M. Panareo - Dip. di Fisica Universita' di Lecce and INFN sez. di Lecce, Lecce, Italy

M. Panareo
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M. Panareo
Dip. di Fisica Universita' di Lecce and INFN sez. di Lecce, Lecce, Italy

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High Energy Physics - Experiment (12)
High Energy Astrophysical Phenomena (12)
Physics - Instrumentation and Detectors (6)
High Energy Physics - Phenomenology (5)
Instrumentation and Methods for Astrophysics (2)
Solar and Stellar Astrophysics (1)

Publications Authored By M. Panareo

The Extreme Energy Events Project is a synchronous sparse array of 52 tracking detectors for studying High Energy Cosmic Rays (HECR) and Cosmic Rays-related phenomena. The observatory is also meant to address Long Distance Correlation (LDC) phenomena: the network is deployed over a broad area covering 10 degrees in latitude and 11 in longitude. An overview of a set of preliminary results is given, extending from the study of local muon flux dependance on solar activity to the investigation of the upward-going component of muon flux traversing the EEE stations; from the search for anisotropies at the sub-TeV scale to the hints for observations of km-scale Extensive Air Shower (EAS). Read More

Drift chambers operated with helium-based gas mixtures represent a common solution for tracking charged particles keeping the material budget in the sensitive volume to a minimum. The drawback of this solution is the worsening of the spatial resolution due to primary ionisation fluctuations, which is a limiting factor for high granularity drift chambers like the MEG II tracker. We report on the measurements performed on three different prototypes of the MEG II drift chamber aimed at determining the achievable single-hit resolution. Read More

The MEG experiment makes use of one of the world's most intense low energy muon beams, in order to search for the lepton flavour violating process $\mu^{+} \rightarrow {\rm e}^{+} \gamma$. We determined the residual beam polarization at the thin stopping target, by measuring the asymmetry of the angular distribution of Michel decay positrons as a function of energy. The initial muon beam polarization at the production is predicted to be $P_{\mu} = -1$ by the Standard Model (SM) with massless neutrinos. Read More

The events recorded by ARGO-YBJ in more than five years of data collection have been analyzed to determine the diffuse gamma-ray emission in the Galactic plane at Galactic longitudes 25{\deg} < l < 100{\deg} and Galactic latitudes . The energy range covered by this analysis, from ~350 GeV to ~2 TeV, allows the connection of the region explored by Fermi with the multi-TeV measurements carried out by Milagro. Our analysis has been focused on two selected regions of the Galactic plane, i. Read More

