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En el mundo submarino, conocer la posición de la embarcación es de vital importancia dado que esta debe estar equipada con todo lo necesario para socorrer al buceador en caso de emergencia. También es importante de cara a planear la inmersión. Una mala planificación puede suponer que nos alejemos demasiado o que, debido a un mal cálculo de las corrientes, a la hora de regresar a la embarcación nos encontremos con que no tenemos reservas suficientes de oxígeno para finalizar la inmersión de forma segura. Los métodos que existen actualmente de posicionamiento bajo la superficie del mar se dividen principalmente en el método cableado y el método inalámbrico. El método cableado consiste en unir el elemento a localizar (un buceador o un ROV) con un elemento con flotabilidad, del cuál sería conocida su posición geográfica por GPS, lo cual evita los inconvenientes de la comunicación por ondas bajo el agua pero resta libertad de movimiento al estar atado a la superficie por un cable. En cuanto a los métodos inalámbricos: permiten al barco o a la estación de superficie conocer la posición del elemento sumergido mediante el uso de tecnologías sonoras de comunicación u ópticas. En este trabajo se establecen las bases para la creación de un sistema de posicionamiento bajo el agua que permita al buceador conocer la posición de la embarcación en todo momento mediante el uso de elementos acústicos y la interpretación de la señal recibida. El sistema planteado emplea técnicas de localización mediante acústica submarina y e impresión 3D para la fabricación del encapsulado que mantenga seco y asegurado todo el hardware necesario. Dado que la onda sonora se transmite de forma esférica, cualquier buceador con un dispositivo compatible con el transmisor, es decir, que sea capaz de descifrar la información recibida, podrá conocer la posición de la embarcación durante el transcurso de la inmersión.

[SPA] Desde hace años, en el campo de la acústica submarina, se ha desarrollado una línea de investigación con especial relevancia para aplicaciones de vigilancia ambientaly seguridad marítima que explora las posibilidades de los fenómenos no lineales de propagación del sonido, especialmente el referido al efecto paramétrico. Este artículo muestra los resultados de utilizar una nueva técnica de modulación basada en señales de barrido senoidal. Para esta modulación se presenta una cadena de información de 16 bits, con una frecuencia portadora de 200 kHz y mediante la aplicación del método de la correlación cruzada, se evalúan las limitaciones y mejoras de esta técnica de procesamiento. Esto permite alcanzar mejoras en la discriminación de los bits. Finalmente, se realiza una simulación de la influencia de la propagación en una señal acústica para un dispositivo acústico convencional y paramétrico., [ENG] For years, in the field of underwater acoustics, a line of research with special relevance for applications of environmental monitoring and maritime security has been developed that explores the possibilities of non-linear phenomena of sound propagation, especially the referring to the so-called parametric effect or self-modulation. This work shows the results of using a new modulation technique based on sine-sweep signals. For this modulation, a 16-bit strings of information is presented with 200 kHz carrier frequency and, by applying the cross-correlation method, the limitations and improvements of this processing technique are evaluated. This allows to achieve improvements in the discrimination of the bits used in underwater parametric acoustic communications. Finally, a simulation of the influence of propagation on an acoustic signal is performed for a conventional and a parametric acoustic device.

[SPA] Las comunicaciones en entornos submarinos se han convertido en un campo de investigación de gran interés en los últimos años por sus múltiples aplicaciones como, por ejemplo, monitorizar el medio marino para mantener la biodiversidad, perfilar el subfondo marino y avanzar en su conocimiento, controlar la navegación y el tránsito naval, defensa y seguridad, entre otros. Dado que la ondas acústicas presentan ciertas ventajas para su propagación en el medio marino, el desarrollo de transductores acústicos submarinos ha experimentado un aumento significativo como tecnologías de transmisión para sistemas de comunicación subacuática. Sin embargo, la propagación de las ondas en el mar tiene limitaciones, debido a la atenuación y absorción de la señal en el medio, la presencia de ruido, y especialmente, el efecto multicamino; mecanismos que pueda llegar a provocar una importante distorsión en la que se registra la señal en el receptor respecto a la que fue emitida. En aras de salvar este efecto, en esta tesis se plantean métodos de comunicación basados en el fenómeno de propagación no lineal llamado efecto paramétrico, que permite una comunicación directiva mediante el uso de transductores de alta frecuencia y alta intensidad cuyas ondas no lineales dan lugar, en su propagación, a la aparición de bajas frecuencias en el medio. Con esto, se prevén varias ventajas: comunicarse solo en la dirección deseada, y disminuir en su mayoría las múltiples reflexiones que podrían empeorar la calidad de la comunicación en aguas poco profundas. Además, en la presente tesis se aborda una forma particular de modulación basada en la concatenación de señales de banda ancha tipo sweep, en contraste con las técnicas clásicas de modulación tipo seno. Este tipo de modulación, estudiada desde el punto de vista del efecto paramétrico, permitirá un elevado grado de detección y disminución de tasas de error mejorando, aún más, las prestaciones de la comunicación. A pesar de las múltiples aplica, [ENG] Communications in underwater environments have become a field of research of great interest in recent years due to its applications, such as, for example, monitoring the marine environment to maintain biodiversity, profiling the seabed and advancing its knowledge, controlling the navigation and naval traffic, defense and security, among others. Since acoustic waves have certain advantages for their propagation in the marine environment, the development of underwater acoustic transducers has experienced a significant increase as transmission technologies for underwater communication systems. However, underwater acoustic has several limitations, due to the attenuation and absorption of the signal in the medium, the presence of noise, and especially, the multipath effect; mechanisms that can cause a significant distortion in which the signal is registered in the receiver with respect to which it is emitted. In order to overcome this effect, in this work communication methods based on the phenomenon of non-linear propagation called the parametric effect are proposed, that allows directive communication by using of high-frequency and high intensity transducers whose non-linear waves give rise, in their propagation, to the occurrence of low frequencies in the middle. With this, several advantages are foreseen: communicating only in the desired direction, and mostly reducing the multiple reflections that could worsen the quality of communication in shallow waters. Furthermore, this work deals with a particular form of modulation based on the concatenation of broadband sweep signals, in contrast to the classic techniques of sine-type modulation. This type of modulation, studied from the point of view of the parametric effect, will allow a high degree of detection and a reduction in error rates, further improving communication performance.

