Recent Developments of the Real-Time Capabilities of IceCube
|
|
|
- Darlene Mitchell
- 5 years ago
- Views:
Transcription
1 Recent Developments of the Real-Time Capabilities of IceCube Thomas Kintscher for the IceCube Collaboration TAUP 2015 Neutrinos B Torino, 2015/09/10
2 Multi-Messenger Observations > Combination of different messengers: Increased sensitivity Obtain the complete picture o ot Pr > IceCube: 4π 24/7 trigger capability > Follow-Up Observatories: Ne utr in ns Ph oto ns os Sensitive to different wavelengths/messengers Limited field of view, weather-dependent Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 2
3 Transient and Variable Sources > Temporal evolution of astrophysical objects GRB: s AGN flare: ~ 10 d SN: ~ 100 d > Wide variety of timescales for evolution > Detectable in time-dependent analyses > Improved sensitivity from multi-wavelength observations Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 3
4 The IceCube Neutrino Observatory > 1km³ detector for Cherenkov light > In this talk: μ-tracks from CC νμ-int. > Angular resolution of 1 deg Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 4
5 The Follow-Up Procedure Photons AGN/SN/GRB/... Neutrinos IceCube Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 5
6 The Follow-Up Procedure Analysis Alerts! Photons Iridium AGN/SN/GRB/... Events Neutrinos IceCube Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 6
7 (Current) Follow-Up Observatories > Gamma rays MAGIC (1 alert / year) VERITAS (3 alerts / year) HESS (t.b.d.) Energy ranges: ~ 50 GeV 50 TeV FoV: ~ 3.5 deg. > Optical PTF (9 alerts / year) > FoV: 7.3 sq. deg. ZTF (under construction) > FoV: 47 deg. > X-rays: SWIFT-XRT (7 alerts / year) FoV: 0.4 deg. ( 1.1 deg.) Energy: kev Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 7
8 Follow-Up System in IceCube > Real-time event selection at the South Pole Fast event reconstruction and filtering Pick well-reconstructed tracks > Likelihood analysis in the North Optical/X-Ray: short timescale (fixed to 100 s), all-sky Gamma-Ray: variable clustering of events (up to 21 d), source list Significance calculation Alert generation > Forwarding to follow-up observatories Test of source visibility Contacted by automated s AMON stream: sub-threshold events for correlation analyses > Total latency: a few minutes! Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 8
9 Status: Follow-Up with Gamma-Ray Observation > Marginalized likelihood: Si/Bi: PDFs containing spatial, energy and timing information > Test statistic: > Significance threshold determined by allocated observation time: VERITAS: -log10(p) = (3.5σ) 40% observation probability (weather, etc.) ~ 3 alerts / year Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 9
10 Status: Alerts from Gamma-Ray Follow-Up > Running stable since March 2012 > Number of physics alerts sent so far: 14 > Latest alert: 2015/07/05 Nobserved: 4 Duration: 1.2 d -log10(pre-trial p-value): > Alert forwarded to VERITAS > No observation due to scheduled maintenance... 1 deg Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 10
11 Status: Alerts from Gamma-Ray Follow-Up > Running stable since March 2012 > Number of physics alerts sent so far: 14 > Most significant: 2012/11/09 Nobserved: 6 Duration: d -log10(pre-trial p-value): > Alert forwarded to VERITAS > No significant evidence for gamma-ray emission seen 1 deg Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 11
12 Status: Follow-Up with Optical/X-ray Observations > Tracks from the northern sky > Closely clustered events on very short timescales Angular distance: < 3.5 Temporal distance: < 100 s > Test quantity: angular separation, reconstruction quality, events in telescope's FoV, small time intervals > Forwarding to PTF: 9 alerts / year SWIFT: 7 alerts / year Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 12
13 Status: Alerts from Optical/X-ray Follow-Up > 2012/03/30: Most significant OFU alert to PTF Two neutrinos within 1.7 s > Detection of core-collapse supernova PTF12csy within 0.14 deg Distance: 300 Mpc Age: > 169 days > p-value: (2.6σ) > Chance detection, neutrinos likely unrelated to SN > [arxiv: ], accepted by ApJ NEW REF SUB SDSS Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 13
14 Status: No triplet from Optical/X-ray Follow-Up > After 3 years: no triplet observed! > Assume: Diffuse ν-flux from GRBs Number of triplets? SWIFT: ~1500 GRBs/year/hemisphere > 4500 GRBs emitting diffuse flux > 10s of GRBs generating triplets > but none observed! Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 14
15 Status: No triplet from Optical/X-ray Follow-Up > After 3 years: no triplet observed! > Assume: Diffuse ν-flux from GRBs Number of triplets? SWIFT: ~1500 GRBs/year/hemisphere > 4500 GRBs emitting diffuse flux > 10s of GRBs generating triplets > but none observed! > brightest GRB: < 3 neutrinos! > Scaled contribution from GRBs yields limit on astrophysical ν-flux! (Paper in preparation by Nora Linn Strotjohann et al.) Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 15
