[a]Thomas P. Armstrong

# Monte Carlo Simulations and Validation of NectarCAM, a Medium Sized
Telescope Camera for CTA

Heide Costantini  Jean-François Glicenstein  Jean-Philippe Lenain  Ullrich
Schwanke  Thomas Tavernier

###### Abstract

The upcoming Cherenkov Telescope Array (CTA) ground-based gamma-ray
observatory will open up our view of the very high energy Universe, offering
an improvement in sensitivity of 5-10 times that of previous experiments.
NectarCAM is one of the proposed cameras for the Medium-Sized Telescopes (MST)
which have been designed to cover the core energy range of CTA, from 100 GeV
to 10 TeV. The final camera will be capable of GHz sampling and provide a
field of view of 8 degrees with its 265 modules of 7 photomultiplier each (for
a total of 1855 pixels). In order to validate the performance of NectarCAM, a
partially-equipped prototype has been constructed consisting of only the inner
61-modules. It has so far undergone testing at the integration test-bench
facility in CEA Paris-Saclay (France) and on a prototype of the MST structure
in Adlershof (Germany). To characterize the performance of the prototype,
Monte Carlo simulations were conducted using a detailed model of the 61 module
camera in the CORSIKA/sim_telarray framework. This contribution provides an
overview of this work including the comparison of trigger and readout
performance on test-bench data and trigger and image parameterization
performance during on-sky measurements.

##  1 Introduction

CTA is the next generation of ground based imaging atmospheric telescopes,
representing the move from current experiments to a full observatory. With its
two arrays covering both hemispheres, it will provide an order of 5-10 times
improvement in sensitivity. Using three different sizes of telescope, it will
be able to observe gamma rays with energies between 20 GeV to over 300 TeV.
The bulk of this energy range will be met with the 12 m diameter Medium Sized
Telescope (MST). NectarCAM is one of the proposed cameras which will be
mounted on the MST [1]. Its concept is based on a modular design, where a
module consists of 7 photomultiplier tubes (PMTs) and an associated set of
readout and trigger electronics. The full camera will consist of 1855 PMTs
providing an 8 degree field of view. The readout is based on the NECTAr ASIC
which is able to store data in a circular buffer with GHz sampling until the
camera is triggered (resulting in a 60 ns readout window). The camera has two
gain channels with the nominal voltage able to measure the single photo-
electron (p.e.) level and a higher gain providing a dynamic range up to 2000
p.e. (with a linearity of 5%).

The trigger logic of NectarCAM uses a multi-level scheme in order to reduce
the number of random triggers from noise, while maximising the number of
shower images recorded. In the first step, or the Level 0 (L0) trigger, a copy
of the analog signal from an individual pixel is sent to the L0 ASIC, where
the signal is compared to a programmable voltage threshold using a
discriminator circuit. The output of the discriminator consists of gate pulse,
reshaped to a programmable gate width at the trigger FPGA which also handles
the Level 1 (L1) trigger fabric. The L1 trigger is based on the processing of
L0 signals of overlapping 37-pixels regions, where the signal from each
7-pixel module is shared with its 6 neighbours. Several trigger algorithms can
be implemented, but the default 3 Nearest Neighbours (3NN) is currently used
in NectarCAM.

A first demonstrator prototype of NectarCAM has been constructed and
evaluated. Consisting of only the central 427 PMTs, this prototype has
facilitated full testing and validation of the camera concept. The majority of
the tests have been carried out at the CEA Paris-Saclay dark room test bench
(France), a 12 m long dark room which is equiped with a LED pulser and
continuous Night Sky Background (NSB) emulating light. To allow further tests,
including integration with the telescope structure, the demonstrator was
mounted on the prototype MST located in Adlershof (Berlin, Germany) where on-
sky observations were carried out.

The performance of CTA is estimated using Monte Carlo (MC) simulations of
particle air showers produced by gamma rays and background protons and
electrons. The response to the resulting Cherenkov light through the telescope
optics and camera electronics therefore needs to be well understood. A large
effort has gone into ensuring the models for each telescope are accurate,
through performing matching simulations to tests carried out in the lab and
on-sky. In this paper, a summary of the results from this process with
NectarCAM will be presented, covering dark room tests in Section 2 and on-sky
tests in Sections 3.

##  2 Simulation of Test Bench

For the work presented in this paper, the simulation software CORSIKA (v6.9)
and sim_telarray (2018-11-07) are used [2, 3]. A light source similar to the
LED flasher is implemented in the simulations including the wavelength (405
nm), the light pulse shape (Gaussian with a standard deviation of 0.64 ns) and
the angular distribution (flat response over 11.4 degrees opening angle). The
model for the camera used in the sim_telarray simulations was updated with
various lab measurements and design specifications. Some model parameters were
adjusted during the comparisons presented in this section and are mainly
parameters which are difficult to measure directly in a lab. While there are
many intermediate results in the validation process, the two main outcomes
presented here are the validation of the readout in terms of the intensity
resolution, and the matching of the trigger performance for both the L0 and L1
stages.

###  2.1 Verification of Readout Performance

Figure 1: The derived intensity resolution for nominal NSB ($\sim$250 MHz) in
blue and high NSB ($\sim$1GHz) in orange, where the ranges are due to the
uncertainty of the NSB test bench source. Also shown is the CTA requirements
on the intensity resolution for these two levels.

The reconstructed charge was studied at the CEA dark chamber with a LED
flasher and the NSB source. Before the measurement was made, the linearity of
the response was tested and the cross-talk between pixels was measured to be
negligible. Data were taken at a range of values of NSB between 0 - 1 GHz. The
data were calibrated using the pedestals obtained without light sources (dark
events) and the measured gain derived from the single p.e. spectrum, obtained
using the method described in Ref. [4]. For the simulations, a data set of a
1000 events was created for each illumination in the range of sub p.e. to
greater than 2000 p.e.. The camera simulation was performed with a range of
NSB values chosen in the same range as the data. The gain and pedestal values
are generated automatically by sim_telarray.