[EN] A full chain simulation of the acoustic hadrontherapy monitoring for brain tumours is presented in this work. For the study, a proton beam of 100 MeV is considered. In the first stage, Geant4 is used to simulate the energy deposition and to study the behaviour of the Bragg peak. The energy deposition in the medium produces local heating that can be considered instantaneous with respect to the hydrodynamic time scale producing a sound pressure wave. The resulting thermoacoustic signal has been subsequently obtained by solving the thermoacoustic equation. The acoustic propagation has been simulated by FEM methods in the brain and the skull, where a set of piezoelectric sensors are placed. Last, the final received signals in the sensors have been processed in order to reconstruct the position of the thermal source and, thus, to determine the feasibility and accuracy of acoustic beam monitoring in hadrontherapy.

[EN] A novel method to analyse the spatial distribution of neutrino candidates recorded with the ANTARES neutrino telescope is introduced, searching for an excess of neutrinos in a region of arbitrary size and shape from any direction in the sky. Techniques originating from the domains of machine learning, pat- tern recognition and image processing are used to purify the sample of neutrino candidates and for the analysis of the obtained skymap. In contrast to a dedicated search for a speci¿c neutrino emission model, this approach is sensitive to a wide range of possible morphologies of potential sources of high-energy neutrino emission. The application of these methods to ANTARES data yields a large-scale excess with a post-trial signi¿cance of 2.5¿ . Applied to public data from IceCube in its IC40 con¿guration, an excess consistent with the results from ANTARES is observed with a post-trial signi¿cance of 2.1¿ .

[ES] En este artículo se presenta la monitorización acústica del uso de partículas pesadas en tratamientos oncológicos con haces de protones a partir del estudio de la señal de presión generada por el efecto termoacústico debido a la incidencia de un haz de protones con una energía de 100 MeV para un caso específico de ependioma. El perfil espacial de la deposición de energía ha sido simulado empleando el método Monte Carlo en la herramienta de cálculo Geant4 junto con las librerías disponibles para incluir la interacción de las partículas con el tejido cerebral y la estructura ósea del cráneo. La señal termoacústica resultante es obtenida discretizando una solución particular de la ecuación de ondas termoacústica. Con esto, la fase de propagación y transmisión se ha simulado empleando el método de elementos finitos (FEM). Finalmente, se ha reconstruido la posición de la fuente de energía depositada evaluando el tiempo de llegada (TOA) a un conjunto de puntos sobre la superficie del cráneo., [EN] This article presents the acoustic monitoring of the use of heavy particles in oncological treatments with proton beams from the study of the pressure signal generated by the thermoacoustic effect due to the incidence of a proton beam with an energy of 100 MeV for a specific case of ependyoma. The spatial profile of the energy deposition has been simulated using the Monte Carlo method in the Geant4 calculation tool together with the available libraries to include the interaction of the particles with the brain tissue and the bone structure of the skull. The resulting thermoacoustic signal is obtained by discretizing a particular solution of the thermoacoustic wave equation. With this, the propagation and transmission phase has been simulated using the finite element method (FEM). Finally, the position of the deposited energy source has been reconstructed by evaluating the time of arrival (TOA) at a set of points on the surface of the skull.

[ES] En la última década, la terapia con haces de partículas pesadas (hadrones) ha sido una de las líneas de investigación con mayores estudios y avances en medicina nuclear. El número de centros de terapia con haces de partículas pesadas y los resultados en tratamiento especializado en tumores en la infancia cuando la cirugía no es el método más seguro, revelan una mejora sustancial frente a la radiación clásica con electrones y fotones. Así, el uso de protones como uno de los principales candidatos en hadronterapia, plantea retos importantes en la monitorización y localización de la deposición de energía durante la sesión de radiación en el paciente, pues implica procesos complejos de simulación y localización de las partículas al final de su recorrido. El objetivo de esta tesis es, por tanto, evaluar el conjunto de herramientas necesarias para estudiar los procesos de generación del haz, de su comportamiento en el medio, y la localización de este por medio de tecnologías basadas en métodos analíticos, numéricos y experimentales sobre el efecto termoacústico. Para ello se plantean cuatro capítulos que describen cada uno de los métodos que intervienen en el objetivo de localización y un capítulo final que resume un caso específico en la detección y localización del pico de Bragg. El capítulo I presenta un análisis del estado del arte sobre las estadísticas mundiales de la enfermedad del cáncer, de su implicación en la sociedad, de los métodos actuales de diagnóstico, tratamiento y monitorización que desvelan la necesidad de estudiar nuevas técnicas en terapia de hadrones. Se presenta, además, la hadronterapia desde un punto de vista tecnológico, donde se definen los sistemas de generación, emisión y posicionamiento del haz. El capítulo II enmarca los aspectos físicos que describen los procesos que dan lugar al modelo analítico del pico de Bragg, de su implicación en los modelos termoacústicos y una comparativa de resultados experimentales con simulaciones basadas e, [CA] En les últimes dècades, la teràpia amb feixos de partícules pesades (hadrones) ha sigut una de les línies d'investigació amb majors estudis i avanços en medicina nuclear. El número de centres de teràpia amb feixos de partícules pesades i els resultats en tractament especialitzat en tumors infantils quan la cirurgia no és el mètode mes segur, revelen una majoria substancial front a la radiació clàssica amb electrons i fotons. L'ús de protons com un dels principals candidats en hadronterapia, planteja reptes importants en la monitorització i localització de la deposició d' energia durant la sessió de radiació en el pacient, ja que implica processo complexos de simulació i localització de deposició de les partícules al final del seu recorregut. L'objectiu d'aquesta tesi és avaluar el conjunt de ferramentes necessàries per a estudiar els processos de generació del feix, del seu comportament al medi i la localització d'aquest mitjançant tecnologies basades en mètodes analítics, numèrics i experimentals sobre l'efecte termoacustic. Per això, es plantejant quatre capítols que descriuen cadascun dels mètodes que intervenen en l'objectiu de localització i un capítol final que resumeix un cas específic en la detecció i localització del pic de Bragg. A capítol I es presenta un anàlisi de l'estat de 'art sobre les estadístiques mundials d'infermetat del càncer, de la seua implicació en la societat, dels mètodes actuals de diagnòstic, tractament i monitorització que mostren la necessitat d'estudiar noves tècniques en teràpia d'hadrons. A més, es presenta l'adronterapia des d'un punt de vista tecnològic, on es defineixen els sistemes de generació, emissió i posicionament del feix. El capítol II emmarca els aspectes físics que descriuen els processos que duen al model analític del pic de Bragg, de la seua implicació en els models termoacústic i iuan comparativa de resultats experimentals amb simulacions basades en la desratització del model analític i models Monte Carlo. Així, [EN] In the last decade, heavy particle beam therapy (hadrons) has been one of the main lines of research with the most studies and advances in nuclear medicine. The number of heavy particle beam therapy centres and the results of specialized treatment for childhood tumours when surgery is not the safest method, reveal a substantial improvement over classical radiation with electrons and photos. Thus, the use of protons as one of the main candidates in hadrontherapy, poses significant challenges in monitoring and locating energy deposition during the radiation session in the patient, as it involves complex simulation processes and the localization of the particles at the end of their way. The aim of this thesis is, to evaluate the set of tools necessary to study the bem generation processes, their behaviour in the medium, and its localization by means of analytical, numerical and experimental methods on the thermoacoustic effect. To do this, four chapters are presented. Each one of these, describes methods involved in the localization objective and a final chapter that summarized a specific case in the detection and localization od the Bragg Peak. Chapter I presents a state-of-the-art analysis of global cancer disease statistics, their involvement in society, current diagnostic, treatment and monitoring methods that reveal the need to study new technologies in hadrontherapy. It is presented from a technology point of view, where the beam generation, emission and positioning system are defined. Chapter II frames the physical aspects that describe the processes that give rise to the analytical model of the Bragg Peak, its involvements in thermoacoustic models and a comparison of experimental results with simulations based on the discretization of the analytical model and Monte Carlo models. Thus, Chapter III defines the piezoelectric effect and its implication in the optimization of piezoelectric ceramics. For this, this thesis bases the results on the behaviour of th

