Distributions of Fitted Values vs Input Values and

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Estimated Errors.

The true parameters are taken (or inferred) from the 3EG catalog assuming a power-law spectrum. See the description of the default parameteriztion parameterization in the Likelihood tutoialtutorial).

Error estimates for any single fit are given by taking the square root of the diagonal elements of the covariance matrix, which in turn is estimated as the inverse Hessian of the -log-likelihood. Note that the definition of the confidence interval corresponds to a specified change in the log-likelihood along a given direction in parameter space. The estimates obtained from the inverse Hessian are only accurate insofar as the likelihood surface at the local minimum can be accurately represented as a quadratic function of the model parameters. The error estimates reported below are averaged over each set of Monte Carlo trials.

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Counts maps for the Crab_Pulsar, the hree three anticenter sources, and extragalactic diffuse tests are prepared for the following geometry:
E _min = 30, E _max = 3e5 MeV, 39 bins, logrithmically spaced
RA _center = 83 ^o, eighty 0.5 ^o pixels
Dec _center = 22 ^o, eighty 0.5 ^o pixels

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Three strong sources in the Galactic anticenter region.

• PKS0528+134
  

  Prefactor		Index
  true +/- est.	MC	true +/- est.	MC
  13.65 +/- 1.62	14.35 +/- 1.68	-2.46 +/- 0.10	-2.54 +/- 0.10

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• Crab
  

  Prefactor		Index
  true +/- est.	MC	true +/- est.	MC
  27.00 +/- 2.04	26.82 +/- 2.08	-2.19 +/- 0.06	-2.15 +/- 0.06

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• Geminga
  

  Prefactor		Index
  true +/- est.	MC	true +/- est.	MC
  23.29 +/- 1.65	23.61 +/- 1.73	-1.66 +/- 0.03	-1.66 +/- 0.04

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