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Agenda
for the parallel workshop sessions in Low-Energy Neutrinos (Geo, Solar, Supernova).
All links marked with a⇓ can be used to show/hide the abstracts and presentations.
Click here to show/hide all presentations and abstracts and here for a print version.
You may also download the compact program booklet (PDF, 1.9 MB)
and an abstract booklet (PDF, 0.4 MB).
As long as authors provided us with PDF versions of their slides, the corresponding downloads are available on this page.
Monday – Sep 5, 2011
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14:30 – 16:20 |
Low-Energy Neutrinos W1
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Parallel Session (Clubraum 3) – Chair:
Walter Potzel
14:30
(15' + 5')
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Testing the sterile neutrino hypothesis at the solar sector⇓
slides
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Antonio Palazzo (TU München)
Non-negligible mixing among active
neutrinos and new sterile species has been put forward as a possible solution of old and new neutrino data anomalies. Such a hypothesis can be tested looking at various neutrino data sets. Here we investigate the imprints of sterile neutrinos on the solar sector data, showing that they can provide very stringent constraints on such exotic particles.
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14:50
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Precision measurement of the 7Be solar neutrino flux and its day-night asymmetry with Borexino⇓
slides
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Barbara Caccianiga (INFN Milano)
We present the most recent results published by Borexino, the only experiment able to detect in real-time solar neutrinos below 1 MeV. We measure the flux of 7Be solar neutrinos with a total error below 5% and its day-night asymmetry with an error of ~1%. Compared with the latest SSM predictions our measurement rejects the no-oscillation hypothesis at 4.9σ and provides a precise measurement of the survival probability in the vacuum dominated oscillation regime. We find a 7Be day-night asymmetry consistent with zero within the error. We show that this result alone is able of rejecting the LOW solution at more than 8.5σ. Combined with the other solar neutrino data it isolates the LMA-MSW solution at Δχ2>190 without using KamLAND anti-neutrino data.
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15:10
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Final results from the Sudbury Neutrino Observatory⇓
slides
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Nikolai Tolich (University of Washington)
The Sudbury Neutrino Observatory (SNO) was designed to solve the so-called solar neutrino anomaly by measuring the total flux of active neutrinos from the Sun. By measuring the number of neutrinos detected as the electron type, SNO was able to measure neutrino oscillation parameters. By making precise measurements of both the solar neutrino oscillation parameters and the flux of neutrinos from 8B decay in the Sun, the SNO collaboration could shed light on some remaining mysteries about neutrino oscillations and solar fusion. I will present the results of this final reanalysis of the SNO data.
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15:30
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Scintillator phase of the SNO+ experiment⇓
slides
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Valentina Lozza (TU Dresden)
The SNO+ experiment is the follow up of the SNO experiment, replacing the heavy water volume with about 1000 tons of liquid scintillator (LAB) in order to shift the sensitive threshold to the low energy range. The 6000 m.w.e. natural rock shielding, and the use of ultra-clean materials makes the detector suitable for neutrinos studies. The main physical goals are the detection of pep and CNO solar neutrinos, geo-neutrinos, the possible observation of neutrinos from supernova and the study of reactor oscillations. Complementing this neutrino program, SNO+ will also search for 150Nd (5.6% abundance) neutrinoless double beta decay, loading the liquid scintillator with 0.1% natural Neodymium. After a review of the general SNO+ setup, the physics of the solar neutrino phase will be presented.
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15:50
(12' + 3')
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Measuring the pep and CNO neutrinos with Borexino⇓
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Cristian Galbiati (Princeton University)
Borexino is a low-background liquid scintillator detector, designed to measure the flux of sub-MeV solar neutrinos. The collaboration is currently working on determining the rates of the CNO and pep solar neutrinos. Knowledge of the CNO neutrino rate is critical to addressing the Solar Metallicity Problem, while the pep neutrinos are an excellent probe of the vacuum-matter transition region in the LMA-MSW solution. The main challenge for these measurements is the characterization and removal of cosmogenic and radiogenic background. I will present the current status of the pep and CNO neutrino analyses, discussing the recent purification campaign as well as several data analysis techniques that have been developed to significantly reduce the cosmogenic 11C background.
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16:05
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A step toward CNO solar neutrinos detection in liquid scintillators⇓
slides
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Francesco Villante (Università dell' Aquila and INFN-LNGS)
The detection of CNO solar neutrinos in ultrapure liquid scintillator detectors is limited by the background
produced by Bismuth-210 nuclei that undergo beta-decay to Polonium-210 with a lifetime of about 7 days.