Recording underwater impulsive noise data is an important aspect of mitigating its environmental impact and improving maritime environmental management systems. This paper describes the method used and results of the spatial monitoring of both the baseline noise level and the impulsive noise sources in the Port of Cartagena. An autonomous vessel was equipped with a smart digital hydrophone with a working frequency range between 10 and 200 kHz and a received voltage response (RVR) of, approximately, −170 dB re 1V/µPa. A GIS map was drawn up with the spatiotemporal distribution of the basal sound pressure levels by coupling the acoustic data with the vessel’s GPS positions to identify the sources of the impulsive noise of interest and their temporal characteristics. The loading of cargo containers was identified as the main source of impulse noise. This study is the first of a series designed to obtain accurate information on underwater noise pollution and its potential impact on biodiversity in the Port of Cartagena.

En este trabajo, se pretende realizar un estudio comparativo sobre los diferentes algoritmos de machine- learning basados en aprendizaje supervisado y evaluar su robustez frente a la discriminación de señales acústicas de calibración reales obtenidas mediante detectores de partículas. El objeto de este TFM es la revisión y comparación de distintos algoritmos de machine-learning para acústica pasiva. • Implementación de los algoritmos de interés. • Aplicación a la discriminación de señales acústicas en detectores de partículas

[EN] In the framework of the search for dark matter in the form of WIMPs using superheated liquids, a study is conducted to establish a computational procedure aimed at determining how the thermodynamic conditions kept inside a particle detector affect the acoustic signal produced by bubble nucleation. It is found that the acoustic energy injected into the liquid by the growing vapour bubble increases as the liquid pressure is decreased and the superheat degree is increased, the former effect being crucial for the generation of a well-intelligible signal. A good agreement is met between the results of the present study and some experimental data available in the literature for the amplitude of the acoustic signal. Additionally, the higher loudness of the alpha-decay events compared with those arising from neutron-induced nuclear recoils is described in terms of multiple nucleations.

[EN] In the past decade, a new class of bright transient radio sources with millisecond duration has been discovered. The origin of these so-called fast radio bursts (FRBs) is still a mystery, despite the growing observational efforts made by various multiwavelength and multimessenger facilities. To date, many models have been proposed to explain FRBs, but neither the progenitors nor the radiative and the particle acceleration processes at work have been clearly identified. In this paper, we assess whether hadronic processes may occur in the vicinity of the FRB source. If they do, FRBs may contribute to the high-energy cosmic-ray and neutrino fluxes. A search for these hadronic signatures was carried out using the ANTARES neutrino telescope. The analysis consists in looking for high-energy neutrinos, in the TeV-PeV regime, that are spatially and temporally coincident with the detected FRBs. Most of the FRBs discovered in the period 2013-2017 were in the field of view of the ANTARES detector, which is sensitive mostly to events originating from the Southern hemisphere. From this period, 12 FRBs were selected and no coincident neutrino candidate was observed. Upper limits on the per-burst neutrino fluence were derived using a power-law spectrum, dN/DE nu proportional to E-nu(-gamma), for the incoming neutrino flux, assuming spectral indexes gamma = 1.0, 2.0, 2.5. Finally, the neutrino energy was constrained by computing the total energy radiated in neutrinos, assuming different distances for the FRBs. Constraints on the neutrino fluence and on the energy released were derived from the associated null results.

[EN] Hadrontherapy makes it possible to deliver high doses of energy to cancerous tumors by using the large energy deposition in the Bragg-peak. However, uncertainties in the patient positioning and/or in the anatomical parameters can cause distortions in the calculation of the dose distribution. In order to maximize the effectiveness of heavy particle treatments, an accurate monitoring system of the deposited dose depending on the energy, beam time, and spot size is necessary. The localized deposition of this energy leads to the generation of a thermoacoustic pulse that can be detected using acoustic technologies. This article presents different experimental and simulation studies of the acoustic localization of thermoacoustic pulses captured with a set of sensors around the sample. In addition, numerical simulations have been done where thermo-acoustic pulses are emitted for the specific case of a proton beam of 100 MeV.

