentist analysis; furthermore, we provide the possibility of adding a self-developed machine learning event classification algorithm to increase sensitivity. In this talk, we will present the analysis framework and result of this Bayesian approach, as well as the inclusion of the machine learning result.

Speaker: Mr Aobo Li (Boston University)

Slides taup_final_aobo_v7.pdf

Neutrino #11

Convener: Dr Itaru Shimizu (Tohoku University)

166 Developing a long time supernova simulation framework

Massive stars cause huge explosions called core collapse supernovae(CCSNe) at the end of their evolution. A CCSNe is one of the strongest explosion, which releases 10 percent of the star's mass of the solar in some 10's of seconds. Most of this energy is released as neutrinos.The four fundamental interactions of nature are involved in CCSNe, and CCSNe are complex and difficult to model theoretically. Neutrinos carry information about the stellar core, so neutrino detectors around the world are waiting for a CCSNe nearby the earth. The Super-kamiokande(SK) water Cherenkove detector is also continuously monitoring for CCSNe. If a CCSN happens in our galaxy, SK can detecte about 10,000 events over more than 10 seconds. However, most theoretical simulations concentrate on only the first 1 second, which determines whether the explosion successes. Therefore, we can not compare a theory and observation when a galactic supernova is detected. For galactic supernova in near future, a long time simulation is needed. An integrated framework is being developed, which simulates supernova neutrino in one dimension from a core collapse to detection at SK.In the present study, we consider three models which lead to different neutron star models and have simulated the neutrino emission up to 20 seconds. These model have already been simulated up to 20 seconds. In this report, the difference in expected neutrino signals at SK for these models will be shown.

Speaker: Mr Masamitsu Mori (Kyoto University)

Slides taup2019_mori.pptx

167 Observing Supernova Neutrino Light Curves with Super-Kamiokande: Expected Event Number over Ten Seconds

Supernova neutrinos are crucially important to probe the final phases of massive star evolution. As is well known from observations of SN1987A, neutrinos provide information on the physical conditions responsible for neutron star formation and on the supernova explosion mechanism. However, there is still no complete understanding of the long-term evolution of neutrino emission in supernova explosions, although there are a number of modern simulations of neutrino radiation hydrodynamics, which study neutrino emission at times less than one second after the bounce. In the present work we systematically calculate the number of neutrinos that can be observed in Super-Kamiokande over periods longer than ten seconds using the database of Nakazato et al. (2013) anticipating that neutrinos from a Galactic supernova can be detected for several tens of seconds. We find that for a supernova at a distance of 10 kpc, neutrinos remain observable for longer than 30 s for a low-mass neutron star ($1.20M_\odot$ gravitational mass) and even longer than 100 s for a high-mass neutron star ($2.05M_\odot$). These scenarios are much longer than the observations of SN1987A and longer than the duration of existing numerical simulations. We propose a new analysis method based on the cumulative neutrino event distribution as a function of reverse time from the last observed event, as a useful probe of the neutron star mass. Our result demonstrates the importance of complete modeling of neutrino light curves in order to extract physical quantities essential for understanding supernova explosion mechanisms, such as the mass and radius of the resulting neutron star.

Speaker: Dr Yudai Suwa (Kyoto Sangyo Universiy)

Slides 337.pdf

168 Pre-SN neutrino emission from massive stars and their detection

Pre-supernova (pre-SN) neutrinos are emitted from a core of massive stars, which are supposed to be progenitors of core-collapse supernovae (CCSNe). Although it was seemed to be difficult to detect pre-SN neutrinos because of their low energy, detection of pre-SN neutrinos comes into view owing to the recent development of detectors. We believe that future detection of pre-SN neutrinos will give us a big impact as much as the historical neutrino events at SN1987A. In this talk, we focus on the importance of pre-SN neutrino detection in two points of view: evidence for the theory of stellar evolution and SN alarm. In the former, we show the luminosities and spectra of neutrinos for two types of progenitors: FeCCSN- and ECSN-progenitors, and discuss their distinguishability from observations in all flavor. In the latter, we describe the predictions of SN alarms at current and planned neutrino detectors based on the time profiles of pre-SN neutrinos. This is closely related with multi-messenger studies and the SNEWS project, in which a prompt alert of the occurrence of SN event at our Galaxy is provided for the astronomical community. We also mention a relation between pre-SN neutrinos and SN alarm.

Speaker: Ms Chinami Kato (Tohoku univeristy)

Slides TAUP2019_kato.pdf

169 Supernova Model Discrimination with Hyper-Kamiokande

This talk presents results of a study using Hyper-Kamiokande (HK) to distinguish different supernova models. With $\mathcal{O}(10^5)$ events expected in HK from a supernova near the galactic centre, such a model comparison will allow us to go beyond a simple determination of parameters of the neutrino flux, and to verify assumptions going into current supernova models.

Speaker: Jost Migenda (University of Sheffield)

Slides 20190910_SN_model_discrimination.pdf

170 38 years of galactic observations in searching for neutrino bursts from core collapse supernovae with the Baksan Underground Scintillation Telescope

The core collapse of a massive star in the Milky Way will produce a neutrino burst, which will be detected by the Baksan Underground Scintillation Telescope (BUST). The stable and enough low background at the BUST is a clear asset for searching for neutrino bursts. Now two parts of the facility (with the total mass of 242 tons) are used as independent coinciding detectors. Such approach allows us to increase dependability detection of the neutrino signal and the radius of sensitivity of the BUST. The facility has the potential to see a supernova in the Galaxy independently from other detectors. No burst candidate for the core collapse has been detected during the observation period of June 30, 1980, to December 31, 2018. The actual observation time is 33.02 years. This is the longest observation time of our Galaxy with neutrinos at the same facility. An upper bound on the mean frequency of gravitational collapses in the Galaxy is ≤ 7.0 per century (at 90% C.L.).

Speaker: Prof. Valeriy Petkov (Institute for Nuclear Research of the Russian Academy of Sciences)

Slides Petkov_Collaps_TAUP-19.pdf

Neutrino #12

Convener: Dr Itaru Shimizu (Tohoku University)

171 Updated geoneutrino measurement with Borexino

There are still several unanswered fundamental questions concerning our planet and in particular, about the deep Earth, from where we lack direct samples. Today, thanks to the progress in neutrino-detection techniques, geoneutrinos, antineutrinos from the decays of long-lived radioactive elements inside the Earth, can be exploited as a new and unique tool to study our planet. Borexino has presented its latest geoneutrino measurement in 2015. Thanks to both more acquired data, as well as to improved analysis techniques in an enlarged fiducial volume, we provide an updated measurement with significantly improved precision. The talk will describe the key elements of the updated analysis and will present the measured geoneutrino signal. Geological interpretation and significance of the new result will be discussed, as for example in terms of the corresponding radiogenic heat, geoneutrino signal from the Earth’s mantle or the limit to the hypothetical georeactor. This talk is presented in the name of the Borexino collaboration.

Speaker: Prof. Livia Ludhova (Forschungszentrum Juelich, IKP-2)

Slides LudhovaGeonuBorexinoTAUP2019.pdf

172 Latest result of solar neutrino analysis in Super-Kamiokande

Super-Kamiokande (SK), a 50 kton water Cherenkov detector in Japan, is observing neutrinos and searching for proton decay and neutrino produced by dark matter. In solar neutrino analysis, 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. The installation of new front-end electronics in 2008 marks the beginning of the 4th phase of SK (SK-IV). On 2018 May, we finished taking data of SK-IV whose live time is about 3000 days and started the refurbishment work in order to clean the inside of the detector and to seal the water tank to prevent water tank toward SK-Gd. In this presentation, we overview the latest solar neutrino results in SK-IV, for example, the precise measurement of 8B solar neutrino flux, its energy spectrum and oscillation parameters. In addition, we discuss the future prospect of the new phase of SK-V.

Speaker: Dr Yuuki Nakano (Kobe university)

Slides taup_nakano_upload.pdf

173 Jinping Neutrino Experiment: a Status Report

A large liquid scintillator detector is being planed and actively developed in China JinPing underground laboratory. We envision a 5kt detector at 7000 w.m.e. overburden to target terrestrial, solar and supernovae relic neutrinos. A 1t prototype detector has been installed onsite in 2017. Liquid scintillator performance, radioactive and cosmogenic backgrounds, simulation and analysis pipelines have been carefully investigated. We report status of the Jinping Neutrino Experiment project and milestones of R&D studies.

Speaker: Prof. Benda Xu (Tsinghua University)

Slides Neutrino-20190910-BendaXu-r1.pdf

174 Astrophysical neutrinos at Hyper-Kamiokande

Hyper-Kamiokande (Hyper-K) is a proposed next generation neutrino experiment, aiming at the measurement which starts at 2027. Hyper-K project includes a high intensity accelerator neutrino beamline at J-PARC and one or two far detectors. Each far detector will provide the fiducial volume of 0.19 Mt ultra-pure water and water Cherenkov detection, with its cylindrical water tanks surrounded with newly developed photo-sensors. Due to its world-largest volume, superior performance of the new photodetector and the location at deep underground, Hyper-K will also have great capability for neutrino astrophysics and push back the frontiers. In this presentation, the Hyper-K’s detector performance for MeV neutrinos will be shown. Then the issues for neutrino astrophysics and our reach will be discussed, i.e., for solar neutrino, supernova burst neutrino and supernova relic neutrino observations.

Speaker: Dr Takatomi Yano (ICRR, U-Tokyo)

Slides TAUP2019_v3.pdf

New Technology #2

175 22Ne(p,gamma)23Na cross section measurement at astrophysical energies.

Because of a large number of uncertain resonances in the Gamow window, the 22Ne(p,gamma)23Na reaction rate was the most uncertain in the NeNa cycle. Recently, a new direct study of the 22Ne(p,gamma)23Na reaction has been performed at the Laboratory for Underground Nuclear Astrophysics (LUNA). A windowless gas target and two complementary setups have been used, to obtain both high resolution and high efficiency measurements. The new resonances at 156.2, 189.5 and 259.7 keV have been discovered and their decay scheme has been determined. The tentative resonances at 71 and 105 keV have not been observed and improved upper limits have been put on their strength. Moreover, the high-efficiency setup allowed the measurement of the non-resonant cross section at unprecedented low energies. The thermonuclear reaction rate based on the new measurements has been evaluated.

Speaker: Dr Federico Ferraro (University of Genoa)

Slides TAUP_2019_Ferraro.pdf

176 Search for non-Newtonian gravity with optically-levitated microspheres

The universal law of gravity has undergone stringent tests for a long time over a significant range of length scale, from an atomic scale to a planetary scale. Of particular interest is the short distance regime, where modifications to Newtonian gravity may arise from axion-like particles and extra dimensions. We have constructed an ultra-sensitive force sensor based on optically-levitated microspheres with a force sensitivity of $\sim10^{-17}$ N/$\sqrt{\rm Hz}$ for the purposed of investigating non-Newtonian forces in the 1-100 $\mu$m range. Microspheres interact with a variable-density attractor mass made by alternating silicon and gold segments with periodicity of $\sim 50$ $\mu$m. The attractor can be located as close as $\sim10$ $\mu$m to a microsphere. We report on the characterization of this system, its sensitivity, and some preliminary results. Further technological developments to reduce background are expected to provide orders of magnitude improvement in the sensitivity, going beyond current constraints on non-Newtonian interactions.

Speaker: Dr Akio Kawasaki (Stanford University)

Slides 2019TAUPRev2.pptx

177 Front End Electronics Module Design for the Schwarzschild-Couder Telescope (SCT) Camera

The SCT telescope has been proposed as a medium-sized telescope for the Cherenkov Telescope Array. One of the major upgrades is the design of the new Front End Electronics Module (FEEM). The new FEEMs aim to read-out and digitize the SiPM pre-amplified signals down to the single photoelectron (phe). This phe signal is assumed equivalent to a signal with 2 mV peak amplitude and 500 MHz maximum bandwidth. The FEEM should have a linear response up to 2 V for a required dynamic range of 1000 phe. A FEEM noise equivalent of 0.5 phe - 1 mV of RMS noise - is an acceptable value. Due to the severe mechanical constraints, and to have a very compact electronics and low noise performance, the FEEM consists of two stacked-up submodules, one dedicated to the generation of the power supplies and the other one to house the FPGA, which reads out and sends digitized data to the main backplane. An FEEM is capable of digitizing 64 analog channels with a sampling frequency of 1 GSamples/s.

Speaker: Dr Massimiliano Bitossi (National Institute for Nuclear Physics - Pisa Section)

Slides TAUP2019_FEEM_MBitossi190822.pptx

178 A binned likelihood for stochastic models

Metrics of model goodness-of-fit, model comparison, and model parameter estimation are the main categories of statistical problems in science. Bayesian and frequentist methods that address these questions often rely on a likelihood function, which is the key ingredient in order to assess the plausibility of model parameters given observed data. In some complex systems or experimental setups, predicting the outcome of a model cannot be done analytically, and Monte Carlo techniques are used. In this paper, we present a new analytic likelihood that takes into account Monte Carlo uncertainties, appropriate for use in the large and small sample size limits. Our formulation performs better than semi-analytic methods, prevents strong claims on biased statements, and provides improved coverage properties compared to available methods.