Both the data and the simulations were processed using the prototype
processing pipeline for CTA, ctapipe (version v0.8.0) [5], where the charge
was extracted using an integration window of width of 16 ns starting 6 ns
before the peak of the signal. This was chosen to encompass the full pulse
width recorded in the waveform. In order to include the effect of the photon
detection efficiency (PDE) in the results, the values in p.e. were converted
back to photons, using a conversion factor of 3.73 ph p.e.-1 derived from the
total camera efficiency at 405 nm (the wavelength of the flasher). The
intensity resolution was then calculated, using the expression

$\frac{\sigma_{I}}{I}=\frac{\sqrt{\frac{1}{N}\Sigma_{t=1}(I_{rec,i}-\bar{I}_{rec})^{2}}}{\bar{I}_{rec}},$
(1)

where $I_{rec,i}$ is the intensity measured for the $i$th event and
$\bar{I}_{rec}$ is the mean over events. This form of intensity resolution
does not take into account any bias present in the reconstruction. This
requires an absolute calibrated light source which was not available. The
results for two separate NSB regimes are shown in Figure 1, where these
represent the nominal dark sky conditions and high NSB conditions. From here
it can be seen that the simulations and data match well, providing confidence
in the model constructed for the camera.

###  2.2 Verification of Trigger Performance

|
---|---
Figure 2: Left: L0 threshold as a function of illumination, where the black
lines represent the dispersion of measurements from different pixels taken in
the lab and the blue is the simulations. Right: The difference between the L1
50% trigger threshold values for data and simulations for the same
illumination.

The trigger efficiency was studied with the same dark chamber set up as with
the readout study but excluding the use of the NSB source. The gains of each
pixel were ajusted based on flat fielding measurements. For each illumination,
data were recorded with a range of trigger threshold levels ensuring that the
transition from 100% to 0% trigger rate was recorded. For the simulation, a
dataset of 1000 events was created for each illumination level and trigger
threshold from sub p.e. to $\sim$40 p.e., the same used in the test bench, and
the trigger efficiency was recorded.

In a first step, only the performance of the L0 trigger was considered, i.e.
the trigger efficiency of each pixel separately. In each scan, the trigger
threshold which provided a 50% trigger efficiency was recorded. The results
are shown in the left panel of Figure 2 where it can be seen that the
relationship between expected light level in p.e. and the L0 threshold in
digital counts at 50% trigger efficiency matches the data very well.

In a second step, simulations were performed using a single module of 7 pixels
with a 3NN (next neighbours) trigger condition in order to evaluate the L1
performance. The right panel of Figure 2 shows the comparison of the L1
threshold at 50% trigger efficiency for data and MC with matching illumination
levels. It can be seen that the trigger level matches well (within 5%) further
providing confidence in the simulation model.

##  3 Simulation of Test Observations at Adlershof

Figure 3: Left: Wavelength dependent efficiency model parameters, including
the quantum efficiency, the mirror reflectivity, the UV Pass filter along with
the total convolved efficiency. Middle: Example image of star from which the
on-sky PSF was extracted. A non-smooth distribution of light is present due to
misaligned mirror segments. The blue circle is the 80% containment radius, the
green lines denote the ring used for background subtraction; the yellow (solid
+ dashed) circles denote two different ways to estimate the centre of gravity.
Right: An image of the baffle mounted in front of the camera in order to
reduce the NSB.

In May and June of 2019, tests were performed with the NectarCAM demonstrator
mounted on the MST prototype structure in Adlershof. While the main goal was
to perform integration tests, several changes were implemented to reduce the
NSB contribution from the surrounding light pollution, resulting in the
successful observation of air-shower events. To test the model constructed for
the camera in realistic conditions, simulations were performed to compare to
the air-shower data observed. However, before this could be done, several
changes had to be made.

  * •

UV Filter - To help reduce the level of NSB, a UV Pass filter was placed in
front of the camera. The transmission as a function of wavelength can be seen
in the left panel of Figure 3 along with the PDE, mirror reflectivity and
total transmission (values obtained through measurements or from manufacturer
specifications).

  * •

Mirror Layout - Missing mirror facets at the time of observations were removed
from the model (18 out of 86). In addition the mirrors had begun to show signs
of degradation due to their prolonged exposure to the environment at
Adlershof. This will be evaluated when comparing the observed proton rate of
the telescope (See Section 3.1).

  * •

Point Spread Function - The PSF was measured on site using a white target in
front of the focal plane and a CCD camera mounted on the telescope structure.
Images of stars were taken and the 80% containment angle was measured. The
average value obtained was 0.218 deg, about three times worse than expected
due to the non-smooth distribution of light in the image, most likely
originating from misaligned mirrors (see middle panel of Figure 3). The
spread, but not the structure, was matched in the simulations.

  * •

Shadowing - In addition to the UV filter, a baffle was also mounted on the
camera to reduce the amount of background light entering the camera, as can be
seen in the right panel in Figure 3. The effect of this on the shadowing on
the camera was evaluated using the ray tracing software ROBAST [6].

For the CORSIKA site simulation, the following parameters were adopted:
Altitude of 37 m; MODTRAN atmospheric transmissivity model for tropical
atmosphere; NRLMSISE-00 atmospheric density and refractive index model for CTA
northern site; Magnetic field strength of H = 18.450 $\mu$T and Z = 45.351
$\mu$T, calculated from the Latitude and Longitude of the site location of
$\phi=52.43^{\circ}$ N, $\lambda=13.54^{\circ}$ E and British Geological
Survey World Magnetic
Model.111http://www.geomag.bgs.ac.uk/data_service/models_compass/wmm_calc.html
While the atmospheric models are clearly not tuned to the site in Adlershof,
they were the available models that extended to sea level. The simulated
initiating particles were protons as it is expected that only background
events were observed.

###  3.1 Threshold Scan Comparison

---
Figure 4: Threshold scan for data in red and simulations in blue. For the MC
simulation a range of NSB values is shown and only one mirror reflectivity
value is shown (60%). The data matches well to a NSB rate between 0.2 and 0.3
GHz (NSB rates provided in the legend).

During the on-sky tests at Adlershof, one of the frequent measurements was
that of the threshold scan. This is a series of measurements of the trigger
rate as a function of trigger threshold, similar to that performed in Section
2.2, which would be used to choose a safe observational trigger level. For
this study, three on-sky runs that were carried out under similar
observational conditions were used (pointing at dark sky spot, open shutter,
nominal HV, internal trigger).

For the simulations, the trigger rate from proton showers and NSB have to be
calculated separately. For this study $1.25\times 10^{6}$ proton showers were
simulated with CORSIKA between the energy range of 80 GeV and 50 TeV with an
energy spectrum of $E^{-2}$. Showers were set to originate from a field of
view of radius 10∘ centered 20∘ from zenith and were scattered at observation
level in an area of 600 m radius. For the telescope simulation, the model used
in Section 2 was adopted with the changes reported at the start of this
Section. In addition, the NSB rate, the mirror reflectivity (degradation), and
the trigger threshold were varied to find matching values to the data.