[ES] La temática del siguiente trabajo gira alrededor de la arquitectura bioclimática. El objetivo se centra en el estudio de dos sistemas, el muro Trombe y el muro EcoCooler. Ambos destinados a conseguir el bienestar y confort higrotérmico en las viviendas aprovechando las condiciones ambientales y minimizando el consumo energético. Se han desarrollado ensayos para cuantificar y poder llegar a una conclusión de la eficacia de estos sistemas. Los experimentos desarrollados se han realizado tanto en laboratorio, en condiciones controladas, como en el exterior. Los resultados obtenidos permiten mejorar la comprensión del desarrollo de estos sistemas., [EN] This project is about bioclimatic architecture. The objective is the study of two systems, the Trombe wall and the EcoCooler wall. Both systems have been designed to achieve the hygrothermal comfort in homes taking advantage of environmental conditions and reducing the energy consumption. Models have been developed to quantify and be able to reach a conclusion about the effectiveness of these systems. The experiments developed have been carried out both in the laboratory, under controlled conditions, and outside. The results obtained allow for an improved understanding of their development.

[EN] The results of three different searches for neutrino candidates, associated with the IceCube-170922A event or from the direction of TXS 0506+056, by the ANTARES neutrino telescope, are presented. The ¿rst search refers to the online follow-up of the IceCube alert; the second is based on the standard time-integrated method employed by the Collaboration to search for point-like neutrino sources; the third uses information from the IceCube time-dependent analysis that reported bursting activity centered on 2014 December 13, as input for an ANTARES time-dependent analysis. The online follow-up and the time-dependent analysis yield no events related to the source. The time-integrated study performed over a period from 2007 to 2017 ¿ts 1.03 signal events, which corresponds to a p-value of 3.4% (not considering trial factors). Only for two other astrophysical objects in our candidate list has a smaller p-value been found. When considering that 107 sources have been investigated, the post-trial p-value for TXS 0506+056 corresponds to 87%.

[EN] One of the main objectives of the ANTARES telescope is the search for point-like neutrino sources. Both the pointing accuracy and the angular resolution of the detector are important in this context and a reliable way to evaluate this performance is needed. In order to measure the pointing accuracy of the detector, one possibility is to study the shadow of the Moon, i.e. the de¿cit of the atmospheric muon ¿ux from the direction of the Moon induced by the absorption of cosmic rays. Analysing the data taken between 2007 and 2016, the Moon shadow is observed with 3.5¿ statistical signi¿cance. The detector angular resolution for downward-going muons is 0.73¿ ±0.14¿. The resulting pointing performance is consistent with the expectations. An independent check of the telescope pointing accuracy is realised with the data collected by a shower array detector onboard of a ship temporarily moving around the ANTARES location.

[EN] Neutrino telescopes have been proposed as efficient tools for indirect dark matter searches, especially using the Sun as source for its good capability to capture dark matter and since we do not expect high-energy neutrinos from it. However, the last statement should be taken with caution because high-energy neutrinos may come from cosmic particle interactions in the atmosphere of the Sun and producing neutrinos. In this work, we describe an analysis of the ANTARES neutrino telescope optimised for the observation of neutrinos coming from the atmosphere of the Sun due to cosmic particles interactions. Focusing in the 10 GeV - 10 TeV energy range and using 2007-2012 data, the sensitivity obtained for the flux is approximately 1012 km-2 y -1 , whereas the expected flux is two order of magnitudes below. From this, we can conclude that present high-energy neutrino telescopes dark matter searches in the Sun can indeed neglect this contribution, but could play a role in future detectors with better neutrino flux sensitivities in the 10 GeV - 10 TeV energy range and very good angular resolution.

[EN] The existence of diffuse Galactic neutrino production is expected from cosmic-ray interactions with Galactic gas and radiation ¿elds. Thus, neutrinos are a unique messenger offering the opportunity to test the products of Galactic cosmic-ray interactions up to energies of hundreds of TeV. Here we present a search for this production using ten years of Astronomy with a Neutrino Telescope and Abyss environmental RESearch (ANTARES) track and shower data, as well as seven years of IceCube track data. The data are combined into a joint likelihood test for neutrino emission according to the KRAg model assuming a 5 PeV per nucleon Galactic cosmic-ray cutoff. No signi¿cant excess is found. As a consequence, the limits presented in this Letter start constraining the model parameter space for Galactic cosmic-ray production and transport.

[EN] This paper presents a study of different types of parametric signals with application to submarine acoustic telecommunications. In all of them, the carrier frequency is 200 kHz, which corresponds to that resonation of the transducer under study, while they differ by the different modulations they present. In this sense, we study modulations with sweeps (4 to 40 kHz), in which represent binary codes (zeros and ones), getting closer to the application in acoustic telecommunications. The different properties of the transmitting signals in terms of communication speed, directivity, efficiency and power needed are discussed as well.

[EN] We report the discovery of four Fast Radio Bursts (FRBs) in the ongoing SUrvey for Pulsars and Extragalactic Radio Bursts at the Parkes Radio Telescope: FRBs 150610, 151206, 151230 and 160102. Our real-time discoveries have enabled us to conduct extensive, rapid multimes-senger follow-up at 12 major facilities sensitive to radio, optical, X-ray, gamma-ray photons and neutrinos on time-scales ranging from an hour to a few months post-burst. No counterparts to the FRBs were found and we provide upper limits on afterglow luminosities. None of the FRBs were seen to repeat. Formal ¿ts to all FRBs show hints of scattering while their intrinsic widths are unresolved in time. FRB 151206 is at low Galactic latitude, FRB 151230 shows a sharp spectral cut-off, and FRB 160102 has the highest dispersion measure (DM = 2596.1 ± 0.3 pc cm¿3) detected to date. Three of the FRBs have high dispersion measures (DM > 1500 pc cm¿3), favouring a scenario where the DM is dominated by contributions from the intergalactic medium. The slope of the Parkes FRB source counts distribution with ¿uences >2Jyms is ¿ =¿2.2+01..62 and still consistent with a Euclidean distribution (¿ =¿3/2). We also ¿nd that the all-sk¿y rate is 1.7+¿10..59 × 103FRBs/(4¿ sr)/day above ~2 Jy ms and there is currently no strong evidence for a latitude-dependent FRB sky rate.

