Calibration of the underground muon detector of the Pierre Auger Observatory. (arXiv:2012.08016v2 [astro-ph.IM] UPDATED)
The <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Pierre_Auger/0/1/0/all/0/1">Pierre Auger Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Aab_A/0/1/0/all/0/1">A. Aab</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abreu_P/0/1/0/all/0/1">P. Abreu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aglietta_M/0/1/0/all/0/1">M. Aglietta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albury_J/0/1/0/all/0/1">J.M. Albury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allekotte_I/0/1/0/all/0/1">I. Allekotte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almela_A/0/1/0/all/0/1">A. Almela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alvarez_Muniz_J/0/1/0/all/0/1">J. Alvarez-Muñiz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Batista_R/0/1/0/all/0/1">R. Alves Batista</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anastasi_G/0/1/0/all/0/1">G.A. Anastasi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anchordoqui_L/0/1/0/all/0/1">L. Anchordoqui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrada_B/0/1/0/all/0/1">B. Andrada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andringa_S/0/1/0/all/0/1">S. Andringa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aramo_C/0/1/0/all/0/1">C. Aramo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferreira_P/0/1/0/all/0/1">P.R. Araújo Ferreira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Velazquez_J/0/1/0/all/0/1">J. C. Arteaga Velázquez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asorey_H/0/1/0/all/0/1">H. Asorey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Assis_P/0/1/0/all/0/1">P. Assis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_G/0/1/0/all/0/1">G. Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Badescu_A/0/1/0/all/0/1">A.M. Badescu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakalova_A/0/1/0/all/0/1">A. Bakalova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balaceanu_A/0/1/0/all/0/1">A. Balaceanu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbato_F/0/1/0/all/0/1">F. Barbato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luz_R/0/1/0/all/0/1">R.J. Barreira Luz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_K/0/1/0/all/0/1">K.H. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellido_J/0/1/0/all/0/1">J.A. Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berat_C/0/1/0/all/0/1">C. Berat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertaina_M/0/1/0/all/0/1">M.E. Bertaina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertou_X/0/1/0/all/0/1">X. Bertou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biermann_P/0/1/0/all/0/1">P.L. Biermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bister_T/0/1/0/all/0/1">T. Bister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biteau_J/0/1/0/all/0/1">J. Biteau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blazek_J/0/1/0/all/0/1">J. Blazek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bleve_C/0/1/0/all/0/1">C. Bleve</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bohacova_M/0/1/0/all/0/1">M. Boháčová</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boncioli_D/0/1/0/all/0/1">D. Boncioli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonifazi_C/0/1/0/all/0/1">C. Bonifazi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arbeletche_L/0/1/0/all/0/1">L. Bonneau Arbeletche</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borodai_N/0/1/0/all/0/1">N. Borodai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Botti_A/0/1/0/all/0/1">A.M. Botti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brack_J/0/1/0/all/0/1">J. Brack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bretz_T/0/1/0/all/0/1">T. Bretz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Orchera_P/0/1/0/all/0/1">P.G. Brichetto Orchera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Briechle_F/0/1/0/all/0/1">F.L. Briechle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buchholz_P/0/1/0/all/0/1">P. Buchholz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bueno_A/0/1/0/all/0/1">A. Bueno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buitink_S/0/1/0/all/0/1">S. Buitink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buscemi_M/0/1/0/all/0/1">M. Buscemi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caballero_Mora_K/0/1/0/all/0/1">K.S. Caballero-Mora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caccianiga_L/0/1/0/all/0/1">L. Caccianiga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Canfora_F/0/1/0/all/0/1">F. Canfora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caracas_I/0/1/0/all/0/1">I. Caracas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carceller_J/0/1/0/all/0/1">J.M. Carceller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caruso_R/0/1/0/all/0/1">R. Caruso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castellina_A/0/1/0/all/0/1">A. Castellina</a>, et al. (318 additional authors not shown)
To obtain direct measurements of the muon content of extensive air showers
with energy above $10^{16.5}$ eV, the Pierre Auger Observatory is currently
being equipped with an underground muon detector (UMD), consisting of 219 10
$mathrm{m^2}$-modules, each segmented into 64 scintillators coupled to silicon
photomultipliers (SiPMs). Direct access to the shower muon content allows for
the study of both of the composition of primary cosmic rays and of high-energy
hadronic interactions in the forward direction. As the muon density can vary
between tens of muons per m$^2$ close to the intersection of the shower axis
with the ground to much less than one per m$^2$ when far away, the necessary
broad dynamic range is achieved by the simultaneous implementation of two
acquisition modes in the read-out electronics: the binary mode, tuned to count
single muons, and the ADC mode, suited to measure a high number of them. In
this work, we present the end-to-end calibration of the muon detector modules:
first, the SiPMs are calibrated by means of the binary channel, and then, the
ADC channel is calibrated using atmospheric muons, detected in parallel to the
shower data acquisition. The laboratory and field measurements performed to
develop the implementation of the full calibration chain of both binary and ADC
channels are presented and discussed. The calibration procedure is reliable to
work with the high amount of channels in the UMD, which will be operated
continuously, in changing environmental conditions, for several years.
To obtain direct measurements of the muon content of extensive air showers
with energy above $10^{16.5}$ eV, the Pierre Auger Observatory is currently
being equipped with an underground muon detector (UMD), consisting of 219 10
$mathrm{m^2}$-modules, each segmented into 64 scintillators coupled to silicon
photomultipliers (SiPMs). Direct access to the shower muon content allows for
the study of both of the composition of primary cosmic rays and of high-energy
hadronic interactions in the forward direction. As the muon density can vary
between tens of muons per m$^2$ close to the intersection of the shower axis
with the ground to much less than one per m$^2$ when far away, the necessary
broad dynamic range is achieved by the simultaneous implementation of two
acquisition modes in the read-out electronics: the binary mode, tuned to count
single muons, and the ADC mode, suited to measure a high number of them. In
this work, we present the end-to-end calibration of the muon detector modules:
first, the SiPMs are calibrated by means of the binary channel, and then, the
ADC channel is calibrated using atmospheric muons, detected in parallel to the
shower data acquisition. The laboratory and field measurements performed to
develop the implementation of the full calibration chain of both binary and ADC
channels are presented and discussed. The calibration procedure is reliable to
work with the high amount of channels in the UMD, which will be operated
continuously, in changing environmental conditions, for several years.
http://arxiv.org/icons/sfx.gif
