BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Radio Detection of the Highest Energy Neutrinos DTSTART:20150504T143000Z DTEND:20150504T150000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4092@events.icecube.wisc.edu DESCRIPTION:Speakers: Abigail Vieregg (o=research\,ou=Institutions\,dc=ice cube\,dc=wisc\,dc=edu)\n\nUltra-high energy neutrino astronomy sits at the boundary between particle physics and astrophysics. Through neutrino ast rophysics\, we can probe the nature of the ultra-high energy universe in a unique way and test our understanding of particle physics at energies muc h greater than those achievable at particle colliders. The future of ultr a-high energy neutrino detection lies with ground-based radio arrays\, whi ch would represent an enormous leap in sensitivity. I will discuss design s and plans for radio detection experiments that would discover cosmogenic neutrinos (peaking at ~100 PeV) even in the most pessimistic of GZK produ ction models\, and how to design a detector that would extend the IceCube detection of PeV astrophysical neutrinos to higher energies by using a rad io phased array.\n\nhttps://events.icecube.wisc.edu/event/68/contributions /4092/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4092/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrinos from Gamma Ray Bursts in the IceCube and ARA Era DTSTART:20150505T140000Z DTEND:20150505T142500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4093@events.icecube.wisc.edu DESCRIPTION:https://events.icecube.wisc.edu/event/68/contributions/4093/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4093/ END:VEVENT BEGIN:VEVENT SUMMARY:IceCube Present and Future DTSTART:20150504T140000Z DTEND:20150504T142500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4094@events.icecube.wisc.edu DESCRIPTION:Speakers: Olga Botner (Uppsala university)\n\nhttps://events.i cecube.wisc.edu/event/68/contributions/4094/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4094/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino Astronomy in the Mediterranean: Past\, Present and Future DTSTART:20150504T150000Z DTEND:20150504T153000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4095@events.icecube.wisc.edu DESCRIPTION:Speakers: Ronald Bruijn (Universiteit van Amsterdam/Nikhef)\n\ nEfforts to exploit the waters of the Mediterranean Sea for neutrino \nast ronomy have been ongoing for about two decades. After a brief recognition of early history\, some recent results of Antares will be presented\, with a focus on the complementarity to the IceCube neutrino observatory. The A ntares neutrino telescope has demonstrated that a nanosecond precision tim ing combined with the good optical properties of sea water can lead to hig h-precision all-flavour neutrino astronomy.\nThe first phase of a new gene ration deep-sea neutrino\ntelescope\, KM3NeT\, is being constructed and wi ll consist\nof 24 800 m high detection units\, instrumented with 18 multi- PMT Digital Optical Modules (DOMs). The innovative design of the DOMs all ow for good photon counting capabilities and a large angular acceptance. S ubsequent phases (ARCA\, phase-2) are foreseen to culminate in a multi-cu bic kilometer scale neutrino detector in the Mediterranean. Current progre ss\, including results from prototype lines\, will be presented.\n\nhttps: //events.icecube.wisc.edu/event/68/contributions/4095/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4095/ END:VEVENT BEGIN:VEVENT SUMMARY:Signatures of dark matter sterile neutrinos in core-collapse super novae DTSTART:20150505T192300Z DTEND:20150505T194500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4096@events.icecube.wisc.edu DESCRIPTION:Speakers: MacKenzie Warren (University of Notre Dame)\, Grant Mathews (University of Notre Dame)\, Toshitaka Kajino (National Astronomic al Observatory of Japan)\, Jun Hidaka (National Astronomical Observatory o f Japan)\, Matthew Meixner (University of Notre Dame)\n\nThe nature of dar k matter and the explosion mechanism of core-collapse supernovae may both be explained by the presence of a sterile neutrino. Observations of galaxi es and galaxy clusters are indicative of a $\\sim$keV mass sterile neutrin o. Oscillations between an electron neutrino and a sterile neutrino in the $\\sim$keV mass range may provide an efficient energy transport mechanism between the proto-neutron star and stalled shock wave. We have performed simulations of core-collapse supernovae for a range of sterile neutrino ma sses and mixing angles that are consistent with dark matter. We have found that\, for many choices of mass and mixing angle\, the presence of a ster ile neutrino is sufficient to enhance the neutrino reheating and result in a successful explosion.\n\nhttps://events.icecube.wisc.edu/event/68/contr ibutions/4096/ LOCATION:Northwoods\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4096/ END:VEVENT BEGIN:VEVENT SUMMARY:Coherent Elastic Neutrino-Nucleus Scattering (CEvNS) DTSTART:20150505T191800Z DTEND:20150505T193600Z DTSTAMP:20261014T080200Z UID:indico-contribution-4097@events.icecube.wisc.edu DESCRIPTION:Speakers: Robert Cooper (Indiana University)\n\nLow-energy neu trinos can have de Broglie wavelengths that are larger than target nuclei. \nAt these energies\, coherent elastic neutrino-nucleus scattering (CEvNS ) is predicted to be the dominant interaction\, yet it remains unseen. \nM easuring CEvNS is difficult because elastic scattering deposits very littl e energy in a detector and neutron backgrounds are difficult to control\, especially at accelerators. \nNevertheless\, a discovery measurement is th e first part in a larger program to use the CEvNS interaction to understan d supernova dynamics and detection\, probe the weak interaction\, and sear ch for non-standard interactions and neutrino magnetic moments. \nIn this talk\, I will highlight the physics motivations for measuring CEnuNS and t wo experimental efforts to discover it at accelerators. \nThe CENNS colla boration plans to use a large liquid argon detector near the Fermilab Boos ter Neutrino Beam in a far-off-axis configuration\, and the COHERENT colla boration will use a number of low-energy-threshold detector technologies t o measure CEvNS in a basement location at the Oak Ridge National Laborator y Spallation Neutron Source.\n\nhttps://events.icecube.wisc.edu/event/68/c ontributions/4097/ LOCATION:WI Idea (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4097/ END:VEVENT BEGIN:VEVENT SUMMARY:Implications of IceCube's neutrino discoveries for ultrahigh-energ y cosmic rays DTSTART:20150505T221200Z DTEND:20150505T222400Z DTSTAMP:20261014T080200Z UID:indico-contribution-4098@events.icecube.wisc.edu DESCRIPTION:Speakers: Matt Kistler (Stanford University)\n\nThe discovery by IceCube of the first high-energy neutrinos with plausible extraterrestr ial origins is likely informing us about some of the most extreme environm ents in the Universe. I will discuss from a theoretical perspective what this new flux has already told us about the inner workings of the sources of extragalactic cosmic rays. Additionally\, I will touch upon connection s with a variety of other observations along with how these can be strengt hened in coming years.\n\nhttps://events.icecube.wisc.edu/event/68/contrib utions/4098/ LOCATION:Union South URL:https://events.icecube.wisc.edu/event/68/contributions/4098/ END:VEVENT BEGIN:VEVENT SUMMARY:Muon-Induced Backgrounds in DM-Ice NaI(Tl) Dark Matter Detectors DTSTART:20150505T201500Z DTEND:20150505T203000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4099@events.icecube.wisc.edu DESCRIPTION:Speakers: Antonia Hubbard (University of Wisconsin\, Madison)\ n\nDM-Ice is a NaI(Tl) experiment searching for an annually-modulating dar k matter signal. The DM-Ice17 detector has successfully operated in the So uth Pole ice for three years\, and R&D efforts for the full-scale detector are underway at FNAL and the Boulby Underground Laboratory. I present an analysis of the muon background in DM-Ice\, including long-lived phosphore scence observed in both DM-Ice17 and DM-Ice37. The DM-Ice17 muon analysis also includes events that are coincident with IceCube. The expected annua l modulation in the rate of muons is observed.\n\nhttps://events.icecube.w isc.edu/event/68/contributions/4099/ LOCATION:Northwoods\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4099/ END:VEVENT BEGIN:VEVENT SUMMARY:Star-Forming Galaxies as Sources of High Energy Neutrinos DTSTART:20150505T220000Z DTEND:20150505T222000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4100@events.icecube.wisc.edu DESCRIPTION:Speakers: Tova Yoast-Hull (University of Wisconsin-Madison)\, J. S. Gallagher (University of Wisconsin-Madison)\, Ellen Zweibel (UW-Madi son)\n\nWe discuss the production of high energy neutrinos and gamma-rays in intensely star-forming galaxies. With our semi-analytic physical model of cosmic ray interactions\, we analyze the radio and gamma-ray propertie s of nearby starburst galaxies using simplified astrophysical assumptions. Key physical processes in the models include pion production & decay\, i nverse Compton scattering\, photon-photon interactions\, and synchrotron e mission. Results for nearby starburst galaxies demonstrate the utility of the model in predicting cosmic ray interaction rates and the subsequent p roduction of energetic particles. These results also establish that even the most extreme star-forming systems are unlikely to be point sources of neutrinos\, unless their cosmic ray spectrum flattens at high energies.