PAHEN 2019, Berlin
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Europe/Berlin
1.101 (HU Berlin)
1.101
HU Berlin
Dorotheenstraße 24
10117 Berlin
Germany
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Registration: Is open during the conference. 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany -
12:30
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13:30
Lunch 1h on your own
on your own
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Presentation of recent results: Chair: Markus Ackermann 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany- 13:40
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14:10
Measurement of the diffuse astrophysical muon neutrino spectrum with ten years of IceCube data 20mThe IceCube Neutrino Observatory has established the measurement of a flux of high-energy astrophysical neutrinos in several detection channels. Here, we present an update to the analysis of through-going muon-neutrinos from the Northern Hemisphere. It was extended to almost ten years of data which have been re-processed (Pass-2) applying consistent event-selections and reconstructions. Additionally, an improved treatment of systematic uncertainties on the atmospheric fluxes was implemented. We present results of the updated spectral fit and discuss how the measurement compares to other results.Speaker: Joeran Stettner (RWTH Aachen University)
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Results from the ANITA Experiment 30mI will summarize results to date from ANITA, a NASA Long Duration Balloon payload that has had four successful flights in Antarctica. ANITA is sensitive to two kinds of radio emission from particle showers: Askaryan emission from ultra-high energy (UHE) neutrinos interacting in the Antarctic ice, and Geomagnetic emission from UHE particles showering in the atmosphere. The latter channel is sensitive to cosmic ray air showers and air showers from any other UHE particles, such as tau leptons created in charged current tau neutrino interactions in the Earth or ice. I will discuss the results from searches in these channels with ANITA and possible interpretations of events observed with ANITA. I will also discuss a proposed follow-up NASA balloon mission, the Payload for Ultrahigh Energy Observations (PUEO), which will improve on ANITA’s sensitivity dramatically, improving sensitivity to UHE neutrinos in this energy regime, and providing follow-up on the events observed thus far with ANITA.Speaker: Abigail Vieregg (University of Chicago)
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Coffee Break 30m
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Overview of neutrino sources 1: Chair: Walter Winter 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany-
16:00
Neutrinos from blazars 30mIceCube has recently reported the discovery of high-energy neutrinos of astrophysical origin, opening up the PeV sky. These observations are challenging to interpret on the astronomical side and have triggered a fruitful collaboration across particle and astro-physics. I will present our work on blazars as possible neutrino sources, discuss briefly the association of some very high-energy IceCube neutrinos with the blazar TXS 0506+056, and show that TXS 0506+056 is not what it looks like.Speaker: Dr Paolo Padovani (European Southern Observatory)
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Postersession 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany
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The TXS 0506+056: Chair: Anna Franckowiak 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany-
09:00
High-Energy neutrinos from AGN? 30mActive Galactic Nuclei (AGN) have long been suggested among the candidate sources of cosmic high-energy neutrinos. If hadronic processes operate in the AGN jets, a lot can be learnt by combining neutrino observations with the putative accompanying electromagnetic information. This is motivated by the fact that both radiations may be pictured in the same astrophysical particle-cascades scenario, cascades that are ultimately originated by cosmic rays. While to date, no neutrino point sources have been identified at high confidence, a promising ground for discovery could be the search for transient and variable neutrino/electromagnetic sources, in which case the atmospheric neutrino and muon backgrounds can be reduced by taking advantage of time- and space-coincidence. Recent outcomes in this field will be presented.Speaker: Dr Sara Buson (NASA-GSFC)
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Coffee Break 30m
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Overview of neutrino sources, 2: Chair: Andrea Palladino 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany- 11:00
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11:30
Diffuse Neutrino Flux from Jetted AGN 20mActive galactic nuclei (AGN) with relativistic jets powered by accretion onto their central supermassive black hole are the most powerful persistent sources of electromagnetic radiation in the Universe, with bolometric luminosities of $\sim 10^{43}-10^{48}$ erg s$^{-1}$. Jetted AGN are promising cosmic ray accelerators and have abundant radiation fields for the production of high-energy neutrinos. As a result, they have been suggested as possible neutrino sources long before the discovery of an astrophysical neutrino flux by IceCube. In light of observational constraints and the recent neutrino detections associated with the blazar TXS 0506+056, I am going provide an overview of theoretical predictions for the diffuse neutrino flux from jetted AGN.Speaker: Dr Maria Petropoulou Petropoulou (Princeton University)
