Nebraska’s Statewide Outreach and Education Experiment
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Transcript of Nebraska’s Statewide Outreach and Education Experiment
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Nebraska’s Statewide Outreach and Education Experiment
The Cosmic Ray Observatory Project
Dan ClaesUniversity of Nebraska-Lincoln
Washington Area Large Time-coincidence Array
SALTA Schoolsand the
Henderson Mine ProjectThursday, October 14, 2004
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CROP article in Lincoln Journal Star, 7 August 2003
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The Chicago Air Shower ArrayThe Chicago Air Shower Array
•Located in the Utah Desert•1089 stations, 15m spacing•covering 0.23 square km
each houses 4 scintillators w/tubes1 high and 1 low voltage supply
CROP/ WALTA/ SALTA recycle detectors from the Chicago Air Shower Array
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U.S. Army PhotoSeptember 30,
1999
The CROP team at Chicago Air Shower Array (CASA) site
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CASA detectors’ new home at the University of Nebraska
2000 scintillator panels, 2000 PMTs, 500 low and power supplies at UNL
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PMMA (polymethyl methacrylate)doped with a scintillating fluor
Read out by 10 stage
EMI 9256 photomultiplier tube
Recycling material inherited from The Chicago Air Shower Array
2 ft x 2 ft x ½ inch
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•EMI Photomultiplier tubes are working
•Typical efficiency of counters 85% - 95%
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CROP Workshops
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Oscilloscope
training
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Tearingthe oldCASA
counters apart
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Scraping, sanding and polishing
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Wrapping & light-tighting
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Electronics lessons
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• LabView (PC)
• At-a-glance monitoring of incoming data
•Graham Wheel (UWash) Jared Kite (UNL)
Monitoring Program for Data Acquisition Card
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Cosmic Ray Observatory Project
Collecting Data with CROP DAQ Card Interface
Doing an Efficiency Scan
1. Disconnect the 4 signal cables from the DAQ card. These are the cables that connect to your 4 detectors.2. Open the CROP_DAQ LabVIEW Program.
3. Click on the "Efficiency" tab make sure the Efficiency Scan button is ON(lit up).
4. Click on the "Threshold Scan" tab make sure the Threshold Scan button is OFF.
5. Click on the "Data Collection Settings" tab and set the timer ON (green button lit up).
6. Click on the "Data Acquisition" tab and to begin run click on (upper left corner under the Edit menu).
http://crop.unl.edu/tutorials/Online help and tutorials available.
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On-Line Oscilloscope Cheat Sheets
http://unlhep2.unl.edu/~CROP/oscihomepage.html
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April 2001 participant meeting at UNL
Marian High Schoolstudents presenting
results and discussingcosmic rays withProf. Jim Cronin,
University of Chicago
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Barometric Pressure (mmHg)
727 747
4-F
old
Coi
nci
den
ces
/ 2 h
ours
3000
4200
• Statistical error bars shown• 1.3% decrease per mmHg
Marian High School’s Measurement of Cosmic Ray Rate vs. Barometric Pressure
http://marian.creighton.edu/~besser/physics/barometer.html
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Mount Michael Benedictine High School
“The Science Teacher”, November 2001
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The Washington-Area Large-ScaleTime-Coincidence Array
http://www.phys.washington.edu/~waltahttp://www.phys.washington.edu/~walta
Seattle area map showing schools
• CROP’s closest relative
• University of Washington, Seattle Jeff Wilkes, et al.
• also using refurbished CASA detectors
• WALTA/CROP/FNAL collaboration developing DAQ PC electronics card
• Funding limited, but used QuarkNet association to fund 1st WALTA workshop, August 2001
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WALTA/QuarkNet One-week Summer Workshop
University of WashingtonAugust 2001
Seattle teachers and WALTA staff Refurbishing CASA scintillators
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• Aspen High School, Aspen, CO
• Basalt High School, Basalt, CO
• Roaring Fork Valley High School, Carbondale, CO
• Lake County High School, Leadville, CO The highest-elevation school in U.S. -- 10,152 feet above sea level
SALTA: Snowmass Area Large Time-Coincidence Array
Empire
• Clear Creek High School, Empire, CO
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Leadville1
10 miles
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Polishing scintillatoredges outside
Conference Center
Making detectors light-tight
SALTA Workshop, July 2001, Snowmass, CO
massphototube
gluing
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Henderson Mine Visit
Dec 4, 2003hosted by
Chip deWolfe
Marc Whitley Diana Kruis Nancy Spletzer Aspen High School Basalt High School Clear Creek High School
Michelle Ernzen Laura FrenchLake County School Roaring Fork Valley
Hans-Gerd BernsUniversity of Washington
Dan ClaesUniversity of Nebraska
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Scouted 3 possible locationsbetween 2800-3900 ft depths
110 power available
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•Can't survey the proposed site, but plan to use spots away from glory hole (where blasting still common & overhead rock broken up) •Topological graphs and CAD tools can provide good estimates of overburden at survey-able spots.