\n\ nhttps://events.icecube.wisc.edu/event/68/contributions/4100/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4100/ END:VEVENT BEGIN:VEVENT SUMMARY:Measurement of Muon Neutrino Disappearance with IceCube/DeepCore DTSTART:20150505T211500Z DTEND:20150505T213000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4101@events.icecube.wisc.edu DESCRIPTION:Speakers: Matt Dunkman (o=psu\,ou=Institutions\,dc=icecube\,dc =wisc\,dc=edu)\n\nNew event reconstruction techniques have resulted in a h igh statistics atmospheric neutrino sample from the first three years of d ata from the complete IceCube Neutrino Observatory. The more densely instr umented DeepCore sub-array\, with an energy threshold around 10 GeV\, is v ery sensitive to the first atmospheric oscillation minima. I will present the current constraints on oscillation parameters $\\theta_{23}$ and $\\De lta m_{32}$ from IceCube.\n\nhttps://events.icecube.wisc.edu/event/68/cont ributions/4101/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4101/ END:VEVENT BEGIN:VEVENT SUMMARY:Waxman and Bahcall meet Auger in a single energy bin DTSTART:20150504T203000Z DTEND:20150504T205000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4102@events.icecube.wisc.edu DESCRIPTION:Speakers: Luis Anchordoqui (City University of New York)\, Pie rre Auger Collaboration (Av. San Mart ́ın Norte 306\, 5613 Malargu ̈e\, Mendoza\, Argentina)\n\nCosmic neutrinos with energies near 10^9 GeV and above are detectable with the Surface Detector array of the Pierre Auger O bservatory. We report here on searches through Auger data from 1 January 2 004 until 20 June 2013. No neutrino candidates were found\, yielding a lim it to the diffuse flux of ultra-high energy neutrinos that challenges the Waxman-Bahcall benchmark predictions.\n\nhttps://events.icecube.wisc.edu/e vent/68/contributions/4102/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4102/ END:VEVENT BEGIN:VEVENT SUMMARY:The Ordinary and the Wondrous: Neutrinos from Star-Forming Galaxie s and from Extraterrestrial Megaprojects DTSTART:20150505T200900Z DTEND:20150505T203200Z DTSTAMP:20261014T080200Z UID:indico-contribution-4103@events.icecube.wisc.edu DESCRIPTION:Speakers: Brian Lacki (Institute for Advanced Study)\n\nStar-f orming galaxies (SFGs) are among the most numerous extragalactic sources. I describe my results in calculating the extragalactic radiation from SFG s at all energies. I construct very simple models of galaxies using empir ical relations like the Schmidt law to estimate the properties of galaxies \, and then use basic one-zone models of radiative transfer to calculate t he stellar\, dust\, supernovae\, and nonthermal emission. My approach all ows for a self-consistent calculation that allows me to compare the energe tics of the gamma-ray and TeV/PeV neutrino backgrounds with the UV/IR and the MeV supernova neutrino backgrounds. I discuss the energetics issues t hat make it hard for SFGs to explain all of the IceCube PeV neutrino backg round.\n\nExtraterrestrial beings (ETs) are among the most spectacular pos sible discoveries imaginable. If ETs wish to experimentally test Grand Un ified or Planck scale physics\, they could end up building particle accele rators bigger and brighter than stars. These could radiate high energy ne utrinos\, perhaps of far higher energy than ultra high energy cosmic rays. I describe current limits on Planck energy neutrinos from experiments an d an indirect "W-burst" limit\, and consider how we might build a much big ger effective YeV neutrino detection experiment. These limits indicate th at particle accelerators (natural or artificial) with galaxy-scale luminos ities are very rare\, hosted by perhaps less than 1 in 10^4 SFGs.\n\nhttps ://events.icecube.wisc.edu/event/68/contributions/4103/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4103/ END:VEVENT BEGIN:VEVENT SUMMARY:The cosmic-ray air shower signal in Askaryan radio detectors DTSTART:20150504T204500Z DTEND:20150504T210000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4104@events.icecube.wisc.edu DESCRIPTION:Speakers: Krijn de Vries (VUB/IIHE)\, O'Murchadha Aongus (ULB/ IIHE)\, Olaf Scholten (KVI-CART/RUG/VUB/IIHE)\, Stijn Buitink (VUB)\, Nick van Eijndhoven (VUB/IIHE)\, Thomas Meures (ULB/IIHE)\n\nRecently it has b een shown that the radio detection technique can be used as a new and comp lementary detection method for the detection of high-energy cosmic-ray-ind uced air showers. Along with the detection of the radio emission from air showers\, it is shown that the emission can be predicted in great detail e stablishing the radio emission models. A cosmic-ray air shower hitting a s urface\, for example an ice-sheet\, before it dies out in air will next to the in-air emission also induce a strong transition radiation component. We derived an analytical expression for this coherent transition radiation . This allows us to calculate the radio emission from high-energy cosmic-r ay air showers hitting the ice before the shower dies out in air. This sig nal can be observed by the currently operating Askaryan radio detectors\, like e.g. ARA or Arianna\, where it is shown that without directional info rmation or surface veto techniques it will be very hard to distinguish the air shower signal from an in-ice neutrino induced particle cascade of sim ilar energy.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/410 4/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4104/ END:VEVENT BEGIN:VEVENT SUMMARY:SIBYLL 2.3 and MCEq\, a customizable numerical solver for atmosphe ric lepton fluxes DTSTART:20150505T192300Z DTEND:20150505T194600Z DTSTAMP:20261014T080200Z UID:indico-contribution-4105@events.icecube.wisc.edu DESCRIPTION:Speakers: Anatoli Fedynitch (CERN/KIT)\, Thomas Gaisser (Unive rsity of Delaware)\, Todor Stanev (Bartol Research Institute\, Dept of Phy sics and Astronomy\, University of Delaware)\, Ralph Engel (KIT)\, Felix R iehn (KIT)\n\nThe precision of atmospheric lepton flux calculations is lim ited by various factors. One source of uncertainty is the parameterization of the primary cosmic ray flux. Typically\, calculations are performed fo r a single atmospheric profile\, approximating either a global atmosphere or one specific location. The control of uncertainties arising from hadron ic interaction models is the most challenging part of these calculations. We have created an updated version of popular multi-purpose event generato r SIBYLL\, employing recent accelerator data together with atmospheric lep ton measurements in the development process. It contains a model for produ ction of charm quarks and it is thus tailored to the particular needs of c urrent astroparticle physics research. The matrix cascade equation (MCEq) program is an open-source code for numerical calculations of the atmospher ic muon and neutrino flux. The open-source code allows users to calculate fluxes in very high speed\, using custom or pre-defined parameterizations of the primary cosmic-ray spectrum/composition and arbitrary atmospheric p rofiles. We will use this code to discuss inclusive lepton fluxes calculat ed with the current version of SIBYLL.\n\nhttps://events.icecube.wisc.edu/ event/68/contributions/4105/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4105/ END:VEVENT BEGIN:VEVENT SUMMARY:Muon-induced spallation backgrounds for MeV astrophysical neutrino signals in Super-Kamiokande DTSTART:20150504T213000Z DTEND:20150504T214500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4106@events.icecube.wisc.edu DESCRIPTION:Speakers: Shirley Li (The Ohio State University)\n\nHigh energ y cosmic ray muons not only are backgrounds for high energy astrophysical neutrinos\, they also produce serious background for low energy neutrino s earches. When muons interact in detectors\, their energy losses lead to n uclear breakup (“spallation”) processes. The subsequent beta decays o f unstable daughter nuclei mimic MeV neutrino signals. This background ha s been understudied in water detectors. We show how muons produce these s pallations through showers\, and how to implement more effective backgroun d rejection techniques using this information. This could lead to new phy sics results\, as both solar and Diffuse Supernova Neutrino Background stu dies are background-limited\, and reducing backgrounds by even a factor of a few could quickly lead to new discoveries. This work is in collaborati on with Prof. John Beacom.\n\nhttps://events.icecube.wisc.edu/event/68/con tributions/4106/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4106/ END:VEVENT BEGIN:VEVENT SUMMARY:Diffuse Neutrinos & Gamma Rays - Complementary Views on the High-E nergy Universe. DTSTART:20150504T193000Z DTEND:20150504T200000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4107@events.icecube.wisc.edu DESCRIPTION:Speakers: Markus Ackermann (o=desy-zeuthen\,ou=Institutions\,d c=icecube\,dc=wisc\,dc=edu)\n\nNon-thermal processes in our cosmos have be en studied for several decades through the observation of individual sourc es and diffuse emission in γ rays. However\, the universe is transparent to γ rays only at MeV and GeV energies. Above 100 GeV\, they are increasi ngly absorbed in interactions with the omnipresent radiation background fr om stars and the CMB. At TeV energies γ-ray observations are restricted t o our local cosmic environment\, at hundreds of TeV even to our own Galaxy . \n\nNeutrinos fortunately do not have this limitation. They can travel c osmological distances and escape from dense environments without significa nt absorption. They are therefore our only direct probe of non-thermal pro cesses above tens of TeV for most of the volume of our universe\, and sinc e their discovery by IceCube in 2013 available as an additional cosmic mes senger. \n\nI will review the current status of the observations of extrag alactic γ rays and astrophysical neutrinos\, followed by a discussion of what we can learn from these observations about the sites of cosmic-ray ac celeration and the physics processes involved.