16 Summary and Outlook Mature selection of high-quality tracks in real-time Several running analyses: gamma-ray, optical, x-ray Physics results: Chance observation of supernova Limits on transients Physics analysis and alert distribution within 5 minutes! > Improved event selection More precise angular error estimator, latest reconstructions better sensitivity... > Generic analysis: unbiased all-sky, arbitrary timescales Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 17
17 Thank you for your attention! Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 18
18 Backup Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 19
19 Status: Recent Alerts from GFU > Running stable since March 2012 > Number of physics alerts sent so far: 14 Time (UTC) -log10(pre-trial p-value) Nobs Duration (days) Follow-up :47: No :53: No :52: Yes (MAGIC) No :28: Yes (VERITAS) Yes :36: No :10: (4.01) 8 (10) (20.73) Yes (MAGIC) No :18: (4.59) 8 (10) (19.667) Yes (VERITAS) Yes :28: Yes (MAGIC) No :42: No :47: No :05: Yes (VERITAS) Yes :00: (5.04) 3 (4) (0.576) Yes (VERITAS) No :55: No Experiment observed Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page
20 Updates for IC86-5: Single Event Stream Trigger Trigger Level 1 (µ tracks) Level 1 (µ tracks) Level 2 (hq selection) Level 2 (hq selection) Straight Cuts Binned Analysis Alert Generation For each: OFU/ GFU BDT Selection LLH Analysis Visibility/Significance Alert Generation Follow-Up Observatory South Pole > New Design: For each: OFU/ GFU Follow-Up Observatory > Recent SPTS testing successful! Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 22 North > Previous Design:
21 Updates for IC86-5: GFU BDT Selection > Old: straight cuts, upgoing only > New: BDT event selection using PyBDT Upgoing BDT > Trained with spectrum of -2.7 > Training Variables: Bayesian LLH Ratio (MPE Fit, Line Fit) Length of direct hits (Time Window C) Number of direct hits (Time Window C) Speed from Line Fit MPE Fit Zenith Log10(MuE) Scaled MPE llh: -log L / (Ndom 3.5) Max(cos(SplitFit Zenith) cos(mpe Zenith)) Cos(Min(SplitFit Zenith)) cos(mpe Zenith) 0.5 Separation Empty distance / Length of direct hits (C) Smoothness (Sall) Log10(Qtot) Distance to `Center of Gravity' Downgoing BDT > Combination of spectral weights -1, -2 and -3 > Same training variables > No Bayesian LLH Ratio Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 23
22 Updates for IC86-5: GFU BDT Selection > Upgoing BDT: Efficiency: Rate: > Compared to straight cuts: Method Data rate Atm. Nu Rate E-2 efficiency Straight Cuts 2.0 mhz 1.9 mhz 69 % BDT Cut 1.9 mhz 1.7 mhz 81 % (+12%) Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 24
23 Updates for IC86-5: GFU BDT Selection > Downgoing BDT: Rate: ~ 0.1 mhz in each bin Piecewise polynomial fit Zenith-dependent BDT Cut > Total rate: ~7 mhz Upgoing: 2 mhz Downgoing: 5 mhz ~110 kb/day via Prio-1 Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 25
24 Updates for IC86-5: GFU Likelihood Analysis > Unbinned likelihood: > Test statistic: > Significance threshold determined by observation time: VERITAS: -log10(p) = (3.5σ) 40% observation probability (weather, etc.) ~ 1 event / year Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 26
25 Updates for IC86-5: Real-time Monitoring > 'Good Run List' not available online > Need to assess detector stability and event quality in real-time Clustering of events recorded during stable running conditions Detector live time influences likelihood > Current GFU stability criteria: In-Ice Simple Multiplicity Trigger Muon Filter rate Online Level 2 Filter rate > Sliding window averages: > Stability score: Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 27
26 Updates for IC86-5: Real-time Monitoring > Very good agreement with Good Run List > Conservative live time estimate > Previously: Queried from Pole > New setup: Needs input from Madison Until now: Rates transferred with Prio-2 via I3Live >Desirable: Transfer trigger rates with Prio-1 Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 28
27 Future Plans for GFU/OFU/XFU > Similar event selections for OFU and GFU Merge! Also a generalised likelihood? > Meanwhile: Better reconstructions available in Online Level 2 Make use of them! (fast) SplineMPE Paraboloid for upgoing events Further improvements possible? > Sensitivity study: Plot using current selection Goal: Come close to offline PS sensitivity! Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 29
