Download - Status of km3 check
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Status of km3 check
ANTARES MC WG, Tue 12th Jun 2012
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Km3 Progression: a reminder…• rbr v0.1: used km3 v3r7
– Treated direct photons from electrons as being emitted at the Cherenkov angle• Km3 v3r9:
– fixed ‘single-band issue’• direct photons from electrons treated as scattered photons.• Fix acts to reduce event rate (less ‘on-cone’ hits)
– Fixed ‘energy-loss mismatch’ between gen and km3• Previously, e-loss between 0.3 and 0.72 GeV was discarded• Fix acts to increase the event rate (more eloss in km3)
– v3r10: only cosmetic changes• Km3 v4
– Added chromatic dispersion (no obvious net effect expected)– V4r0 v4r1: buggy. Use v4r2
• rbr v2:– Modify hit v4r2 to use the new angular efficiency via aa.txt and aa.f
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Behaviour v3r7-v4r2• Step 1: Use toy experiments to assess behaviour
– Run 3x106 toy events per trial• B1: 1 TeV muon, 25m PMT distance, pointing away• B2: 1 TeV muon, 25m PMT distance, pointing towards• B3: 1 TeV muon, 50m PMT distance, pointing away• B4: 1 TeV muon, 50m PMT distance, pointing towards
– This analysis is complete as of 11:30 am today• Step 2: Use rbr runs
– use exactly the same MUPAGE/GENHEN events (only km3 and TE randomness applies).
– Use 10 runs: 34433, 35360, 35750, 36430, 37230, 37340, 53240, 53450, 53620, 54250.
– Analysis incomplete: 50% computation finished + need to decide how to characterise output
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What I did exactly…• v3r7, v3r9, v4r2:
– Check out clean copy and make executables– Build gen & hit tables and run km3 w. standard options– v3rX have ¼ statistics of v4rY (smaller internal arrays)– Gen rad file: gen-water-radii-5-20s-partic-0.0075.dat
• v4r2 rbr:– Tables from /sps/km3net/mc/rbr/v2/prod_inputs/km3tables/
– Use clean co-ed and built km3mc v4r2– May have used a different gen radii file!
• Ran many events on the cluster and got… results!
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B2 (1 TeV, 25 m, facing towards)
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B4 (1 TeV, 50 m, facing towards)
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B1 (1 TeV, 25 m, facing away)
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B3 (1 TeV, 50 m, facing away)
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B2 (1 TeV, 25 m, facing towards)
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B4 (1 TeV, 50 m, facing towards)
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B1 (1 TeV, 25 m, facing away)
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B3 (1 TeV, 50 m, facing away)
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What can we conclude from this?• Not as much as we might expect!– Effect in slides 9-12 due to chromatic dispersion (c-d)(main
diff between v3 and v4 plots)– c-d acts to delay the peak– Of course we then have less photons after a certain time!
• But…– Both v4r2 for cases B1 and B3 (facing away) have definitely
lower cumulative distributions than v3rX– Could this be the source of the reduced counts?
• Q: What is the effect on rbr simulations?• A: Still to find out…
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OK, onto the future…• v4r3:– Minimum effang of 10-6 (solves 2nd early-photon problem)– New theta-binning (BELO/BEHI of 0.45) (‘v4r3 pure’)
• Solves early-photon problem• Effect on total photon number: increases it! (no hard reason)
– Added seawater to gen (expect ~4% fewer photons) (‘v4r3 sea’)• v4r4– Wavelength-dependent ‘eta’ (fraction of Rayleigh) (‘v4r4 MR’)– New hit method to input and sample PMT parameters:
implement new effective angle calculation (‘v4r4 new effang’)
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B2 (1 TeV, 25 m, facing towards)
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B4 (1 TeV, 50 m, facing towards)
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B1 (1 TeV, 25 m, facing away)
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B3 (1 TeV, 50 m, facing away)
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B2 (1 TeV, 25 m, facing towards)
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B4 (1 TeV, 50 m, facing towards)
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B1 (1 TeV, 25 m, facing away)
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B3 (1 TeV, 50 m, facing away)
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Conclusion on recent updates• Changes v4r2-v4r3: BELO/BEHI most important• All other changes minsmall
• Effect of new angular efficiency:– v4r2 vs rbr_v4r2 (slides 9-12, blue vs pink)
• slightly reduced number of hits for PMTs facing towards a track• Increased number of hits for PMTs facing away from the track
– v4r4 vs v4r4_new effang (slides 19-22, light blue vs yellow)• Reduced number of hits for PMTs facing towards a track• Increased number of hits for PMTs facing away from the track
– This is inconsistant!
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Effang plot
Difference can not be due to different implementations of the effective angle!
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Further check…
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Possible explanation?– When compiling km3 with the function ‘getaa’, I had to
remove all binaries and recompile from scratch to avoid insanity.
– There is no known reason for this behaviour: could be f77 or make problem.
– Perhaps something strange gets introduced here?
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Where commeth the wobbles?
• Scattered photons from muons!
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Why?• Speed up in km3: merge muon track segments at large
distances for scattered photons– Tracks: intrinsically 1m– Merging: x3, x9, and x27 at comparable distances– Merging is too coarse!
• Solution: – multiply all merging distances by a factor– Implementation: allow FFKEY ‘DIVTK [float]’ to km3
• Test: use DIVTK 2. in B4
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Problem solved
• DIVTK=2 seems to work!