\n\nhttps://events.icecube.w isc.edu/event/68/contributions/4107/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4107/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino Portal Dark Matter: From Dwarf Galaxies to IceCube DTSTART:20150505T190000Z DTEND:20150505T192300Z DTSTAMP:20261014T080200Z UID:indico-contribution-4108@events.icecube.wisc.edu DESCRIPTION:Speakers: JJ Cherry (LANL)\, Alexander Friedland (LANL)\, Ian Shoemaker (CP3)\n\nIt has been suggested that the baseline scenario of col lisionless cold dark matter over-predicts the numbers of satellite galaxie s\, as well as the dark matter (DM) densities in galactic centers. This a pparent lack of structure at small scales can be accounted for if one post ulates neutrino-DM and DM-DM interactions mediated by light O(MeV) force c arriers. We consider a simple\, consistent model of neutrinophilic DM wit h these features where DM and a "secluded'' SM-singlet neutrino species ar e charged under a new U(1) gauge symmetry. An important ingredient of this model is that the secluded sector couples to the Standard Model fields on ly through neutrino mixing. We observe that the secluded and active neutri nos recouple\, leading to a large relic secluded neutrino population. Thi s relic population can prevent small-scale halos from collapsing\, while a t the same time significantly modifying the optical depth of ultra-high-en ergy neutrinos recently observed at Icecube. We find that the bulk of the parameter space accommodating an (a)symmetric thermal relic has potentiall y observable consequences for the IceCube high energy signal\, with some o f the parameter space already ruled out by the existing data. Future data may confirm this mechanism if either spectral absorption features or corr elations with nearby sources are observed.\n\nhttps://events.icecube.wisc. edu/event/68/contributions/4108/ LOCATION:Northwoods\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4108/ END:VEVENT BEGIN:VEVENT SUMMARY:The status of Himalayan Gamma Ray Observatory (HiGRO) DTSTART:20150504T213000Z DTEND:20150504T215500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4116@events.icecube.wisc.edu DESCRIPTION:Speakers: B. S. Acharya (WIPAC and Tata Institute of Fundament al Research)\n\nWork on VHE gamma-ray astronomy using the Atmospheric Cher enkov Technique started in India way back in 1969\,soon after the discover y of pulsars. The latest in this series of experiments is the HiGRO projec t located at very high altitude (4.3km)\, at Hanle in the Ladakh region of Himalayas. In the first phase of this project 7 telescope array called HA GAR was installed the year 2008. It is an array of wavefront sampling non- imaging telescopes having a threshold energy of about 200 GeV for gamma-ra ys. It is the first ACT array operating at very high altitudes. A 21-m ima ging telescope (called MACE)\, built by BARC group\, will be commissioned at the same site adjascent to HAGAR array in this year. With MACE\, the th reshold energy of gamma-rays is expec to be about a few tens of GeV. Regul ar observations of galactic and extra galactic objects using HAGAR are goi ng on since October 2008. I shall describe the current status the HiGRO pr oject at Hanle.\n\n(on behalf of HiGRO Collaboration)\n\nhttps://events.ic ecube.wisc.edu/event/68/contributions/4116/ LOCATION:Northwoods (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4116/ END:VEVENT BEGIN:VEVENT SUMMARY:Wave-Packet Treatment for Detection of Accelerator Neutrinos DTSTART:20150505T201000Z DTEND:20150505T202800Z DTSTAMP:20261014T080200Z UID:indico-contribution-4109@events.icecube.wisc.edu DESCRIPTION:Speakers: Cheng-Hsien Li (University of Minnesota\, Twin Citie s)\, Yongzhong Qian (University of Minnesota\, Twin Cities)\n\nNeutrinos a re treated as point particles in Monte Carlo simulations for predicting de tector counting rate. In this talk\, a theoretical study on possible confl ict between point-particle and wave-packet pictures in accelerator neutrin o experiments will be presented. It is a quantum-mechanical phenomenon tha t neutrino wave packets spread as they propagate in space. The effect of l ongitudinal spreading on neutrino oscillation probabilities has been studi ed in various theoretical frameworks. However\, comparatively less attenti on has been paid to the implication of transverse spreading of neutrino wa ve packets. In accelerator neutrino experiments\, Lorentz boost restricts neutrinos from spreading in the forward direction\, while the transverse s preading tends to “defocus” neutrinos from their classical paths. As a consequence\, the transverse spreading smears the kinematic distribution of neutrinos from pion decay and could distort the measured neutrino energ y spectrum. Our approach treats neutrinos as wave packets\, for which the detector counting rate is derived using simple quantum-mechanical treatmen t. Considering the geometric setup and beam profile similar to the MINOS a nd NOvA experiments\, we demonstrate that the transverse spreading of neut rino wave packets would result in a shifted energy spectrum from that pred icted in point particle scenario if the wave packet acquires an initial tr ansverse width less than approximately 10 fm from pion decay. Absence of s uch spectral shift in current or future near detector data could in turn c onstrain the initial transverse width of a neutrino wave packet from pion decay.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4109/ LOCATION:WI Idea (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4109/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrinoless Double Beta Decay: Status and Prospects of CUORE and KamLAND-Zen DTSTART:20150505T163000Z DTEND:20150505T170000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4110@events.icecube.wisc.edu DESCRIPTION:Speakers: Thomas ODonnell (UC Berkeley and Lawrence Berkeley N ational Lab)\n\nNeutrinoless double beta decay ($0\\nu\\beta\\beta$) is th eoretically motivated but has never been observed. Its discovery would de monstrate lepton number violation\, establish neutrinos are Majorana fermi ons and possibly constrain the absolute neutrino-mass\\\n scale.\nThe last decade has seen tremendous experimental progress in the search for this d ecay but to push the frontier forward improved detectors combining excelle nt energy resolution\, extremely low background\, and ton-yr exposures ar e required.\nCUORE and KamLAND-Zen are meeting this challenge in two very different ways\; the former with $^{130}$Te in TeO$_{2}$ bolometers and th e latter with $^{136}$Xe-loaded liquid scintillator. In this talk I will give a brief overview of both these experiments\\\n and their status. In p articular I will present recent results from CUORE-0\, a single-tower prot otype of the CUORE experiment and describe the onging Phase-II of KamLAND- Zen.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4110/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4110/ END:VEVENT BEGIN:VEVENT SUMMARY:Atmospheric neutrinos from perturbative charm production and decay DTSTART:20150505T190000Z DTEND:20150505T192300Z DTSTAMP:20261014T080200Z UID:indico-contribution-4111@events.icecube.wisc.edu DESCRIPTION:Speakers: Mary Hall Reno (University of Iowa)\, Rikard Enberg (University of Uppsala)\, Atri Bhattacharya (University of Arizona)\, Ina Sarcevic (University of Arizona)\, Anna Stasto (Pennsylvania State Univers ity)\n\nThe high energy atmospheric neutrino flux is dominated by charm pr oduction by cosmic ray interactions in the atmosphere\, followed by their prompt decays. Using next-to-leading order QCD and several cosmic ray flux parameterizations\, the prompt atmospheric neutrino flux is discussed\, a long with uncertainties associated with the perturbative evaluation.\n\nht tps://events.icecube.wisc.edu/event/68/contributions/4111/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4111/ END:VEVENT BEGIN:VEVENT SUMMARY:Detecting high-energy neutrinos with RADAR DTSTART:20150505T192000Z DTEND:20150505T194000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4112@events.icecube.wisc.edu DESCRIPTION:Speakers: Krijn de Vries (VUB/IIHE)\, Aongus O'Murchadha (ULB/ IIHE)\, Kael Hanson (UW Madision / ULB)\, Thomas Meures (ULB/IIHE)\n\nRece ntly IceCube for the first time in history discovered high-energy cosmic n eutrinos with energies up to several PeV\, where at higher energies IceCub e runs out of statistics. At even higher energies in the EeV region\, even though no detection has been claimed so-far\, the Askaryan radio detector s start to become sensitive. We discuss the radar detection technique as a new method to detect a high-energy neutrino induced particle cascade in i ce. It is shown that using this method\, it is feasible to detect high-ene rgy neutrino induced particle cascades in ice with an primary neutrino ene rgy threshold of several PeV. Therefore\, the radar detection technique pr ovides a very promising means to cover the currently existing sensitivity gap between several PeV where IceCube runs out of statistics and several E eV where the Askaryan radio detectors become sensitive.\n\nhttps://events. icecube.wisc.edu/event/68/contributions/4112/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4112/ END:VEVENT BEGIN:VEVENT SUMMARY:PROSPECT: a short-baseline reactor antineutrino measurement DTSTART:20150505T213000Z DTEND:20150505T214500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4113@events.icecube.wisc.edu DESCRIPTION:Speakers: Karin Gilje (Illinois Institute of Technology)\n\nTh ere has been increasing tension between direct reactor antineutrino measur ements and models of antineutrino production.\nAs a result\, several colla borations have proposed to make high-resolution measurements of the reacto r neutrino spectrum at a short baseline.\nOne such collaboration is PROSPE CT (the Precision Reactor Oscillation SPECTrum measurement).