MANTS Meeting
→
Europe/Berlin
Garching, Germany
Garching, Germany
LRZ Leibniz-Rechenzentrum der Bayerischen Akademie der Wissenschaften, Boltzmannstraße 1, 85748 Garching
<img alt src="https://events.icecube.wisc.edu/conferenceDisplay.py/getPic?picId=1&confId=52">
Directions to the <a href="http://www.lrz.de/wir/kontakt/weg_en/">LRZ</a>
Buy the XXL train ticket each day from downtown Munich. As you leave the Garching Forschungszentrum station, walk straight ahead along the avenue of poplar trees. Our building will then be the last one on the right, and Kim will be to the right after you go in the door on that corner.
You can check the price of your train ticket <a href="http://www.mvv-muenchen.de/en/homepage/index.html">here</a>
Description
The MANTS meeting will be in Garching, Germany near Munich on Oct 14-15. The fee for the meeting will be 150 Euros to be paid with cash upon arrival.
The banquet will be Monday night, 20:00 at CAVOS Taverna, Koeniginstraße, 34, 80802 Muenchen www.cavos-taverna.de.
The banquet will be Monday night, 20:00 at CAVOS Taverna, Koeniginstraße, 34, 80802 Muenchen www.cavos-taverna.de.
Participants
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Registration All Day
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Status and Highlights from Experiments: HE 009 - near Kim
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Baikal / GVD: Zhan-Arys Dzhilkibaev
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3
Baikal/GVDThe Prototyping phase of the BAIKAL-GVD project has been started in April 2011 with the deployment of a three string engineering array which comprises all basic elements and systems of the Gigaton Volume Detector (GVD) in Lake Baikal. In April 2012 the version of engineering array which comprises the first full-scale string of the GVD demonstration cluster has been deployed and operated during 2012. The first stage of the GVD demonstration cluster which consists of three strings is deployed in April 2013. We describe the configuration and design of the 2013 engineering array and discussed the first results of array operation.Speaker: Prof. Zhan-Arys Dzhilkibaev (Institute for nuclear research)
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3
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KM3Net: Uli Katz
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4
News from KM3NeTThe KM3NeT neutrino telescope in the Mediterranean Sea is approaching the first construction phase in 2014/15. The technical solutions to be implemented will be discussed and first results of prototyping activities presented. The talk will conclude with an outlook to the future plans for KM3NeT.Speaker: Prof. Uli Katz (ECAP / Univ. Erlangen)
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4
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Astrophysical Interpretation of IceCube Excess: Markus Ahlers
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11:00
Break
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Low Energy: Horsal HE 008
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6
Introducing WOM: The Wavelength-Shifting Optical ModuleLarge-scale underground water-Cherenkov neutrino observatories rely on single photon sensors whose sensitive area for Cherenkov photons one wants to maximise. Low dark noise rates and dense module spacing will thereby allow to substantially decrease the energy threshold in future projects. We describe a feasibility study of a novel type of single photon sensor that employs organic wavelength-shifting material (WLS) to capture Cherenkov photons and guide them to a PMT readout. Different WLS materials have been tested in lab measurements as candidates for use in such a sensor and photon capture efficiencies as high as 50 % have been achieved. Based on these findings we estimate that the effective photosensitive area of a prototype built with existing technology can easily exceed that of modules currently used e. g. in IceCube. Additionally, the dark noise rate of such a module can be exceptionally low in the order of 10 Hz. This is of special importance when targeting low-energy neutrinos that yield only few photons that need to be distinguished from noise hitsSpeaker: Lukas Schulte (o=bonn,ou=Institutions,dc=icecube,dc=wisc,dc=edu)
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6
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Simulations: Horsal HE 009
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8
Status of simulations for ORCASimulation activities for the feasibility study of ORCA for measuring the neutrino mass hierarchy are described. The two mainstream simulation chains, one with a 'reference' detector and one with a dense detector are presented.Speaker: Salvatore Galata (APC)
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9
The km3 simulation packageThe km3 simulation package is the standard software suite used by the ANTARES collaboration to simulate the emission and detection of Cherenkov photons. Here, the three programs comprising km3 are described, and the performance of km3's latest revision evaluated. Particular focus is paid to the use of the one-particle approximation, by which Cherenkov emission from hadronic cascades is simulated, and its applicability to ANTARES, KM3NeT, and ORCA.Speaker: Dr Clancy James (University of Erlangen-Nuernberg)
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10
Understanding Atmospheric Background in Neutrino TelescopesIn this presentation I'll review the importance to improve atmospheric neutrino production to probe the sources of systematics in the background estimation for neutrino telescopes. The generation of prompt components by heavy quark mesons is also discussed.Speaker: Dr Paolo Desiati (University of Wisconsin - Madison)
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Atmospheric muons rejection for ORCAA strong background for the observation of atmospheric neutrino induced upgoing muons is due to the presence of wrongly reconstructed muons. A strategy for the rejection of this background is presented, relying on the output of the reconstruction code "reco".Speaker: Mr Luigi Antonio Fusco (INFN and University of Bologna)
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8
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13:00
Lunch will be provided
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Future Detectors - Low Energy: HE 009 - near Kim
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Intrinsic physics limitations: Clancy James / Jannik Hofestadt
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16
Intrinsic physics limitations to reconstructionAt the characteristic energies (~20 GeV and below) at which ORCA/PINGU will look for hierarchy-dependent effects in the neutrino interaction rate, random fluctuations in the event characteristics will play a significant roll in limiting the accuracy of any reconstruction. In this contribution, the effects of such fluctuations in the determination of the energy and direction of muon tracks and shower events is investigated for neutrino interactions in seawater. These are presented as limitations both for a 'perfect' detector (all photons detected) and the reference ORCA detector, where only some photons will be detected.Speaker: Dr Clancy James (University of Erlangen-Nuernberg)
