Developing the Galactic diffuse emission model for the
GLAST Large Area Telescope
Igor V. Moskalenko∗,†, Andrew W. Strong∗∗, Seth W. Digel‡,† and Troy A. Porter§
∗Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305
†Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94309
∗∗Max-Plank-Institut für extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany
‡Stanford Linear Accelerator Center, 2575 Sand Hill Rd, Menlo Park, CA 94025
§Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, CA 95064
Abstract. Diffuse emission is produced in energetic cosmic ray (CR) interactions, mainly protons and electrons, with the
interstellar gas and radiation field and contains the information about particle spectra in distant regions of the Galaxy. It may
also contain information about exotic processes such as dark matter annihilation, black hole evaporation etc. A model of
the diffuse emission is important for determination of the source positions and spectra. Calculation of the Galactic diffuse
continuum γ-ray emission requires a model for CR propagation as the first step. Such a model is based on theory of particle
transport in the interstellar medium as well as on many kinds of data provided by different experiments in Astrophysics and
Particle and Nuclear Physics. Such data include: secondary particle and isotopic production cross sections, total interaction
nuclear cross sections and lifetimes of radioactive species, gas mass calibrations and gas distribution in the Galaxy (H2, H I,
H II), interstellar radiation field, CR source distribution and particle spectra at the sources, magnetic field, energy losses,
γ-ray and synchrotron production mechanisms, and many other issues. We are continuously improving the GALPROP model
and the code to keep up with a flow of new data. Improvement in any field may affect the Galactic diffuse continuum γ-ray
emission model used as a background model by the GLAST LAT instrument. Here we report about the latest improvements
of the GALPROP and the diffuse emission model.
Keywords: gamma rays, cosmic rays, diffuse background, interstellar medium, gamma ray telescope
PACS: 95.55.Ka, 95.85.Pw, 98.35.-a, 98.38.-j, 98.38.Cp, 98.58.Ay, 98.70.Sa, 98.70.Vc
DISCUSSION AND RESULTS
We give a very brief summary of GALPROP; for details we refer to the relevant papers [1]-[6] and a dedicated
website. The propagation equation is solved numerically on a spatial grid, either in 2D with cylindrical symmetry in
the Galaxy or in full 3D. The boundaries of the model in radius and height, and the grid spacing, are user-definable.
Parameters for all processes in the propagation equation can be controlled on input. The distribution of CR sources can
be freely chosen, typically to represent supernova remnants. Source spectral shape and isotopic composition (relative
to protons) are input parameters. Cross-sections are based on extensive compilations and parameterizations [7]. The
numerical solution is evolved forward in time until a steady-state is reached; a time-dependent solution is also an
option. Starting with the heaviest primary nucleus considered (e.g., 64Ni) the propagation solution is used to compute
the source term for its spallation products, which are then propagated in turn, and so on down to protons, secondary
electrons and positrons, and antiprotons. In this way secondaries, tertiaries, etc., are included. Primary electrons are
treated separately. The proton, helium, and electron spectra are normalized to data; all other isotopes are determined
by the source composition and propagation. γ-rays and synchrotron emission are computed using interstellar gas data
(for pion-decay and bremsstrahlung) and the interstellar radiation field (ISRF) model (for inverse Compton). The
computing resources required by GALPROP are moderate by current standards.
Recent extensions to GALPROP include
• new detailed calculation of the ISRF [8, 9]
• proper implementation of the anisotropic inverse Compton scattering using new ISRF (Figure 1, left)
• interstellar gas distributions based on current HI and CO surveys [10, 11]
• new parameterization of the π0 production in pp-collisions [12] which includes the diffraction dissociation
• non-linear MHD wave – particle interactions (wave damping) [6] are included as an option
• the kinetic energy range is now extended down to ∼1 keV
http://arxiv.org/abs/0704.1328v1
 0  10  20  30  40  50  60  70  80  90
Galactic latitude, degrees
intermediate latitudes
Eγ=2 GeV
anti-GC
l=180°
FIGURE 1. Left: The ratio of anisotropic IC to isotropic IC for Galactic longitudes l = 0◦ and 180◦ vs. Galactic latitude. Right:
γ-ray spectrum of inner Galaxy (330◦ < l < 30◦, |b| < 5◦) for an optimized model. Vertical bars: COMPTEL and EGRET data,
heavy solid line: total calculated flux. This is an update of the spectrum shown in [5].
