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KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 1 IVM/Stanford-KIPAC 1 PAMELA Workshop, Rome/May 12, 2009
Igor V. Moskalenko (stanford/kipac)
Instroduction to
Astrophysics of Cosmic Rays
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 2
Goals To give an overview of astrophysics of cosmic
rays To show the place of recent data in the overall
picture Target audience: particle and high-energy
physicists Organization
– A bit of history– General information on CRs– Understanding CR propagation (models)– New data– Instrumentation– Conclusion
There is nothing new to be discovered in physics now. All that remains is more and more precise measurement. — Lord Kelvin, 1900
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 3
An experiment in nature, like a text in the Bible, is capable of different interpretations, according to the preconceptions of the interpreter. — William Jones,1781
There is no deficit in explanations of the PAMELA positron excess (Adriani+08): >370 papers since Oct 2008!– Various species of the dark matter (most of papers)– Pulsars– SNRs– Microquasars– a GRB nearby– …
Perhaps we have to discuss a deficit of positrons, not their excess!
Unfortunately, >99.7% of these explanations are wrong …Because there is only one correct explanation
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 4
One Good Experiment is Worth Thousand Theories…
ATIC electrons: >270 citations (in ~1 yr) PPB-BETS electrons: >150 citations (in ~1 yr) Fermi LAT electrons: >170 citations (in <1 yr) HESS electrons: >100 citations (in <1 yr) PAMELA positron fraction: >370 citations (in ~1 yr) PAMELA antiprotons: >150 citations (in <1 yr) BESS program (only journal papers): ~1000 citations
Of course, most of citations are coming from particle physics★ using NASA ADS
TeV Particle Astrophysics 2009Page 5
A Particle Physicist’s View (pre ~2000)
• An Astronomer does stamp collecting• An Astrophysicist does engineering• A Particle physicist does fundamental
science
» .....we have been humbled!
− Persis Drell
TeV Particle Astrophysics 2009Page 6
Summary Thoughts
• Wealth of data and excitement– This is a healthy field!– Multiwavelength/Multimessager/Multicultural
• We are bold in our aspirations!– Will be a rich field for decades to come
• Astrophysics is an essential part of Particle Physics!!
− Persis Drell
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 7
100 Years of Cosmic Rays
1912Victor Hess, an Austrian scientist,
took a radiation counter (a simple electroscope) on a balloon flight
He rose to 17,500 feet (without oxygen) and measured that the amount of radiation increases as the balloon climbed
Nobel Prize: 1936
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 8
Early Discoveries of New Particles in CRs1929
Bothe (Nobel Prize 1954) and Kolhorster verified that the cloud chamber tracks were curved. Thus the cosmic radiation was charged particles
1932 a discovery of positron by C. Anderson (Nobel
Prize 1936)
1937a discovery of muon by Neddermeyer &
Anderson and simultaneously by Street & Stevenson
1947pions predicted by Yukawa (1935, Nobel Prize
1949) to explain the force that binds the nucleus together were discovered (C. Powell et al.; Nobel Prize 1950)
kaons were discovered by Rochester & Butler
C. Anderson
H.Yukawa
W.Bothe
C.Powell
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 9
Renaissance of Particle AstrophysicsParticle astrophysics, which has recently emerged as an
interdisciplinary science, is flourishing nowadays.
It was born in the early days of cosmic-ray physics about a century ago and then reborn twice, first with the launch of the first X-ray telescopes, and second with the discovery that the matter in the universe is dominated by something dark, the dark matter.
The latter rebirth brought an army of particle physicists into astrophysics, while astrophysicists began to realize that supersymmetry can play a role on a macro scale.
Particle astrophysics is now a busy intersection between high-energy astrophysics, particle physics, and cosmology.
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 10
General information on CRs
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 11
All Particle CR Spectrum
GZK cutoff
This is an astonishing observation!
All particle CR spectrum is almost featureless. It can be described as a single power-law with index -3 in >12 decades in energy and >32 decades in intensity!
There are only 3 well-established features:
–the knee –the ankle –GZK cutoff
A lot of information is hidden in the spectra and abundances of individual CR species: nuclear isotopes, antiprotons, electrons, positrons (+diffuse gamma rays)
CRs are the only probes of the interstellar material available to us.
