Simeone

Underwater acoustic detection of UHE neutrinos with the ANTARES experiment

Abstract

The ANTARES Neutrino Telescope is a water Cherenkov detector composed of an array of approximately 900 photomultiplier tubes in 12 vertical strings, spread over an area of about 0.1 km with an instrumented height of about 350 metres. ANTARES, built in the Mediterranean Sea, is the biggest neutrino telescope operating in the northern hemisphere. Acoustic sensors (AMADEUS project) have been integrated into the infrastructure of ANTARES, grouped in small arrays, to evaluate the feasibility of a future acoustic neutrino telescope in the deep sea operating in the ultra-high energy regime. In this contribution, the basic principles of acoustic neutrino detection will be presented. The AMADEUS array of acoustic sensors will be described and the latest results of the project summarized.

{IEEEkeywords}

Acoustic neutrino detection, Beam-Forming, AMADEUS

missingmissing1 missingIntroduction

Almost everything we know about the Universe came from its observation by means of electromagnetic radiation. Using photons as observation probe it has been possible to discover very energetic sources. However, photons are highly absorbed by matter and so their observation only allows us to directly obtain information of the surface process at the source. Moreover energetic photons interact with the infrared photon background and are attenuated during their travel from the source toward us.
Observation of the proton component of cosmic rays can give information about the sources but, since they are charged, low energy protons are deflected by the magnetic galactic fields and loose the directional information that would allow us to point back to their source. Ultra high energy protons are slightly deflected by magnetic fields and in principle could be a good probe for the high energy Universe. Unfortunately, as pointed out by Greisen-Zatsepin-Kuz’min [1] [2], the proton interactions with the CMBR(GZK effect) will reduce the proton energy and make them not useful as astroparticle probes for the high energy Universe.
In order to directly observe the physical mechanism of distant and energetic sources we need to use a neutral, stable and weakly interacting messenger: the neutrino. The interest in studying such high energy sources arises from the fact that much of the classical astronomy is related to the study of the thermal radiation, emitted by stars or dust, while the non thermal energy density in the Universe is roughly equal to the thermal one and it is assumed to play a relevant role in its evolution.
The experimental techniques proposed to identify the cosmic neutrino signatures are mainly three: the detection of Cherenkov light originating from charged leptons produced by neutrino interactions in water or ice; the detection of acoustic waves produced by neutrino induced energy deposition in water, ice or salt; the detection of radio pulses following a neutrino interaction in ice or salt.

Figure 1: Acoustic storeys are present in four different configurations; two of them contain commercial hydrophones (one upward and one downward looking), one contains custom built hydrophones and the last is made of sensors inside three glass spheres.

2 Acoustic neutrino detection

The acoustic detection technique of neutrino-induced cascades, in water or ice, is based on the thermo-acoustic effect [3] [4]. The cascade energy is deposited in a narrow region of the medium, inducing a local heating and resulting in a rapid expansion of the water (or ice). The simultaneous expansion of the medium along the shower leads to a coherent sound emission in the plane perpendicular to the shower axis.
Simulations performed by many authors [5] [6] show that the bipolar acoustic neutrino pulse is tens of microseconds long and has a peak-to-peak amplitude of about 100 mPa at 1km distance if originated by a shower of 10 eV. The signal is largely collimated in the plane perpendicular to the shower axis and its amplitude decreases by almost two order of magnitude in few degrees.
The acoustic detectors are composed of many acoustic sensors distributed in a wide instrumented volume; by measuring the acoustic induced neutrino pulse with several sensors it will be possible to infer the shower direction. The interest in this technique is related to the high attenuation length (km) of the sound in water (or ice). Consequently it is possible to instrument a large volume using a relatively low number of sensors.