28 Summary > Previously: GFU/OFU/XFU run reliably for years Established feasibility of online follow-up > What we did recently: Introduced Online Single Event Stream OFU/GFU BDT Pole (now) Southern sky included! Likelihood Madison (very soon) > What we need: Real-time stability monitoring > What happens next: Alert forwarding to HESS Common event selection, improved sensitivity Thomas Kintscher Real-Time Capabilities of IceCube 2015/09/10 Page 30
Multiwavelength Search for Transient Neutrino Sources with IceCube's Follow-up Program
Multiwavelength Search for Transient Neutrino Sources with IceCube's Follow-up Program Nora Linn Strotjohann for the DESY Real-Time Group GROWTH Meeting at Caltech, July 26th 2016 The IceCube Neutrino
A new IceCube starting track event selection and realtime event stream
A new IceCube starting track event selection and realtime event stream Sarah Mancina Kyle Jero Advisor: Albrecht Karle Neutrino Parallel TeVPA 2017 Columbus, OH August 8th, 2017 IceCube and Atmospheric
IC59+40 Point Source Analysis. Mike Baker, Juan A Aguilar, Jon Dumm, Chad Finley, Naoko Kurahashi, Teresa Montaruli. 12 May 2011
IC59+40 Point Source Analysis Mike Baker, Juan A Aguilar, Jon Dumm, Chad Finley, Naoko Kurahashi, Teresa Montaruli 12 May 2011 http://wiki.icecube.wisc.edu/index.php/ic59+40_point_source_analysis Goals
The Shadow of the Moon in IceCube
The Shadow of the Moon in IceCube Laura Gladstone University of Wisconsin, Madison for the IceCube Collaboration Young Scientists Forum 46th Rencontres de Moriond La Thuile, Italy 1 Motivation: we know
The Present and Future Real-Time Alerts from AMON
The Present and Future Real-Time Alerts from AMON TeVPA August 9th 2017 AMON team 1 Outline What and who is AMON What s being/been done Upcoming AMON - ν alerts 2 The AMON Idea AMON searches for multimessenger
PoS(ICRC2015)1052. Neutrino-triggered target-of-opportunity programs in IceCube. The IceCube Collaboration,
Neutrino-triggered target-of-opportunity programs in IceCube The IceCube Collaboration, http://icecube.wisc.edu/collaboration/authors/icrc15_icecube E-mail: Dariusz.Gora@desy.de IceCube is capable of monitoring
Multi-Messenger Programs in ANTARES: Status and Prospects. Véronique Van Elewyck Laboratoire AstroParticule et Cosmologie (Paris)
Multi-Messenger Programs in ANTARES: Status and Prospects Laboratoire AstroParticule et Cosmologie (Paris) An overview Externally triggered neutrino searches: the example of GRBs Strategies for data acquisition
Multi-messenger studies of point sources using AMANDA/IceCube data and strategies
Multi-messenger studies of point sources using AMANDA/IceCube data and strategies Cherenkov 2005 27-29 April 2005 Palaiseau, France Contents: The AMANDA/IceCube detection principles Search for High Energy
Follow-up of high energy neutrinos detected by the ANTARES telescope
Follow-up of high energy neutrinos detected by the ANTARES telescope, on behalf of the ANTARES, TAROT, ROTSE, MASTER and SWIFT Collaborations Aix Marseille Université, CNRS/IN2P3, CPPM UMR 7346, 13288,
Cosmic Neutrinos in IceCube. Naoko Kurahashi Neilson University of Wisconsin, Madison IceCube Collaboration
Cosmic Neutrinos in IceCube Naoko Kurahashi Neilson University of Wisconsin, Madison IceCube Collaboration HEM KICP UChicago 6/9/2014 1 Outline IceCube capabilities The discovery analysis with updated
Towards Neutrino Astronomy with IceCube+ANTARES+KM3NeT
Towards Neutrino Astronomy with IceCube+ANTARES+KM3NeT Vincent Bertin (CPPM) on behalf of Damien Dornic (CPPM) FCPPL meeting @ Marseille Marseille 25 May 2018 NEUTRINO AS COSMIC MESSENGER Neutrinos: smoking
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis: http://area51.berkeley.edu/manuscripts Goals! Perform an all-sky search
High-energy neutrino detection with the ANTARES underwater erenkov telescope. Manuela Vecchi Supervisor: Prof. Antonio Capone
High-energy neutrino detection with the ANTARES underwater erenkov telescope Supervisor: Prof. Antonio Capone 1 Outline Neutrinos: a short introduction Multimessenger astronomy: the new frontier Neutrino
Astroparticle Physics with IceCube
Astroparticle Physics with IceCube Nick van Eijndhoven nickve.nl@gmail.com http://w3.iihe.ac.be f or the IceCube collaboration Vrije Universiteit Brussel - IIHE(ULB-VUB) Pleinlaan 2, B-1050 Brussel, Belgium
High energy neutrino astronomy with the ANTARES Cherenkov telescope
High energy neutrino astronomy with the ANTARES Cherenkov telescope P.Vernin CEA/Irfu/SPP On behalf of the ANTARES collaboration IWARA 2009 Conference Maresias, Sao Paulo, Brazil, 4-8/10/2009 i r f u saclay
Searches for astrophysical sources of neutrinos using cascade events in IceCube
Searches for astrophysical sources of neutrinos using cascade events in IceCube Mike Richman TeVPA 2017 August 8, 2017 Source Searches with IceCube Cascades TeVPA 17 Mike Richman (Drexel University) 1
Recent Observations of Supernova Remnants
1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) 2 Contents Supernova Remnants
IceCube: Dawn of Multi-Messenger Astronomy