[EN] The ANTARES detector is at present the most sensitive neutrino telescope in the northern hemisphere. The highly signi¿cant cosmic neutrino excess observed by the Antarctic IceCube detector can be studied with ANTARES, exploiting its complementing ¿eld of view, exposure, and lower energy threshold. Searches for an all-¿avor diffuse neutrino signal, covering nine years of ANTARES data taking, are presented in this Letter. Upward-going events are used to reduce the atmospheric muon background. This work includes for the ¿rst time in ANTARES both track-like (mainly nm) and shower-like (mainly ne) events in this kind of analysis. Track-like events allow for an increase of the effective volume of the detector thanks to the long path traveled by muons in rock and/or sea water. Shower-like events are well reconstructed only when the neutrino interaction vertex is close to, or inside, the instrumented volume. A mild excess of high-energy events over the expected background is observed in nine years of ANTARES data in both samples. The best ¿t for a single power-law cosmic neutrino spectrum, in terms of per-¿avor ¿ux at 100 TeV, is (1.7+-1.0)10-18 GeV¿1 cm¿2 s¿1 sr¿1 with spectral index G=2.4+0.5-0.4. The null cosmic ¿ux assumption is rejected with a signi¿cance of 1.6¿.

[EN] This paper presents a study of different types of parametric signals with application to underwater acoustic communications. In all the signals, the carrier frequency is 200 kHz, which corresponds to the resonance frequency of the transducer under study and different modulations are presented and compared. In this sense, we study modulations with parametric sine sweeps (4 to 40 kHz) that represent binary codes (zeros and ones), getting closer to the application in acoustic communications. The different properties of the transmitting signals in terms of bit rate reconstruction, directivity, efficiency, and power needed are discussed as well.

El objetivo de este proyecto consiste en implementar un sistema autónomo basado en Arduino para monitorizar ciertos parámetros termodinámicos, como son la temperatura, la humedad y la radiación solar, para posteriormente analizar los resultados obtenidos en diferentes situaciones. El funcionamiento de este sistema se comprueba tanto en condiciones de laboratorio como mediante medidas in situ de elementos constructivos y de espacios habitables. Algunos de los experimentos realizados se contrastan con simulaciones numéricas que permitirán entender el sistema implementado en su conjunto., The objective of this project is to implement an autonomous system based on Arduino to monitor certain thermodynamic parameters, such as temperature, humidity, and solar radiation, and then analyze the results obtained in different situations. The operation of this system is tested both in laboratory conditions and by on-site measurements of construction elements and living spaces. Some of the experiments carried out are contrasted with numerical simulations that will allow us to understand the system implemented.

[EN] Bubble chambers used in detectors for detecting dark matter use piezoelectric sensors in order to detect and discriminate the acoustic signals from bubbles growth in the superheated liquid when a particle interaction occurs. The Research Group in Applied Acoustics to Astroparticles Detection from UPV developed a particle detector, whose acoustic sensors are attached to the outer walls of the chamber. In order to optimize the operation of the sensor, both analytical and numerical models are developed, as well as experimental tests for characterization of sensors design were performed. The results of these studies allows a particular design criterion for the construction of such sensor for future dark matter bubble chamber detectors., [ES] Las cámaras de burbujas empleadas en los detectores para la detección de materia oscura, utilizan sensores piezoeléctricos para detectar y discriminar las señales acústicas emitidas por las burbujas que se generan a partir de la interacción de partículas con el fluido sobrecalentado presente en el interior de dicha cámara. El grupo de Investigación en Acústica Aplicada a la Detección de Astropartículas de la UPV ha desarrollado un modelo de detector de partículas, cuyos sensores acústicos se encuentran pegados en las paredes exteriores de la cámara. Con el objetivo de entender el comportamiento y optimizar el funcionamiento del sensor, se desarrollan modelos analíticos y numéricos, así como pruebas experimentales para su caracterización. Los resultados de estos estudios permiten tener un criterio de diseño para la adecuada construcción de tales sensores en futuras cá- maras de burbujas para la detección de materia oscura

[EN] Cherenkov light induced by radioactive decay products is one of the major sources of background light for deep-sea neutrino telescopes such as ANTARES. These decays are at the same time a powerful calibration source. Using data collected by the ANTARES neutrino telescope from mid 2008 to 2017, the time evolution of the photon detection ef¿ciency of optical modules is studied. A modest loss of only 20% in 9 years is observed. The relative time calibration between adjacent modules is derived as well.

The research group on Acoustics Applied to the Detection of Astroparticles of the UPV collaborates in the development of the KM3NeT neutrino telescope. Currently, an array calibrator is developed to emulate the acoustic pulse of the neutrino when it interacts with the water and calibrates the hydrophones of the telescope. Said pulse has the characteristic that being of a low frequency between 20 to 50 kHz, has a very narrow directivity pattern. In this work, a previous study with parametric signals is made that allows us to understand the generation of the parametric effect using a flat transducer. To characterise an element of the array calibrator by studying the linear and nonlinear magnitudes of directivity, attenuation and voltage variation, and presenting an adjustment value that shows the generation of the parametric effect, especially appreciable with the parametric sweep signals of long duration (1000 ¿s). Finally, a simulation of the behavior in directivity of the array of 5 elements is performed, hoping that from 100 m the entire array behaves as a single element., El grupo de investigación en Acústica Aplicada a la Detección de Astropartículas de la UPV colabora en el desarrollo del Telescopio de neutrinos KM3NeT. Actualmente, se desarrolla un calibrador en forma de array para emular el pulso acústico del neutrino cuando este interactúa en el agua y calibrar así los hidrófonos del telescopio. Dicho pulso, tiene la característica que siendo de baja frecuencia entre los 20 a 50 kHz, presenta un patrón de directividad bastante estrecho. En este trabajo se realiza un estudio previo con señales paramétricas que permiten entender la generación del efecto paramétrico empleando un transductor plano. Para posteriormente, caracterizar un elemento del array calibrador estudiando las magnitudes lineales y no lineales de directividad, atenuación y variación de voltaje, y presentando un valor de ajuste que evidencia la generación del efecto paramétrico, especialmente apreciable con la señales sweep paramétricas de larga duración (1000 µs). Finalmente, se realiza una simulación del comportamiento en directividad del array de 5 elementos, esperando que a partir de los 100 m todo el array se comporte como un único elemento.

