1 universita’ del salento facoltà di scienze mm.ff.nn time measurements with the argo-ybj...
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UNIVERSITA’ DEL SALENTOUNIVERSITA’ DEL SALENTOFacoltà di Scienze MM.FF.NNFacoltà di Scienze MM.FF.NN
TIME MEASUREMENTS WITH THE ARGO-YBJ DETECTORTIME MEASUREMENTS WITH THE ARGO-YBJ DETECTOR
Dott.ssa Anna Karen Calabrese MelcarneDott.ssa Anna Karen Calabrese Melcarne
Dottorato di Ricerca in Fisica XIX ciclo
Settore scientifico FIS/04
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OUTLINE
ARGO-YBJ as a ground-based detector
Timing calibration in EAS experiments (Characteristic Plane Method)
Characteristic Plane (CP) correction applied to ARGO-YBJ data
Physics results after calibration
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Cosmic Ray SpectrumCosmic Ray Spectrum
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Observation of Extensive Air Showers produced in the atmosphere by primary ’s
and nuclei
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High Altitude Cosmic Ray Laboratory @ YangBaJingSite Altitude: 4300 m a.s.l. , ~ 600 g/cm2
Site Coordinates: longitude 90° 31’ 50” E, latitude 30° 06’ 38” N
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Cosmic ray physics
• anti-p / p ratio at TeV energy• spectrum and composition (Eth few TeV)• study of the shower space-time structure
VHE -Ray Astronomy Search for point-like (and diffuse) galactic and extra-galactic sources at few hundreds GeV energy threshold
Search for GRB’s (full GeV / TeV energy range)
Sun and Heliosphere physics (Eth few GeV)
Main Physics GoalsMain Physics Goals
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Layer (92% active surface) of Resistive Plate Chambers (RPC), covering a large area (5600 m2)
+ sampling guard ring+ 0.5 cm lead converter
time resolution ~1 nsspace resolution = strip
10 Pads (56 x 62 cm2)for each RPC
1 CLUSTER = 12 RPC
78 m
111 m
99 m
74 m
BIGPAD
ADC
RPC
(43 m2)
ARGO-YBJ layoutARGO-YBJ layout
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RPC is suited to be used as element of a surface RPC is suited to be used as element of a surface detectordetector
RPC
PAD
Resistive Plate ChamberLow cost , high efficiency, highspace & time resolution (1 ns),easy access to any part of detector,robust assembling, easy to achieve>90% coverage, mounting withoutmechanical supports.
2850x1258mm2
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Detector performancesDetector performances
good pointing accuracy (less than 0.5°)
detailed space-time image of the shower front
capability of small shower detection ( low E threshold)
large FoV (2) and high “duty-cycle” (100%)
continuous monitoring of the sky (-10°< <70°)Impossible for Atmospheric Cherenkov telescopes
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Full space-time reconstruction
Shower topology
Structure of the shower front
A unique way
to study EAS
74 m
60 m
90 m
150 ns
50 m
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Study of the EAS space-time structureStudy of the EAS space-time structure
The High space-time granularity of the ARGO-YBJ detector allows a deep study of shower phenomenology
with unique performance
Example 1: Very energetic shower
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Arrival Direction ReconstructionArrival Direction Reconstruction
Conical Fit
2E
PE
PE0
PP
2 )mc
yl
c
xtt(
EEEEEE sinsinm and cossinl
2PE
PE
PE0
PP
2 )c
Rm
c
yl
c
xtt(
Planar Fit
In EAS experiments for an event E the time tEP can be measured on each fired detector unit P, whose position (xP,yP) is well known
Primary direction cosines
angle azimuth
angle zenith
E
E
This quantity is not a proper 2 . Indeed the measurement unit is ns2
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Timing CalibrationTiming Calibration
P= residual correction + systematic correction
•Residuals correction reduces the differences between fit time and measured time
•Systematic correction guarantees the removal of the complete offset
Taking into account the time offset P typical of the detector unit
PEPEE0PEP ymxl)tΔt(c Plane-equation
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The air shower arrival directions have the following distribution:
.constd
dN
The systematic offset introduces a quasi-sinusoidal modulation in azimuth distribution
l0=sin0cos0 and m0=sin0cos0 disform the original angular distribution
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Characteristic Plane (CP) Definition
Fake Plane (FP)
PEPEE0PEP ymxl)tΔt(c Real Plane (RP)
P'EP
'E
'E0
resPEP ymxl)tt(c
resPE0
PPP c
yb
c
xaΔ On average
E0'
E0E0E'EE
'E tt mmb lla
Assuming uniform azimuth distribution
'E
'E mb and la
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CP Method Checks (Fast MC simulation)
Azimuth distribution before calibration Azimuth distribution after calibration
Time offsets introduced in the time measurement CP correction removes the time offsets
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CP method works also when a pre-modulation on primary azimuth angle is present
The CP method annulls <l> and <m> leaving a sinusoidal modulation on the distribution of the new ’’ azimuth angle
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Residual correction has been applied twice and systematic correction has been
applied according to the values:
A Gaussian fit is applied in the range ±10 ns around the bin with maximum number of entries
ARGO-YBJ DATA(ARGO-42, ARGO-104, ARGO-
130)
4'4' 1067m and 10304l
c
ym
c
xlΔ P'
EP'
EresPP
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Correction
Residuals after correction
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Effect of conical shape of the shower front
planar fit
Conical shape
FULL SIMULATION
Corsika+ARGOG codes
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CP method with conical correction
PE0
pE
PEEP
resP R
ct
c
ym
c
xlt
t
Planar residual after CP conical correction
Conical residual after CP conical correction
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Geomagnetic field effect
In the geomagnetic field, the secondary charged particles generated in EAS are stretched by the Lorentz force
2e
2
cosE2
sinBhd Average shift in the shower
plane for a secondary electron
electrons ofenergy average E
North) magnetic 0(shower theof angleazimuth
shower theof anglezenith
ninclinatio cgeomagneti
cos sinsincoscosacos
field cgeomagneti B
rajectoryelectron t theofheight verticalaverage h
e
H
HH
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θcos
χsing
2
YBJ - the geomagnetic effect is stronger for showers from North than for showers from South
This difference is more evident for larger zenith angles
H = 45° at ARGO-YBJ
15°
35°
45°
55°
cos sinsincoscos acos HH
=
=
North South
=
=
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Estimate of South-North asymmetry: MC
)]4p2cos(3p)2pcos(1p1[0pd
dN
N events from North (161.5º < Φ < 341.5º )
S events from South (161.5º >Φ and Φ >341.5º)
%1NS
NS2
Tibet AS estimate 2.5% higher rate from South direction with respect to North direction (geomagnetic field effect + slope of the hill where the array is located)
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Estimate of South-North asymmetry: Data
As expected CP method annulls the mean values of the primary direction cosines but a small sinusoidal modulation is still present in azimuth distribution
The mean values of direction cosines after CP correction are
1.0% 0.9%
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TDC peaks distribution
Before correction
After correction
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TDC method to update the calibration
TDC peak distribution after calibration has a regular concave shape
Without hardware change and with the same trigger, the concave surface should remain unvaried
On the other hand ….