\nThe goal is two-fold: a precision reactor antineutrino spectrum measurement and a ster ile neutrino search.\nThe detector will be installed near the High Flux Is otope Reactor (HFIR) at Oak Ridge National Laboratory.\nHFIR uses Highly E nriched Uranium which means a pure U-235 antineutrino spectrum.\nAn absolu te measurement of this spectrum will constrain the current and future reac tor models and improve our understanding of the total reactor antineutrino spectrum.\nAdditionally\, the planned detector is sufficiently large to p erform a search for sterile neutrinos on the eV scale.\nOver the last year \, PROSPECT has constructed and installed several prototypes in preparatio n for the final 2-ton Lithium-doped liquid scintillator detector.\nThis ta lk will describe the status of PROSPECT in its various stages and the pred icted sensitivity of its measurements.\n\nhttps://events.icecube.wisc.edu/ event/68/contributions/4113/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4113/ END:VEVENT BEGIN:VEVENT SUMMARY:Toward the Identification of the Cosmic Neutrino Origin DTSTART:20150505T210000Z DTEND:20150505T211200Z DTSTAMP:20261014T080200Z UID:indico-contribution-4114@events.icecube.wisc.edu DESCRIPTION:Speakers: Kohta Murase (Institute for Advanced Study)\n\nTo re veal the origin of diffuse PeV neutrinos observed in IceCube\, we need to identify a single source. I discuss various possibilities in light of curr ent and future neutrino detectors\, and show that many of the proposed sce narios including dark matter models can be critically tested. A natural a nd intriguing possibility is that >0.1 PeV neutrinos originate from cosmic -ray reservoirs like starburst galaxies and galaxy clusters. We emphasize that identifying gamma-ray counterparts is necessary to establish that the y are neutrino emitters.\n\nhttps://events.icecube.wisc.edu/event/68/contr ibutions/4114/ LOCATION:Union South URL:https://events.icecube.wisc.edu/event/68/contributions/4114/ END:VEVENT BEGIN:VEVENT SUMMARY:MicroBooNE - a not-so-micro LArTPC DTSTART:20150506T160000Z DTEND:20150506T163000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4115@events.icecube.wisc.edu DESCRIPTION:Speakers: Anne Schukraft (Fermilab)\n\nMicroBooNE is a short b aseline neutrino experiment with a liquid argon time projection chamber (L ArTPC) located 470m downstream of the proton target in the Fermilab Booste r Neutrino Beam. The LArTPC detection technology delivers bubble-chamber i mage quality of the neutrino interaction with a fully automated triggering \, readout and reconstruction chain. With sensitivity in the neutrino ener gy region between 100 MeV and 2 GeV\, MicroBooNE is about to deliver a lar ge statistic sample for interaction processes in the quasi-elastic and res onance regimes\, much in demand for the theoretical understanding of neutr ino interactions and how they are influenced by nuclear effects. The setup of MicroBooNE in an L/E region similar to the LSND and MiniBooNE experime nts will further investigate their electron neutrino appearance measuremen ts\, potentially being an indication for the existence of sterile neutrino flavors. In particular\, MicroBooNE will be able to resolve the nature of the yet unexplained excess of electron-like events in the energy region o f 200 to 475 MeV observed by MiniBooNE. \nMicroBooNE is also serving as a technology demonstrator for future liquid-argon experiments\, such as the next long-distance neutrino oscillation experiment ELBNF\, and it represe nts the first detector of Fermilab’s short-baseline neutrino program (SB N).\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4115/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4115/ END:VEVENT BEGIN:VEVENT SUMMARY:The Greenland Neutrino Observatory DTSTART:20150505T190000Z DTEND:20150505T192000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4117@events.icecube.wisc.edu DESCRIPTION:Speakers: Keith Bechtol (KICP\, University of Chicago)\n\nThe goals of the proposed Greenland Neutrino Observatory (GNO) are to measure the flux of ultra-high energy neutrinos and use this particle beam for tes ts of fundamental physics at energy scales that cannot be easily achieved on the Earth. The GNO concept exploits the Askaryan effect and the radio-t ransparency of glacial ice\, which together enable hundred-cubic-kilometer volumes of ice to be monitored with sparse instrumentation. GNO will cons ist of an array of radio antenna stations deployed near Summit Station in central Greenland\, atop a 3 km deep ice sheet. Analysis of field measurem ents indicate a radio attenuation length of approximately 1000 m at 300 MH z in the upper 1.5 km of ice. We are currently investigating the logistics of operating at Summit Station\, assembling a prototype station to be dep loyed in summer 2015\, and are developing simulation tools to optimize the design and configuration of the antenna stations.\n\nhttps://events.icecu be.wisc.edu/event/68/contributions/4117/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4117/ END:VEVENT BEGIN:VEVENT SUMMARY:On Observing Anisotropy of Cosmic Neutrinos DTSTART:20150505T194000Z DTEND:20150505T200000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4118@events.icecube.wisc.edu DESCRIPTION:Speakers: Sheldon Campbell (The Ohio State University)\n\nThe angular distribution of neutrino events provides constraints on the source s. One specific observable is the angular power spectrum. This presentatio n outlines new formal results that clarify the path toward measuring angul ar power spectra of cosmic neutrinos. We'll discuss the source information that such measurements would reveal.\n\nhttps://events.icecube.wisc.edu/e vent/68/contributions/4118/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4118/ END:VEVENT BEGIN:VEVENT SUMMARY:A measurement of the diffuse astrophysical muon neutrino flux usin g multiple years of IceCube data. DTSTART:20150504T211000Z DTEND:20150504T213000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4119@events.icecube.wisc.edu DESCRIPTION:Speakers: Sebastian Schoenen (o=rwth\,ou=Institutions\,dc=icec ube\,dc=wisc\,dc=edu)\, Leif Raedel (o=rwth\,ou=Institutions\,dc=icecube\, dc=wisc\,dc=edu)\n\nThe IceCube Collaboration measured an all-flavor\, hig h-energy astrophysical neutrino flux. In order to identify the sources of this flux\, high-energy muon neutrinos are ideal messenger particles becau se of their excellent angular resolution. However\, the first step is to c onfirm the observed flux in the muon neutrino channel using IceCube data f rom 2009 through 2014. The main background for this search are cosmic-ray- induced atmospheric muon neutrinos. High-purity neutrino event samples wil l be analyzed using a two-dimensional likelihood approach\, taking full ad vantage of the information of neutrino energies and arrival directions wit h a consistent treatment of systematic uncertainties. The results of this analysis initially using IceCube data from 2009 through 2012 will be prese nted.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4119/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4119/ END:VEVENT BEGIN:VEVENT SUMMARY:Background from Cosmogenic Activation in the DM-Ice Dark Matter Ex periment DTSTART:20150505T194500Z DTEND:20150505T200000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4120@events.icecube.wisc.edu DESCRIPTION:Speakers: Walter Pettus (University of Wisconsin - Madison)\n\ nDM-Ice is a quarter-ton-scale dark matter experiment planned for deployme nt deep in the ice at the South Pole. This experiment will search for the expected annual modulation signature in the dark matter signal using low-b ackground NaI(Tl) scintillating crystals. Cosmogenic activation of the det ectors during transport to and storage at the South Pole (altitude 9\,301 feet) has the potential to produce long-lived radioisotopes which will add a significant source of background and threaten the discovery potential o f this experiment. In data from the presently operating DM-Ice17 detectors \, we examine decaying regions of the spectrum to identify activated isoto pes and estimate activation effects. We compare these activation estimates to our simulation for the DM-Ice17 detectors and discuss the effects on t he full-scale DM-Ice experiment.\n\nhttps://events.icecube.wisc.edu/event/ 68/contributions/4120/ LOCATION:Northwoods\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4120/ END:VEVENT BEGIN:VEVENT SUMMARY:Reactor Neutrinos: Recent Results and Future Prospects DTSTART:20150506T140000Z DTEND:20150506T143000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4121@events.icecube.wisc.edu DESCRIPTION:Speakers: Karsten Heeger (Yale University)\n\nhttps://events.i cecube.wisc.edu/event/68/contributions/4121/ LOCATION:The Marquee (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4121/ END:VEVENT BEGIN:VEVENT SUMMARY:Fermi Results on High-Energy Gamma-Ray Sources DTSTART:20150504T163000Z DTEND:20150504T170000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4122@events.icecube.wisc.edu DESCRIPTION:Speakers: Alice Harding (NASA Goddard Space Flight Center)\n\n The Fermi Gamma-Ray Space Telescope has detected a variety of gamma-ray so urces in the range 30 MeV to 300 GeV\, many of which may be accelerating p articles to PeV energies. I will review the results of observations of Ga lactic sources of high-energy gamma-rays such as pulsars and their nebulae \, supernova remnants and gamma-ray binaries\, as well as extragalactic so urces such as active galaxies\, starburst galaxies and gamma-ray bursts. Which of these may be sources of high-energy neutrinos will also be discus sed.