1. GALPROP tutorial Igor Moskalenko (Stanford U.)

2. Igor V. Moskalenko 2 November 17, 2005GALPROP manual/Rome2, Italy Obtaining GALPROP The link: http://www.mpe.mpg.de/~aws/dlp/zxc/kty/v42.3p/ Contains c++, fortran routines & input files (dat-files, compass gas maps, and isrf) Dedicated GALPROP Web-site will go online soon! –Controlled changes in GALPROP: tests + documentation +… –New version(s) + archive versions –Post relevant information: best models, gas maps, ISRF, nuclear cross sections… –Allow for communication with users –Ability to run GALPROP on-line…

3. Igor V. Moskalenko 3 November 17, 2005GALPROP manual/Rome2, Italy I/O galdef-file gas: COR, HIR, IAQ-files RFComposite –(fits) file dat-files (xsec, nuc.network) GALPROP (c++ & fortran) nuclei –(fits) file (R=Rsun) nuclei_full –(fits) file (whole galaxy) γ-ray emissivities –(fits) files (brems, IC, π 0 ) γ-ray skymaps –(fits) files (rings; brems, IC, π 0 ) FITS GALDEF v42.3 FITS same level dirs Heliospheric modulation: on-the-fly in a plotting routine

4. Igor V. Moskalenko 4 November 17, 2005GALPROP manual/Rome2, Italy Example Makefile #CXX = g++-2.95 #FC = g77-2.95 CFITSIO = ${GLAST_EXT}/cfitsio/v2470 CPPFLAGS = -O3 -Wno-deprecated -I${CFITSIO}/include FFLAGS = LIBS = -lm -lg2c FITSLIB = -L$(CFITSIO)/lib -lcfitsio -Wl, rpath,$(CFITSIO)/lib LDFLAGS = $(FITSLIB) $(LIBS) FOBJS := $(patsubst %.f,%.o,$(wildcard *.f)) CCOBJS := $(patsubst %.cc,%.o,$(wildcard *.cc)) galprop: ${FOBJS} ${CCOBJS} $(CXX) *.o -o $@ ${LDFLAGS}

5. Igor V. Moskalenko 5 November 17, 2005GALPROP manual/Rome2, Italy Some Editing Tested for g++ v2.9x compiler. New g++ compiler v3.x is more strict –routines require some editing: using namespace std; #include

6. Igor V. Moskalenko 6 November 17, 2005GALPROP manual/Rome2, Italy GALPROP Input: galdef-files GALPROP is parameter-driven (user can specify everything!) Grids 2D/3D –options; symmetry options (full 3D, 1/8 -quadrants) Spatial, energy/momentum, latitude & longitude grids Ranges: energy, R, x, y, z, latitude & longitude Time steps Propagation parameters D xx, V A, V C & injection spectra (p,e) X-factors (including R-dependence) Sources Parameterized distributions Known SNRs Random SNRs (with given/random spectra), time dependent eq. Other Source isotopic abundances, secondary particles (pbar, e ±, γ, synchro), anisotropic IC, energy losses, nuclear production cross sections…

7. Igor V. Moskalenko 7 November 17, 2005GALPROP manual/Rome2, Italy Algorithm primary source functions (p, He, C.... Ni) source abundances, spectra primary propagation -starting from maxA=64 source functions (Be, B...., e +,e -, pbars) using primaries and gas distributions secondary propagation tertiary source functions tertiary propagation  -rays (IC, bremsstrahlung, π o -decay) radio: synchrotron (i) CR –fixing propagation (ii) γ-rays

8. Igor V. Moskalenko 8 November 17, 2005GALPROP manual/Rome2, Italy GALPROP Output/FITS files Provides literally everything: All nuclei and particle spectra in every grid point (x,y,R,z,E) -FITS files Separately for π 0 -decay, IC, bremsstrahlung: Emissivities in every grid point (x,y,R,z,E,process) Skymaps with a given resolution (l,b,E,process) Output of maps separated into H I, H 2, and rings to allow fitting X, metallicity gradient etc.

