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NEMO geometry studies

NEMO geometry studies. R. Coniglione and P. Sapienza. Istituto Nazionale di Fisica Nucleare- Laboratori Nazionali del Sud. NEMO geometry and bar length effects Geometry studies:  Energy dependence  Angular dependence  Atmospheric muons. Bar length effect. The geometry.

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NEMO geometry studies

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  1. NEMO geometry studies R. Coniglione and P. Sapienza Istituto Nazionale di Fisica Nucleare- Laboratori Nazionali del Sud • NEMO geometry and bar length effects • Geometry studies: • Energy dependence • Angular dependence • Atmospheric muons R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  2. Bar length effect • The geometry • Inputs in the Antares codes • Muon simulation up-going • Trigger based on (local coincidence) or (high amplitude hit p.e.>2.5p.e.) • Capo Passero water parameters • Trigger (floor coincidence 3 / 4 or amp. >2.5 p.e.) - Aart strategy • old angular efficiency in PMT • Effective muon area as a function of the bar length and the optical background rate • Bar length 20, 15, 10, 7.5, 1 m • Optical background 35,50,100,150 kHz •  from to ….. 20m 1 m R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  3. Bar length effect 35 kHz bar length 20m  bar length 15m bar length 10m bar length 7.5m bar length 1m quality cut applied 1°@1TeV Effective area ratio with respect to 20m R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  4. Bar length effect 50 kHz – quality cut applied 1°@1TeV Muon effective area Effective area ratio with respect to 20m bar length 20m  bar length 15m bar length 10m bar length 7.5m bar length 1m R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  5. Bar length effect 15m bar lenght Vertical muons cos qm >0.8 (~36°) RMS ~24° RMS ~55° 50 kHz background Em 102104 GeV j- jrec q-qrec 1m bar lenght RMS ~27° RMS ~65° q-qrec j- jrec R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  6. Bar length effect 100 kHz – quality cut applied 1°@1TeV Ratio with respect to 20m Muon effective area bar length 20m  bar length 15m bar length 10m bar length 7.5m bar length 1m R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  7. Bar length effect 150 kHz – quality cut applied 1°@1TeV Muon effective area Ratio with respect to 20m bar length 20m  bar length 15m bar length 10m bar length 7.5m bar length 1m R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  8. Bar length effect quality cut applied 1°@1TeV Muon effective area Bar lenght 1m Bar lenght 20m 35 kHz  50 kHz 100 kHz 150kHz R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  9. Geometry studies • The geometries • Inputs • Neutrino simulation E-2 spectrum • ANTARES water parameters • New PMT angular acceptance (fit1 Genova Antares note 2008-001) • 40 kHz background • Trigger based on (local coincidence) or (high amplitude hit p.e.>2.5p.e.) • Aart reconstruction R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  10. data Genova param (Valencia meeting) data Genova param (Valencia meeting) rec. track/s rec. track/s Aart strategy Aart strategy L > -6.3 No QC q data Genova param (Valencia meeting) Aart strategy L q Aart strategy L > -6.3 data = 0.65 reco tr/s MC = 0.72 reco tr/s ratio = 0.9 Aart strategy NO QC data = 0.97 reco tr/s MC = 0.87 reco tr/s ratio = 1.1 From A. Margiotta R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  11. After cut applied to reject n and muon background in sensitivity studies for point like sources Energy spectrum of detectable neutrinos Energy range of interest: 1-100 TeV Geometry studies: the energy range =1.5 =2.5 =2 R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  12. Detector performance vs n energy Without quality cut n up-going 40 kHz DW=m-mrec DW=n-mrec ANT_127 (9525PMT) NEMO_127 (9144PMT) With Quality cut DW = n-mrec Aneff (m2) Aneff (m2) ratio R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  13. Detector performance vs n zenith angle Ant_127 With quality cut DW = n-mrec 102 103 GeV 103 104 GeV 104 105 GeV 105 106 GeV 106 107 GeV NEMO 127 DW = n-mrec R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  14. Detector performance vs n zenith angle 103 104 GeV 104 105 GeV  ANT_127  NEMO_127 These results, with the new PMT angular acceptance, confirm the best performance for vertical muons of the tower-like geometry. -> New trigger could be explored R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  15. Detector performance: the atmospheric muonswork in progress • The geometries • Inputs • Atmospheric muons simulated with Okada • ANTARES depth 2400m • ANTARES water parameters • New PMT angular acceptance (fit1 Genova) • 40 kHz background • Trigger based on (local coincidence) or (high amplitude hit p.e.>2.5p.e.) • Aart reconstruction NEMO_127 ANT_127 R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  16. Detector performance vs atmospheric muons At the can level ANT_127 NEMO_127 Flux NEMO_127 Flux ANT_127 ~ 3 R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  17. Detector performance vs atmospheric muons Energy spetrum at the can of reconstructed muons No quality cut applied Reconstructed muons No quality cut applied ANT_127 NEMO_127 ANT_127 NEMO_127 cos qmrec Flux ANT_127 Flux NEMO_127 Misreconstructed flux (cos qmrec >0 ) ~ 3 R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  18. Down going muons Median and effective area for down-going muons ANT_127 NEMO_127 R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  19. Atmospheric muons: PMT angular acceptance effect Reconstructed muons No quality cut applied Genova PMT angular acceptance Old PMT angular acceptance ANT_127 NEMO_127 ANT_127 NEMO_127 R. Coniglione, KM3NeT, Catania 10-13 March ‘08

  20. OUTLOOK • Simulations for the “reference” detector described in the S. Kuch thesis are in progress. • New triggers that optimize the performance for each detector geometry should be implemented • Mupage simulation to explore the effects of multi-muon events • Sensitivity studies for different neutrino sources and different geometries R. Coniglione, KM3NeT, Catania 10-13 March ‘08

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