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4122/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4122/ END:VEVENT BEGIN:VEVENT SUMMARY:The status of India-based Neutrino Observatory (INO) DTSTART:20150505T214500Z DTEND:20150505T220000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4123@events.icecube.wisc.edu DESCRIPTION:Speakers: B. S. Acharya (WIPAC and Tata Institute of Fundament al Research)\n\nIn this talk I shall narrate our plans of building a new u nderground laboratory facility in southern India called India-based neutri no observatory (INO). A 50 kilo-ton magnetised Iron CALorimeter (ICAL)is o ne of the first experiments proposed to be housed in this observatory for the study of neutrino properties like mass hierarchy\, precision measureme nt of oscillation parameters etc. using the atmospheric neutrinos. The det ails of this ICAL project and its present status will also be covered in t his talk.\n\n(on behalf of INO-ICAL Collaboration)\n\nhttps://events.icecu be.wisc.edu/event/68/contributions/4123/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4123/ END:VEVENT BEGIN:VEVENT SUMMARY:Overview of JUNO DTSTART:20150506T143000Z DTEND:20150506T150000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4124@events.icecube.wisc.edu DESCRIPTION:Speakers: Chao Zhang (Brookhaven National Laboratory)\n\nThe J iangmen Underground Neutrino Observatory (JUNO) is a multipurpose neutrino experiment aiming to determine the neutrino mass hierarchy and precisely measure the neutrino oscillation parameters by detecting reactor antineutr inos at ~50 km baselines using a 20-kiloton liquid scintillator detector p laced at 1800-m.w.e deep underground. JUNO is also capable of observing su pernova neutrinos\, studying the atmospheric neutrinos\, solar neutrinos\, geoneutrinos\, and other physics. The international collaboration of JUNO was established in 2014 and the civil construction has started in 2015. J UNO is planning to start data taking around 2020. The scientific opportuni ties and the status of JUNO will be presented in this talk.\n\nhttps://eve nts.icecube.wisc.edu/event/68/contributions/4124/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4124/ END:VEVENT BEGIN:VEVENT SUMMARY:Ultra-high-energy emission from an evolving gamma-ray burst: neutr inos\, cosmic rays\, and gamma rays DTSTART:20150505T211200Z DTEND:20150505T212400Z DTSTAMP:20261014T080200Z UID:indico-contribution-4125@events.icecube.wisc.edu DESCRIPTION:Speakers: Mauricio Bustamante (CCAPP Ohio State University)\, Walter Winter (DESY)\, Kohta Murase (Institute for Advanced Study)\, Phili pp Baerwald (Pennsylvania State University)\n\nGamma-ray bursts (GRBs) are potential sources of ultra-high-energy neutrinos and\, arguably\, constit ute the object class within which neutrino point sources may sooner be ide ntified. For that reason\, it is important to have a clear idea of what si gnals to expect from them. We present a model where the neutrino\, gamma r ay\, and cosmic ray emission from the burst is made up of the superpositio n of emission from individual internal collisions\, each one occurring at different sites within the relativistic jet of the burst\, and at differen t stages of its evolution. As a result\, collisions take place under a ran ge of physical conditions\, and we find that neutrino production through p roton-photon interactions occurs predominantly in collisions around the ph otospheric radius\, where the particle densities are higher\; cosmic ray p roduction occurs mainly in the central regions of the jet\; and gamma-ray emission comes from collisions at large radii\, where the optical depth is low enough for photons to be able to escape. We compute a new and robust minimal diffuse GRB neutrino flux prediction\, which\, in contrast to the calculations based on a single representative internal collision\, is larg ely independent of GRB parameters other than the total energy emitted in g amma-rays and the fraction of that energy that is carried by cosmic-ray pr otons. While the current IceCube configuration will not be able to probe t his flux\, it might be within the reach of a high-energy extension of the detector.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4125/ LOCATION:Union South URL:https://events.icecube.wisc.edu/event/68/contributions/4125/ END:VEVENT BEGIN:VEVENT SUMMARY:Understanding the anisotropy of cosmic rays at TeV and PeV energie s DTSTART:20150504T211500Z DTEND:20150504T213000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4126@events.icecube.wisc.edu DESCRIPTION:Speakers: Martin Pohl (DESY)\, Robert Rettig (University Potsd am)\n\nThe anisotropy in cosmic-ray arrival directions in the TeV-PeV ener gy range shows both large and small-scale structures. While the large-scal e anisotropy may arise from diffusive propagation of cosmic rays\, the ori gin of the small-scale structures remains unclear. We perform three-dimens ional Monte-Carlo test-particle simulations\, in which the particles propa gate in both magnetostatic and electromagnetic turbulence derived from a t hree-dimensional isotropic power spectrum. However\, in contrast to earlie r studies\, we do not use a backtracking method for the computation of the particle trajectories\, and hence anisotropy must build up from a large-s cale isotropic (or dipole) boundary condition. It has been recently argued that the turbulent\nmagnetic field itself generates the small-scale struc tures of the anisotropy if a global cosmic-ray dipole moment is present. O ur code is well suited to test that hypothesis.\n\nhttps://events.icecube. wisc.edu/event/68/contributions/4126/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4126/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of the Project 8 Experiment DTSTART:20150505T193600Z DTEND:20150505T195400Z DTSTAMP:20261014T080200Z UID:indico-contribution-4127@events.icecube.wisc.edu DESCRIPTION:Speakers: Benjamin LaRoque (UC Santa Barbara)\n\nProject 8 is developing a new approach to the tritium-endpoint method of direct neutrin o mass measurement. First results from a proof-of-principle system demonst rate the Cyclotron Radiation Emission Spectroscopy technique by measuring the conversion electron spectrum of krypton-83m. I will provide an overvie w of the technique and released results\, as well as future prospects.\n\n https://events.icecube.wisc.edu/event/68/contributions/4127/ LOCATION:WI Idea (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4127/ END:VEVENT BEGIN:VEVENT SUMMARY:On Extensions of IceTop to Veto Air Showers for Neutrino Astronomy with IceCube DTSTART:20150504T213000Z DTEND:20150504T215000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4128@events.icecube.wisc.edu DESCRIPTION:Speakers: Jan Auffenberg (o=uwmad\,ou=Institutions\,dc=icecube \,dc=wisc\,dc=edu)\n\nceCube is the world’s largest high-energy neutrino observatory\, built at the geographic South Pole. For neutrino astronomy\ , a large background-free sample of well-reconstructed astrophysical neutr inos is essential. The main background for this signal are muons and neutr inos which are produced in cosmic-ray air showers in the Earth's atmospher e. The coincident detection of these air showers by the surface detector I ceTop has been proven to be a powerful veto for atmospheric neutrinos and muons in the field of view of the southern hemisphere. This motivates a si gnificant extension of IceTop. First estimates indicate that such a veto d etector will more than double the discovery potential of current point sou rce analyses. Here\, we present the motivation and capabilities of differe nt technologies based on simulations and measurements.\n\nhttps://events.i cecube.wisc.edu/event/68/contributions/4128/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4128/ END:VEVENT BEGIN:VEVENT SUMMARY:Results from Telescope Array DTSTART:20150505T150000Z DTEND:20150505T153000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4129@events.icecube.wisc.edu DESCRIPTION:Speakers: Douglas Bergman (University of Utah)\n\nI will prese nt the latest results from Telescope Array including measurements of UHECR composition and anisotropy. I will present preliminary results at lower e nergies from TALE. Finally\, I will present plans for TAx4 and for the Non -Imaging Cherenkov array (NICHE). NICHE and TALE provide the possibility o f doing Cherenkov hybrid measurements in the energy region just above the Knee.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4129/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4129/ END:VEVENT BEGIN:VEVENT SUMMARY:Monitoring TeV Gamma-ray Sources for Flaring States with HAWC DTSTART:20150504T205000Z DTEND:20150504T211000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4130@events.icecube.wisc.edu DESCRIPTION:Speakers: Ian Wisher (University of Wisconsin - Madison)\n\nTh e flux of many TeV gamma-ray emitters exhibits time variability. Detection of these flaring states across multiple wavelengths will lead to a better understanding of the acceleration processes occurring in the source. The High-Altitude Water Cherenkov (HAWC) Observatory is an extensive air-showe r detector located near Pico de Orizaba in Mexico which is sensitive to Te V gamma rays. Designed as a survey instrument\, the HAWC detector has a la rge field of view and nearly 100% uptime. This makes HAWC an ideal instrum ent to monitor sources for transient flaring states. We will present a met hod of monitoring sources using a Bayesian blocks algorithm to detect chan ges in the flux and report alerts in real time. We also discuss the sensit ivity of the method using data from the construction phase of HAWC.