9. Igor V. Moskalenko 9 November 17, 2005GALPROP manual/Rome2, Italy Spatial Grids Z R,x,y 0 1 2 3 4 5 6 7 1 Typical grid steps (can be arbitrary!) Δz = 0.1 kpc, ΔΔz = 0.01 kpc (gas averaging) ΔR = 1 kpc ΔE = x1.2 (log-grid)

10. Igor V. Moskalenko 10 November 17, 2005GALPROP manual/Rome2, Italy GALPROP Calculations Constraints Bin size (x,y,z) depends on the computer speed, RAM; final run can be done on a very fine grid ! No other constraints ! –any required process/formalism can be implemented Calculations (γ -ray related)  Vectorization options  Now 64 bit to allow unlimited arrays  Heliospheric modulation: routinely force-field, more sophisticated model ? 1.For a given propagation parameters: propagate p, e, nuclei, secondaries (currently in 2D) 2.The propagated distributions are stored 3.With propagated spectra: calculate the emissivities (π 0 -decay, IC, bremss) in every grid point 4.Integrate the emissivities over the line of sight: GALPROP has a full 3D grid, but currently only 2D gas maps (H2, H I, H II) Using actual annular maps (column density) at the final step High latitudes above b=40˚ -using integrated H I distribution

11. Igor V. Moskalenko 11 November 17, 2005GALPROP manual/Rome2, Italy Dark Matter in GALPROP DM annihilation products: χ 0 χ 0 −> p, pbar, e +, e −, γ A set of routines (gen_DM_source.cc) to assign The DM density profile (NFW, isothermal etc.) Source functions for p, pbar, e +, e − Source function for γ’s A set of user-defined parameters (10 int, 10 double precision) in galdef-file  DM annihilation products particles are propagated in the same model as CR particles.  Calculation of skymaps for DM γ-rays

12. Igor V. Moskalenko 12 November 17, 2005GALPROP manual/Rome2, Italy galdef_44_599278 -I

13. Igor V. Moskalenko 13 November 17, 2005GALPROP manual/Rome2, Italy galdef_44_599278 -II

14. Igor V. Moskalenko 14 November 17, 2005GALPROP manual/Rome2, Italy galdef_44_599278 -III

15. Igor V. Moskalenko 15 November 17, 2005GALPROP manual/Rome2, Italy galdef_44_599278 -IV

16. Igor V. Moskalenko 16 November 17, 2005GALPROP manual/Rome2, Italy Nuclear Reaction Network+Cross Sections p,EC,β + β -, n Be 7 Be 10 Al 26 Cl 36 Mn 54 Plus some dozens of more complicated reactions. But many cross sections are not well known… V 49 Ca 41 Cr 51 Fe 55 Co 57 Ar 37 Secondary, radioactive ~1 Myr & K-capture isotopes

17. Igor V. Moskalenko 17 November 17, 2005GALPROP manual/Rome2, Italy Nuclear Reaction Network III I II IV V nuc_package.cc

18. Igor V. Moskalenko 18 November 17, 2005GALPROP manual/Rome2, Italy nuc_package.cc: Stable & Long-lived Isotopes

19. Igor V. Moskalenko 19 November 17, 2005GALPROP manual/Rome2, Italy nuc_package.cc: Long-Lived Isotopes

20. Igor V. Moskalenko 20 November 17, 2005GALPROP manual/Rome2, Italy nuc_package.cc: “Boundary” Nuclei

21. Igor V. Moskalenko 21 November 17, 2005GALPROP manual/Rome2, Italy isotope_cs_eval.dat

22. Igor V. Moskalenko 22 November 17, 2005GALPROP manual/Rome2, Italy Transport Equations ~90 (no. of CR species) ψ(r,p,t) – ψ(r,p,t) – density per total momentum sources (SNR, nuclear reactions…) convection diffusion diffusive reacceleration E-loss convection fragmentation radioactive decay

