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

Slides:



Advertisements
Similar presentations
R.Shanidze, B. Herold, Th. Seitz ECAP, University of Erlangen (for the KM3NeT consortium) 15 October 2009 Athens, Greece Study of data filtering algorithms.
Advertisements

Trigger issues for KM3NeT the large scale underwater neutrino telescope the project objectives design aspects from the KM3NeT TDR trigger issues outlook.
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.
Kay Graf Physics Institute 1 University of Erlangen ARENA 2006 University of Northumbria June 28 – 30, 2006 Integration of Acoustic Neutrino Detection.
Use of floating surface detector stations for the calibration of a deep-sea neutrino telescope G. Bourlis, N. A. B. Gizani, A. Leisos, A. G. Tsirigotis,
Kay Graf University of Erlangen for the ANTARES Collaboration 13th Lomonosov Conference on Elementary Particle Physics Moscow, August 23 – 29, 2007 Acoustic.
H Yepes, C Bigongiari, J Zuñiga, JdD Zornoza IFIC (CSIC - Universidad de Valencia) NEWS ON ABSORPTION LENGTH MEASUREMENT WITH THE OB SYSTEM ANTARES COLLABORATION.
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:
AN UPDATE ON ABSORPTION LENGTH MEASUREMENT WITH THE OB SYSTEM ANTARES Collaboration Meeting Paris (France), September 20th-24th H Yepes, J Barrios IFIC.
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.
The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
J.P. Gómez-González. Outline Introduction: The ANTARES neutrino telescope Time calibration Muon track residuals based method: Description and implementation.
Prototype string for a km3 Baikal neutrino telescope Roma International Conference on Astroparticle Physics V.Aynutdinov, INR RAS for the Baikal Collaboration.
A feasibility study for the detection of SuperNova explosions with an Undersea Neutrino Telescope A. Leisos, A. G. Tsirigotis, S. E. Tzamarias Physics.
Special Issues on Neutrino Telescopy Apostolos G. Tsirigotis Hellenic Open University School of Science & Technology Particle and Astroparticle Physics.
KM3NeT detector optimization with HOU simulation and reconstruction software A. G. Tsirigotis In the framework of the KM3NeT Design Study WP2 - Paris,
The ANTARES experiment is currently the largest underwater neutrino telescope and is taking high quality data since Sea water is used as the detection.
The Transverse detector is made of an array of 256 scintillating fibers coupled to Avalanche PhotoDiodes (APD). The small size of the fibers (5X5mm) results.
Hanoi, Aug. 6-12, 2006 Pascal Vernin 1 Antares Status report P.Vernin CEA Saclay, Dapnia On behalf of the Antares collaboration P.Vernin
Francisco Salesa Greus IFIC (CSIC–Universitat de València, Spain) Representing the KM3NeT Consortium 4 th International Workshop on Very Large Volume Neutrino.
AN UPDATE ON ABSORPTION LENGTH MEASUREMENT WITH THE OB SYSTEM ANTARES Collaboration Meeting Paris (France), September 20th-24th H Yepes, J Zuñiga IFIC.
1 S. E. Tzamarias Hellenic Open University N eutrino E xtended S ubmarine T elescope with O ceanographic R esearch Readout Electronics DAQ & Calibration.
Report of the HOU contribution to KM3NeT TDR (WP2) A. G. Tsirigotis In the framework of the KM3NeT Design Study WP2 Meeting - Marseilles, 29June-3 July.
Antoine Kouchner Université Paris 7 Laboratoire APC - CEA/Saclay for the ANTARES collaboration Neutrino Astronomy: a new look at the Galaxy Astronomy Neutrino.
CEA DSM Irfu The ANTARES Neutrino Telescope A status report Niccolò Cottini on behalf of the ANTARES Collaboration 44 th Rencontres de Moriond February.
Piera Sapienza – VLVNT Workshop, 5-8 october 2003, Amsterdam Introduction and framework Simulation of atmospheric  (HEMAS and MUSIC) Response of a km.
V.Bertin CPPM / ANTARES Coll. - Moriond ANTARES : A deep-sea 0.1 km² neutrino telescope Vincent Bertin - CPPM-Marseille on behalf of the Antares.
SINP MSU, July 7, 2012 I.Belolaptikov behalf BAIKAL collaboration.
Special Issues on Neutrino Telescopy Apostolos G. Tsirigotis Hellenic Open University School of Science & Technology Particle and Astroparticle Physics.
Status of gravitational lens paper Internal note: Results of the optical properties of sea water in the ANTARES site with the OB system.
