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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, how and why? The ANTARES detector... Detection technique

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Recent Results from the ANTARES experiment

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  1. 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

  2. Outline • -astronomy: what, where, how and why? • The ANTARES detector... • Detection technique • Antares facts & figures • Detector operation • First Physics Analysis • Point Source Search • Transient Source Search • Indirect Dark Matter Search • Multimessenger approach • Conclusions Manuela Vecchi

  3. Neutrino Astronomy • Protons and photons are absorbed or deflected since they interact with matter/radiation. • Neutrinos can travel unscattered opening a new window on the far Universe. • Electrically neutral  not bent by the magnetic fields • Interacts very slightly  escape from the dense areas of the Universe • No absorption  observation at cosmological distances • Only weakly interacting particles  low interaction cross section large detection volume is required  quasar Manuela Vecchi

  4. Detection principle ANTARES 12 lines MC 3D PMTarray Cherenkov light from  42° Sea bed   interaction • Neutrinos can interact in the medium surrounding the telescope. They can be detected using the visible Čerenkov radiation produced as the high-energy charged lepton passes through the transparent medium. A deepunderwater/ice detector is required to reduce the number of atmospheric μs. Manuela Vecchi

  5. Detection principle 3D PMTarray Cherenkov light from  42° Sea bed   interaction • Our GOALs: • Search for production sites of HE neutrinos • Understand production mechanisms of HE neutrinos • Search for Dark Matter (WIMPs) • Exotic particles.... • Neutrinos can interact in the medium surrounding the telescope. They can be detected using the visible Čerenkov radiation produced as the high-energy charged lepton passes through the transparent medium. A deepunderwater/ice detector is required to reduce the number of atmospheric μs. Manuela Vecchi

  6. The ANTARES site Institut M. Pacha Electro-optical Cable of 40 km Manuela Vecchi

  7. The ANTARES detector • 12 Lines • 25 storeys / line • 3 PMTs / storey • 885 PMTs Buoy Floor 14.5 m 350 m Junctionbox 100 m Electro-optical Cable ~60-75 m Depth : 2475 m Manuela Vecchi

  8. Detector Milestones ~60 m • MILOM: 17th Mar 2005 • Line 1: 2nd Mar 2006 • Line 2: 21st Sep 2006 • Line 3, 4, 5: 29th Jan 2007 • Line 6, 7, 8, 9, 10: 7th Dec 2007 • Line 11, 12: 30th May 2008 Manuela Vecchi

  9. Optical Background 40K • 40K Decay Continuous 30kHz background • Bioluminescence  30kHz background, MHz outbursts… Counting rate for 2 PMTs on line 1, as a function of time Manuela Vecchi

  10. Muon flux at the detector 108 atmospheric per year* 103 atmospheric per year* Atmosphere Sea Earth cosmic * Reconstructed tracks in 12 line detector • The data sample is dominated by the flux of atmospheric muons propa- gating downward through the detector. Atmospheric neutrinos contribute providing a flux that is 4-5 orders of magnitude less abundant than that of atmospheric muons. Manuela Vecchi

  11. Track reconstruction • Track reconstructed as upgoing through the detector, as seen in the online event display. Each box correnspond to 1 detection line. arXiv:0908.0816v1 Manuela Vecchi

  12. Track reconstruction Depth • Track reconstructed as upgoing through the detector, as seen in the online event display. Each box correnspond to 1 detection line. Time arXiv:0908.0816v1 Manuela Vecchi

  13. 5-lines data (2007) 2007 data - 19 •106 triggers Total: 245 days Selected: 168 days Detected event are mainly due to downgoing atmospheric muons Down  Up  Manuela Vecchi

  14. 5-lines data (2007)  candidate events Neutrino candidate events: Data: 168 observed MC: 1643(stat)33(theor) 16 (syst) 2007 data - 19 •106 triggers Total: 245 days Selected: 168 days Down  Up  Manuela Vecchi

  15. Atmospheric muons studies Zenith Angle Distribution Azimuth angle distribution data CORSIKA (QGSJET01) + NSU model data data MC uncert. MUPAGE CORSIKA (QGSJET01) + NSU model CORSIKA (QGSJET01) + NSU model 5 lines data CORSIKA (QGSJET01) + Horandel model MC uncert. Systematic uncertainty due to uncertainties in the primary CR flux and hadronic models. No quality cut (QC) applied. Manuela Vecchi

  16. Point source search - 2007data Selected sources for 2007 point source search • Stringent cuts to ensure low background and good resolution. • Search applied to 25 selected sources. • All-sky search has also been performed. • Blinding policy followed Two independent statistical methods used: BINNED and UNBINNED Manuela Vecchi

