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P. BernardiniSeptember 10, 2006
ARGO-YBJ experiment
andTeV gamma astronomy
ARGO-YBJ detector
Cosmic rays
VHE -astronomy
Conclusions
YangBaJing (Tibet, China)
High Altitude Cosmic RayLaboratory (4300 m a.s.l.)
Longitude 90° 31’ 50” EastLatitude 30° 06’ 38” North
Astrophysical Radiation Ground-based Observatory
-ray astronomy Gamma Ray Burst physics Cosmic Ray physics Sun and Eliosphere physics
Detector layout
10 Pads = 1 RPC (2.80 1.25 m2)
78 m
111 m
99 m
74 m
12 RPC = 1 cluster ( 5.7 7.6 m2 ) 8 Strips = 1 Pad
(56 62 cm2) 42 clusters
104 clusters130 cluste
rs
BIGPAD
ADC
RPC
Read-out ofthe charge induced on“Big Pads”
Layer (95% active surface) of
Resistive Plate Chambers (RPC),
covering a large area (5800 m2)
+ sampling guard ring
+ 0.5 cm lead as -converter
December 2004 42 clusters January 2006 104 clusters June 2006 130 clusters
guard-ring under construction
Fall 2006: 154 clusters in data-taking
lead transport by means of the new Tibetan railway
Summer 2007: fully operative
Time Resolution (ns)
1 ns level
t (ns) HV (kV)
7.3 kV
HV (kV)
RPC layout & performance
• Bakelite RPC (5 1011 m)• Operation in streamer mode• Ar (15%) Isobuthane (10%) TFE (75%)• Efficiency >95 % at 7.5 kV (10 kV at s.l.)• Time resolution ~1 ns
Off-line Time Calibration & Angular Resolution Real events are used to calibrate the detector
(offline procedure in agreement with sampling hardware procedure) Measured angular resolution (even-odd method) in agreement with expected resolution
after
befor
e
residuals
= 0.09 ns
Final configuration
Longitudinal EAS
development
(Corsika simulation)
Primary energy: 1000 TeV
Proton
Iron
Argo-YBJ altitude
Main detector features and performance
Resistive Plate Chambers (RPC) as active elements
Space information from Strips ( pixel 6.5 62 cm2 )
Time information from 8-strip Pads ( resolution 1 ns)
Large area ( 11000 m2 ) and full coverage ( 5800 m2 )
High altitude (4300 m a.s.l.)
Pointing accuracy ( < 0.5°)
Detailed space-time image of the shower front
Detection of small shower (low threshold energy)
Field of View and duty-cycle 100%continuous monitoring of
the skyin the range -10°< <70°
Operation modes
Shower mode
Detection of Extensive Air Showers (direction, size, core …)
Trigger requirement: minimum number of fired pads
20 fired pads on the central carpet: rate ~5 kHz
Aims :cosmic-ray physics (threshold : few TeV)VHE -astronomy (threshold ~300 GeV) search for gamma-ray bursts
Scaler mode
counting rate (n 1,2,3,4) for each cluster, averaged in 0.5 s
Aims: detector and environment monitorflaring phenomena (GRB, solar flares) with a threshold of few GeV
Detector Control System
RPC current Barometric pressure
Temperature
Relative humidity
Continuous monitor of many detector and site parameters
EAS arrival times• Agreement with Poissonian statistics• Dead time and spurious effects are under control
Distribution of time differencebetween consecutive events
Distribution of event-multiplicityin a time window of 1 s
Unprecedented
view of showers
74 m
60 m
90 m
120 ns
Cosmic rayswith ARGO-
YBJ
Measurements
Size as Hit multiplicity (pad & strip)
Analog read-out of RPC pulse charges
Lateral density profile
Shower space-time morphology
Angular distributions (azimuth, zenith)
..... Energy spectrum
Chemical composition
Proton cross section
Check of the hadron interaction models
.....
