Search for diffuse cosmic neutrino fluxes with the ANTARES detector Vladimir Kulikovskiy The ANTARES Collaboration 3-9 August 2014ANTARES diffuse flux.

Slides:

Advertisements

Similar presentations

Trigger issues for KM3NeT the large scale underwater neutrino telescope the project objectives design aspects from the KM3NeT TDR trigger issues outlook.

Advertisements

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.

London Collaboration Meeting September 29, 2005 Search for a Diffuse Flux of Muon Neutrinos using AMANDA-II Data from Jessica Hodges University.

Longitude Latitude A recent analysis of the Fermi-LAT data by M. Su et al. [1] revealed two large spherical structures centered by our Galactic Center.

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.

Sean Grullon For the IceCube Collaboration Searching for High Energy Diffuse Astrophysical Neutrinos with IceCube TeV Particle Astrophysics 2009 Stanford.

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:

Energy Reconstruction Algorithms for the ANTARES Neutrino Telescope J.D. Zornoza 1, A. Romeyer 2, R. Bruijn 3 on Behalf of the ANTARES Collaboration 1.

Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Photograph: Forest Banks Gary C. Hill University of Wisconsin, Madison for.

1 TEV PA Meeting July 2009 Preliminary Fermi-LAT Limits on High Energy Gamma Lines from WIMP Annihilation Yvonne Edmonds representing the Fermi-LAT Collaboration.

The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.

C.Distefano Barcelona July 4 – 7, 2006 LNS Detection of point-like neutrino sources with the NEMO-km 3 telescope THE MULTI-MESSENGER APPROACH TO UNIDENTIFIED.

SEARCHES for STEADY SOURCES of COSMIC NEUTRINOS in ANTARES J. P. Gómez-González, on behalf of the ANTARES Collaboration IFIC (CSIC-Universitat de València)

Atmospheric Neutrino Oscillations in Soudan 2

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.

Coincidence analysis in ANTARES: Potassium-40 and muons  Brief overview of ANTARES experiment  Potassium-40 calibration technique  Adjacent floor coincidences.

EHE Search for EHE neutrinos with the IceCube detector Aya Ishihara for the IceCube collaboration Chiba University.

Potential Neutrino Signals from Galactic  -Ray Sources Alexander Kappes, Christian Stegmann University Erlangen-Nuremberg Felix Aharonian, Jim Hinton.

Apostolos Tsirigotis Simulation Studies of km3 Architectures KM3NeT Collaboration Meeting April 2007, Pylos, Greece The project is co-funded by the.

Antoine Kouchner Université Paris 7 Laboratoire APC - CEA/Saclay for the ANTARES collaboration Neutrino Astronomy: a new look at the Galaxy Astronomy Neutrino.

Special Issues on Neutrino Telescopy Apostolos G. Tsirigotis Hellenic Open University School of Science & Technology Particle and Astroparticle Physics.

4. Einstein Angle and Magnification The angular deflection for a relativistic neutrino with mass m ʋ that passes by a compact lens of mass M with impact.

Agustín Sánchez-Losa IFIC (CSIC-Universitat de València) Transient sources, like AGNs or Gamma Ray Bursters, are among.

KM3NeT International Solvay Institutes 27  29 May 2015, Brussels, Belgium. Maarten de Jong Astro-particle and Oscillations Research with Cosmics in the.

Neutrino Diffuse Fluxes in KM3NeT Rezo Shanidze, Thomas Seitz ECAP, University of Erlangen (for the KM3NeT consortium) 15 October 2009 Athens, Greece.

Dorothea Samtleben Leiden University / NIKHEF, Amsterdam.

SEARCHING FOR A DIFFUSE FLUX OF ULTRA HIGH-ENERGY EXTRATERRESTRIAL NEUTRINOS WITH ICECUBE Henrik Johansson, for the IceCube collaboration LLWI H.

C Alexander Kappes for the IceCube Collaboration 23 rd European Cosmic-Ray Symposium Moscow, 7. July 2012 Neutrino astronomy with the IceCube Observatory.

Recent Results from Searches for Astrophysical Neutrinos with the IceCube Neutrino Telescope Alexander Kappes Seminar APC, Paris, June 14, 2013.

Latest Results from the MINOS Experiment Justin Evans, University College London for the MINOS Collaboration NOW th September 2008.

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.

Data collected during the year 2006 by the first 9 strings of IceCube can be used to measure the energy spectrum of the atmospheric muon neutrino flux.

Alexander Kappes Erlangen Centre for Astroparticle Physics for the ANTARES collaboration IAU GA, SpS 10, Rio de Janeiro, Aug Status of Neutrino.

Search for Electron Neutrino Appearance in MINOS Mhair Orchanian California Institute of Technology On behalf of the MINOS Collaboration DPF 2011 Meeting.

The AMANDA-II Telescope - Status and First Results - Ralf Wischnewski / DESY-Zeuthen for the AMANDA Collaboration TAUP2001, September.