3 AMADEUS project

The AMADEUS [7] (Antares Modules for Acoustic DEtection Under the Sea) project is fully integrated into the ANTARES [8] [9] [10] Cherenkov neutrino telescope (Fig. 1); Its main goal is to evaluate the feasibility of a future acoustic neutrino telescope in the deep sea operating in the ultra-high energy regime.
ANTARES is located in the Mediterranean Sea about 40 km south of Toulon (France) at a depth of about 2500m. It is composed of 12 vertical structures, called lines and labeled L1 - L12. An additional line (IL07) is equipped with several instruments used for environmental monitoring. Each detection line holds up to 25 storeys, each of them contains three photomultipliers (PMTs) and the electronics needed to acquire the PMT signals and send them to shore. The storeys are vertically separated by 14.5 m starting at a height of about 100m above sea floor. Each line is fixed to the sea floor by an anchor and held vertically by a buoy.
Three special storeys (Acoustic Storeys) are present on both L12 and IL7, each storey contains six acoustic sensors and the electronics used to acquire, pre-process and send the samples to the onshore laboratory. The hydrophones signals are amplified up to a sensitivity of 0.05V/Pa, filtered using a bandpass filter from 1 kHz to 100 kHz and sampled at 250 ksps with a resolution of 16 bit. The acquisition system is able to produce up to 1.5 TB per day; in order to select interesting signals and reduce the data rate as well as the storage requirements, three online triggers are implemented at level of the acoustic storey:

  • Minimum bias filter, that stores 10 s of samples every hour.

  • Threshold filter, that store signals of amplitude greater than the selected threshold.

  • Matched filter, that store signals of cross correlation with the expected bipolar signal greater than the selected threshold.

These filters reduce the data sent to the onshore laboratory by two orders of magnitude. The AMADEUS project is fully integrated into the ANTARES data acquisition system, in particular all the samples acquired by AMADEUS are tagged with an absolute time, common to the whole experiment, with a precision better than 1ns. This allows to correlate acoustic signals acquired in different parts of the apparatus and represents, at the moment, an unique underwater hydrophone array acquiring synchronously.

Figure 3: Mapping of the arrival directions of transient signals. The map is produced using the data acquired by the second storey on IL07 about 180m above the sea-bed. The origin is defined by the westward direction with respect to the horizontal of that storey. 90 (-90) in longitude corresponds to north (south), 90 (-90) in latitude to vertically downward-going acoustic signals (upward-going).

4 First AMADEUS results

The underwater enviroment is an highly noisly ambient: thus the characterization of this background is of fundamental importance to develop detection algorithms able to identify neutrino induced acoustic signals. One of the main opportunity given by the AMADEUS system, is to study this background.
The noise sources can be classified in two main group:

  • Transient signals (like the ones expected by the UHE neutrinos). These signals contains a finite amount of energy and have a finite duration in time.

  • Stationary random signals. These signals have statistical properties that are invariant with respect to a translation in time and are often characterized by their power spectral density (PSD).

In the following subsections the contribution of these two kinds of signals will be discussed.

4.1 Transient Signals

Each storey of the AMADEUS project is an array of hydrophones; taking advantage of these geometry, it is possible to reconstruct the arrival direction of the pressure wave on the storey using a technique called beam-forming.
The Beam-forming is a MISO (Multi Input Single Output) technique [11] originally developed to passively detect submarines with an underwater array of hydrophones. This technique analyses the data acquired by an array of sensors to compute the arrival direction of the incident waves. The array of sensors samples the wave-front in space and time and the samples of different sensors are combined, using the proper time delays, to sum up coherently all the waves arriving on the array from a specific direction; this will lead to an increase of the signal to noise ratio (SNR) since the spatially white noise will be averaged out. Since we don’t know the arrival direction of the incident wave we need to compute the time delays for many different arrival directions and produce an angular map of the incident pressure wave as the one reported in figure 2. The aliases that are present in this map are due to delays (directions) for which two or more of the six hydrophones sum coherently. The only direction for which all the hydrophones sum up coherently is the true one.

Figure 2: Example of beamforming output used to reconstruct a transient signal direction. The beamforming output is a function of the number of hydrophones whose signals sum up coherently, assuming that the transient signals arrive from that specific direction.