The whole physics is involved: various branches of Astrophysics, MHD, shock waves, plasma physics, atomic, nuclear, & particle physics, exotic physics – SUSY…
Galactic
Galactic+extragalactic
extragalactic
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 12
Positrons and antiprotons constitute a tiny fraction of the total CR flux, yet may contain signatures of new physics!
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 13
Spectra of CR nuclei
Examples of spectra of individual elements in cosmic rays
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 14
Elemental abundances in CRs and in the Solar System
“Output”: CR abundances (ACE)
“Input”: solar system abundances
LiBeB
CNO
F
Fe
ScTiV
CrMn
Si
Cl
Al
A lot of information is hidden in elemental and isotopic abundances of CR.The elements which are rare in the solar system, such as Li, Be, B, Sc, Ti, V, and some others, appear to be abundant in CRs.They are called “secondaries” because they are produced by spallations of heavier nuclei (so-called “primary”, e.g. C, O, Fe) during the CR propagation. The CR age deduced from the amount of secondaries is ~10 Myr.
“prim
ary”
“sec
onda
ry”
“sec.”
“prim
.”
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 15
Heavy Nuclei in CRs
Heavy nuclei are produced in SN explosions. They can’t propagate from large distances because of the very large inelastic cross section.
Wiedenbeck+2007
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 16
Isotopic Data
Very detailed isotopic data exist at low energies!(Isotopes of the same element are connected by lines)
Wiedenbeck+2001
ACE dataSolar SystemACE: 100-200 MeV/nucleon
Atomic number
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 17
Fermi-LAT 1-year Gamma-Ray Skymap
~80% of gamma-rays are produced by CR interactions with interstellar gas and radiation field! – therefore, the diffuse Galactic gamma rays trace CR proton and electron spectra throughout the Galaxy
Galactic plane
Sources
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 18
To make sense of all these data, one needs a model!
A theory is something nobody believes, except the person who made it. An experiment is something everybody believes, except the person who made it. − Albert Einstein
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 19
Transport Equation…
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 20
CRs in the Interstellar Medium
e+-
PHe
CNO
X,γ
gas
gas
ISRF
e+-π+-
P_
LiBeB
ISM
•diffusion •energy losses •reacceleration •convection •production of secondaries π0
IC
bremss
ACEhelio-modulation
p
42 sigma (2003+2004 data)
HESS
SNR RX J1713-3946
PSF
B
HeCNO Fl
ux
20 GeV/n
CR species: Only 1 location modulation
e+-
π+-
PAMELA
BESS
Fermi
HESS
Chandra
WIMPannihil.
P_
P,
e+-
X,γ
synchrotron
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 21
CR Propagation: the Milky Way Galaxy
Halo
Gas, sources
100
pc 40 kpc
4-12
kp
c
0.1-0.01/ccm
1-100/ccm
Intergalactic spaceR Band image of NGC891
1.4 GHz continuum (NVSS), 1,2,…64 mJy/ beam
Optical image: Cheng et al. 1992, Brinkman et al. 1993Radio contours: Condon et al. 1998 AJ 115, 1693
NGC891
Sun
“Flat halo” model (Ginzburg & Ptuskin 1976)
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 22
Nuclear component in CR: What we can learn?