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11:50
Neutrinos from optical transients with IceCube 20mSince the detection of high-energy cosmic neutrinos at the IceCube Neutrino Observatory in 2013, there has been an on-going search to find suitable transient or variable source candidates. Despite recent evidence identifying a flaring blazar as a likely neutrino source, the vast majority of the diffuse neutrino flux measured by IceCube remains unexplained. The latest IceCube results testing time-dependent correlation between neutrinos and optical transients will be presented.Speaker: Mr Robert Stein (DESY Zeuthen)
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Lunch 1h 30m on your own
on your own
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Multi-messenger physics: Chair: Elil Waxman 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany- 14:00
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14:30
Neutrinos from NS-NS mergers 20mThe mergers of neutron stars are expected to produce high-energy neutrinos through particle acceleration inside the relativistic jets. In this talk, I will discuss future prospects for high-energy neutrino detection coincident with gravitational waves. We consider two neutrino production scenarios. One is the late-time engine activity of the short gamma-ray bursts. High-energy neutrinos are efficiently produced in the jets of the prolonged activity owing to their lower Lorentz factor. The other is choked jet systems where the relativistic jets fail to penetrate the merger ejecta. In this case, photons are absorbed by the ejecta, while neutrinos escape from the system and can be detected. For both scenarios, the future project, such as IceCube-Gen2, will likely detect the neutrinos coincident with gravitational waves.Speaker: Dr Shigeo Kimura (Tohoku University)
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Coffee Break 30m
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Future perspective 1: Chair: Marek Kowalski 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany-
16:00
IceCube-Upgrade and IceCube-Gen2 30mAfter the discovery of high-energy cosmic neutrinos and the likely observation of a first neutrino source with the IceCube neutrino telescope, the realization of a next generation neutrino telescope at the South Pole, IceCube-Gen2, is progressing. As a first step, the IceCube detector will be upgraded with seven new strings to be deployed near the center of the existing detector during during the 2022/23 Polar season. The main goals are world-leading sensitivity to neutrino oscillation physics including tau neutrino appearance and significantly improved calibration of the existing detector which can also be applied to archival data. IceCube-Gen2 will then consist of additional ~140 strings which will instrument 8 km3 of ice with the main goal of high-energy neutrino astrophysics. The talk discusses the physics case for both detectors and presents the current project status.Speaker: Alexander Kappes
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The Giant Radio Array for Neutrino Detection 30mThe Giant Radio Array for Neutrino Detection (GRAND) project aims to detect ultra-high-energy cosmic neutrinos, cosmic rays, and gamma rays with a radio antenna array deployed over a total area of 200 000 km2 in mountainous regions, in several favorable locations around the world. The strategy of GRAND is to detect air showers above 10^17 eV that are induced by the interaction of high-energy particles in the atmosphere or in the Earth crust, through its associated coherent radio-emission in the 50-200 MHz range. In its final configuration, GRAND plans to reach a sensitivity of ~10^{-10} GeV cm^-2 s^-1 sr^-1 above 5*10^{17} eV and a sub-degree angular resolution. The 300-antenna pathfinder array, GRANDProto300 is planned to be deployed in 2021. It aims at demonstrating autonomous radio detection of inclined air-showers, and make measurements of the composition and the muon content of cosmic rays around the ankle energy. In this talk, we will show preliminary designs and simulation results, plans for the ongoing, staged approach to construction, and the rich research program made possible by the proposed sensitivity and angular resolution.Speaker: Dr Kumiko Kotera (Institut d'Astrophysique de Paris)
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Dinner 4h Pier13, Tempelhofer Damm 227, 12099 Berlin
Pier13, Tempelhofer Damm 227, 12099 Berlin
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Neutrino oscillations: Chair: Gennaro Miele 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany- 09:00
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Coffee Break 20m
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BSM and Future perspective 2: Chair: Christian Spiering 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany-
11:20
ANITA events and interpretations in terms of BSM physics 20mSpeaker: Derek Brindley Fox
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Closing 1.101
1.101
HU Berlin
Dorotheenstraße 24 10117 Berlin Germany
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