Polonium-210 nuclei are unstable and decay with a lifetime equal to about 200 days emitting alpha-particles
that can be also detected.
We propose to determine the Bi-210 background by looking at the time evolution of alpha-decay rate of Po-210. A sufficient accuracy can be obtained in a relatively short time. As an example, if the initial Po-210 event rate is 2000cpd/100 ton or lower, a Borexino-like detector could start discerning CNO neutrino signal from Bi-210 background in about 1 yr.
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Tuesday – Sep 6, 2011
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14:30 – 16:20 |
Low-Energy Neutrinos W2
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Parallel Session (Clubraum 3) – Chair:
Aldo Ianni
14:30
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Towards a refined reference Earth model for geo-neutrinos⇓
slides
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Fabio Mantovani (INFN Ferrara)
Geo-neutrino data from KamLAND and Borexino provide insights into Earth’s energetics and radiogenic heat production. In 2013, SNO+ will begin to collect data; the era of the exploration of our planet through geo-neutrinos is open. One aim is to discriminate among models for the bulk composition of the Earth, which are based on cosmochemical arguments and geochemical and geophysical observations. In order to determine the U and Th concentration of the deep Earth with geo-neutrinos, the regional crustal contribution to the geo-neutrino flux needs to be determined from detailed geological studies. We are developing an improved reference model for the crust and lithospheric mantle using new compilations of geochemical data for sediments, oceanic and continental crust. The expected geo-neutrino signal and its uncertainties have been calculated for detectors at several locations.
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14:50
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Low energy neutrino physics at KamLAND⇓
slides
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Hiroko Watanabe (Tohoky University)
The KamLAND experiment has many scientific motivations of low energy neutrino physics. I will present recent results of KamLAND neutrino analysis such as supernova relic neutrino limits, geo neutrinos and solar neutrinos, etc.
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15:10
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Antineutrino studies with Borexino detector⇓
slides
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Oleg Smirnov (Joint Institute for Nuclear Research)
Spectral contributions corresponding to two known anti-neutrino sources were observed by Borexino: νe produced in nuclear reactors and geo-neutrinos. Presence of geo-neutrino signal is confirmed at 99.997% c.l. and 99.6% c.l. is reported for exclusion of no-oscillations hypothesis for the reactor neutrino on the average base of 1000 km. An upper limit of 3 TW at 90% c.l. has been established for the power of hypothetical geo-reactor. A sensitive search for other possible anti-neutrino sources has been performed, including the search for solar anti-neutrinos and other, unspecified and model-independent νe fluxes.
New data have been accumulated by Borexino since the last release, their impact on the geo-neutrino and reactor antineutrino studies will be discussed.
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15:30
(12' + 3')
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Final results of neutrino-electron scattering cross-section measurements and constraints on new physics⇓
slides
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Henry Wong (Academia Sinica)
The antineutrino-electron elastic scattering cross-section was measured with a CsI(Tl) scintillating crystal array having a total mass of 187 kg. The detector was exposed to an average reactor neutrino flux of 6.4x1012 cm-2s-1 at the Kuo-Sheng Nuclear Power Station in Taiwan.
We will present final resuls with 29882/7369 kg-days of Reactor ON/OFF data, on the cross-section and the standard electroweak parameters, weak mixing angle and (gV,gA) measurements, the test on charged-current neutral-neutral interference, as well as limits on neutrino magnetic moments and charge radius squared.
We will also present constraints on NSI and Unparticle Physics (UP) in antineutrino-electron interaction channel based on this data set as well as our previos data sets with ULE-HP Ge detectors.
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15:45
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Neutrino electromagnetic properties and new bounds on neutrino magnetic moments⇓
slides
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Alexander Studenikin (Moscow State University & JINR (Dubna))
A short review on neutrino electromagnetic properties is presented. In particular, developments in studies, both theoretical and experimental, of neutrino magnetic moments are discussed. The recent claim that through an enhancement of the neutrino magnetic moment scattering cross section, due to atomic ionization effects in Ge detectors, there is a significant improvement of the best upper limit for the neutrino magnetic moment is critically analyzed.
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16:00
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Detecting extragalactic supernova neutrinos in the ice of the South Pole⇓
slides
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Marek Kowalski (University of Bonn)
With current neutrino detectors and a rate of 2 galactic SNe per century, awaiting the next SN discovery requires patience. The perspective changes instantly, once the sensitivity of neutrino detectors reaches a scale allowing the detection of SNe in neighboring galaxies. A low-energy neutrino detector of 10 Mton mass would deliver several SN detections per year, thereby opening enormous new scientific opportunities. In this talk we describe the motivation, along with detector concepts, that utilize the clear ice at the South Pole and have the potential to reach the required sensitivity in a cost effective manner. This work is part of a set of R&D studies done in conjunction with PINGU (Phased IceCube Next Generation Upgrade), an upgrade to IceCube that will be proposed in the near future.