IceCube: Dawn of Multi-Messenger Astronomy Introduction Detector Description Multi-Messenger look at the Cosmos Updated Diffuse Astrophysical Neutrino Data Future Plans Conclusions Ali R. Fazely, Southern
THE EHE EVENT AND PROSPECTS FROM THE ICECUBE NEUTRINO OBSERVATORY. Lu Lu 千葉大
THE EHE EVENT 170922 AND PROSPECTS FROM THE ICECUBE NEUTRINO OBSERVATORY Lu Lu 千葉大 2 3 On-source n p TeV - PeV pp p n The Cosmic Neutrinos TeV->EeV p gp p n photopion production n GZK cosmogenic n EeV
High Energy Neutrino Astrophysics Latest results and future prospects
High Energy Neutrino Astrophysics Latest results and future prospects C. Spiering, Moscow, August 22, 2013 DETECTION PRINCIPLE Detection Modes Muon track from CC muon neutrino interactions Angular resolution
Antonio Capone Univ. La Sapienza INFN - Roma
Observations of HE Neutrino and Multimessenger AstroParticle Physics Antonio Capone Univ. La Sapienza INFN - Roma 1 Talk outline High Energy Astrophysical Neutrino Detection in a multi-messenger scenario
A Summary of recent Updates in the Search for Cosmic Ray Sources using the IceCube Detector
A Summary of recent Updates in the Search for Cosmic Ray Sources using the IceCube Detector The IceCube Collaboration E-mail: tessa.carver@unige.ch In 2012 the IceCube detector observed the first clear
IceCube: Ultra-high Energy Neutrinos
IceCube: Ultra-high Energy Neutrinos Aya Ishihara JSPS Research Fellow at Chiba University for the IceCube collaboration Neutrino2012 at Kyoto June 8 th 2012 1 Ultra-high Energy Neutrinos: PeV and above
Neutrinos from the Milky Way. 18th Symposium on Astroparticle Physics in the Netherlands Erwin Visser
Neutrinos from the Milky Way 18th Symposium on Astroparticle Physics in the Netherlands 23-10-2013 Erwin Visser Outline How are these neutrinos produced? Why look for them? How to look for them The ANTARES
Detector Stability on short time scales
Detector Stability on short time scales 1 I am going to talk about... Tests used in an offline GRB analysis Cumulative Test Likelihood Test Tests for online burst filter 2 Tests used in an offline GRB
Gamma-rays, neutrinos and AGILE. Fabrizio Lucarelli (ASI-SSDC & INAF-OAR)
Gamma-rays, neutrinos and AGILE Fabrizio Lucarelli (ASI-SSDC & INAF-OAR) Outlook 2 Overview of neutrino astronomy Main IceCube results Cosmic neutrino source candidates AGILE search for γ-ray counterparts
Measuring the neutrino mass hierarchy with atmospheric neutrinos in IceCube(-Gen2)
Measuring the neutrino mass hierarchy with atmospheric neutrinos in IceCube(-Gen2) Beyond the Standard Model with Neutrinos and Nuclear Physics Solvay Workshop November 30, 2017 Darren R Grant The atmospheric
Catching Neutrinos with an IceCube
Catching Neutrinos with an IceCube Mathieu Labare (for the IceCube Collaboration) Vrije Universiteit Brussel - IIHE mlabare@icecube.wisc.edu 04 04 2011, Neutrino-Gamma Workshop @ Marseille IceCube Collaboration
neutrino astronomy francis halzen university of wisconsin
neutrino astronomy francis halzen university of wisconsin http://icecube.wisc.edu 50,000 year old sterile ice instead of water we built a km 3 neutrino detector 3 challenges: drilling optics of ice atmospheric
Multi-wavelength follow-up observations of ANTARES neutrino alerts
Multi-wavelength follow-up observations of ANTARES neutrino alerts D. Dornic (CPPM) D. Turpin (IRAP), M. Ageron, V. Bertin, J. Brunner, A. Mathieu (CPPM), F. Schüssler, B. Vallage (CEA/IRFU), S. Basa (LAM)
Mariola Lesiak-Bzdak. Results of the extraterrestrial and atmospheric neutrino-induced cascade searches with IceCube
Results of the extraterrestrial and atmospheric neutrino-induced cascade searches with IceCube Mariola Lesiak-Bzdak Stony Brook University for IceCube Collaboration Geographic South Pole" Outline: } Motivation
Neutrino Astronomy at the South Pole AMANDA and IceCube
1 Neutrino Astronomy at the South Pole AMANDA and IceCube Ignacio Taboada University of California - Berkeley Topics in Astroparticle and Underground Physics Zaragoza. Sept 10-14, 2005 2 The IceCube Collaboration
Neutrino Astronomy with IceCube at the Earth's South Pole
Neutrino Astronomy with IceCube at the Earth's South Pole Naoko Kurahashi Neilson (Drexel University) Yale NPA Seminar, Jan 26th, 2017 1 How it started... Highest energy particles observed Charged particles
VERS UNE ASTRONOMIE NEUTRINO AVEC IceCube+ANTARES+KM3NeT
VERS UNE ASTRONOMIE NEUTRINO AVEC IceCube+ANTARES+KM3NeT DAMIEN DORNIC (CPPM) CFR Cos: Meeting de la communauté de recherche sur le rayonnement cosmique!! APC - 26-28 mars 2018 NEUTRINO AS COSMIC MESSENGER
Lawrence Berkeley National Laboratory Lawrence Berkeley National Laboratory
Lawrence Berkeley National Laboratory Lawrence Berkeley National Laboratory Title Neutrino Physics with the IceCube Detector Permalink https://escholarship.org/uc/item/6rq7897p Authors Kiryluk, Joanna
