galprop code for crcode for cr propagation and diffuse...

GALPROP code for CRGALPROP code for CRGALPROP code for CR propagation and diffuse

emissions

GALPROP code for CR propagation and diffuse

emissionsemissionsemissions

Igor V. MoskalenkoIgor V. MoskalenkoStanford & KIPACStanford & KIPAC

SciNeGHE 2010, Trieste – September 6, 2010 :: IVM/Stanford-KIPAC 1

ContentsContents

Introduction to propagation of CRsIntroduction to propagation of CRs

Building a model of the diffuse emission

Effect of anisotropic inverse Compton scattering

Building a model of the diffuse emission

Effect of anisotropic inverse Compton scattering

A view from far far away: multi-wavelength luminosity of the Milky WayA view from far far away: multi-wavelength luminosity of the Milky Wayy y

Bayesian analysis of propagation parameters

y y

Bayesian analysis of propagation parameters

GALPROP WebRunGALPROP WebRun


CR Propagation: Milky Way GalaxyCR Propagation: Milky Way Galaxy1 kpc ~ 3×1021 cm1 kpc ~ 3×1021 cm1 kpc 3 10 cm1 kpc 3 10 cm

Optical image: Cheng et al. 1992, Brinkman et al. 1993Radio contours: Condon et al. 1998 AJ 115, 1693

Optical image: Cheng et al. 1992, Brinkman et al. 1993Radio contours: Condon et al. 1998 AJ 115, 1693

Halo0.1-0.01/ccm

NGC891

SunSun

Intergalactic spaceR Band image of NGC891R Band image of NGC891


R Band image of NGC891R Band image of NGC8911.4 GHz continuum (NVSS), 1,2,…64 1.4 GHz continuum (NVSS), 1,2,…64 mJymJy/ beam/ beam “Flat halo” model (Ginzburg & Ptuskin 1976)“Flat halo” model (Ginzburg & Ptuskin 1976)

CRs in the Interstellar MediumCRs in the Interstellar Medium

ISMISMSNR RX J1713SNR RX J1713--39463946SNR RX J1713SNR RX J1713--39463946SNR RX J1713SNR RX J1713--39463946

ee±±e±

X,γX,γISMISM

42 sigma (2003+2004 data)SNR RX J1713SNR RX J1713--39463946

42 sigma (2003+2004 data)42 sigma (2003+2004 data)SNR RX J1713SNR RX J1713--39463946SNR RX J1713SNR RX J1713--39463946

ChandraChandraChandra

eee

PPHeHePP

HeHeISRFISRF•diffusion•diffusion

•energy losses •energy losses •diffusive reacceleration•diffusive reacceleration

•diffusion•diffusion•energy losses •energy losses

•diffusive reacceleration•diffusive reacceleration

ICICHESSPSF

HESSHESSPSFPSF

BBBHESSHESSHESS

CNOCNOCNOCNO gasgasgasee++--e +-

ππ++--π+-

•diffusive reacceleration•diffusive reacceleration•convection•convection

•production of •production of secondariessecondaries

•diffusive reacceleration•diffusive reacceleration•convection•convection

•production of •production of secondariessecondaries

ππ 00π 0 FermiFermiFermiWIMPWIMPaannihilnnihil..WIMPWIMPaannihilnnihil..

PP__PP__

P,P,P,P, X,γX,γ

ee±±e± gasgasgas

PP__PP__

LiBeBLiBeBLiBeBLiBeBpppp

HeHeCNOCNOHeHe

CNOCNO

Flux

Fluxππ

++--π+-

ee±±e±

eee solar modulation

ACEACE

CNOCNOCNOCNO

20 GeV/n20 GeV/n

CR species:O l 1 l ti

CR species:O l 1 l ti

BESSBESS

eee


ACEACEhelio-modulationhelio-modulation

Only 1 locationmodulationOnly 1 locationmodulationPAMELAPAMELA

Components of realistic CR propagation modelComponents of realistic CR propagation model

Detailed gas distribution (energy losses, π0, bremsstrahlung)

I t t ll di ti fi ld (IC ± l )

Detailed gas distribution (energy losses, π0, bremsstrahlung)

I t t ll di ti fi ld (IC ± l )Interstellar radiation field (IC, e± energy losses)

Nuclear & particle production cross sections & the reaction

Interstellar radiation field (IC, e± energy losses)