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16
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16:00
Break
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Future Detectors - Low Energy: HE 009 - near Kim
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Studies to PINGU's sensitivity to Neutrino Mass Hierarchy: Walter Winter
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17
PINGU mass hierarchy sensitivityI present an independent study of the PINGU mass hierarchy sensitivity based on the GLoBES (General Long Baseline Experiment Simulator) software, with the same methods and assumptions as used for the beam experiments. Particular attention will be given to the treatment of experiment properties and parameter correlations.Speaker: Dr Walter Winter (Wurzburg university)
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17
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Discussion
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Social Dinner - CAVOS Taverna, Koeniginstrasse, 34 80802 Muenchen www.cavos-taverna.de
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Reconstruction: High Energy - Horsal 008
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19
The cascade reconstruction in the Baikal experimentA new analysis of the data from the NT200 neutrino telescope based on the reconstruction of parameters for high-energy cascades generated in neutrino interactions has yielded new upper limits on the diffuse neutrino fluxes predicted by a number of theoretical models. The upper limit on the all-flavor neutrino flux with an energy spectrum E-2 is 2.9 10-7 GeV cm-2 s-1 ster-1Speaker: Bair Shaybonov (JINR)
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19
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Reconstruction: Low Energy - Konferenzraum - down the stairs across from Kim into the building next door, up one flight of stairs, and follow the signs to the room
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Reconstruction and energy estimation for tracksThe reconstruction algorithm used for the ORCA feasibility study will be described. The code reconstructs the direction of muon track coming from the muon neutrino and estimates the muon energy. The performance of the algorithm will be shown.Speaker: Agata Trovato (LNS - INFN)
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25
Reconstruction and energy estimation for tracksResults for an alternative track reconstruction in Orca using the GridFit method developed within Antares.Speaker: Mr Robert Bormuth (Nikhef)
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A particle identification algorithm for PINGUWe will describe a particle identification algorithm based on identification of "superluminal" hits -- photons arriving earlier than expected from propagation of light from a reconstructed cascade vertex.Speaker: Ty DeYoung (o=psu,ou=Institutions,dc=icecube,dc=wisc,dc=edu)
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11:00
Break
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Future Detectors - High Energy: Horsaal 008
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Neutrino Self-Veto: Tom Gaisser
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28
Atmospheric neutrino self-vetoMuons produced in the same event as an atmospheric neutrino will exclude the atmospheric neutrino from a sample of events required to originate inside a fiducial volume of a detector. I will discuss how the veto is evaluated for use in the IceCube High Energy Starting Event analysis.Speaker: Thomas Gaisser (University of Delaware)
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28
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Intermediate energy starting tracks: Jacob Feintzeig
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29
Lowering IceCube's energy threshold for point source searches in the southern skyVeto techniques are opening up new doors for point source searches in IceCube. Traditional IceCube point source analyses are only sensitive to PeV-scale fluxes in the southern hemisphere. We demonstrate that extending the “high-energy starting event” veto to lower energies allows IceCube to probe southern sky sources in the 10 TeV – 1 PeV regime. After discussing the event selection and analysis method, we will show projected sensitivities and compare them to ANTARES point source analyses.Speaker: Jacob Feintzeig (University of Wisconsin--Madison)
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29
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Veto and HE Starting Events - Nathan Whitehorn
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Air Cherenkov Surface Veto: Tyce DeYoung
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A low energy air Cherenkov veto systemPreliminary ideas regarding a surface veto array based on simple imaging air Cherenkov telescopes will be presented. Early studies suggest that cosmic ray primaries responsible for atmospheric neutrinos above an energy threshold of a few TeV could be tagged efficiently.Speaker: Tyce DeYoung (o=psu,ou=Institutions,dc=icecube,dc=wisc,dc=edu)
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31
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12:45
Lunch
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Future Detectors - High Energy: Horsaal 008
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Considerations for surface veto strategies / IceVeto: Albrecht Karle / Jan Auffenberg
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32
Considerations for a surface veto array and a look at event ratesI will have a brief look at a surface veto array upgrade. Simulated event rates in IceCube suggest that surface veto detectors will add of order 10 muon neutrino events after atmospheric veto cut depending the threshold. Such strategies may offer benefits for lower energy source searches. They need to be compared to other muon neutrino search channels.Speaker: Albrecht Karle (o=uwmad,ou=Institutions,dc=icecube,dc=wisc,dc=edu)
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32
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Multi-string extensions / IceCube ++ studies: Christopher Wiebusch / David Altmann
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Discussion
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Future Directions in Neutrino Astronomy: Horsaal 008
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Global Neutrino Telescope Coordination: Christian Spiering / TBD
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Panel Discussion
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