The proton rate is calculated by finding the trigger efficiency as a function
of energy and using the following expression,

$R_{\mathrm{proton}}=S\cdot\Omega\int_{E_{min}}^{E_{max}}\phi(E)\cdot\frac{N(E)_{trig}}{N(E)_{sim}}~{}dE,$
(2)

where the simulated area is defined as $S=\pi r^{2}$ with r = 600 m and the
simulated solid angle as $\Omega=2\pi\cdot(1-\cos(\theta))$ with $\theta=10$
degrees. The proton flux, $\phi(E)$, was taken from Ref. [7] and is defined as
$\phi(E)=9.6\times 10^{-2}\cdot\left(E/TeV\right)^{-2.70}\textrm{
TeV${}^{-1}$~{}s${}^{-1}$~{}m${}^{-2}$ sr${}^{-1}$}.$

For the NSB simulation, a CORSIKA file containing $10^{5}$ events with no
Cherenkov light is used. The rate is calculated using ratio of triggered
events to an equivalent simulated observation time, determined by the number
of simulated events and the width of the readout window. Once the proton and
NSB rates are determined, they are added to obtain the complete threshold
scan. The results of this can be seen in Figure 4 where it was found that a
mirror degradation down to 60% was required to match the proton spectrum. This
might not all be due to the weathering of the mirrors, but could also
encompass loss of efficiency in other parts of the system or the use of not
ideal atmospheric models. Ideally for a more reliable result, images from muon
rings are used to measure the total throughput efficiency, however not enough
events were recorded for this analysis. For the NSB it was found that a value
of 0.3 GHz was required to match the data. This value is in agreement with
measurements that were taken earlier in the campaign.

###  3.2 Hillas Parameter Comparison

With updates to the telescope model obtained in the previous sections, a full
simulation was performed using $25\times 10^{6}$ proton showers between 80 GeV
and 100 TeV. The on-sky data were calibrated using per pixel gain measurements
recorded in the lab. Although interleaved pedestals were available for some of
the data sets, for simplicity they were instead estimated from the average
over the events for each run, using the first 10 samples in each waveform. The
data were processed with ctapipe [5], where the charge was extracted and the
images were cleaned using a two-level threshold, where only core pixels with
at least 10 p.e. and any boundary pixels with at least 6 p.e. were kept,
discarding any images that had less than 4 pixels remaining.

Figure 5: Comparison of selected Hillas parameters. The results from the
simulation have been re-weighted to the assumed background proton spectrum
from [7] and the rate per bin has been calculated for each set of results.

For both MC and data, the cleaned images were fit with an ellipsoid in order
to extract the Hillas parameters [8] and the distributions were normalised to
the expected rate. For the simulations, equation (2) was used to determine the
rate. For the on-sky data the rate was calculated using the observation time
of 26.65 min. In addition, simulated events are weighted before the
construction of the histograms as
$\frac{\phi_{p}}{\phi_{mc}}E^{\Gamma_{p}-\Gamma_{sim}}$ where $\Gamma_{p}$ is
the assumed proton spectral index (-2.7), $\Gamma_{sim}$ is the simulated
spectral index (-2), and $\phi_{mc}$ is the simulated flux normalisation. The
resulting distributions can be seen in Figure 5, where a good agreement is
found.

##  4 Conclusion

In this paper an overview of the main results produced during the model
validation of NectarCAM has been shown. Concerning the comparison of results
from the lab tests, both the readout and the trigger show good agreement. For
the on-sky results, even though the conditions were not ideal for the
observation of Cherenkov air-showers, an agreement was found through the
scaling of the NSB (to 0.3 GHz) and the mirror degradation (down to 60% of the
original model). From these results, it is concluded that a good understanding
of the camera has been achieved.

Acknowledgements: We gratefully acknowledge financial support from the
agencies and organizations listed here: www.cta-
observatory.org/consortium_acknowledgments

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  * Tavernier et al. [2019] Tavernier, T., Glicenstein, J. F., Brun, F. 2019. Status and performance results from NectarCam - a camera for CTA medium sized telescopes. 36th International Cosmic Ray Conference, 36.
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## Full Authors List: CTA Collaboration