Flux vs strip size
Lateral density profile
By means of the RPC analog measurement, a further extension is possible up to thousand TeV31 m
3500 particles
35 m
Energy up to hundreds of TeV by using the strip size
~10% systematic error on Ns
Comparison of ARGO-data with JACEE and RUNJOB spectra
“Bridge” between direct and indirect measurements
Flux versus strip size
(data and simulations)
High space/time granularity permits unprecedeted studies
on the EAS phenomenology(different topologies and time structures)
Very energetic shower
Evidence of strong conical shape in small showers
showerfront
show
er a
xis
shower core
Study of the time thicknessof the shower front
conical fit Average time residuals vs distance from the core
resid
ual
(ns)
core distance (m)
200<Nhit<500
DataSimulation (1-30 TeV)with Corsika + QGSjet
Azimuth () distribution
Expected behaviour in the angular range where the overburden atmosphereincreases as 1/cos
xo vertical depth (606 g/cm2 at YBJ)
attenuation length of showers
Deviations from this behaviour (sec - 1 > 1) due to misreconstructed events andhorizontal air showers
/ xαwith
1θ sec α exp I I
0
0
Fit: I0 = (165 ± 9) s-1 sr-1
= 5.6 ± 0.1
k is determined by simulations (interaction model dependent),selecting energy and age ranges by means of the actualexperimental observables
Flux attenuation and p-Air cross section
x0
1secexp )( 0
0 xII
Measurement of the flux attenuation
for fixed energies (and shower ages)
p-Air p-p]/[104.2][
2
INT4
INT
cmgmb
k
Airp
p-Air cross section… ARGO-YBJ approach
This analysis is a first test of such technique… to be employed in unexplored energy regions
R70 radius of circle including 70% of hits
Event selection based on
(a) “shower size” as Nhit (pad multiplicity)
(b) core reconstructed in a fiducial area (30 x 30 m2)
(c) constraints on shower density profile and extension (R70 < 20 m)
data = (81.3 ± 0.6) g/cm2 data
= (76 ± 2) g/cm2
(sec -1) distributions
Full Monte Carlo simulation of proton showersCorsika + QGSjet, detector response,trigger and analysis chain used for real data
Energy
estimate
Nhit<500 Nhit>500
<Ep>= 3.67 ± 0.04 TeV <Ep>= 14.3 ± 0.2 TeV
QGSjet from with 104.2
][ ]/[ k
4
2
Airp
Airp mbcmg
MC = (75.4 ± 0.8) g/cm2 MC
= (71 ± 1) g/cm2
k-factor
evaluation
k = 0.96 ± 0.05 k = 0.97 ± 0.05
p-N cross section
Hit numbers <E> (TeV) k p-Air (mb) p-N (mb)
< 500 3.67 ± 0.04 0.96 ± 0.05 283 ± 15 40 ± 4
> 500 14.3 ± 0.2 0.97 ± 0.05 307 ± 20 47 ± 5
VHE gamma astronomy
Exciting results in -astronomyMany important discoveries from Imaging
Atmospheric Cerenkov Telescopes (HESS, MAGIC and so on)
new sources in the Galactic Plane (SNR, PWN …) source in the Galactic Center new Active Galactic Nuclei many sources have been
mapped (spectrum) SNRs as VHE -radiation sources and sites of cosmic-ray production
HESS survey of the Galactic plane
LSI+61 303Micro-Quasar
1ES1218 (z=0.18)New Source
PG 1553 (Z>0.25) New source
Some sources detected by MAGIC
Complementary measurements Sky survey looking for emission from unknown gamma-sources
Monitor variable sources (i.e. variable luminosity of Mrk 421)
Improve the sensitivity to flaring sources and GRB’s
Probe structures larger than Cerenkov telescope Field of View
Ground-based detectors with:
- large effective area- high angular resolution- duty-cycle close to 100%- wide Field of View
The energy threshold of sampling EAS arrays is too high (tens of TeV)
The high altitude and the full coverageallow to lower the energy threshold
large exposure(FoV time)}
MilagroWater-Cerenkov EAS
detector (2630 m a.s.l.)located near Los Alamos
5000 m2 pond with an external array of 175 water tanks
First PMT layer under 1.5 m of waterSecond PMT layer under 8 m of water (sensitive to hadronic component of the shower, used for background rejection)
HAWC
Cygnus Region
Mrk 421
Crab Nebula
Energy threshold ~2 TeV
Angular Resolut. ~0.5°
ARGO-YBj approach
Lower energy threshold as an effect of the altitude ( ~300 GeV)
Continuous monitoring of the entire overhead sky (FoV duty-cycle
100%)
Angular resolution (<0.5°)
Search for point-like or extended sources looking for flux excess in proper angular bins
Increase the flux sensitivity with the /h discrimination (space-time pattern of the showers)
Npad > 500 <E> ~ 20 TeV
West East
So
uth
N
ort
h Observed significance:
n = 3.9
Expected significance:
n = 4.0
The measured deficit size (0.6°±0.3°) is compatible with the simulated Moon
size (0.4°)
Observed event deficit compatible
with the expected one
The Moon shadow
Implementing /h discrimination (I)
The photon signal is statistically identified by looking for an excess,
from a given direction, over a background due to charged cosmic
rays
The study of the shower space-time pattern can allow /h
discrimination and then larger sensitivity
Encouraging results from
Multiscale analysis + ANN
Photon Shower Proton Shower
Implementing /h discrimination (II)
Results obtained with different algorithmsbased on the analysis of the shower imageMultiscale shower image analysis Shower topology and Lat. Dens. Funct.
/h discrimination
First results with 42 clusters
( 0.6 billion events in 1000 hours live time )
Mkn 421
Mkn 501Crab
The distributionof the standard deviations
do not show any excessfor this small sample
Search for GRB’sThe data collected in scaler mode (E > 1 GeV) are
analyzed searching for possible high energy tails of GRBs
The search is performed on satellite-triggered bursts
( Three sigma cut )
ARGO-YBJ
EAS-TOP
Chacaltaya
The ARGO sensitivity to GRB’s (42 clusters) Fluence limits for HETE/Swift observed GRBs
ConclusionsARGO-YBJ
The detector is almost completed (presently 130/154 clusters in data taking)
Data analysis shows good performance in shower reconstruction
First results in cosmic ray physics. Promising extension to unexplored Ep regions. In the future, check of the hadronic interaction models. Contributions to atmospheric neutrino study ?
-astronomy
The -sky is more and more crowded
Atmospheric Cerenkov and full-coverage EAS detectors are complementary to detect steady and transient, point-like and extended -sources, to discover where and how cosmic rays (and neutrinos) are produced
The contribution of ARGO-YBJ is beyond the corner