antares status report

ANTARES Status report Experiment overview Status of construction Status of operation Status of physics analysesPresentation at ICATPP07. Oct 8, 2007. Como, ItalyDmitry Zaborov(ITEP, Moscow, Russia)on behalf of the ANTARES collaboration

D. Zaborov. ANTARES status report

Collaboration & experiment location


Detection principlenmg43Sea floorp104 atmmp, a107 atmgReconstruction of m trajectory (~ n) from timing and position of PMT hits interactionCherenkov light from m3D PMT array1-100 cosm


Detector layout~70 m 12 lines (900 PMTs) 25 storeys / line 3 PMTs/storey350 m100 m14.5 mJunctionboxReadout cables40 km toshoreSea bed ~ -2500 ma storey


A few remarks on detector performanceSensitivity to - and - (via -> decay) neutrino using muon tracksHigh angular resolution (0.3 at 10 TeV)Effective area close to 0.1 km2 in TeV range (with 12 Lines)Sensitivity to all neutrino types using showersHigh energy resolution (~25%)Significant sensitivity in sub-TeV rangesearch for dark matter (neutralino)neutrino oscillationspoint-like sourcesSky coverage complementary to AMANDA/IceCubeLooking through the EarthMostly Southern sky is visibleField of view follows Earth rotationMost of our Galaxy within field of view (Galactic center, intermediate-mass black holes, )


Basic detection and calibration elementsOptical Beacon with blue LEDs:timing calibration


Detector Line deployment


Submarine cable connection


Current statusIL07seismometer100 mNJunction box

Submarinecable to shore

4250 N 610E5 detector lines operational (since January 29th)(Oct. 2007)4 lines + instrumentation line are awaiting connection3 lines to be deployed


Construction schedule* Source: ANTARES schedule v070910, ANTARES-L, collaboration meetings


Instrumentation Line IL07New six-storey instrumentation line (MILOM had 3 storeys)Includes modified MILOM instruments:2 ADCPs (Acoustic Doppler Current Profilers), shooting up & down2 CT (Conductivity-Temperature) probes with water pump2 CSTAR devices with improved sensitivity & horizontal mechanical mounting (measure optical properties of the water)Sound VelocimeterSeismometer with direct Ethernet linkIncludes several new instruments:2 Sensitive cameras + IR flash looking at an Optical ModuleO2 probeIncludes 3 acoustic detection storeys equipped with 6 hydrophones each


In situ calibration with Potassium-40 (recently invented)40K40Cage- (b decay)gCherenkovCoincidence plotPeak offsetRate of correlated coincidencesHigh precision (~5%) monitoring of OM efficienciesLED Beacon calibration confirmed13.4 HzMC prediction 13+/-4 HzMean 0RMS 0.7 ns*no charge calibration usedNo dependence on bioluminescent activity has been observed - this confirms the single photon character of bioluminescent emission


Data collected with 5 Lines (Oct 1, 2007)* Line 3 is connected since Jan 27, Lines 4 & 5 since Jan 29, 2007 Physics data taking with 5 Lines started the same day


An example of muon bundle eventDowngoing muon seen with one Lineheighthit time


A neutrino candidate event (5 lines)=35o


First resultsReconstructed nadir angle (very preliminary)Neutrino candidatesAtmosphericmuonsdowngoingupgoingSubset of Line 1-5 data (4.3 M events)Quality cut for upgoing tracksNo alignment used


Ongoing analysesMuon flux is being measured (and compared to Monte Carlo calculations):Using trigger rateNeed precise knowledge of absolute OM efficiency and background-induced trigger rateNumber of reconstructed tracksNeed high level of control over systematic uncertainties of the reconstruction algorithms(NEW) coincidence correlation analysis Use correlated coincidences in adjacent detector storeys (typical signature of physics events)Access to low energy muon flux, depth dependence(!), angular information (fraction of vertical muons)Smaller dependence on OM efficienciesAngular distribution is under studyDifferent reconstruction approaches are being tried


Ongoing analyses (continued)Atmospheric neutrino fluxRelies on thorough understanding of reconstruction efficiencyNeutrino sky mapping & search for point-like sourcesOngoing, see presentation by Fransisco SalesaSetting limits on diffuse fluxUsing showersGRB neutrinoAnalyzing data for 100 GRB alertsGalactic center triggerFirst directional trigger in ANTARES (operating since July)Dark matterNeutralino annihilation in the Sun - start looking forOther sources - relies on point source searchExoticsMonopoles, nuclearites and more


OutlookFive detector lines are operating in the sea the largest neutrino detector in the Northern hemisphere. Four more lines + new instrumentation line have been deployed and are awaiting connection. The last three are prepared.Data taking is ongoing with nearly nominal efficiency. Background conditions are affordable. Data sample is growing by 106 muon triggers every week.The concept and the design of the experiment are proved. Detector calibration can be performed with the required precision. Upward-going neutrinos can be separated from atmospheric muons.Physics analysis is advancing. Atmospheric muons and neutrinos are measured.The experiment is already fully functional and keeps delivering data. Need to finish construction and accumulate more data.


Spare slides


Sea features vs. detector features


Data acquisition, Clock & TriggerAll-data-to-shore DAQHigh bandwidth fiber-optic network (1 GBit /sec/ Line, DWDM)Designed to withstand heavy bioluminescenceFiber-optic clock systemSynchronize electronics modules with precise GPS clock on shoreDeliver commandsOnshore triggerPure softwareRuns on dedicated PC farmAllows for highly efficient customized triggersMany triggers can be run in parallel (just need CPU power)GRB triggerStart on satellite GRB alertSave all data within sufficiently long snapshot (cache in memory)Analyze offlineDirectional triggersGalactic centerSunAny other potential source


antares status report

Documents

antares status reporta

antares status reportdata

antares collaborationd

antares schedule v070910

lines instrumentation

storeys line

connection3 lines

timing calibration