calibration of the pierre auger observatory with lhc ...€¦ · calibration of the pierre auger...
TRANSCRIPT
![Page 1: Calibration of the Pierre Auger Observatory with LHC ...€¦ · Calibration of the Pierre Auger Observatory with LHC Forward Detectors Ralf Ulrich DESY Seminar 18./19. Januar 2011](https://reader034.vdocuments.us/reader034/viewer/2022052012/6028c758b27f11122543f077/html5/thumbnails/1.jpg)
Calibration of thePierre Auger Observatory with
LHC Forward Detectors
Ralf Ulrich
DESY Seminar 18./19. Januar 2011
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Cosmic Rays and Extensive Air Showers
Ralf Ulrich 1
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Particle Accelerators: Man-Made versus Cosmic Rays
Large Hadron Collider (LHC)
Acceleration to 7TeV
Interactions at 14TeV
Ultra-High Energy Cosmic Rays
Acceleration to > 100.000.000TeV
Interactions up to ∼ 300TeV
Fundamental physics in
extreme environments at
extreme energies
Ralf Ulrich 2
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Overview
Our understanding of hadronic interactions at cosmic ray energiesis incomplete
◮ The interpretation of air shower data is very model dependent
◮ Hadronic interaction features are not well constraint at cosmic rayenergies
◮ Calibrate air shower simulations at LHC energy
◮ Determine properties of hadronic interactions at ultra-high energiesfrom cosmic ray data
AstrophysicsParticle Physics
Extensive Air Showers Cosmic Rays
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Overview of Cosmic Ray Data
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Characterization of Current Situation
Large amounts of high quality cosmic ray dataAuger, HiRes, AGASA, TA, Future: Auger-North, JEM-EUSO
BUT
Lack of reliable hadronic interaction models,which are needed for a detailed
interpretation
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Energy Flux
Energy (eV/particle)
1310 1410 1510 1610 1710 1810 1910 2010
)1.
5 e
V-1
sr
-1 s
ec-2
J(E
) (
m2.
5S
cale
d flu
x E
1310
1410
1510
1610
1710
1810
1910
(GeV)ppsEquivalent c.m. energy 210 310 410 510 610
RHIC (p-p)
-p)γHERA (
Tevatron (p-p)LHC (p-p)
ATIC
PROTON
RUNJOB
KASCADE (QGSJET 01)
KASCADE (SIBYLL 2.1)KASCADE-Grande (prel.)
Tibet ASg (SIBYLL 2.1)
HiRes-MIA
HiRes I
HiRes IIAuger SD 2008
LHC
Auger
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Physics of the Knee
◮ Astrophysical scenarios: Eknee ∝ Z
◮ Particle physics: Eknee ∝ A⇒>20% of missing energy at LHC ...
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Physics of the Knee
◮ Astrophysical scenarios: Eknee ∝ Z
◮ Particle physics: Eknee ∝ A⇒>20% of missing energy at LHC ...
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Physics of the Knee
◮ Astrophysical scenarios: Eknee ∝ Z
◮ Particle physics: Eknee ∝ A⇒>20% of missing energy at LHC ...
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Physics of the Knee
◮ Astrophysical scenarios: Eknee ∝ Z
◮ Particle physics: Eknee ∝ A⇒>20% of missing energy at LHC ...