4 sites have been identified ranging from 3000 – 4000 overburden
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January 13-15 – Claes visits the SALTA schools to check out condition of detectors and meet with students
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Cosmic Ray Scintillator TestingThreshold Testing Results
Online exponential fit program: http://cms.dt.uh.edu/Faculty/BecerraL/ExpFit.htm
Results posted by students from Basalt High School
Threshold(mv) Hits per minute
20 263885
30 220347
40 133871
50 94560
60 54108
70 66733
80 31927
90 25696
100 8011
Scintillator Two
f(x) = 480410.6452 (.9682754831^x)Coefficient of correlation: .9488743319
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A Threshold ScanRather than focussing on a single fit to the entire range of data, recognize that two different physics processes are at play. Both generate counts, but with rates that drop off differently with increasing threshold.(Both drop ~exponentially, which is why we use a logarithmic plot).
At LOW THRESHOLD we expect to be dominated by noise, which plummets rapidly with threshold. Its exponential drop should ideally look like a straight line on a logarithmic plot. At HIGH THRESHOLD the background noise should be pretty much eliminated, and any additional increase in threshold will actually start cutting into the real signal. Real signals are, on average, larger, so the drop is less severe.
This defines two regions with relatively flat (linear) response. Because of the statistical fluctuates common in random events like noise or cosmic ray counts, how straight the lines are may depend on how long you ran at each data point (at least 10-15 minutes should be OK). Of course the two regions overlap, so there's a middle region that curves. But we can focus on the first few…
points at each extreme to determine our linear fits, as I have done (by eye) above. We use the intersection of the two lines to select the threshold (which looks to be about 65 mV in the example above to me).
It's a nice to try and confirm your selection by eye. Recall you can set trigger threshold on the oscilloscope. A very low threshold will have the oscilloscope almost continuously triggering, revealing a band of noise (see above). Moving the threshold just far enough to kill the noise and give only the flickering images of healthy signals can give you an approximate idea of where the threshold should be set. See if you can confirm this sort of behavior for the setting your scans suggest you use.
Recall the DAQ card has a built-in x2 amplifier, so uses thresholds twice the size of the ones you'll need for the oscilloscope trigger (i.e., a threshold of 65mV from the DAQcard scan corresponds to a 32mV trigger threshold on the oscilloscope).
Example of follow-up discussion posted in response:
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Aspen Center for Physics July, 2004: Back for MORE!
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Aspen Center for Physics Education & Outreach WorkshopJuly 6-8 SALTA schools take over the library, setting up cosmic ray telescopes, for training in the new DAQcard
that will be used in all their data-taking.
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¼ in lead
Detectors•telescoped pair with coincidence requirement against noise•sandwiched with lead sheet
have been reconfigured into muon telescopes
•At mining level (3000 mwe) the rate for any single (2 ft 2 ft) panel will be low
•We take two such modules down into the mine
•May need week(s) long runs
We are moving the detectors at 2-3 week intervals
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with dust a problem for a PCwe house a low-power serial digital data logger
A portable stand holds each muon telescopes.
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Desktop Base StationAn ~identical pair of modules are running in a fixedlocation (surface office) to establish our baseline
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where dust may be a problem for a PC
we house the low-power serial digital data loggeralongside the DAQcard
thanks to Hans Berns’ initial testing withAcumen Instruments Databridge
development kit
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SALTA’s Henderson Project is launched September 29, 2004
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Clear CreekHigh School
studentsset up thesatellitemodules
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1st undergroundrun started
2:12pm9/28/04
8100Electrical
Shop
Clear CreekHigh School
instructorNancy Spletzer
does the Honors
Punching the RUN
button
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The future
At the conclusion of Henderson measurements• revive the original cosmic ray grid plans for SALTA
• work with schools to plug into CROP-WALTA
• recruit neighboring schools to expand the grid
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Wherever/whenever the UNO facility is built
I hope to see monitors at the lab entrance (and/or Visitor’s Center) featuring the high school report, so
again local schools can feel they are making a contribution to the experiment.
At the same time, their data will be part of the CROP-WALTA network.
a cosmic ray grid on area schoolswill continuously monitor
the local cosmic "weather"reporting it as close to live
as we can to the lab.