mini- H igh A ltitude W ater C herenkov experiment
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Transcript of mini- H igh A ltitude W ater C herenkov experiment
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
mini-High Altitude Water Cherenkov experiment
e
145 meters
4 meters
Andrew SmithUniversity of Maryland
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
What is miniHAWC?
• Milagro – Existing water Cherenkov all-sky gamma-ray observatory.
• HAWC – A “science” driven effort to construct an all-sky observatory with point source sensitivity of the Whipple 10m.
• miniHAWC – Demonstrate HAWC technology at low cost with Milagro PMTs/instrumentation.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
What is the Sensitivity of miniHAWC?
Answer: ~15x Milagro. 1y ~60mCrab source at 5
Interpretation 1: Designers of Milagro are Stupid.Interpretation 2: Designers of miniHAWC are Smart.
Designers of Milagro = Designers of miniHAWC
Interpretation 3: Designers of Milagro/miniHAWC were naive, but have wised up.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Critical Variables
• Size – Bigger is better until you reach sqrt(A) regime.
• Photocathode Density – More is better until you detect all the particles.
• Altitude – Higher is better until you can’t breathe. Diminishing returns.
Tools: PMTs (8” Hamamatsu), Water, black and white materials.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Detector Layout
Milagro:450 PMT (25x18) shallow (1.4m) layer273 PMT (19x13) deep (5.5m) layer175 PMT outriggers
Instrumented Area: ~40,000m2
PMT spacing: 2.8mShallow Area: 3500m2
Deep Area: 2200m2
HAWC:5625 or 11250 PMTs (75x75x1,2)Single layer at 4m depth or 2 layers at Milagro depths
Instrumented Area: 90,000m2
PMT spacing: 4.0mShallow Area: 90,000m2
Deep Area: 90,000m2
miniHAWC:841 PMTs (29x29)5.0m spacingSingle layer with 4m depth
Instrumented Area: 90,000m2
PMT spacing: 4.0mShallow Area: 90,000m2
Deep Area: 90,000m2
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Equipment
• Milagro DAQ:– 898 8” Hamamatsu PMTs– Single data/HV cable ~150m length – Custom front end boards. Analog to level crossing
conversion. (Amplitude through time over threshold.)– FASTBUS TDC– VME – FASTBUS interface with VME readout– 2000Hz maximum readout with ave multiplicity ~20-30%
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
How do you make an EAS array more sensitive to gamma-ray sources?• Energy Threshold
– Altitude– Big, hermetic, sensitive
• Angular Resolution– Big Lever Arm
• gamma/hadron Separation– Must detect penetrating particles
Sensitivity increase is the product of the improvement made in each category.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
4500m
2600m
Difference between 2600m (Milagro) and 4500m (Tibet):~ 6x number of particles~ 2x lower energy threshold
Altitude
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Hadron induced cosmic ray showers contain 5-20x more energyin penetrating +/- and hadrons than EM particles.
High Pt hadronic interactions lead to wide lateral distributions.
Need mass! Need large Area!
Muon/hadron Detection
HAWCminiHAWC
Milagro
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
High Altitude Detector w/o /hadron separation
ARGO: ~6000m2 RPC detector.
Reported at ICRC expect sensitivity of 8-13/year on the Crab.
Milagro currently achieves~8/year on the Crab.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Curtains
• A high altitude version of Milagro would trigger at >10kHz. Need to control spurious triggers due to single muons.
• Install curtains to optically isolate the the PMTs.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Simulation Strategy
• Use Milagro Simulation/Reconstruction software.
• Use observed Milagro crab signal to anchor simulations to reality. Shared systematics with Milagro.
• Use new /hadron discrimination variable for HAWC/miniHAWC that excludes the core location.
CMilagro = (nPMTs above 2 PE)/(Max “muon layer” hit)
CminiHAWC = (nPMTs above 2 PE)/(Max “muon layer” hit > 20m from core)
• As an illustration, consider 2 trigger threshold: 50 PMTs, 200 PMTs.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
= ~0.4 deg = ~0.25 deg
Angular Resolution
/hadron Separation
Cut: nTop/cxPE>5.0Eff = 34%Eff CR= 3%
Cut: nTop/cxPE>5.0Eff = 56%Eff CR= 1.5%
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Triggering with Curtains
• Multiplicity trigger at ~80 PMTs gives same trigger rate as Milagro at 50 PMTs• Much higher Gamma area.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Effective Area
Detector size
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Energy (Crab Spectrum, nTop/cxPE>5.0., <30O)Significance fromCrab Transit (~5 hr) 4
Crab signif/year 80
5 point source sensitivity reach ~60mCrabof 1 year survey
Energy Resolution ~30% above median
Angular Resoultion 0.25O-0.40O
S/B (hard cuts) ~ 1:1 for CrabTypical day 20 excess on 25 bkg
Q(Milagro -> miniHAWC) = 15!
Single layer doesn't limit sensitivity
miniHAWC Sensitivity
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Curtains Test in Milagro
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Site
– High Altitude.– Power– Internet– Don’t need darkness or
good weather…– YBJ very interested. – Chinese don’t have money for site prep.
(ARGO)– Investigating a site in Mexico.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Cost - Detector Elements
• Pond (0.2-2.0 M$)• Black Liner Material (~100k$ @ $1/m2 )• Pump/Recirculation System. (~$200k$)• PMTs – Reuse with base and encapsulation w/ new
connectors.• Cables – Purchase new. (~100$k)• Front End Electronics – keep as is.• TDC and DAQ
– 2kHz DAQ keep current electronics– Faster VME TDCs (~200$k)
• Online computing – A few computers can reconstruct in real time. (~10$k)
• Building – Assemble functional DAQ in a trailer and ship to site. (~200$k)
• Internet Access – Live with slow internet if necessary. Need prompt alert capability.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Issues – The Good/Bad• Simple Analysis- Event weighting could increase
sensitivity further. In Milagro Q=1.6.