Propagation parameters:
Diffusion coeff., halo size, Alfvén speed,
convection velocity…Energy markers:Reacceleration,
solar modulation
Local medium: Local Bubble
Material & acceleration sites, nucleosynthesis
(r-vs. s-processes)
Stable secondaries: Li, Be, B, Sc, Ti, V
Radio (t1/2~1 Myr): 10Be, 26Al, 36Cl, 54Mn
K-capture: 37Ar,49V, 51Cr, 55Fe, 57Co
Short t1/2 radio 14C & heavy Z>30
Heavy Z>30: Cu, Zn, Ga, Ge, Rb
Nucleo-synthesis: supernovae,
early universe, Big Bang…
Solar modulation
Extragalacticdiffuse γ-rays:
blazars, relic neutralino
Dark Matter (p,đ,e+,γ)-
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 23
A Model of CR Propagation in the Galaxy
• Gas distribution (energy losses, π0, brems)• Interstellar radiation field (inverse Compton, e± energy
losses)• Isotopic & particle production cross sections• Gamma-ray production: brems, inverse Compton, π0
• Energy losses: ionization, Coulomb, brems, IC, synch• Solve transport equations for all CR species• Fix propagation parameters• Then we a ready for “precise” Astrophysics:
- background for indirect DM searches and other exotics- propagation of the DM signal- CR fluxes in distant locations- Galactic/extragalactic diffuse gamma-ray emission
(extragalactic emission may also contain signatures of exotic physics)
- background for astrophysical gamma-ray sources- studies of the origin of CRs and interstellar medium
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 24
Transport Equations ~90 (no. of CR species)
ψ(r,p,t) – density per total momentum
df
Vpdtdp
p
ppppDpp
VxxD
prqttpr
31
22
][
),(),,( sources (SNR, nuclear reactions…)
convection (Galactic wind)
diffusion
diffusive reacceleration (diffusion
in the momentum space)
E-loss
fragmentation
radioactive decay
+ boundary conditions
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 25
How It Works: Fixing Propagation Parameters
Using secondary/primary nuclei ratio (B/C) & flux:
• Diffusion coefficient and its index• Propagation mode and its parameters (e.g.,
reacceleration VA, convection Vz)• Propagation parameters are model-
dependent• Make sure that the spectrum is fitted as well
Radioactive isotopes:Galactic halo size Zh
Zh increase
Be10/Be9
Ek, MeV/nucleon
Carbon
Ek, GeV/nucleon
Parameters (model dependent):D~ 1028 (ρ/1 GV)α cm2/sα ≈ 0.3-0.6Zh ~ 4-6 kpcVA ~ 30 km/s
Boron/Carbon (B/C)
Inters
tellar
Ek, MeV/nucleon
E2 F
lux
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 26
Discrimination of the propagation models
Reacceleration
Standard diffusion
• Different propagation models are tuned to fit the low energy part of sec./prim. ratio where the accurate data exist
• The sharp peak at ~1 GeV/nucleon has been confirmed by Pamela
ACEUlyssesVoyagers
CREAM
Ahn+’08
B/C
• However, the differ at high energies which will allow to discriminate between them when more accurate data will be available
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 27
Secondary/Primary Nuclei Ratio
Jones+’01
B/C
Sub-Fe/Fe
Being tuned to one type of secondary/primary ratio (e.g. B/C ratio) the propagation model should be automatically consistent with all secondary/primary ratios:
- sub-Fe/Fe- He3/He4
- pbar/p
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 28
Importance of the Pbar/P Ratio
Similarly to other secondary/ primary ratios, pbar/p ratio can be used to derive the propagation parameters
Different ratios probe different volumes in the Galaxy with the pbar/p ratio probing the largest volume since the pbar inelastic cross section is ~40 mb (vs. ~270 mb for Carbon, vs. ~750 mb for Iron)
The interstellar spectrum of pbars can be calculated because of the production threshold is large vs. the injection spectra of other nucleons which are assumed
Therefore, it can be used to probe interstellar spectrum of protons, solar modulation, and, of course, to search for signatures of exotic physics
Abe+’08
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 29
Importance of the Pbar/P Ratio (Cont’ed)
Systematic measurements of pbars in CRs (BESS) allow us to study heliospheric modulation and charge-sign effects
Important also for e+/e ratio
Abe+’08
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 30
Nuclear Reaction Network + Cross Sections
p,EC,β+
β-, n
Be7 Be10
Al2
6
Cl3
6
Mn5
4
Plus some dozens of more complicated reactionsBut many cross sections are not well known…
V4
9
Ca4
1
Cr5
1
Fe5
5
Co5
7
Ar3
7
Secondary,radioactive ~1 Myr
& K-capture isotopes
Many different isotopes in CRs are produced via spallations of heavier nuclei: A+(p,He)→B*+X
p
n
“stable”
isotopes
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 31
Effect of Cross Sections: Radioactive Secondaries
Different size from different ratios…
Zhalo,kpc
ST
W
27Al+p26Al
In determination of the propagation parameters one has to take into account:
Errors in CR measurements (@ HE & LE)Errors in production cross sectionsErrors in the lifetime estimates
natSi+p26Al
W
STT1/2=?