1 N eutrino E xtended S ubmarine T elescope with O ceanographic R esearch Operation and performance of the NESTOR test detector.
Agustín Sánchez-Losa IFIC (CSIC-Universitat de València) Transient sources, like AGNs or Gamma Ray Bursters, are among.
Ronald Bruijn – 10 th APP Symposium Antares results and status Ronald Bruijn.
NESTOR SIMULATION TOOLS AND METHODS Antonis Leisos Hellenic Open University Vlvnt Workhop.
Status and first results of the KASCADE-Grande experiment
Detection of electromagnetic showers along muon tracks Salvatore Mangano (IFIC)
CEA DSM Irfu Reconstruction and analysis of ANTARES 5 line data Niccolò Cottini on behalf of the ANTARES Collaboration XX th Rencontres de Blois 21 / 05.
The ANTARES detector: background sources and effects on detector performance S. Escoffier CNRS Centre de Physique des Particules de Marseille on behalf.
Antares Slow Control Status 2007 International Conference on Accelerator and Large Experimental Physics Control Systems - Knoxville, Tennessee - October.
The ANTARES Project Sino-French workshop on the Dark Universe Stephanie Escoffier Centre de Physique des Particules de Marseille On behalf of the ANTARES.
Ciro Bigongiari, Salvatore Mangano Results of the optical properties of sea water with the OB system.
5 June 2002DAQ System Engineering Requirements 1 DAQ System Requirements DOM Main Board Engineering Requirements Review David Nygren.
Time and amplitude calibration of the Baikal-GVD neutrino telescope Vladimir Aynutdinov, Bair Shaybonov for Baikal collaboration S Vladimir Aynutdinov,
Comparison of different km3 designs using Antares tools Three kinds of detector geometry Incoming muons within TeV energy range Detector efficiency.
PMT measurements in Antares Oleg Kalekin on behalf of Antares collaboration VLVnT 2011 Erlangen
ANTARES Status report  Experiment overview  Status of construction  Status of operation  Status of physics analyses Presentation at ICATPP’07. Oct.
Z. Cao, H.H. He, J.L. Liu, M. Zha Y. Zhang The 2 nd workshop of air shower detection at high altitude.
Detecting Air Showers on the Ground
Calibration of Under Water Neutrino Telescope ANTARES Garabed HALLADJIAN October 15 th, 2008 GDR Neutrino, CPPM, Marseille.
1 Ciro Bigongiari, Salvatore Mangano Results of the optical properties of sea water with the OB system.
A. Tsirigotis Hellenic Open University N eutrino E xtended S ubmarine T elescope with O ceanographic R esearch Reconstruction, Background Rejection Tools.
Simona Toscano In the frame of KM3NeT consortium VLV T workshop - Toulon, April 2008.
VLVNT’08 - ToulonM. Ardid – Positioning System of the ANTARES Neutrino Telescope Positioning system of the ANTARES Neutrino Telescope Miguel Ardid (IGIC.
Isabella Amore VLV T08, Toulon, France April 2008 International Workshop on a Very Large Volume Neutrino Telescope for the Mediterranean Sea Results.
Status and Perspectives of the BAIKAL-GVD Project Zh.-A. Dzhilkibaev, INR (Moscow), for the Baikal Collaboration for the Baikal Collaboration September.
KM3NeT Optical Calibration Umberto Emanuele IFIC (CSIC – University of Valencia, Spain) WPF/L KM3NeT Meeting Nikhef 5 th - 7 th July
KM3NeT P.Kooijman Universities of Amsterdam & Utrecht for the consortium.
ANTARES Lessons learned from its completion
White Rabbit in KM3NeT Mieke Bouwhuis NIKHEF 9th White Rabbit Workshop
An expected performance of Dubna neutrino telescope
The Antares Neutrino Telescope
Antares Collaboration
Systematic uncertainties in MonteCarlo simulations of the atmospheric muon flux in the 5-lines ANTARES detector VLVnT08 - Toulon April 2008 Annarita.
M.Bou-Cabo, J.A. Martínez.-Mora on behalf of the ANTARES Collaboration
Calculation of detector characteristics for KM3NeT
ANTARES time calibration
on behalf of the NEMO Collaboration
Antares Collaboration
Atmospheric muons in ANTARES
Nanobeacon: A low cost calibration instrument for KM3NeT
Presentation transcript:

Coincidence analysis in ANTARES: Potassium-40 and muons  Brief overview of ANTARES experiment  Potassium-40 calibration technique  Adjacent floor coincidences as very basic atmospheric muon signal ITEP winter school Feb 12, 2008 Dmitry Zaborov (ITEP, Moscow, Russia)