Cherenkov Telescope Array ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP
Cherenkov Telescope Array A SENSITIVE PROBE OF EXTREME UNIVERSE ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP 2015 1 The CTA Observatory SST ( 4m) LST ( 23m) MST ( 12m) South North
Status of the MAGIC telescopes
SNOWPAC 2010 Status of the MAGIC telescopes Pierre Colin for the MAGIC collaboration Max-Planck-Institut für physik (Munich) Status of the MAGIC telescopes MAGIC-1 MAGIC-2 Outline: Recent results of the
Neutrino Radiography of the Earth with the IceCube Neutrino Observatory
Neutrino Radiography of the Earth with the IceCube Neutrino Observatory Dec.4. 2012 AGU Fall Meeting 2012 in San Francisco Kotoyo Hoshina, Hiroyuki Tanaka and IceCube Collaboration Scan our Earth with
Search for Point-like. Neutrino Telescope
Search for Point-like Sources with the ANTARES Neutrino Telescope Francisco Salesa Greus IFIC (CSIC Universitat de València, Spain) On behalf of the ANTARES collaboration Outline Neutrino astronomy. The
Search for diffuse cosmic neutrino fluxes with the ANTARES detector
Search for diffuse cosmic neutrino fluxes with the ANTARES detector Vladimir Kulikovskiy The ANTARES Collaboration 1 Overview ANTARES description Full sky searches Special region searches Fermi bubbles
Search for GeV neutrinos associated with solar flares with IceCube
Search for GeV neutrinos associated with solar flares with IceCube The IceCube Collaboration http://icecube.wisc.edu/collaboration/authors/icrc17_icecube E-mail: gdewasse@icecube.wisc.edu Since the end
Muon Reconstruction in IceCube
Muon Reconstruction in IceCube K.Hoshina for the IceCube collaboration June 26 2008 International workshop on High Energy Earth Science in Tokyo Introduction 2 IceCube is... A cubic-kilometer neutrino
A Multimessenger Neutrino Point Source Search with IceCube
A Multimessenger Neutrino Point Source Search with IceCube Mădălina Chera FLC Group Meeting 04.10.2010 Mădălina Chera Overview 1 Introduction to UHE Cosmic Rays and Neutrino Astrophysics; 2 Motivation
MWL. A Brief Advertisement Before Your Regularly Scheduled Program
MWL A Brief Advertisement Before Your Regularly Scheduled Program PKS 1441+25 PKS 1441+25 z=0.939! VHE detection over more than a single day! PKS 1441+25 37.7% polarization! PKS 1441+25 Continues optical
IceCube Results & PINGU Perspectives
1 IceCube Results & PINGU Perspectives D. Jason Koskinen for the IceCube-PINGU Collaboration koskinen@nbi.ku.dk September 2014 Neutrino Oscillation Workshop Otranto, Lecce, Italy 2 IceCube Detector ~1km
Heaven-Sent Neutrino Interactions From TeV to PeV
Heaven-Sent Neutrino Interactions From TeV to PeV Mauricio Bustamante Niels Bohr Institute, University of Copenhagen UCL HEP Seminar London, December 08, 2017 Two seemingly unrelated questions 1 Where
On the scientific motivation for a wide field-of-view TeV gamma-ray observatory in the Southern Hemisphere
On the scientific motivation for a wide field-of-view TeV gamma-ray observatory in the Southern Hemisphere for the HAWC collaboration E-mail: miguel@psu.edu Observations of high energy gamma rays are an
Detection of transient sources with the ANTARES telescope. Manuela Vecchi CPPM
Detection of transient sources with the ANTARES telescope Manuela Vecchi CPPM Multimessenger Astronomy CRs astronomy feasible at energies higher than 1019 ev extragalactic origin UHECRs horizon limited
The Astrophysical Multimessenger Observatory Network: Science, Infrastructure, and Status
The Astrophysical Multimessenger Observatory Network: Science, Infrastructure, and Status Azadeh Keivani (For the AMON Team) The Pennsylvania State University NASA s Goddard Space Flight Center April 7,
Neutrinos as astronomical messengers
I Taboada / Georgia Tech Aug 10, 2010 Neutrinos as astronomical messengers Photon 10 21 B 10 18 Neutrino 10 15 Cosmic ray 10 12 10 9 High- energy neutrino detec5on: tradi5onal way Astrophysical neutrino
PoS(NOW2016)041. IceCube and High Energy Neutrinos. J. Kiryluk (for the IceCube Collaboration)
IceCube and High Energy Neutrinos Stony Brook University, Stony Brook, NY 11794-3800, USA E-mail: Joanna.Kiryluk@stonybrook.edu IceCube is a 1km 3 neutrino telescope that was designed to discover astrophysical
FACT. Alerts from TeV Gamma Rays in the Context of Multi Messenger Astrophysics. Daniela Dorner for the FACT Collaboration
FACT Alerts from TeV Gamma Rays in the Context of Multi Messenger Astrophysics for the FACT Collaboration First G APD Cherenkov Telescope Major Goals Proof of principle: Silicon based photo sensors (G
Earth WIMP search with IceCube. Jan Kunnen for the IceCube Collaboration
Earth WIMP search with IceCube Jan Kunnen for the IceCube Collaboration 1 Outline 1. Indirect Earth WIMP detection with neutrinos I. how, II. status, III. theoretical predictions 2. The IceCube Neutrino
How bright can the brightest neutrino source be?