Speaker: Austin Schneider (University of Wisconsin Madison)

Slides TAUP2019_Schneider_Likelihood.pdf

Wednesday, September 11

179 Direct dark matter search

Speaker: Dr Masaki Yamashita (ICRR Univ. of Tokyo)

Slides PlenaryV_yamashita.pdf

180 New ideas in conventional detectors

Speaker: Dr Thomas Shutt (SLAC, Stanford)

Slides Web_PlENARY_V_Shutt.pdf

181 Small scale direct dark matter search experiment

Speaker: Dr Susana Cebrian (Zaragoza)

Slides Web_PLENARY_V_CEBRIAN.pdf

10:30 AM Coffee break

182 Dark matter axion search experiments

Speaker: Dr Gray Rybka (Washington Univ.)

Slides WEB_PlENARY_VI_rybka_TAUP.pdf

183 Dark matter local density determination based on recent observations

Speaker: Dr Pablo Fernández de Salas (OKC (Stockholm University))

Slides Web_PLENARY_VI_PABLO_FERNANDEZ_DE_SALAS.pdf

184 Dark matter search in accelerators

Speaker: Dr Priscilla Pani (DESY)

Slides Web_PLENARY_VI_PANI.pdf

Cosmology #1

Convener: Prof. Masahiro Kawasaki (ICRR, University of Tokyo)

185 Results of gravitational lensing and primordial gravitational waves from the POLARBEAR experiment

POLARBEAR is a cosmic microwave background radiation (CMB) polarization experiment located at the Atacama desert in Chile. The science goals of the POLARBEAR experiment are to characterize the B-mode signal from gravitational lensing, as well as to search for the B-mode signal created by primordial gravitational waves (PGWs). POLARBEAR started observations in 2012, and has published a series of results from its first and second seasons of observations, including the first measurement of a non-zero B-mode angular auto-power spectrum at sub-degree scales where the dominant signal is gravitational lensing of the CMB. In 2016, we installed a continuously rotating half wave plate (HWP) at the focus of the primary mirror to search PWGs with demonstrating control of low frequency noise. In this talk, we present the first measurement of cross-correlation between the lensing potential, reconstructed from CMB polarization data by POLARBEAR, and the cosmic shear field from galaxy shapes by the Subaru Hyper Suprime-Cam (HSC) survey. We also present the status of the measurement of large angular scale B-mode signal induced by PGWs with the HWP.

Speaker: Yuji Chinone (University of California, Berkeley)

Slides POLARBEAR-HSC-HATLAS_TAUP2019_on_2019-09-11_chinoney.pptx.pdf

186 Particle Physics with the Cosmic Microwave Background with SPT-3G

The Cosmic Microwave Background (CMB) encodes information about the content and evolution of the universe. The presence of light, non-interacting particles impacts the expansion history of the early universe, which alters the temperature and polarization anisotropies of the CMB. In this way, current measurements of the CMB place interesting constraints on the neutrino energy density and mass, and as well as the abundance of other possible light relativistic particle species. I present the status of an on-going 1500 sq. deg. survey with the SPT-3G receiver, a new mm-wavelength camera on the 10-m diameter South Pole Telescope (SPT). The SPT-3G camera consists of 16,000 superconducting transition edge sensors, a 10x increase over the previous generation camera, which allows it to map the CMB with an unprecedented combination of sensitivity and angular resolution. I show early results from the SPT-3G survey, and highlight projected constraints on the abundance of sterile neutrinos and the sum of the neutrino masses, which could help determine the neutrino mass hierarchy.

Speaker: Ms Jessica Avva (University of California, Berkeley)

Slides Avva_Presentation_Toyama_.pdf

187 Searching gamma-rays and dark matter from galaxy clusters at low redshift

We report the identification of a positive cross-correlation signal between the unresolved $\gamma$-ray emission, measured by the Fermi Large Area Telescope, and four different galaxy cluster catalogues: WHY18 (infrared galaxies), SDSSDR9 (optical galaxies), MCXCsub and HIFLUGCS (X-ray galaxies). When confronted with a model that traces the Large Scale Structure contribution to the unresolved extragalactic $\gamma$-ray emission in terms of Active Galactic Nuclei, the analysis rejects the no-signal hypothesis with a significance larger than $2\sigma$ for WHY18, SDSSDR9 and HIFLUGCS, raised to $4\sigma$ for the MCXCsub catalog. For the most significant case of MCXCsub, we also obtain that a sizeable fraction of the correlation signal seems to originate from the more extended objects, thus intriguingly suggesting a possible contribution from the Intra Cluster Medium (ICM). Current statistics are nevertheless unable to firmly assess an ICM origin of this excess. The same cluster catalogues are also used to detect bounds on the mass of the Dark Matter within the WIMP paradigm. The analysis has been performed by introducing an accurate estimation of the power spectrum covariance matrix, built with mock realisations of the gamma and galaxy cluster maps, which allows a precise statistical evaluation of the significance of the measured angular power spectrum.

Speaker: Dr Manuel Colavincenzo (University of Turin)

Slides Colavincenzo.pdf

DM11: Self-interacting dark matter and light mediators

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

188 New avenues for Self-Interacting Dark Matter

Self-interacting dark matter is a well-motivated solution to the core-vs-cusp and the too-big-to-fail problems of the ΛCDM model. In this context, a light particle mediating the self-interactions is typically invoked in order to achieve velocity-dependent effects. In this talk, I will argue that a light mediator is not the only possible way to do that. In particular, I will discuss two new ideas: dark matter scenarios with self-heating as well as dark matter resonant scattering. Based on: Phys.Rev.Lett. 122 (2019) no.7, 071103 JCAP 1807 (2018) no.07, 013

Speaker: Dr Camilo Alfredo Garcia Cely (DESY)

Slides TAUP_CamiloGarciaCely.pdf

189 Decaying warm dark matter and structure formation

We examine the cosmology of warm dark matter (WDM), both stable and decaying, from the point of view of structure formation. We compare the matter power spectrum associated to WDM masses of 1.5 keV and 0.158 keV, with that expected for the stable cold dark matter ΛCDM≡SCDM paradigm, taken as our reference model. We scrutinize the effects associated to the warm nature of dark matter, as well as the fact that it decays. The decaying warm dark matter (DWDM) scenario is well-motivated, emerging in a broad class of particle physics theories where neutrino masses arise from the spontaneous breaking of a continuous global lepton number symmetry. The majoron arises as a Nambu-Goldstone boson, and picks up a mass from gravitational effects, that explicitly violate global symmetries. The majoron necessarily decays to neutrinos, with an amplitude proportional to their tiny mass, which typically gives it cosmologically long lifetimes. Using N-body simulations we show that our DWDM picture leads to a viable alternative to the ΛCDM scenario, with predictions that can differ substantially on small scales. arXiv:1803.05650

Speaker: Prof. Kingman Cheung (National Tsing Hua University)

Slides majoron-DM-taup.pdf

190 BBN constraints on MeV-scale dark sectors

Meta-stable dark sector particles decaying into electrons or photons may non-trivially change the Hubble rate, lead to entropy injection into the thermal bath of Standard Model particles and may also photodisintegrate light nuclei formed in the early universe. We study generic constraints from Big Bang Nucleosynthesis on such a setup, with a particular emphasis on MeV-scale particles which are neither fully relativistic nor non-relativistic during all times relevant for Big Bang Nucleosynthesis. These constraints turn out to be very relevant for a number of well-studied models, e.g. in the context of self-interacting dark matter with light mediators. We then further apply our calculations to the case of MeV-scale dark matter annihilating into electromagnetic radiation. We show that, for p-wave suppressed annihilations, these constraints turn out to be significantly stronger than the ones from CMB observations, and are even competitive with the strongest bounds from other indirect searches.

Speaker: Mr Marco Hufnagel (DESY)

Slides Marco_Hufnagel_TAUP_2019.pdf

191 Hidden Monopole Dark Matter via Axion Portal and its Implications for Direct Search and Beam-Dump Experiments

We study the monopole dark matter (MDM) emerging from a spontaneous breakdown of non- abelian gauge symmetry in the hidden sector. We assume that this hidden MDM was produced as a topological defect during a second-order phase transition in the early universe, and its stability is guaranteed by the topological nature. In particular, we introduce an axion-like particle (ALP), which mediates the interactions between the hidden MDM and nucleus, and the configuration of the ALP field is affected by the Witten effect in the presence of the hidden monopole. We then compute the spin-dependent elastic cross-section of the hidden MDM scattering off a nucleon and compare it to the direct search experiments. To induce the Witten effect, the ALP has to couple to the hidden photons. As a consequence, the bounds coming from the beam-dump experiments and B meson decays for the ALP decay constant are changed. By considering those constraints, we find that the room for the hidden MDM is still large with a benchmark point which can satisfy the relic abundance of dark matter while solving the small-scale problems in galaxy formation.

Speaker: Mr Shu-Yu Ho (Tohoku University)

Slides 11_09_2019_TAUP.pdf

DM12: Annual Modulation

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

192 PICOLON dark matter search

PICOLON (Pure Inorganic Crystal Observatory for LOw-energy Neutr(al)ino) aims to investigate rare events in the field of astroparticle physics, for example, dark matter and double beta decay. The dark matter problem is one of the most important subjects in cosmology and particle physics. Although there are many evidences for the existence of the dark matter, no significant signal has been observed by direct search, except for DAMA/LIBRA experiment. We have been developed highly radiopure NaI(Tl) scintillator to investigate the validity of the annual modulating signal reported by DAMA/LIBRA experiment. An extremely highly pure NaI(Tl) crystal is indispensable for finding significant signal by dark matter. The origins of the serious background are beta rays and gamma rays from $^{210}$Pb and $^{40}$K in the NaI(Tl) crystal. Recently, COSINE group developed a low background NaI(Tl) system. However, they also reported a significant annual modulating signal, their crystal contains a few mBq/kg of $^{210}$Pb. Optimization method to reduce the radioactive contamination, the present status of high sensitivity measurement for dark matter search will be reported.

Speaker: Prof. Ken-Ichi Fushimi (Tokushima University)

Slides Fushimi_PICOLON.pptx

193 Status of COSINE-100

The DAMA/LIBRA collaboration has claimed that an annual modulation signal which is consistent with signal induced by the dark matter interactions is observed by the NaI(Tl) crystal detector. In order to test the DAMA/LIBRA collaboration’s claim, the COSINE experiment searches for interactions of Weakly Interacting Massive Particles (WIMPs) using the same target material. The COSINE-100 detector has been operating since September of 2016 in the 700-m-deep Yangyang underground laboratory. First annual modulation analysis based on the 2-keV energy threshold has been completed and several other analyses are in progress. In addition, studies for the 1-keV threshold have been on-going and analyses based on this threshold is underway. In this presentation, we report the detector design, performance, and recent results of COSINE-100 as well as plans for the next phase, COSINE-200.

Speaker: Dr Young Ju Ko (Istitute for Basic Science)

Slides 190911_yjko_COSINE_TAUP.pdf

194 Dark Matter Searches with the COSINE-100 Experiment

COSINE-100 is a direct dark matter detection experiment that aims to test DAMA/LIBRA’s claim of dark matter discovery using 106 kg of low-background NaI(Tl) detectors submerged in a 2-tonne liquid scintillator veto. The physics run of the experiment began in September 2016, and a 3.5 count/kg/day/keV background level within the 2-6 keV region of interest has been achieved. Several physics analyses, including WIMP searches and an annual modulation search, have been performed using a 2 keV energy threshold. Recently, this threshold has been lowered to 1 keV. In this talk, we describe the method used to lower the threshold to 1 keV and recent results with this lowered threshold.

Speaker: Mr Govinda Adhikari (Sejong University)

Slides TAUP_COSINE_govinda.pdf

195 Results on dark matter annual modulation from ANAIS-112 experiment

DAMA/LIBRA observation of an annual modulation in the detection rate compatible with that expected for dark matter is one of the most puzzling results in the field. ANAIS-112 experiment, using 112.5 kg of NaI(Tl) as target, is taking data at the Canfranc Underground Laboratory in Spain since August 2017 aiming at testing this result using the same target and technique. Preliminary results corresponding to 1.5 years are compatible with the absence of modulation and in some tension with DAMA/LIBRA results. These results support our goal of reaching a 3σ sensitivity to the DAMA/LIBRA result with 5 years of data. ANAIS-112 data taking is progressing smoothly, and the second year will be completed by August 2019. In the talk, we will describe ANAIS-112 experimental set-up, and we will present updated performance and results of the experiment.

