Supernova Energy Reconstruction Flash Match John M. LoSecco - - PowerPoint PPT Presentation

Supernova Energy Reconstruction Flash Match

John M. LoSecco University of Notre Dame November 20, 2019

Supernova Energy Reconstruction Flash Match (John LoSecco) 1/9

Introduction – Energy Reconstruction

◮ Light flash observed ◮ Charge collected ◮ Flash time matched to charge collection ◮ Electron lifetime correction to charge ◮ Corrected charge converted into energy Electrons have a finite lifetime before they are captured and no longer drift. The charge from energy deposited near the far wall is attenuated by about a factor of two while drifting to the collection plane. The light flash is also attenuated via Raleigh scattering. This can be as much as a factor of ≈100 from the far side of the detector. This is an effective attenution length of ≈75 cm.

Supernova Energy Reconstruction Flash Match (John LoSecco) 2/9

Simulations

htemp Entries 788000 Mean 0.02283 Std Dev 0.008934 0.02 0.04 0.06 0.08 0.1 EnuT 5000 10000 15000 20000 25000 30000 35000 40000 htemp Entries 788000 Mean 0.02283 Std Dev 0.008934

EnuT

htemp Entries 788000 Mean 0.0162 Std Dev 0.008299 0.01 0.02 0.03 0.04 0.05 0.06 0.07 0.08 0.09 Heel 5000 10000 15000 20000 25000 30000 35000 40000 htemp Entries 788000 Mean 0.0162 Std Dev 0.008299

Heel

◮ Marley event generator ◮ Supernova νe spectrum; no oscillations – left figure ◮ Uniform in the detector fiducial volume

◮ Compare with electron not neutrino energy – right figure ◮ Simulation reprocessed to get much higher light collection ◮ Simulation “frame” is two full drift times ◮ Only samples without radioactive backgrounds in this talk

Supernova Energy Reconstruction Flash Match (John LoSecco) 3/9

Flash with Distance

50 100 150 200 250 300 350 (abs((0.08*(wireDepoTicks3*.5-Ltf)*2.)+5.0)) 50 100 150 200 250 300 350 abs(Xnu)

abs(Xnu):(abs((0.08*(wireDepoTicks3*.5-Ltf)*2.)+5.0)) {wireDepoTicks3!=0.&&Ltf>-0.1&&Ltf<0.4}

htemp Entries 35 Mean 3.407 Std Dev 0.2434 3 3.2 3.4 3.6 3.8 4 log10(Lef*exp(abs(Xnu)/75.)) 0.5 1 1.5 2 2.5 3 htemp Entries 35 Mean 3.407 Std Dev 0.2434

log10(Lef*exp(abs(Xnu)/75.)) {wireDepoTicks3>0.&&(Ltf>-0.1&&Ltf<0.4)&&(Heel>0.03&&Heel<0.04)&&abs(Xnu)<10.}

Drift time vs drift distance, Left. Comparison of log10 corrected flash pulse amplitude near the collection (blue) and far from it (red) with a 75 cm attenuation length, Right.

Supernova Energy Reconstruction Flash Match (John LoSecco) 4/9

Flash with Distance II

50 100 150 200 250 300 350 abs(Xnu) 2 2.5 3 3.5 4 log10(Lef*exp(abs(Xnu)/75.))

log10(Lef*exp(abs(Xnu)/75.)):abs(Xnu) {wireDepoTicks3>0.&&(Ltf>-0.1&&Ltf<0.4)&&(Heel>0.0125&&Heel<0.0175)&&log10(Lef*exp(abs(Xnu)/75.))>2.}

htemp Entries 485 Mean 1163 Std Dev 493.9 500 1000 1500 2000 2500 3000 3500 Lef*exp(abs(Xnu)/78.5) 5 10 15 20 25 htemp Entries 485 Mean 1163 Std Dev 493.9

Lef*exp(abs(Xnu)/78.5) {wireDepoTicks3>0.&&(Ltf>-0.1&&Ltf<0.4)&&(Heel>0.0125&&Heel<0.0175)&&Lef*exp(abs(Xnu)/75.)<4000.&&abs(Xnu)<22.5}

