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MAGIC sensitivity for pulsed emission from  -ray pulsars

MAGIC sensitivity for pulsed emission from  -ray pulsars. R. de los Reyes & J.L. Contreras Universidad Complutense de Madrid (U.C.M.). Contents. -ray detection from pulsars Pulsar models MAGIC effective area Gammas ( 5-200 GeV) and protons. Effect of Earth’s magnetic field.

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MAGIC sensitivity for pulsed emission from  -ray pulsars

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  1. MAGIC sensitivity for pulsed emission from -ray pulsars R. de los Reyes & J.L. Contreras Universidad Complutense de Madrid (U.C.M.) 14th Int. School, Erice 2004

  2. Contents • -ray detection from pulsars • Pulsar models • MAGIC effective area • Gammas (5-200 GeV) and protons. • Effect of Earth’s magnetic field. • Sensitivity • Pulsar observation times • Conclusions 14th Int. School, Erice 2004

  3. -ray detection from pulsars Cherenkov telescopes (E>80 GeV): Crab unpulsed component  Crab nebula • EGRET (30MeV-30GeV): • 271 detected  sources • 168 unidentified. • 7 high-confidence pulsars. 14th Int. School, Erice 2004

  4. MAGIC Pulsar models • Pulsar γ spectra cutoffs. Two models: • Polar Cap: Ecutoff ~ 10 GeV • Outer gap: Ecutoff ~ 100 GeV. 14th Int. School, Erice 2004

  5. Gammas (5-200 GeV) MAGIC effective area 14th Int. School, Erice 2004

  6. S N S W N E S E N W Effect of Earth’s magnetic field • B @-ray observatory: • Bx, Bz = f(L, , h) • (-observatory longitude, latitude and altitude) 14th Int. School, Erice 2004

  7. B and gamma effective areas 14th Int. School, Erice 2004

  8. (Nel & de Jager, 1996) (Wiebel, PhD thesis, 1998) Sensitivity Gamma and proton fluxes (dN/dE): 14th Int. School, Erice 2004

  9. Observation times(5, Q=1) (b = 2) Crab (=2.08) PSR1951+32 (=1.74) 14th Int. School, Erice 2004

  10. Sensitivity with B 14th Int. School, Erice 2004

  11. Conclusions • MAGIC will cover part of the -spectrum of pulsars. • Large Aeff:possible discovery of new pulsars. • Observation of pulsed emission would discriminate between pulsed emission models in ’s. • B affects the sensitivity depending on the location and the energy threshold of the telescope  Location of new gamma observatories(Ethreshold lower). • At La Palma: important for primary gammas and electrons (>30 and E100 GeV), and negligible for protons  pulsars(tobs  20%). 14th Int. School, Erice 2004

  12. Quality factor improvement /hadron separation techniques Q  2.5 Q = 3 (Crab) Ona-Wilhelmi et al, (private communication) P known previously 14th Int. School, Erice 2004

  13. Lateral distributions: gammas 14th Int. School, Erice 2004

  14. Protons (30 GeV-30 TeV) Gammas (5-200 GeV) MAGIC effective area 14th Int. School, Erice 2004

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