Speaker: Dr María Luisa SARSA (Universidad de Zaragoza)

Slides MLSarsa_ANAIS112results_190911_f.pdf

196 Is a WIMP explanation of the DAMA modulation effect still viable?

Even though there exists cosmological evidence of dark matter (DM) its terrestrial signal has not been observed yet. With no concrete hints of DM from any high energy physics experiment, a bottom-up approach is needed in the analysis of direct detection data. Specifically, the DAMA modulation effect provides a useful benchmark to test such strategies. For instance, we show that analyzing the data in terms of the most general non-relativistic Galilean invariant WIMP-nucleon interaction and/or following a halo-independent approach opens up new possibilities. In particular, we show that the WIMP scenario of proton-philic spin-dependent inelastic Dark Matter (pSIDM) can still provide a viable explanation of the observed DAMA effect in compliance with the constraints from other experiments. We also show that, although the COSINE-100 collaboration has recently tested the DAMA effect using the same target material, for the time being, the comparison between DAMA and COSINE-100 still depends on the particle–physics model.

Speaker: Dr GAURAV KUMAR TOMAR (SOGANG UNIVERSITY)

Slides dd_sensitivity.pdf

HECR #5

197 Latest results of the Pierre Auger Observatory

The Pierre Auger Observatory, in Argentina, has been detecting for more than 15 years ultra-high energy cosmic rays with unprecedented statistics and data quality. Cosmic rays showers above $10^{17}$ eV are accurately measured with a large array of surface detectors covering 3000 km2 and fluorescence telescopes. The operation of a denser sub-array with enhanced triggers has extended the sensitivity of the Surface Detector to lower energies, allowing to measure the spectrum down to 1017.0eV . The most updated analysis concerning the spectrum, anisotropies and mass composition on more than 3 decades in energy will be presented , as well as the stringent limits on photons and neutrinos fluxes. To enlighten these results with a more precise knowledge of the mass composition , the Auger Prime project has been designed and is currently being deployed. The scientific prospects and technical choices will be addressed.

Speaker: Mrs Isabelle Lhenry-Yvon (Institut de Physique Nucléaire d'Orsay, IN2P3/CNRS)

Slides TAUPTOYAMA_LHENRY.pdf

198 Telescope Array: Latest Results and Expansion Plans

The Telescope Array (TA) is an ultra-high energy cosmic ray detector, the largest in the Northern Hemisphere, sensitive to cosmic rays with energies from below 1 PeV to above 100 EeV. The main detector is a hybrid detector consisting of an array of 507 surface detectors covering 700 km$^2$ overlooked by three fluorescence telescope detector stations. The energy range has been extended at the low end by the TA Low Energy (TALE) extension consisting of fluorescence detector stations with higher elevation viewing angle and an infill array of surface detectors. At the lowest energies, around 1 PeV, the TALE fluorescence telescopes operate as imaging air Cherenkov telescopes and work in hybrid with the Non-Imaging Cherenkov (NICHE) array for hybrid Cherenkov observation. TA is also being extended at the highest energies by increasing the covered area by a factor of four in the TAx4 project. In this presentation, we will present the latest cosmic ray spectrum results from TA and TALE, nuclear composition results from TA, both hybrid and stereo, and the latest anisotropy results, including the TA hotspot. We will present the deployment status and commissioning plans from both NICHE and TAx4.

Speaker: Prof. Douglas Bergman (University of Utah)

Slides TA_Results_Plans.pdf

199 Telescope Array search for EeV photons

We present the results of a search for diffuse photons with energies higher than 1 EeV based on Telescope Array surface detector data and a novel neural network event analysis technique. The results of a search for point sources of photons for all directions in the Northern hemisphere and a search for several target source classes are also presented.

Speaker: Dr Yana Zhezher (ICRR, University of Tokyo)

Slides TAUP_Zhezher.pdf

200 Current status and future prospects of the CRAFFT project for the next generation UHECR observatory

The key to understand the origin of the Ultra High Energy Cosmic Ray (UHECR) is higher statistics. One of the concepts to realize the future huge observation is an array of low cost fluorescence telescopes. The fluorescence telescope can measure not only the arrival direction and energy spectrum but also the mass composition which is the important information to understand the UHECR. In order to construct the next generation UHECR observatory, we are developing the Cosmic Ray Air Fluorescence Fresnel lens Telescope (CRAFFT) which uses a Fresnel lens and a few PMTs to reduce the detector cost, and works as stand alone to reduce the maintenance cost. We have constructed four prototype detectors consists of 1.4m$^{2}$ Fresnel lens and an 8 inch PMT at Telescope Array (TA) site, and succeeded to observe the UHECR induced air showers synchronized with the TA detector. The configuration and performance of the CRAFFT detector, result of the test observation and future prospects will be discussed.

Speaker: Dr Daisuke Ikeda (Earthquake Research Institute, University of Tokyo)

Slides crafft_taup2019_ikeda_v2.pdf

201 Extreme Energy Events: an extended multi purpose cosmic ray observatory

EEE is an extended cosmic ray observatory, composed by 59 MRPC-based tracking telescopes, spread over more than 10 degrees in latitude and longitude. Several sites host two or more telescopes in the same town, as local clusters, capable of detecting high energy cosmic showers. The relative distances between the 12 existing clusters range between 86 and 1200 km, allowing the search for rare long distance correlations between cosmic showers. On the other side each EEE telescope is capable of measuring the flux of secondary particles, opening to the study of low energy phenomena such as solar activity and Forbush decreases. The EEE observatory is aiming also to investigate the relation between the cosmic ray flux and the environmental parameters on Earth. During summer 2018 a first measurement campaign was performed by the PolarQuest expedition to the Svalbard islands; a sailboat was equipped with a SiPM-readout scintillator-based detector with the purpose of mapping the low energy cosmic ray flux up to 82 degrees in latitude. The EEE is undergoing a continuous extension and upgrade program, in order to maximize the time exposure and optimize the detection efficiency and the tuning of the stations. New trigger/GPS boards, a set of 42 improved chambers with 250 micron gas gaps and new gas mixtures studies are among the several ongoing activities for enhancing the discovery capabilities of the experiment. The presentation will give and overview of the scientific results as well as of the upgrade activities and technological improvements focused on maximizing the EEE observatory discovery potential.

Speaker: Dr Ivan Gnesi (Fermi Center &amp; INFN LNF Cosenza)

Slides EEE_IG_TAUP2019_.pdf

Neutrino #13

Convener: Dr Itaru Shimizu (Tohoku University)

202 Leptonic CP Violation and the Baryon Asymmetry of the Universe

The phenomenology of 3-neutrino mixing, the current status of our knowledge about the 3-neutrino mixing parameters, including the absolute neutrino mass scale, and of the Dirac and Majorana CP violation in the lepton sector, are summarised. The seesaw mechanism of neutrino mass generation and the related leptogenesis scenario of generation of the baryon asymmetry of the Universe are briefly discussed. The results showing that the CP violation necessary for the generation of the baryon asymmetry of the Universe in leptogenesis can be due exclusively to the Dirac and/or Majorana CP-violating phase(s) in the neutrino mixing matrix $U$ are reviewed.

Speaker: Prof. Serguey Petcov (SISSA/INFN, Trieste, Italy, and Kavli IPMU, Univ. of Tokyo, Japan)

Slides PetcovTAUP110919.pdf

203 Recent T2K Neutrino Oscillation Results

T2K is a long baseline neutrino experiment producing a beam of muon neutrinos at the Japan Particle Accelerator Research Centre on the East coast of Japan and measuring their oscillated state 295 km away at the Super Kamiokande detector. Since 2016 T2K has doubled its data in both neutrino and antineutrino beam modes. Coupled with improvements in analysis techniques this has enabled the experiment to make world leading measurements of the PMNS oscillation parameters \Delta_m^{2}_{32}, sin^2(\theta_{23}) and the CP violating phase \delta_{CP}. In particular the CP conserving values of \delta_{CP} now appear to be disfavoured at the 95\% CL and there are regions of parameter space excluded at the 99.7\% CL. This talk will describe these results and the analysis improvements that have enabled them.

Speaker: Mr Artur Sztuc (Imperial College London)

Slides sztuc_TAUP2019_T2Kresults_110919.pdf

204 Neutrino-Nucleus Interaction Cross-Section Measurements at T2K

A detailed understanding of neutrino(ν)-nucleus interactions is essential for the precise measurement of neutrino oscillations at long baseline experiments, such as T2K. The T2K ND complex, designed to constrain the T2K flux and cross section models, also provides a complementary program of neutrino interaction cross-section measurements. Given the neutrino energy range of the T2K flux, the T2K near detector is in a unique position to make precision measurements of CC0pi processes. Combining multiple CC0pi samples into a single analysis produces relatively high-precision results that can validate new cross-section models and resolve modelling ambiguities. This strategy, which is vital for the future of the field, and recent results will be presented.

Speaker: Dr Callum Wilkinson (LHEP, University of Bern)

Slides Wilkinson_TAUP_2019.pdf

205 Results and Prospects from the NOvA Experiment.

The NOvA experiment is a long-baseline neutrino oscillation experiment that uses the upgraded NuMI beam from Fermilab to detect both electron neutrino appearance and muon neutrino disappearance. NOvA employs two functionally equivalent detectors: a Near Detector, located at Fermilab, and a Far Detector, located at Ash River, Minnesota over an 810 km baseline. NOvA's primary physics goals include precision measurements of neutrino oscillation parameters, such as the large mixing angle and the atmospheric mass-squared splitting, along with probes of the mass hierarchy and the CP violating phase. This talk will present the latest NOvA measurements of the neutrino oscillation parameters using neutrino and antineutrino beams.

Speaker: Dr Fernanda Psihas (University of Texas at Austin)

Slides 20190911NOvATAUP_backups.pdf 20190911NOvATAUP.pdf

Neutrino #14

Convener: Dr Itaru Shimizu (Tohoku University)

206 Collective flavor conversion including the neutrino halo in core-collapse supernovae

Core-collapse supernovae emit high neutrino flux after core bounce. In this environment, the neutrino self-interaction is dominant, and the flavor conversions are induced. These affect observed neutrino spectra on the Earth. We have ever assumed that emitted neutrinos are free-streaming. However, some of neutrinos experience a direction-changing scattering with nuclei and these direction-changed neutrinos can have a larger intersection angle. This effect is called neutrino halo, and it can affect the flavor conversions due to the collective neutrino oscillations. In this work, we investigate this effect in core-collapse supernova model and discuss the event rate at the neutrino detector.

Speaker: Mr Masamichi Zaizen (University of Tokyo)

Slides TAUP2019_Zaizen.pptx

207 Neutrino and Gravitational Wave Signatures of Core-Collapse Supernovae

Neutrino and gravitational wave are indispensable messengers of core-collapse supernovae. Those messengers have important information on how the supernovae are initiated. Helped by recent development of the simulation technique, we can provide the prediction on the gravitational waveforms and neutrino light curves as well as the neutrino spectrum. In addition to the normal non-rotating progenitors, we succeed the simulations of rapidly rotating progenitors. Their messengers have surprisingly interesting features. In this talk, we discuss which physical quantity we can extract from the messengers in the core-collapse supernovae.

Speaker: Prof. Tomoya Takiwaki (National Astronomical Observatory of Japan)

Slides 190909taup.pptx

208 Search for event bursts in XMASS-I correlated with gravitational-wave events

A new era of the gravitational-wave astronomy has recently begun with multi-messenger observations. There are some theoretical predictions that binary neutron-star mergers emit neutrinos with energies similar to those of supernova burst neutrinos. Ton-scale liquid-xenon detectors for direct dark matter searches also have the potential to observe galactic supernova neutrino via coherent elastic neutrino-nucleus scattering (CEvNS). The XMASS-I detector located the Kamioka underground laboratory uses 832 kg of liquid-xenon in its active volume and was stably taking data since November 2013 for more than 5 years, hoping such a rare event to be observed. Using these data, we performed a follow-up search for event bursts correlated with gravitational-wave events. We looked for event bursts without assuming any particular burst model. The results were also interpreted in terms of neutrino fluence. In this talk, we will report results from this search.

Speaker: Dr Katsuki Hiraide (Kamioka Observatory, ICRR, the University of Tokyo)

Slides 190911-conf-hiraide-TAUP2019-GWrelated.pdf

209 Expanding Core-Collapse Supernova (CCSN) Search Horizon of Neutrino Detectors

Core-Collapse Supernovae (CCSN) are expected to release the $99\%$ of their energy through MeV neutrinos and a network of detectors is operative to look for these events. However, when the source distance increases and/or the average energy of emitted neutrinos decreases, the signal statistics drop and the identification of these low statistic astrophysical bursts could be challenging. In a standard search, neutrino detectors characterise the observed clusters of events with a parameter called multiplicity, i.e. the number of collected events in a time-window. We introduce a new parameter called $\xi$ (=multiplicity/duration of the cluster) that adds the information of the temporal behaviour of the expected signal with respect to background. Together with the multiplicity, this parameter can optimise the search as well as increase the search horizon. Also the network of detectors (like SNEWS), that correlate the times in different datasets in order to disentangle a signal from noise, can profit from the new suggested parameter to further optimise the search. Finally, this work could be of importance also for the multi-messenger era, together with gravitational wave network, in order to hunt the CCSNe. Taking into account the small expected CCSN rate, a miss in this detection is not an option.