Log10 corrected light flash pulse amplitude vs distance for 15 MeV pulses, Left. Corrected flash pulse amplitude for near (blue) and far (red) with a 78.5 cm attenuation length, Right

Supernova Energy Reconstruction Flash Match (John LoSecco) 5/9

Reco Energy with Flash or Charge – MC Distance

0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 Heel 0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 (Lef*exp(abs(Xnu)/75.))/1.016e+5

(Lef*exp(abs(Xnu)/75.))/1.016e+5:Heel {wireDepoTicks3>0.&&(Ltf>-0.1&&Ltf<0.4)&&(Heel>0.0&&Heel<0.04)&&Lef*exp(abs(Xnu)/75)<4000.}

0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 Heel 0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 0.045 0.05 (charge*exp(abs(Xnu)/300.)/1.916e5) (charge*exp(abs(Xnu)/300.)/1.916e5):Heel {(Ltf>-0.1&&Ltf<0.4)&&Heel<0.04}

Top: Corrected Flash energy vs MC energy, Left. Corrected Charge energy vs MC energy, Right.

Supernova Energy Reconstruction Flash Match (John LoSecco) 6/9

Reco Energy with Flash or Charge – MC Distance II

0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 0.045 0.05 (charge*exp(abs(Xnu)/300.)/1.916e5) 0.01 0.02 0.03 0.04 0.05 0.06 0.07 0.08 0.09 ((Lef*exp(abs(Xnu)/75.))/1.016e+5)

0.005 0.01 0.015 0.02 0.025 0.03 0.035 0.04 Heel 0.04 − 0.03 − 0.02 − 0.01 − 0.01 0.02 0.03 0.04 ((Lef*exp(abs(Xnu)/75.))/1.016e+5)-(charge*exp(abs(Xnu)/300.)/1.916e5)

Corrected Flash energy vs corrected charge energy, Left Corrected Flash energy minus corrected charge energy vs MC energy.

Supernova Energy Reconstruction Flash Match (John LoSecco) 7/9

Extra Flashes? – Clean Events

Mean number of flashes is 1.54 per event or 1.57 excluding the 2% with no flash. 43% have more than 1 flash.

4 − 3 − 2 − 1 − 1 2 log10(Lef/Lef[0]) 1 2 3 4 5 6 7 8 Ltf

Ltf:log10(Lef/Lef[0]) {wireDepoTicks3!=0.&&!(Ltf>-0.1&&Ltf<0.4)&&(Ltf>-.25&&Ltf<8.)&&NOf>1&&Lef!=Lef[0]}

50 100 150 200 250 300 350 abs(Xnu) 4 − 3 − 2 − 1 − 1 2 log10(Lef/Lef[0])

log10(Lef/Lef[0]):abs(Xnu) {wireDepoTicks3!=0.&&!(Ltf>-0.1&&Ltf<0.4)&&(Ltf>-.25&&Ltf<8.)&&NOf>1&&Lef!=Lef[0]}

The extra flashes are from 10 to 100 times smaller and 1 to 5 µsec late, Left. The extra flashes are weaker if the vertex was near the collection, Right.

Supernova Energy Reconstruction Flash Match (John LoSecco) 8/9

Systematic Errors – Distance correction errors

◮ LRayleigh at 128 nm ... Literature 90, 55±5, 66±3 cm. I calculated ≈ 75 cm from the MC ... use 75 cm to illustrate. ◮ ∆x ≈ 2.5 cm →

∆x LRayleigh = 0.033

◮ Correction is C = ex/LRayleigh ◮ ∆C = ex/LRayleigh

∆x LRayleigh

◮ At x = 100 cm ∆C = 12.5% ◮ At x = 300 cm ∆C = 180% ◮ Drift offset: the vertex is not the drift distance since collection is not at X=0. — systematic error We need redundant flash information. Light collection on two walls.

Supernova Energy Reconstruction Flash Match (John LoSecco) 9/9