23. Igor V. Moskalenko 23 November 17, 2005GALPROP manual/Rome2, Italy Finite Differencing

24. Igor V. Moskalenko 24 November 17, 2005GALPROP manual/Rome2, Italy Finite Differencing: Example

25. Igor V. Moskalenko 25 November 17, 2005GALPROP manual/Rome2, Italy Tri-Diagonal Matrix

26. Igor V. Moskalenko 26 November 17, 2005GALPROP manual/Rome2, Italy Coefficients for the Crank-Nicholson Method

27. Igor V. Moskalenko 27 November 17, 2005GALPROP manual/Rome2, Italy Near Future Developments Full 3D Galactic structure: 3D gas maps (from S.Digel, S.Hunter and/or smbd else) 3D interstellar radiation & magnetic fields (A.Strong & T.Porter) Cross sections: Blattnig et al. formalism for π 0 -production Diffractive dissociation with scaling violation (T.Kamae –param.) Isotopic cross sections (with S.Mashnik, LANL; try to motivate BNL, JENDL-Japan, other Nuc. Data Centers) Modeling the local structure: Local SNRs with known positions and ages Local Bubble, local clouds –may be done at the final calculation step (grid bin size ??) Energy range: Extend toward sub-MeV range to compare with INTEGRAL diffuse emission (continuum; 511 keV line) Heliospheric modulation: Implementing a modern formalism (Potgieter, Zank etc.) Visualization tool (started) using the classes of CERN ROOT package: images, profiles, and spectra from GALPROP to be directly compared with data Improving the GALPROP module structure (for DM studies)

28. Igor V. Moskalenko 28 November 17, 2005GALPROP manual/Rome2, Italy More developments  Point sources: develop algorithm(s) for modeling the background and interface to the rest of GLAST software  Instrumental response: how to implement  Diffuse emission analysis has to include point source catalog!  At least, two diffuse models: with/without the “excess”  Develop test case(s) to test the accuracy of the numerical model (simple gas distribution, no energy losses, uniform ISRF etc.)  Complete C++ package: rewrite several fortran routines in C++  Develop a fitting procedure to make automatic fitting to B/C ratio, CR spectra and abundances  Develop a dedicated Web-site: –Controlled changes in GALPROP: tests +documentation +… –Allow for communication with users –Post relevant information: best models, gas maps, ISRF, nuclear cross sections… –Ability to run GALPROP on-line…

29. Igor V. Moskalenko 29 November 17, 2005GALPROP manual/Rome2, Italy Fixing Propagation Parameters: Standard Way Using secondary/primary nuclei ratio: Diffusion coefficient and its index Propagation mode and its parameters (e.g., reacceleration V A, convection V z ) Radioactive isotopes: Galactic halo size Z h Z h increase B/C Be 10 /Be 9 Interstellar E k, MeV/nucleon

30. Igor V. Moskalenko 30 November 17, 2005GALPROP manual/Rome2, Italy Peak in the Secondary/Primary Ratio Leaky-box model: fitting path-length distribution -> free function B/C Diffusion models:  Diffusive reacceleration  Convection  Damping of interstellar turbulence  Etc. Accurate measurements in a wide energy range may help to distinguish between the models E k, MeV/nucleon too sharp max?

31. Igor V. Moskalenko 31 November 17, 2005GALPROP manual/Rome2, Italy Distributed Stochastic Reacceleration Fermi 2-nd order mechanism B Scattering on magnetic turbulences D pp ~ p 2 V a 2 /D D ~ vR 1/3 - Kolmogorov spectrum I cr E strong reacceleration weak reacceleration ΔEΔE Simon et al. 1986 Seo & Ptuskin 1994 1/3 D xx = 5.2x10 28 (R/3 GV) 1/3 cm -2 s -1 V a = 36 km s -1 γ ~ R -δ, δ=1.8/2.4 below/above 4 GV

32. Igor V. Moskalenko 32 November 17, 2005GALPROP manual/Rome2, Italy Convection Galactic wind Escape length Xe E v R -0.6 wind or turbulent diffusion resonant diffusion Jones 1979 problem: too broad sec/prim peak D~R 0.6 D xx = 2.5x10 28 (R/4 GV) 0.6 cm -2 s -1 dV/dz = 10 km s -1 kpc -1 γ ~ R -δ, δ=2.46/2.16 below/above 20 GV

33. Igor V. Moskalenko 33 November 17, 2005GALPROP manual/Rome2, Italy Damping of Interstellar Turbulence Iroshnikov-Kraichnan cascade: Kolmogorov cascade: W(k) k dissipation 1/10 12 cm 1/10 20 cm Simplified case: 1-D diffusion No energy losses Mean free path nonlinear cascade Ptuskin et al. 2003, 2005

