Скачать презентацию Proposal for a Large Multipurpose Detector LMD at Homestake Скачать презентацию Proposal for a Large Multipurpose Detector LMD at Homestake

1f1e5df407ccbfa35ff7eb725de2ef46.ppt

  • Количество слайдов: 46

Proposal for a Large Multipurpose Detector(LMD) at Homestake MILIND DIWAN Brookhaven National Laboratory 3/6/2006 Proposal for a Large Multipurpose Detector(LMD) at Homestake MILIND DIWAN Brookhaven National Laboratory 3/6/2006 first phase: LMD-1 100 k. T or 200 k. T water Cherenkov, Fiducial: 75 -150 k. T

Participants in LOI for Homestake • D. Cline, M. Diwan, K. Lande, R. Lanou, Participants in LOI for Homestake • D. Cline, M. Diwan, K. Lande, R. Lanou, A. K. Mann, W. Marciano • Speaking for many others. All are welcome. • Close cooperation with UNO on the science. • We advocate building one or two 100 k. T cavities as soon as possible. M. Diwan

Outline of this talk • Will focus on LMD-1, 100 k. T water Cherenkov Outline of this talk • Will focus on LMD-1, 100 k. T water Cherenkov detector at Homestake • Physics topics: • Very Long Baseline Neutrino Oscillation • Nucleon decay • Astrophysical neutrinos • Brief details of study on accelerator beams. M. Diwan

Detector parameters • • Need 500 k. T fiducial mass for proton decay, neutrino Detector parameters • • Need 500 k. T fiducial mass for proton decay, neutrino astrophysics. 100 k. T is initial step => 50 m dia X 50 m high tank. depth ? May not need anti-counter if deep enough. ~10% energy resolution on quasilelastics. Threshold of 5 Me. V for solar and supernova Time res. ~few ns for pattern recognication. Good mu/e separation. <1%. • 1, 2, 3 track separation, NC rejection ~X 20. This level of performance can be obtained with water Cherenkov detector with 20 -40% PMT coverage. => 11000 to 22000 20 inch PMTs for 100 k. T. M. Diwan

What does it look like 50 m diameter and 50 m tall Bigger but What does it look like 50 m diameter and 50 m tall Bigger but based on Super-kamioka. NDE Super. Kamioka. NDE: 22. 5 -50 k. T LMD-1: ~75 -100 k. T M. Diwan

Cavity cost From K. Lande and M. Laurenti 208 weeks 4 cavities for $44 Cavity cost From K. Lande and M. Laurenti 208 weeks 4 cavities for $44 M could be accelerated M. Diwan

Detector cost M. Diwan Detector cost M. Diwan

4850 ft: 100 k. T ~3 M mu/yr with rate of 1 mu/10 sec 4850 ft: 100 k. T ~3 M mu/yr with rate of 1 mu/10 sec => may not need veto-counter Site proposed here The Beam neutrinos will be obvious with a rate of 100 -200/day in 10 mus spills. No pattern recognition beyond time cut is needed. Deep option depth meters water equivalent M. Diwan

Open issues on detector • • • Depth and veto counter - has cost, Open issues on detector • • • Depth and veto counter - has cost, schedule and physics implications. Perhaps only the first module is built without veto-counter for a fast start. Fiducial volume. If SK cut good enough => 75 k. T. PMT coverage: 20 % adequate from SK experience. 40% if very low threshold is needed. PMT size: 13 inch versus 20 inch. Greater number of pixels will give better pattern recognition. Size of detector: very difficult to increase span. If made bigger has cost and schedule implications. 50 meter span seems adequate to contain beam events. M. Diwan

 • • Nucleon decay Large body of work by Hyper. K, and UNO. • • Nucleon decay Large body of work by Hyper. K, and UNO. background levels for the positron+Pion mode • 3. 6/MTon-yr (normal) • LMD-1(100 k. T) will hit 0. 15/MTon-yr (tight) backg. in ~3 yrs. It could be important to perform this first step before building bigger. Sensitity on K-nu mode is about 5 x 10^33 yr Ref: Shiozawa (NNN 05) M. Diwan LMD-1 X 10 yrs 3 X 10^34 yrs