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES2 Detection principle   43° Sea floor p  10 4 atm  p,  10 7  atm  Reconstruction of  trajectory (~ ) from timing and position of PMT hits interaction Cherenkov light from  3D PMT array  cosm effective area ~ 0.1 km 2 in TeV range angular resolution ~ 0.3º at 10 TeV Hadronic showers from CC/NC interactions can be detected as well

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES3 Detector layout ~70 m 12 lines (900 PMTs) 25 storeys / line 3 PMTs/storey 350 m 100 m 14.5 m Junction box Readout cables 40 km to shore Horizontal layout Sea bed ~ m a storey

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES4 Current status L11 L9 L12 L7 L8 L6 L4 L2 L3 L5 L1 IL07 seismometer 100 m N Junction box Submarine cable to shore 42°50’ N 6°10’E 10 detector lines + instrumentation line operational (since December 07) (Feb. 2008) 2 more lines coming soon ~ 2 muons/sec ~ 5 neutrino/day (atmospheric) L10 * Cable path is shown only indicatively

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES5 Basic detection and calibration elements Hydrophone: acoustic positioning Optical Module: 10” PMT in 17” glass sphere photon detection Local Control Module (in Ti container): Front-end ASIC, Clock, DAQ/SC, compass/roll/pitch Optical Beacon with blue LEDs: timing calibration

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES6 In situ calibration with Potassium K 40 Ca  e - (  decay)  Cherenkov Gaussian peak on coincidence plot Peak offset Rate of correlated coincidences High precision (~5%) monitoring of OM efficiencies time calibration confirmed 15 Hz MC prediction 13+/-4 Hz (“NIM” angular acceptance) Mean ≈ 0 RMS 0.7 ns No dependence on bioluminescent activity has been observed - this confirms the single photon character of bioluminescent emission

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES7 Example: calibration of Line 8 Three OM sensitivity factors s i can be extracted using 3 equations rate ij = k * s i * s j factor k gives absolute scale; k can be determined from Monte-Carlo (or, in opposite, used to constrain parameters of Monte-Carlo) OM-OM time offsets determined using K-40 (basically single photoelectrons) w.r.t Dark room calibration (high amplitude laser pulse) * No charge calibration used * No walk correction included Unofficial technical plot I,j=1,2,3

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES8 Time evolution (example) Time delays seem stable (within our accuracy) Gradual decrease is probably due to PMT gain drift Steep changes are threshold tunings Unofficial technical plot K40 runs are taken once a week K40 trigger can run in parallel with other triggers (e.g. GRB trigger or directional triggers) and can be even used for physics analysis as is

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES9 Time evolution of average K-40 coincidence rate start at 12 Hz “degradation” tuning 2 One year of “degradation” could be fully compensated by the tuning tuning 2 -> 15.5 Hz * Other Lines show similar behavior tuning 1 Unofficial technical plot

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES10 Delay between adjacent floors (theory) Δt = L / c ≈ 50 ns Δt ~ L n / c ~ 70 ns L Δt ~ 0 But light hits back of the OM ≈ fixed number for exactly vertical muonsa wide distribution in general from to The most basic signal of physics events in ANTARES Delay between storeys No systematic errors from trigger or reconstruction algorithms No background

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES11 Adjacent floor coincidences: measurement Integral under the peak ~ muon flux Shape is sensitive to angular acceptance of optical modules and angular distribution of muon flux The effect of muon flux reduction with depth is directly (!) measured Low energy threshold (compared to full reconstruction) The analysis can be repeated for every detector storey separately This plot is preliminary Actual comparison of peak amplitude with Monte Carlo will be made after OM angular acceptance issues are fixed, OM efficiency is well known and all dead time corrections applied

Feb 12, 2008D. Zaborov. Coincidence analysis in ANTARES12 Summary A calibration technique using Cherenkov light from Potassium-40 decays in sea water has been developed –Sensitivity of optical modules is now controlled using K-40 –K-40 is also a useful tool for time calibration A simple but powerful technique for atmospheric muon measurement is developed based on the idea of adjacent floor coincidences –First results allowed to reject one of the models of OM angular acceptance –Depth dependence and absolute normalization of atmospheric muon flux can be extracted using this new approach –Possibility to reject certain hadronic interaction models or (less likely) primary flux models is being investigated –Promising prospects to use adjacent floor coincidences in the trigger