34. Igor V. Moskalenko 34 November 17, 2005GALPROP manual/Rome2, Italy Dxx – Diffusion Coefficient Plain diffusion Diffusive reacceleration Reacceleration with damping ~R 0.6 ~β -3

35. Igor V. Moskalenko 35 November 17, 2005GALPROP manual/Rome2, Italy Positrons/electrons p+p->π,K->e ± (MS 1998) –Dermer 1986 method: LE –Stecker Δ-isobar model (isotropic decay), HE –scaling (inv. x-section: Stephens & Badhwar 1981), plus interpolation in between –Pion decay “includes” polarization of muons –Kaon decay – scaling (Stephens & Badhwar 1981) Antiprotons (M et al. 2002) –pp Inclusive production x-section (Tan & Ng 1983) –pA, AA-> pbar –scaling using Gaisser & Schaeffer 1992 or Simon et al. 1998 –results similar –Total inelastic x-section (p: TN’83, A: Moiseev & Ormes 1997) –p+pbar annihilation x-section = (p+pbar) tot – (p+p) tot (LE: TN’83, HE: PDG’00 –Regge parameterization) How It Is Really Done: Secondary Particles

36. Igor V. Moskalenko 36 November 17, 2005GALPROP manual/Rome2, Italy Elemental Abundances: CR vs. Solar System CR abundances: ACE Solar system abundances LiBeB CNO F Fe ScTiV CrMn Si Cl Al O Volatility Na S “input” “output”

37. Igor V. Moskalenko 37 November 17, 2005GALPROP manual/Rome2, Italy Fitting to Measured CR Abundances (ACE vs HEAO-3) Fitting to measured CR abundances in the wide energy range (~0.1 – 30 GeV) is problematic: May indicate systematic or cross-calibration errors

38. Igor V. Moskalenko 38 November 17, 2005GALPROP manual/Rome2, Italy Total Nuclear Cross Sections E kin, MeV/nucleon Wellisch & Axen 1996

39. Igor V. Moskalenko 39 November 17, 2005GALPROP manual/Rome2, Italy Isotopic Production Cross Sections of LiBeB Semi-empirical systematics are not always correct. Results obtained by different groups are often inconsistent and hard to test. Very limited number of nuclear measurements: Evaluating the cross section is very laborious and can’t be done without modern nuclear codes. Use LANL nuclear database and modern computer codes.

40. Igor V. Moskalenko 40 November 17, 2005GALPROP manual/Rome2, Italy LiBeB: Major Production Channels Propagated Abundance * Cross-section Be B C Li N O Li 6 7 9 10 11 13 15 14 Well defined (65%): C 12, O 16 ->LiBeB N 14 -> Be 7 (see Moskalenko & Mashnik 28 ICRC, 2003) Few measurements: C 13,N -> LiBeB B -> BeB Unknown: LiBeB,C 13,N -> LiBeB  “Tertiary” reactions also important! -35% 12 16 A=

41. Igor V. Moskalenko 41 November 17, 2005GALPROP manual/Rome2, Italy Effect of Cross Sections: Radioactive Secondaries Different size from different ratios… Z halo,kp c ST W 27 Al+p  26 Al Errors in CR measurements (HE & LE)Errors in CR measurements (HE & LE) Errors in production cross sectionsErrors in production cross sections Errors in the lifetime estimatesErrors in the lifetime estimates Different origin of elements (Local Bubble ?)Different origin of elements (Local Bubble ?) nat Si+p  26 Al W ST T 1/2 = ? E k, MeV/nucleon

42. Igor V. Moskalenko 42 November 17, 2005GALPROP manual/Rome2, Italy How It Is Really Done: Nucleons Calculated for p+A reactions and scaled for α+A (Ferrando et al. 1988) Calculation of total nuclear cross sections –Letaw et al. 1983 –Wellisch & Axen 1996 (corrected), Z>5 –Barashenkov & Polanski 2001 Calculation of isotopic production cross sections –Webber et al. 1993 (non-renormalized, renormalized); E>200 MeV/nucleon, essentially flat –Silberberg & Tsao 2000 (non-renormalized, renormalized); claim that it works at all energies, but is problematic sometimes –Fits to the available data (LANL, Webber et al., etc.) in the form of a function or a table (see.dat files), but data may not be always available –Use the best of all three, but very time consuming work Nuclear reaction network –Nuclear Data Tables (includes several decay channels + branching) –Standard β ± -decay, emission of p, n –K-capture isotopes can be treated separately