H. Abdalla1, H. Abe2, S. Abe2, A. Abusleme3, F. Acero4, A. Acharyya5, V. Acín
Portella6, K. Ackley7, R. Adam8, C. Adams9, S.S. Adhikari10, I. Aguado-
Ruesga11, I. Agudo12, R. Aguilera13, A. Aguirre-Santaella14, F. Aharonian15,
A. Alberdi12, R. Alfaro16, J. Alfaro3, C. Alispach17, R. Aloisio18, R. Alves
Batista19, J.-P. Amans20, L. Amati21, E. Amato22, L. Ambrogi18, G. Ambrosi23,
M. Ambrosio24, R. Ammendola25, J. Anderson26, M. Anduze8, E.O. Angüner27, L.A.
Antonelli28, V. Antonuccio29, P. Antoranz30, R. Anutarawiramkul31, J. Aragunde
Gutierrez32, C. Aramo24, A. Araudo33,34, M. Araya35, A. Arbet-Engels36, C.
Arcaro1, V. Arendt37, C. Armand38, T. Armstrong27, F. Arqueros11, L.
Arrabito39, B. Arsioli40, M. Artero41, K. Asano2, Y. Ascasíbar14, J.
Aschersleben42, M. Ashley43, P. Attinà44, P. Aubert45, C. B. Singh19, D.
Baack46, A. Babic47, M. Backes48, V. Baena13, S. Bajtlik49, A. Baktash50, C.
Balazs7, M. Balbo38, O. Ballester41, J. Ballet4, B. Balmaverde44, A. Bamba51,
R. Bandiera22, A. Baquero Larriva11, P. Barai19, C. Barbier45, V. Barbosa
Martins52, M. Barcelo53, M. Barkov54, M. Barnard1, L. Baroncelli21, U. Barres
de Almeida40, J.A. Barrio11, D. Bastieri55, P.I. Batista52, I. Batkovic55, C.
Bauer53, R. Bautista-González56, J. Baxter2, U. Becciani29, J. Becerra
González32, Y. Becherini57, G. Beck58, J. Becker Tjus59, W. Bednarek60, A.
Belfiore61, L. Bellizzi62, R. Belmont4, W. Benbow63, D. Berge52, E.
Bernardini52, M.I. Bernardos55, K. Bernlöhr53, A. Berti64, M. Berton65, B.
Bertucci23, V. Beshley66, N. Bhatt67, S. Bhattacharyya67, W. Bhattacharyya52,
S. Bhattacharyya68, B. Bi69, G. Bicknell70, N. Biederbeck46, C. Bigongiari28,
A. Biland36, R. Bird71, E. Bissaldi72, J. Biteau73, M. Bitossi74, O. Blanch41,
M. Blank50, J. Blazek33, J. Bobin75, C. Boccato76, F. Bocchino77, C. Boehm78,
M. Bohacova33, C. Boisson20, J. Boix41, J.-P. Bolle52, J. Bolmont79, G.
Bonanno29, C. Bonavolontà24, L. Bonneau Arbeletche80, G. Bonnoli12, P.
Bordas81, J. Borkowski49, S. Bórquez35, R. Bose82, D. Bose83, Z. Bosnjak47, E.
Bottacini55, M. Böttcher1, M.T. Botticella84, C. Boutonnet85, F. Bouyjou75, V.
Bozhilov86, E. Bozzo38, L. Brahimi39, C. Braiding43, S. Brau-Nogué87, S.
Breen78, J. Bregeon39, M. Breuhaus53, A. Brill9, W. Brisken88, E. Brocato28,
A.M. Brown5, K. Brügge46, P. Brun89, P. Brun39, F. Brun89, L. Brunetti45, G.
Brunetti90, P. Bruno29, A. Bruno91, A. Bruzzese6, N. Bucciantini22, J.
Buckley82, R. Bühler52, A. Bulgarelli21, T. Bulik92, M. Bünning52, M. Bunse46,
M. Burton93, A. Burtovoi76, M. Buscemi94, S. Buschjäger46, G. Busetto55, J.
Buss46, K. Byrum26, A. Caccianiga95, F. Cadoux17, A. Calanducci29, C.
Calderón3, J. Calvo Tovar32, R. Cameron96, P. Campaña35, R. Canestrari91, F.
Cangemi79, B. Cantlay31, M. Capalbi91, M. Capasso9, M. Cappi21, A. Caproni97,
R. Capuzzo-Dolcetta28, P. Caraveo61, V. Cárdenas98, L. Cardiel41, M.
Cardillo99, C. Carlile100, S. Caroff45, R. Carosi74, A. Carosi17, E.
Carquín35, M. Carrère39, J.-M. Casandjian4, S. Casanova101,53, E. Cascone84,
F. Cassol27, A.J. Castro-Tirado12, F. Catalani102, O. Catalano91, D. Cauz103,
A. Ceccanti64, C. Celestino Silva80, S. Celli18, K. Cerny104, M. Cerruti85, E.
Chabanne45, P. Chadwick5, Y. Chai105, P. Chambery106, C. Champion85, S.
Chandra1, S. Chaty4, A. Chen58, K. Cheng2, M. Chernyakova107, G. Chiaro61, A.
Chiavassa64,108, M. Chikawa2, V.R. Chitnis109, J. Chudoba33, L. Chytka104, S.
Cikota47, A. Circiello24,110, P. Clark5, M. Çolak41, E. Colombo32, J.
Colome13, S. Colonges85, A. Comastri21, A. Compagnino91, V. Conforti21, E.
Congiu95, R. Coniglione94, J. Conrad111, F. Conte53, J.L. Contreras11, P.
Coppi112, R. Cornat8, J. Coronado-Blazquez14, J. Cortina113, A. Costa29, H.
Costantini27, G. Cotter114, B. Courty85, S. Covino95, S. Crestan61, P.
Cristofari20, R. Crocker70, J. Croston115, K. Cubuk93, O. Cuevas98, X. Cui2,
G. Cusumano91, S. Cutini23, A. D’Aì91, G. D’Amico116, F. D’Ammando90, P.
D’Avanzo95, P. Da Vela74, M. Dadina21, S. Dai117, M. Dalchenko17, M. Dall’
Ora84, M.K. Daniel63, J. Dauguet85, I. Davids48, J. Davies114, B. Dawson118,
A. De Angelis55, A.E. de Araújo Carvalho40, M. de Bony de Lavergne45, V. De
Caprio84, G. De Cesare21, F. De Frondat20, E.M. de Gouveia Dal Pino19, I. de
la Calle11, B. De Lotto103, A. De Luca61, D. De Martino84, R.M. de Menezes19,
M. de Naurois8, E. de Oña Wilhelmi13, F. De Palma64, F. De Persio119, N. de
Simone52, V. de Souza80, M. Del Santo91, M.V. del Valle19, E. Delagnes75, G.
Deleglise45, M. Delfino Reznicek6, C. Delgado113, A.G. Delgado Giler80, J.
Delgado Mengual6, R. Della Ceca95, M. Della Valle84, D. della Volpe17, D.
Depaoli64,108, D. Depouez27, J. Devin85, T. Di Girolamo24,110, C. Di Giulio25,
A. Di Piano21, F. Di Pierro64, L. Di Venere120, C. Díaz113, C. Díaz-
Bahamondes3, C. Dib35, S. Diebold69, S. Digel96, R. Dima55, A. Djannati-
Ataï85, J. Djuvsland116, A. Dmytriiev20, K. Docher9, A. Domínguez11, D.
Dominis Prester121, A. Donath53, A. Donini41, D. Dorner122, M. Doro55, R.d.C.
dos Anjos123, J.-L. Dournaux20, T. Downes107, G. Drake26, H. Drass3, D.
Dravins100, C. Duangchan31, A. Duara124, G. Dubus125, L. Ducci69, C. Duffy124,
D. Dumora106, K. Dundas Morå111, A. Durkalec126, V.V. Dwarkadas127, J. Ebr33,
C. Eckner45, J. Eder105, A. Ederoclite19, E. Edy8, K. Egberts128, S.
Einecke118, J. Eisch129, C. Eleftheriadis130, D. Elsässer46, G. Emery17, D.
Emmanoulopoulos115, J.-P. Ernenwein27, M. Errando82, P. Escarate35, J.