W – Webber+ST – Silberberg & Tsao- - - – measured
• The error bars can be significantly reduced if more accurate cross sections are used
• Different ratios provide consistent parameters
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 32
Components of the ISM: Views from the Insidesynchrotron
21 cm H I
2.6 mm CO (H2)
dust
stars & star forming
optical
n-stars, BHs
CRs x gas
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 33
ISRF: Large Scale Distribution
R = 0,4,8,12,16 kpc
TotalOptical IR
CMB
Ener
gy
Den
sity
Requires extensive modelling:– Distribution of stars of different
stellar classes in the Galaxy– Dust emission– Radiative transfer
The z scale height is large, takes 10s of kpc at R = 0 kpc to get to level of CMB
Optical + IR (no CMB)
Z=0, R=0 kpc4 kpc8 kpc
12 kpc 16 kpc
optical IR CMB
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 34
Gas distribution in the Milky Way
Sun
Molecular hydrogen H2 is traced using J=1-0 transition of 12CO, concentrated mostly in the plane (z~70 pc, R<10 kpc)
Atomic hydrogen H I (traced by 21 cm emission line) has a wider distribution (z~1 kpc, R~30 kpc)
Ionized hydrogen H II – small proportion, but exists even in halo (z~1 kpc)
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 35
Carbon Monoxide (CO) maps► Extend CO surveys to high latitudes
– newly-found small molecular clouds will otherwise be interpreted as unidentified sources, and clearly limit dark matter studies
► C18O 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
Gal
acti
c La
titu
de
220 200 180 160 140 120 100 80 60 40 20 CfA 1.2mGalactic Longitude
Dame, Hartm
ann, & Thaddeus (2001)Dam
e & Thaddeus (2004)
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 36
Calculation of the Gas Distribution
Neutral interstellar medium – most of the interstellar gas mass– 21-cm H I & 2.6-mm CO (surrogate for H2)– Differential rotation of the Milky Way – plus random motions,
streaming, and internal velocity dispersions – is largely responsible for the spectrum
– Rotation curveV(R) unique line-of-sight velocity-Galactocentric distance relationship
This is the best – but far from perfect – distance measure available Column densities: N(H2)/WCO ratio assumed; a simple approximate
correction for optical depth is made for N(H I); self-absorption of H I remains
Dame+’01
Kalberla+’05
W. Keel
H I
CO
Clemens (1985)
Rotation Curve
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 37
More on gas in the Milky Way
Pohl+’08
Surface mass density of the H2 in M sun pc−2
Sun
Contours of line-of-sight velocities from differential rotation of the Milky Way
Near-far ambiguity
No velocity information
No velocity information
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 38
The Reason of making Experiments is, for the Discovery of the Method of Nature, in its Progress and Operations. − Robert Hooke, 1664
New Experiments
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 39
Antiproton to proton ratio
Adriani+’09
preliminary
Picozza’09
• Pbar/p ratio by PAMELA is consistent with previous measurements by BESS
• Consistent with predictions of propagation models - most of pbars are secondary produced by CRs
• Provide a serious restriction on DM WIMP candidates
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 40
Antiproton Spectrum Measurements of
the absolute pbar flux are more important than the ratio
Also consistent with BESS data and predictions of the propagation models
Testifies that most antiprotons are secondary produced by CR interactions with interstellar gas
26/06/2009 40
preliminary
Picozza’09
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 41
Early Measurements of CR Electrons
Kobayashi+’03
• Early measurements have shown that the spectrum of CR electrons is steeper than that of protons
• Predictions of possible spectral features @ HE associated with local SNR
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 42
Electron Fluctuations/SNR Stochastic EventsGe
V el
ectro
ns100 TeV electrons
GALPROP/Credit S.Swordy
Electron energy loss timescale:
1 TeV: ~300 kyr 100 TeV: ~3 kyr
Compare with CR lifetime ~10 Myr
Energy losses
107 yr
106 yr
Bremsstrahlung
1 TeV
Ioniza
tion
Coulo
mb
IC,
synchrotron
E(
dE/d
t)-1 ,y
r
1 GeV1 MeV
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 43
Latronico+’09
What’s here?