Using the directional information provided by three or more arrays it is possible to reconstruct the acoustic source position. The directional information can be used in conjunction with ray-tracing techniques that allows us to easily take into account the sound propagation in water.
In figure 3 qualitative mapping of the arrival directions of transient acoustic signals are shown. The data sample has been collected with the minimum bias filter during a time period of about 6 months; the figure shows the directions of all reconstructed signals which have an amplitude greater than eight times the standard deviation of the ambient noise. The majority of the reconstructed acoustic signals are received from directions in the upper hemisphere; this is consistent with the expectations since the major sources of transient noise are due to biological and anthropological activities. The few souces visible in the lower left part of the sphere resemble the layout of the ANTARES strings. Those sources are the pingers of the ANTARES acoustic positioning system, emitting acoustic signals at the bottom of each line.

4.2 Correlation between underwater noise and weather condition.

An analysis correlating the ambient acoustic noise level, measured with AMADEUS and the surface weather data was performed for the whole year 2008. The data used in this analysis are the minimum bias ones and the weather condition were measured by 5 station around the ANTARES site:

  • Station 1: Toulon.

  • Station 2: Cap Cepet.

  • Station 3: Hyres.

  • Station 4: Porquerolles.

  • Station 5: Toulon/Ile du Levant.

For each station a daily average of the wind speed and other weather observables are available; in this analysis only the mean wind speed was used. The noise level for a data sample acquired by AMADEUS is evaluated by integrating over the frequency range 1-50 kHz, the mean PSD is calculated using samples of 8.4 seconds duration.

Figure 4: The relative variation of the wind speed, measured by the weather station 2, and the noise level measured by the sensor 17 (IL07). This weather station is located near the sea so its wind measurements are well suited for this kind of analysis.

For better comparability between wind speed and noise level, the daily variation with respect to the annual mean is used. The correlation seems to became more evident for high wind speed (see figure 4).

Figure 5: Correlation coefficient evaluated using different frequency bands. Sensors 6 and 31 have been defective from the beginning of the data taking and thus show no correlation with the weather conditions. Sensor 22 has a non-ideal coupling with the glass sphere and is not sensitive to the higher frequency range.

For frequencies below 21 kHz a strong correlation (50%) is found; for higher frequency the ambient noise decreases and the system noise starts to becomes significant as a consequence the correlation with the weather condition decreases (see figure 5). No systematic different observation is found using the other weather station data; the significance of the correlation is lower as the stations are situated in-land and typically measure lower wind speed.

5 Conclusions

The AMADEUS project is fully operating and the data analysis is going on; this system offers a unique opportunity to study the underwater noise in order to develop and test acoustic triggers, able to discriminate the neutrino-induced signals from underwater background.
The matched filter is the optimum linear filter to discriminate a signal of known shape from a stochastic background of known spectrum. The beam-forming technique allows us to further increase the SNR by a factor that is equal to the number of hydrophones used in the phased array. Moreover the beam-forming technique allows to reconstruct the arrival direction of the incident pressure wave. The directional information, combined with a ray-tracing technique, permits an easy reconstruction of the interaction point. The combination of these techniques could extend the energy range of acoustic detectors and may increase the possibility to measure combined events in an hybrid (optic-acoustic) detector.

References

  1. Greisen, K. Physical Review Letters 16 (1966) 748-750
  2. Zatsepin, G. T. Kuz’min, V. A. Journal of Experimental and Theoretical Physics Letters 4 (1966) 78-80
  3. G.A. Askaryan, B.A. Dolgoshein et al., Nucl. Instrum. Methods 164, 267 (1979).
  4. J.G. Learned, Phys. Rev. 19, 3293 (1979).
  5. Vandenbroucke, Gratta, Lehtinen, Astrophysical Journal 621 (2005) 301-312
  6. Perkin, Doctoral thesis, http://arxiv.org/PS_cache/arxiv/pdf/0801/0801.0991v1.pdf
  7. Robert Lahmann et al, arXiv:0901.0321v1 [astro-ph.IM]
  8. Antares webpage, http://antares.in2p3.fr/
  9. P. Amram et al, Nucl. Instrum. Meth. A484 (2002) 369
  10. M. Ageron et al, Astropart. Phys. 31 (2009) 277.
  11. Barry D. Van Veen, Kevin M. Buckley, IEEE 0740-7467/88/0400-0004
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