sharper fermi -lat images
DESCRIPTION
Sharper Fermi -LAT Images. Stephen K N Portillo , Harvard University with Douglas P Finkbeiner 26 June 2014 Astroparticle Physics ( TeVPA /IDM), Amsterdam. Portillo & Finkbeiner , 1406.0507 submitted to ApJ. Angular Resolution Matters. Signal Region. Galactic Plane Leakage. - PowerPoint PPT PresentationTRANSCRIPT
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Stephen K N PORTILLO, Harvard Universitywith Douglas P FINKBEINER26 June 2014Astroparticle Physics (TeVPA/IDM), Amsterdam
Sharper Fermi-LAT Images
Portillo & Finkbeiner, 1406.0507submitted to ApJ
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Signal Region
Galactic Plane Leakage
Angular Resolution Matters
Galactic Plane (bright and hard to model!)
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Point Spread Function
tungstensilicon
Multiple Coulomb scatteringin tungsten foils (low E)
Limited silicon stripposition resolution (high E)
Conversion insupport material
Hard scatteringMissed silicon hit
Track confusion
Idea
l Eve
ntUni
deal
Eve
nt
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FRONT BACK
[TRANSIENT]
SOURCE
CLEAN
ULTRACLEAN
Event Classes + CTBCORE
Q2
Q1
Dividing the front-converting events…
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Pulsars as Point Sources
- =
On-phase Off-phase Pulsar
(Bill Saxton, NRAO)
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PSF Fitting ULTRACLEAN: Allfront, Q2, Q1
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Effective Area
Surviving Fraction, CLEAN, Q2
×
Effective Area, CLEAN (m2)
(Fermi Science Support Centre)
1
0.22.5 4𝐥𝐨𝐠𝟏𝟎 (𝑬 /MeV )
𝐜𝐨𝐬𝜽
0.5
0
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Effective Area Error Estimate
±0.01
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0.3-0.5 GeV, CLEAN, Allfront
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0.3-0.5 GeV, CLEAN, Q2
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0.3-0.5 GeV, CLEAN, Allfront minus Q2
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Before CTBCORE cut
After CTBCORE cutBefore CTBCORE
After CTBCORE
Daylan et al. (2014), arXiv
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Conclusion
Galactic Plane Leakage
Galactic Plane- =
1
0.22.5 4𝐥𝐨𝐠𝟏𝟎 (𝑬 /MeV )
𝐜𝐨𝐬𝜽
0.5
0
Effective Area
Signal Region
Idea
l Eve
nt
Point-Spread Function
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Check out the maps + IRFs at
http://fermi.skymaps.info/