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 44
Interpretation of CR Electron Data CR electron spectrum is
consistent with a single power-law with index -3.05
Can be reproduced well by the propagation models
Multi-component interpretation is also possible– Dark matter
contribution– Nearby sources (SNR,
pulsars)– …
The key in understanding of the electron spectrum is the origin of the positron excess and the diffuse gamma-ray emission
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 45
PAMELA Positron Fraction
Adriani+’08
The excess in positron fraction is confirmed and extended to higher energies while regular propagation models predict a decrease at HE
Low-energy behavior is expected due to the charge-sign dependent solar modulation
Perhaps the most intriguing puzzle! There is no deficit in explanations (Dark Matter vs. regular Astrophysical
sources) More accurate data including at HE are necessary
Solar modulation
sec. production (GALPROP)
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 46
EGRET: The famous GeV -ray excess
•Physical phenomena?•Dark Matter?• Instrumental artifact?Strong+’00,’04
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 47
Fermi/LAT: Diffuse emission at mid-latitudes Conventional GALPROP model is in agreement
with the LAT data at mid-latitudes (mostly local emission)
This means that we understand the basics of cosmic ray propagation and calculate correctly interstellar gas and radiation field
model
Abdo+’09
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 48
Fermi/LAT: Diffuse γ-ray Emission from the Local Gas
The spectrum of the local gas, after the subtraction of the IC emission, agrees well with the model
Confirms that the local proton spectrum is similar to that from direct measurements
Abdo+’09
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 49
Morphology of the Diffuse Emission @ 150 GeV
Conventional
Dark Matter
Regis&Ullio’09
IC π0
IC π0
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 50
Geminga pulsarMilagro C3
Pulsar (AGILE/Fermi)
MGRO 2019+37
Fermi PulsarSNR CygniFermi Pulsar
HESS, Milagro, Magic
Fermi PulsarMilagro (C4)
3EG 2227+6122Boomerang
PWN
SNR IC433MAGIC, VERITAS
Radio pulsar (new TeV source)
unID(new TeV source)
unID(new TeV source)
Fermi PulsarMGRO 1908+06HESS 1908+063
SNR W51HESS J1923+141
G65.1+0.6 (SNR)Fermi Pulsar (J1958)
New TeV sources
G.Sinnis’09
Milagro: TeV Observations of Fermi SourcesMany γ-ray sources show extended structures at HE – thus they are also the sources of accelerated particles (CRs)
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 51
(Some) Important Questions to Answer
How large is the positron fraction at HE (PAMELA)– Identifies the nature of sources of primary positrons
If SNRs are the sources of primary positrons, this should also affect antiprotons and secondary nuclei @ HE…– Measure pbars and secondary nuclei (PAMELA, CREAM…)
How typical for the local Galactic environment is the observed Fermi/LAT spectrum– If this is the typical spectrum then the sources of primary
positrons are distributed in the Galaxy (could be pulsars, SNRs, or DM)
– If this spectrum is peculiar then there is a local source or sources of primary positrons
– The answer is in the diffuse gamma-ray emission (Fermi/LAT) Dark matter vs Astrophysical source
– Distribution and spectrum of the diffuse γ-ray emission at HE (Fermi)
To answer these important questions we should consider all relevant astrophysical data (CRs, gamma rays) and particle data (LHC) together
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 52
Instrumentation
Nothing tends so much to the advancement of knowledge as the application of a new instrument. — Sir Humphry Davy, 1812
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 53
Fermi/LAT PAMELA
PAMELA
A Constellation of CR and gamma-ray (also CR!) instruments
1 MeV/n 1 GeV/n 1 TeV/n
TIGER
BESS-Polar
TRACERHEAO-3
Fermi/LAT
BESS-PolarAMS-I
ACE
HESSMagicMilagroVeritas
Integral
COMPTELEGRET
BESS-Polar
ATICCREAM
AMS-
I
HEATWMAP
CAPRICEanti-
mat
ter
mat
ter
SUSY
pbarđ, Ħee+
e-
pHeZ≤88<Z≤28Z>28WIMPs
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 54
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 55
Exposure of Different Experiments
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 56
The Key Question
Last couple of years the Cosmic Ray and Astrophysical communities were exposed to the overwhelming amount of new and accurate data and are expecting more to come…
It will probably take a few years to fully appreciate the significance of new information, but it is absolutely clear that we are currently on the verge of dramatic breakthroughs in Astrophysics, Particle Physics, and Cosmology and may soon be able to resolve century-old puzzles such as the origin of cosmic rays and dark matter. Hopefully before 100th anniversary of V.Hess flight in 2012!
The key question to answer is how these new discoveries fit or do not fit into the “standard picture” of the Milky Way galaxy
KEK-CPWS-HEAP2009 – Nov. 10-12, 2009 :: IVM/Stanford-KIPAC 57
Thank you !
You are here
KEK