• the γ-ray calculations extend from keV to tens of TeV (e.g., Figure 1, right), and produce full sky maps as a
function of energy; the output is in the FITS-format
• gas mass calibration (XCO-factors) which can vary with position
• a dark matter package to allow for propagation of the WIMP annihilation products and calculation of the
corresponding synchrotron and γ-ray skymaps
• GALPROP–DarkSUSY interface (together with T. Baltz) will become publicly available soon
• a dedicated website has been developed (http://galprop.stanford.edu)
The GALPROP code [1] was created with the following aims: (i) to enable simultaneous predictions of all relevant
observations including CR nuclei, electrons and positrons, γ-rays and synchrotron radiation, (ii) to overcome the
limitations of analytical and semi-analytical methods, taking advantage of advances in computing power, as CR, γ-
ray and other data become more accurate, (iii) to incorporate current information on Galactic structure and source
distributions, (iv) to provide a publicly-available code as a basis for further expansion. The first point is the most
important: all data relating to the same system, the Galaxy, must have an internal consistency. For example, one cannot
allow a model which fits secondary/primary ratios while not fitting γ-rays or not being compatible with the known
interstellar gas distribution. There are many simultaneous constraints, and to find one model satisfying all of them is a
challenge, which in fact has not been met up to now. Upcoming missions will benefit: GALPROP has been adopted as
the standard for diffuse Galactic γ-ray emission for NASA’s GLAST γ-ray observatory, and is also made use of by the
ACE, AMS, HEAT and Pamela collaborations.
IVM is supported in part by NASA APRA grant, TAP is supported in part by the US Department of Energy.
REFERENCES
1. A. W. Strong, and I. V. Moskalenko, ApJ 509, 212–228 (1998).
2. I. V. Moskalenko, and A. W. Strong, ApJ 493, 694–707 (1998).
3. A. W. Strong, I. V. Moskalenko, and O. Reimer, ApJ 537, 763–784 (2000).
4. I. V. Moskalenko, A. W. Strong, J. F. Ormes, and M. S. Potgieter, ApJ 565, 280–296 (2002).
5. A. W. Strong, I. V. Moskalenko, and O. Reimer, ApJ 613, 962–976 (2004).
6. V. S. Ptuskin et al, ApJ 642, 902–916 (2006).
7. S. G. Mashnik et al., Adv. Space Res. 34, 1288–1296 (2004).
8. I. V. Moskalenko, T. A. Porter, and A. W. Strong, ApJ 640, L155–L158 (2006).
9. T. A. Porter, A. W. Strong, and S. W. Digel, in preparation (2007).
10. P. M. W. Kalberla et al., Astron. Astrophys. 440, 775–782 (2005).
11. T. M. Dame, D. Hartmann, and P. Thaddeus, ApJ 547, 792–813 (2001).
12. T. Kamae et al., ApJ 647, 692–708 (2006).
http://galprop.stanford.edu
	Discussion and Results

  Diffuse emission is produced in energetic cosmic ray (CR) interactions,
mainly protons and electrons, with the interstellar gas and radiation field and
contains the information about particle spectra in distant regions of the
Galaxy. It may also contain information about exotic processes such as dark
matter annihilation, black hole evaporation etc. A model of the diffuse
emission is important for determination of the source positions and spectra.
