The input file items are: Statistics -- number of photons used in the Monte Carlo simulation, for a good spectrum we recommend 10⁶. The unresolved component is due to unresolved gamma ray lines in heavy nuclei; 0 includes this component and 1 excludes it; use 0 for the total spectrum (narrow and broad lines); if you want to see just the narrow lines, you must zero out the accelerated particle abundances of C and heavier nuclei and set the unresolved component parameter to 1. Lines from long term radioactive nuclei (e.g. 0.847 MeV from ⁵⁶Co produced by a p,n reaction on ⁵⁶Fe) are excluded with 1 and included with 0. PL-index gives the spectral index of the accelerated particle spectrum which is a power law in kinetic energy per nucleon down to a low energy cutoff (le cutoff) below which the spectrum is constant. Thin/thick of 1 or 2 is thin or thick target respectively; for both the thin and thick target models the accelerated particles are assumed isotropic in the interaction region. For the thick target the ambient medium is assumed to be neutral. The charge state of the ambient medium does not have a role in the thin target because the particles do not lose energy. The ambient abundances are normalized to H. The accelerated particle abundances are normalized to the protons, with all species having the given abundances at the same energy per nucleon. For both the ambient medium and the accelerated particles for each element the abundance should include all the isotopes of that species. The power law, including the cutoff, is normalized to 1 proton of energy greater than 30 MeV.

The output is in g.spc. The 3 columns are photon energy in MeV, bin width in MeV, and photon production spectrum at the source. The photon energy is given at bin center. The code eint.for will integrate the spectrum over any given photon energy range. For the thick target the spectrum is in photons MeV^-1 and it represents the total gamma ray production for 1 proton greater than 30 MeV. For the thin target the spectrum is in photons MeV^-1 cm³ sec^-1 and it represents the instantaneous production in an ambient medium of unit H density by accelerated particles normalized to 1 proton greater than 30 MeV. The postscript file figure shows the spectrum calculated with gthick.inp with 5x10⁶ photons.

Credit for use of this code should be given to R. Ramaty, R.J. Murphy and B. Kozlovsky, mentioning the WEB page from where the downloading was done. The code is based on the paper by R. Ramaty, B. Kozlovsky and R. E. Lingenfelter, 1979, ApJ (Suppl.), 40, 487 with substantial updates (Kozlovsky, Murphy and Ramaty, 2001, in preparation).

To view postscript (.ps) files
obtain GhostScript & GSview here.