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Wednesday – Sep 7, 2011
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14:30 – 16:15 |
Low-Energy Neutrinos W3
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Parallel Session (Clubraum 3) – Chair:
Michael Wurm
14:30
(15' + 5')
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Site selection for the new generation of giant neutrino detectors⇓
slides
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Wladyslaw Henryk Trzaska (University of Jyväskylä)
SuperK is one of the most successful experiments of modern physics. Its success was possible thanks to the large mass. To go even further one needs an order of magnitude improvement either in size or through improved detection techniques. LAGUNA offers a realistic path towards that goal. The recently completed Design Study has investigated 7 potential sites and 3 detector options: GLACIER, LENA, and MEMPHYS. The project has now entered the second phase where it will determine the full cost of construction, commissioning and long-term operation of the infrastructure, and assess the use of CERN beams for long baseline neutrino physics. The talk will summarize the findings of the Design Study concerning the advantages of each site and discuss the main physics arguments favoring each selection
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14:50
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Future neutrino physics with LENA (Low Energy Neutrino Astronomy)⇓
slides
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Jürgen Winter (TUM)
Taking advantage of the high potential of liquid-scintillator detectors (LSDs), the proposed LENA detector hopes to follow in the footsteps of the Borexino and KamLAND experiments. LSDs feature low-energy threshold, good energy resolution, and efficient background discrimination. LENA's large mass of 50 kt allows for high-statistic measurements of astrophysical and terrestrial low-energy neutrino sources such as the Sun, galactic Supernovae, and the interior of our Earth. Moreover, the observation of the Diffuse Supernova Background (DSNB) and $\nu$s from Dark Matter annihilation seem feasible. New limits might be put on the lifetime of the $K^+\bar\nu$ proton decay channel. As shown in simulations, LENA has remarkable prospects concerning long-baseline neutrino oscillation experiments.
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15:10
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The Memphys experiment⇓
slides
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Thomas Patzak (University Paris Diderot)
MEMPHYS is a proposed 0.5 Mton scale Water Cherenkov experiment to be performed deep underground. Possible sites are under study in the European FP7 design studis LAGUNA and LAGUNA-LBNO. Memphys is a very large multipurpose next- generation neutrino observatory dedicated to nucleon decay, neutrinos from supernovæ, solar and atmospheric neutrinos, as well as neutrinos from a future Super-Beam or β-Beam to measure the mixing angle θ13, the CP violating phase δ and the mass hierarchy. A small- scale prototype, Memphyno, has been constructed with the purpose of serving as a test bench for new photodetection and data acquisition solutions, such as grouped readout systems. The physics potential of the 500 k ton water Cherenkov detector will be demonstrated.
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15:30
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Towards GLACIER, a giant liquid argon TPC detector⇓
slides
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André Rubbia (ETH Zürich)
GLACIER is a proposed giant liquid argon multipurpose next-generation neutrino observatory at the 100 kton scale, dedicated to long baseline neutrino studies for the neutrino mass hierarchy determination and mixing
angle θ13 and CP violating phase δ measurements, to nucleon decay searches and to known and unknown astrophysical neutrino detection. It is one of the three detector options considered in the European FP7 design studies LAGUNA
and LAGUNA-LBNO. A very attractive feature is the ability to measure
interactions with very high precision and granularity thanks to the charge
imaging technology. Technical developments have been proposed to reach the required mass scale. Several detector prototypes have been assembled and operated. We will report on the physics potential of such an observatory and describe the current state of the project.
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15:50
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About a possibility of measuring the central temperature of the sun through the regeneration of the 7Be neutrinos in the Earth⇓
slides
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Ara Ioannisian (Yerevan Physics Institute)
The solar neutrino's 7Be line (Eν=0.862 MeV) has a width of an order of the temperature in the center of the Sun (approx. 1keV).The regeneration of the electron neutrinos from remote structures of the Earth is suppressed due to the averaging of the effect over the width of the 7Be line (oscillation dyeing effect). We discuss a possibility of measuring the width of the beryllium neutrino's line at large liquid scintillator detector (LENA) by measuring the regenerated neutrino flux.