Affiliations: 1ARGO-YBJ Collaboration, 2ARGO-YBJ Collaboration, 3ARGO-YBJ Collaboration, 4ARGO-YBJ Collaboration, 5ARGO-YBJ Collaboration, 6ARGO-YBJ Collaboration, 7ARGO-YBJ Collaboration, 8ARGO-YBJ Collaboration, 9ARGO-YBJ Collaboration, 10ARGO-YBJ Collaboration, 11ARGO-YBJ Collaboration, 12ARGO-YBJ Collaboration, 13ARGO-YBJ Collaboration, 14ARGO-YBJ Collaboration, 15ARGO-YBJ Collaboration, 16ARGO-YBJ Collaboration, 17ARGO-YBJ Collaboration, 18ARGO-YBJ Collaboration, 19ARGO-YBJ Collaboration, 20ARGO-YBJ Collaboration, 21ARGO-YBJ Collaboration, 22ARGO-YBJ Collaboration, 23ARGO-YBJ Collaboration, 24ARGO-YBJ Collaboration, 25ARGO-YBJ Collaboration, 26ARGO-YBJ Collaboration, 27ARGO-YBJ Collaboration, 28ARGO-YBJ Collaboration, 29ARGO-YBJ Collaboration, 30ARGO-YBJ Collaboration, 31ARGO-YBJ Collaboration, 32ARGO-YBJ Collaboration, 33ARGO-YBJ Collaboration, 34ARGO-YBJ Collaboration, 35ARGO-YBJ Collaboration, 36ARGO-YBJ Collaboration, 37ARGO-YBJ Collaboration, 38ARGO-YBJ Collaboration, 39ARGO-YBJ Collaboration, 40ARGO-YBJ Collaboration, 41ARGO-YBJ Collaboration, 42ARGO-YBJ Collaboration, 43ARGO-YBJ Collaboration, 44ARGO-YBJ Collaboration, 45ARGO-YBJ Collaboration, 46ARGO-YBJ Collaboration, 47ARGO-YBJ Collaboration, 48ARGO-YBJ Collaboration, 49ARGO-YBJ Collaboration, 50ARGO-YBJ Collaboration, 51ARGO-YBJ Collaboration, 52ARGO-YBJ Collaboration, 53ARGO-YBJ Collaboration, 54ARGO-YBJ Collaboration, 55ARGO-YBJ Collaboration, 56ARGO-YBJ Collaboration, 57ARGO-YBJ Collaboration, 58ARGO-YBJ Collaboration, 59ARGO-YBJ Collaboration, 60ARGO-YBJ Collaboration, 61ARGO-YBJ Collaboration, 62ARGO-YBJ Collaboration, 63ARGO-YBJ Collaboration, 64ARGO-YBJ Collaboration, 65ARGO-YBJ Collaboration, 66ARGO-YBJ Collaboration, 67ARGO-YBJ Collaboration, 68ARGO-YBJ Collaboration, 69ARGO-YBJ Collaboration, 70ARGO-YBJ Collaboration, 71ARGO-YBJ Collaboration, 72ARGO-YBJ Collaboration, 73ARGO-YBJ Collaboration, 74ARGO-YBJ Collaboration, 75ARGO-YBJ Collaboration, 76ARGO-YBJ Collaboration, 77ARGO-YBJ Collaboration, 78ARGO-YBJ Collaboration, 79ARGO-YBJ Collaboration, 80ARGO-YBJ Collaboration, 81ARGO-YBJ Collaboration, 82LHAASO Collaboration, 83LHAASO Collaboration, 84LHAASO Collaboration, 85LHAASO Collaboration, 86LHAASO Collaboration, 87LHAASO Collaboration, 88LHAASO Collaboration, 89LHAASO Collaboration, 90LHAASO Collaboration, 91LHAASO Collaboration, 92LHAASO Collaboration, 93LHAASO Collaboration, 94LHAASO Collaboration, 95LHAASO Collaboration, 96LHAASO Collaboration, 97LHAASO Collaboration

The measurement of cosmic ray energy spectra, in particular for individual species, is an essential approach in finding their origin. Locating the "knees" of the spectra is an important part of the approach and has yet to be achieved. Here we report a measurement of the mixed Hydrogen and Helium spectrum using the combination of the ARGO-YBJ experiment and of a prototype Cherenkov telescope for the LHAASO experiment. Read More

The extended TeV gamma-ray source ARGO J2031+4157 (or MGRO J2031+41) is positionally consistent with the Cygnus Cocoon discovered by $Fermi$-LAT at GeV energies in the Cygnus superbubble. Reanalyzing the ARGO-YBJ data collected from November 2007 to January 2013, the angular extension and energy spectrum of ARGO J2031+4157 are evaluated. After subtracting the contribution of the overlapping TeV sources, the ARGO-YBJ excess map is fitted with a two-dimensional Gaussian function in a square region of $10^{\circ}\times 10^{\circ}$, finding a source extension $\sigma_{ext}$= 1$^{\circ}$. Read More

The energy spectrum of cosmic Hydrogen and Helium nuclei has been measured, below the so-called "knee", by using a hybrid experiment with a wide field-of-view Cherenkov telescope and the Resistive Plate Chamber (RPC) array of the ARGO-YBJ experiment at 4300 m above sea level. The Hydrogen and Helium nuclei have been well separated from other cosmic ray components by using a multi-parameter technique. A highly uniform energy resolution of about 25% is achieved throughout the whole energy range (100 TeV - 700 TeV). Read More