Nuclear & particle production cross sections & the reaction

network

G d i b hl C 0

network

G d i b hl C 0Gamma-ray production: bremsstrahlung, IC, π0

Energy losses: ionization, Coulomb, brems, IC, synchrotron

Gamma-ray production: bremsstrahlung, IC, π0

Energy losses: ionization, Coulomb, brems, IC, synchrotrongy , , , , y

Solve transport equations for all CR species

gy , , , , y

Solve transport equations for all CR species


Derive the propagation parametersDerive the propagation parameters

Transport Equations ~90 (no. of CR species)Transport Equations ~90 (no. of CR species)

t∂ r )(

VD

prqttprψ

∇∇

=∂

∂

rrr

r

][

),(),,( sources (SNR, nuclear reactions…)sources (SNR, nuclear reactions…)sources (SNR, nuclear reactions…)sources (SNR, nuclear reactions…)

diff idiff idiff idiff i VxxD

ψ

ψψ

⎤⎡ ∂∂

−∇⋅∇+

2

][

convectionconvectionconvectionconvection

diffusiondiffusiondiffusiondiffusion

ppppDp

pψ

⎥⎥⎦

⎤

⎢⎢⎣

⎡

∂∂

∂∂

+ 22 convection convection

(Galactic wind)convection convection

(Galactic wind)diffusive reaccelerationdiffusive reacceleration(diffusion in the momentum space)

diffusive reaccelerationdiffusive reacceleration(diffusion in the momentum space)

Vpdtdp

pψψ ⎥⎦⎤

⎢⎣⎡ ⋅∇−

∂∂

−rr

31EE--losslossEE--lossloss

ψψ((rr p tp t)) –– densityψψ((rr p tp t)) –– densitydf τψ

τψ

−−fragmentationfragmentationfragmentationfragmentation radioactive decayradioactive decayradioactive decayradioactive decay


ψψ((rr,p,t,p,t) ) density per total momentumψψ((rr,p,t,p,t) ) density per total momentum+ boundary conditions+ boundary conditions+ boundary conditions+ boundary conditions

Secondary/primary nuclei ratio & CR propagationSecondary/primary nuclei ratio & CR propagationTypical parameters (model-dependent):

D 1028 ( /1 GV)α 2/Typical parameters (model-dependent):

D 1028 ( /1 GV)α 2/D ~ 1028 (ρ/1 GV)α cm2/sα ≈ 0.3-0.6Zh ~ 4-6 kpc; VA ~ 30 km/s

D ~ 1028 (ρ/1 GV)α cm2/sα ≈ 0.3-0.6Zh ~ 4-6 kpc; VA ~ 30 km/s

Be10/Be9Be10/Be9

Zh increaseZh increase

Using secondary/primary nuclei ratio (B/C) & radioactive isotopes (e.g. Be10):Diffusion coefficient and its indexGalactic halo size ZhPropagation mode and its parameters (e g reacceleration V convection V )

Using secondary/primary nuclei ratio (B/C) & radioactive isotopes (e.g. Be10):Diffusion coefficient and its indexGalactic halo size ZhPropagation mode and its parameters (e g reacceleration V convection V )


Propagation mode and its parameters (e.g., reacceleration VA, convection Vz)Propagation parameters are model-dependentPropagation mode and its parameters (e.g., reacceleration VA, convection Vz)Propagation parameters are model-dependent

Relevant CR and gamma-ray (also CR!) instrumentsRelevant CR and gamma-ray (also CR!) instruments

PAMELApbar

đ,α

pbar

đ,αBESS-Polar

i-mat

ter

i-mat

ter

−

e+

e-

e+

e- Fermi/LATHESSMagic

Integral

AM

S-I HEATWMAP

CAPRICE

anti

anti

p

He

p

He

BESS-PolarAMS-I

gMilagroVeritasCOMPTEL

EGRET ATICC At

erter

Z≤8

8

Fermi-LAT 1-year Gamma-Ray SkymapFermi-LAT 1-year Gamma-Ray Skymap

Galactic plane

Buiding a modelBuiding a model

of the diffuse emissionof the diffuse emission

Sources

Dominating source of gamma rays on the sky. Produced by CR interactions with interstellar Dominating source of gamma rays on the sky. Produced by CR interactions with interstellar


gas and radiation field – the so-called diffuse emission. The diffuse Galactic gamma rays are the tracers of CR proton and electron spectra throughout the Galaxy.gas and radiation field – the so-called diffuse emission. The diffuse Galactic gamma rays are the tracers of CR proton and electron spectra throughout the Galaxy.