TeV Particle Astrophysics Columbus, OH August, 2017 How bright can the brightest neutrino source be? Shin ichiro Ando University of Amsterdam Ando, Feyereisen, Fornasa, Phys. Rev. D 95, 3003 (2017) Lessons
Particle Physics Beyond Laboratory Energies
Particle Physics Beyond Laboratory Energies Francis Halzen Wisconsin IceCube Particle Astrophysics Center Nature s accelerators have delivered the highest energy protons, photons and neutrinos closing
VERITAS Observations of Starburst Galaxies. The Discovery of VHE Gamma Rays from a Starburst Galaxy
VERITAS Observations of Starburst Galaxies The Discovery of VHE Gamma Rays from a Starburst Galaxy Wystan Benbow for the VERITAS Collaboration 1 Harvard-Smithsonian Center for Astrophysics 1 see R.A. Ong
in multimessenger astrophysics.
High Energy Neutrino detection in multimessenger astrophysics. Antonio Capone, University "La Sapienza" and I.N.F.N. Roma, Italy at the The Future of Research on Cosmic Gamma Rays La Palma, Canary Islands
The VERITAS Dark M atter and Astroparticle Programs. Benjamin Zitzer For The VERITAS Collaboration
The VERITAS Dark M atter and Astroparticle Programs Benjamin Zitzer For The VERITAS Collaboration Introduction to VERITAS Array of four IACTs in Southern AZ, USA Employs ~100 Scientists in five countries
Neutrino induced muons
Neutrino induced muons The straight part of the depth intensity curve at about 10-13 is that of atmospheric neutrino induced muons in vertical and horizontal direction. Types of detected neutrino events:
OBSERVATIONS OF VERY HIGH ENERGY GAMMA RAYS FROM M87 BY VERITAS
OBSERVATIONS OF VERY HIGH ENERGY GAMMA RAYS FROM M87 BY VERITAS 1 Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) APOD, 2004 December
Multimessenger test of Hadronic model for Fermi Bubbles Soebur Razzaque! University of Johannesburg
Multimessenger test of Hadronic model for Fermi Bubbles Soebur Razzaque! University of Johannesburg with! Cecilia Lunardini and Lili Yang Multi-messenger Astronomy 2 p π ±# ν# cosmic rays + neutrinos p
Time-domain astronomy with the Fermi Gamma-ray Burst Monitor
Time-domain astronomy with the Fermi Gamma-ray Burst Monitor C. Michelle Hui (NASA/MSFC) on behalf of the Fermi GBM team TeVPA, Aug 11 2017 GBM: FOV >8sr Whole sky every ~90min Fermi Gamma-ray Space Telescope
Implications of neutrino flux limits
Implications of neutrino flux limits by the AMANDA experiment Julia Becker for the IceCube collaboration August 2006 Contents I. Detection principle and detector II. Analysis methods and results I. point
Matt Kistler Ohio State University In collaboration with John Beacom
Prospects for Galactic TeV Neutrino Astronomy Matt Kistler Ohio State University In collaboration with John Beacom Photo: HESS Zwicky s Contributions to GLCW8 COSMIC RA YS FROM SUPER-NO VAE By W. BAADE
SELECTED RESULTS OF THE ANTARES TELESCOPE AND PERSPECTIVES FOR KM3NET. D. Dornic (CPPM) on behalf the ANTARES Coll.