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1 : Centre for Space Research, North-West University, Potchefstroom, 2520, South Africa 2 : Institute for Cosmic Ray Research, University of Tokyo, 5-1-5, Kashiwa-no-ha, Kashiwa, Chiba 277-8582, Japan 3 : Pontificia Universidad Católica de Chile, Av. Libertador Bernardo O’Higgins 340, Santiago, Chile 4 : AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, CEA Paris-Saclay, IRFU/DAp, Bat 709, Orme des Merisiers, 91191 Gif-sur-Yvette, France 5 : Centre for Advanced Instrumentation, Dept. of Physics, Durham University, South Road, Durham DH1 3LE, United Kingdom 6 : Port d’Informació Científica, Edifici D, Carrer de l’Albareda, 08193 Bellaterrra (Cerdanyola del Vallès), Spain 7 : School of Physics and Astronomy, Monash University, Melbourne, Victoria 3800, Australia 8 : Laboratoire Leprince-Ringuet, École Polytechnique (UMR 7638, CNRS/IN2P3, Institut Polytechnique de Paris), 91128 Palaiseau, France 9 : Department of Physics, Columbia University, 538 West 120th Street, New York, NY 10027, USA 10 : University of Oslo, Department of Physics, Sem Saelandsvei 24 - PO Box 1048 Blindern, N-0316 Oslo, Norway 11 : EMFTEL department and IPARCOS, Universidad Complutense de Madrid, 28040 Madrid, Spain 12 : Instituto de Astrofísica de Andalucía-CSIC, Glorieta de la Astronomía s/n, 18008, Granada, Spain 13 : Institute of Space Sciences (ICE-CSIC), and Institut d’Estudis Espacials de Catalunya (IEEC), and Institució Catalana de Recerca I Estudis Avançats (ICREA), Campus UAB, Carrer de Can Magrans, s/n 08193 Cerdanyola del Vallés, Spain 14 : Instituto de Física Teórica UAM/CSIC and Departamento de Física Teórica, Universidad Autónoma de Madrid, c/ Nicolás Cabrera 13-15, Campus de Cantoblanco UAM, 28049 Madrid, Spain 15 : Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland 16 : Universidad Nacional Autónoma de México, Delegación Coyoacán, 04510 Ciudad de México, Mexico 17 : University of Geneva - Département de physique nucléaire et corpusculaire, 24 rue du Général-Dufour, 1211 Genève 4, Switzerland 18 : INFN Dipartimento di Scienze Fisiche e Chimiche - Università degli Studi dell’Aquila and Gran Sasso Science Institute, Via Vetoio 1, Viale Crispi 7, 67100 L’Aquila, Italy 19 : Instituto de Astronomia, Geofísico, e Ciências Atmosféricas - Universidade de São Paulo, Cidade Universitária, R. do Matão, 1226, CEP 05508-090, São Paulo, SP, Brazil 20 : LUTH, GEPI and LERMA, Observatoire de Paris, CNRS, PSL University, 5 place Jules Janssen, 92190, Meudon, France 21 : INAF - Osservatorio di Astrofisica e Scienza dello spazio di Bologna, Via Piero Gobetti 93/3, 40129 Bologna, Italy 22 : INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5 - 50125 Firenze, Italy 23 : INFN Sezione di Perugia and Università degli Studi di Perugia, Via A. Pascoli, 06123 Perugia, Italy 24 : INFN Sezione di Napoli, Via Cintia, ed. G, 80126 Napoli, Italy 25 : INFN Sezione di Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Rome, Italy 26 : Argonne National Laboratory, 9700 S. Cass Avenue, Argonne, IL 60439, USA 27 : Aix-Marseille Université, CNRS/IN2P3, CPPM, 163 Avenue de Luminy, 13288 Marseille cedex 09, France 28 : INAF - Osservatorio Astronomico di Roma, Via di Frascati 33, 00040, Monteporzio Catone, Italy 29 : INAF - Osservatorio Astrofisico di Catania, Via S. Sofia, 78, 95123 Catania, Italy 30 : Grupo de Electronica, Universidad Complutense de Madrid, Av. Complutense s/n, 28040 Madrid, Spain 31 : National Astronomical Research Institute of Thailand, 191 Huay Kaew Rd., Suthep, Muang, Chiang Mai, 50200, Thailand 32 : Instituto de Astrofísica de Canarias and Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain 33 : FZU - Institute of Physics of the Czech Academy of Sciences, Na Slovance 1999/2, 182 21 Praha 8, Czech Republic 34 : Astronomical Institute of the Czech Academy of Sciences, Bocni II 1401 - 14100 Prague, Czech Republic 35 : CCTVal, Universidad Técnica Federico Santa María, Avenida España 1680, Valparaíso, Chile 36 : ETH Zurich, Institute for Particle Physics, Schafmattstr. 20, CH-8093 Zurich, Switzerland 37 : The University of Manitoba, Dept of Physics and Astronomy, Winnipeg, Manitoba R3T 2N2, Canada 38 : Department of Astronomy, University of Geneva, Chemin d’Ecogia 16, CH-1290 Versoix, Switzerland 39 : Laboratoire Univers et Particules de Montpellier, Université de Montpellier, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France 40 : Centro Brasileiro de Pesquisas Físicas, Rua Xavier Sigaud 150, RJ 22290-180, Rio de Janeiro, Brazil 41 : Institut de Fisica d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona), Spain 42 : University of Groningen, KVI - Center for Advanced Radiation Technology, Zernikelaan 25, 9747 AA Groningen, The Netherlands 43 : School of Physics, University of New South Wales, Sydney NSW 2052, Australia 44 : INAF - Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese (TO), Italy 45 : Univ. Savoie Mont Blanc, CNRS, Laboratoire d’Annecy de Physique des Particules - IN2P3, 74000 Annecy, France 46 : Department of Physics, TU Dortmund University, Otto-Hahn-Str. 4, 44221 Dortmund, Germany 47 : University of Zagreb, Faculty of electrical engineering and computing, Unska 3, 10000 Zagreb, Croatia 48 : University of Namibia, Department of Physics, 340 Mandume Ndemufayo Ave., Pioneerspark, Windhoek, Namibia 49 : Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland 50 : Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, 22761 Hamburg, Germany 51 : Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan 52 : Deutsches Elektronen-Synchrotron, Platanenallee 6, 15738 Zeuthen, Germany 53 : Max-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany 54 : RIKEN, Institute of Physical and Chemical Research, 2-1 Hirosawa, Wako, Saitama, 351-0198, Japan 55 : INFN Sezione di Padova and Università degli Studi di Padova, Via Marzolo 8, 35131 Padova, Italy 56 : Escuela Politécnica