Diffuse Galactic GammaDiffuse Galactic Gamma--ray ray EmissionEmissionDiffuse Galactic GammaDiffuse Galactic Gamma--ray ray EmissionEmission

Origin and propagation of cosmic rays– Nature and distribution of CR

sources

Origin and propagation of cosmic rays– Nature and distribution of CR

sources

Foreground against which sources are detected− Point sources: limitation on

Foreground against which sources are detected− Point sources: limitation on

– Abundances of primary species– Production of secondary species– The propagation mode and its

– Abundances of primary species– Production of secondary species– The propagation mode and its

sensitivity− Extended sources: disentanglement

Indirect dark matter detection

sensitivity− Extended sources: disentanglement

Indirect dark matter detectionp p grelationship to magnetic turbulence in the ISM

Interstellar Medium

p p grelationship to magnetic turbulence in the ISM

Interstellar Medium

− Predicted γ-ray/CR signals− relies on accurate treatment of

standard astrophysical sources

− Predicted γ-ray/CR signals− relies on accurate treatment of

standard astrophysical sources– Distribution of HI, H2, HII gas– Nature of XCO relation in Galaxy– Distribution and intensity of

i ll di i fi ld d

– Distribution of HI, H2, HII gas– Nature of XCO relation in Galaxy– Distribution and intensity of

i ll di i fi ld d

Foreground for isotropic diffuse background− Whatever its nature

Foreground for isotropic diffuse background− Whatever its nature

interstellar radiation field and formation of H2interstellar radiation field and formation of H2


Fermi-LAT: diffuse gammasFermi-LAT: diffuse gammasC ti l GALPROP d l i i t ith thC ti l GALPROP d l i i t ith thConventional GALPROP model is in agreement with the Fermi-LAT data at mid-latitudes (mostly local emission)The EGRET “GeV excess” is not confirmedThis means that we understand the basics of cosmic ray

Conventional GALPROP model is in agreement with the Fermi-LAT data at mid-latitudes (mostly local emission)The EGRET “GeV excess” is not confirmedThis means that we understand the basics of cosmic rayThis means that we understand the basics of cosmic ray propagation and calculate correctly interstellar gas and radiation field, at least, locally

This means that we understand the basics of cosmic ray propagation and calculate correctly interstellar gas and radiation field, at least, locally

model


Abdo+’09

Diffuse emission at low to high Galactic latitudes

Diffuse emission at low to high Galactic latitudes

Pion-decay and inverse Compton emission are two dominant components – allow us to probe the average CR proton and electron spectra

Pion-decay and inverse Compton emission are two dominant components – allow us to probe the average CR proton and electron spectra

High latitudesThe GALPROP predictions agree wellThe GALPROP predictions agree well

along the line of sightalong the line of sight

Low latitudes

predictions agree well with the LAT datapredictions agree well with the LAT data

Abdo+’10

Mid-latitudes


Spectrum of isotropic diffuse γ-ray emissionSpectrum of isotropic diffuse γ-ray emission

index=2.41±0.05

2010


Accessed every 6 years (1998, 2004, 2010, 2016,…)Time-dependent: increasingly steepens with time…Accessed every 6 years (1998, 2004, 2010, 2016,…)Time-dependent: increasingly steepens with time…

Diffuse Gammas – Local SpectrumDiffuse Gammas – Local Spectrum

Mid-latitudes: Mid-latitudes: (200°

Example: latitude profile of the inner Galaxy Example: latitude profile of the inner Galaxy


Fractional count residuals: (theory-data)/dataFractional count residuals: (theory-data)/data

Agreement for models is overall goodAgreement for models is overall good

srs=SNR, Zh=4kpc, Rmax=20kpc, TS=150K, mag=5srs=SNR, Zh=4kpc, Rmax=20kpc, TS=150K, mag=5

Agreement for models is overall good but features in residuals are at ~ % levelDifference between illustrative models due to variations of model parameters

Agreement for models is overall good but features in residuals are at ~ % levelDifference between illustrative models due to variations of model parametersA)A) pp

difference between residualsdifference between residualsA)A)

A-B=A-B=srs=Lorimer,

Zh=6kpc, Rmax=20kpc,

mag=5,

srs=Lorimer, Zh=6kpc,

Rmax=20kpc, mag=5, g

optically thin HIg

optically thin HIB)B)

A-C=A-C=srs=OB,

Zh=8kpc, Rmax=30kpc,

2

srs=OB, Zh=8kpc,

Rmax=30kpc, 2


mag=2, optically thin HI

mag=2, optically thin HIC)C)