Speaker: Mr Odysse Halim (Gran Sasso Science Institute (GSSI), L’Aquila, Italy; INFN (Istituto Nazionale Fisica Nucleare) sezione di Laboratori Nazionali del Gran Sasso (LNGS), Assergi, Italy)

Slides TAUP_Odysse.pdf

210 Pathways to Observing Supernova Neutrinos

Paleo-detectors are a proposed experimental technique in which one would search for traces of recoiling nuclei in minerals up to $1 \mathrm{\,Gyr}$ old. Even reading out a relatively small target sample ($100 \mathrm{\,g}$), would therefore allow one to search for very rare events thanks to the large exposure, $\epsilon \sim 100 \mathrm{\,g\,Gyr} = 105 \mathrm{\,t\,yr}$. I will show how paleo-detectors can be used to measure the nuclear recoils induced by neutrinos from galactic core collapse supernovae. In particular, I will show that it is possible to make a direct measurement of the average core collapse supernova rate in the Milky Way. Paleo-detectors will also contain information about the time-dependence of the local supernova rate over the past $\sim 1 \mathrm{\,Gyr}$. Measuring such a time evolution would provide a direct determination of the local star formation history. In addition I will investigate possible deviations to the diffuse supernova Neutrino background that might be observable with Super-Kamiokande.

Speaker: Mr Thomas Edwards (GRAPPA, University of Amsterdam)

Slides SN_neutrinos_TAUP_Edwards.pdf

Neutrino #15

Convener: Dr Itaru Shimizu (Tohoku University)

211 Measurements of the reactor antineutrinos with DANSS experiment

The detector of the reactor antineutrino DANSS is placed on a movable platform below 3.1 GW industrial reactor of Kalininskaya Nuclear Power Plant. The sensitive volume of the detector is a cubic meter of plastic scintillator assembled from 2500 strips with dual readout by SiPM and conventional PMTs (in groups of 50 strips). The detector position provides a high neutrino flux on one side and an overburden of about 50 m.w.e. on another side, resulting in counting rate up to 5000 inverse beta-decay events per day with cosmic muons induced background as low as 2%. The distance between the reactor core and the detector is changed in a week cycle of 10,7, 11.7 and 12.7 m. This allows systematic-free comparison of the antineutrino spectra measured at different distances by the same detector. This talk presents results of 2.5 year of data collection with nearly 3 million of neutrino events collected.

Speaker: Dr Igor Alekseev (Alikhanov Institute for Theoretical and Experimental Physics NRC KI)

Slides alekseev_danss4taup.pdf alekseev_danss4taup.pptx

212 Latest results from the Double Chooz experiment with near and far detectors

Three flavors neutrino mixing is now established, and the current and next-generation neutrino experiments aim to discover CP violation in neutrino sector and reveal full picture of neutrino mixing. Measurements of neutrino oscillation parameters are still important subjects as the unknown properties of neutrinos, such as CP violation phase, are often measured in combination with the other parameters. The most precise measurement of theta13 is given by reactor experiments and Double Chooz (DC) is a pioneering experiment among those. We report the latest theta13 measurements from DC using two detectors at different baselines from reactor cores. Systematic uncertainties on the reactor flux prediction and IBD detection are strongly canceled in comparison of the measurements by two detectors. Cancellation of the flux uncertainty is designed in DC as a consequence of nearly iso-flux experimental setup which is unique feature among three reactor experiments. DC employed a new method to detect all neutron capture channels to enlarge the effective target mass and enhance statistics of IBD signals. DC reported slightly higher value of theta13 than other two experiments, although it is still consistent within the uncertainties. To validate the accuracy of the measurement, DC demonstrated several cross-check analyses. We also report reactor neutrino flux measurements including neutrino yield from fission interactions, spectral distortion and residual neutrinos when reactor is turn off. Influence of spectral distortion to theta13 measurement is also discussed.

Speaker: Masaki Ishitsuka (Tokyo University of Science)

Slides TAUP2019-DoubleChooz-Ishitsuka.pdf

213 NEOS: reactor neutrino experiment at short baseline

Numbers of experiments are trying to measure an active-to-sterile neutrino oscillation using nuclear reactors. A precise determination of the energy spectrum is also important to make the most of the reactor neutrinos. The NEOS experiment is being conducted at 24 meter distance from a 2.8 gigawatt thermal power nuclear reactor core. It aims at finding a short baseline oscillation due to eV scale sterile neutrino, and to provide a reactor neutrino energy spectrum with a high resolution and a high signal-to-background ratio.

Speaker: Dr YOOMIN OH (Center for Underground Physics, Institute for Basic Science)

Slides Neutrino15_yoomin.pdf

214 Search for eV Sterile Neutrinos – The STEREO Experiment

During the last decade, the smallest neutrino mixing angle $\theta_{13}$ was determined with high precision thanks to reactor antineutrino experiments. However, two anomalies are still persistent: the absolute flux of detected reactor antineutrinos and their spectrum shape. Also known as Reactor Antineutrino Anomaly (RAA), the flux anomaly could be explained by introducing a light sterile neutrino eigenstate which is mixing with other flavors via the oscillation mechanism. Indeed, the RAA would be solved by oscillation parameters around $\sin^{2}(2\theta_{ee}) = 0.14$ and $\Delta m_{41}^{2} = 2.4~\textrm{eV}^{2}$. The \textsc{Stereo} experiment aims at searching for oscillation patterns with parameters within the RAA allowed region by measuring the antineutrino spectra for different propagation lengths. \textsc{Stereo} was one of the first experiments designed to probe for an eV mass scale sterile neutrino and is taking data since the end of 2016 at the ILL reactor in Grenoble (France). The antineutrinos are emitted by a compact nuclear reactor core and are detected in 6 identical cells covering propagation lengths from 9 to 12 m. This configuration allows to test several oscillation scenarios without any spectrum prediction. Therefore \textsc{Stereo} is able to detect an oscillation pattern unambiguously. The first results have been released in 2018, and most of the RAA parameter space has been excluded with only 66 (138) days reactor-on (off) data. In this talk, the latest results of \textsc{Stereo} will be presented with significantly improved sensitivity to the oscillation of a sterile neutrino, as well as a discussion of the antineutrino spectrum shape.

Speaker: Mr Adrien BLANCHET (CEA/Irfu/DPhN)

Slides STEREO_TAUP_2019.pdf

New Technology #3

215 Carbon Nanotube as anisotropic target for dark matter.

Directional detection of Dark Matter particles (DM) could be accomplished by studying either ion or electron recoils in large arrays of parallel carbon nanotubes. For instance, a MeV mass DM particle could scatter off a lattice electron, resulting in the transfer of sufficient energy to eject the electron from the nanotube surface. The electron can eventually be detected whenever an external electric field is added to drive it from the open ends of the array. This detection scheme would offer an anisotropic response and could be used to select an orientation of the target with respect to the DM wind. A compact sensor, in which the cathode element is substituted with a dense array of parallel carbon nanotubes, could serve as the basic detection unit which - if adequately replicated -would allow to explore a significant region of light DM mass and cross-section. A similar detection scheme can be devised in case DM would scatter on the surface of a CNT and a carbon ion might be ejected – allowing to investigate the existence of a few GeV mass DM particle. We report about the Monte Carlo simulations of such a system and the R&D towards a prototype detector.

Speaker: Prof. Gianluca Cavoto (Sapienza Univ Roma and INFN Roma)

Slides CNT-TAUP2019.pdf

216 Light detection in DarkSide-20k

The DarkSide programme aims to a WIMP direct detection using a dual phase argon time projection chamber. The next generation experiment, DS-20k, will be a detector in excess of 20 tonnes of fiducial mass. A pivotal aspect to the sensitivity of the experiment is its light detection technology. The DarkSide collaboration decided to adopt a new family of photo-sensors called Silicon Photomultipliers (SiPMs). The talk will introduce the design of a DarkSide Photo Detector Module (PDM), a 25cm^2 array of SiPMs read-out as a single channel. The PDM’s performances in terms of photon detection efficiency, dark count rate, and correlated noises will be outlined, including an overview of the detailed characterisation of the detector’s signal-to-noise ratio and its time resolution. Then the signal extraction strategies will be discussed, focusing on the optical analog cryogenic transmission using radiopure fibers immune to electronic noise injection in the detector. Finally, an overview of the silicon packaging strategies adopted by the DarkSide collaboration will be introduced with attention to the mass-production of the 13000 PDMs, to the material selection and to the high radiopurity result achieved.

Speaker: Claudio Savarese (Princeton University)

Slides DS-20k_LightDetection_Savarese.pdf

217 Low Radioactivity Argon for Dark Matter and Rare Event Searches

The DarkSide-50 dark matter search experiment demonstrated that argon derived from deep underground sources can be highly reduced in 39Ar, and since then the demand for this commodity has risen. Several fundamental physics experiments require argon reduced in 39Ar as well as 42Ar, as well as other rising needs in other scientific fields (e.g., age-dating). With the expanded needs come the questions of availability and how to approach the challenges associated with its production and characterization.  This talk will provide a global picture of low-radioactivity underground argon procurement, from its production to quality control and quality assurance. We will detail the DarkSide-20k plan for extracting more argon from the DarkSide-50 source through a project called Urania, as well as another project which will serve to isotopically separate 39Ar from 40Ar, called Aria. Finally, DART is a small (~1 L) chamber that will measure the depletion factor of 39Ar in UAr. The detector will be immersed in the LAr active volume of ArDM (LSC, Spain), which will act as a veto for gammas, allowing a precise measurement of the 39Ar residual activity.

Speaker: Dr Walter Marcello Bonivento (INFN)

Slides TAUP_Bonivento_2019.pptx

218 The XENONnT Neutron Veto Detector

The XENONnT project, the next phase of the XENON program, will feature a new TPC with an active target of ~6 tonnes of Xenon (~4 tonne fiducial) and will implement a series of technological solutions aiming to further suppress the dominant background (BG) sources and boost the physics reach of the experiment. Neutrons are a particularly dangerous BG for direct WIMP dark matter searches; their nuclear recoils with the target nucleus are often indistinguishable from nuclear recoils produced by WIMP-nuclear collisions. To further remove this neutron BG, we surround the large active Xe volume with a dedicated detector capable of tagging neutrons with high efficiency (nVeto), a water Cherenkov detector doped with gadolinium. In this talk, we will report on the design studies, radioactive background requirements and expected performance of the XENONnT nVeto detector.

Speaker: Dr Shingo Kazama (Nagoya University)

Slides XENONnT_nVeto_TAUP_SKazama.pdf

219 A measurement of the scintillation decay time constant in liquid xenon with the XMASS-I detector

Liquid xenon has been used in many modern experiments. The scintillation light of xenon is produced by the de-excitation of dimer state Xe$_{2}^{*}$. The dimer is produced by the direct excitation of xenon atoms or the recombination process between electrons and xenon ions. The dimer has both a singlet and triplet state, each with its own decay time constant. Since the ratio of the singlet to triplet states and the recombination time depends on the deposit energy density, the scintillation decay constant information can be used for particle discrimination between nuclear recoil and electron recoil. XMASS-I experiment is a single phase liquid xenon detector primarily for dark matter search. We measured the scintillation decay time constant of both electron recoil and nuclear recoil using calibration sources irradiating the XMASS-I detector. In this talk, we will present the result of the measurement of the scintillation decay time constant with XMASS-I detector.

Speaker: Dr Koichi Ichimura (Kamioka Observatory, ICRR, the University of Tokyo)

Slides 190911-TAUP-ichimura.pdf

Cosmology #2

Convener: Prof. Masahiro Kawasaki (ICRR, University of Tokyo)

220 Improved nuclear reaction network for a reliable estimate of primordial Deuterium yield

A fundamental requisite to get a precise determination of light nuclide primordial abundances is the correct evaluation of the nuclear reaction rates of the BBN reaction network, as well as the corresponding uncertainties. In particular, for the primordial deuterium the most important nuclear inputs are the deuteron-deuteron transfer reactions, D(D,n)3He and D(D,p)3H, and the D(p,gamma)3He radiative capture. In this talk, I will review the current status in this field, with particular emphasis on the statistical method of analysis of experimental data to get the rates for deuterium synthesis.

Speaker: Prof. Ofelia Pisanti (University of Naples Federico II)

Slides Deuterium.pdf

221 Active-sterile neutrino oscillations in the early Universe with the complete mixing matrix

In the framework of a 3+1 scheme, we consider the thermalisation of sterile neutrinos in the early Universe taking into account the full 4x4 mixing matrix. The evolution of the neutrino energy distributions is found solving the momentum-dependent kinetic equations with full collision terms, as in our previous analyses of flavour neutrino decoupling in the standard case. The degree of thermalisation of the sterile state is shown in terms of the effective number of neutrinos ($N_{\rm eff}$) and its dependence on the three additional mixing angles ($\theta_{14}$, $\theta_{24}$ and $\theta_{34}$) is discussed. Our results are relevant for fixing the contribution of a fourth light neutrino species to the cosmological energy density, whose value is very restricted by the final Planck analysis.