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TDC peak dependence on temperature (night-day difference)
A collective shift (~3 ns) is observed.
Method odd-even events
The main effect of the TDC dependence on temperature is a shift of all TDC peaks, negligible for calibration and a minor effect is present but it is of the order of 0.2 ns
C4ΔT
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TDC dependence on offline CLUSTERs
The effect of offline CLUSTERs is visible only in peculiar conditions, thus this effect on the TDC calibration is negligible
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Angular Resolution
MC/data
Chess board method
72 parameter : the value in the angular distribution which contains ~72 % of the events
The residual correction improves the angular resolution
Even/Odd
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Moon shadow: absolute pointing
The systematical correction improves the absolute pointing
Significance map of the Moon shadow selecting events with a number of fired pads > 500 (~ 5 TeV median energy) and with zenith angle of the incident direction < 45°. 558 hours of observation.
)TeV(E
Z1.5Δ
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Time structure of EAS front
The curvature (Td) of the shower front as the mean of time residuals with respect to a planar fit
The thickness (TS) of the shower front as RMS of time residuals with respect to a conical fit
Shower curvature
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COMPARISON DATA-simulation
SIMULATION
COMPARISON proton-photon
Shower thickness
Shower thickness
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Conclusions
Characteristic Plane calibration has been defined and studied
Calibration with planar and conical fit for ARGO-42, ARGO-104, ARGO-130
Fast TDC calibration
South-North azimuthal asymmetry studied with full simulation
Improvements in the angular resolution and absolute pointing
Study on time structure of the shower front
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Papers
• G.Aielli et al., Nucl.Instr. And Meth., A562 (2006) 92• H.H.He, P.Bernardini, A.K.Calabrese Melcarne, S.Z.Chen, ”Detector Time
Offset and Off-line Calibration in EAS Experiments”, Astroparticle Physics 27 (2007) 528-531
Conferences and proceedings
• A.K.Calabrese Melcarne, “Time Calibration of the ARGO-YBJ detector”, *Cividale 2005 High Energy Gamma Ray Experiments*, 183-187
• P.Bernardini et al., “Time Calibration of the ARGO-YBJ experiment”, 29th International Cosmic Ray Conference, Pune 2005, 5-147
• A.K.Calabrese Melcarne, “Calibrazione del rivelatore ARGO-YBJ”, XCII Congresso Nazionale Societa’ Italiana di Fisica, atticon3408 III-C-39
• B.Wang et al., “Preliminary results on the Moon shadow with ARGO-YBJ”, 30th International Cosmic Ray Conference, Merida 2007, Mexico
• A.K.Calabrese Melcarne, I.De Mitri, G.Marsella, L.Perrone, G.Petronelli,A.Surdo, G.Zizzi , “Study of cosmic ray shower front and time structure with ARGO-YBJ”, 30th International Cosmic Ray Conference, Merida 2007, Mexico
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ARGO internal notes
Note 2004/02 • P.Bernardini, A.K.Calabrese Melcarne, C.Pino, “Time calibration of six Cluster”
Note 2005/02• P.Bernardini, A.K.Calabrese Melcarne, C.Pino, “Time-Calibration of the ARGO-YBJ detector (42 Clusters)”
Note 2006/03• P.Bernardini, A.K.Calabrese Melcarne, I.De Mitri, G.Mancarella, “Study of the arrival times of cosmic rays”
Note 2006/04• S.Z.Chen, A.K.Calabrese Melcarne, H.H.He, P.Bernardini, B.G.Sun, F.R.Zhu,”Characteristic Plane Method with Conical Correction”
Note 2006/05• P.Bernardini, A.K.Calabrese Melcarne, G.Mancarella, M.Khakian Ghomi, “Analysis of shower clusters”
Note 2007/03• A.K.Calabrese Melcarne, S.Z.Chen, P.Bernardini, H.H.He, “Conical Calibration for 130 Clusters and automatic updating”