Anisotropic IC scattering in the GalaxyAnisotropic IC scattering in the Galaxy

The formalism and effect of anisotropic IC The formalism and effect of anisotropic IC p Cscattering in the Galaxy: IM & Strong’00Varies over the sky

p Cscattering in the Galaxy: IM & Strong’00Varies over the skyyGives ×(0.7-2) more gammas vs isotropic approximation

yGives ×(0.7-2) more gammas vs isotropic approximationppHas to be taken into account when modeling the diffuse emission

ppHas to be taken into account when modeling the diffuse emission


IM & Strong’00

Standard ISRF (10 kpc halo)Standard ISRF (10 kpc halo)

i t i /i t i i ii t i /i t i i ianisotropic/isotropic aniso sum iso sum anisotropic/isotropic aniso sum iso sum

50 MeV

35 GeV

SciNeGHE 2010, Trieste – September 6, 2010 :: IVM/Stanford-KIPAC 18Porter+, in preparation

Bulge×10 model (10 kpc halo)Bulge×10 model (10 kpc halo)i t i /i t i i ii t i /i t i i ianisotropic/isotropic aniso sum iso sum anisotropic/isotropic aniso sum iso sum

50 MeV

35 GeV


Ratio Bulge×10/Standard (10 kpc halo)Ratio Bulge×10/Standard (10 kpc halo)i t i k i ii t i k i ianisotropic skymap aniso sum iso sum anisotropic skymap aniso sum iso sum

50 MeV

35 GeV


Milky Way from far far away…Milky Way from far far away…Milky Way from far far away…Milky Way from far far away…


Multi-wavelength luminosity of the Milky WayMulti-wavelength luminosity of the Milky Way

“Proximity” of the MW plus direct

t ll

“Proximity” of the MW plus direct

t ll

opticalopticalpp

measurements allow us to construct its detailed “microscopic” model (GALPROP)

measurements allow us to construct its detailed “microscopic” model (GALPROP)

IRIR

HeHe( )

Integral properties of the MW – a useful template

( )

Integral properties of the MW – a useful template e−e−for studies of the normal galaxies

S l 2010 A JL

for studies of the normal galaxies

S l 2010 A JL

synchsynchπ0π0

ICICγ totalγ total

ee

Strong et al. 2010, ApJLin press Strong et al. 2010, ApJLin press

bremssbremss


Milky Way as electron calorimeterMilky Way as electron calorimeterCalculations for Zhalo= 4 kpcCalculations for Zhalo= 4 kpchalo pLeptons lose ~60% of their energyγ-rays: 50-50 by nucleons and by leptons

halo pLeptons lose ~60% of their energyγ-rays: 50-50 by nucleons and by leptons

Cosmic rays7.90×1040 erg/sCosmic rays7.90×1040 erg/s

SynchrotronSynchrotron

Primary nucleons98.6%

Primary nucleons98.6%

Synchrotron0.35%

Synchrotron0.35%

BremsstrahlungBremsstrahlung PrimaryPrimarydd Bremsstrahlung0.15%Bremsstrahlung

0.15%

Inverse ComptonInverse Compton

yelectrons

1.41%

yelectrons

1.41%

Secondaryleptons

e+: 0.33%e−: 0.10%

Secondaryleptons

e+: 0.33%e−: 0.10%

Total gamma raysTotal gamma raysNeutral pionsNeutral pions

p0.58%

p0.58%


g y1.6%g y1.6%

p0.85%

p0.85%

* The percentages in brackets show the values relative to the luminosity of their respective lepton populations

* The percentages in brackets show the values relative to the luminosity of their respective lepton populations

Constrains on CR propagation d l f l b l

Constrains on CR propagation d l f l b lmodels from global scansmodels from global scans


Bayesian approach (Θ vector of parameters D available observations):Bayesian approach (Θ vector of parameters D available observations):

MethodologyMethodologyBayesian approach (Θ – vector of parameters, D – available observations):Bayesian approach (Θ – vector of parameters, D – available observations):

P(Θ | D) =P(D |Θ)P(Θ)

P(D)P(Θ|D) – posterior distribution of parameters P(D|Θ) – likelihood function (for fixed D)P(Θ|D) – posterior distribution of parameters P(D|Θ) – likelihood function (for fixed D)

P(D)

( | ) ( )P(Θ) – prior distributionP(D) – Bayesian evidenceBayesian approach allows for a more sophisticated treatment of systematics