\n\nhtt ps://events.icecube.wisc.edu/event/68/contributions/4130/ LOCATION:Northwoods (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4130/ END:VEVENT BEGIN:VEVENT SUMMARY:KPipe: A Short-Baseline Muon-Neutrino Disappearance Experiment usi ng Neutrinos from Kaon Decay-at-rest DTSTART:20150505T195400Z DTEND:20150505T201000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4131@events.icecube.wisc.edu DESCRIPTION:Speakers: Taritree Wongjirad (MIT)\, Janet Conrad (MIT)\, Mich ael Shaevitz (Columbia University)\n\nRecently\, anomalies consistent with neutrino oscillations with mass splittings on the order of 1 eV2 have bee n observed. These anomalies have been seen in experiments measuring nue ap pearance and nue/nue-bar disappearance\, while no corresponding evidence f or muon neutrino disappearance has been detected. A common interpretation of the anomalies involves postulating the existence of one or more “ste rile” neutrinos that\, unlike the three Standard Model neutrinos\, do no t interact via the electroweak force. While models with sterile neutrinos can explain the current data\, they all require that some amount of muon neutrino disappearance must occur\, with several models indicating that ev idence for the process might have been just below the sensitivities of pas t experiments. In this talk\, I present a new type of experiment that wil l search for muon neutrino disappearance at the Materials and Life Science Facility (MLF)\, which is a part of the JPARC accelerator complex in Toka i\, Japan. The facility features a high intensity\, pulsed beam of 3 GeV protons used to produce neutron\, muons\, and neutrinos for various experi ments. In our proposal\, we would measure mono-energetic neutrinos coming from kaon decay-at-rest with a detector consisting of a 3 m diameter by 9 0 m long pipe filled with liquid scintillator. This setup would aim to mea sure directly the L/E oscillation wave in the event rate along the length of the detector. Such a signal would provide convincing evidence for a ste rile neutrino and avoids some of the difficulties in past experiments in c haracterizing the incoming neutrino flux and modeling neutrino-nucleus int eraction cross sections.\n\nhttps://events.icecube.wisc.edu/event/68/contr ibutions/4131/ LOCATION:WI Idea (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4131/ END:VEVENT BEGIN:VEVENT SUMMARY:Ultra-Fast Magnetic Sensing for Large-Area Detection of High Energ y Particles DTSTART:20150504T203000Z DTEND:20150504T204500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4132@events.icecube.wisc.edu DESCRIPTION:Speakers: David Saltzberg (University of California\, Los Ange les)\, Peihao Sun (University of California\, Los Angeles)\n\nCascades fro m high-energy particles produce a brief current and associated magnetic fi elds. Even sub-nanosecond duration magnetic fields can be detected with a relatively low bandwidth system by latching image currents on a capacitor. At accelerators\, this technique is employed routinely by beam-current mo nitors\, which work for pulses even as fast as femtoseconds. We discuss sc aling up these instruments in size\, to 100 meters and beyond\, to serve a s a new kind of ground- and space-based high-energy particle detector whic h can instrument large areas relatively inexpensively. This new technique may be used to detect and/or veto ultra-high energy cosmic-ray showers. It may also be applied to searches for hypothetical highly charged particles . In addition\, these detectors may serve to search for extremely short ma gnetic field pulses of any origin\, faster than other detectors by orders of magnitude.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/41 32/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4132/ END:VEVENT BEGIN:VEVENT SUMMARY:Astrophysical Sources of the IceCube Cosmic Neutrino Events DTSTART:20150505T210000Z DTEND:20150505T212000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4140@events.icecube.wisc.edu DESCRIPTION:Speakers: Soebur Razzaque (University of Johannesburg)\n\nIceC ube Neutrino Observatory has recently detected over 30 very high-energy ne utrino events which are most likely of cosmic origin. Due to poor angular resolution of cascade-type events\, which dominate the event list\, ident ification of astrophysical source(s) as origin of these neutrino events is proving to be difficult. I will present a scenario where the detected c osmic neutrinos originate from Galactic and extragalactic sources.\n\nhttp s://events.icecube.wisc.edu/event/68/contributions/4140/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4140/ END:VEVENT BEGIN:VEVENT SUMMARY:IceCube neutrinos: What we have learned DTSTART:20150505T143000Z DTEND:20150505T150000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4141@events.icecube.wisc.edu DESCRIPTION:Speakers: Eli Waxman (Weizmann Inst.)\n\na\n\nhttps://events.i cecube.wisc.edu/event/68/contributions/4141/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4141/ END:VEVENT BEGIN:VEVENT SUMMARY:The Present and Future of Long Baseline Neutrino Oscillations with T2K and DUNE DTSTART:20150506T163000Z DTEND:20150506T170000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4133@events.icecube.wisc.edu DESCRIPTION:Speakers: Alexander Himmel (Duke University)\n\nNeutrinos osci llate among flavors as they travel because a neutrino of a particular flav or is a also a superposition of multiple neutrinos with slightly different masses.  The interferometric nature of oscillations allows this mixing t he be measured\, but it requires powerful neutrino sources and massive det ectors.  T2K\, with the J-PARC neutrino beam and Super-Kamiokande as far detector\, uses a narrow band\, off-axis beam to make measurements of neut rino oscillations at an L/E precisely tuned to atmospheric-sector oscillat ions. DUNE (formerly ELBNF) will use an even more powerful\, wide band\, on-axis beam from Fermilab and a massive\, underground liquid argon time p rojection chamber to measure atmospheric oscillations with unprecedented p recision. Here I will present the latest oscillation results from the T2K experiment as well as the status of DUNE\, and its prospects for address ing the questions which the current generation of experiments cannot.\n\nh ttps://events.icecube.wisc.edu/event/68/contributions/4133/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4133/ END:VEVENT BEGIN:VEVENT SUMMARY:High-energy neutrinos from a nearby newborn pulsar DTSTART:20150505T212000Z DTEND:20150505T214000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4134@events.icecube.wisc.edu DESCRIPTION:Speakers: Ke Fang (University of Chicago)\n\nThe electromagnet ic wind of a fast-spinning pulsar provides favorable sites for cosmic ray acceleration from PeV to ultrahigh energies. We show that high-energy neut rinos are guaranteed to be produced in this system\, when the accelerated particles interact with the dense baryons of the supernova ejecta. We stud y the light curves and energy spectrum of the neutrinos using both numeric al and analytical methods. We find that the neutrino spectral index varie s from 1.5 to 2\, as a result of the interplay between the pulsar spin-dow n and the evolution of the supernova environment. We then discuss the impa ct of the chemical composition of the parent cosmic rays on the neutrino p roduction. Moreover\, we apply to the scenario to existing nearby young pu lsars and find the corresponding neutrino flux consistent with the current non-detections. Finally\, we explore the detectability of the high-energy neutrinos from future newborn pulsars in the Local Universe in light of c urrent and next generation neutrino telescopes.\n\nhttps://events.icecube. wisc.edu/event/68/contributions/4134/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4134/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for primordial black hole evaporation signal with AMON DTSTART:20150505T212400Z DTEND:20150505T213600Z DTSTAMP:20261014T080200Z UID:indico-contribution-4135@events.icecube.wisc.edu DESCRIPTION:Speakers: Gordana Tešić (o=psu\,ou=Institutions\,dc=icecube\ ,dc=wisc\,dc=edu)\n\nPrimordial black holes (PBHs) are expected to explode violently during the last few seconds of their lives\, producing jets of high energy particles. These particles could be detected in coincidence by several observatories with large fields of view\, such as IceCube and ANT ARES (neutrinos)\, HAWC and Fermi LAT (gamma rays) and Pierre Auger (neutr ons). The short temporal structure of the anticipated PBH evaporation sign al provides a very low false positive rate for any possible detection. We will present the discovery potential of the Astrophysical Multimessenger O bservatory Network (AMON) for PBH evaporation events. AMON aims to discove r multimessenger transient sources by performing real-time and archival co incidence searches from multiple observatory subthreshold data streams. In this approach\, a distinctive PBH evaporation signature may be probed by conducting coincidence analysis from a few years of subthreshold neutrino\ , gamma-ray and neutron data. Detection of PBHs would be a scientific brea kthrough confirming Hawking’s hypothesis of black hole radiation and cos mological models of phase transitions\, and would allow us to probe physic s at the highest energy scale as well as quantum gravity.\n\nhttps://event s.icecube.wisc.edu/event/68/contributions/4135/ LOCATION:Union South URL:https://events.icecube.wisc.edu/event/68/contributions/4135/ END:VEVENT BEGIN:VEVENT SUMMARY:First cosmogenic neutrino limits from the ARA detector at the Sout h Pole DTSTART:20150504T205000Z DTEND:20150504T211000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4136@events.icecube.wisc.edu DESCRIPTION:Speakers: Aongus Ó Murchadha (o=ulb\,ou=Institutions\,dc=icec ube\,dc=wisc\,dc=edu)\n\nThe Askaryan Radio Array (ARA) is an ultra-high e nergy (>100 PeV) cosmic neutrino detector which is in phased construction near the South Pole. ARA searches for radio Cherenkov-like emission from p article cascades induced by neutrino interactions in the ice using radio f requency antennas (~150-800MHz) deployed at a design depth of 200m in the Antarctic ice. A prototype ARA Testbed station was deployed at ~30m depth in the 2010-2011 season and the first three full ARA stations were deploye d in the 2011-2012 and 2012-2013 seasons. We present the first neutrino se arch with ARA using data taken in 2011-2012 with the ARA Testbed\, and 201 1-2014 with the first full ARA stations along with the resulting constrain ts on the neutrino flux from 100 PeV to 100 EeV.