[EN] Gamma-ray bursts are thought to be sites of hadronic acceleration, thus neutrinos are expected from the decay of charged particles, produced in p gamma interactions. The methods and results of a search for muon neutrinos in the data of the ANTARES neutrino telescope from four bright GRBs (GRB 080916C, GRB 110918A, GRB 130427A and GRB 130505A) observed between 2008 and 2013 are presented. Two scenarios of the fireball model have been investigated: the internal shock scenario, leading to the production of neutrinos with energies mainly above 100 TeV, and the photospheric scenario, characterized by a low-energy component in neutrino spectra due to the assumption of neutrino production closer to the central engine. Since no neutrino events have been detected in temporal and spatial coincidence with these bursts, upper limits at 90 per cent confidence level on the expected neutrino fluxes are derived. The non-detection allows for directly constraining the bulk Lorentz factor of the jet Gamma and the baryon loading f(p)

[EN] ANTARES is currently the largest neutrino telescope operating in the Northern Hemisphere, aiming at the detection of high-energy neutrinos from astrophysical sources. Neutrino telescopes constantly monitor at least one complete hemisphere of the sky, and are thus well-suited to detect neutrinos produced in transient astrophysical sources. A time-dependent search has been applied to a list of 33 X-ray binaries undergoing high flaring activities in satellite data (RXTE/ASM, MAXI and Swift/BAT) and during hardness transi-tion states in the 2008 2012 period. The background originating from interactions of charged cosmic rays in the Earth s atmosphere is drastically reduced by requiring a directional and temporal coincidence with astrophysical phenomena. The results of this search are presented together with comparisons between the neutrino flux upper limits and the neutrino flux predictions from astrophysical models. The neutrino flux upper limits resulting from this search limit the jet parameter space for some astrophysical models.

[EN] Despite dedicated research has been carried out to adequately map the distribution of the sperm whale in the Mediterranean Sea, unlike other regions of the world, the species population status is still presently uncertain. The analysis of two years of continuous acoustic data provided by the ANTARES neutrino telescope revealed the year-round presence of sperm whales in the Ligurian Sea, probably associated with the availability of cephalopods in the region. The presence of the Ligurian Sea sperm whales was demonstrated through the real-time analysis of audio data streamed from a cabled-to- shore deep-sea observatory that allowed the hourly tracking of their long-range echolocation behaviour on the Internet. Interestingly, the same acoustic analysis indicated that the occurrence of surface shipping noise would apparently not condition the foraging behaviour of the sperm whale in the area, since shipping noise was almost always present when sperm whales were acoustically detected. The continuous presence of the sperm whale in the region confirms the ecological value of the Ligurian sea and the importance of ANTARES to help monitoring its ecosystems

[EN] On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40-+88 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M¿. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identi¿cation of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient¿s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993followedbyashortgamma-rayburst(GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.

[EN] A search for magnetic monopoles using five years of data recorded with the ANTARES neutrino telescope from January 2008 to December 2012 with a total live time of 1121 days is presented. The analysis is carried out in the range b>0.6 of magnetic monopole velocities using a strategy based on run-by-run Monte Carlo simulations. No signal above the background expectation from atmospheric muons and atmospheric neutrinos is observed, and upper limits are set on the magnetic monopole flux ranging from 5.7x10-16 to 1.5x10-18 cm-2 . s-1.sr-1.

[EN] New results are reported from the operation of the PICO-60 dark matter detector, a bubble chamber filled with 52 kg of C3F8 located in the SNOLAB underground laboratory. As in previous PICO bubble chambers, PICO-60 C3F8 exhibits excellent electron recoil and alpha decay rejection, and the observed multiple-scattering neutron rate indicates a single-scatter neutron background of less than one event per month. A blind analysis of an efficiency-corrected 1167-kg day exposure at a 3.3-keV thermodynamic threshold reveals no single-scattering nuclear recoil candidates, consistent with the predicted background. These results set the most stringent direct-detection constraint to date on the weakly interacting massive particle (WIMP)-proton spin-dependent cross section at 3.4 x 10(-41) cm(2) for a 30-GeVc(-2) WIMP, more than 1 order of magnitude improvement from previous PICO results.

[EN] A search for high-energy neutrino emission cor-related with gamma-ray bursts outside the electromagnetic prompt-emission time window is presented. Using a stack-ing approach of the time delays between reported gamma-ray burst alerts and spatially coincident muon-neutrino sig-natures, data from the Antares neutrino telescope recorded between 2007 and 2012 are analysed. One year of public data from the IceCube detector between 2008 and 2009 have been also investigated. The respective timing profiles are scanned for statistically significant accumulations within 40 days of the Gamma Ray Burst, as expected from Lorentz Invariance Violation effects and some astrophysical models. No signif-icant excess over the expected accidental coincidence rate could be found in either of the two data sets. The average strength of the neutrino signal is found to be fainter than one detectable neutrino signal per hundred gamma-ray bursts in the Antares data at 90% confidence level.

[EN] Advanced LIGO detected a significant gravitational wave signal (GW170104) originating from the coalescence of two black holes during the second observation run on January 4th, 2017. Anall-sky high-energy neutrino follow-up search has been made using data from the Antares neutrino telescope, including both upgoing and downgoing events in two separate analyses. No neutrino candidates were found within +/- 500 s around the GW event time nor any time clustering of events over an extended time window of +/- 3 months. The non-detection is used to constrain isotropic-equivalent high-energy neutrino emission from GW170104 to less than similar to 1.2 x 10(55) erg for a E-2 spectrum. This constraint is valid in the energy range corresponding to the 5-95% quantiles of the neutrino flux [3.2 TeV; 3.6 PeV], if the GW emitter was below the Antares horizon at the alert time.

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved., [EN] We report on the discovery of a new fast radio burst (FRB), FRB 150215, with the Parkes radio telescope on 2015 February 15. The burst was detected in real time with a dispersion measure (DM) of 1105.6 ± 0.8 pc cm-3;3, a pulse duration of 2.8+1.2-0.25 ms, and a measured peak flux density assuming that the burst was at beam centre of 0.7+0.2-0.1 Jy. The FRB originated at a Galactic longitude and latitude of 24.66º,5.28º and 25º away from the Galactic Center. The burst was found to be 43 ± 5 per cent linearly polarized with a rotation measure (RM) in the range -9 < RM < 12 rad m-2 (95 per center confidence level), consistent with zero. The burst was followed up with 11 telescopes to search for radio, optical, X-ray, gamma-ray and neutrino emission. Neither transient nor variable emission was found to be associated with the burst and no repeat pulses have been observed in 17.25 h of observing. The sightline to the burst is close to the Galactic plane and the observed physical properties of FRB 150215 demonstrate the existence of sight lines of anomalously low RM for a given electron column density. The Galactic RM foreground may approach a null value due to magnetic field reversals along the line of sight, a decreased total electron column density from the Milky Way, or some combination of these effects. A lower Galactic DM contribution might explain why this burst was detectable whereas previous searches at low latitude have had lower detection rates than those out of the plane.