  17. Point source search - 2007data ANTARES 2007 skymap 5 line data - 94 candidate neutrino events selected in 168 active days. No significant excess has been found. Selected sources for 2007 point source search • Stringent cuts to ensure low background and good resolution. • Search applied to 25 selected sources. • All-sky search has also been performed. • Blinding policy followed Two independent statistical methods used: BINNED and UNBINNED arXiv:0909.1262v1 Manuela Vecchi

  18. Point source search - Results • Upper limits (90% c.l.), as a function of the declination, for the selected point-like sources. arXiv:0909.1262v1 Manuela Vecchi

  19. Search for transient sources The satellite triggered data taking efficiency during all alert message broadcasts from the GCN arXiv:0908.0818v1 • Search for  candidates in correlation with GRB alerts from satellites. Whenever an alert is received, a dedicated data-taking is performed. The response time of the satellite triggered data taking in Antares to a satellite alert message. Manuela Vecchi

  20. Indirect dark matter search • Cold Dark Matter Candidate: decays of neutralinos (WIMPs) gravitationally trapped in massive objects, i.e. the Sun, can produce HE s detectable by ANTARES. arXiv:0905.2316v3 A search for s from neutralino annihilation in the Sun has been performed on 2007 data. Data sample 68.4 effective days No discovery 90% C.l. Upper limit mSugra model predictions green : WMAP favoured relic density red : > WMAP favoured relic density blue : < WMAP favoured relic density Manuela Vecchi

  21. 2007-2008 data 2007 (5 lines) : 168 d.  19 •106 triggers 2008 ( 9 lines): 173 d.  65•106 triggers TOTAL 341 days lifetime. Single & multi-line fit events are shown. Up  Down  •  MC error band (theoretical + systematic) 30% •  MC error band (theoretical + systematic) 50% Manuela Vecchi

  22. 2007-2008 data 2007 (5 lines) : 168 d.  19 •106 triggers 2008 ( 9 lines): 173 d.  65•106 triggers TOTAL 341 days lifetime.  candidate events Up  Down  • All 2007/2008 silver runs ~ 1000s •  MC error band (theoretical + systematic) 30% •  MC error band (theoretical + systematic) 50% Manuela Vecchi

  23. 2007-2008 skymap ANTARES 2007-2008 skymap (scrambled data) • 750 multilines neutrino candidates from 2007 and 2008, for 341 days of detector lifetime. Manuela Vecchi

  24. Multimessenger approach www.gwhen-2009.org • Agreement with TAROT*: • optical telescope at • La Silla (CL) • FOV: 1.86° x 1.86° • Fast (~10s) re-positioning • Optical follow-upof • transient sources • triggered by the ANTARES detector • The trigger is satisfied when: 1 evt with E > few TeV or 2 evts detected within  = 3° x 3°. arXiv:0908.0804v2 * Télescopes à Action Rapide pour les Objets Transitoires • Joint searches between gravitational-wave interferometers and ANTARES. • Possible common sources (GRBs from core-collapse SN or from BH/NS binary merger; SGR;powerful magnetars; hidden sources) • Sky regions in common • Expected low signals, coincidences increase chances of detection arXiv:0908.2454v1 Manuela Vecchi

  25. Conclusions • The ANTARES experiment is complete and taking data. • First analyses on 2007 data show that the detector perfomance is well within expectactions. • First upper limits to the flux of neutrinos from point-like sources have been set. • First flux limits from ‘hard’ and ‘soft’ neutralino annihilation in the Sun have been set. • Analysis of 2008 data is under way. • Multimessenger approach is strongly pursued. • …detected 1000 neutrino candidates, a lot more science to come....... Manuela Vecchi

  26. Backup slides Manuela Vecchi

  27. 2007 data Results of 2 independent analysis Observed: 168 events MC: 1643(stat)33(theor) 16 (syst) Observed: 185 events MC: 2184(stat)41(theor) +3-42 (syst) Manuela Vecchi

  28. The trigger  • Front end chip digitizes charge and time of a light signal • All data transmitted through multiplexed Gigabit links • the whole data flow can not be written to disk • Computer farm running a software trigger: • look in all directions for light signals • compatible with a muon track • when found, write a Physics Event • Other triggers exist: • cluster of storeys,GRBs, Galactic Center, … “ALL DATA TO SHORE” SCHEME: Manuela Vecchi

  29. Expected performance Effective area Ndet=Aeff × Time × Flux Manuela Vecchi

  30. Indirect DM search (2) ANTARES FULL DETECTOR Predicted measured flux of  + anti from neutralino annihilation in the Sun, for the full ANTARES detector, after 5 years. • ANTARES 2007 data • Upper limit to the flux of  + anti • from neutralino annihilation in the Sun, compared to other experiments, as a function of neutralino mass. Manuela Vecchi

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