Speaker: Dr Sergio Pastor (IFIC (CSIC-Univ Valencia))

Slides pastor_TAUP2019.pdf pastor_TAUP2019.pptx

222 MeV-scale reheating temperature and thermalization of three active neutrinos by radiative and hadronic decays of massive particles

We determine the minimum value of the reheating temperature set by Big-Bang Nucleosynthesis by considering both radiative and hadronic decays of long-lived massive particles. In the current study, effects of neutrino oscillation and neutrino self-interaction are taken into account in the calculation of the neutrino thermalization. We adopt updated observational bounds on the primordial abundance of light elements. An obtained lower bound on the reheating temperature is $T_{\,\rm RH}$ > 2.6 MeV in the case of the 100% radiative decay, and $T_{\,\rm RH}$ > 3 MeV − 5 MeV in the case with hadronic decays depending on the mass of the massive particles and the hadronic branching ratio of the decay. Also, we find that the effects of neutrino oscillation and neutrino self-interaction increase the lower bound at the level of O(10)% in the case of the 100% radiative decay and O(1)% in the case with hadronic decays.

Speaker: Mr Takuya Hasegawa (KEK / Sokendai)

Slides TAUP2019_TH_PDF.pdf

DM13: WIMP Dark Matter II

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

223 Analysis and Dark Matter Search Results from DEAP-3600 with 231 Live Days at SNOLAB

DEAP-3600 is a dark matter direct detection experiment operating 2 km underground at SNOLAB (Sudbury, Canada). This single-phase detector consists of 3.3 tonnes of liquid argon (LAr), viewed by an array of 255 photomultiplier tubes through 50 cm of acrylic. The collaboration has recently released dark matter search results from the first year of running (November 2016 to October 2017), with a total live time of 231 days. This talk will detail the analysis underlying these results, including the development of a detailed background model, which constitute the most sensitive search performed with a LAr target for WIMPs with a mass greater than 30 GeV.

Speaker: Dr Shawn Westerdale (Carleton University)

Slides taup2019_swesterdale.pdf

224 Dark Matter Search with DEAP-3600 at SNOLAB

DEAP-3600 is searching for dark matter particle interactions on several tonnes of liquid argon at SNOLAB. The detector, operating since late 2016, contains 3.3 tonnes of argon in a large ultralow-background spherical acrylic vessel and detects interactions by observing scintillation photons. Excellent pulse-shape discrimination between nuclear and electronic recoils has been demonstrated in argon, and the detector has been designed for control of radioactive backgrounds from all sources, with particularly good sensitivity to high-mass WIMPs. An overview of the project, recent results from the first long exposure dark matter search released in early 2019 and future plans will be presented.

Speaker: Prof. Mark Boulay (Carleton University)

Slides deap_boulay_taup_2019.pdf

225 Search for WIMP-$^{129}$Xe inelastic scattering using particle identification in XMASS-I

A search for inelastic scattering of Weakly Interacting Massive Particles (WIMPs) off $^{129}$Xe was conducted in XMASS-I. In the inelastic scattering, the nucleus of $^{129}$Xe is excited via spin-dependent interaction. For a more sensitive search, a particle identification using the waveform was introduced to separate the beta-ray events and the others. Using XMASS-I data ($\mathrm{800\; days\times 327\; kg}$), which is 48 times larger statistics than our previous search, we conducted the search and found no significant signal. We obtained a limit on the WIMP-neutron cross section $\sigma < 4.1 \times 10^{-39}\; \mathrm{cm^2}$ (90% C.L.) for $200\; \mathrm{GeV}/c^2$ WIMP. This result is more stringent by a factor of 7.7 than the existing experimental result. In this talk, we will present the method of particle identification and the result of this search.

Speaker: Mr Takumi Suzuki (ICRR)

Slides T-20190911-suzuki-TAUP-DM13-inelastic.pdf

226 High Mass WIMP Results with DarkSide-50 and Prospects for Ds20k/Argo

The DarkSide-50 direct-detection dark matter experiment is a dual-phase argon time projection chamber operating at Laboratori Nazionali del Gran Sasso (LNGS) of INFN. It is sensitive to WIMPs with masses above 50 GeV/c2 by exploiting the exceptional pulse shape discrimination of the scintillation signal in LAr. A blind analysis, using (16,660+-270) kg d exposure using a target of low-radioactivity argon extracted from underground sources and no events were found in the dark matter selection box, setting a 90% CL upper limit for the dark matter-nucleon spin-independent cross-section of 1.14E-44 cm^2 (3.78E-44 cm^2, 3.43E-43 cm^2) for a WIMP mass of 100 GeV/c^2 (1 TeV/c^2, 10 TeV/c^2). This result show the strong potential of LAr-based detectors in searching for WIMPs. This technology will be further exploited with DarkSide-20k, a 23 ton fiducial volume dual-phase TPC that will be installed at LNGS in 2022, and with ARGO, a 300 ton fiducial volume detector, expected to come online by the end of the next decade and that will push the sensitivity down to the neutrino floor.

Speaker: Dr Yi Wang (UCLA)

Slides DS-50_High_Mass_WIMP.pdf

227 Results of direct dark matter detection with CDEX experiment at CJPL

The China Dark Matter Experiment (CDEX), located at the China Jinping Underground Laboratory (CJPL) whose overburden is about 2400m rock, aims at direct searches of light Weakly Interacting Massive Particles (WIMPs). A single-element 994-gram p-type point contact (PPC) germanium detector (CDEX1B) runs inside a solid passive shielding system. To achieve lower background, a prototype 10kg PPC germanium detector array (CDEX10), consisting of three detector strings with three germanium crystals each, is directly immersed in the liquid nitrogen. With the energy threshold of 160eV, the limits on WIMP-nucleus scattering are set by energy spectra and annual modulation analysis, respectively. Incorporating Migdal effect and bremsstrahlung emissions, the data are re-analyzed to search sub-GeV WIMPs. In addition, other DM candidates, i.e. dark photon and axion, are constrained. Finally, the future plan of CDEX experiment in CJPL-II is introduced.

Speaker: Prof. Hao Ma (Tsinghua University)

Slides CDEX_status_TAUP19_MH.pdf

228 New Analysis Results from the LUX Dark Matter Experiment

The LUX (Large Underground Xenon) was a dark matter experiment using a two-phase Xe Time Projection Chamber located at the Sanford Underground Research Facility (SURF) in Lead, South Dakota 2012-2017. It previously published three separate world-leading limits on the spin-independent cross-section for Weakly Interacting Massive Particle (WIMP) dark matter via direct detection, with a fiducial mass of up to 150 kg. The LUX detector has been precision calibrated over a wide energy range from 170 eV to many MeV with very high statistics using a number of novel procedures. These analyses have provided an unprecedented level of understanding in the response of liquid Xe to many types of particle interaction. I will report on the most recent analysis efforts the LUX collaboration is making which further exploit the data from the four years of detector operation. The new analyses include rare event searches for Dark Matter candidates including sub- GeV dark matter, Mirror Dark Matter, LIPs, time-modulated signals and signals from S2-only (ionization) events. I will also discuss how LUX is also being used to better understand the potential detector performance of future dual-phase detectors for WIMP-nucleon scattering, and to demonstrate new analysis methods that can be used to improve our discrimination of backgrounds within next-generation experiments.

Speaker: Prof. Vitaly Kudryavtsev (University of Sheffield)

Slides LUX-TAUP2019-VK.pdf

DM14: New Ideas in Sub-GeV Dark Matter

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

229 Sub-GeV Dark Matter in Superfluid He-4: an Effective Theory Approach

We employ an effective field theory to study the detectability of sub-GeV dark matter through its interaction with the gapless excitations of superfluid 4He. In a quantum field theory language, the possible interactions between the dark matter and the superfluid phonon are solely dictated by symmetry. We compute the rate for the emission of one and two phonons, and show that these two observables combined allow for a large exclusion region for the dark matter masses. Our approach overcomes several limitations of standard techniques, and allows to compute differential distributions, hardly accessible otherwise. The method presented here is easily extendible to different models of dark matter.

Speaker: Dr Angelo Esposito (EPFL Lausanne CH)

Slides TAUP_2019.pdf

230 Development of a New Detector that Uses Liquid He and Field Ionization to Search for Light Dark Matter

We describe a new detector for dark matter searches by direct detection based upon the quantum evaporation of He atoms from a cold surface and their detection using field ionization. The single atom sensitivity of the field ionization array and the $<1$ meV binding energy of a He atom to the surface of liquid He open the door for the detection of dark matter particles with mass as low as $1$ MeV/c$^2$. When a dark matter particle collides with an atom in liquid He it produces phonons and rotons. When the rotons arrive at the surface they can evaporate a He atom, which can be detected by a field ionization array. This dense array of sharp, positively charged metal tips will ionize the He atoms in a strong electric field and accelerate them to a high kinetic energy. A calorimeter with a low heat capacity can easily measure the impact of even just one of these He ions. We will present the design of the proposed detector as well as the results of preliminary field ionization experiments.

Speaker: David Osterman (Brown University)

Slides TAUP_2019_-_David_Osterman.pptx

231 LBECA: A Low Background Electron Counting Apparatus for Sub-GeV Dark Matter Detection

Two-phase noble liquid detectors, with large target masses and effective background reduction, are currently leading the dark matter direct detection for WIMP masses above a few GeV. Due to their sensitivity to single ionized electron signals, these detectors were shown to also have strong constraints for sub-GeV dark matter via their scattering on electrons. In fact, the most stringent direct detection constraints for sub-GeV dark matter down to as low as ~5 MeV come from noble liquid detectors, namely XENON10, DarkSide-50 and XENON100, although these experiments still suffer from high background at single or a few electron level. LBECA is a planned 100-kg scale liquid xenon experiment with significant reduction of the single and a few electron background and will improve the sensitivity to sub-GeV dark matter by at least three orders of magnitude compared to the current best constraints. We will present several R&D efforts that are in advanced stages to address the single and few electron background by the LBECA collaborative institutions (LLNL, LBNL, Purdue, Stony Brook, UCSD). The parameter space that is relevant to the dark matter content in the Universe and will be probed by the LBECA experiment will be shown.

Speaker: Prof. Kaixuan Ni (University of California San Diego)

Slides LBECA_KNI_TAUP2019.pdf

232 The Light-only Liquid Xenon Project

The Light-only Liquid Xenon (LoLX) project aims to study the properties of light emission in liquid xenon (LXe). Investigating timing characteristics of both the scintillation and Cherenkov light, LoLX will explore the abilities of single-phase LXe detectors as particle detectors and in medical imaging devices. The first phase of the LoLX detector consists of 24 Hamamatsu VUV4 Silicon photomultipliers (SiPMs), giving a total of 96 channels arranged in an octagonal cylinder. Covering 92 of the channels are 225 nm long pass filters which block the Xe scintillation light allowing for independent measurements of the long-wavelength Cherenkov and VUV scintillation light. The first stage of LoLX aims to measure the Cherenkov and scintillation yields from $^{90}$Sr beta-decays and $^{210}$Po alpha-decays. This data is used to validate optical transport simulations using GEANT4 and verify measurements of the VUV light reflectivity performed at TRIUMF. This validation is a vital input into the design of next-generation LXe experiments. Future phases of the project will upgrade to fast waveform digitizers with 10 ps timing accuracy and 3D integrated digital SiPMs (from U.Sherbrooke). These upgrades will allow precision characterization of Xe scintillation and evaluation of the capabilities to separate the Cherenkov signal using the prompt arrival times. LoLX will begin commissioning in late summer with first data in early fall. The current state and outlook for the LoLX project will be presented.

Speaker: Dr Thomas McElroy (McGill University)

Slides https://drive.google.com/file/d/13YVpZMUYc8Sw7SxVWFc3CPCewk-J_RFe/view?usp=sharing

233 Atomic many body calculations for dark matter scattering on electrons: Ge & Xe Detectors

Scattering of light dark matter (LDM) particles with atomic electrons is studied in the context of effective field theory. Contact and long-range interactions between dark matter and an electron are both considered. A state-of-the-art many-body method is used to evaluate spin independent atomic ionization cross sections of LDM-electron scattering. New upper limits are derived on parameter space spanned by LDM mass and effective coupling strengths using data from the CDMSlite, XENON10, and XENON100 experiments. Comparison with existing calculations shows disagreement and indicates the importance of atomic many-body physics in direct LDM searches.