[EN] Using data recorded with the ANTARES telescope from 2007 to 2015, a new search for dark matter annihilation in the Milky Way has been performed. Three halo models and five annihilation channels, WIMP + WIMP -> b (b) over bar, W+W-, tau(+)tau(-), mu(+)mu(-) and v (v) over bar, with WIMP masses ranging from 50 2 GeV/C-2 to 100 Tev/C-2, were considered. No excess over the expected background was found, and limits on the thermally averaged annihilation cross-section were set.

Dark matter detectors based on superheated fluids set WIMP-nucleus interaction limits based on registering acoustic signals in combination with the information of other sensors. For this reason, in order to distinguish the background events from those originated by new particle interactions, it is crucial to know the behaviour of the acoustic signal within the detector. The aim of this Thesis is to study the set of acoustic techniques and technologies necessary for the analysis, characterization and optimization of the different parts that compose a dark matter detector based on superheated fluids. From these studies, we draw conclusions for the design of a Geyser detector. The research is organized in four Chapters that approach the processes that take place from the bubble generation in the superheated fluid to the discrimination analysis. The study begins in Chapter I, where we study the interaction of WIMPs with matter and the consequent bubble creation and growth. In Chapter II we analyse the acoustic processes from the emitted sound wave in the growth of these bubbles, until they arrive at the sensors, going through the different media of the detector. Chapter III deals with the characterization, design and optimization of the transducers that record these acoustic signals. In Chapter IV, the signal processing techniques are studied in order to extract the greatest amount of information from the different signals of interest, as well as the characteristics of the sources. Finally, in Chapter V, we present the conclusions of these researches for the design and control of the proposed Geyser detector, called MODA-LS. In addition, due to its importance in the increasingly sensitive dark matter searches, we analyse the so-called neutrino sensitivity grounds, both in direct dark matter searches with superheated fluids and indirect searches with neutrino telescopes, in Annexes A and B respectively. All these activities form a common and unified framework in this new, Lo detectores de materia oscura basados en fluidos sobrecalentados establecen límites de interacción WIMP-núcleo a partir de, entre otros aspectos, las señales acústicas registradas. Por ello, entender los distintos aspectos que puedan influir en dicha señal acústica es crucial para distinguir los eventos que provengan de fondos indeseados respecto a los de interacciones de nuevas partículas. El objetivo de esta Tesis es abordar el estudio del conjunto de técnicas y tecnologías acústicas necesarias para el análisis, caracterización y optimización de las distintas partes que componen un detector de materia oscura basado en fluidos sobrecalentados. Con ello, se extraen conclusiones para el diseño de un detector Geyser. La investigación se organiza en cuatro Capítulos que abordan los procesos que tiene lugar desde la generación de burbujas en el fluido sobrecalentado hasta el análisis para su discriminación. El estudio se inicia en el Capítulo I, donde se estudia la interacción de los WIMP con la materia y la consiguiente creación y crecimiento de burbujas. En el Capítulo II se analizan los procesos acústicos que tienen lugar desde se emiten las ondas acústicas en el crecimiento de estas burbujas, hasta que llegan a los sensores, a través de los distintos medios que conforman un detector. En el Capítulo III se aborda la caracterización, diseño y optimización de los transductores que registran estas señales. En el Capítulo IV se estudian las técnicas de procesado de señal para extraer la mayor cantidad de información de las distintas señales de interés, así como de las características de las fuentes que las generan. Por último, en el Capítulo V, se exponen las conclusiones de estas investigaciones para el diseño y control del detector Geyser propuesto, MODA-LS. Adicionalmente, dada su importancia en la cada vez más sensible búsqueda de materia oscura, en los Anexos A y B analizamos los llamados suelos de sensibilidad por neutrinos, tanto en búsqueda directa de materia o, Els detectors de matèria fosca basats en fluids sobreescalfats estableixen els límits d'interacció WIMP-nucli a partir de, entre altres aspectes, les senyals acústiques registrades. Llavors, entendre els aspectes que puguin influir en aquesta senyal acústica és crucial per a distingir els esdeveniments provinents de fons no desitjats respecte als de interaccions de noves partícules. L'objectiu d'aquesta Tesis és abordar l'estudi del conjunt de tècniques i tecnologies acústiques necessàries per a l'anàlisi, caracterització i optimització de les distintes parts que conformen un detector de matèria fosca basat en fluids sobreescalfats. Amb això, s'extrauen conclusions per al disseny d'un detector Geyser. La investigació s'organitza en quatre Capítols que aborden els processos que tenen lloc des de la generació de bombolles en el fluid sobreescalfat fins a l'anàlisi per a la seva discriminació. L'estudi s'inicia en el Capítol I, amb la interacció dels WIMP amb la matèria i la consegüent creació i creixement de bombolles. Al Capítol II s'analitzen els processos acústics que tenen lloc des que s'emeten les ones acústiques en el creixement d'aquestes bombolles fins que arriben als sensors, a través dels diferents medis que conformen un detector. Al Capítol III es tracta la caracterització, disseny i optimització dels transductors que registren aquests senyals. Al Capítol IV s'estudien les tècniques de processat de senyal per extreure la major quantitat d'informació així com de les característiques de les fonts que les generen. Finalment, al Capítol V, s'exposen les conclusions d'aquestes investigacions per al disseny i control del detector Geyser proposat, MODA-LS. Addicionalment, donada la seva importància en la cada vegada més sensible cerca de matèria fosca, en els annexos A i B analitzem els anomenats sòls de sensibilitat per neutrins, tant en cerca directa de matèria fosca amb fluids sobreescalfats com indirecta per als telescopis de neutrins, respectivament. Tots aqu

A novel algorithm to reconstruct neutrino-induced particle showers within the ANTARES neutrino telescope is presented. The method achieves a median angular resolution of 6º, for shower energies below 100 TeV. Applying this algorithm to 6 years of data taken with the ANTARES detector, 8 events with reconstructed shower energies above 10 TeV are observed. This is consistent with the expectation of about 5 events from atmospheric backgrounds, but also compatible with diffuse astrophysical flux measurements by the IceCube collaboration, from which 2 4 additional events are expected. A 90% C.L. upper limit on the diffuse astrophysical neutrino flux with a value per neutrino flavour of E2·Oi 90% =4.9 cm-2· sr-1 is set, applicable to the energy range from 23 TeV to 7.8 PeV, assuming an unbroken E-2 spectrum and neutrino flavour equipartition at Earth.