Calculation of the Galactic diffuse continuum gamma-ray emission requires a
model for CR propagation as the first step. Such a model is based on theory of
particle transport in the interstellar medium as well as on many kinds of data
provided by different experiments in Astrophysics and Particle and Nuclear
Physics. Such data include: secondary particle and isotopic production cross
sections, total interaction nuclear cross sections and lifetimes of radioactive
species, gas mass calibrations and gas distribution in the Galaxy (H_2, H I, H
II), interstellar radiation field, CR source distribution and particle spectra
at the sources, magnetic field, energy losses, gamma-ray and synchrotron
production mechanisms, and many other issues. We are continuously improving the
GALPROP model and the code to keep up with a flow of new data. Improvement in
any field may affect the Galactic diffuse continuum gamma-ray emission model
used as a background model by the GLAST LAT instrument. Here we report about
the latest improvements of the GALPROP and the diffuse emission model.

Developing the Galactic diffuse emission model for the
GLAST Large Area Telescope
Igor V. Moskalenko∗,†, Andrew W. Strong∗∗, Seth W. Digel‡,† and Troy A. Porter§
∗Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305
†Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94309
∗∗Max-Plank-Institut für extraterrestrische Physik, Postfach 1312, D-85741 Garching, Germany
‡Stanford Linear Accelerator Center, 2575 Sand Hill Rd, Menlo Park, CA 94025
§Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, CA 95064
Abstract. Diffuse emission is produced in energetic cosmic ray (CR) interactions, mainly protons and electrons, with the
interstellar gas and radiation field and contains the information about particle spectra in distant regions of the Galaxy. It may
also contain information about exotic processes such as dark matter annihilation, black hole evaporation etc. A model of
the diffuse emission is important for determination of the source positions and spectra. Calculation of the Galactic diffuse
continuum γ-ray emission requires a model for CR propagation as the first step. Such a model is based on theory of particle
transport in the interstellar medium as well as on many kinds of data provided by different experiments in Astrophysics and
Particle and Nuclear Physics. Such data include: secondary particle and isotopic production cross sections, total interaction
nuclear cross sections and lifetimes of radioactive species, gas mass calibrations and gas distribution in the Galaxy (H2, H I,
H II), interstellar radiation field, CR source distribution and particle spectra at the sources, magnetic field, energy losses,
γ-ray and synchrotron production mechanisms, and many other issues. We are continuously improving the GALPROP model
and the code to keep up with a flow of new data. Improvement in any field may affect the Galactic diffuse continuum γ-ray
emission model used as a background model by the GLAST LAT instrument. Here we report about the latest improvements
of the GALPROP and the diffuse emission model.
Keywords: gamma rays, cosmic rays, diffuse background, interstellar medium, gamma ray telescope
PACS: 95.55.Ka, 95.85.Pw, 98.35.-a, 98.38.-j, 98.38.Cp, 98.58.Ay, 98.70.Sa, 98.70.Vc
DISCUSSION AND RESULTS
We give a very brief summary of GALPROP; for details we refer to the relevant papers [1]-[6] and a dedicated
website. The propagation equation is solved numerically on a spatial grid, either in 2D with cylindrical symmetry in
the Galaxy or in full 3D. The boundaries of the model in radius and height, and the grid spacing, are user-definable.
Parameters for all processes in the propagation equation can be controlled on input. The distribution of CR sources can
be freely chosen, typically to represent supernova remnants. Source spectral shape and isotopic composition (relative
to protons) are input parameters. Cross-sections are based on extensive compilations and parameterizations [7]. The
numerical solution is evolved forward in time until a steady-state is reached; a time-dependent solution is also an
option. Starting with the heaviest primary nucleus considered (e.g., 64Ni) the propagation solution is used to compute
the source term for its spallation products, which are then propagated in turn, and so on down to protons, secondary
electrons and positrons, and antiprotons. In this way secondaries, tertiaries, etc., are included. Primary electrons are
treated separately. The proton, helium, and electron spectra are normalized to data; all other isotopes are determined
by the source composition and propagation. γ-rays and synchrotron emission are computed using interstellar gas data
(for pion-decay and bremsstrahlung) and the interstellar radiation field (ISRF) model (for inverse Compton). The
computing resources required by GALPROP are moderate by current standards.
