IceCube: Multiwavelength Approach to

Slides:



Advertisements
Similar presentations
A Multi - wavelength Study of Blazars with WIYN- VERITAS-IceCube Kirsten L. Larson The College of Wooster Advisor: Teresa Montaruli University of Madison-Wisconsin.
Advertisements

OBSERVATIONS OF AGNs USING PACT (Pachmarhi Array of Cherenkov Telescopes) Debanjan Bose (On behalf of PACT collaboration) “The Multi-Messenger Approach.
14.5m 100 m ~480 m Junction Box ~70 m String-based detector; Downward-looking (45°) PMTs; 2475 m deep; 12 detection lines 25 storeys / line 3 PMTs / storey.
High-energy particle acceleration in the shell of a supernova remnant F.A. Aharonian et al (the HESS Collaboration) Nature 432, 75 (2004) Nuclear Physics.
Observations of the AGN 1ES with the MAGIC telescope The MAGIC Telescope 1ES Results from the observations Conclusion The MAGIC Telescope.
TeVPA, July , SLAC 1 Cosmic rays at the knee and above with IceTop and IceCube Serap Tilav for The IceCube Collaboration South Pole 4 Feb 2009.
M. Kowalski Search for Neutrino-Induced Cascades in AMANDA II Marek Kowalski DESY-Zeuthen Workshop on Ultra High Energy Neutrino Telescopes Chiba,
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:
Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Photograph: Forest Banks Gary C. Hill University of Wisconsin, Madison for.
Search for point sources of cosmic neutrinos with ANTARES J. P. Gómez-González IFIC (CSIC-Universitat de València) The ANTARES.
Alexander Kappes UW-Madison 4 th TeVPA Workshop, Beijing (China) Sep. 24 – 28, 2008 The Hunt for the Sources of the Galactic Cosmic Rays — A multi-messenger.
Potential Neutrino Signals from Galactic  -Ray Sources Alexander Kappes, Christian Stegmann University Erlangen-Nuremberg Felix Aharonian, Jim Hinton.
Neutrino Point Source Searches with IceCube 22 String Configuration Michael Baker, for the IceCube Collaboration University of Wisconsin, Madison APS April.
Observations of TeV blazars seem to be well explained by leptonic synchrotron inverse-Compton models, but there may be an hadronic mechanism involved as.
Multi-TeV  -ray Astronomy with GRAPES-3 Pravata K Mohanty On behalf of the GRAPE-3 collaboration Tata Institute of Fundamental Research, Mumbai Workshop.
The IceCube Neutrino Observatory is a cubic kilometer detector at the geographic South Pole. We give an overview of searches for time-variable neutrino.
Matteo Palermo “Estimation of the probability of observing a gamma-ray flare based on the analysis of the Fermi data” Student: Matteo Palermo.
Summary WG4 – Neutrino Astronomy experimental part Mieke Bouwhuis: Results from ANTARES Georgio Riccobene: Results from NEMO and KM3NeT Dave Besson: Radio.
The Character of High Energy Emission From The Galactic Binary LS Andy Smith Smithsonian Astrophysical Observatory (for the VERITAS collaboration)
PHY418 Particle Astrophysics
Kirsten Münich University of Dortmund, Germany Analysis strategies and recent results from AMANDA-II.
High-energy gammas from the giant flare of SGR of December 2004 in AMANDA Juande D. Zornoza on behalf of the IceCube.
Combining Gamma and Neutrino Observations Christian Spiering, DESY.
Gamma-Ray Burst Working Group Co-conveners: Abe Falcone, Penn State, David A. Williams, UCSC,