La tecnología usada en detectores para la búsqueda de materia oscura utilizan sensores piezoeléctricos. El grupo de Investigación en Acústica Aplicada a la Detección de Astropartículas de la UPV trabaja en el desarrollo de un detector de partículas, junto a él se ha realizado este trabajo en el cual se desarrolla un estudio sobre la caracterización de materiales piezoeléctricos y su comportamiento en cerámicas PZT. Se usa el método de la impedancia para caracterizar medidas de frecuencia de resonancia y antiresonancia, que posteriormente son utilizadas para resolver coeficientes que definen las matrices de comportamiento piezoeléctrico. Una vez analizadas se estudia mediante elementos finitos en COMSOL Multyphisic y cuyos resultados se comparan con las mediciones hechas en laboratorio. Una vez realizado el estudio previo se pasa a la fase de optimización donde se simularán los coeficientes obtenidos variando sus dimensiones para poder analizar su mejor comportamiento. Todo ello con un material innovador como son las cerámicas radiopuras, The technology used in the detectors for the search of dark matter uses piezoelectric sensors. The group of search in Applied Acoustic to the detection of Astroparticles of the UPVworks in developing of a study about the characterization of piezoelectric materials and their behaviour in PZT ceramics. Impedance method is used to characterize not only resonance frequency measures, but also nonresonance ones, which are later used to solve coefficients which define piezoelectric behaviour matrices. Once they have already been analyzed, they are studied with finite elements in COMSOL Multyphisic and their results are compared to measurements taken in the laboratory. After having finished with the previous study, we move to optimization phase where coefficients will be simulated varying their dimensions to be able to analyze their best behaviour. All this process is performed with an innovative materials which are known as radiopure ceramics

[EN] The flux of very high-energy neutrinos produced in our Galaxy by the interaction of accelerated cosmic rays with the interstellar medium is not yet determined. The characterization of this flux will shed light on Galactic accelerator features, gas distribution morphology and Galactic cosmic ray transport. The central Galactic plane can be the site of an enhanced neutrino production, thus leading to anisotropies in the extraterrestrial neutrino signal as measured by the IceCube Collaboration. The ANTARES neutrino telescope, located in the Mediterranean Sea, offers a favorable view of this part of the sky, thereby allowing for a contribution to the determination of this flux. The expected diffuse Galactic neutrino emission can be obtained, linking a model of generation and propagation of cosmic rays with the morphology of the gas distribution in the Milky Way. In this paper, the so-called "gamma model" introduced recently to explain the high-energy gamma-ray diffuse Galactic emission is assumed as reference. The neutrino flux predicted by the "gamma model" depends on the assumed primary cosmic ray spectrum cutoff. Considering a radially dependent diffusion coefficient, this proposed scenario is able to account for the local cosmic ray measurements, as well as for the Galactic gamma-ray observations. Nine years of ANTARES data are used in this work to search for a possible Galactic contribution according to this scenario. All flavor neutrino interactions are considered. No excess of events is observed, and an upper limit is set on the neutrino flux of 1.1 (1.2) times the prediction of the "gamma model," assuming the primary cosmic ray spectrum cutoff at 5 (50) PeV. This limit excludes the diffuse Galactic neutrino emission as the major cause of the "spectral anomaly" between the two hemispheres measured by IceCube.

[EN] The Advanced LIGO observatories detected gravitational waves from two binary black hole mergers during their first observation run (O1). We present a high-energy neutrino follow-up search for the second gravitational wave event, GW151226, as well as for gravitational wave candidate LVT151012. We find two and four neutrino candidates detected by IceCube, and one and zero detected by ANTARES, within +/- 500 s around the respective gravitational wave signals, consistent with the expected background rate. None of these neutrino candidates are found to be directionally coincident with GW151226 or LVT151012. We use nondetection to constrain isotropic-equivalent high-energy neutrino emission from GW151226, adopting the GW event's 3D localization, to less than 2 x 10(51)-2 x 10(54) erg.

[EN] A search for cosmic neutrino sources using the data collected with the ANTARES neutrino telescope between early 2007 and the end of 2015 is performed. For the first time, all neutrino interactions-charged and neutral-current interactions of all flavors-are considered in a search for point-like sources with the ANTARES detector. In previous analyses, only muon neutrino charged-current interactions were used. This is achieved by using a novel reconstruction algorithm for shower-like events in addition to the standard muon track reconstruction. The shower channel contributes about 23% of all signal events for an E-2 energy spectrum. No significant excess over background is found. The most signal-like cluster of events is located at (alpha, delta) = (343.8 degrees, 23.5 degrees) with a significance of 1.9 sigma. The neutrino flux sensitivity of the search is about E(2)d Phi/dE = 6 x 10(-9) GeV cm(-2) s(-1) for declinations from -90 degrees up to -42 degrees, and below 10(-8) GeV cm(-2) s(-1) for declinations up to 5 degrees. The directions of 106 source candidates and 13 muon track events from the IceCube high-energy sample events are investigated for a possible neutrino signal and upper limits on the signal flux are determined.

[EN] The MOSCAB experiment (Materia OSCura A Bolle) uses the "geyser technique", a variant of the superheated liquid technique of extreme simplicity. Operating principles of the new dark matter detector and technical solutions of the device are reported in detail. First results obtained in a series of test runs taken in laboratory demonstrate that we have successfully built and tested a geyser-concept bubble chamber that can be used in particle physics, especially in dark matter searches, and that we are ready to move underground for extensive data taking.

[EN] Circular piezoelectric transducers with axial polarization are proposed as low frequency acoustic sensors for dark matter bubble chamber detectors. The axial vibration behaviour of the transducer is studied by three different methods: analytical models, FEM simulation, and experimental setup. To optimize disk geometry for this application, the dependence of the vibrational modes in function of the diameter-to-thickness ratio from 0.5 (a tall cylinder) to 20.0 (a thin disk) has been studied. Resonant and antiresonant frequencies for each of the lowest modes are determined and electromechanical coupling coefficients are calculated. From this analysis, due to the requirements of radiopurity and little volume, optimal diameter-to-thickness ratios for good transducer performance are discussed.