Upload
hoai
View
40
Download
0
Tags:
Embed Size (px)
DESCRIPTION
Cosmic Ray Physics with the IceCube Observatory. Hermann Kolanoski Humboldt- Universit ä t zu Berlin and DESY for the IceCube Collaboration. IceCube Detector. Detector Completion Dec 2010. CR Analyses air showers in IceTop muon (bundle)s in IceCube atm. neutrinos in IceCube - PowerPoint PPT Presentation
Citation preview
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 1
Hermann KolanoskiHermann Kolanoski
Humboldt-UniversitHumboldt-Universitäät zu Berlin and t zu Berlin and DESYDESY
for the IceCube Collaborationfor the IceCube Collaboration
Cosmic Ray Physics Cosmic Ray Physics with the with the
IceCube ObservatoryIceCube Observatory
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 2
IceCube DetectorDetector Completion Dec 2010
IceCube with IceTop is a 3-dim Air Shower Detector
unprecedented volume
CR Analyses
•air showers in IceTop
•muon (bundle)s in IceCube
•atm. neutrinos in IceCube
•IceCube - IceTop coinc.
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 3
Energy range of IceCube/IceTop< PeV > EeV
Anchor to direct measurement of
composition ~300 TeV
Look for transition to extra-galactic <
EeV
(IceTop EAS)
(in-ice µ,ν)
Outline
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 4
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 5
Final IceTop Detector Array 2011
final detector:81 stations (162 tanks)
mostly ~ 125 m; In-fill array: 3 inserts +5 closest stations
In-fill
~125 m
Calibration: Vertical Equivalent Muons
1 VEM ≈ 125 PE
signal distribution in untriggered
calibration runs
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 6
IceTop Signal Recording
charge [PE]
volta
ge
time [ns]
leading edge
baseline
3.3 ns; 128 bins 420 ns
DOMs
snow height on tanksmuon signal
e.m. background
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 7
Trigger and Data SelectionSingle DOM above threshold (~0.2 VEM):
digitization of waveform (3.3 ns bins)
Local Coincidence (‘HLC hits’): both tanks above threshold
readout of full waveform to IceCube Lab
Soft Local Coincidence (‘SLC hits’):all DOMs above threshold send a timestamp and integrated charge
catch single muons
Single tank trigger for calibration with single muons
Reconstruction: standard ( 3 stations) 0.3 PeVinfill extension: 100 TeV
Select extended air showers:
Shower Size Spectrum with IT73
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 8
IT73 (90% of final) cos𝛉 > 0.8 A = 52×104 m2 >3 stations
10
100
1000events per bin
per year
(log10S125 = 0.05)
IT73 data(preliminary)
IT73 simulation
Work in progress
Effective Area
IceTop only
IC-IT coinc.
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube
IT73/IC79 configuration, >3 stations , cos𝛉>=0.8, A=0.52 km2
9
Cosmic Ray Spectrum
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 10
IceTop IT73 only:>5 stations cos𝛉>=0.8, A=52.1×104 m2
‘flattening’, also observed in IT26,
Kascade-G.
work on systematics in progress
CR Spectrum with IT26
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 11
preliminary
arXiv 1202.3039, submitted to ApP
CR Spectrum: Comparison with other Experiments
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 12
Cosmic Rays: spectrum and composition
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 13
IceCubes
ho
we
r a
xis
HE MuonsTeV’s
electro-mag. particles: MeV’s
LE MuonsGeV’sIceTop
IceCube/IceTop's Strength
EM
IN-ICE COMPOSITION SENSITIVE VARIABLES I
S125: shower size at the surface
K70: size of muon bundle in-ice
IceTopIn
-ice
Pure Iron
Pure proton
Neural Networkoutput
IC/IT40 Composition Analysis
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 14
FIRST ATTEMPT FOR COMPOSITION (IC40)
Preliminary
Preliminary
Preliminary
IC/IT40 Composition Analysis: Results
~ 1month of IC40 subarray (with little snow)
energy from 1 to 30 PeV (only)
systematics dominated
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 15
major progressexpected for the next
analyseswith larger detector
Submitted to Astrop. Phys.
separation power(expected to improve)
IN-ICE COMPOSITION SENSITIVE VARIABLES II
IT73/IC79 Composition Analysis
16
In-ic
e
IceTop
Muon stochastic loss
Avg. muon energy loss
for same deposited energy:
more stochastic loss
more HE muons lighter elements
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube
Exploit additional mass sensitive observables
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 17
Supporting Composition Measurements
1 VEM charge enhanced if
signalem signalmuon
Muon counting in air shower dataZenith angle dependence of shower size
Proton assumption
Iron assumption
IT26 spectrum analysis 1-100 PeV- arXiv:1202.3039
preliminary
preliminary
Surface muon content
simulation
PeV Gamma with InIce Veto against muons
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 18
HI column densities
IceTop shower with no activity in IceCube
upper limit E = 1.2 – 6.0 PeV (90% c.l.)
--- sensitivity E = 1 – 10 PeV (90% c.l.)
