at the p ierre a uger o bservatory as measured w ith ... · instituto galego de física de altas...
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The Cosmic Ray Spectrum above 4 EeVas measured with inclined showers recorded at the Pierre Auger ObservatoryHans P. Dembinski1 for the Pierre Auger Collaboration2
1 IEKP, KIT Karlsruhe, Postfach 3640, D-76021 Karlsruhe, Germany2 Observatorio Pierre Auger, Av. San Martín Norte 304, 5613 Malargüe, Argentina
(Full author list: http://www.auger.org/archive/authors_2011_05.html)
Enrique Zas
Instituto Galego de Física de Altas Enerxías
(Universidad de Santiago de Compostela)
1st IGFAE/LIP Workshop Braga 5th May 2018
Cosmic ray showers and neutrinos at the Pierre
Auger Observatory
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Pierre Auger Observatory
3000 km2
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TA
Auger
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TA
Auger
Designed to find the sources of UHECRsMeasuring spectrum Arrival directions Composition
with unprecedentedprecision
In addition we have shown that
it is good to search for UHE ns
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Spectrum
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Isotropic Fluorescence light
from nitrogen
(~4 g per meter of track)
Particle array
Fluorescence
TA and the Pierre Auger
Observatory are Hybrid:
Combine the two
succesful techniques
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TA SD 2013
4,580 km2 sr y
Auger SD
40,000 km2 sr y
Four independent spectra
x (km)-30 -20 -10 0 10
y (k
m)
-5
0
5
10
15
Graph
Event Id: 11549518
= 59.7619N° 0.04± ° = 161.11f, ° 0.04± ° = 81.18q
X = 3744.18 m, Y = 3668.25 m = 0.66dof/n2c
Example Event (48°, E~70 EeV)
“Vertical” < 600 1500/750 Hybrid
Inclined 600-800
SD
FD+SD
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Combined Results
F. Fenu; Proc. of ICRC 2017, PoS (2017) 486.
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3.9 σ discrepancy
(broken power law fit)
Not due to biases in
energy or exposure
Common declination
band agreement
same break points
TA Auger: anisotropy issues?
Auger TA
different d
same d
TAAuger
3.9 σ
D. Ivanov; Proc. of ICRC 2017, PoS (2017) 498.
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[deg]d-80 -60 -40 -20 0 20 40 60 80
)d(w
0.0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
1.6
1.8
Normalized exposure for Auger South site
°<60q
°<80q<°60Auger
Auger
q<600
TA
Sky coverage
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Auger Collab. Science 2017) 357 (2017) 1266-1270
Anisotropy searches: dipole E>8 EeV!
• More details to appear soon
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Starburst Galaxies → 390
f = 10%, ψ = 130
pre-trial p-value: 4 × 10−6�post-trial p-value: 4 × 10−5��post-trial significance: 3.9 σ��
AGN Swift-BAT Catalogue → 600
f = 7%, ψ = 70
pre-trial p-value: 5 × 10−4�post-trial p-value: 3 × 10−3��post-trial significance: 2.7 σ��
Other signs of smaller angle correlations
Highest Energy CR
and g ray sources, particularly
Star Burst Galaxies
NGC4045
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Multi-messenger: Neutrino search potential
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O(800 g cm-2)
µ
Typical air shower
Xma
x
CR
CRn
ntt
µ860 g cm-2 ATMOSPHERE
EARTH
Suitable for EeV n search
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CR
CRn
ntt
µ860 g cm-2 ATMOSPHERE
EARTH
O(800 g cm-2)
µ
Typical air shower
Xma
x
Suitable for EeV n search
Neutrino: Inclined air shower with broad component
“Young” shower Broad pulse
“Old” shower Narrow pulse
Sig
na
l (V
EM
)
Sig
na
l (V
EM
)
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Three search categories (different flavor sensitivities for ES and DG):
- (1) ES Earth skimming tau neutrinos
Between 900 and 950 (upcoming)
Decay early
- DG Atmospheric interactions (q > 600 Xatm
> 1700 g cm-2)
+ (2) DGL 600<q<750
+ (3) DGH 750<q<900
To trigger SD array
All n NC & nµ CC 20% energy to shower
neCC 100% energy to shower
ntCC 20% to shower #1 50% to shower #2
CR
16
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<AoP> = mean value of Area-over-Peak in
event
backgro
und
Earth Skimming searchMost sensitivity [0.2 - 2] EeV practically excluded to zeniths [900
- 950]
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ES 79.4%
DGH 17.6%
DGL 3.0%
ne
10.1%
nµ 3.8%
nt
86.1%
Relative contributions (E-2 1ux)
Combined
ES
DGH
(750<q<900)
DGL (600<q<750)
Phys. Rev. D 91, 092008 (2015); Ap JL 755:L4 (2012)Exposure etot(En)
1 Jan 04 – 31 Mar 17
Very sensitive to ES nt
CHANNELS
FLAVOURS
E. Zas; Proc. of ICRC 2017, PoS (2017) 972.
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J. Alvarez-Muñiz Highlight talk
ICRC2017
flavor ratio
(1:1:1)
Limits to di+use ,ux
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Search for UHEn in coincidence with Gravitational Wave events with Auger
Gravitational Wave events (GW150914 & GW151226)
detected by Advanced-LIGO detectors (also LVT151012
candidate):- Inferred source: merger of binary black-hole at D = 410 &
440 Mpc- ~ 3 & 1 solar masses released in the form of GW- Position in the sky uncertain: few 100 deg2
20
LIGO & Virgo Collab. Phys. Rev. Lett. 116, 061102 & 241103 (2016)
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Instantaneous coverage
Sensitivity limited to
large zenith angles =>
Instantaneous sky
Coverage is limited
BUT: Covered region
has excellent
sensitivity to ES nt
(Surface area >> Ice3)
i.e. GW150914, GW151226, GW170104 (& LVT151012)
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Limits to radiated n energy Pierre Auger Collab., Phys. Rev. D 94, 122007 (2016)
22GW150914 and LVT151012 similar constraints, GW170114
weakerGW150914 and LVT151012 similar constraints, GW170114
weaker
GW151226 (1 day steady): E< (0.5, 3 solar masses) for -550 < d < 570
GW151226 (1 day steady): E< (0.5, 3 solar masses) for -550 < d < 570
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NS coalescence: A leap in Science
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SKY MAP 170817
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The Pierre Auger Observatory has a rich program in which the
IGFAE group is actively involved
I have selected recent results that are particularly relevant
Reconstruction and spectrum measurement leading to:
The discovery of Large Scale Anisotropy
Signs of smaller scale anisottropies: SBG
The potential as a neutrino detector
Role in GW detection of BH mergers
Constraints of neutrino fluxes in GW170817
Summary
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Thank you