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Sharper Fermi -LAT Images

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.

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Sharper Fermi -LAT Images

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  1. Sharper Fermi-LAT Images Stephen K N Portillo, Harvard Universitywith Douglas P Finkbeiner26 June 2014AstroparticlePhysics (TeVPA/IDM), Amsterdam Portillo & Finkbeiner, 1406.0507submitted to ApJ

  2. Angular Resolution Matters Signal Region Galactic Plane Leakage (bright and hard to model!) Galactic Plane

  3. Point Spread Function Conversion insupport material Multiple Coulomb scatteringin tungsten foils (low E) tungsten Unideal Event silicon Ideal Event Missed silicon hit Hard scattering Limited silicon stripposition resolution (high E) Track confusion

  4. Event Classes + CTBCORE FRONT BACK Dividing the front-converting events… Q2 Q1

  5. Pulsars as Point Sources - = Off-phase On-phase Pulsar (Bill Saxton, NRAO)

  6. PSF Fitting ULTRACLEAN: Allfront, Q2, Q1

  7. Effective Area 1 Surviving Fraction, CLEAN, Q2 Effective Area, CLEAN (m2) 0.5 0.2 2.5 4 0 (Fermi Science Support Centre)

  8. Effective Area Error Estimate

  9. 0.3-0.5 GeV, CLEAN, Allfront

  10. 0.3-0.5 GeV, CLEAN, Q2

  11. 0.3-0.5 GeV, CLEAN, Allfront minus Q2

  12. Before CTBCORE cut After CTBCORE cut Before CTBCORE After CTBCORE Daylanet al. (2014), arXiv

  13. Conclusion Point-Spread Function Signal Region 1 Galactic Plane Leakage - = 0.5 Galactic Plane Effective Area 0.2 2.5 4 0 Ideal Event

  14. Check out the maps + IRFs athttp://fermi.skymaps.info/

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