Recent extensions to GALPROP include
• new detailed calculation of the ISRF [8, 9]
• proper implementation of the anisotropic inverse Compton scattering using new ISRF (Figure 1, left)
• interstellar gas distributions based on current HI and CO surveys [10, 11]
• new parameterization of the π0 production in pp-collisions [12] which includes the diffraction dissociation
• non-linear MHD wave – particle interactions (wave damping) [6] are included as an option
• the kinetic energy range is now extended down to ∼1 keV
http://arxiv.org/abs/0704.1328v1
 0  10  20  30  40  50  60  70  80  90
Galactic latitude, degrees
intermediate latitudes
Eγ=2 GeV
anti-GC
l=180°
FIGURE 1. Left: The ratio of anisotropic IC to isotropic IC for Galactic longitudes l = 0◦ and 180◦ vs. Galactic latitude. Right:
γ-ray spectrum of inner Galaxy (330◦ < l < 30◦, |b| < 5◦) for an optimized model. Vertical bars: COMPTEL and EGRET data,
heavy solid line: total calculated flux. This is an update of the spectrum shown in [5].
• the γ-ray calculations extend from keV to tens of TeV (e.g., Figure 1, right), and produce full sky maps as a
function of energy; the output is in the FITS-format
• gas mass calibration (XCO-factors) which can vary with position
• a dark matter package to allow for propagation of the WIMP annihilation products and calculation of the
corresponding synchrotron and γ-ray skymaps
• GALPROP–DarkSUSY interface (together with T. Baltz) will become publicly available soon
• a dedicated website has been developed (http://galprop.stanford.edu)
The GALPROP code [1] was created with the following aims: (i) to enable simultaneous predictions of all relevant
observations including CR nuclei, electrons and positrons, γ-rays and synchrotron radiation, (ii) to overcome the
limitations of analytical and semi-analytical methods, taking advantage of advances in computing power, as CR, γ-
ray and other data become more accurate, (iii) to incorporate current information on Galactic structure and source
distributions, (iv) to provide a publicly-available code as a basis for further expansion. The first point is the most
important: all data relating to the same system, the Galaxy, must have an internal consistency. For example, one cannot
allow a model which fits secondary/primary ratios while not fitting γ-rays or not being compatible with the known
interstellar gas distribution. There are many simultaneous constraints, and to find one model satisfying all of them is a
challenge, which in fact has not been met up to now. Upcoming missions will benefit: GALPROP has been adopted as
the standard for diffuse Galactic γ-ray emission for NASA’s GLAST γ-ray observatory, and is also made use of by the
ACE, AMS, HEAT and Pamela collaborations.
IVM is supported in part by NASA APRA grant, TAP is supported in part by the US Department of Energy.
REFERENCES
1. A. W. Strong, and I. V. Moskalenko, ApJ 509, 212–228 (1998).
2. I. V. Moskalenko, and A. W. Strong, ApJ 493, 694–707 (1998).
3. A. W. Strong, I. V. Moskalenko, and O. Reimer, ApJ 537, 763–784 (2000).
4. I. V. Moskalenko, A. W. Strong, J. F. Ormes, and M. S. Potgieter, ApJ 565, 280–296 (2002).
5. A. W. Strong, I. V. Moskalenko, and O. Reimer, ApJ 613, 962–976 (2004).
6. V. S. Ptuskin et al, ApJ 642, 902–916 (2006).
7. S. G. Mashnik et al., Adv. Space Res. 34, 1288–1296 (2004).
8. I. V. Moskalenko, T. A. Porter, and A. W. Strong, ApJ 640, L155–L158 (2006).
9. T. A. Porter, A. W. Strong, and S. W. Digel, in preparation (2007).
10. P. M. W. Kalberla et al., Astron. Astrophys. 440, 775–782 (2005).
11. T. M. Dame, D. Hartmann, and P. Thaddeus, ApJ 547, 792–813 (2001).
12. T. Kamae et al., ApJ 647, 692–708 (2006).
http://galprop.stanford.edu
	Discussion and Results