43. Igor V. Moskalenko 43 November 17, 2005GALPROP manual/Rome2, Italy Interstellar Gas ► Extend CO surveys to high latitudes – newly-found small molecular clouds will otherwise be interpreted as unidentified sources, and clearly limit dark matter studies ► C 18 O observations (optically thin tracer) of special directions (e.g. Galactic center, arm tangents) – assess whether velocity crowding is affecting calculations of molecular column density, and for carefully pinning down the diffuse emission 20 0 -20 -40 Galactic Latitude 220 200 180 160 140 120 100 80 60 40 20 0 CfA 1.2m Galactic Longitude Dame, Hartmann, & Thaddeus (2001) Dame & Thaddeus (2004)

44. Igor V. Moskalenko 44 November 17, 2005GALPROP manual/Rome2, Italy Distribution of Interstellar Gas Neutral interstellar medium –21-cm H I & 2.6-mm CO (stand in for H 2 ) Near-far distance ambiguity, rotation curve, optical depth effects, … Dame et al. (1987) Hartmann & Burton (1997) (25°, 0°) W. Keel CO H I G.C. 25° Seth Digel

45. Igor V. Moskalenko 45 November 17, 2005GALPROP manual/Rome2, Italy Seth Digel’05

46. Igor V. Moskalenko 46 November 17, 2005GALPROP manual/Rome2, Italy Gas Distribution Sun Molecular hydrogen H 2 is traced using J=1-0 transition of 12 CO, concentrated mostly in the plane (z~70 pc, R<10 kpc) Atomic hydrogen H I (radio 21 cm) has a wider distribution (z~1 kpc, R~30 kpc) Ionized hydrogen H II (visible, UV, X) small proportion, but exists even in halo (z~1 kpc) Z=0,0.1,0.2 kpc

47. Igor V. Moskalenko 47 November 17, 2005GALPROP manual/Rome2, Italy Gas Rings: HI (Inner & Outer Galaxy) Seth Digel’05

48. Igor V. Moskalenko 48 November 17, 2005GALPROP manual/Rome2, Italy Seth Digel’05 Gas Rings: HI (Our Neighborhood)

49. Igor V. Moskalenko 49 November 17, 2005GALPROP manual/Rome2, Italy Bremsstrahlung (Koch & Motz 1959, SMR2000) –many different regimes: –LE: 0.01 < E kin < 0.07 MeV –nonrelativistic non-screened brems –Intermediate: 0.07 < E kin <2 MeV –HE: E kin > 2 MeV arbitrary screening: unshielded charge, 1-, 2- electron atoms (form factors, Hylleraas, Hertree-Fock wave functions) –Fano-Sauter limit: k->E kin “Anisotropic” IC (MS2000) –Takes into account the anisotropic angular distribution of background photons Neutral pion decay (see “secondary positrons/electrons”) Synchrotron radiation (Ginzburg 1979, Ghisellini et al. 1988) –Averaging over pitch angle –Uses total magnetic field (regular + random) Emissivities: uses “real” H 2, H I gas column densities (“rings”) Skymap calculations: integration over the line of sight How It Is Really Done: Gammas

50. Igor V. Moskalenko 50 November 17, 2005GALPROP manual/Rome2, Italy Uncertainties in the Propagation Models Production cross sections of isotopes and pbars Typical errors ~50%  Fitting to B/C ratio may introduce errors in D xx Propagation models and parameters  Gas distribution in the Galaxy Ambient spectrum of CR (solar modulation, GeV excess in γ’s !)  Current knowledge of CR diffusion Heliospheric modulation  Depends on rigidity  Similar for all nuclei A/Z~ +2 Different for protons A/Z=+1 and pbars A/Z=-1 Systematic errors of measurements Difficult to account for Simultaneous measurements of Li, Be, B, C, secondary e +, p in a wide energy range ~100 MeV/nucleon – 100 GeV/nucleon are needed to understand CR propagation and distinguish between the models: looking forward to Pamela launch! _