• sensitivity for E = 1 PeV (90% c.l.)
preliminary
PeV Gamma: Point source sensitivity
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 19
TeV-sources extrapolatedto 1PeV without cut-off
IceCube 5 year sensitivity to point sources
lowest declination reached by the Galactic plane
preliminary
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 20
Low energy transient rate variations from Sun, SN, GRB, ...
Since than: IceTop increased spectral sensitivity taking differential rates at multiple thresholds
[ApJ Lett 689 (2008) L65]Sun flare observation Dec 13, 2006:
rate increase at 2 different thresholds
Galactic CR Spectrum
• GOES spacecraft
GRB sensitivity: Large events but unmonitored part of the sky
GeV 10 ,200 ,cm erg10 oo25 EF
May 17, 2012 – GLE 71
H.Kolanoski - Cosmic Ray Physics with IceCube 21
MPE
SPE1
SPE2SPE3
IceTop Rates plotted here are averages of the four groups
shown above.
• ~1% enhancement in SPE1 & SPE2• Tiny enhancements in SPE3/MPE• Unusual slow decay or second phase
ECRS, July 3-8, 2012
Observations
preliminary
Cosmic rays in IceCube (deep ice)
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 22
High Energy Muons in the Deep Ice
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 23
muon bundlesingle HE muon
Nµ~A0.23 E0.77
Muon Multiplicity
Q3.
5 d
N/d
Q
Q ~ Nµ
Test composition models
10 TeV 10 EeV
enlarged energy range witout coincidence
Spectra from Muon Bundles
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 24
preliminary
preliminary
preliminary
room for prompt muons from charm?
Comparison to Poly-Gonato Model
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 25
Poly-Gonato (+G-H3a extra-galactic)
E1
.7-w
eig
hte
d
total (polygonato + extragal.)no efficiency correction included
heavier than iron(extrapolated from
low energies)
extragalactic
room for prompt muons?
Atmospheric
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 26
at high energies remaining background
for comic neutrinos
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 27
Cosmic Rays: High-pT muonsHigh-pT muons modeled by QCD simulation (π, K, c, …)
O(10 m)
> 135 m
bundle
LS muon
power law
exponential
pQCD
preliminary
preliminary
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 28
High-pT Muons: Zenith Angle Distribution
DPMJET
QGSJET
MC=data
strong disagreementfor QGSJET & Sybill
π
K
c
Zenith angle dependences:
• π, K interaction vs. decay competition
• prompt: no dependence larger K/π ratio and/or more prompt?
d > 135 m
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 29
Cosmic Ray Anisotropy Large Scale ─ Compared to Northern Sky
the orientation of the dipole momentdoes not correspond to the relative motion
in the Galaxy (Compton-Getting effect)
diffusive transport from nearby sources?observed small scale (10°) structures few pc distance
in-ice only
Cosmic Ray Anisotropy
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 30
IceCube
IceTop
• CR Rate ~ 10 Hz in IT81 (E > 100 TeV)
• ~3 x 108 events / year
• Sensitive to > 10-4 anisotropy
• CR Rate ~ 2 kHz in IC86 (E > 10 TeV)
• ~6 x 1010 CR events / year
• Sensitive to > 10-5 anisotropy
Measurements with IceCube and IceTop
Air showers in IceTop :
in principle much betterenergy resolution, binning limited by statistics
potential of including composition sensitivity
Muons in IceCube:
lower energy; larger zenith range;higher sensitivitiessmall scale structures
IC59 - 400 TeV
IC59 - 20 TeV
IT73 - High energy (~2 PeV), preliminary
Energy Dependence of CR Anisotropy
31
• Anisotropy changes in position, size
• Above 400 TeV there’s indication of an increase in strength.ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube
preliminary (IT73)
Summary
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 32
• Cosmic Ray energy spectrum (‚flattening‘ at ~ 23 PeV)
• CR composition (first coinc. results, different methods model test), PeV γ rays
• connecting direct measurements with dominantly extra-galactic CR
• physics of airshowers: high-pT muons, composition, K/π, charm, …
• transient events: heliospheric physics, GRB, …
• CR anisotropy in PeV range, likely increase with energy
IceCube/IceTop is a unique 3-dim Air Shower Detector
Results:
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 33
Backup Slides
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 34
35
ENERGY RESOLUTION
SNOW CORRECTIONS
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 36
Feb. 2012
cos
0 z
meas eSS
Snow corrected(in shower reco)
Events selected bycore location
CR Spectrum: Comparison with IT26 and IT40
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 37
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 38
Strategies of Composition Analyses
proton
N
X / g cm-2
earlier
e/m
μ
first interaction
observationN
X / g cm-2
e/m
μearlier
more
heaviernucleus
• IceTop & InIce
IceTop EM vs InIce MUON
• IceTop
- zenith angle of e.m. - curv. of shower front
- GeV-muons in IceTop:
• IceTop & Radio
(future?)- shower max. Xmax
Complementary methods
reduce model dependency~ 680 g cm-2
Big Coincident Event
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 39
CR Spectrum: Comparison with other Experiments
ECRS, July 3-8, 2012 H.Kolanoski - Cosmic Ray Physics with IceCube 40