\n\nhttps://events.icecube .wisc.edu/event/68/contributions/4136/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4136/ END:VEVENT BEGIN:VEVENT SUMMARY:Gamma Rays from Cosmic Ray Collisions with the Sun Observed with F ermi DTSTART:20150504T211000Z DTEND:20150504T213000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4137@events.icecube.wisc.edu DESCRIPTION:Speakers: Kenny\, Chun Yu NG (CCAPP\, The Ohio State Universit y)\, John Beacom (CCAPP\, The Ohio State University)\, Annika Peter (CCAPP \, The Ohio State University)\, Carsten Rott (Sungkyunkwan University)\n\n The Sun is a bright gamma ray source due to interactions between cosmic ra ys and the solar atmosphere. These gamma rays were detected from 0.1 to 1 0 GeV by Fermi with 18 months of data\, and were found to be in disagreeme nt with theoretical predictions. In this work we update the measurement u sing 6 years of Fermi data. The improved statistics allow us to detect th e gamma rays up to 100 GeV and discover new features in the gamma ray spec trum. This provides a solid basis for revisiting the theoretical modeling of cosmic ray interactions with the Sun. Thorough understanding of the h adronic gamma ray production process helps predicting the corresponding ne utrino flux\, which may allow the Sun to be detectable by IceCube.\n\nhttp s://events.icecube.wisc.edu/event/68/contributions/4137/ LOCATION:Northwoods (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4137/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for Gamma-Ray Emission from DES Dwarf Spheroidal Galaxy Can didates with Fermi-LAT Data DTSTART:20150504T203000Z DTEND:20150504T205000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4138@events.icecube.wisc.edu DESCRIPTION:Speakers: Keith Bechtol (KICP\, University of Chicago)\n\nDue to their proximity\, high dark matter content\, and apparent absence of no n-thermal processes\, Milky Way dwarf spheroidal satellite galaxies (dSphs ) are excellent targets for the indirect detection of dark matter. Recentl y\, eight new dSph candidates were discovered using the first year of data from the Dark Energy Survey (DES). We searched for gamma-ray emission coi ncident with the positions of these new objects in six years of Fermi Larg e Area Telescope data. We found no significant excesses of gamma-ray emiss ion. Under the assumption that the DES candidates are dSphs with dark matt er halo properties similar to the known dSphs\, we computed individual and combined limits on the velocity-averaged dark matter annihilation cross s ection for these new targets. If confirmed\, they will constrain the annih ilation cross section to lie below the thermal relic cross section for dar k matter particles with masses < 20 GeV annihilating via the b-bbar or tau +tau- channels.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/ 4138/ LOCATION:Northwoods (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4138/ END:VEVENT BEGIN:VEVENT SUMMARY:Anisotropy in Cosmic Ray Arrival Directions Using IceCube and IceT op DTSTART:20150504T210000Z DTEND:20150504T211500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4139@events.icecube.wisc.edu DESCRIPTION:Speakers: Frank McNally (IceCube)\n\nWe provide an update on t he continued observation of anisotropy in the arrival direction distributi on of cosmic rays in the southern hemisphere. The IceCube neutrino observa tory recorded more than 250 billion events between May 2009 and May 2014. Subtracting dipole and quadrupole fit maps\, we can use these increased st atistics to see significant small-scale structure that approaches our medi an angular resolution of $3^{\\circ}$ . The expanded dataset also allows f or a more detailed study of the anisotropy for various cosmic-ray median e nergies. The large-scale structure observed at median eneries near 20 TeV appears to shift around 100 TeV\, with the high-energy skymap showing a st rong deficit also present in IceTop maps of similar energies.\n\nhttps://e vents.icecube.wisc.edu/event/68/contributions/4139/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4139/ END:VEVENT BEGIN:VEVENT SUMMARY:Stability Analysis of DM-Ice17 DTSTART:20150505T200000Z DTEND:20150505T201500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4142@events.icecube.wisc.edu DESCRIPTION:Speakers: Zachary Pierpoint (UW-Madison)\n\nDM-Ice17\, a 17 kg sodium iodide prototype detector for the proposed DM-Ice experiment\, was deployed in the Antarctic Ice at the geographic South Pole in December 20 10\, and has been in operation since January 2011. I will present a stabil ity analysis of three years of data\, with a focus on sources of noise and time-dependent effects that could mimic or obfuscate a dark matter modula tion. Due to the small mass of the detector\, the analysis does not signif icantly probe dark matter regions of interest but does provide further evi dence that the Antarctic ice provides an ideal location for dark matter an nual modulation searches.\n\nhttps://events.icecube.wisc.edu/event/68/cont ributions/4142/ LOCATION:Northwoods\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4142/ END:VEVENT BEGIN:VEVENT SUMMARY:Status of the NOvA Experiment DTSTART:20150506T170000Z DTEND:20150506T173000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4143@events.icecube.wisc.edu DESCRIPTION:Speakers: Ryan Patterson (California Institute of Technology)\ n\n​The NOvA long-baseline neutrino oscillation experiment at Fermilab h as transitioned from construction to operation\, with the 14-kton Far Dete ctor and the 0.3-kton Near Detector now collecting neutrino data. With it 's full planned exposure\, NOvA will make the most precise measurements to date of the atmospheric neutrino sector\, and NOvA's 810-km baseline give s it a unique sensitivity among existing experiments for measuring the neu trino mass hierarchy\, a critical missing piece of the neutrino framework. I will summarize the construction and commissioning of NOvA\, current an alysis activities\, and the physics outlook of the experiment.\n\nhttps:// events.icecube.wisc.edu/event/68/contributions/4143/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4143/ END:VEVENT BEGIN:VEVENT SUMMARY:Origin of the ankle in the ultra-high energy cosmic ray spectrum a nd extragalactic protons below it DTSTART:20150505T194600Z DTEND:20150505T200900Z DTSTAMP:20261014T080200Z UID:indico-contribution-4144@events.icecube.wisc.edu DESCRIPTION:Speakers: Luis Anchordoqui (City University of New York)\, Mic hael Unger (New York University)\, Glennys Farrar (New York University)\n\ nThe sharp change in slope of the ultra-high energy cosmic ray (UHECR) spe ctrum around 10^9.6 GeV (the ankle)\, combined with evidence of a light bu t extragalactic component near and below the ankle and intermediate compos ition above\, has proved exceedingly challenging to understand theoretical ly. We propose a mechanism whereby photo-disintegration of ultra-high ene rgy nuclei in the region surrounding a UHECR accelerator naturally account s for the observed spectrum and inferred composition at Earth. We discuss the conditions required to reproduce the spectrum above 10^8.5 GeV and th e composition\, which -- in our model -- consists below the ankle of extra galactic protons and the high energy tail of Galactic cosmic rays\, and ab ove the ankle of surviving nuclei from the extended source. Predictions fo r the spectrum and flavors of neutrinos resulting from this process will b e presented\, and also implications for candidate sources.\n\nhttps://even ts.icecube.wisc.edu/event/68/contributions/4144/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4144/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent results from MINERvA DTSTART:20150505T190000Z DTEND:20150505T191800Z DTSTAMP:20261014T080200Z UID:indico-contribution-4145@events.icecube.wisc.edu DESCRIPTION:Speakers: Cheryl Patrick (Northwestern University)\n\nFermilab 's MINERvA experiment is designed to make precision measurements of muon n eutrino scattering cross sections on a variety of nuclear targets. Its 1-2 0 GeV energy range (which has since been increased for our current data-ta king) should be of particular interest to PINGU. After introducing the MIN ERvA detector\, I will describe several recently-published results that ar e already being used by the neutrino community to improve their modeling o f neutrino interactions. There will also be a chance to look at interestin g analyses that will be published in the coming months\, and at the plans for MINERvA's longer-term future.\n\nhttps://events.icecube.wisc.edu/event /68/contributions/4145/ LOCATION:WI Idea (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4145/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmology overview DTSTART:20150504T190000Z DTEND:20150504T193000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4146@events.icecube.wisc.edu DESCRIPTION:Speakers: Scott Dodelson (Fermilab/Chicago)\n\nNeutrinos produ ced in the early universe leave their imprint on the cosmic microwave back ground and on large scale structure. Current measurements add to our const raints on neutrino physics\, and ambitious surveys over the coming decade aim to measure the sum of the neutrino masses. Beyond these goals\, observ ations can detect cracks in the 3-neutrino paradigm and might even resolve long-standing cosmological anomalies.