( | ) ( )P(Θ) – prior distributionP(D) – Bayesian evidenceBayesian approach allows for a more sophisticated treatment of systematicsBayesian approach allows for a more sophisticated treatment of systematicsNested sampling algorithm by John Skilling’04,06 and MultiNest by Feroz&Hobson’08 (SuperBayeS code by Ruiz de Austri+’06, Trotta+’08)T t l 1 4×105 l 13 CPU

Bayesian approach allows for a more sophisticated treatment of systematicsNested sampling algorithm by John Skilling’04,06 and MultiNest by Feroz&Hobson’08 (SuperBayeS code by Ruiz de Austri+’06, Trotta+’08)T t l 1 4×105 l 13 CPUTotal 1.4×105 samples, ~13 CPU yearsThe posterior distribution is in excellent agreement with one from MCMC Representative data from ACE, ISOMAX, HEAO-3, ATIC-2, CREAM

Total 1.4×105 samples, ~13 CPU yearsThe posterior distribution is in excellent agreement with one from MCMC Representative data from ACE, ISOMAX, HEAO-3, ATIC-2, CREAM


Fit a total of 17 parameters, best fit chi-squared/dof ~ 1 More details in the paper (to be submitted in a few days)Fit a total of 17 parameters, best fit chi-squared/dof ~ 1 More details in the paper (to be submitted in a few days)

Posterior probability distributionsPosterior probability distributionsNormalization of the diffusion coeff. and its index

- the best fit

ti l li t i

- the best fit

ti l li t ivertical line – posterior mean

vertical line – posterior mean

Alfven speed Halo sizecolor bar – 68%, 95% error

rangescolor bar – 68%, 95% error

ranges

Reacceleration modelReacceleration modelInjection index below/above the break @ 1 GV

Parameters are very close to those derived by the eye-fitting

Parameters are very close to those derived by the eye-fitting


y y gmethod

y y gmethod

2D posterior probability distributions2D posterior probability distributions

Contours enclose 68% and Contours enclose 68% and 95% probability regions

- best fit

95% probability regions

- best fit

● posterior mean● posterior mean● - posterior mean● - posterior mean


Examples of the fits: B/C and Be ratiosExamples of the fits: B/C and Be ratios

B/C ratio

Be10/Be9 ratioBe /Be ratio


Examples: Carbon and pbarsExamples: Carbon and pbars

Carbon

pbars

(not fitted!)


(not fitted!)

GALPROP WebRunGALPROP WebRunGALPROP WebRun

galprop.stanford.edu

GALPROP WebRun

galprop.stanford.edugalprop.stanford.edugalprop.stanford.edu


Igor Moskalenko

for the GALPROP development team

Igor Moskalenko

for the GALPROP development team

GALPROP WebRunGALPROP WebRun

GALPROP WebRun is a service that allows to run GALPROP via the WWWGALPROP WebRun is a service that allows to run GALPROP via the WWW

No local installation of the code or related libraries is necessary, only a web browser is requiredNo local installation of the code or related libraries is necessary, only a web browser is required

Available at http://galprop.stanford.edu/webrun

Calculations can be performed on a new cluster at Stanford University, using

Available at http://galprop.stanford.edu/webrun

Calculations can be performed on a new cluster at Stanford University, using the most recent GALPROP v54, older versions are also available

The service is free and open to the community. Registration is required

the most recent GALPROP v54, older versions are also available

The service is free and open to the community. Registration is required

Acknowledge by citing the web-page and the introduction paper http://arxiv.org/abs/1008.3642 (submitted to Computer Physics Acknowledge by citing the web-page and the introduction paper http://arxiv.org/abs/1008.3642 (submitted to Computer Physics


Communications)Communications)

Configuring GALPROP via WebRunConfiguring GALPROP via WebRun


Interactive interface for parameter entryParameters are validated to avoid misconfgured runsInteractive interface for parameter entryParameters are validated to avoid misconfgured runs

Running calculationsRunning calculations


Multiple simultaneous runs are allowedSharing resources fairly between usersMultiple simultaneous runs are allowedSharing resources fairly between users

Evaluating and obtaining resultsEvaluating and obtaining results

Archive with FITS files (output) available to the ownerArchive with FITS files (output) available to the owner


Archive with FITS files (output) available to the ownerURL to the archive may be shared with anyoneQuick peek possible with built-in plot templates

Archive with FITS files (output) available to the ownerURL to the archive may be shared with anyoneQuick peek possible with built-in plot templates

Computing cluster (galprop.stanford.edu)Computing cluster (galprop.stanford.edu)


Thank you !y

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