A Search for Neutrinos from the Galactic Plane 1 Jon Dumm w/ Chad Finley & Martin Wolf MANTS Meeting - Amsterdam Oct 17, 2015.

Search for neutrinos from gamma-ray bursts with the ANTARES telescope D. Dornic for the ANTARES Collaboration.

PHY418 Particle Astrophysics

High-energy gammas from the giant flare of SGR of December 2004 in AMANDA Juande D. Zornoza on behalf of the IceCube.

IceCube & ANTARES Constraints to the IceCube signal from ANTARES & Combined Point Source Analysis IceCube/ANTARES J. Brunner CPPM 20/01/2015.

Longitude Latitude A recent analysis of the Fermi-LAT data by M. Su et al. [1] revealed two large spherical structures centered by our Galactic Center.

POINT SOURCE ANALYSIS WITH 5-LINE DATA SUMMARY AWG PHONE CALL Juan Pablo Gómez-Gozález 20 th April

Sebastian Kuch, Rezo Shanidze Preliminary Studies of the KM3NeT Physics Sensitivity KM3NeT Collaboration Meeting Pylos, Greece, April 2007.

Potential Neutrino Signals from Galactic  -Ray Sources Alexander Kappes, Christian Stegmann University Erlangen-Nuremberg Felix Aharonian, Jim Hinton.

A search for neutrinos from long-duration GRBs with the ANTARES underwater neutrino telescope arxiv C.W. James for the ANTARES collaboration.

Results from the ANTARES Neutrino Telescope VLVNT - Roma 14/7/2015 ANTARES Results - M. Spurio 1 Maurizio Spurio VLVnT– Roma 14/09/2015.

Alexander Kappes Erlangen Centre for Astroparticle Physics XIV Lomonosov Conference Moscow, August 25, 2009 High-energy neutrinos from Galactic sources.

A New Upper Limit for the Tau-Neutrino Magnetic Moment Reinhard Schwienhorst      ee ee

Prospects of Identifying the Sources of the Galactic Cosmic Rays with IceCube Alexander Kappes Francis Halzen Aongus O’Murchadha University Wisconsin-Madison.

I'm concerned that the OS requirement for the signal is inefficient as the charge of the TeV scale leptons can be easily mis-assigned. As a result we do.

1 Cosmic Ray Physics with IceTop and IceCube Serap Tilav University of Delaware for The IceCube Collaboration ISVHECRI2010 June 28 - July 2, 2010 Fermilab.

EHE Search for EHE neutrinos with the IceCube detector Aya Ishihara Chiba University.

Response of the KM3NeT detector to neutrinos from Fermi bubbles.

Roma International Conference on Astroparticle Physics Rome, May 2013 Juan de Dios Zornoza (IFIC – Valencia) in collaboration with G. Lambard (IFIC) on.

The IceCube Neutrino Observatory is a cubic kilometer detector currently under construction at the geographic South Pole. We will give an overview of searches.

On behalf of the ARGO-YBJ collaboration

Muons in IceCube PRELIMINARY

IceCube Collaboration Meeting

Search for neutrinos from gamma-ray bursts with the ANTARES telescope

discovery potential of Galactic sources

John Kelley for the IceCube Collaboration

Diffuse neutrino flux J. Brunner CPPM ESA/NASA/AVO/Paolo Padovani.

Alexander Kappes Francis Halzen Aongus O’Murchadha

MC studies of the KM3NeT physics performance Rezo Shanidze

Claudio Bogazzi * - NIKHEF Amsterdam ICRC 2011 – Beijing 13/08/2011

Unfolding performance Data - Monte Carlo comparison

Atmospheric muons in ANTARES

Presentation transcript:

Search for diffuse cosmic neutrino fluxes with the ANTARES detector Vladimir Kulikovskiy The ANTARES Collaboration 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 1

Overview ANTARES description Full sky searches Special region searches Fermi bubbles Milky Way Future plans 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 2

The ANTARES detector 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 3 12 lines (885 10” PMTs) 25 storeys/line 3 PMTs / storey 5-line setup in 2007 completed in 2008 Junction box In the Mediterranean Sea (near Toulon) at 2500 m depth 14.5 m 350 m 100 m 40 km to shore station LED beacon storey Visibility

Detector performance 83% of cosmic track events (E -2 spectrum) are reconstructed better than 1 o (selected with Λ>-5.2 and β<1 o ). 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 4 Shower events: after the muon filter (the cut on the reduced vertex log-likelihood at 7.9) νμνμ μ ν CC track-like events shower-like events ν μ (NC), ν e, ν τ PRELIMINARY E ANN (mean, RMS) Schnabel 2013 NIM A MC shower energy [GeV] MC shower energy [GeV] (fit dir.; υdir) [deg] logE fit /E MC