We studied the radiative muon decay $\mu^+ \to e^+\nu\bar{\nu}\gamma$ by using for the first time an almost fully polarized muon source. We identified a large sample (~13000) of these decays in a total sample of 1.8x10^14 positive muon decays collected in the MEG experiment in the years 2009--2010 and measured the branching ratio B($\mu^+ \to e^+\nu\bar{\nu}\gamma$) = (6. Read More

The ARGO-YBJ detector is an extensive air shower array that has been used to monitor the northern $\gamma$-ray sky at energies above 0.3 TeV from 2007 November to 2013 January. In this paper, we present the results of a sky survey in the declination band from $-10^{\circ}$ to $70^{\circ}$, using data recorded over the past five years. Read More

The MEG (Mu to Electron Gamma) experiment has been running at the Paul Scherrer Institut (PSI), Switzerland since 2008 to search for the decay \meg\ by using one of the most intense continuous $\mu^+$ beams in the world. This paper presents the MEG components: the positron spectrometer, including a thin target, a superconducting magnet, a set of drift chambers for measuring the muon decay vertex and the positron momentum, a timing counter for measuring the positron time, and a liquid xenon detector for measuring the photon energy, position and time. The trigger system, the read-out electronics and the data acquisition system are also presented in detail. Read More

We report the observation of a very high energy \gamma-ray source, whose position is coincident with HESS J1841-055. This source has been observed for 4.5 years by the ARGO-YBJ experiment from November 2007 to July 2012. Read More

We propose the continuation of the MEG experiment to search for the charged lepton flavour violating decay (cLFV) \mu \to e \gamma, based on an upgrade of the experiment, which aims for a sensitivity enhancement of one order of magnitude compared to the final MEG result, down to the $6 \times 10^{-14}$ level. The key features of this new MEG upgrade are an increased rate capability of all detectors to enable running at the intensity frontier and improved energy, angular and timing resolutions, for both the positron and photon arms of the detector. On the positron-side a new low-mass, single volume, high granularity tracker is envisaged, in combination with a new highly segmented, fast timing counter array, to track positron from a thinner stopping target. Read More

As one of the brightest active blazars in both X-ray and very high energy $\gamma$-ray bands, Mrk 501 is very useful for physics associated with jets from AGNs. The ARGO-YBJ experiment is monitoring it for $\gamma$-rays above 0.3 TeV since November 2007. Read More

We report the observation of TeV gamma-rays from the Cygnus region using the ARGO-YBJ data collected from 2007 November to 2011 August. Several TeV sources are located in this region including the two bright extended MGRO J2019+37 and MGRO J2031+41. According to the Milagro data set, at 20 TeV MGRO J2019+37 is the most significant source apart from the Crab Nebula. Read More

ARGO-YBJ is an air shower detector array with a fully covered layer of resistive plate chambers. It is operated with a high duty cycle and a large field of view. It continuously monitors the northern sky at energies above 0. Read More