Potential Neutrino Signals from Galactic  -Ray Sources Alexander Kappes, Christian Stegmann University Erlangen-Nuremberg Felix Aharonian, Jim Hinton.
1 Multi-Messenger approach in IceCube E. Resconi (Max-Planck-Institute for Nuclear Physics, Heidelberg) LAUNCH, Heidelberg, March 2007.
ICECUBE Collaboration meeting, Berkeley Markus Ackermann Status of Point Source Searches Markus Ackermann for Elisa Bernardini, Elisa.
08/2006Julia Becker, Universität Dortmund TeV particle astrophysics, Madison Julia Becker for the IceCube collaboration August 2006 by the AMANDA experiment.
Prospects of Identifying the Sources of the Galactic Cosmic Rays with IceCube Alexander Kappes Francis Halzen Aongus O’Murchadha University Wisconsin-Madison.
1 Cosmic Ray Physics with IceTop and IceCube Serap Tilav University of Delaware for The IceCube Collaboration ISVHECRI2010 June 28 - July 2, 2010 Fermilab.
Strategies in the search for astrophysical neutrinos Yolanda Sestayo, MPI-k Heidelberg for the IceCube collaboration VLVνT 09, Athens.
Counterparts to Single Neutrinos
Downgoing Muons in the IceCube experiment: Final presentation for Phys 735, Particle, Prof. Sridhara Dasu L.Gladstone 2008 Dec 3.
The IceCube Neutrino Observatory is a cubic kilometer detector currently under construction at the geographic South Pole. We will give an overview of searches.
Cosmogenic Muon Background
Imaging the Neutrino Universe with AMANDA and IceCube
On behalf of the ARGO-YBJ collaboration
High Energy Neutrinos and Gamma Rays from the Galactic Center
Search for neutrinos from gamma-ray bursts with the ANTARES telescope
Julia Becker for the IceCube collaboration
The RoboPol Optical Polarization Monitoring Program
Recent Results of Point Source Searches with the IceCube Neutrino Telescope Lake Louise Winter Institute 2009 Erik Strahler University of Wisconsin-Madison.
Observation of Pulsars and Plerions with MAGIC
Theoretical status of high energy cosmic rays and neutrinos
astroparticle physics with ARGO-YBJ
Pierre Auger Observatory Present and Future
Lecture 5 Multi-wavelength cosmic background
John Kelley for the IceCube Collaboration
GLAST Workshop April 13, 2007 Argonne National Lab
08/27/04 Strategies for the search for prompt muons in the downgoing
Songzhan Chen Institute of High Energy Physics (IHEP) Nanjing
Status and prospects of the IceCube Neutrino Telescope
Brennan Hughey for the IceCube Collaboration
Cherenkov  April 2005 Palaiseau, France Contents: 
Prospects and Status of the KM3NeT Neutrino Telescope E. Tzamariudaki
Diffuse neutrino flux J. Brunner CPPM ESA/NASA/AVO/Paolo Padovani.
Anisotropy of Primary Cosmic Rays
Alexander Kappes Francis Halzen Aongus O’Murchadha
Neutrinos as probes of ultra-high energy astrophysical phenomena
Multi-Messenger Astronomy Workshop
Brennan Hughey for the IceCube Collaboration
Claudio Bogazzi * - NIKHEF Amsterdam ICRC 2011 – Beijing 13/08/2011
Unfolding performance Data - Monte Carlo comparison
_____________________________
宇宙線スペクトルと GeV-TeV diffuse-g emission
Time-Dependent Searches for Neutrino Point Sources with IceCube
Time-Dependent Searches for Neutrino Point Sources with IceCube
Sci. 1-3 Telescopes- then and Now Pages 18-23
Fermi LAT Observations of Galactic X-ray binaries
Presentation transcript:

IceCube: Multiwavelength Approach to Transient Neutrino Point Source Candidates http://icecube.wisc.edu Elisa Resconi, for the IceCube coll. (Max-Planck-Institute for Nuclear Physics, Heidelberg) TeV Particle Astrophysics II 28-31 August 2006. Madison, WI

106 : 1 n Fn (E, W) l 1. Construction of the Neutrino Sample IceCube event IceCube event n l 106 : 1 Fn (E, W) Elisa Resconi

Fn (E, W) = Fatm + Fgalactic + Fextra- galactic 2. Extraction of Astronomical Information Fn (E, W) = Fatm + Fgalactic + Fextra- galactic Cosmic ray showers in the Earth’s atmosphere: p, K decay  E-3.7  20% uncertainty “diffuse” flux: CR interaction with interstellar gas. “point-like”: galactic sources  E-2  ? “diffuse” flux: p decay from pg interaction with 2.7oK cosmic radiation “point-like”: extra-galactic sources  E-2  ? TeV-Blazar discussed here See also at this conference: “Implications of neutrino flux limits” J. Becker for IceCube, talk “Search for a Diffuse Flux of TeV to PeV Muon Neutrinos with AMANDA-II” J. Hodges for IceCube, poster

No significant excess found Blind analysis strategy Fgalactic(E,W), Fextra-galactic(E,W) point-like sources Ref. M. Ackermann, “The multimessenger approach ..”, Barcelona, 07.06 On-Source Off-Source = 00-04 AMANDA-II preliminary: 2000-2004 (1001 live days), 4282 n from northern hemisphere No significant excess found Blind analysis strategy Variable sources ? Elisa Resconi

dFatm(t)/dt = 1 / year 3o sky-bin Multi-wavelength approach: photon light curves used for the improvement in identify possible neutrinos emitted by astronomical sources Synthetic light curve Photon Rate (counts/sec) 2000 2001 2002 2003 1 Nr of n Time dFatm(t)/dt = 1 / year 3o sky-bin 1 n / day sky-bin ~ 310 -3 How can we discriminate these events ? What can we learn from photon observations?

3. Transient Point Sources The photon-neutrino link Access to photon data Analysis of photon data Selection of neutrino “proxy” waveband Availability / calibration / dead-time correction ….. WHAT IS A FLARE ? Elisa Resconi

3.1 The photon – neutrino link: HBL (LBL) Synchrotron proton blazar model (ref. A. Mücke et al, Astroparticle Phy, 18 (2003) 593-613) proton (highly magnetized environment) electron γ synchr. pγ γ synchr.  ,  γ γ synchr e,  γ synchr casc. (e±) γ synchr γ X LBL HBL P.Giommi et al.,A&A 445, 843-855 (2006) Elisa Resconi

X- ray band γ- ray band X- AND γ-ray  emission Interpretation Data HBL X- AND γ-ray  emission X- ray band γ- ray band C O R E L A T I N Interpretation primary electron AND secondary electron (casc.) only p, if only synchrotron (no ) Data huge amount of data, monitor + high sensitivity sporadic, no monitor, difficult to combine Strategy Light curve interpretation define “flares” define periods of high activity collect all the data available, improve definition of “flare” Elisa Resconi

3.3 Photon data: WHAT IS A FLARE ? Light Curve Interpretation: characteristic flux level(s) impulsive events (flares) statistical studies on the timescales of variability correlated activities across wavebands periods of HE neutrino emission: Construction of an hypothesis test Maximum Likelihood Blocks applied to X- and -ray light curves [E. Resconi, L. Costamante, D. Franco, E. Flaccomio, A. Gross, icecube/200608002]

X-ray: an example All-Sky-Monitor (RXTE), Mkn 421 All-Sky-Monitor, RXTE, 10 years X-ray monitor zoom Mkn 421 Elisa Resconi

All-Sky-Monitor, Maximum-Likelihood-Blocks zoom Mkn 421 Elisa Resconi

All-Sky-Monitor, Maximum-Likelihood-Blocks, Characteristic level zoom Mkn 421 Rchar Elisa Resconi

Hypothesis test: need to be blind!  sample determined a priori Time periods selected a priori  in the time periods /  atmospheric expected All-Sky-Monitor, Maximum-Likelihood-Blocks, Characteristic level zoom Mkn 421 Elevated levels or flares : ~ 15 % + 3 Rchar Characteristic level (band) Depends on: source + detector Elisa Resconi

TeV -ray: preliminary The light curves are very sporadic Compilation of historical light curves: under construction Mkn 421, Whipple public data, Maximum Likelihood Blocks Elisa Resconi

Multi-wavelength: X- vs -ray “Orphan” region Correlated corridor -ray flux “Anti-orphan” region X-ray flux, PCA (MLB blocks) Elisa Resconi

Future: … transition to a ‘multi-messengers’ approach - IceCube as a ( half ) – All-Sky-Monitor in neutrino: - Filed of view: northern sky - High duty cycle Idea: use neutrinos in order to trigger gamma-ray telescopes (see E. Bernardini, “The multimessenger approach..” Barcelona, 07.06) - Critical points under discussion: - selection of the sources: the phenomenology is limited - statistical interpretation of possible coincidences: -ray flare rate, catalogue … - blindness of the data: minimal impact with off-line analysis Status: TEST run between AMANDA and Magic of 3 months approved. Elisa Resconi

Summary Looking in the right direction and in the right moment is a good idea! From existing models: selection of proxy wavebands (HBL discussed) Photon light curves under compilation Photon light curve analysis with a global method (MLB) Selection of periods of possible neutrino emission: global & non arbitrary Next: test on the data Elisa Resconi