• Can reconstruct showers down to 20 PMTs if we could trigger at 6kHz.
• Site.
• Calibration.
• Noise.
Milagro in 1.4y ~8/y
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Summary
• 15x Sensitvity increase over Milagro~3x from Altitude,Area~3x from /hadron separation~1.5x from Angular resolution
• ~60mCrab sensitivity (5 in 1year)
• Mostly proven technology– Leverage $1.5M investment in Milagro equipment– Could construct rapidly if site available.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
An Ideal Air Shower Gamma-Ray Detector:
1) Large Physical AreaCollection AreaContain CoreSample Lateral Tails
2) High Efficiency for 20 MeV Continuous DetectorEfficient e Converter
3) Calorimetry Hadron/Muon Identification
4) Altitude~40gm/cm2 increase in altitude double ground level particles.Lowers threshold.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
1) Large Physical Area
(Diagram Showing Shower Curvature)
Core position reconstruction required for accurate angle reconstruction. --> Core must be contained within detector --> Effective area <~ Physical Area --> 104 to 105 m2 detector required to rival area of IACTs --> Long lever arm for angle reconstruction.
Shower front is curved.Without core position: Pointing error dominated by systematics ==>
PSF >~ 0.7O
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
2) High Efficiency for detection of 20MeV Gamma-Rays
In extended air showers 's out number e+/- by 5-10 to 1.
Mean energy of EAS 's is ~20 MeV. ( not strongly correlated with primary VHE energy.)
Plot showing spectrumof showering particles
Plot Showing de/dxfor electrons.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
HAWC layout
75x75 grid of 8” PMTs - in 2 layers (depth =2m,6m, separation = 4m)
Angle reconstruction with top layer. Calorimetry with bottom layer
Opaque “curtains” separate PMT cells.Eliminate “cross talk” between counter.Limits trigger rate compared to Milagro
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
How does the HAWC design measure up?
1) Size: – 300mx300m = 90,000 m2
2) Efficiency: Water acts a both conversion medium and radiator. ~1 PE/25 MeV
3) Calorimetry: Deep (~15Xo) PMT layer for Muon/Hadron rejection.
4) Altitude: Select optimal site.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Simulation Strategy
Simulate various HAWC geometries at 2 altitudes.Compare results with Milagro. (Milagro sensitivity verified by observations of the Crab.)
2 altitudes considered: 4500m ( ~Tibet Lab altitude) 5200m ( ~Atacama Plateau)
2 sets of cuts considered: Std - 50 PMT multiplicity cut Hard - 200 PMT multiplicity cut
= ~0.4 deg = ~0.25 deg
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Gamma-Hadron Separation:
Remove events with one or more large hits away from the core ---> muon/hadrons in lateral tails ---> “cxPE” is largest bottom layer hit with R
core>10m
---> “nTop” is number of PMTs hit in top layer
Cut: nTop/cxPE>10.0Eff = 40%Eff CR = 5%
Cut nTop/cxPE>10.0Eff g = 65%Eff CR = 2%
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Energy of reconstructed events (Crab Spectrum)nTop/cxPE>10., <30O
Altitude = 4500m
Altitude = 5200m
Threshold Lower at zenith.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Point Source Sensitivity of HAWC:
Altitude 5200m 4500mCrab Transit (~4 hr) 25 10 Median Energy
Time to 5 10min 60min
5 point source sensitivity reach 10mCrab 25mCrabof 1 year survey
Energy Resolution ~30% above median
~1/4 sensitivity of HESS (40/hr) with>1000x the exposure!
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
miniHAWC:
HAWC is a potentially large complex project.
Consider a another possibility, the relocation of the Milagro apparatusto an optimized pond located at a high altitude site.
Milagro owns ~900 8” Hamamatsu PMTs and a DAQ capable of 2000Hz readout.
--> Single layer consisting of a 29x29 Grid of PMTs with 5m separation (150mx150m pond) and 4m depth.
--> Utilize same reconstruction and /hadron separation methods as HAWC.
--> Simulation altitude 4500m.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Summary:
Current EAS arrays are not detecting/utilizing the “whole” shower. Huge improvements in /hadron separation possible.
Excellent angular resolution possible.
miniHAWC/HAWC could survey the entire northern or southern skyto a sensitivity of ~60mCrab/10mCrab. (conservative estimates)
Limiting detector to a single layer doesn't seem to reduce sensitivity. Could reduce cost of HAWC instrumentation by factor of ~2-3
Wide field of view and high duty cycle:SurveysPrompt VHE GRB emission?AGN monitor.Ideal for study of diffuse/extended sources.???
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
The Diffuse Galactic Plane in miniHAWC and HAWC
Use Neutral H map to trace out VHE Gamma-Ray flux. Normalize to Milagroobserved TeV diffuse emission from the Galactic plane.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
Conclusions
• Milagro and other air-shower arrays play an important and complementary roll in VHE astronomy.– Survey
– GRBs
– Extended/Diffuse Sources
– Monitoring Variable Sources
– Solar Activity Monitoring
– Water Cherenkov Method has not been exploited efficently
– Design improbments (Size, Altitude, …) lead to much better than sqrt(N) sensitivity improvents.
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
October 20-21, 2005 “Towards the Future” Workshop Andrew Smith
1) Size: – 150m x 150m = 22,500 m**2
2) Efficiency: Water acts a both conversion medium and radiator (Cherenkov) ~1 PE/40 MeV
3) Calorimetry: Deep (~15Xo) PMT layer for Muon/Hadron rejection.
4) Altitude: Select an optimal site.