Authors: G. Aielli1, C. Bacci2, B. Bartoli3, P. Bernardini4, X. J. Bi5, C. Bleve6, P. Branchini7, A. Budano8, S. Bussino9, A. K. Calabrese Melcarne10, P. Camarri11, Z. Cao12, A. Cappa13, R. Cardarelli14, S. Catalanotti15, C. Cattaneo16, P. Celio17, S. Z. Chen18, T. L. Chen19, Y. Chen20, P. Creti21, S. W. Cui22, B. Z. Dai23, G. D'Alí Staiti24, Danzengluobu25, M. Dattoli26, I. De Mitri27, B. D'Ettorre Piazzoli28, M. De Vincenzi29, T. Di Girolamo30, X. H. Ding31, G. Di Sciascio32, C. F. Feng33, Z. Y. Feng34, Zhenyong Feng35, F. Galeazzi36, P. Galeotti37, R. Gargana38, Q. B. Gou39, Y. Q. Guo40, H. H. He41, Haibing Hu42, Hongbo Hu43, Q. Huang44, M. Iacovacci45, R. Iuppa46, I. James47, H. Y. Jia48, Labaciren49, H. J. Li50, J. Y. Li51, X. X. Li52, B. Liberti53, G. Liguori54, C. Liu55, C. Q. Liu56, M. Y. Liu57, J. Liu58, H. Lu59, X. H. Ma60, G. Mancarella61, S. M. Mari62, G. Marsella63, D. Martello64, S. Mastroianni65, X. R. Meng66, P. Montini67, C. C. Ning68, A. Pagliaro69, M. Panareo70, L. Perrone71, P. Pistilli72, X. B. Qu73, E. Rossi74, F. Ruggieri75, L. Saggese76, P. Salvini77, R. Santonico78, P. R. Shen79, X. D. Sheng80, F. Shi81, C. Stanescu82, A. Surdo83, Y. H. Tan84, P. Vallania85, S. Vernetto86, C. Vigorito87, B. Wang88, H. Wang89, C. Y. Wu90, H. R. Wu91, Z. G. Yao92, B. Xu93, L. Xue94, Y. X. Yan95, Q. Y. Yang96, X. C. Yang97, A. F. Yuan98, M. Zha99, H. M. Zhang100, JiLong Zhang101, JianLi Zhang102, L. Zhang103, P. Zhang104, X. Y. Zhang105, Y. Zhang106, Zhaxisangzhu107, Zhaxiciren108, X. X. Zhou109, F. R. Zhu110, Q. Q. Zhu111, G. Zizzi112
Affiliations: 1The ARGO-YBJ Collaboration, 2The ARGO-YBJ Collaboration, 3The ARGO-YBJ Collaboration, 4The ARGO-YBJ Collaboration, 5The ARGO-YBJ Collaboration, 6The ARGO-YBJ Collaboration, 7The ARGO-YBJ Collaboration, 8The ARGO-YBJ Collaboration, 9The ARGO-YBJ Collaboration, 10The ARGO-YBJ Collaboration, 11The ARGO-YBJ Collaboration, 12The ARGO-YBJ Collaboration, 13The ARGO-YBJ Collaboration, 14The ARGO-YBJ Collaboration, 15The ARGO-YBJ Collaboration, 16The ARGO-YBJ Collaboration, 17The ARGO-YBJ Collaboration, 18The ARGO-YBJ Collaboration, 19The ARGO-YBJ Collaboration, 20The ARGO-YBJ Collaboration, 21The ARGO-YBJ Collaboration, 22The ARGO-YBJ Collaboration, 23The ARGO-YBJ Collaboration, 24The ARGO-YBJ Collaboration, 25The ARGO-YBJ Collaboration, 26The ARGO-YBJ Collaboration, 27The ARGO-YBJ Collaboration, 28The ARGO-YBJ Collaboration, 29The ARGO-YBJ Collaboration, 30The ARGO-YBJ Collaboration, 31The ARGO-YBJ Collaboration, 32The ARGO-YBJ Collaboration, 33The ARGO-YBJ Collaboration, 34The ARGO-YBJ Collaboration, 35The ARGO-YBJ Collaboration, 36The ARGO-YBJ Collaboration, 37The ARGO-YBJ Collaboration, 38The ARGO-YBJ Collaboration, 39The ARGO-YBJ Collaboration, 40The ARGO-YBJ Collaboration, 41The ARGO-YBJ Collaboration, 42The ARGO-YBJ Collaboration, 43The ARGO-YBJ Collaboration, 44The ARGO-YBJ Collaboration, 45The ARGO-YBJ Collaboration, 46The ARGO-YBJ Collaboration, 47The ARGO-YBJ Collaboration, 48The ARGO-YBJ Collaboration, 49The ARGO-YBJ Collaboration, 50The ARGO-YBJ Collaboration, 51The ARGO-YBJ Collaboration, 52The ARGO-YBJ Collaboration, 53The ARGO-YBJ Collaboration, 54The ARGO-YBJ Collaboration, 55The ARGO-YBJ Collaboration, 56The ARGO-YBJ Collaboration, 57The ARGO-YBJ Collaboration, 58The ARGO-YBJ Collaboration, 59The ARGO-YBJ Collaboration, 60The ARGO-YBJ Collaboration, 61The ARGO-YBJ Collaboration, 62The ARGO-YBJ Collaboration, 63The ARGO-YBJ Collaboration, 64The ARGO-YBJ Collaboration, 65The ARGO-YBJ Collaboration, 66The ARGO-YBJ Collaboration, 67The ARGO-YBJ Collaboration, 68The ARGO-YBJ Collaboration, 69The ARGO-YBJ Collaboration, 70The ARGO-YBJ Collaboration, 71The ARGO-YBJ Collaboration, 72The ARGO-YBJ Collaboration, 73The ARGO-YBJ Collaboration, 74The ARGO-YBJ Collaboration, 75The ARGO-YBJ Collaboration, 76The ARGO-YBJ Collaboration, 77The ARGO-YBJ Collaboration, 78The ARGO-YBJ Collaboration, 79The ARGO-YBJ Collaboration, 80The ARGO-YBJ Collaboration, 81The ARGO-YBJ Collaboration, 82The ARGO-YBJ Collaboration, 83The ARGO-YBJ Collaboration, 84The ARGO-YBJ Collaboration, 85The ARGO-YBJ Collaboration, 86The ARGO-YBJ Collaboration, 87The ARGO-YBJ Collaboration, 88The ARGO-YBJ Collaboration, 89The ARGO-YBJ Collaboration, 90The ARGO-YBJ Collaboration, 91The ARGO-YBJ Collaboration, 92The ARGO-YBJ Collaboration, 93The ARGO-YBJ Collaboration, 94The ARGO-YBJ Collaboration, 95The ARGO-YBJ Collaboration, 96The ARGO-YBJ Collaboration, 97The ARGO-YBJ Collaboration, 98The ARGO-YBJ Collaboration, 99The ARGO-YBJ Collaboration, 100The ARGO-YBJ Collaboration, 101The ARGO-YBJ Collaboration, 102The ARGO-YBJ Collaboration, 103The ARGO-YBJ Collaboration, 104The ARGO-YBJ Collaboration, 105The ARGO-YBJ Collaboration, 106The ARGO-YBJ Collaboration, 107The ARGO-YBJ Collaboration, 108The ARGO-YBJ Collaboration, 109The ARGO-YBJ Collaboration, 110The ARGO-YBJ Collaboration, 111The ARGO-YBJ Collaboration, 112The ARGO-YBJ Collaboration