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Longitudinal Profiles
]2Depth [g/cm
300 400 500 600 700 800 900 1000
]2E
nerg
y de
posi
t [P
eV/g
/cm
0
2
4
6
8
10
12
14
16
18
20
Auger event
Height a.s.l. (m)60008000100001200014000
E ∼ 1019 eV
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Longitudinal Profiles
]2Depth [g/cm
300 400 500 600 700 800 900 1000
]2E
nerg
y de
posi
t [P
eV/g
/cm
0
2
4
6
8
10
12
14
16
18
20Auger event
Iron
Height a.s.l. (m)60008000100001200014000
E ∼ 1019 eV
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Longitudinal Profiles
]2Depth [g/cm
300 400 500 600 700 800 900 1000
]2E
nerg
y de
posi
t [P
eV/g
/cm
0
2
4
6
8
10
12
14
16
18
20Auger event
Nitrogen
Height a.s.l. (m)60008000100001200014000
E ∼ 1019 eV
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Longitudinal Profiles
]2Depth [g/cm
300 400 500 600 700 800 900 1000
]2E
nerg
y de
posi
t [P
eV/g
/cm
0
2
4
6
8
10
12
14
16
18
20Auger event
Proton
Height a.s.l. (m)60008000100001200014000
E ∼ 1019 eV
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Average Xmax
18 18.5 19 19.5 20
]2>
[g
/cm
max
<X
650
700
750
800
850
Energy [eV]
1810 1910 2010
SIBYLL 2.1QGSJet01cQGSJetII.3EPOS 1.61
Auger (PRL 2010)
HiRes (PRL 2010)
proton
iron
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Fluctuations of Xmax
17.5 18 18.5 19 19.5 20
]2)
[g
/cm
max
RM
S(X
10
20
30
40
50
60
70
80
90
Energy [eV]
1810 1910 2010
proton
iron
Auger (PRL 2010)
SIBYLLQGSJetQGSJetIIEPOS
⇒ Strong trend to reduced fluctuations at high energyRalf Ulrich 10
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Hadronic Interactions – Cosmic Ray-Air Cross Section
Limit: no fluctuation in the air shower after firstinteraction
σcr−air =〈m〉
RMS(X1)>
〈m〉RMS(Xmax)
(Energy/eV)10
log11 12 13 14 15 16 17 18 19 20
Cro
ss s
ectio
n
[mb]
400
600
800
1000
1200
1400
proton
QGSJET01cNEXUS 3.96SIBYLL 2.1QGSJETII.3
helium
oxygen
Energy [eV]1110 1210 1310 1410 1510 1610 1710 1810 1910 2010
[GeV]ppsEquivalent c.m. energy 210 310 410 510
)max
Lower limit from Auger RMS(X
Tevatron
LHC
Accelerator data (p−p) + Glauber
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Extensive Air Showers and Hadronic Interactions
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Extended Heitler Model
n=1
n=2
n=3
charged neutral
primary
+ -o
IX
Shower maximum
Xmax ≈ λI + X0 lnE0
Nmult E e.m.crit
Muon number at observationlevel
Nµ = Nπ± =
(
E0
E Icrit
)β
where
β = ln(
23 Nmult
)
/ ln (Nmult) ≈ 0.9
(J. Matthews, APP 22 (2005) 387)
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Beyond the Heitler Model ...
◮ Cross Section: λ
◮ Multiplicity: nmult
◮ Elasticity: kela = Emax/Etot
◮ Charge ratio: c = nπ0/(nπ0 + nπ− + nπ+)
◮ Nuclear primary: A
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Analysis of Cosmic Ray Data
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KASCADE - Electron/Muon-Frequencies
i2 χD
evia
tion
0
2
4
6
8
10
12
14
tr.µlg N
4 4.5 5 5.5 6 6.5
elg
N
5
5.5
6
6.5
7
7.5
8
i2 χD
evia
tion
0
2
4
6
8
10
12
14
tr.µlg N
4 4.5 5 5.5 6 6.5
elg
N
5
5.5
6
6.5
7
7.5
8
(KASCADE, APP:24 1 (2005), astro-ph/0505413)Ralf Ulrich 16
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Pierre Auger Observatory: Xmax vs. Muons
18 18.5 19 19.5 20
]2>
[g
/cm
max
<X
650
700
750
800
850
Energy [eV]
1810 1910 2010
SIBYLL 2.1QGSJet01cQGSJetII.3EPOS 1.61
Auger (PRL 2010)
HiRes (PRL 2010)