Astrophysical Neutrinos Event rates. LMD-1(100 k. T), assume 5 yrs • • Atmospheric Nus: Astrophysical Neutrinos Event rates. LMD-1(100 k. T), assume 5 yrs • • Atmospheric Nus: ~10000 muon, ~5000 electrons. (Ref: Kajita nnn 05) Solar Nus: >63000 elastic scattering E>5 Me. V (including Osc. ) (Ref: uno) Galactic Supernova: ~30000/10 sec in all channels. (~1000 elastic events). (Ref: uno) Relic Supernova: (ref: Ando nnn 05) • • flux: ~5 (1. 1) /cm 2/sec Enu>10 (19) Me. V rate: 75 (35) events over backg ~100 ! Need analysis with these numbers M. Diwan

M. Diwan M. Diwan

M. Diwan M. Diwan

M. Diwan M. Diwan

M. Diwan M. Diwan

M. Diwan M. Diwan

60 Ge. V 28 Ge. V M. Diwan 60 Ge. V 28 Ge. V M. Diwan

 • Sensitivity to CP is independent of Important points distance! (see P. Huber’s • Sensitivity to CP is independent of Important points distance! (see P. Huber’s calculation) • The size of detectors and beam power needed does not depend on theta_13 (as long as it is not very small) • We need low energy broad band beam. Must have ~4 m wide tunnel. I have assumed 200 m length. Low energy horn also(with target deep M. Diwan inside)

US possibilities for beam Proton beam energy Proton beam power FNAL MI (Mc. Ginnis US possibilities for beam Proton beam energy Proton beam power FNAL MI (Mc. Ginnis upgrade) Ep=8 -120 Ge. V 1 -2 MW X (Ep/120 Ge. V) FNAL MI (with 8 Ge. V LINAC) Ep=8 -120 Ge. V 2 MW @ any Ep BNL-AGS (upgrade 2. 5 - 5 Hz) Ep=28 Ge. V 1 -2 MW Source M. Diwan

US possible baselines Sourc e Distanc e Depth Comment 1290 km 4850/77 00 ft US possible baselines Sourc e Distanc e Depth Comment 1290 km 4850/77 00 ft no beam, DUSEL site, capable of large exca. Henderso FNAL 1500 km ~4000 ft n no beam, DUSEL site, capable of large exca. Detector Homestak FNAL e BNL Homestak 4850/77 2540 km e 00 ft study of beam and physics exists and documented BNL Hendersn 2767 km ~4000 ft -- shorter baseline means more events. longer baseline means bigger effects. M. Diwan

Neutrino Event rates Source-det Detector size FNAL-HS(1290) 100 k. T FNALHend(1500) FNAL-HS(1290) 100 k. Neutrino Event rates Source-det Detector size FNAL-HS(1290) 100 k. T FNALHend(1500) FNAL-HS(1290) 100 k. T Event rate for beam E and power neutrino running 0. 5 [email protected] Ge. V ~30, 000 CC ~10, 000 NC 0. 5 [email protected] Ge. V ~22, 000 ~7500 2 [email protected] Ge. V 78, 000 CC 27, 000 NC using Miniboone data 1094 CC FNAL-HS(1290) 100 k. T 2 [email protected] Ge. V 425 NC 5 X 10^7 sec of running assumed ~10000 CC NOVA(810)* 30 k. T 0. 65 [email protected] ~3000 NC *rescaled: NOv. A assumes 2 e 7 sec * 5 yrs of running in their proposal M. Diwan

How to achieve the total exposure • For CP violation we need (indep. of How to achieve the total exposure • For CP violation we need (indep. of baseline or size of theta_13) (Marciano) • 2500 k. T*MW*(10^7) sec for neutrinos 1 yr ~ 1 e 7 sec 500 k. T 1 MW 5 yrs Past approach 1 yr ~ 2 10^7 sec 100 k. T We could go to 200 k. T if only 2 MW 1 MW 6. 25 yrs Possible at FNAL with new Proton driver M. Diwan