Speaker: Dr Mukesh Kumar Pandey (1Department of Physics, National Taiwan University, Taipei 10617, Taiwan)

Slides Web_DM14_MukeshKumarPandey.pdf

234 High sensitivity tests of Spin statistics in the Gran Sasso Underground Laboratory

The VIP2 (VIolation of the Pauli Exclusion Principle) experiment at the Gran Sasso underground laboratory (LNGS) is testing standard quantum mechanics by searching for possible violation of the Pauli Exclusion Principle (PEP) – a consequence of the spin statistics theorem. Due to the high sensitivity it can also test present models of quantum gravity, which can embed PEP violations. VIP2 is extremely sensitive to Pauli-forbidden atomic transitions in copper atoms using precision X-ray spectroscopy. We will present the used experimental method for the search of Pauli-forbidden X-ray transitions in copper atoms, produced by "new" electrons, which could have tiny probability to undergo Pauli-forbidden transition to the ground state already occupied by two electrons. We will describe the VIP2 experimental setup and recent optimizations. The goal of VIP2 is to test the PEP for electrons in accordance with the Messiah-Greenberg super-selection rule at unprecedented accuracy, down to a limit in the probability that PEP is violated at the level of 10E-31. We will present current experimental results and discuss implications of a possible violation. Work partially supported by the Austrian Science Fund (project P 30635-N36)

Speaker: Dr Johann Marton (Senior Scientist)

Slides VIP2-JMarton.pptx

HECR #6

235 Variations of cosmic ray muon flux during thunderstorms as a tool for studying electric field distribution and particle production processes in the atmosphere

The variations of secondary cosmic rays during thunderstorm periods are under study at the Baksan Neutrino Observatory for many years. Large-area groups of scintillation detectors of the Carpet air shower array operate in a single-particle mode measuring the count rates of the soft component cosmic rays (electrons, positrons and gamma rays in the energy range 10-30 MeV) and of muons with energy thresholds 100 MeV and 1 GeV. The near-ground electric field and precipitation electric current are also measured every second together with atmospheric pressure and temperature. At recent stages of the experiment the geomagnetic data are included into analysis, and optical observations are organized for night thunderstorms with remote video cameras viewing the region above thunderclouds from a distance of 75 km. The regression curves ‘intensity versus field’ were obtained in this experiment long ago. These functions are approximated by second order polynomials both for the soft component and muons, quadratic coefficients having different signs (negative for muons and positive for the soft component), while linear coefficients are of the same sign (negative). In addition to this regular behavior, from the very beginning the bright sporadic variations were also observed, in the case of the soft component called much later TGE (terrestrial ground enhancement) events. TGEs were interpreted as a result of cycling generation of particles in acceleration regions with feedback loop, where electrons and positrons are accelerated in different directions in one and the same field. Bright muon intensity disturbances, which are a subject matter of this report, can be of different polarities (positive and negative). In addition, they can be accompanied by TGE or not. The theoretical analysis has shown that the amplitude of muon disturbance is connected with potential difference between the ground level and the effective altitude of muon production. The field in the stratosphere can exceed the critical value for runaway electrons and generation of particles of TGE type takes place at very high altitudes. In fact, this is a slow (semi-stable) process of particle production representing a high-altitude discharge of a new type. We present some experimental observations of a nighttime thunderstorm glow by remote video cameras that confirm this model.

Speaker: Dr Alexander Lidvansky (Institute for Nuclear Research, Russian Academy of Sciences, Moscow)

Slides muons_lidvansky1.ppt

236 Search for diffuse cosmic gamma rays of ultra-high energies with the Baksan air shower array

The Baksan EAS array is located in the North Caucasus region near Mount Elbrus at an altitude of 1700 m above see level. The basic part of the array is a ground level detector called the Carpet (200 m^2), surrounded by six outdoor huts with 9 m^2 of scintillation counters in each. The array is permanently modernized and extended. Its previous Carpet-2 configuration included an underground muon detector (MD) with a total area of 175 m^2. At the present time the Carpet-3 project is realized with increased area of the muon detector (up to 410 m^2) in order to search for muon-poor showers presumably initiated by primary cosmic gamma rays. The status and prospects of the experiment are discussed, and some preliminary data are presented.

Speaker: Dr Alexander Lidvansky (Institute for Nuclear Research, Russian Academy of Sciences, Moscow)

Slides gamma_lidvansky2.ppt

237 Ten years of cosmic muons observation with Borexino

The Borexino detector at Gran Sasso has now accumulated over ten years of continuous data which represent a magnificent opportunity to study the cosmic muon flux at a deep underground location. We present here a precision measurement of the flux and of the expected seasonal modulation. We present the correlation with the atmospheric temperature variations from global atmospheric models. We measure the correlation parameters and infer the kaon-to-pion ratio in the production of cosmic muons from high energy primaries. We also find evidence of a long term modulation that is not present in the atmospheric data and we investigate a possible positive correlation with the solar activity. Finally we observe a seasonal modulation of the production rate of cosmogenic neutrons that is in phase with the muon modulation but shows a surprisingly larger amplitude

Speaker: Mr Davide D'Angelo (University of Milano)

Slides taup3.pdf

238 High-multiplicity muon events observed with EMMA array

We present, for the first time, high-multiplicity data collected with a segmented scintillator array of the cosmic-ray experiment EMMA (Experiment with Multi Muon Array). The data were acquired over the period of 450 days using 800 plastic scintillator pixels probing the fiducial area of ~100 m2. The results are interpreted in terms of CORSIKA simulations. Several events with densities in excess of 10 muons per m2 were observed. At the second stage of the analysis, the high-multiplicity events will be matched with precision tracking data extracted from the multi-layer drift chambers of EMMA. Observation of high-density muon bundles were first reported by the LEP experiments: DELPHI, L3+C, and ALEPH. More recently, the ALICE experiment at CERN has provided new results together with improved interpretation benefiting from the updated cross section values extracted from the recent LHC results. While the tracking performance of ALICE is superior to EMMA, ALICE has been able to collect cosmic-ray data for the average of only 9 days per year yielding the total 2010-2018 exposure of just 93 days. The cosmic-ray experiment EMMA, located at the depth of 75 meters (210 m.w.e.) in the Pyhäsalmi mine in Finland, has a similar overburden but a larger footprint and collects data continuously. The two types of detectors used by EMMA are drift chambers and plastic scintillation detectors. In the presentation, a short description of the setup will be given followed by the latest results, simulations, comparison with other experiments, and outlook.

Speaker: Wladyslaw Henryk Trzaska (University of Jyvaskyla)

Slides Trzaska_HighMultiplicity_comp.pptx

239 LHCf: LHC forward experiment for CR interaction study

The precise knowledge of the hadronic interaction is one of keys for a proper understanding of properties of high energy cosmic-rays. Large Hadron Collider (LHC) provides unique opportunities for us to study hadronic interactions at the very high collision energy equivalent to $10^{17}$ eV cosmic-ray interactions. The LHC forward (LHCf) experiment aims to have measurements of neutral particles, photons, neutral pions, and neutrons, emitted in the zero degree region of proton-proton collisions at an LHC interaction point. These energetic particles play an important role in cosmic-ray induced air shower developments. LHCf have position-sensitive sampling calorimeters installed at +/- 140 m from the ATLAS interaction point, and we performed several operations with $\sqrt{s}$ = 0.9-13 TeV pp and $\sqrt{s_{NN}}$ = 5-8 TeV pPb collisions since LHC started in 2009. In this presentation, we will report about our results from the past operations as well as the future prospects about operations scheduled for the LHC-Run3 period.

Speaker: Dr Hiroaki Menjo (Nagoya University)

Slides 20190911_TAUP_Menjo.pdf

240 Recent results status and perspectives from ANTARES and KM3NeT Mediterranean Neutrino Telescopes.

The primary goal of the ANTARES telescope is the search for astrophysical neutrinos in the TeV-PeV range. ANTARES has searched for neutrino sources in the Southern Sky at TeV energies and set constraints on the origin of the cosmic neutrino flux discovered by IceCube. ANTARES has actively developed a manifold multi-messenger program, both in real time and offline. Of particular interest the searches triggered by gravitational wave observations. Thanks to its excellent angular resolution, dedicated searches for promising neutrino source candidates and several interesting regions like the Galactic Plane or the Fermi Bubbles were performed, using for the first time also a sample of cascade events with a median angular resolution of about 3 degrees. The results on the indirect search for DM with the ANTARES detector, looking for neutrinos from the centre of Galaxy, from the Sun and from the centre of the Earth will be also presented and discussed. The high quality of the data provided by ANTARES and the competitiveness of the achieved results, demonstrate the tremendous potential of the new, much larger array, KM3NeT. The status and the perspectives of that project for neutrino astronomy, with its two telescopes ORCA and ARCA, will be reported.

Speaker: Prof. Antonio Capone (Physics Department, University "La Sapienza" and INFN, Roma)

Slides TAUP2019_Capone.pdf TAUP2019_Capone.pptx

Neutrino #16 & Outreach

Convener: Dr Itaru Shimizu (Tohoku University)

241 Sensitivity to leptonic CP violation at Hyper-Kamiokande

Hyper-Kamiokande is a next generation water Cherenkov detector, an order of magnitude larger than Super-Kamiokande, capable of large and diverse physics studies. Among these, it will study long baseline oscillation physics with great detail, thanks not only to a larger volume and higher detection efficiency, but also to an improved accelerator and near detector system at J-PARC. In order to perform precise measurement of the oscillation parameters, it is essential that systematic uncertainties are well understood. To do so, we study the effect and impact that the systematic errors have on the overall sensitivity of the experiment, with particular care for the CP violating phase. Being able to determine the value of the CP violating phase can bring about deep implications to a variety of the theoretical models. In this talk, I will give a theoretical background on CP violation in the leptonic sector, quickly moving to the description of the experiment. I will then explain our methodology and finally show some study results.

Speaker: Mr Tommaso Boschi (Queen Mary University of London)

Slides BoschiTAUP2019.pdf

242 Performances of multi-PMT photodetector for the Hyper-Kamiokande experiment (the Hyper-Kamiokande proto-collaboration)

Hyper-Kamiokande, a 260 kton water Cherenkov detector to be built in Japan, is the next generation of the Super-Kamiokande experiment. Its broad physics program includes nucleon decay, neutrinos from astronomical and human-made beam, with the main focus to determine the leptonic CP violation. To detect the weak Cherenkov light generated by neutrino interactions or proton decay, the primary photo-detector candidate are 20-inch PMTs. In order to enhance the Hyper-Kamiokande physics sensitivity, the use of multi-PMT modules is considered as a complement of the primary candidates. A multi-PMT Optical Module based on a pressure vessel instrumented with multiple small diameter photosensors, readout electronics and power, offers several advantages as increased granularity, reduced dark rate, weaker sensitivity to Earth’s magnetic field, improved timing resolution and directional information with an almost isotropic field of view. In the first part of this talk, we will briefly present the multi-PMT modules developed for Hyper- Kamiokande, as well as introduce the first masurements of their individual PMT performances. We will then show their positive impact on the sensitivity of the Hyper-Kamiokande Intermediate Water Cherenkov detector, which motivated their choice as the primary photosensor candidate. We will finally conclude by presenting the impact of these modules on the physics of the Hyper-Kamiokande far detector.

Speaker: Mr Benjamin Quilain (Kavli IPMU, WPI, The University of Tokyo)

Slides HyperK_20190913_HyperKamiokandemPMT_TAUP2019_Quilain_v2.pdf

243 Status of DUNE Experiment

The Deep Underground Neutrino Experiment (DUNE) is a next-generation long-baseline experiment. DUNE will utilize a high-intensity neutrino beam produced at Fermilab and will measure electron-neutrino appearance and muon-neutrino disappearance with its 40 kiloton (fiducial mass) Liquid Argon far detector at the Sanford Underground Research Facility (SURF) in Lead, South Dakota, 1300 km from Fermilab. The goals of DUNE are studies of neutrino oscillations, including CP violation and neutrino mass hierarchy determination, and searches for nucleon decays and supernova neutrinos, as well as precision neutrino physics at the near site. The DUNE far detectors are based on liquid argon time projection chamber (LArTPC) technology, which offers an excellent spatial resolution, high neutrino detection efficiency, and superb background rejection. The large DUNE far detector single phase LArTPC prototype (ProtoDUNE-SP) at CERN has taken beam and cosmic data in 2018. The dual phase prototype (ProtoDUNE-DP) is under construction and will be operated soon. In this talk, we will discuss the status and physics reach of the DUNE experiment, as well as the first data taken from protoDUNE-SP.

Speaker: Prof. Jianming Bian (University of California, Irvine)

Slides DUNE_TAUP2019_09_11.pdf

244 Status of The Dual Phase Liquid Argon TPC Developments for the DUNE experiment.

Future giant LArTPCs at the 10 kton fiducial mass scale are now in the design and prototyping phase at CERN in the context of the Deep Underground Neutrino Experiment (DUNE). This technology is very attractive as it is cost-effective, scalable to the multi-kiloton level. LArTPCs are excellent calorimeters with the ability to 3D reconstruct and perform PID of ionizing tracks.Two technologies are considered for DUNE: single and dual phase LAr TPC. The dual phase design features a charge amplification system inserted in a gas layer before charge collection. In 2017, a dual phase LArTPC demonstrator (4.2t) has recorded cosmic rays at CERN. Charge and scintillation light were collected, and preliminary results will be shown. Large (~300 t) single and dual phase LArTPC prototypes has been constructed at the CERN neutrino platform. The dual phase prototype construction is almost finished, its commissioning will start in a few weeks. The status of the dual phase prototype will be presented.