proton
iron
]2DX [g/cm0 200 400 600 800 1000 1200 1400 1600 1800 2000
[VE
M]
µS
0
5
10
15
20
25
30
(Energy scale: +26%)
DX=Xobs − Xmax
Muonsignalat1000m
proton
iron
data > 60deg
data < 60deg
(Auger/HiRes Xmax: PRL 2010,
Muons: e.g. ICRC 2007, arXiv:0706.1921 [astro-ph])
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Cosmic Ray Analysis/Modeling Uncertainties
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Modeling UncertaintiesCross Section Multiplicity
(Energy/eV)10
log13 14 15 16 17 18 19 20
Cro
ss s
ectio
n (p
roto
n−ai
r)
[mb]
200
300
400
500
600
700
800
QGSJET01cEPOS 1.61SIBYLL 2.1QGSJETII.3
Energy [eV]1310 1410 1510 1610 1710 1810 1910 2010
[GeV]ppsEquivalent c.m. energy 310 410 510
TevatronLHC
accelerator data (p−p) + Glauber
(E/eV)10
log11 12 13 14 15 16 17 18 19 20
Mul
tiplic
ity
0
500
1000
1500
2000
2500
3000
Energy [eV]
1110 1210 1310 1410 1510 1610 1710 1810 1910 2010
Elasticity
total / EmaxE0 0.2 0.4 0.6 0.8 1
prob
abili
ty
0
0.01
0.02
0.03
0.04
0.05
0.06
eV19EPOS, protons at 10eV19QGSJET, protons at 10
eV19QGSJETII, protons at 10eV19SIBYLL, protons at 10eV19NEXUS, protons at 10
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Estimate Importance On Air Shower Interpretation
Modify specific features of hadronic interactions during air showerMonte-Carlo simulation:
◮ Assume logarithmically growing deviation from original modelprediction above 1015 eV.
◮ Below 1015 eV the original model is used.
◮ The parameter f19 denotes the nominal deviation at 1019 eV.
αmodified(E) = α
HE−model(E) ·(
1 + (f19 − 1) · log10(E/1 PeV)log10(10EeV/1PeV)
)
Where α can be:◮ Cross Section: σprod
had◮ Multiplicity: nmult
◮ Elasticity: kela = Eleading/Emax
◮ Pion-Charge Ratio: c = nπ0/(nπ0 + nπ+ + nπ−)
(R. Ulrich et al., submitted to PRD, arXiv 1010.4310 [hep-ph])
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Estimate Importance On Air Shower Interpretation
Modify specific features of hadronic interactions during air showerMonte-Carlo simulation:
◮ Assume logarithmically growing deviation from original modelprediction above 1015 eV.
◮ Below 1015 eV the original model is used.
◮ The parameter f19 denotes the nominal deviation at 1019 eV.
αmodified(E) = α
HE−model(E) ·(
1 + (f19 − 1) · log10(E/1 PeV)log10(10EeV/1PeV)
)
Where α can be:◮ Cross Section: σprod
had◮ Multiplicity: nmult
◮ Elasticity: kela = Eleading/Emax
◮ Pion-Charge Ratio: c = nπ0/(nπ0 + nπ+ + nπ−)
(R. Ulrich et al., submitted to PRD, arXiv 1010.4310 [hep-ph])
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Results for 〈Xmax〉
Proton Iron
19f0.2 0.3 0.4 1 2 3 4 5 6
]2
[g/c
mm
axM
ean
X
700
750
800
850
900
19f0.2 0.3 0.4 1 2 3 4 5 6
]2
[g/c
mm
axM
ean
X
700
750
800
850
900
◮ 〈Xmax〉 can be shifted significantly
◮ Data are suggesting◮ Intermediate mass, mixed composition, or:◮ Large cross section for a proton dominated composition◮ Small cross section for a iron dominated composition
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Results for 〈Xmax〉
Proton Iron
19f0.2 0.3 0.4 1 2 3 4 5 6
]2
[g/c
mm
axM
ean
X
700
750
800
850
900
19f0.2 0.3 0.4 1 2 3 4 5 6
]2
[g/c
mm
axM
ean
X
700
750
800
850
900Auger dataHiRes data
◮ 〈Xmax〉 can be shifted significantly
◮ Data are suggesting◮ Intermediate mass, mixed composition, or:◮ Large cross section for a proton dominated composition◮ Small cross section for a iron dominated composition