M. Diwan M. Diwan

includes anti running, but large fraction of M. Diwan the result is from nu includes anti running, but large fraction of M. Diwan the result is from nu running for normal

We prefer to think of CP as a parameter measurement M. Diwan We prefer to think of CP as a parameter measurement M. Diwan

Very easy to get this effect Does not need extensive pattern recognition. Can enhance Very easy to get this effect Does not need extensive pattern recognition. Can enhance the second minimum by background subtraction. M. Diwan

Assumptions • • • M. Diwan WBB: nu: 100 k. T*2 MW*6 yr. antinu: Assumptions • • • M. Diwan WBB: nu: 100 k. T*2 MW*6 yr. antinu: 100 k. T*2 MW*6 yr syst: 10% on bck Antinu runnining is over -constraint for normal hierarchy. T 2 HK: nu: 1000 k. T*4 MW*3 yr antinu: 1000 k. T*4 MW*3 yr syst: 2% on bck NOVA 2: nu: 30 k. T*2 MW*6 yr+ 80 k. T*2 MW*3 yr antinu: same*6 yr+3 yr syst: 5% on bck

M. Diwan M. Diwan

Open issues on beam • • • What is the correct proton energy and Open issues on beam • • • What is the correct proton energy and power level from FNAL What is the cost of a new beam To get intensity at low energies must have ~4 meters diameter tunnel. I have length of 200 meters to get the spectra in this talk. How should we tailor the spectrum for maximum signal/noise ? If tunnel is wide WE CAN ALWAYS RUN OFFAXIS by moving and tilting the horn/target. (upto 1 deg. ) What is the time sequence ? Proposal on next slide. M. Diwan

 • • • Summary Physics case for a 100 k. T detector at • • • Summary Physics case for a 100 k. T detector at Homestake. nucleon decay, astrophysical neutrinos, long baseline. Lowest risk most cost effective option for a long baseline second generation experiment. Money ? It will cost money, but time and scientific manpower issues more important. Possible time sequence: • • • 100 k. T + 0. 5 MW (60 Ge. V)=> 68 evts/day 200 k. T + 1 MW (30 Ge. V) => 180 evts/day 200 k. T + 2 MW (30 Ge. V)=> 360 evts/day M. Diwan

EXTRAS M. Diwan EXTRAS M. Diwan

from T. Kirk M. Diwan from T. Kirk M. Diwan

from T. Kirk M. Diwan from T. Kirk M. Diwan

Electron neutrino appearance physics parameter extraction For 1000 - 2000 km baseline effects across Electron neutrino appearance physics parameter extraction For 1000 - 2000 km baseline effects across energy band. M. Diwan

What about anti-nu running • Depends on mass hierarchy. • To be completely risk-free What about anti-nu running • Depends on mass hierarchy. • To be completely risk-free need • 5000 k. T*MW*(10^7) sec 1 yr ~ 1 e 7 sec 500 k. T 2 MW 5 yrs Past approach 1 yr ~ 2 e 7 sec 200 k. T 2 MW 6. 25 yrs Possible at FNAL with new Proton Driver M. Diwan

We want to grow to. . 4850 focus on 100 k. T at the We want to grow to. . 4850 focus on 100 k. T at the moment Some of these cavities could house other types of detectors including liquid Argon, liquid scint. , etc. Safety req. will be different M. Diwan

How to build it. . M. Diwan How to build it. . M. Diwan

M. Diwan M. Diwan

M. Diwan M. Diwan

M. Diwan M. Diwan

M. Diwan M. Diwan

Comparison to 1290 km to 2540 km M. Diwan Comparison to 1290 km to 2540 km M. Diwan

M. Diwan M. Diwan

M. Diwan M. Diwan