GALPROP is a numerical model of particle propagation in the Galaxy which incorporates as much realistic astrophysical input as possible together with latest theoretical developments. The model is designed to perform cosmic-ray propagation calculations for nuclei, antiprotons, electrons and positrons, and computes diffuse γ-rays and synchrotron emission in the same framework.

• Registration ( Why register?) If you are or about to become a GALPROP user, we encourage you to register. By registering you will get notifications about the latest software updates, new releases, and bug fixes. You will also be able to participate in the forum.         • Latest public version         • Plotting routines (IDL, C++, ROOT)         • GALPROP archive         • Web - based user interface to GALPROP         • Motivation and Acknowledgements         • About cosmic-ray transport

GALPROP LATEST PUBLIC ROUTINES

•  Latest public version v50.1p (bugs fixed)
•  Data files (FITS-files to be placed in the FITS folder):
    gas maps (by Seth W. Digel)
    interstellar radiation field (T.A.Porter & A.W.Strong, astro-ph/0507119)
• Sample galdef-files (to be placed in the GALDEF folder):
    galdef_50p_599278 conventional model with constant X_co-factor
    galdef_50p_999726 plain diffusion model with constant X_co-factor
    ...other models will be added

•  Latest full GALPROP manual
•  For GALPROP compilation on a Mac, see a note by Pat Nolan
• The analytical solution of the transport equation for electrons, energy losses ~E², used to test GALPROP. See Bulanov & Dogiel (1974, eq.[8]) for details; a factor of 1/[2pi] in their solution is missing -perhaps an error


PLOTTING ROUTINES

• A c++ plotting routine for cosmic-ray species
• An IDL routine to plot gamma-ray spectra and profiles
• ROOT-based plotting package GALPLOT (to install GALPLOT, you will need slalib)
• EGRET data that were used in GALPROP publications (2000-2004): counts and exposure


GALPROP ARCHIVE

Previous GALPROP versions (including sample input galdef-files and FITS-files):
• v50p (tar.gz)
• v42.3p (tar.gz)
• v41p (tar.gz)
• Older data files separately (FITS-files to be placed in the FITS folder):
    gas maps and interstellar radiation field  


WEB-BASED USER INTERFACE TO GALPROP

While the full information from a GALPROP run is contained in the output FITS files, this may not be convenient for all users. To facilitate the access to our published models, we have developed a Web interface, supporting various formats. In the first step we make avalable spectra of all CR species (isotopes of H through Ni, antiprotons, electrons, positrons) in the solar neighbourhood as calculated in our published models. The interface includes a simple form in the Web browser while the output results are provided as computer readable tables and graphics files. For every posted model, a user may require any of the following:

◊ spectra of any particular isotope or arbitrary combination of isotopes or elements in the requested units and scale, ◊ isotopic ratios vs. energy, which may include arbitrary isotopes in numerator/denominator, ◊ isotopic distribution of an arbitrary element, ◊ relative elemental and isotopic abundances at arbitrary energy, ◊ and electron/positron spectra and their ratio.

Both interstellar and heliospheric (force-field modulated) values are provided. In the near future we are going to upgrade it to allow those values to be requested for any arbitrary point in the Galaxy, and to add the spectrum of diffuse γ - rays for any given sky region as calculated in GALPROP models.


MOTIVATION AND ACKNOWLEDGEMENTS

Studies and discoveries in cosmic-ray physics and generally in astrophysics provide a fertile ground for research in many areas of particle physics and cosmology, such as the search for dark matter, antimatter, new particles, and exotic physics, studies of the nucleosynthesis, origin of Galactic and extragalactic γ-ray diffuse emission, formation of the large scale structure of the universe, heliospheric modulation etc. In its turn, astrophysics of cosmic rays and γ-rays depends very much on the quality of the data and their proper interpretation. The accuracy of current cosmic-ray experiments such as Ulysses, Advanced Composition Explorer (ACE), the Voyagers, TIGER and especially near future missions such as GLAST, AMS, BESS-Polar, CREAM, Pamela, and possibly ACCESS, far exceeds the accuracy of the current propagation models, of which the "leaky-box" model has remained one of the main research tools for the last 50 years. These near-future missions are specifically designed to target dark matter signals in cosmic rays and diffuse γ-rays, search for antimatter, study the diffuse Galactic and extragalactic diffuse emission, and provide outstanding quality data on cosmic ray species in a wide energy range. Meanwhile, recent developments in astrophysics, such as detailed 3-dimensional maps of the Galactic gas distribution, detailed studies of composition of interstellar dust, grains, the Local Bubble, interstellar radiation and magnetic fields, and new classes of sources of cosmic rays, all have implications for the interpretation of data obtained from ballon-borne and space experiments. The same is true of accurate measurements of nuclear isotopic production cross sections and new particle data. Having all the latest results and theories easily accessible would be advantageous for the scientific community as well as for planning and setting the goals for new missions.

The GALPROP code is so far an effort of two individuals (Igor V. Moskalenko & Andrew W. Strong). Other people have contributed by providing the data sets (Seth W. Digel, Stepan G. Mashnik, Troy A. Porter, Olaf Reimer) or their own nuclear cross section codes (V. S. Barashenkov, A. Polanski, R. Silberberg, C. H. Tsao, W. R. Webber). We thank Irina V. Malkova for her help in designing and supporting this Web-site.

This GALPROP Web-site is supported by NASA through APRA "Laboratory Astrophysics" grant, by Stanford University, and by GALPROP project. This is a free service to the Astrophysical community. GALPROP source code and datasets can be freely copied, however, it is requested that in any subsequent use of this work be given appropriate acknowledgment.

Web-master:   Irina V. Malkova   imal@galprop.stanford.edu