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Results for RMS(Xmax)
Proton Iron
19f0.2 0.3 0.4 1 2 3 4 5 6
]2
[g/c
mm
axR
MS
X
20
40
60
80
100
19f0.2 0.3 0.4 1 2 3 4 5 6
]2
[g/c
mm
axR
MS
X
20
40
60
80
100
◮ RMS(Xmax) mostly impacted by cross section, and elasticity
◮ Iron induced showers very robust
◮ Auger data only marginally compatible with protons in a high crosssection scenario
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Results for RMS(Xmax)
Proton Iron
19f0.2 0.3 0.4 1 2 3 4 5 6
]2
[g/c
mm
axR
MS
X
20
40
60
80
100Auger data
19f0.2 0.3 0.4 1 2 3 4 5 6
]2
[g/c
mm
axR
MS
X
20
40
60
80
100
◮ RMS(Xmax) mostly impacted by cross section, and elasticity
◮ Iron induced showers very robust
◮ Auger data only marginally compatible with protons in a high crosssection scenario
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Results for Muon Numbers
Proton Iron
19f0.2 0.3 0.4 1 2 3 4 5 6
QG
SII
µ/N µ
Rel
ativ
e N
0.8
1
1.2
1.4
1.6
19f0.2 0.3 0.4 1 2 3 4 5 6
QG
SII
µ/N µ
Rel
ativ
e N
0.6
0.8
1
1.2
1.4
1.6
cross sectionmultiplicityelasticitycharge ratio
◮ Multiplicity and Pion charge ratio are shifting model predictions
◮ Auger muon data incompatible with proton scenario
◮ Even for iron primaries: multiplicity must be high andpion-charge-ratio small
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Results for Muon Numbers
Proton Iron
19f0.2 0.3 0.4 1 2 3 4 5 6
QG
SII
µ/N µ
Rel
ativ
e N
0.8
1
1.2
1.4
1.6
19f0.2 0.3 0.4 1 2 3 4 5 6
QG
SII
µ/N µ
Rel
ativ
e N
0.6
0.8
1
1.2
1.4
1.6
cross sectionmultiplicityelasticitycharge ratio
◮ Multiplicity and Pion charge ratio are shifting model predictions
◮ Auger muon data incompatible with proton scenario
◮ Even for iron primaries: multiplicity must be high andpion-charge-ratio small
Caution: Definition of Muon number is not identical, e.g.:
Auger measures at 1000m, Simulations give total muon number
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LHC Data
as a benchmark for existing models
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Rise of Secondary Multiplicity
(T. Pierog)
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Rise of Secondary Multiplicity
(D. d’Enterria et al., to be published)
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Multiplicity Distribution
(D. d’Enterria et al., to be published)
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Pseudorapidity Distribution, NSD
(T. Pierog)
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Pseudorapidity Distribution, INEL
(T. Pierog)
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Average Transverse Momentum
(D. d’Enterria et al., to be published)Ralf Ulrich 30
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Extrapolation to GZK Energies
(D. d’Enterria et al., to be published)
⇒ Data at 14TeV are mandatory
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Interactions with Nuclei/Air
(T. Pierog)
Air Showers: p-Air, A-Air, π-Air, ...
⇒ not just p-p, but nuclei and nuclei combinations
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Forward Detectors
(TOTEM, ZDC, CASTOR)
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Forward Detectors
ηPseudorapidity -10 -5 0 5 10
[G
eV]
ηE
nerg
y flo
w d
E/d
0
200
400
600
800
1000
1200
1400
1600
1800 CMS HFCASTOR ZDC
Model predictions
⇒ Crucial for air showers is particle production in forward direction!
