New constraints on all flavor Galactic diffuse neutrino emission with the ANTARES telescope

被引:44
作者
Albert, A. [1 ]
Andre, M. [2 ]
Anghinolfi, M. [3 ]
Anton, G. [4 ]
Ardid, M. [5 ]
Aubert, J. -J. [6 ]
Avgitas, T. [7 ]
Baret, B. [7 ]
Barrios-Marti, J. [8 ]
Basa, S. [9 ]
Belhorma, B. [10 ]
Bertin, V. [6 ]
Biagi, S. [11 ]
Bormuth, R. [12 ,13 ]
Bourret, S. [7 ]
Bouwhuis, M. C. [12 ]
Bruijn, R. [12 ,14 ]
Brunner, J. [6 ]
Busto, J. [6 ]
Capone, A. [15 ,16 ]
Caramete, L. [17 ]
Carr, J. [6 ]
Celli, S. [15 ,16 ,18 ]
El Moursli, R. Cherkaoui [19 ]
Chiarusi, T. [20 ]
Circella, M. [21 ]
Coelho, J. A. B. [7 ]
Coleiro, A. [7 ,8 ]
Coniglione, R. [11 ]
Costantini, H. [6 ]
Coyle, P. [6 ]
Creusot, A. [7 ]
Diaz, A. F. [22 ]
Deschamps, A. [23 ]
De Bonis, G. [15 ,16 ]
Distefano, C. [11 ]
Di Palma, I. [15 ,16 ]
Domi, A. [3 ,24 ]
Donzaud, C. [7 ,25 ]
Dornic, D. [6 ]
Drouhin, D. [1 ]
Eberl, T. [4 ]
El Bojaddaini, I. [26 ]
El Khayati, N. [19 ]
Elsasser, D. [27 ]
Enzenhofer, A. [6 ]
Ettahiri, A. [19 ]
Fassi, F. [19 ]
Felis, I. [5 ]
Fusco, L. A. [20 ,28 ]
机构
[1] Univ Haute Alsace, GRPHE, Inst Univ Technol Colmar, 34 Rue Grillenbreit BP 50568, F-68008 Colmar, France
[2] Tech Univ Catalonia, Lab Appl Bioacoust, Barcelona 08800, Spain
[3] INFN, Sez Genova, Via Dodecaneso 33, I-16146 Genoa, Italy
[4] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany
[5] Univ Politecn Valencia, Inst Invest Gestio Integrada Zones Costaneres IGI, C Paranimf 1, Gandia 46730, Spain
[6] Aix Marseille Univ, CNRS, IN2P3, CPPM, Marseille, France
[7] Univ Paris Diderot, APC, CNRS, IN2P3,CEA,IRFU,Observ Paris,Sorbonne Paris Cite, Paris, France
[8] Univ Valencia, CSIC, Inst Fis Corpuscular, IFIC, C Catedrat Jose Beltran 2, E-46980 Valencia, Spain
[9] LAM, Pole Etoile Site Chateau Gombert, Rue Frederic Joliot Curie 38, F-13388 Marseille 13, France
[10] Natl Ctr Energy Sci & Nucl Tech, BP 1382,RP 10001, Rabat, Morocco
[11] INFN, LNS, Via S Sofia 62, I-95123 Catania, Italy
[12] Nikhef, Sci Pk, Amsterdam, Netherlands
[13] Leiden Univ, Huygens Kamerlingh Onnes Lab, Leiden, Netherlands
[14] Univ Amsterdam, Inst Hoge Energie Fys, Sci Pk 105, NL-1098 XG Amsterdam, Netherlands
[15] INFN, Sez Roma, Ple Aldo Moro 2, I-00185 Rome, Italy
[16] Univ Roma La Sapienza, Dipartimento Fis, Ple Aldo Moro 2, I-00185 Rome, Italy
[17] Inst Space Sci, RO-077125 Bucharest, Magurele, Romania
[18] Gran Sasso Sci Inst, Viale Francesco Crispi 7, I-00167 Laquila, Italy
[19] Univ Mohammed V Rabat, 4 Ave Ibn Battouta,BP 1014, RP-10000 Rabat, Morocco
[20] INFN, Sez Bologna, Viale Berti Pichat 6-2, I-40127 Bologna, Italy
[21] INFN, Sez Bari, Via E Orabona 4, I-70126 Bari, Italy
[22] Univ Granada, Dept Comp Architecture & Technol CITIC, E-18071 Granada, Spain
[23] Observ Cote Azur, IRD, CNRS, Geoazur,UCA, Sophia Antipolis, France
[24] Univ Genoa, Dipartimento Fis, Via Dodecaneso 33, I-16146 Genoa, Italy
[25] Univ Paris Sud, F-91405 Orsay, France
[26] Univ Mohammed 1, Lab Phys Matter & Radiat, BP 717, Oujda 6000, Morocco
[27] Univ Wurzburg, Inst Theoret Phys & Astrophys, Emil Fischer Str 31, D-97074 Wurzburg, Germany
[28] Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy
[29] Univ Blaise Pascal, IN2P3, CNRS, Lab Phys Corpusculaire,Clermont Univ, BP 10448, F-63000 Clermont Ferrand, France
[30] INFN, Sez Catania, Viale Andrea Doria 6, I-95125 Catania, Italy
[31] Aix Marseille Univ, LSIS, CNRS, ENSAM,UMR 7296, F-13397 Marseille, France
[32] Univ Toulon & Var, CNRS, LSIS, UMR 7296, F-83957 La Garde, France
[33] Inst Univ France, F-75005 Paris, France
[34] Royal Netherlands Inst Sea Res NIOZ, Landsdiep 4, NL-1797 SZ T Horntje, Texel, Netherlands
[35] Friedrich Alexander Univ Erlangen Nurnberg, Dr Remeis Sternwarte & Erlangen Ctr Astroparticle, Sternwartstr E 7, D-96049 Bamberg, Germany
[36] Moscow MV Lomonosov State Univ, Skobeltsyn Inst Nucl Phys, Moscow 119991, Russia
[37] Aix Marseille Univ, MIO, CNRS, INSU,IRD,UM 110, F-13288 Marseille 9, France
[38] Univ Sud Toulon Var, F-83957 La Garde, France
[39] Univ Catania, Dipartimento Fis & Astron, Viale Andrea Doria 6, I-95125 Catania, Italy
[40] CEA Saclay, Direct Sci Mat, Inst Rech Fondament Univers, Serv Phys Particules, F-91191 Gif Sur Yvette, France
[41] INFN, Sez Pisa, Largo B Pontecorvo 3, I-56127 Pisa, Italy
[42] Univ Pisa, Dipartimento Fis, Largo B Pontecorvo 3, I-56127 Pisa, Italy
[43] INFN, Sez Napoli, Via Cintia, I-80126 Naples, Italy
[44] Univ Federico II Napoli, Dipartimento Fis, Via Cintia, I-80126 Naples, Italy
[45] Univ Granada, Dept Fis Teor & Cosmos, E-18071 Granada, Spain
[46] Univ Granada, CAFPE, E-18071 Granada, Spain
[47] Univ Strasbourg, CNRS, IPHC, UMR 7178, F-67000 Strasbourg, France
[48] Univ Amsterdam, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands
关键词
SPATIAL-DISTRIBUTION; ELEMENTAL GROUPS; ENERGY-SPECTRA; HEMISPHERE; SEARCH; RAYS;
D O I
10.1103/PhysRevD.96.062001
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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.
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页数:8
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