SELECTED RESULTS OF THE ANTARES TELESCOPE AND PERSPECTIVES FOR KM3NET D. Dornic (CPPM) on behalf the ANTARES Coll. MORIOND VHEPU @ La Thuile, March 2017 Neutrino telescopes: science scope Low$Energy$$
1. GAMMA-RAY BURSTS & 2. FAST RADIO BURSTS
1. GAMMA-RAY BURSTS & 2. FAST RADIO BURSTS WITH TAM, Pak Hin (Sun Yat-sen University/ICRR) GAMMA-RAY BURST OBSERVATIONS WITH CTA LESSONS LEARNT FROM FERMI/LAT TAM, Pak Hin (Sun Yat-sen University/ICRR,
Results from the ANTARES neutrino telescope
EPJ Web of Conferences 116, 11006 (2016) DOI: 10.1051/epjconf/201611611006 C Owned by the authors, published by EDP Sciences, 2016 Results from the ANTARES neutrino telescope M. Spurio, on behalf of the
High Energy Neutrino Astronomy
High Energy Neutrino Astronomy VII International Pontecorvo School Prague, August 2017 Christian Spiering, DESY Zeuthen Content Lecture 1 Scientific context Operation principles The detectors Atmospheric
GRB observations at very high energies with the MAGIC telescopes
GRB observations at very high energies with the telescopes Markus Garczarczyk - for the collaboration - Markus GRB2012 Garczarczyk Munich GRB2012 May 2012 Munich Major Atmospheric Gamma-ray Imaging Cherenkov
VERITAS Performance Gernot Maier
VERITAS Performance Gernot Maier Alliance for Astroparticle Physics What scientific impact will VERITAS have in the next 3-5 years? Galactic long-term plan Performance Operations LTP & Performance May
Sungkyunkwan University, Korea
Neutrino Oscillation Tomography rottnospam@skku.nospamedu Sungkyunkwan University, Korea Spectrometry of the Earth using Neutrino Oscillations (Sungkyunkwan U.), Akimichi Taketa (ERI, Tokyo), Debanjan
Lobster X-ray Telescope Science. Julian Osborne
Lobster X-ray Telescope Science Julian Osborne What we want The whole high-energy sky right now 1.00E+13 1.00E+12 1 / f_lim (100 s) 1.00E+11 1.00E+10 1.00E+09 1.00E+08 0.0000001 0.000001 0.00001 0.0001
Highlights from the ARGO-YBJ Experiment
Highlights from the ARGO-YBJ Experiment Ivan De Mitri University of Salento and Istituto Nazionale di Fisica Nucleare Lecce, Italy On behalf of the ARGO-YBJ Collaboration 12th International Conference
Neutrino Astronomy. Ph 135 Scott Wilbur
Neutrino Astronomy Ph 135 Scott Wilbur Why do Astronomy with Neutrinos? Stars, active galactic nuclei, etc. are opaque to photons High energy photons are absorbed by the CMB beyond ~100 Mpc 10 20 ev protons,
AGIS (Advanced Gamma-ray Imaging System)
AGIS (Advanced Gamma-ray Imaging System) Seth Digel, Stefan Funk and Hiro Tajima SLAC National Accelerator Laboratory Kavli Institute for Particle Astrophysics and Cosmology Outline AGIS project and status
Recent Results from the ANTARES experiment
Recent Results from the ANTARES experiment Manuela Vecchi on behalf of the ANTARES Collaboration University of Roma La Sapienza and INFN ICATPP09- Como: October 6th 2009 Outline -astronomy: what, where,
Search for high energy neutrino astrophysical sources with the ANTARES Cherenkov telescope
Dottorato di Ricerca in Fisica - XXVIII ciclo Search for high energy neutrino astrophysical sources with the ANTARES Cherenkov telescope Chiara Perrina Supervisor: Prof. Antonio Capone 25 th February 2014
VERITAS detection of VHE emission from the optically bright quasar OJ 287
VERITAS detection of VHE emission from the optically bright quasar OJ 287 S. Zola & NASA/JPL S. O Brien For The VERITAS Collaboration Outline 1. OJ 287 2. Historical Observations and Monitoring Programs
Physics of Short Gamma-Ray Bursts Explored by CTA and DECIGO/B-DECIGO
Physics of Short Gamma-Ray Bursts Explored by CTA and DECIGO/B-DECIGO Hiroyasu Tajima Institute for Space Earth Environmental Research Nagoya University 17th DECIGO Workshop Nov 1, 18 Nagoya University
Search for GeV neutrinos associated with solar flares with IceCube
Search for GeV neutrinos associated with solar flares with IceCube for the IceCube Collaboration Vrije Universiteit Brussel E-mail: gdewasse@icecube.wisc.edu Solar flare neutrinos from the decay of mesons
Very High Energy monitoring of the radio galaxy M87 with MAGIC during a low emission state between 2012 and 2015
Very High Energy monitoring of the radio galaxy M87 with MAGIC during a low emission state between 2012 and 2015 ICRR, U-Tokyo and Max-Planck-Institute for Physics, Munich and P. Bangale, M. Manganaro,
VERITAS: exploring the high energy Universe
VERITAS: exploring the high energy Universe K. Ragan McGill University Queen's - March '09 VERITAS 1 Outline Beyond the optical Very high-energy (VHE) gamma-ray astrophysics Ground-based observations Cherenkov
H.E.S.S. multi-messenger and real-time follow-up observations
H.E.S.S. multi-messenger and real-time follow-up observations Fabian Schüssler (Irfu/CEA-Saclay) on behalf of the H.E.S.S. collaboration TevPA 2015, Kashiwa The H.E.S.S. multi-messenger and GRB team A.
PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY. Paolo Lipari Vulcano 27 may 2006
PERSPECTIVES of HIGH ENERGY NEUTRINO ASTRONOMY Paolo Lipari Vulcano 27 may 2006 High Energy Neutrino Astrophysics will CERTAINLY become an essential field in a New Multi-Messenger Astrophysics What is
Very High-Energy Gamma- Ray Astrophysics
Very High-Energy Gamma- Ray Astrophysics David A. Williams Santa Cruz Institute for Particle Physics UC Santa Cruz Quarknet July 12, 2013 Detecting High Energy Gamma Rays High Sensitivity HESS, MAGIC,
Exploring Fermi-LAT Extended GeV Emission with Stacking Analysis
Exploring Fermi-LAT Extended GeV Emission with Stacking Analysis Judy Racusin (NASA/GSFC) Jim Chiang (Stanford) on behalf of the Fermi-LAT Collaboration Motivation LAT extended emission has been seen in
The VelaX pulsar wind nebula in the TeV regime. Bernhard Glück for the H.E.S.S. Collaboration July 8th, 2009, Boston
The VelaX pulsar wind nebula in the TeV regime Bernhard Glück for the H.E.S.S. Collaboration July 8th, 2009, Boston Outline The H.E.S.S. Experiment Results for PWN VelaX from observation 2004 to 2006 Follow
A New View of the High-Energy γ-ray Sky with the Fermi Telescope
A New View of the High-Energy γ-ray Sky with the Fermi Telescope Aurelien Bouvier KIPAC/SLAC, Stanford University On behalf of the Fermi collaboration SNOWPAC, 2010 The Fermi observatory Launch: June 11
Neutrino Astronomy fast-forward
Neutrino Astronomy fast-forward Marek Kowalski (DESY & Humboldt University Berlin) TeVPA 2017, Columbus, Ohio Credit: M. Wolf/NSF The promised land The Universe is opaque to EM radiation for ¼ of the spectrum,
TeV Future: APS White Paper
TeV Future: APS White Paper APS commissioned a white paper on the "Status and Future of very high energy gamma ray astronomy. For preliminary information, see http://cherenkov.physics.iastate.edu/wp Working
IceCube & DeepCore Overview and Dark Matter Searches. Matthias Danninger for the IceCube collaboration
IceCube & DeepCore Overview and Dark Matter Searches for the IceCube collaboration Content Overview: IceCube DeepCore (DOMs, geometry, deep ice properties, trigger & filter) Dark Matter searches: (current
IceCube. francis halzen. why would you want to build a a kilometer scale neutrino detector? IceCube: a cubic kilometer detector
IceCube francis halzen why would you want to build a a kilometer scale neutrino detector? IceCube: a cubic kilometer detector the discovery (and confirmation) of cosmic neutrinos from discovery to astronomy
High energy neutrino signals from NS-NS mergers
High energy neutrino signals from NS-NS mergers He Gao 高鹤 University of Nevada Las Vegas Collaborators: Bing Zhang, Xue-Feng Wu & Zi-Gao Dai 2013-05-08 Multi-Messenger Workshop @ KIAA EM signals for a
Lecture 20 High-Energy Astronomy. HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric
Lecture 20 High-Energy Astronomy HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric Tut 5 remarks Generally much better. However: Beam area. T inst
Origin of Cosmic Rays
Origin of Cosmic Rays Part 2: Neutrinos as Cosmic Ray messengers Lecture at the J. Stefan Institute Ljubljana within the course: 'Advanced particle detectors and data analysis' Hermann Kolanoski Humboldt-Universität
GLAST and beyond GLAST: TeV Astrophysics
GLAST and beyond GLAST: TeV Astrophysics Outline: Greg Madejski Assistant Director for Scientific Programs, SLAC / Kavli Institute for Astrophysics and Cosmology Recent excitement of GLAST and plans for
Search for the Sources of High Energy Astrophysical Neutrinos with VERITAS
Search for the Sources of High Energy Astrophysical Neutrinos with VERITAS Ava Ghadimi CUNY Baccalaureate for Unique and Interdisciplinary Studies New York, NY Columbia University, Nevis Laboratories REU
VERITAS Design. Vladimir Vassiliev Whipple Observatory Harvard-Smithsonian CfA
VERITAS Design Vladimir Vassiliev Whipple Observatory Harvard-Smithsonian CfA VERITAS design goals VERITAS is a ground-based observatory for gamma-ray astronomy VERITAS design is derived from scientific
The H.E.S.S. Standard Analysis Technique
The H.E.S.S. Standard Analysis Technique Wystan Benbow for the H.E.S.S. Collaboration Max Planck Institut für Kernphysik Postfach 103980 D-69029 Heidelberg, Germany The High Energy Stereoscopic System
High Energy Emission. Brenda Dingus, LANL HAWC
High Energy Emission from GRBs Brenda Dingus, LANL HAWC What are GRBs? Cosmological distance Typical observed z>1 Energy released is up to few times the rest mass of Sun (if isotropic) in a few seconds