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Predicted Particle Production in Forward Direction
[GeV]hadE0 1000 2000 3000 4000 5000 6000 7000
had
dP/d
E
0
0.0002
0.0004
0.0006
0.0008
0.001
0.0012CASTOR (hadrons)
SIBYLL
QGSJET
EPOS
QGSJETII
[GeV]hadE0 2000 4000 6000 8000 10000
had
dP/d
E
0
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
0.45
0.5-310×
ZDC (hadrons)
chN0 10 20 30 40 50 60
chdP
/dN
0
0.01
0.02
0.03
0.04
0.05
0.06
0.07
0.08
TOTEM T2
(
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Impact of Modified Multiplicity
[GeV]hadE0 1000 2000 3000 4000 5000 6000 7000
had
dP/d
E
0
0.0002
0.0004
0.0006
0.0008
0.001
CASTOR (hadrons)SIBYLL, standard
2×eV)19(10mult
SIBYLL, n
0.5×eV)19(10mult
SIBYLL, n
[GeV]hadE0 2000 4000 6000 8000 10000
had
dP/d
E
0
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
0.45
0.5-310×
ZDC (hadrons)
chN0 10 20 30 40 50 60
chdP
/dN
0
0.01
0.02
0.03
0.04
0.05
0.06
0.07
0.08
TOTEM T2
(cf. Ulrich et al., submitted, arXiv:1010.4310v1 [hep-ph])
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Impact of Modified Elasticity
[GeV]hadE0 1000 2000 3000 4000 5000 6000 7000
had
dP/d
E
0
0.0002
0.0004
0.0006
0.0008
0.001
0.0012CASTOR (hadrons)
SIBYLL, standard
0.6×eV)19(10ela
SIBYLL, k
0.2×eV)19(10ela
SIBYLL, k
[GeV]hadE0 2000 4000 6000 8000 10000
had
dP/d
E
0
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
0.45
0.5-310×
ZDC (hadrons)
chN0 10 20 30 40 50 60
chdP
/dN
0
0.01
0.02
0.03
0.04
0.05
0.06
0.07
0.08
TOTEM T2
(cf. Ulrich et al., submitted, arXiv:1010.4310v1 [hep-ph])
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Potential Impact of LHC on
Interpretation of EAS Data
At the example of a precise measurement of the elasticity andCASTOR
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Relevance of CASTOR for Cosmic Ray Interpretation
Size
Heig
ht
air shower
X max
CASTOR
E [GeV]ΣTotal Energy 0 1000 2000 3000 4000 5000 6000 7000
EΣdP
/d
0
0.0002
0.0004
0.0006
0.0008
0.001
0.0012
SIBYLL, original
0.6×eV) 19SIBYLL, elasticity(10
0.2×eV) 19SIBYLL, elasticity(10
18 18.5 19 19.5 20
]2>
[g
/cm
max
<X
650
700
750
800
850
Energy [eV]
1810 1910 2010
SIBYLL, original 0.6×eV) 19SIBYLL, elasticity(10 0.2×eV) 19SIBYLL, elasticity(10
SIBYLL, original 0.6×eV) 19SIBYLL, elasticity(10 0.2×eV) 19SIBYLL, elasticity(10
Auger (PRL 2010)
proton, SIBYLL
iron, SIBYLL
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Impact of Elasticity / Leading Particles
18 18.5 19 19.5 20
]2>
[g
/cm
max
<X
650
700
750
800
850
Energy [eV]
1810 1910 2010
Auger (PRL 2010)
proton, SIBYLL
iron, SIBYLL
Without LHC
◮ Precise measurement of elasticity at 300GeV
◮ Extrapolation uncertainty grows by 10% per decade in energy
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Impact of Elasticity / Leading Particles
18 18.5 19 19.5 20
]2>
[g
/cm
max
<X
650
700
750
800
850
Energy [eV]
1810 1910 2010
Auger (PRL 2010)
proton, SIBYLL
iron, SIBYLL
With LHC
◮ Precise measurement of elasticity at 14TeV
◮ Extrapolation uncertainty grows by 10% per decade in energy
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Summary
◮ High energy models need tuning to data as close to the phase spacerelevant in air showers as possible
◮ Interaction characteristics has impact on air shower observables onthe same order of magnitude as as primary mass composition
⇒ Almost impossible to “measure” mass composition from air shower
observables in the moment
◮ If cosmic ray mass composition is constrained⇒ Air shower data sensitive to interaction physics up to ∼ 300TeV
So far:
◮ LHC data is well bracketed by cosmic ray models
◮ Cosmic ray community needs the data at 14TeV and high η
OutlookHelmholtz Young Investigator Group at KIT:CMS forward physics / Pierre Auger Observatory