Superior de Jaén, Universidad de Jaén, Campus Las Lagunillas s/n, Edif. A3, 23071 Jaén, Spain 57 : Department of Physics and Electrical Engineering, Linnaeus University, 351 95 Växjö, Sweden 58 : University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein, 2000 Johannesburg, South Africa 59 : Institut für Theoretische Physik, Lehrstuhl IV: Plasma-Astroteilchenphysik, Ruhr-Universität Bochum, Universitätsstraße 150, 44801 Bochum, Germany 60 : Faculty of Physics and Applied Computer Science, University of Lódź, ul. Pomorska 149-153, 90-236 Lódź, Poland 61 : INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano, Via A. Corti 12, 20133 Milano, Italy 62 : INFN and Università degli Studi di Siena, Dipartimento di Scienze Fisiche, della Terra e dell’Ambiente (DSFTA), Sezione di Fisica, Via Roma 56, 53100 Siena, Italy 63 : Center for Astrophysics | Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02180, USA 64 : INFN Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy 65 : Finnish Centre for Astronomy with ESO, University of Turku, Finland, FI-20014 University of Turku, Finland 66 : Pidstryhach Institute for Applied Problems in Mechanics and Mathematics NASU, 3B Naukova Street, Lviv, 79060, Ukraine 67 : Bhabha Atomic Research Centre, Trombay, Mumbai 400085, India 68 : Center for Astrophysics and Cosmology, University of Nova Gorica, Vipavska 11c, 5270 Ajdovščina, Slovenia 69 : Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany 70 : Research School of Astronomy and Astrophysics, Australian National University, Canberra ACT 0200, Australia 71 : Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA 72 : INFN Sezione di Bari and Politecnico di Bari, via Orabona 4, 70124 Bari, Italy 73 : Laboratoire de Physique des 2 infinis, Irene Joliot-Curie,IN2P3/CNRS, Université Paris-Saclay, Université de Paris, 15 rue Georges Clemenceau, 91406 Orsay, Cedex, France 74 : INFN Sezione di Pisa, Largo Pontecorvo 3, 56217 Pisa, Italy 75 : IRFU/DEDIP, CEA, Université Paris-Saclay, Bat 141, 91191 Gif-sur-Yvette, France 76 : INAF - Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 77 : INAF - Osservatorio Astronomico di Palermo "G.S. Vaiana", Piazza del Parlamento 1, 90134 Palermo, Italy 78 : School of Physics, University of Sydney, Sydney NSW 2006, Australia 79 : Sorbonne Université, Université Paris Diderot, Sorbonne Paris Cité, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies, LPNHE, 4 Place Jussieu, F-75005 Paris, France 80 : Instituto de Física de São Carlos, Universidade de São Paulo, Av. Trabalhador São-carlense, 400 - CEP 13566-590, São Carlos, SP, Brazil 81 : Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona, IEEC-UB, Martí i Franquès, 1, 08028, Barcelona, Spain 82 : Department of Physics, Washington University, St. Louis, MO 63130, USA 83 : Saha Institute of Nuclear Physics, Bidhannagar, Kolkata-700 064, India 84 : INAF - Osservatorio Astronomico di Capodimonte, Via Salita Moiariello 16, 80131 Napoli, Italy 85 : Université de Paris, CNRS, Astroparticule et Cosmologie, 10, rue Alice Domon et Léonie Duquet, 75013 Paris Cedex 13, France 86 : Astronomy Department of Faculty of Physics, Sofia University, 5 James Bourchier Str., 1164 Sofia, Bulgaria 87 : Institut de Recherche en Astrophysique et Planétologie, CNRS-INSU, Université Paul Sabatier, 9 avenue Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France 88 : School of Physics and Astronomy, University of Minnesota, 116 Church Street S.E. Minneapolis, Minnesota 55455-0112, USA 89 : IRFU, CEA, Université Paris-Saclay, Bât 141, 91191 Gif-sur-Yvette, France 90 : INAF - Istituto di Radioastronomia, Via Gobetti 101, 40129 Bologna, Italy 91 : INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Via U. La Malfa 153, 90146 Palermo, Italy 92 : Astronomical Observatory, Department of Physics, University of Warsaw, Aleje Ujazdowskie 4, 00478 Warsaw, Poland 93 : Armagh Observatory and Planetarium, College Hill, Armagh BT61 9DG, United Kingdom 94 : INFN Sezione di Catania, Via S. Sofia 64, 95123 Catania, Italy 95 : INAF - Osservatorio Astronomico di Brera, Via Brera 28, 20121 Milano, Italy 96 : Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, 2575 Sand Hill Road, Menlo Park, CA 94025, USA 97 : Universidade Cruzeiro do Sul, Núcleo de Astrofísica Teórica (NAT/UCS), Rua Galvão Bueno 8687, Bloco B, sala 16, Libertade 01506-000 - São Paulo, Brazil 98 : Universidad de Valparaíso, Blanco 951, Valparaiso, Chile 99 : INAF - Istituto di Astrofisica e Planetologia Spaziali (IAPS), Via del Fosso del Cavaliere 100, 00133 Roma, Italy 100 : Lund Observatory, Lund University, Box 43, SE-22100 Lund, Sweden 101 : The Henryk Niewodniczański Institute of Nuclear Physics, Polish Academy of Sciences, ul. Radzikowskiego 152, 31-342 Cracow, Poland 102 : Escola de Engenharia de Lorena, Universidade de São Paulo, Área I - Estrada Municipal do Campinho, s/n°, CEP 12602-810, Pte. Nova, Lorena, Brazil 103 : INFN Sezione di Trieste and Università degli Studi di Udine, Via delle Scienze 208, 33100 Udine, Italy 104 : Palacky University Olomouc, Faculty of Science, RCPTM, 17. listopadu 1192/12, 771 46 Olomouc, Czech Republic 105 : Max-Planck-Institut für Physik, Föhringer Ring 6, 80805 München, Germany 106 : CENBG, Univ. Bordeaux, CNRS-IN2P3, UMR 5797, 19 Chemin du Solarium, CS 10120, F-33175 Gradignan Cedex, France 107 : Dublin City University, Glasnevin, Dublin 9, Ireland 108 : Dipartimento di Fisica - Universitá degli Studi di Torino, Via Pietro Giuria 1 - 10125 Torino, Italy 109 : Tata Institute of Fundamental Research, Homi Bhabha Road, Colaba, Mumbai 400005, India 110 : Universitá degli Studi di Napoli "Federico II" - Dipartimento di Fisica "E. Pancini", Complesso universitario di Monte Sant’Angelo, Via Cintia - 80126 Napoli, Italy 111 : Oskar Klein Centre, Department of Physics, University of Stockholm, Albanova, SE-10691, Sweden 112 : Yale University, Department of Physics and Astronomy, 260 Whitney Avenue, New Haven, CT 06520-8101, USA 113 : CIEMAT, Avda. Complutense 40, 28040 Madrid, Spain 114 : University of Oxford, Department of Physics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, United Kingdom 115 : School of Physics & Astronomy, University of Southampton, University Road, Southampton SO17 1BJ, United Kingdom 116 : Department of Physics and Technology, University of Bergen, Museplass 1, 5007 Bergen, Norway 117 : Western Sydney University, Locked Bag 1797, Penrith, NSW 2751, Australia 118 : School of Physical Sciences, University of Adelaide, Adelaide SA 5005, Australia 119 : INFN Sezione di Roma La Sapienza, P.le Aldo Moro, 2 - 00185 Roma, Italy 120 : INFN Sezione di Bari, via Orabona 4, 70126 Bari, Italy 121 : University of Rijeka, Department of Physics, Radmile Matejcic 2, 51000 Rijeka, Croatia 122 : Institute for Theoretical Physics and Astrophysics, Universität Würzburg, Campus Hubland Nord, Emil-Fischer-Str. 31, 97074 Würzburg, Germany 123 : Universidade Federal Do Paraná - Setor Palotina, Departamento de Engenharias e Exatas, Rua Pioneiro, 2153, Jardim Dallas, CEP: 85950-000 Palotina, Paraná, Brazil 124 : Dept. of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, United Kingdom 125 : Univ. Grenoble Alpes, CNRS, IPAG, 414 rue de la Piscine, Domaine Universitaire, 38041 Grenoble Cedex 9, France 126 : National Centre for nuclear research (Narodowe Centrum Badań Jądrowych), Ul. Andrzeja Sołtana7, 05-400 Otwock, Świerk, Poland 127 : Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA 128 : Institut für Physik & Astronomie, Universität Potsdam, Karl-Liebknecht-Strasse 24/25, 14476 Potsdam, Germany 129 : Department of Physics and Astronomy, Iowa State University, Zaffarano Hall, Ames, IA 50011-3160, USA 130 : School of Physics, Aristotle University, Thessaloniki, 54124 Thessaloniki, Greece 131 : King’s College London, Strand, London, WC2R 2LS, United Kingdom 132 : Escola de Artes, Ciências e Humanidades, Universidade de São Paulo, Rua Arlindo Bettio, CEP 03828-000, 1000 São Paulo, Brazil 133 : Dept. of Astronomy & Astrophysics, Pennsylvania State University, University Park, PA 16802, USA 134 : National Technical University of Athens, Department of Physics, Zografos 9, 15780 Athens, Greece 135 : University of Wisconsin, Madison, 500 Lincoln Drive, Madison, WI, 53706, USA 136 : Astronomical Observatory of Taras Shevchenko National University of Kyiv, 3 Observatorna Street, Kyiv, 04053, Ukraine 137 : Department of Physics, Purdue University, West Lafayette, IN 47907, USA 138 : Unitat de Física de les Radiacions, Departament de Física, and CERES-IEEC, Universitat Autònoma de Barcelona, Edifici C3, Campus UAB, 08193 Bellaterra, Spain 139 : Institute for Space-Earth Environmental Research, Nagoya University, Chikusa-ku, Nagoya 464-8601, Japan 140 : Department of Physical Science, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan 141 : Department of Physics, Nagoya University, Chikusa-ku, Nagoya, 464-8602, Japan 142 : Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen Centre for Astroparticle Physics (ECAP), Erwin-Rommel-Str. 1, 91058 Erlangen, Germany 143 : Santa Cruz Institute for Particle Physics and Department of Physics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA 144 : IRFU / DIS, CEA, Université de Paris-Saclay, Bat 123, 91191 Gif-sur-Yvette, France 145 : INFN Sezione di Trieste and Università degli Studi di Trieste, Via Valerio 2 I, 34127 Trieste, Italy 146 : School of Physics & Center for Relativistic Astrophysics, Georgia Institute of Technology, 837 State Street, Atlanta, Georgia, 30332-0430, USA 147 : Alikhanyan National Science Laboratory, Yerevan Physics Institute, 2 Alikhanyan Brothers St., 0036, Yerevan, Armenia 148 : INAF - Telescopio Nazionale Galileo, Roche de los Muchachos Astronomical Observatory, 38787 Garafia, TF, Italy 149 : INFN Sezione di Bari and Università degli Studi di Bari, via Orabona 4, 70124 Bari, Italy 150 : University of Split - FESB, R. Boskovica 32, 21 000 Split, Croatia 151 : Universidad Andres Bello, República 252, Santiago, Chile 152 : Academic Computer Centre CYFRONET AGH, ul. Nawojki 11, 30-950 Cracow, Poland 153 : University of Liverpool, Oliver Lodge Laboratory, Liverpool L69 7ZE, United Kingdom 154 : Department of Physics, Yamagata University, Yamagata, Yamagata 990-8560, Japan 155 : Astronomy Department, Adler Planetarium and Astronomy Museum, Chicago, IL 60605, USA 156 : Faculty of Management Information, Yamanashi-Gakuin University, Kofu, Yamanashi 400-8575, Japan 157 : Department of Physics, Tokai University, 4-1-1, Kita-Kaname, Hiratsuka, Kanagawa 259-1292, Japan 158 : Centre for Astrophysics Research, Science & Technology Research Institute, University of Hertfordshire, College Lane, Hertfordshire AL10 9AB, United Kingdom 159 : Cherenkov Telescope Array Observatory, Saupfercheckweg 1, 69117 Heidelberg, Germany 160 : Tohoku University, Astronomical Institute, Aobaku, Sendai 980-8578, Japan 161 : Department of Physics, Rikkyo University, 3-34-1 Nishi-Ikebukuro, Toshima-ku, Tokyo, Japan 162 : Department of Physics and Astronomy and the Bartol Research Institute, University of Delaware, Newark, DE 19716, USA 163 : Institut für Astro- und Teilchenphysik, Leopold-Franzens-Universität, Technikerstr. 25/8, 6020 Innsbruck, Austria 164 : Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112-0830, USA 165 : IMAPP, Radboud University Nijmegen, P.O. Box 9010, 6500 GL Nijmegen, The Netherlands 166 : Josip Juraj Strossmayer University of Osijek, Trg Ljudevita Gaja 6, 31000 Osijek, Croatia 167 : Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka 560-0043, Japan 168 : Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan 169 : Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Cracow, Poland 170 : Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 171 : University of Alabama, Tuscaloosa, Department of Physics and Astronomy, Gallalee Hall, Box 870324 Tuscaloosa, AL 35487-0324, USA 172 : Department of Physics, University of Bath, Claverton Down, Bath BA2 7AY, United Kingdom 173 : University of Iowa, Department of Physics and Astronomy, Van Allen Hall, Iowa City, IA 52242, USA 174 : Anton Pannekoek Institute/GRAPPA, University of Amsterdam, Science Park 904 1098 XH Amsterdam, The Netherlands 175 : Faculty of Computer Science, Electronics and Telecommunications, AGH University of Science and Technology, Kraków, al. Mickiewicza 30, 30-059 Cracow, Poland 176 : Faculty of Science, Ibaraki University, Mito, Ibaraki, 310-8512, Japan 177 : Faculty of Science and Engineering, Waseda University, Shinjuku, Tokyo 169-8555, Japan 178 : Institute of Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University in Toruń, ul. Grudziądzka 5, 87-100 Toruń, Poland 179 : Graduate School of Science and Engineering, Saitama University, 255 Simo-Ohkubo, Sakura-ku, Saitama city, Saitama 338-8570, Japan 180 : Division of Physics and Astronomy, Graduate School of Science, Kyoto University, Sakyo-ku, Kyoto, 606-8502, Japan 181 : Centre for Quantum Technologies, National University Singapore, Block S15, 3 Science Drive 2, Singapore 117543, Singapore 182 : Institute of Particle and Nuclear Studies, KEK (High Energy Accelerator Research Organization), 1-1 Oho, Tsukuba, 305-0801, Japan 183 : Department of Physics and Astronomy, University of Sheffield, Hounsfield Road, Sheffield S3 7RH, United Kingdom 184 : Centro de Ciências Naturais e Humanas, Universidade Federal do ABC, Av. dos Estados, 5001, CEP: 09.210-580, Santo André - SP, Brazil 185 : Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Universitá di Catania, Via S. Sofia 78, I-95123 Catania, Italy 186 : Department of Physics, Humboldt University Berlin, Newtonstr. 15, 12489 Berlin, Germany 187 : Texas Tech University, 2500 Broadway, Lubbock, Texas 79409-1035, USA 188 : University of Zielona Góra, ul. Licealna 9, 65-417 Zielona Góra, Poland 189 : Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, 72 boul. Tsarigradsko chaussee, 1784 Sofia, Bulgaria 190 : University of Białystok, Faculty of Physics, ul. K. Ciołkowskiego 1L, 15-254 Białystok, Poland 191 : Faculty of Physics, National and Kapodestrian University of Athens, Panepistimiopolis, 15771 Ilissia, Athens, Greece 192 : Universidad de Chile, Av. Libertador Bernardo O’Higgins 1058, Santiago, Chile 193 : Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan 194 : Department of Applied Physics, University of Miyazaki, 1-1 Gakuen Kibana-dai Nishi, Miyazaki, 889-2192, Japan 195 : School of Allied Health Sciences, Kitasato University, Sagamihara, Kanagawa 228-8555, Japan 196 : Departamento de Astronomía, Universidad de Concepción, Barrio Universitario S/N, Concepción, Chile 197 : Charles University, Institute of Particle & Nuclear Physics, V Holešovičkách 2, 180 00 Prague 8, Czech Republic 198 : Astronomical Observatory of Ivan Franko National University of Lviv, 8 Kyryla i Mephodia Street, Lviv, 79005, Ukraine 199 : Kobayashi-Maskawa Institute (KMI) for the Origin of Particles and the Universe, Nagoya University, Chikusa-ku, Nagoya 464-8602, Japan 200 : Graduate School of Technology, Industrial and Social Sciences, Tokushima University, Tokushima 770-8506, Japan 201 : Space Research Centre, Polish Academy of Sciences, ul. Bartycka 18A, 00-716 Warsaw, Poland 202 : Instituto de Física - Universidade de São Paulo, Rua do Matão Travessa R Nr.187 CEP 05508-090 Cidade Universitária, São Paulo, Brazil 203 : International Institute of Physics at the Federal University of Rio Grande do Norte, Campus Universitário, Lagoa Nova CEP 59078-970 Rio Grande do Norte, Brazil 204 : University College Dublin, Belfield, Dublin 4, Ireland 205 : Centre for Astro-Particle Physics (CAPP) and Department of Physics, University of Johannesburg, PO Box 524, Auckland Park 2006, South Africa 206 : Departamento de Física, Facultad de Ciencias Básicas, Universidad Metropolitana de Ciencias de la Educación, Santiago, Chile 207 : Núcleo de Formação de Professores - Universidade Federal de São Carlos, Rodovia Washington Luís, km 235 CEP 13565-905 - SP-310 São Carlos - São Paulo, Brazil 208 : Physik-Institut, Universität Zürich, Winterthurerstrasse 190, 8057 Zürich, Switzerland 209 : Department of Physical Sciences, Aoyama Gakuin University, Fuchinobe, Sagamihara, Kanagawa, 252-5258, Japan 210 : University of the Free State, Nelson Mandela Avenue, Bloemfontein, 9300, South Africa 211 : Faculty of Electronics and Information, Warsaw University of Technology, ul. Nowowiejska 15/19, 00-665 Warsaw, Poland 212 : Rudjer Boskovic Institute, Bijenicka 54, 10 000 Zagreb, Croatia 213 : Department of Physics, Konan University, Kobe, Hyogo, 658-8501, Japan 214 : Kumamoto University, 2-39-1 Kurokami, Kumamoto, 860-8555, Japan 215 : University School for Advanced Studies IUSS Pavia, Palazzo del Broletto, Piazza della Vittoria 15, 27100 Pavia, Italy 216 : Aalto University, Otakaari 1, 00076 Aalto, Finland 217 : Agenzia Spaziale Italiana (ASI), 00133 Roma, Italy 218 : Observatoire de la Cote d’Azur, Boulevard de l’Observatoire CS34229, 06304 Nice Cedex 4, Franc