Speaker: Dr Laura Zambelli (LAPP - CNRS/IN2P3)

Slides lzambelli_TAUP2019.pdf

245 Outreach for Hyper-Kamiokande

Hyper-Kamiokande is a next generation neutrino and nucleon decay experiment that is expected to start taking data in 2027. In this talk, I will discuss recent outreach efforts with a special focus on the difficulties and opportunities that arise when doing outreach for an experiment that is still years away from completion.

Speaker: Jost Migenda (University of Sheffield)

Slides 20190911_Outreach_for_HK.pdf

Neutrino #17

Convener: Dr Itaru Shimizu (Tohoku University)

246 The Status of AMoRE Double Beta Decay Experiment

AMoRE (Advanced Mo-based Rare process Experiment) is searching for neutrinoless double beta decay of Mo-100. A pilot experiment, AMoRE-Pilot, was operated with six 40Ca100MoO4 (CMO) crystals of total mass ~1.9 kg in a cryostat at the Yangyang underground laboratory with the minimum overburden of 700 m. Ever since the AMoRE-Pilot had started in August 2015, two major improvements in its configuration took place to reduce its background level. The first one is replacement of detector components with high radio-activities. Secondly, polyethylene (PE) blocks were installed outside of the muon detectors together with borated rubber sheets inside the muon counters and outside of the lead shield to reduce external neutron backgrounds. Using the AMoRE-pilot data in different configurations, background modeling of the AMoRE-Pilot was performed. We will present backgrounds of the detector before/after the improvements and the modeling results. We plan to reduce the background level even further in the next phase experiment, AMoRE-I, which would have thirteen CMO and four LMO (Li2100MoO4) crystals with a total mass of ~6 kg. The background reduction plan with an improved shielding will be described.

Speaker: Mr Kyungmin Seo (Department of Physics, Sejong University)

Slides 20190911_TAUP2019_AMoREstatus_v6.pdf

247 First data from the CUPID-Mo neutrinoless double beta decay experiment

The Cryogenic Underground Observatory for Rare Events (CUORE) is the first ton-scale cryogenic bolometer experiment searching for neutrinoless double beta decay (0νββ). The technology for it’s successor, CUPID (CUORE Upgrade with Particle ID) is designed to probe 0νββ is the so-called inverted mass hierarchy region and is currently being employed in the CUPID-Mo demonstrator searching for 0νββ in $^{100}$Mo. This demonstrator consists of an array of 20 enriched ~0.2 kg Li$_2$MoO$_4$ crystals complemented by 20 cryogenic Ge bolometers to distinguish alpha from beta/gamma events by the detection of both heat and scintillation light signals. Commissioning started in Dec 2018 and we switched to routine data taking in spring 2019. In this talk, we will present results from this first data, confirming an excellent bolometric performance of $\sim$5-6 keV energy resolution (FWHM) at 2615 keV, full alpha to beta gamma separation and improved estimates on the radiopurity of the crystals. We will conclude with an update on the status of the experiment, an expectation of the sensitivity of CUPID-Mo as well as the prospects for CUPID.

Speaker: Dr Benjamin Schmidt (Lawrence Berkeley National Laboratory)

Slides CUPID_Mo_TAUP2019_BenjaminSchmidt.pdf

248 Discovery potential of next-generation neutrinoless double-β decay experiments

With KamLAND-Zen and CUORE now taking data, LEGEND-200 and SNO+ under construction, and nEXO, CUPID, and LEGEND-1000 under consideration for major funding in the US and Europe, we are now entering the era of ton-scale neutrinoless double beta decay searches. We will present our evaluation of the sensitivity of these searches based on the exposure and background rates anticipated by each experiment. We will discuss how recent advances in nuclear theory are allowing qualitatively new understanding of the connection between neutrinoless double-beta decay and its underlying mediation mechanism.  We will explore the discovery potential of this international effort for observing new physics assuming different nuclear and particle physics theory frameworks, including the exchange of light/heavy neutrinos and supersymmetric models. The impact of efficiencies and systematic uncertainties on the reach of the different experiments will also be discussed and compared.

Speaker: Dr Matteo Agostini (Technical University Munich)

Slides agostini-0vbb-discovery-taup-v2.pdf

249 LEGEND: The future of neutrinoless double-beta decay search with germanium detectors

The observation of neutrinoless double beta ($0\nu\beta\beta$) decay would establish both the violation of lepton number conservation and the Majorana nature of the neutrino. It will also constrain the neutrino mass hierarchy and scale in the light-neutrino exchange mechanism. The current experiments using $^{76}$Ge for $0\nu\beta\beta$ decay search, the $\mathrm{M\small{AJORANA}}$ $\mathrm{D\small{EMONSTRATOR}}$ and $\mathrm{G\small{ERDA}}$, lead the field in both the ultra-low background and the energy resolution achieved. Building on their success, the LEGEND experiment will conduct an improved search with the goal of reaching a half-life sensitivity beyond $10^{28}$ years. In order to achieve this goal, the enriched Ge detector mass has to be increased up to tonne-scale and the backgrounds further reduced. LEGEND will pursue a phased approach with the first phase expected to start in 2021 with about 200 kg of $^{76}$Ge-enriched detectors operating at LNGS of INFN in Italy. The plans and physics reach of LEGEND together with the various ongoing R&D activities will be presented.

Speaker: Dr Anna Julia Zsigmond (Max Planck Institute for Physics)

Slides LEGEND_2019Sept_TAUP_AJZsigmond.pdf

250 CUPID: Cuore Upgrade with Particle ID

CUPID is the next generation Double Beta Decay experiment based on scintillating bolometers. The already developed CUORE infrastructure will become the site in which the new detector will be installed. The technology, successfully tested in LNGS by CUPID-0 and in Modane Laboratory by CUPID-Mo and it, will provide the rejection capability that allows to reduce the background by two orders of magnitude with respect to the CUORE background. This result will be achieved using enriched Li2 100MoO4 crystals for the study of the isotope 100Mo. Moreover, this approach demonstrated a very high energy resolution in the heat signal, 5 keV FWHM at 3 MeV, and a relatively low energy threshold for the light signal, that helps in particles identification. The estimated discover sensitivity of CUPID is of the order of 20 meV for the effective neutrino Majorana mass.

Speaker: Prof. Maura Pavan (Universita di Milano-Bicocca e sez. INFN di Milano-Bicocca)

Slides CUPID_Taup2019_MauraPavan.pdf

Neutrino #18

Convener: Dr Itaru Shimizu (Tohoku University)

251 Impact of theoretical reactor flux uncertainties and of the near detector on the JUNO measurements

In this work we present a detailed study of the theoretical uncertainties of the reactor antineutrino flux for the JUNO experiment, characterising their impact on the mass ordering discrimination and on the precise measurement of the mass-mixing oscillation parameters. We also study how much the high statistics of the near detector JUNO-TAO will improve the JUNO mass ordering discriminating power and we quantify the impact of TAO data on the bounds of oscillation parameters.

Speaker: Prof. Antonio Marrone (University of Bari and INFN Bari)

Slides TAUP2019_Marrone.pdf

252 Design and Status of JUNO

The Jiangmen Underground Neutrino Observatory (JUNO) is a 20 kton multi-purpose liquid scintillator detector currently being built in a dedicated underground laboratory in Jiangmen (PR China). Data taking is expected to start in 2021. JUNO’ s main physics goal is to determin the neutrino mass ordering using electron anti-neutrinos from two nuclear power plants at a baseline of about 53 km. JUNO aims for an unprecedented energy resolution of 3% at 1 MeV for the central detector, with which the mass ordering can be measured with 3 – 4 $\sigma$ significance within six years of operation. Most neutrino oscillation parameters in the solar and atmospheric sectors can also be measured with an accuracy of 1% or better. Furthermore, being the largest liquid scintillator detector of its kind, JUNO will monitor the neutrino sky continuously for contributing to neutrino and multi-messenger astronomy. In this talk JUNO’s design as well as the status of its construction will be presented, together with a short excursion into its rich R&D program.

Speaker: Hans Theodor Josef Steiger (Technische Universität München)

Slides

• TaupJunoSteiger2019.pdf
• TaupJunoSteiger2019.pptx
• TaupJunoSteiger2019small.pdf

253 PHYSICS PROSPECTS OF THE JUNO EXPERIMENT

The Jiangmen Underground Neutrino Observatory is a 20 kton multi-purpose liquid scintillator detector currently being built in China in a dedicated underground laboratory and expected to start data taking in 2021. JUNO's primary physics goal is the determination of the neutrino mass ordering, with an expected significance of 3-4 sigma in six years of data taking, by measuring the oscillation pattern of electron antineutrinos coming from two nuclear power plants at a baseline of 53 km. Besides this fundamental aim, its large target mass, unprecedented energy resolution of 3% at 1 MeV, and vertex reconstruction capability will provide a unique facility for vast opportunities in particle physics and astrophysics. JUNO will have a very rich physics program, which includes the measurement at a sub-percent level of the solar neutrino oscillation parameters, the detection of low-energy neutrinos coming from galactic core-collapse supernova, the measurement of the diffuse supernova neutrino background, the detection of neutrinos coming from the Sun, the Earth and the Earth's atmosphere. Moreover JUNO will be sensitive to searches for nucleon decays and neutrinos resulting from dark matter annihilation in the Sun. In this talk I will give an overview on the JUNO physics potential and discuss the performance of the JUNO detector for the various proposed measurements.

Speaker: Dr Monica Sisti (University of Milano-Bicocca and INFN)

Slides MonicaSisti_TAUP2019.pdf

254 WATCHMAN: A Remote Reactor Monitor and Advanced Instrumentation Testbed

The remote detection of undeclared nuclear reactors, which could be used for production of material used to make nuclear weapons, is a key goal for global nuclear security. To address this challenge, the WATer Cherenkov Monitor for Anti-Neutrinos (WATCHMAN) is beginning construction in Boulby Underground Laboratory, in the UK. WATCHMAN will aim to develop the necessary technology to demonstrate the ability to monitor nuclear reactors at distances of tens of kilometers or farther. The first phase of the experiment aims to build and operate a kiloton-scale gadollinium-doped water Cherenkov detector to detect anti-neutrinos coming from the Hartlepool Nuclear Power Station, located at a distance of 25 km from Boulby. In addition to reactor monitoring, WATCHMAN will also act as an Advanced Instrumentation Testbed for next-generation neutrino detectors. Future upgrades are expected to include novel advancements such as Water-based Liquid Scintillator (WbLS) and Large Area Picosecond PhotoDetectors (LAPPDS). A detailed summary of the project plan and reactor monitoring goals of WATCHMAN, along with possible future detector R&D will be presented.

Speaker: Christopher Grant (Boston University)

Slides WM_TAUP2019_CGrant_reduced.pdf

New Technology #4

255 The search for Majorana neutrinos with a background-free gaseous Xenon TPC at the tonne scale.

The next generation of experiments looking for neutrinoless double beta decay will require detectors with tonne-scale masses and with zero background events in their region of interest. At present there is no technology that has proven to be capable of reaching such background levels. However, improvements in different aspects of the current technologies may allow for a background-free high pressure xenon TPC at this scale. I will present the current R&D efforts in the NEXT Collaboration that will allow for an improved topological identification of the events and for a reduced radioactive budget. In addition I will show recent advances on the possibility of tagging the Barium ion produced in the double beta decay of Xenon. Such tagging would allow for an unambiguous identification of double beta decay.

Speaker: Dr Francesc Monrabal (DIPC)

Slides talk_TAUP2019.pdf

256 Neutron multiplicity in neutrino interactions and new technologies with ANNIE

The Accelerator Neutrino Neutron Interaction Experiment (ANNIE) aims at measuring the neutron abundance in the final state of neutrino-nucleus interactions. This measurement will have a direct impact on our understanding of neutrino interactions and will lead to a better reduction of systematic errors and an improvement of signal-background discrimination in future large neutrino detectors, thus impacting long baseline oscillation experiments as well as proton decay searches and supernova detection. With a volume of about 30 tons of pure water doped with gadolinium to enhance neutron tagging efficiency, ANNIE will provide a measurement of the neutron yield of neutrino interactions as a function of the neutrino energy in the well-characterized Booster Neutrino Beam at Fermilab. The modularity of ANNIE will allow it to perform several fundamental tests of new technologies to be used in neutrino detectors, such as a novel kind of photodetectors called Large Area Picosecond Photodetectors and Water-based Liquid Scintillator, a newly-developed detection medium. The technology behind the ANNIE detector will have a noticeable impact on the development of future large water Cherenkov detectors as well as on detection techniques for neutrino physics. This presentation will describe the construction of the ANNIE detector and the technological capabilities of the next physics phase starting in the fall of 2019.

