The MEV project: design and testing of a new high-resolution telescope for Muography of Etna Volcano

The MEV project aims at developing a muon telescope expressly designed for the muography of Etna Volcano. In particular, one of the active craters in the summit area of the volcano would be a suitable target for this experiment. A muon tracking telescope with high imaging resolution was built and tested during 2017. The telescope is a tracker based on extruded scintillating bars with WLS fibres and featuring an innovative read-out architecture. It is composed of three XY planes with a sensitive area of \SI{1}{m^2}; the angular resolution does not exceeds \SI{0.4}{\milli\steradian} and the total angular aperture is about $\pm$\SI{45}{\degree}. A special effort concerned the design of mechanics and electronics in order to meet the requirements of a detector capable to work in a hostile environment such as the top of a tall volcano, at a far distance from any facility. The test phase started in January 2017 and ended successfully at the end of July 2017. An extinct volcanic crater (the Monti Rossi, in the village of Nicolosi, about 15km from Catania) is the target of the measurement. The detector acquired data for about 120 days and the preliminary results are reported in this work

Localizzazione probabilistica 3D (NonLinLoc) applicata all’area calabro-peloritana

Sono presentati e discussi i risultati preliminari relativi ad una ri-localizzazione probabilistica non-lineare 3D dei terremoti dell’area compresa tra il Tirreno meridionale e l’Arco Calabro-Peloritano (Italia meridionale). Scopo del lavoro è dimostrare che l’applicazione di un’approccio probabilistico non-lineare nella localizzazione dei terremoti può fornire dei risultati più accurati ai fini della sorveglianza, ovviando al problema degli outlier, rispetto alle tecniche di localizzazione lineari (e.g. Hypoellipse), che minimizzano simultaneamente tutti i residui tra fasi osservate e calcolate. Il programma utilizzato è NonLinLoc [Lomax, et al., 2000; Lomax, et al., 2001; Lomax, 2005; http://www.alomax.net/nlloc; NonLinLoc di seguito] il quale permette di effettuare un’efficiente ricerca globale dello spazio dei parametri ipocentrali (coordinate spaziali e tempo origine) ottenendo una stima della funzione densità di probabilità (pdf, probability density function) a posteriori. La pdf fornisce una descrizione completa della localizzazione e delle sue incertezze; il campionamento dello spazio dei parametri ipocentrali è stato fatto mediante la tecnica Oct-tree nella regione compresa tra 37.75 e 39.40 N in latitudine e tra 14.80 e 16.80 E in longitudine, e utilizzando tutti gli eventi con profondità H ≤30 km. La struttura dell’Oct-tree è stata imposta in 100,000 celle ed un insieme di queste celle viene poi salvata in modo da poter rappresentare graficamente la pdf mediante nubi di punti a diversa densità. Il dataset utilizzato per le nostre analisi è composto da 1,304 terremoti, di 1.0<M<4.3, registrati nel periodo compreso tra il 1994 e il 2006; il modello di velocità 3D adottato è stato ottenuto da Barberi et al., 2008 [poster presentato a questo convegno] invertendo lo stesso dataset, mediante l’utilizzo del software TomoDD. I risultati ottenuti sono stati confrontati sia con le localizzazioni 1D (Hypoellipse) che con quelle 3D. Si evidenzia una maggiore clusterizzazione degli eventi e, soprattutto, un evidente miglioramento della qualità delle localizzazioni utilizzando il modello di velocità crostale 3D. Per cui riteniamo che, l’applicazione del metodo probabilistico associato ad un buon modello di velocità 3D, può essere utilizzato ai fini di sorveglianza

High cadence spectropolarimetry of moving magnetic features observed around a pore

Moving magnetic features (MMFs) are small-size magnetic elements that are seen to stream out from sunspots, generally during their decay phase. Several observational results presented in the literature suggest them to be closely related to magnetic filaments that extend from the penumbra of the parent spot. Nevertheless, few observations of MMFs streaming out from spots without penumbra have been reported. The literature still lacks of analyses of the physical properties of these features. We investigate physical properties of monopolar MMFs observed around a small pore that had developed penumbra in the days preceding our observations and compare our results with those reported in the literature for features observed around sunspots. We analyzed NOAA 11005 during its decay phase with data acquired at the Dunn Solar Telescope in the FeI 617.3$nm and the CaII 854.2$ nm spectral lines with IBIS, and in the G-band. The field of view showed monopolar MMFs of both polarities streaming out from the leading negative polarity pore of the observed active region. Combining different analyses of the data, we investigated the temporal evolution of the relevant physical quantities associated with the MMFs as well as the photospheric and chromospheric signatures of these features. We show that the characteristics of the investigated MMFs agree with those reported in the literature for MMFs that stream out from spots with penumbrae. Moreover, observations of at least two of the observed features suggest them to be manifestations of emerging magnetic arches.Comment: Accepted by A&

Ultrahigh-energy neutrino follow-up of Gravitational Wave events GW150914 and GW151226 with the Pierre Auger Observatory

On September 14, 2015 the Advanced LIGO detectors observed their first gravitational-wave (GW) transient GW150914. This was followed by a second GW event observed on December 26, 2015. Both events were inferred to have arisen from the merger of black holes in binary systems. Such a system may emit neutrinos if there are magnetic fields and disk debris remaining from the formation of the two black holes. With the surface detector array of the Pierre Auger Observatory we can search for neutrinos with energy above 100 PeV from point-like sources across the sky with equatorial declination from about -65 deg. to +60 deg., and in particular from a fraction of the 90% confidence-level (CL) inferred positions in the sky of GW150914 and GW151226. A targeted search for highly-inclined extensive air showers, produced either by interactions of downward-going neutrinos of all flavors in the atmosphere or by the decays of tau leptons originating from tau-neutrino interactions in the Earth's crust (Earth-skimming neutrinos), yielded no candidates in the Auger data collected within $\pm 500$ s around or 1 day after the coordinated universal time (UTC) of GW150914 and GW151226, as well as in the same search periods relative to the UTC time of the GW candidate event LVT151012. From the non-observation we constrain the amount of energy radiated in ultrahigh-energy neutrinos from such remarkable events.Comment: Published version. Added journal reference and DOI. Added Report Numbe

Multi-resolution anisotropy studies of ultrahigh-energy cosmic rays detected at the Pierre Auger Observatory

We report a multi-resolution search for anisotropies in the arrival directions of cosmic rays detected at the Pierre Auger Observatory with local zenith angles up to $80^\circ$ and energies in excess of 4 EeV ($4 \times 10^{18}$ eV). This search is conducted by measuring the angular power spectrum and performing a needlet wavelet analysis in two independent energy ranges. Both analyses are complementary since the angular power spectrum achieves a better performance in identifying large-scale patterns while the needlet wavelet analysis, considering the parameters used in this work, presents a higher efficiency in detecting smaller-scale anisotropies, potentially providing directional information on any observed anisotropies. No deviation from isotropy is observed on any angular scale in the energy range between 4 and 8 EeV. Above 8 EeV, an indication for a dipole moment is captured; while no other deviation from isotropy is observed for moments beyond the dipole one. The corresponding $p$-values obtained after accounting for searches blindly performed at several angular scales, are $1.3 \times 10^{-5}$ in the case of the angular power spectrum, and $2.5 \times 10^{-3}$ in the case of the needlet analysis. While these results are consistent with previous reports making use of the same data set, they provide extensions of the previous works through the thorough scans of the angular scales.Comment: Published version. Added journal reference and DOI. Added Report Numbe