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16:05
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Potential of the Andes underground laboratory for neutrino geophysics and astrophysics⇓
slides
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Renata Zukanovich Funchal (Universidade de São Paulo)
Recently the construction of an underground laboratory inside the Agua Negra tunnel in the Andes between Argentina and Chile has been proposed. If constructed, it will be the first
under ground laboratory for particle physics and astrophysics in the Southern Hemisphere. In this talk we will discuss the potential advantages of a neutrino detector placed in this laboratory to contribute to geophysics by measuring geoneutrinos and to astrophysics by measuring neutrinos coming from Galactic core collapse supernova.
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Thursday – Sep 8, 2011
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16:50 – 18:35 |
Low-Energy Neutrinos W4
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Parallel Session (Millerzimmer) – Chair:
Amol Dighe
16:50
(15' + 5')
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Development of InP solid state detector and liquid scintillator contaning metal complex for measurement of pp/7Be solar neutrinos and neutrinoless double beta decay⇓
slides
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Yoshiyuki Fukuda (Miyagi University of Education)
A large volume radiation detector using a semi-insulating Indium Phosphide (InP) photodiode has been developed for measurement of pp/7Be solar neutrinos. This detector was designed to measure both electron emitted from neutrino capture of 115In and scintillation light from liquid xenon interacted by gammas emitted by the excited state of 115Sn. For another possibility for the observation of pp/7Be and the neutrinoless double beta decay experiment, we have also developed an organic liquid scintillator which contains 8-quinolinolate indium and zirconium complex, respectively. Here we report the performance of InP detector and the gamma-ray induced luminescence of liquid scintillator with metal complexes.
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17:10
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The detection of supernova neutrinos⇓
slides
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Kate Scholberg (Duke University)
When a massive star collapses at the end of its life, nearly all of the gravitational binding energy of the resulting remnant is released in the form of neutrinos. The burst of neutrinos from a Galactic core collapse
supernova will be detected in neutrino detectors worldwide. This talk will cover supernova neutrino detection techniques in general, current supernova
neutrino detectors, prospects for specific future experiments, and outstanding questions for experimentalists and theorists to address in order to get the most from
the next Galactic supernova burst.
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17:30
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New possibilities in supernova accretion phase from dense matter effect.⇓
slides
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Sovan Chakraborty (II. Institute for Theoretical Physics, Hamburg University)
The accretion phase in Supernova (SN) emits large neutrino (nu) fluxes with distinct flavor hierarchy, offering the best detection opportunity of flavor oscillations. We study the possibility of SN neutrino oscillations in the accretion phase, using recent neutrino radiation hydrodynamics simulation. In contrast to what expected with only nu-nu interactions, the multi-angle effects associated with the dense ordinary matter suppress the collective oscillations in the accretion phase for a typical iron core SN. This suppression of oscillation implies the negligible role of flavor evolutions in neutrino heating and explosion dynamics. Moreover accretion phase signal from a galactic SN, with MSW in SN mantle and Earth matter, can reveal neutrino mass hierarchy, in the large θ13 limit.
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17:50
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Sterile neutrinos in supernovae⇓
slides
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Irene Tamborra (Max Planck Institute for Physics)
Motivated by the recent hints for sterile neutrinos coming from reactor anomalies and cosmology, we discuss active-sterile conversions in supernovae. By including the feedback effect on the electron abundance due to neutrino oscillations, we study the impact of sterile neutrinos on both the oscillated neutrino fluxes and the rapid neutron capture process.
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18:10
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Possible trace of neutrino non-standard interactions in the supernova⇓
slides
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João Pulido (CFTP - IST Universidade Técnica de Lisboa)
Neutrino non-standard interactions (NSI), previously introduced for the sun, are studied in the supernova context. The decay into antineutrinos, which has been shown to be implied by dense matter, cannot be seen experimentally, owing to the smallness of the antineutrino production probability. The effect that may be visible and providing a clear indication of NSI is the possible appearance of a significant electron neutrino event rate in the low energy range below 0.8 MeV.
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18:30
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Search for supernova relic neutrinos at Super-Kamiokande⇓
slides
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Kirk Bays (University of California, Irvine)
The diffuse supernova relic neutrino signal has never been observed. Currently the world's best upper flux limit comes from a search for inverse beta decay of anti-neutrinos in the Super-Kamiokande (SK) detector. A new SK study utilizes a novel method of spallation tagging, improved event selection, and an expanded data set to lower the analysis energy threshold and improve overall accuracy. Full results of this new study (including a combined upper flux limit of 2.6-2.8 &nue events cm-2 s-1, Enu > 17.3 MeV) will be presented, as well as a short update on the research and development of using Gadolinium for neutron tagging.
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