Speaker: Prof. Weinstein Amanda (Iowa State University)

Slides ANNIE_TAUP2019_2019-09-11.pdf

257 LiquidO: A Novel Neutrino Detection Technology

LiquidO is a new neutrino detection technology which uses opaque, or translucent, liquid scintillator, like milk or paraffine. The scintillation lights are confined within a few cm area by multiple scatterings and are read out by wave length shifting fibers stretched inside. Typical spacing between the fibers are ~cm and the points of origins of the scintillation light emission can be measured with the corresponding space resolution. Low energy (~MeV) neutrinos are identified by detecting electron or positron generated by the charged current interactions, while typical backgrounds are gamma rays or recoiled proton by fast neutron. Those signals have differenct event topologies and can be separated using the spacial pattern of the scintillation light emissions measured by LiquidO. Therefore, strong background rejection and separation of electron neutrino and anti electron neutrino are anticipated by the LiquidO based detector. The LiquidO team has developed a small test system, called micro-liquid and proved the principle of the scintillation light confinement using 1MeV monochlomatic electron beam. Now the team is constructing larger test system, called mini-Liquid, to observe the event pattern. In this talk, the priciple, R&D status and possible applications of the LiquidO technology will be explained.

Speaker: Prof. Fumihiko Suekane (Tohoku Univ.)

Slides 190911_suekane_2.pdf

258 The active Pulse Tube noise cancellation technique of the CUORE experiment

The Cryogenic Underground Observatory for Rare Events (CUORE) experiment at Gran Sasso National Laboratory of INFN searches for neutrinoless double beta decay (0νββ) of $^{130}$Te using 742 kg of TeO$_2$ crystals operated as cryogenic bolometers at ~10 mK [1]. The CUORE cryostat – the today’s biggest milli-Kelvin infrastructure in the world [2] – provides the necessary cooling power at 4 K by means of five Pulse Tube (PT) cryocoolers. The success of the experiment stands on the capability to mitigate the mechanical vibrations injected into the cryostat by the PT pressure waves, which can significantly spoil the detector energy resolution despite standard passive countermeasures such as mechanical decouplers/insulators. In this contribution we present an innovative, simple and effective technique to drive the coherent superposition of the PT pressure oscillations in order to achieve active cancellation of the vibrations transmitted to the detector array. The “active PT noise cancellation” (APTNC) system allows to drastically suppress the detector noise by reducing the noise power at PT fundamental frequency (1.4 Hz) and higher harmonics up to a factor 10$^4$ [3]. The APTNC technique is currently an essential part of the CUORE data taking campaign, which lead to the best limit on the 0νββ half-life of $^{130}$Te to date [4]. This result demonstrates the effectiveness of the method and will ease the development of large cryogen-free systems at milli-Kelvin temperatures for future large-mass bolometric and calorimetric arrays devoted to rare events search. [1] D.R. Artusa et al. (CUORE collaboration), “Searching for neutrinoless double-beta decay of $^{130}$Te with CUORE”, Adv. High Energy Phys. 2015, 879871, 2015 [2] C. Alduino et al., “The CUORE cryostat: a 10-mK infrastructure for large bolometric arrays”, arXiv 1904:05745, accepted by Cryogenics, 2019 [3] A. D’Addabbo et al. “An active noise cancellation technique for the CUORE Pulse Tube Cryocoolers”, Cryogenics, 93:56–65, 2018 [4] C. Alduino et al. (CUORE collaboration), “First Results from CUORE: A Search for Lepton Number Violation via 0νββ Decay of $^{130}$Te”, Phys. Rev. Lett., 120, 132501, 2018

Speaker: Dr Antonio D'Addabbo (GSSI-INFN)

Slides The_active_Pulse_Tube_noise_cancellation_technique_of_the_CUORE_experiment_for_upload.pptx

259 Phonon-Mediated KIDs as Light Detectors for Rare Event Search: The CALDER Project

Background rejection plays a crucial role for experiments searching for rare events, like neutrino-less double beta decay and dark matter interactions. Among the several detection technologies that were proposed to study these processes, cryogenic calorimeters stand out for the excellent energy resolution and the intrinsic radio-purity. Moreover, they can be coupled to a light detector that measures the scintillation or Cherenkov light emitted by interactions in the calorimeter, enabling the identification of the interacting particle by exploiting the different light emission. This feature allows to disentangle signal events from background produced by all the other interactions (mainly alpha particles) that, otherwise, would prevent the achievement of a high sensitivity. The technology for light detection must ensure an RMS noise resolution in the range 20-100 eV, an active surface of several cm$^2$, a fast time response and a high intrinsic radio-purity. Furthermore, the detectors would benefit from high multiplexing capabilities, in order to reduce the number of electronics channels for the read-out, as well as the heat load for the cryogenic apparatus. Finally they must feature a robust and reproducible behaviour, as next generation detectors will need hundreds of devices. In this contribution I will present the results of the CALDER project, a proposed technology for light detection which aim to realise a device with all the aforementioned features for the CUORE experiment upgrade, the CUPID experiment. CALDER takes advantage from the very good energy resolution and from the natural multiplexed read-out provided by Kinetic Inductance Detectors (KIDs). I will show the latest results obtained with the final prototype of light detector and, by exploiting the 10 $\mu$s time response of our KIDs, I will also present for the first time the measurement of the scintillation decay constant at 10 mK of a Li$_2$MoO$_4$ crystal, the selected cryogenic scintillating calorimeter for CUPID.

Speaker: Dr Nicola Casali (INFN-Roma1)

Slides TAUP_CALDER.pdf

260 Reveal the K40 Geoneutrinos

Potassium, K, element is volatile, and its precipitation is not the same as refractory U and Th elements in the Earth. A measurement of the K elements in the Earth is of interest to understand the chemical evolution of the Earth. Furthermore, the discussion on the Ar40-K40 system of the air, and the crust and upper mantle is one of the supports for the depleted and enriched two-layer mantle structure. The detection of K40 neutrinos may lead to new knowledge of the Earth. Previously only U and Th geoneutrinos can be detected with the inverse beta process with a 1.8 MeV threshold. K40 geoneutrinos are hard to discover for its low energy and high solar neutrino background. In this work we found that Liquid scintillator Cherenkov neutrino detectors can be used to detect the K40 geoneutrinos. Liquid scintillator Cherenkov detectors feature both energy and direction measurement for charge particles. With the elastic scattering process of neutrinos and electrons, K40 geoneutrinos can be detected without any intrinsic physical threshold. With the directionality, the dominant intrinsic background originated from solar neutrinos in common liquid scintillator detectors can be suppressed. With the studies of MeV electrons Geant4 simulation, quantum and detection efficiency, and Cherenkov direction reconstruction algorithm, it is found that we can detected K40 energy geoneutrinos with 3 standard deviations with a kilo-ton scale detector. We are on the cutting edge to reveal this geoneutrino component in the near future. The result and relevant features will be reported.

Speaker: Dr Zhe Wang (Tsinghua University)

Slides Hunting-K40-geoneutrinos.pdf

Thursday, September 12

261 Neutrino theory

Speaker: Dr Eligio Lisi (INFN-Bari)

Slides PLENARY_VII_ELIGIO_LISI.pdf

262 Neutrino Oscillation experiments

Speaker: Dr Hirohisa Tanaka (SLAC, Stanford Univ.)

Slides PLENARY_VII_HirohisaTanaka_TAUP.pdf

263 Sterile neutrino

Speaker: Dr David Caratelli (Fermilab)

Slides PLENARY_VII_Caratelli_TAUP2019.pdf

10:30 AM Coffee break

264 Solar neutrinos

Speaker: Dr Kai Zuber (TU-Dresden)

Slides PLENARY_VIII-Zuber.pdf

265 Geo neutrinos

Speaker: Dr Hiroko Watanabe (Tohoku Univ.)

Slides PLENARY_VIII_HirokoWatanabe.pdf

266 Supernova neutrino

Speaker: Dr Evan O'Connor (Stockholm Univ.)

Slides Web_PLENARY_VIII_OCONNOR.pdf

Cosmology #3

Convener: Prof. Masahiro Kawasaki (ICRR, University of Tokyo)

267 Cosmology with Fermi-LAT

The light emitted by all galaxies across the history of the Universe is encoded in the intensity of the extragalactic background light (EBL), the diffuse cosmic radiation field at ultraviolet, optical, and infrared wavelengths. The EBL is a source of opacity for high-energy gamma rays via pair production, leaving a characteristic attenuation imprint in the spectra of distant gamma-ray sources. In this talk, I will report on a new measurement of the EBL using gamma-ray data from both the Large Area Telescope on board the Fermi Gamma-ray Space Telescope and ground-based Imaging Atmospheric Cherenkov Telescopes. This unprecedented measurement has allowed us to derive the cosmic star-formation history, the number density of faint galaxies during the re-ionization epoch, and also the expansion rate of the Universe and its matter content, all of this using independent and complementary methodologies to existing ones.

Speaker: Dr Alberto Dominguez (Universidad Complutense de Madrid)

Slides TAUP.pdf

268 Multiwavelength studies of the epoch of reionization

Reionization is a unique epoch in Cosmology and studies of the epoch of reionization (EoR) can tell us important information about ionization history, first luminous objects, and structure formation in the early Universe. However, the EoR is still poorly understood so far. In light of this, we investigate to what extent experiments observing at different wavelengths can detect the EoR signatures that could be produced by various physical processes, such as scattering between photons of the cosmic microwave background and free electrons that were stripped from neutral hydrogen atoms by ultraviolet radiation, stellar emission from the primeval objects and 21 cm emission from the neutral hydrogen content surrounding the ionizing regions. In this talk, I will show a few newly developed techniques for detecting the EoR signatures at different wavelengths.

Speaker: Dr Chang Feng (University of Illinois at Urbana-Champaign)

Slides TAUP2019_ChangFeng.pdf

269 Gravitational Waves from Phase Transition in a QCD-like hidden sector

In this talk, we will discuss the testability of a scale invariant extension of the standard model with a QCD-like hidden sector by using the gravitational wave (GW) signal. The scale invariance is dynamically broken by the non-perturbative effects, which can be used to explain the origin of masses of the Higgs boson and the dark matter. In a certain region of the parameter space, the chiral phase transition in the QCD-like hidden sector is of first order. We will estimate the GW signal from the phase transition and show the parameter points which predict a sizable GW signal by future space based detectors.

Speaker: Dr Mayumi Aoki (Kanazawa U.)

Slides TAUP_AOKI.pdf

270 Gravitational Waves Induced by Scalar Perturbations during a Gradual Transition from an Early Matter Era to the Radiation Era

We revisit the effects of an early matter dominated era on gravitational waves induced by scalar perturbations. We carefully take into account the evolution of the gravitational potential, the source of these induced gravitational waves, during a gradual transition from an early matter dominated era to the radiation dominated era, where the transition timescale is comparable to the Hubble time at that time. Realizations of such a gradual transition include the standard perturbative reheating with a constant decay rate. Contrary to previous works, we find that the presence of an early matter dominated era does not necessarily enhance the induced gravitational waves due to the decay of the gravitational potential around the transition from an early matter dominated era to the radiation dominated era. This talk will be based on our paper, arXiv:1904.12878.

Speaker: Mr Keisuke Inomata (ICRR, The University of Tokyo)

Slides TAUP_2019_0912_inomata_pdf.pdf

271 Enhancement of Gravitational Waves Induced by Scalar Perturbations due to a Sudden Transition from an Early Matter Era to the Radiation Era

We study gravitational waves induced from the primordial scalar perturbations at second order around the reheating of the Universe. We consider reheating scenarios in which a transition from an early matter dominated era to the radiation dominated era completes within a timescale much shorter than the Hubble time at that time. We find that an enhanced production of induced gravitational waves occurs just after the reheating transition because of fast oscillations of scalar modes well inside the Hubble horizon. This enhancement mechanism just after an early matter-dominated era is much more efficient than a previously known enhancement mechanism during an early matter era, and we show that the induced gravitational waves could be detectable by future observations if the reheating temperature $T_{\text{R}}$ is in the range $T_\text{R}$ \lesssim $7\times 10^{-2} \, \text{GeV}$ or $20 \, \text{GeV}$ \lesssim $T_\text{R}$ \lesssim 2 $\times 10^7 \, \text{GeV}$. This is the case even if the scalar perturbations on small scales are not enhanced relative to those on large scales, probed by the observations of the cosmic microwave background. This talk will be based on our paper, arXiv:1904.12879.

Speaker: Dr Takahiro Terada (KEK)

Slides Terada_GW_enh_TAUP.pdf

DM15: Accelerator Searches for Dark Matter

Convener: Prof. Shigetaka Moriyama (ICRR, The University of Tokyo)

272 Light Fermionic Dark Matter with Light Scalar Mediator

A light fermionic weakly interacting massive particle (WIMP) dark matter is investigated by studying its minimal renormalizable model, where it requires a scalar mediator to have an interaction between the WIMP and standard model particles. We perform a comprehensive likelihood analysis of the model involving the latest but robust constraints and those will be obtained in the near future. In addition, we pay particular attention to properly take the kinematically equilibrium condition into account. It is shown that near-future experiments and observations such as low-mass direct dark matter detections, flavor experiments and CMB observations play important roles to test the model. Still, a wide parameter region will remain even if no WIMP and mediator signals are detected there. Future lepton colliders will significantly test this remaining region.

Speaker: