The KM3NeT/ARCA Calibration Unit

The KM3NeT/ARCA Calibration Unit 𝑎 Istituto Nazionale di Fisica Nucleare - Sezione di Bologna, Viale Berti-Pichat 6/2, 40127 Bologna, Italy 𝑏 Università di Bologna, Dipartimento di Fisica e Astronomia, Viale Berti Pichat 6/2, 40127 𝑐 Istituto Nazionale di Fisica Nucleare - Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy 𝑑 Istituto Nazionale di Fisica Nucleare - Laboratori Nazionali del Sud Via S. Sofia 62, 95125 Catania, Italy 𝑒 Istituto Nazionale di Fisica Nucleare - Sezione di Napoli Via Cintia, 80126 Napoli, Italy 𝑓 Istituto Nazionale di Fisica Nucleare - Sezione di Roma Piazzale Aldo Moro 2, 00185 Roma, Italy E-mail: [email protected] The KM3NeT/ARCA calibration unit is a dedicated calibration system designed to improve the accuracy of the acoustic positioning system of the detector optical modules and monitor the water column physical properties. The calibration unit is composed of a calibration base and an instrumentation unit, connected with an electrical inter-link cable. The deployment of one calibration unit for each of the two building-blocks, in which the ARCA detector is subdivided, is foreseen, with the őrst one to be deployed in 2024. The calibration base is made of an anchoring structure, connected for power supply and communication to a junction-box, where an acoustic beacon and a hydrophone used for the positioning system are mounted and which hosts a pressure vessel containing the required electronics. The instrumentation unit consists of an anchoring base and a 750m-long inductive line, kept vertical by a top buoy and equipped with oceanographic sensors. The base is linked to the calibration base for power and readout and hosts an absolute pressure gauge used as depth reference and a vessel containing the electronics for managing sensor communication. The line hosts two sound velocimeters and two conductivity-temperature-depth probes equipped with dissolved oxygen sensors, to measure sound velocity and allow for the determination of acoustic wave speed, and two Doppler current sensors to provide information on sea current speed and direction, further improving the accuracy of the positioning system. 38th International Cosmic Ray Conference (ICRC2023) 26 July - 3 August, 2023 Nagoya, Japan ∗ Speaker © Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). https://pos.sissa.it/ PoS(ICRC2023)1193 M. Anghinolfi,𝑐 F. Benfenati,𝑎,𝑏,∗ R. Cereseto,𝑐 R. Cocimano,𝑑 K. Leismuller,𝑑 C. D’Amato,𝑑 S. Dalle Fabbriche,𝑑 S. Mastroianni,𝑒 P. Migliozzi,𝑒 C.M. Mollo,𝑒 C. Nicolau, 𝑓 S. Ottonello,𝑐 G.Pellegrini,𝑎 G. Riccobene,𝑑 L. Roscilli,𝑒 A. Rovelli𝑑 and S.Viola𝑑 for the KM3NeT collaboration F. Benfenati The KM3NeT/ARCA Calibration Unit 1. Introduction 2. Positioning calibrations Under the effect of deep sea currents, DOMs tend to ŕoat around the vertical position which must hence be continuously monitored as well as their orientation, provided by internal compass data. This is done by means of a relative acoustic positioning system (APS) which relies on an auto-calibrating Long-Baseline (LBL) system of emitters and receivers displaced in the detector volume, located on the detector elements and on additional autonomous tripods. The accuracy in the determination of the DOMs position with respect to the LBL reference system, required to reach the desired detector angular resolution, is ∼10 cm [7] CUs are going to improve the APS in several ways: adding permanent acoustic beacons and hydrophones in the sea-ŕoor network, 2 PoS(ICRC2023)1193 The KM3NeT underwater neutrino telescope consists of two detectors, ORCA and ARCA [1], implemented as large-volume 3D arrays of Digital Optical Modules (DOMs) [2] hosting photomultipliers tubes (PMTs) and placed at a depth of ∼2450 m off-shore Toulon, France (ORCA) and of ∼3500 m off-shore Sicily, Italy (ARCA). Both detectors are made of vertically aligned Detection Units (DUs), each hosting 18 DOMs. In their őnal conőguration, ARCA will have 230 DUs and ORCA 115 DUs. Each DOM contains 31 3-inch PMTs, calibration and positioning instrumentation including a light emitter and readout electronic boards named Central Logic Boards (CLBs). Each DU is equipped with a top buoy to provide vertical support and is anchored to the sea-ŕoor with a heavy anchor frame which also incorporates the DU Base Module (DU-BM) and calibration devices such as hydrophones, lasers, acoustic beacons. The DU-BM hosts the electronics for powering the DU and a CLB for instrument control and data readout. In ARCA, DUs are connected to submarine Junction-Boxes (JBs), which act as electrical and optical őber distribution systems, distributing data and power from the main electro-optical cables to the DUs and vice-versa. JBs are also endowed with hydrophones, lasers and acoustic beacons. While both ARCA and ORCA feature the same detection elements, they have distinct layouts designed to suit their respective scientiőc objectives; in particular, ARCA is designed to study cosmic neutrinos from the TeV to PeV scale and their possible astrophysical sources. The PMT array detects Cherenkov light emitted when relativistic charged particles traverse the detector volume. The recorded data is then utilised to determine the direction and energy of the incoming neutrino, which is responsible for generating these particles. In order to reconstruct neutrino direction with a precision better than 1◦ , DOMs need to be synchronised with nanosecond accuracy [3], and their exact location determined with an accuracy < 20 cm [4]. Having an impact on sound propagation, sea water properties must be continuously monitored because they affect the positioning calibrations. To meet these goals, KM3NeT is going to deploy several dedicated Calibration Units (CUs). Measurements of the environmental parameters will be also exploited for Earth and marine sciences studies, providing the capability for continuous online monitoring of the marine ecosystem for extended durations. Due to the different speciőc requirements of ARCA and ORCA detectors and their sizes, the design of the CUs differs between the two sites. This proceeding provides a comprehensive description of the features, the objectives and the current status of the őrst ARCA CU that will be depolyed shortly; for the ORCA CU, refer to [5]. F. Benfenati The KM3NeT/ARCA Calibration Unit providing measurements of sea currents along water column and allowing the characterization of sound velocity in the medium with precise measurements to be used in combination with data from the APS. 3. KM3NeT/ARCA Calibration Unit IU 2024 70 0 m CB Figure 1: The current ARCA sea-ŕoor map; coloured circles (boxes) indicate installed and next-to-bedeployed (Sep. 2023) DUs (JBs), while the straight lines indicate the inter-link cables connecting the DUs to the JBs. The colour scheme follows the sequence of marine campaigns indicated by a progressive number and the year. Highlighted are the positions of the CB and of the IU. The IU position is chosen to be in safe distance from the DU array and, according to the dominant current measured at site, to minimise the risk of line drifting into the őeld during deployment and recovery operations. 3.1 KM3NeT/ARCA Calibration Base The main role of the CB is to contribute to the detector APS by adding a LBL hydrophone and an acoustic beacon to the network. These instruments are mounted on the CB frame and are connected to a BM which contains the electronics for managing the power and communication both with the shore station and with the IU. The main components of the CB are described in the following subsections and are shown in Fig 2a. 3 PoS(ICRC2023)1193 The Calibration Unit is divided into two main components, connected by a 700m-long electrical ROV-operable inter-link cable: the Calibration Base (CB) and the Instrumentation Unit (IU). The CB will be connected to a JB via a 300m-long standard DU electro-optical inter-link for power and communication with the shore station. Detailed descriptions of the CB and the IU are in Sec. 3.1 and Sec. 3.2. Their locations at the ARCA site are shown in Fig. ?? along with the foreseen dates of deployment. ‡ F. Benfenati The KM3NeT/ARCA Calibration Unit ‡ ‡ e connector is inclined 18 ° from the horizontal plane LBL Hydrophone k to tion Unit Front panel with ODI connector to IU ODI connector to JB (moved to front panel) 2.5 m LBL LBLAcoustic AcousticBeacon Beacon 3 Sacrificial Sacrificial zynch anodes zinc anodes m 2.5 m (a) (b) Figure 2: (a): mechanical structure of the Calibration Base: components and instrumentation are highlighted. (b): the Calibration Base during integration. 3.1.1 Anchoring frame The CB is a compact structure made of primary and secondary iron crossbars welded together in a conőguration which is expected to be effective against corrosion phenomena. It has a central load-bearing beam and two lateral beams to support the hydrophone and the acoustic beacon, and it features a high density polyethylene (PEHD 500) front panel where the ODI ROV-operable plugs [9] for the inter-links towards the JB and the IU are integrated. PEHD 500 is also used for the supports that őx the BM, the hydrophone and the acoustic beacon to the structure. All the bolts and screws used to őx the components with plastic supports are made of titanium. In order to guarantee protection against corrosion for long-term deployment, all the metal surface is coated with anti-corrosion painting (standard NORSOK M-501 [8]) and a cathodic protection system with eleven ∼12 kg sacriőcial zinc anodes located on the bottom sides and on the central beam is applied. The base includes őberglass grids easing the assembly and preventing the anti-corrosion painting from scratching during integration. Initially, the structure was built with a support for hosting the inter-link towards the JB and the corresponding ODI connector was foreseen to be integrated on a panel adjacent to the central beam; since this inter-link has been separately deployed in advance, the connector has been moved to the front panel to facilitate ROV operations. 3.1.2 Instruments The selected hydrophone is the DG1330, a digital omni-directional hydrophone speciőcally designed and produced by Colmar S.r.l. [10] for KM3NeT to be operated at 3500m depth. It consists of a spherical piezo-ceramic element, read-out by an analogue board splitting the signal in two lines with different gains (+46 dB and +26 dB). The low gain channel has been implemented in order to prevent signal saturation due to the acoustic emission from the beacon in close proximity (∼3 m), while the high gain channel is used for analyzing data received from distant beacons, spanning up to a few kilometers, as well as for studying faint acoustic signals, such as those related to bio4 PoS(ICRC2023)1193 Base Module F. Benfenati The KM3NeT/ARCA Calibration Unit 3.1.3 Base Module The mechanical container of the ARCA CB-BM is made of titanium and it is identical to the standard ARCA DU-BM, except for the interface ŕange where the connectors for the CB instruments and for the two jumper cables towards the plugs for the IU and the JB inter-links are located. The internal frame is also identical, excluding the electrical and optical elements used to connect the DU-BM to DOMs. The BM hosts the following electronics boards: • The Base Power Supply (BPS) board receives 375VDC power from the JB and converts it into low voltage to power other electronic boards installed in the BM, the CB instruments and the IU. • The Central Logic Board is the core of KM3NeT front-end electronics, installed inside each DOM and BM. Regardless of the detector element where they are integrated, all CLBs are identical except for the installed őrmware. The CLB in the CB-BM receives commands and the common clock from the shore station and, through the FMC board, it interfaces the BPS, the CB instruments and the IU. Communication between CLB and shore station is established using an SFP laser integrated into the CLB. • The FPGA Mezzanine Card (FMC) is a piggy pack board mounted on the CLB. It enables CLB communication with BPS, CB instruments and IU. 3.2 KM3NeT/ARCA Instrumentation Unit The role of the IU is to acquire data regarding sea water properties. It is composed of the Instrumentation Line (IL) and the recoverable frame, shown in Fig. 3a. The IL is an inductive line, kept vertical by a top buoy, which both provides support for the oceanographic sensors and acts as transmission medium of the inductive transducers used to communicate with them, avoiding additional conductors. The frame consists in a metallic anchoring structure which hosts the Base Container (IU-BC) where the electronic boards are located, a front panel with the ROV bulkhead 5 PoS(ICRC2023)1193 acoustics, environmental noise, and acoustic neutrino detection [11]. It includes an analogue signal high-pass őltering stage at 700 Hz to reject the low frequency ambient sea noise and improve the signal to noise ratio in the detection of beacon pulses range (20-40 kHz). The sampling frequency is 195.3 kHz, and the acceptance frequency range is 5-90 kHz. The two streams are sampled with a stereo 24 bit commercial ADC (CS-4270) and converted into AES/EBU protocol using a digital interface transmitter. The acoustic beacon is the Mediterraneo Senales Maritimas [12] MAB 100, endowed with a FFR SX30 acoustic transducer. The electronic boards are contained in a shielded titanium case resisting up to 4000m of depth. The beacon is programmed to autonomously emit every 30s its unique modulation signature carried by a sweep signal ranging from 40kHz to 36kHz, but it can also emit with external triggers. Both instruments are connected to the CB-BM via a common GISMA [13] MCIL6M connector, and linked through it to the CLB via the FMC board (see Sec. 3.1.3). Connection for power and communication is done via RS-485 with a RJ45 connector for the hydrophone, while the acoustic beacon power is taken directly from the BPS board (see Sec. 3.1.3) and communication uses RS-232 lines connected to the FMC. The clock from the CLB, synchronised to the master clock in the shore station, is exploited to timestamp data retrieved by the hydrophone and can be used to emit synchronised triggers to the acoustic beacon. F. Benfenati The KM3NeT/ARCA Calibration Unit Instrumentation Line Buoy Inductive Cable Coupler Oceanographic instruments Base Container 700m inter-link to CB Recoverable Frame Zinc anode (b) (a) Figure 3: (a): ARCA IU main components. (b): the IU recoverable frame after integration. plug for connecting the IU-BC to the CB, an absolute pressure gauge and the inductive coupler for the IL. Communication between the CB and IU instrumentation occurs through inductive modems. Two types of modem are present: a Seabird [14] Inductive Modem Module (IMM) hosted inside the IU-BC to allow the communication between the CLB in the CB-BM and inductive sensors, and Seabird SBE-44 Underwater Inductive Modems to interface non-inductive serial sensors to the line. The SBE-44 provides also battery power to connected sensors through a wired power link. A Seabird Inductive Cable Coupler, located on the frame, couples the IMM to the inductive cable. 3.2.1 Recoverable frame The recoverable frame structure is made of stainless steel coated with anti-corrosive painting (standard NORSOK M-501) and cathodic protection is granted by two ∼12 kg welded sacriőcial zinc anodes. The front panel and the support ŕoor for the IU-BC and the other devices are built in PEHD 500. The frame has been designed in order to be recovered every two years, together with the IL, for batteries change and instrument re-calibration. To preserve the inter-link cable to the CB during recovery operations, a long-term cable parking terminal frame will be used. 3.3 Base container The IU Base Container is a titanium pressure vessel containing an electronic board that receives the power and communication lines from the CB. The IMM is mounted on this board, from which it receives 12V power and which also includes a serial converter from RS-422 to RS-232 standards. The board is connected to the CB through a DMS connector on one of the vessel ŕange via a jumper cable to the ROV connector on the front panel. On the other ŕange, another DMS connector is used for the cable coupler connection to the board. The ŕoor and the supports which őx the container and the instruments are made of PEHD 500, while titanium screws are used. 6 PoS(ICRC2023)1193 ODI connector F. Benfenati The KM3NeT/ARCA Calibration Unit 3.3.1 Instrumentation Line • Two non-inductive sound velocity sensors. They perform a direct measurement of the sound velocity in water, thus contributing to improve APS őts. • Two non-inductive Doppler current sensors. They perform measurements of the sea current along the 3 directions and will be used to improve the mechanical DU line őt model [15]. • One non-inductive pressure gauge, used as absolute depth reference to improve the accuracy of the APS; its measurements will also allow geo-oceanographic studies on the variation of sea depth and can be used to monitor earthquakes and tsunamis. Collected data will be made available to European oceanographic observatories and organizations such as ESONET-EMSO [18]. The instruments will be distributed along the water column as Height from seabed (m) 650 600 550 200 150 100 0 Instrument Measurement Valeport [20] mini-SVS Seabird SBE-37 IMP-ODO MicroCAT CTD AAndera [19] ZPulse Doppler Current Sensor 4520R Valeport mini-SVS Seabird SBE-37 IMP-ODO MicroCAT CTD AAndera ZPulse Doppler Current Sensor 4520R Paroscientiőc [21] Digiquartz Depth Sensor 8CB4000-I Sound velocity Conductivity, temperature, pressure Current velocity Sound velocity Conductivity, temperature, pressure Current velocity Pressure Table 1: Oceanographic sensors mounted on the Inductive Line, and respective indicative height from the seabed. shown in Tab. 1, where models are also indicated. 4. Outlooks and conclusions The őrst ARCA CB is fully tested and ready to be deployed, while the IU is under őnalisation: the recoverable frame is integrated, and instruments have to be conőgured and mounted on the 7 PoS(ICRC2023)1193 The inductive cable is a 750m-long, 3x19-strands galvanised jacketed wire rope with swaged socket terminations to allow grounding with seawater. The IU is equipped with the following instruments: • Two native inductive conductivity-temperature-depth probes with pressure and optical dissolved oxygen sensors. They measure conductivity, temperature and depth and allow indirect calculations of sound velocity in water as a function of temperature, pressure and salinity through Chen and Millero [16] or Del Grosso’s [17] formulas. They will be used to improve the őts of the APS. Measurements of oxygen and salt concentration (the latter inferred from conductivity) in water, as well as its temperature, will be used for oceanographic studies; F. Benfenati The KM3NeT/ARCA Calibration Unit inductive cable; a őnal communication test with the integrated IU will be done before preparation for deployment, foreseen in 2024. Firmware for CLB and software for communication with CB and IU instrumentation have been tested. The software update to the detector control system required for interfacing to the IU instruments and to store its data in the KM3NeT database is under development. References 8 PoS(ICRC2023)1193 [1] S. Adrian-Martinez et al. [the KM3Net Coll.], Letter of intent for KM3NeT 2.0, J. Phys. G 43, 084001 (2016). [arXiv:1601.07459 [astro-ph.IM]]. [2] S. Aiello et al. [the KM3Net Coll.], The KM3NeT multi-PMT optical module, JINST 18, no.02, T02001 (2023). [3] R. Coniglione et al. [on behalf of the KM3Net Coll.], KM3NeT Time Calibration, PoS ICRC2019, 868 (2021). [4] G. Riccobene et al. [on behalf of the KM3Net Coll.], The Positioning system for KM3NeT, EPJ Web Conf., 207 07005 (2019). [5] R. Le Breton et al. [on behalf of the KM3Net Coll.], The calibration units of KM3NeT, JINST 16, no.09, C09004 (2021). [6] S. Aiello et al. [the KM3Net Coll.], KM3NeT broadcast optical data transport system, JINST 18, no.02, T02001 (2023). [7] S. Viola et al. [on behalf of the KM3NeT Coll.], The KM3NeT acoustic positioning system, PoS ICRC2017, 1031 (2017). [8] NORSOK standard documentation: https://online.standard.no [9] Teledyne ODI website: http://www.teledynemarine.com/odi [10] Colmar S.r.l website: http://www.colmaritalia.it [11] D. Diego-Tortosa, M. Ardid, M. Bou-Cabo, G. Lara and J. A. Martínez-Mora, Development of a trigger for acoustic neutrino candidates in KM3NeT, [arXiv:2211.10149 [astro-ph.IM].]. [12] Mediterráneo Señales Marítimas website: https://mesemar.com/en/home/ [13] GISMA website: https://www.gisma-connectors.de/ [14] Seabird website: https://www.seabird.com/ [15] D. Diego-Tortosa et al. [on behalf of the KM3Net Coll.], KM3NeT Detection Unit Line Fit reconstruction using positioning sensors data, JINST 16, no.09, C09023 (2021). [16] C-T. Chen and F.J. Millero, Speed of sound in seawater at high pressures, J. Acoust. Soc. Am. 62(5) (1977). [17] V. A. Del Grosso, New equation for the speed of sound in natural waters (with comparisons to other equations) J. Acoust. Soc. Am 56(4)(1974). [18] EMSO website: https://emso.eu/ [19] Aandera website: https://www.aanderaa.com/ [20] Valeport website: https://www.valeport.co.uk/ [21] Paroscientiőc website: https://paroscientific.com/ F. Benfenati The KM3NeT/ARCA Calibration Unit Full Authors List: The KM3NeT Collaboration 9 PoS(ICRC2023)1193 S. Aiello𝑎 , A. Albert𝑏,𝑏𝑑 , S. Alves Garre𝑐 , Z. Aly𝑑 , A. Ambrosone 𝑓 ,𝑒 , F. Ameli𝑔 , M. Andreℎ , E. Androutsou𝑖 , M. Anguita 𝑗 , L. Aphecetche 𝑘 , M. Ardid𝑙 , S. Ardid𝑙 , H. Atmani𝑚 , J. Aublin𝑛 , L. Bailly-Salins𝑜 , Z. Bardačová𝑞, 𝑝 , B. Baret𝑛 , A. BariegoQuintana𝑐 , S. Basegmez du Pree𝑟 , Y. Becherini𝑛 , M. Bendahman𝑚,𝑛 , F. Benfenati𝑡,𝑠 , M. Benhassi𝑢,𝑒 , D. M. Benoit𝑣 , E. Berbee𝑟 , V. Bertin𝑑 , S. Biagi𝑤 , M. Boettcher 𝑥 , D. Bonanno𝑤 , J. Boumaaza𝑚 , M. Bouta 𝑦 , M. Bouwhuis𝑟 , C. Bozza 𝑧,𝑒 , R. M. Bozza 𝑓 ,𝑒 , H.Brânzaş𝑎𝑎 , F. Bretaudeau 𝑘 , R. Bruijn𝑎𝑏,𝑟 , J. Brunner𝑑 , R. Bruno𝑎 , E. Buis𝑎𝑐,𝑟 , R. Buompane𝑢,𝑒 , J. Busto𝑑 , B. Caiffi𝑎𝑑 , D. Calvo𝑐 , S. Campion𝑔,𝑎𝑒 , A. Capone𝑔,𝑎𝑒 , F. Carenini𝑡,𝑠 , V. Carretero𝑐 , T. Cartraud𝑛 , P. Castaldi𝑎 𝑓 ,𝑠 , V. Cecchini𝑐 , S. Celli𝑔,𝑎𝑒 , L. Cerisy𝑑 , M. Chabab𝑎𝑔 , M. Chadolias𝑎ℎ , A. Chen𝑎𝑖 , S. Cherubini𝑎 𝑗,𝑤 , T. Chiarusi𝑠 , M. Circella𝑎𝑘 , R. Cocimano𝑤 , J. A. B. Coelho𝑛 , A. Coleiro𝑛 , R. Coniglione𝑤 P. Coyle𝑑 , A. Creusot𝑛 , A. Cruz𝑎𝑙 , G. Cuttone𝑤 , R. Dallier 𝑘 , Y. Darras𝑎ℎ , A. De Benedittis𝑒 , B. De Martino𝑑 , V. Decoene 𝑘 , R. Del Burgo𝑒 , U. M. Di Cerbo𝑒 , L. S. Di Mauro𝑤 , I. Di Palma𝑔,𝑎𝑒 , A. F. Díaz 𝑗 , C. Diaz 𝑗 , D. DiegoTortosa𝑤 , C. Distefano𝑤 , A. Domi𝑎ℎ , C. Donzaud𝑛 , D. Dornic𝑑 , M. Dörr𝑎𝑚 , E. Drakopoulou𝑖 , D. Drouhin𝑏,𝑏𝑑 , R. Dvornický𝑞 , T. Eberl𝑎ℎ , E. Eckerová𝑞, 𝑝 , A. Eddymaoui𝑚 , T. van Eeden𝑟 , M. Eff𝑛 , D. van Eijk𝑟 , I. El Bojaddaini 𝑦 , S. El Hedri𝑛 , A. Enzenhöfer𝑑 , G. Ferrara𝑤 , M. D. Filipović𝑎𝑛 , F. Filippini𝑡,𝑠 , D. Franciotti𝑤 , L. A. Fusco 𝑧,𝑒 , J. Gabriel𝑎𝑜 , S. Gagliardini𝑔 , T. Gal𝑎ℎ , J. García Méndez𝑙 , A. Garcia Soto𝑐 , C. Gatius Oliver𝑟 , N. Geißelbrecht𝑎ℎ , H. Ghaddari 𝑦 , L. Gialanella𝑒,𝑢 , B. K. Gibson𝑣 , E. Giorgio𝑤 , I. Goos𝑛 , D. Goupilliere𝑜 , S. R. Gozzini𝑐 , R. Gracia𝑎ℎ , K. Graf𝑎ℎ , C. Guidi𝑎 𝑝,𝑎𝑑 , B. Guillon𝑜 , M. Gutiérrez𝑎𝑞 , H. van Haren𝑎𝑟 , A. Heijboer𝑟 , A. Hekalo𝑎𝑚 , L. Hennig𝑎ℎ , J. J. Hernández-Rey𝑐 , F. Huang𝑑 , W. Idrissi Ibnsalih𝑒 , G. Illuminati𝑠 , C. W. James𝑎𝑙 , M. de Jong𝑎𝑠,𝑟 , P. de Jong𝑎𝑏,𝑟 , B. J. Jung𝑟 , P. Kalaczyński𝑎𝑡,𝑏𝑒 , O. Kalekin𝑎ℎ , U. F. Katz𝑎ℎ , N. R. Khan Chowdhury𝑐 , A. Khatun𝑞 , G. Kistauri𝑎𝑣,𝑎𝑢 , C. Kopper𝑎ℎ , A. Kouchner𝑎𝑤,𝑛 , V. Kulikovskiy𝑎𝑑 , R. Kvatadze𝑎𝑣 , M. Labalme𝑜 , R. Lahmann𝑎ℎ , G. Larosa𝑤 , C. Lastoria𝑑 , A. Lazo𝑐 , S. Le Stum𝑑 , G. Lehaut𝑜 , E. Leonora𝑎 , N. Lessing𝑐 , G. Levi𝑡,𝑠 , M. Lindsey Clark𝑛 , F. Longhitano𝑎 , J. Majumdar𝑟 , L. Malerba𝑎𝑑 , F. Mamedov 𝑝 , J. Mańczak𝑐 , A. Manfreda𝑒 , M. Marconi𝑎 𝑝,𝑎𝑑 , A. Margiotta𝑡,𝑠 , A. Marinelli𝑒, 𝑓 , C. Markou𝑖 , L. Martin 𝑘 , J. A. Martínez-Mora𝑙 , F. Marzaioli𝑢,𝑒 , M. Mastrodicasa𝑎𝑒,𝑔 , S. Mastroianni𝑒 , S. Miccichè𝑤 , G. Miele 𝑓 ,𝑒 , P. Migliozzi𝑒 , E. Migneco𝑤 , S. Minutoli𝑎𝑑 , M. L. Mitsou𝑒 , C. M. Mollo𝑒 , L. Morales-Gallegos𝑢,𝑒 , C. Morley-Wong𝑎𝑙 , A. Moussa 𝑦 , I. Mozun Mateo𝑎𝑦,𝑎𝑥 , R. Muller𝑟 , M. R. Musone𝑒,𝑢 , M. Musumeci𝑤 , L. Nauta𝑟 , S. Navas𝑎𝑞 , A. Nayerhoda𝑎𝑘 , C. A. Nicolau𝑔 , B. Nkosi𝑎𝑖 , B. Ó Fearraigh𝑎𝑏,𝑟 , V. Oliviero 𝑓 ,𝑒 , A. Orlando𝑤 , E. Oukacha𝑛 , D. Paesani𝑤 , J. Palacios González𝑐 , G. Papalashvili𝑎𝑢 , V. Parisi𝑎 𝑝,𝑎𝑑 , E.J. Pastor Gomez𝑐 , A. M. Păun𝑎𝑎 , G. E. Păvălaş𝑎𝑎 , S. Peña Martínez𝑛 , M. Perrin-Terrin𝑑 , J. Perronnel𝑜 , V. Pestel𝑎𝑦 , R. Pestes𝑛 , P. Piattelli𝑤 , C. Poirè 𝑧,𝑒 , V. Popa𝑎𝑎 , T. Pradier𝑏 , S. Pulvirenti𝑤 , G. Quéméner𝑜 , C. Quiroz𝑙 , U. Rahaman𝑐 , N. Randazzo𝑎 , R. Randriatoamanana 𝑘 , S. Razzaque𝑎𝑧 , I. C. Rea𝑒 , D. Real𝑐 , S. Reck𝑎ℎ , G. Riccobene𝑤 , J. Robinson 𝑥 , A. Romanov𝑎 𝑝,𝑎𝑑 , A. Šaina𝑐 , F. Salesa Greus𝑐 , D. F. E. Samtleben𝑎𝑠,𝑟 , A. Sánchez Losa𝑐,𝑎𝑘 , S. Sanőlippo𝑤 , M. Sanguineti𝑎 𝑝,𝑎𝑑 , C. Santonastaso𝑏𝑎,𝑒 , D. Santonocito𝑤 , P. Sapienza𝑤 , J. Schnabel𝑎ℎ , J. Schumann𝑎ℎ , H. M. Schutte 𝑥 , J. Seneca𝑟 , N. Sennan 𝑦 , B. Setter𝑎ℎ , I. Sgura𝑎𝑘 , R. Shanidze𝑎𝑢 , Y. Shitov 𝑝 , F. Šimkovic𝑞 , A. Simonelli𝑒 , A. Sinopoulou𝑎 , M.V. Smirnov𝑎ℎ , B. Spisso𝑒 , M. Spurio𝑡,𝑠 , D. Stavropoulos𝑖 , I. Štekl 𝑝 , M. Taiuti𝑎 𝑝,𝑎𝑑 , Y. Tayalati𝑚 , H. Tedjditi𝑎𝑑 , H. Thiersen 𝑥 , I. Tosta e Melo𝑎,𝑎 𝑗 , B. Trocmé𝑛 , V. Tsourapis𝑖 , E. Tzamariudaki𝑖 , A. Vacheret𝑜 , V. Valsecchi𝑤 , V. Van Elewyck𝑎𝑤,𝑛 , G. Vannoye𝑑 , G. Vasileiadis𝑏𝑏 , F. Vazquez de Sola𝑟 , C. Verilhac𝑛 , A. Veutro𝑔,𝑎𝑒 , S. Viola𝑤 , D. Vivolo𝑢,𝑒 , J. Wilms𝑏𝑐 , E. de Wolf𝑎𝑏,𝑟 , H. Yepes-Ramirez𝑙 , G. Zarpapis𝑖 , S. Zavatarelli𝑎𝑑 , A. Zegarelli𝑔,𝑎𝑒 , D. Zito𝑤 , J. D. Zornoza𝑐 , J. Zúñiga𝑐 , and N. Zywucka 𝑥 . 𝑎 INFN, Sezione di Catania, Via Santa Soőa 64, Catania, 95123 Italy 𝑏 Université de Strasbourg, CNRS, IPHC UMR 7178, F-67000 Strasbourg, France 𝑐 IFIC - Instituto de Física Corpuscular (CSIC - Universitat de València), c/Catedrático José Beltrán, 2, 46980 Paterna, Valencia, Spain 𝑑 Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France 𝑒 INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, Via Cintia ed. G, Napoli, 80126 Italy 𝑓 Università di Napoli łFederico IIž, Dip. Scienze Fisiche łE. Panciniž, Complesso Universitario di Monte S. Angelo, Via Cintia ed. G, Napoli, 80126 Italy 𝑔 INFN, Sezione di Roma, Piazzale Aldo Moro 2, Roma, 00185 Italy ℎ Universitat Politècnica de Catalunya, Laboratori d’Aplicacions Bioacústiques, Centre Tecnològic de Vilanova i la Geltrú, Avda. Rambla Exposició, s/n, Vilanova i la Geltrú, 08800 Spain 𝑖 NCSR Demokritos, Institute of Nuclear and Particle Physics, Ag. Paraskevi Attikis, Athens, 15310 Greece 𝑗 University of Granada, Dept. of Computer Architecture and Technology/CITIC, 18071 Granada, Spain 𝑘 Subatech, IMT Atlantique, IN2P3-CNRS, Université de Nantes, 4 rue Alfred Kastler - La Chantrerie, Nantes, BP 20722 44307 France 𝑙 Universitat Politècnica de València, Instituto de Investigación para la Gestión Integrada de las Zonas Costeras, C/ Paranimf, 1, Gandia, 46730 Spain 𝑚 University Mohammed V in Rabat, Faculty of Sciences, 4 av. Ibn Battouta, B.P. 1014, R.P. 10000 Rabat, Morocco 𝑛 Université Paris Cité, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France 𝑜 LPC CAEN, Normandie Univ, ENSICAEN, UNICAEN, CNRS/IN2P3, 6 boulevard Maréchal Juin, Caen, 14050 France 𝑝 Czech Technical University in Prague, Institute of Experimental and Applied Physics, Husova 240/5, Prague, 110 00 Czech Republic 𝑞 Comenius University in Bratislava, Department of Nuclear Physics and Biophysics, Mlynska dolina F1, Bratislava, 842 48 Slovak Republic 𝑟 Nikhef, National Institute for Subatomic Physics, PO Box 41882, Amsterdam, 1009 DB Netherlands 𝑠 INFN, Sezione di Bologna, v.le C. Berti-Pichat, 6/2, Bologna, 40127 Italy 𝑡 Università di Bologna, Dipartimento di Fisica e Astronomia, v.le C. Berti-Pichat, 6/2, Bologna, 40127 Italy 𝑢 Università degli Studi della Campania "Luigi Vanvitelli", Dipartimento di Matematica e Fisica, viale Lincoln 5, Caserta, 81100 Italy 𝑣 E. A. Milne Centre for Astrophysics, University of Hull, Hull, HU6 7RX, United Kingdom F. Benfenati The KM3NeT/ARCA Calibration Unit 𝑤 INFN, Laboratori Nazionali del Sud, Via S. Soőa 62, Catania, 95123 Italy University, Centre for Space Research, Private Bag X6001, Potchefstroom, 2520 South Africa 𝑦 University Mohammed I, Faculty of Sciences, BV Mohammed VI, B.P. 717, R.P. 60000 Oujda, Morocco 𝑧 Università di Salerno e INFN Gruppo Collegato di Salerno, Dipartimento di Fisica, Via Giovanni Paolo II 132, Fisciano, 84084 Italy 𝑎𝑎 ISS, Atomistilor 409, Măgurele, RO-077125 Romania 𝑎𝑏 University of Amsterdam, Institute of Physics/IHEF, PO Box 94216, Amsterdam, 1090 GE Netherlands 𝑎𝑐 TNO, Technical Sciences, PO Box 155, Delft, 2600 AD Netherlands 𝑎𝑑 INFN, Sezione di Genova, Via Dodecaneso 33, Genova, 16146 Italy 𝑎𝑒 Università La Sapienza, Dipartimento di Fisica, Piazzale Aldo Moro 2, Roma, 00185 Italy 𝑎 𝑓 Università di Bologna, Dipartimento di Ingegneria dell’Energia Elettrica e dell’Informazione "Guglielmo Marconi", Via dell’Università 50, Cesena, 47521 Italia 𝑎𝑔 Cadi Ayyad University, Physics Department, Faculty of Science Semlalia, Av. My Abdellah, P.O.B. 2390, Marrakech, 40000 Morocco 𝑎ℎ Friedrich-Alexander-Universität Erlangen-Nürnberg (FAU), Erlangen Centre for Astroparticle Physics, Nikolaus-Fiebiger-Straße 2, 91058 Erlangen, Germany 𝑎𝑖 University of the Witwatersrand, School of Physics, Private Bag 3, Johannesburg, Wits 2050 South Africa 𝑎 𝑗 Università di Catania, Dipartimento di Fisica e Astronomia "Ettore Majorana", Via Santa Soőa 64, Catania, 95123 Italy 𝑎𝑘 INFN, Sezione di Bari, via Orabona, 4, Bari, 70125 Italy 𝑎𝑙 International Centre for Radio Astronomy Research, Curtin University, Bentley, WA 6102, Australia 𝑎𝑚 University Würzburg, Emil-Fischer-Straße 31, Würzburg, 97074 Germany 𝑎𝑛 Western Sydney University, School of Computing, Engineering and Mathematics, Locked Bag 1797, Penrith, NSW 2751 Australia 𝑎𝑜 IN2P3, LPC, Campus des Cézeaux 24, avenue des Landais BP 80026, Aubière Cedex, 63171 France 𝑎 𝑝 Università di Genova, Via Dodecaneso 33, Genova, 16146 Italy 𝑎𝑞 University of Granada, Dpto. de Física Teórica y del Cosmos & C.A.F.P.E., 18071 Granada, Spain 𝑎𝑟 NIOZ (Royal Netherlands Institute for Sea Research), PO Box 59, Den Burg, Texel, 1790 AB, the Netherlands 𝑎𝑠 Leiden University, Leiden Institute of Physics, PO Box 9504, Leiden, 2300 RA Netherlands 𝑎𝑡 National Centre for Nuclear Research, 02-093 Warsaw, Poland 𝑎𝑢 Tbilisi State University, Department of Physics, 3, Chavchavadze Ave., Tbilisi, 0179 Georgia 𝑎𝑣 The University of Georgia, Institute of Physics, Kostava str. 77, Tbilisi, 0171 Georgia 𝑎𝑤 Institut Universitaire de France, 1 rue Descartes, Paris, 75005 France 𝑎𝑥 IN2P3, 3, Rue Michel-Ange, Paris 16, 75794 France 𝑎𝑦 LPC, Campus des Cézeaux 24, avenue des Landais BP 80026, Aubière Cedex, 63171 France 𝑎𝑧 University of Johannesburg, Department Physics, PO Box 524, Auckland Park, 2006 South Africa 𝑏𝑎 Università degli Studi della Campania "Luigi Vanvitelli", CAPACITY, Laboratorio CIRCE - Dip. Di Matematica e Fisica - Viale Carlo III di Borbone 153, San Nicola La Strada, 81020 Italy 𝑏𝑏 Laboratoire Univers et Particules de Montpellier, Place Eugène Bataillon - CC 72, Montpellier Cédex 05, 34095 France 𝑏𝑐 Friedrich-Alexander-Universität Erlangen-Nürnberg (FAU), Remeis Sternwarte, Sternwartstraße 7, 96049 Bamberg, Germany 𝑏𝑑 Université de Haute Alsace, rue des Frères Lumière, 68093 Mulhouse Cedex, France 𝑏𝑒 AstroCeNT, Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Rektorska 4, Warsaw, 00-614 Poland 𝑥 North-West The authors acknowledge the őnancial support of the funding agencies: Agence Nationale de la Recherche (contract ANR-15-CE310020), Centre National de la Recherche Scientiőque (CNRS), Commission Européenne (FEDER fund and Marie Curie Program), LabEx UnivEarthS (ANR-10-LABX-0023 and ANR-18-IDEX-0001), Paris Île-de-France Region, France; Shota Rustaveli National Science Foundation of Georgia (SRNSFG, FR-22-13708), Georgia; The General Secretariat of Research and Innovation (GSRI), Greece Istituto Nazionale di Fisica Nucleare (INFN), Ministero dell’Università e della Ricerca (MIUR), PRIN 2017 program (Grant NAT-NET 2017W4HA7S) Italy; Ministry of Higher Education, Scientiőc Research and Innovation, Morocco, and the Arab Fund for Economic and Social Development, Kuwait; Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; The National Science Centre, Poland (2021/41/N/ST2/01177); The grant łAstroCeNT: Particle Astrophysics Science and Technology Centrež, carried out within the International Research Agendas programme of the Foundation for Polish Science őnanced by the European Union under the European Regional Development Fund; National Authority for Scientiőc Research (ANCS), Romania; Grants PID2021-124591NB-C41, -C42, -C43 funded by MCIN/AEI/ 10.13039/501100011033 and, as appropriate, by łERDF A way of making Europež, by the łEuropean Unionž or by the łEuropean Union NextGenerationEU/PRTRž, Programa de Planes Complementarios I+D+I (refs. ASFAE/2022/023, ASFAE/2022/014), Programa Prometeo (PROMETEO/2020/019) and GenT (refs. CIDEGENT/2018/034, /2019/043, /2020/049. /2021/23) of the Generalitat Valenciana, Junta de Andalucía (ref. SOMM17/6104/UGR, P18-FR-5057), EU: MSC program (ref. 101025085), Programa María Zambrano (Spanish Ministry of Universities, funded by the European Union, NextGenerationEU), Spain; The European Union’s Horizon 2020 Research and Innovation Programme (ChETEC-INFRA - Project no. 101008324). 10 PoS(ICRC2023)1193 Acknowledgements