\n\nhttps://events.icecube.wisc.edu/ event/68/contributions/4146/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4146/ END:VEVENT BEGIN:VEVENT SUMMARY:Ultra-high energy cosmic rays DTSTART:20150505T170000Z DTEND:20150505T173000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4147@events.icecube.wisc.edu DESCRIPTION:Speakers: Michael Unger (New York University)\n\nIn this talk I will present recent results on the flux\, composition\nand arrival direc tions of ultra-high energy cosmic rays from the\nPierre Auger Observatory and the Telescope Array.\nFurthermore\, I will discuss the plans and prosp ects for astroparticle\nresearch at ultra-high energies within the next de cade.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4147/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4147/ END:VEVENT BEGIN:VEVENT SUMMARY:AMON: transition to real-time operations DTSTART:20150505T214800Z DTEND:20150505T220000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4148@events.icecube.wisc.edu DESCRIPTION:Speakers: Gordana Tešić (o=psu\,ou=Institutions\,dc=icecube\ ,dc=wisc\,dc=edu)\n\nThe Astrophysical Multimessenger Observatory Network (AMON) will link the world's leading high-energy neutrino\, cosmic-ray\, g amma-ray and gravitational wave observatories by performing real-time coin cidence searches for multimessenger sources from observatory subthreshold data streams. The resulting coincidences will be distributed to interested parties in the form of electronic alerts for real-time follow-up observat ion. We will present the science case\, design elements\, current and proj ected partner observatories\, and status of the AMON project. Observatorie s that already signed the AMON Memorandum of Understanding (MoU) include t he IceCube and ANTARES Neutrino Observatories\, the HAWC and VERITAS gamma -ray observatories\, the Pierre Auger Cosmic Ray Observatory and the Swift satellite experiment. AMON is an open network seeking new triggering and follow-up observatories\, as well as collaborators interested in the scien tific goals of AMON. The prototype of the AMON server has been online sinc e August 2014 and processing archival data. Currently\, we are deploying n ew high-uptime servers and will be ready to start issuing alerts as early as summer 2015. We will also discuss the primary results of implementing a new real-time analysis of the IceCube high-energy starting events (HESE) at the South Pole that will relay event positions for high-energy events t o AMON.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4148/ LOCATION:Union South URL:https://events.icecube.wisc.edu/event/68/contributions/4148/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrinoless double beta decay with EXO-200 DTSTART:20150505T210000Z DTEND:20150505T211500Z DTSTAMP:20261014T080200Z UID:indico-contribution-4149@events.icecube.wisc.edu DESCRIPTION:Speakers: Yung-Ruey Yen (Drexel University)\n\nThe Enriched Xe non Observatory (EXO-200) is one of the most sensitive searches for neutri noless double beta decay (bb0v) in the world. With 175 kg of enriched liqu id xenon (80% Xe-136) as both the source of decay and the detection medium \, the experiment uses an ultralow background time projection chamber inst alled at the Waste Isolation Pilot Plant\, a salt mine with a 1600 m water equivalent overburden. The EXO-200 detector has demonstrated excellent en ergy resolution and background rejection capabilities in setting a limit o f 1.1x10^25 yr at 90% C.L. on the bb0v half-life of Xe-136. The current re sults from the two years of data-taking will be presented. Due to the succ ess of EXO-200\, the tonne scale next generation experiment\, nEXO\, is be ing developed with a target sensitivity to bb0v half-life of Xe-136 of 5x1 0^27 yr.\n\nhttps://events.icecube.wisc.edu/event/68/contributions/4149/ LOCATION:Landmark\, 3rd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4149/ END:VEVENT BEGIN:VEVENT SUMMARY:Liquid Argon TPCs for Neutrino Detection DTSTART:20150506T150000Z DTEND:20150506T153000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4150@events.icecube.wisc.edu DESCRIPTION:Speakers: Joseph Zennamo (University of Chicago)\n\nAs neutrin o physics transitions into an era of precision measurements we need scalea ble detectors which provide a detailed picture of how neutrinos interact w ith matter. Liquid Argon Time Projection Chambers (LArTPC) are one such de tector technology\, that combines both bubble chamber quality images with fine grained calorimetry. I will discuss how these detectors work and enab le us to study a wide range of neutrino properties.\n\nhttps://events.icec ube.wisc.edu/event/68/contributions/4150/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4150/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrinos from Galactic Microquasars DTSTART:20150505T214000Z DTEND:20150505T220000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4151@events.icecube.wisc.edu DESCRIPTION:Speakers: Luiz da Silva (University of Wisconsin - Milwaukee)\ n\nMotivated by recent IceCube observations we re-examine the idea that mi croquasars are high energy neutrino emitters. By stretching to the maximum the parameters of the Fermi engine we show that the nearby high-mass X-ra y binary LS 5039 could accelerate protons up to above about 20 PeV. These highly relativistic protons could subsequently interact with the plasma pr oducing neutrinos up to the maximum observed energies. After that we adopt the spatial density distribution of high-mass X-ray binaries obtained fro m the deep INTEGRAL Galactic plane survey and we assume LS 5039 typifies t he microquasar population to demonstrate that these powerful compact sourc es could provide a dominant contribution to the diffuse neutrino flux rece ntly observed by IceCube.\n\nhttps://events.icecube.wisc.edu/event/68/cont ributions/4151/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4151/ END:VEVENT BEGIN:VEVENT SUMMARY:TeV Astrophysics at the HAWC Observatory DTSTART:20150504T160000Z DTEND:20150504T163000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4152@events.icecube.wisc.edu DESCRIPTION:Speakers: Segev BenZvi (University of Rochester)\n\nThe field of TeV gamma-ray astrophysics is currently dominated by two types of air s hower experiments: imaging air Cherenkov telescopes (IACTs)\, which conduc t very sensitive but low-uptime pencil-beam surveys of the gamma-ray sky\; and surface arrays\, which are moderately sensitive but carry out synopti c surveys with high uptime. The High Altitude Water Cherenkov Observatory \, or HAWC\, is a surface array of 300 water Cherenkov detectors deployed 4100 m above sea level in Sierra Negra\, Mexico. It is sensitive to cosmi c rays and gamma rays between 100 GeV and 100 TeV\, and observes two-third s of the sky each day. HAWC is uniquely suited to study very high energy sources of cosmic rays and search for regions of extended gamma-ray emissi on. Because of its high uptime\, HAWC will also play a crucial role in tr iggering multi-wavelength and multi-messenger studies of active galactic n uclei\, gamma-ray bursts\, and other transient sources. The observatory w as completed in January 2015\, but observations with the partially-finishe d detector began in July 2013. We will describe the first year of data co llected with HAWC\, which includes the observation of TeV emission from th e Galactic Plane and other known Galactic sources\, a number of AGN\, and the anisotropy of cosmic rays at 1 TeV. We will also discuss the prospect s for a robust multi-wavelength and multi-messenger program with HAWC.\n\n https://events.icecube.wisc.edu/event/68/contributions/4152/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4152/ END:VEVENT BEGIN:VEVENT SUMMARY:AMON Searches for Jointly-Emitting Neutrino + Gamma-Ray Transients DTSTART:20150505T213600Z DTEND:20150505T214800Z DTSTAMP:20261014T080200Z UID:indico-contribution-4153@events.icecube.wisc.edu DESCRIPTION:Speakers: Azadeh Keivani (The Pennsylvania State University)\n \nWe present the results of archival coincidence analyses between public n eutrino data from the 40-string and 59-string configurations of IceCube (I C40 and IC59) with contemporaneous public gamma-ray data from Fermi LAT an d Swift. Our analyses have the potential to discover statistically signifi cant coincidences between high-energy neutrinos and gamma-ray signals\, an d hence\, possible jointly-emitting neutrino/gamma-ray transients. This wo rk is an example of more general multimessenger studies that the Astrophys ical Multimessenger Observatory Network (AMON) aims to perform. AMON\, cur rently under development at Penn State\, will link multiple current and fu ture sensitive high-energy neutrino\, cosmic rays and follow-up observator ies as well as gravitational wave facilities. This single network enables near real-time coincidence searches for multimessenger astrophysical trans ients and their electromagnetic counterparts. During the talk\, we will pr esent the component high-energy neutrino and gamma-ray datasets\, the stat istical approaches that we used\, and the results of analyses of the IC40/ 59+LAT and IC40/59+Swift datasets.\n\nhttps://events.icecube.wisc.edu/even t/68/contributions/4153/ LOCATION:Union South URL:https://events.icecube.wisc.edu/event/68/contributions/4153/ END:VEVENT BEGIN:VEVENT SUMMARY:Theory benchmarks for IceCube-Gen2 DTSTART:20150505T200000Z DTEND:20150505T202000Z DTSTAMP:20261014T080200Z UID:indico-contribution-4154@events.icecube.wisc.edu DESCRIPTION:Speakers: Walter Winter (DESY)\n\nWe discuss quantitative benc hmarks from theoretical models for the optimization of the next generation volume upgrade of IceCube. Examples include the perspectives for flavor i dentification\, the searches for GRBs\, and the potential to use the Glash ow resonance to discriminate pp from pgamma interactions.\n\nhttps://event s.icecube.wisc.edu/event/68/contributions/4154/ LOCATION:The Marquee\, 2nd Floor (Union South) URL:https://events.icecube.wisc.edu/event/68/contributions/4154/ END:VEVENT END:VCALENDAR