Diffuse cosmic ν  flux  Updated analysis: (855 days livetime)  Improved energy estimate based on dE/dX Unblinded result: n obs =8 n bkg =8.4 Muon contamination negligible (<0.4%)  Analysis sensitivity:  E 2  = 4.7 x GeV cm -2 s -1 sr -1  Upper limit (no systematic errors included):  E 2   = 4.8 x GeV cm -2 s -1 sr -1 (45 TeV< E < 10 PeV)  1.4 expected signal event for E 2   = 1.2 x GeV cm -2 s -1 sr -1 (IceCube HESE measurement) 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 5

29 Jan 2007 – 31 December 2012 (total livetime: 1247 days, burn sample: 135 days) Shower reconstruction algorithm. Compares well with simulation (“run-by-run Monte Carlo” with environmental conditions simulated). Selection chain: Muon filter -> Hits -> 2 lines -> No spark events -> Fitted zenith > 94 o & E shower > 10 TeV Sensitivity per neutrino flavour: Contribution to the event counting Event numbers after the final cuts Cosmic signal events Atmospheric background events Cosmic signal (test flux 1.2*10-8 per flavour) 1.75 Conventional atmospheric neutrinos 2.32 Prompt atmospheric neutrinos 0.56 Tau neutrino estimation (prompt) Atmospheric muon extrapolation 1.85 Correction for missing vertex showers in CC muon simulations High multiplicity muon bundles TOTAL August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 6 Shower analysis PRELIMINARY

Limits on normalization for an E -2 flux: Feldman-Cousins 90% CL upper limit Including systematic uncertainties using Pole 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 7 Shower analysis -unblinding CutObs. ev.Exp. back. Zenith>94 o 6082±40 Energy>10 TeV PRELIMINARY

Analysis typeShowersTrack Nu flavoursAll flavoursMuonic Period (1247 days) (885 days) Exp. background events Observed events88 Upper limit, (per flavour, 90% CL, systematic included) 4.9× ×10 -8 Energy range23 TeV < E < 7.8 PeV45 TeV < E < 10 PeV Diffuse flux summary 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 8 PRELIMINARY Schnabel 2014, Phys. Proc. 00 (TAUP2014)

PRELIMINARY

Special regions Fermi Bubbles Excess of gamma-rays (together with X-rays and radio) in extended “bubbles” above and below the Galactic Centre. Homogenous intensity, hard spectrum (E -2 ) probably with cutoff Galactic Wind scenario and other hadronic models predict neutrino flux. Its muonic component can be estimated as: Milky Way The Galactic plane is the most populated region CRs can interact and produce neutrinos. E -2.6 spectrum expected (leptons can decay due to the low density). Magnetic field can enhance the neutrino signal. 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 10 Su et al ApJ Crocker & Aharonian, 2011 Phys. Lett. B

Special regions Fermi Bubbles Gamma-rays observation with hard E -2 spectrum (Fermi-LAT) Milky Way CR interact with interstellar medium Pion decay: neutrinos, gammas 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 11 Credit: NASA/DOE/FERMI LAT/D. Finkbeiner et al. FERMI-LAT diffuse flux (E=3.4 GeV)

Search zones, offzones Fermi bubbles zone is approximated with Lemniscate of Bernoulli (0.8 sr) Size of the Galactic plane region is optimized according to different models and MRF Background is estimated from the off-zones (same size, shape and average detector efficiency) Number of off-zones is fixed for Fermi bubbles analysis – three Depends on the on-zone size for Galactic plane (eight after the optimization) 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU sr 0.8 sr

Fermi bubbles: results 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 13 N obs = 16 = data analyzed (806 days of livetime) 16 events observed (11 background expected) 1.2 sigma significance 90% C.L. upper limits are set

Galactic Plane - results 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU data analyzed Observed 177 events (166 background expected) 0.8 sigma excess – 90% C.L. are set PRELIMINARY

Special regions - summary Upper limits for the neutrino flux from the Fermi bubble regions: no energy cutoff: A=5.3 (6 TeV < E υ < 2 PeV) 500 TeV cutoff : A=8.4 (6 TeV < E υ < 600 TeV) 100 TeV cutoff : A=16.0 (5 TeV < E υ < 200 TeV) 50 TeV cutoff : A=24.3 (5 TeV < E υ < 160 TeV) Upper limits for the neutrino flux from the Galactic Plane central region (90% of the signal): (178 GeV < E υ < 70.8 TeV) 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 15 PRELIMINARY Adriàn-Martìnez et al EPJ C 74 2

Conclusions and plans ANTARES – the first undersea Neutrino Telescope. It is in its 7 th year of operation. Despite its moderate size, but thanks to its location and excellent angular resolution it is yielding: Diffuse flux sensitivity in the relevant range Best limits for the Galactic Centre and the Fermi bubble regions The measurements can be improved: It is planned to run during 2015 and, probably, longer More data are already collected and not analyzed yet Joint track and shower analyses are in development Prepare for the next generation Mediterranean neutrino telescope – KM3NeT 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 16

two of the 8 observed events (diffuse flux analysis with showers 3-9 August 2014ANTARES diffuse flux searches (V. Kulikovskiy) VHEPU 17