The sun blocks cosmic ray particles from outside the solar system, forming a detectable shadow in the sky map of cosmic rays detected by the ARGO-YBJ experiment in Tibet. Because the cosmic ray particles are positive charged, the magnetic field between the sun and the earth deflects them from straight trajectories and results in a shift of the shadow from the true location of the sun. Here we show that the shift measures the intensity of the field which is transported by the solar wind from the sun to the earth. Read More

Affiliations: 1Dip. di Fisica Universita' di Napoli and INFN sez. di Napoli, Napoli, Italy, 2Universita' del Sannio, Benevento and INFN sez. di Napoli, Napoli, Italy, 3Dip. di Fisica Universita' di Napoli and INFN sez. di Napoli, Napoli, Italy, 4Dip. di Fisica Universita' di Napoli and INFN sez. di Napoli, Napoli, Italy, 5Dip. di Fisica Universita' di Lecce and INFN sez. di Lecce, Lecce, Italy, 6Dip. di Fisica Universita' di Lecce and INFN sez. di Lecce, Lecce, Italy, 7Dip. di Fisica Universita' di Lecce and INFN sez. di Lecce, Lecce, Italy, 8Dip. di Fisica Universita' di Lecce and INFN sez. di Lecce, Lecce, Italy, 9Dip. di Fisica Universita' di Lecce and INFN sez. di Lecce, Lecce, Italy, 10Dip. di Fisica Universita' di Lecce and INFN sez. di Lecce, Lecce, Italy

The ARGO-YBJ experiment has been designed to detect air shower events over a large size scale and with an energy threshold of a few hundreds GeV. The building blocks of the ARGO-YBJ detector are single-gap Resistive Plate Counters (RPCs). The trigger logic selects the events on the basis of their hit multiplicity. Read More