New constraints on all flavor Galactic diffuse neutrino emission with the ANTARES telescope
New constraints on all flavor Galactic diffuse neutrino emission with the ANTARES telescope
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DOI：
10.1103/physrevd.96.062001
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发表时间：
2017-05
影响因子：
5
通讯作者：
A. Albert;M. Andr'e;M. Anghinolfi;G. Anton;M. Ardid;J. Aubert;T. Avgitas;B. Baret;J. Barrios-Mart'i;S. Basa;B. Belhorma;V. Bertin;S. Biagi;R. Bormuth;S. Bourret;M. Bouwhuis;R. Bruijn;J. Brunner;J. Busto;A. Capone;L. Caramete;J. Carr;S. Celli;R. Moursli;T. Chiarusi;M. Circella;J. Coelho;A. Coleiro;R. Coniglione;H. Costantini;P. Coyle;A. Creusot;A. D'iaz;A. Deschamps;G. Bonis;C. Distefano;I. Palma;A. Domi;C. Donzaud;D. Dornic;D. Drouhin;T. Eberl;I. Bojaddaini;N. Khayati;D. Elsasser;A. Enzenhofer;A. Ettahiri;F. Fassi;I. Felis;L. Fusco;S. Galata;P. Gay;V. Giordano;H. Glotin;T. Gr'egoire;R. G. Ruiz;K. Graf;S. Hallmann;H. Haren;A. Heijboer;Y. Hello;J. Hern'andez-Rey;J. Hossl;J. Hofestadt;C. Hugon;G. Illuminati;C. James;M. Jong;M. Jongen;M. Kadler;O. Kalekin;U. Katz;D. Kiessling;A. Kouchner;M. Kreter;I. Kreykenbohm;V. Kulikovskiy;C. Lachaud;R. Lahmann;D. Lefèvre;E. Leonora;M. Lotze;S. Loucatos;M. Marcelin;A. Margiotta;A. Marinelli;J. A. Mart'inez-Mora;R. Mele;K. Melis;T. Michael;P. Migliozzi;A. Moussa;S. Navas;E. Nezri;Mukharbek Organokov;G. E. Puavualacs;C. Pellegrino;C. Perrina;P. Piattelli;V. Popa;T. Pradier;L. Quinn;C. Racca;G. Riccobene;A. S'anchez-Losa;M. Saldaña;I. Salvadori;D. Samtleben;M. Sanguineti;P. Sapienza;F. Schussler;C. Sieger;M. Spurio;T. Stolarczyk;M. Taiuti;Y. Tayalati;A. Trovato;D. Turpin;C. Tonnis;B. Vallage;V. Elewyck;F. Versari;D. Vivolo;A. Vizzoca;J. Wilms;J. Zornoza;J. Z'uniga;D. Gaggero;D. G. G. -. U. D. H. A. -. I. Colmar-D.-G.-G.-.-U.-D.-H.-A.-.-I.-Colmar-1422209660;34 rue du Grillenbreit BP 50568 - 68008 Colmar;France.;Technical University of Catalonia;Laboratory of Applied Bioacoustics;Rambla Exposici'o;08800 Vilanova i la Geltr'u;Barcelona;Spain.;I. Genova;33 viaDodecaneso;16146 Genova;Italy.;Friedrich-Alexander-Universitat Erlangen-Nurnberg;Erlangen Centre for Astroparticle Physics;1. Erwin-Rommel-Str.;91058 Erlangen;H Germany;1. Institutd'Investigaci'operalaGesti'oIntegradadeles-1.-1422210245;46730 Gandia;A. Univ.;CNRSIN2p3;Cppm;Marseille;Apc;U. Diderot;CEAIrfu;O. Paris;Sorbonne Paris Cit'e;I. -. I. D. F. C. C. C. Beltr'an-I.-.-I.-D.-F.-C.-C.-C.-Beltr'an-1422210430;2. E. Paterna;Valencia;Lam Marseille;Pole de l''etoile Site de Chateau-Gombert-Pole-de-l''etoile-Site-de-Chateau-Gombert-1422209613;38 rueFr'ed'ericJoliot-Curie;13388 Marseille Cedex;13;National Center for Theoretical Sciences;Nuclear Techniques;B.P.1382;R. P. Rabat;Morocco.;I. N. D. Sud;64 viaS.Sofia;95125 Catania;Nikhef;Science Park;Amsterdam;The Netherlands.;Huygens Laboratorium;Universiteit Leiden;U. Amsterdam;Instituut voor Hoge-Energie Fysica;Science Park 105;1098 XG Amsterdam;Infn Roma;2. P.leAldoMoro;00133 Roma;Dipartimento di Fisica dell'Universita di RomaLa Sapienza-Dipartimento-di-Fisica-dell'Universita-di-RomaLa-1997533322;Institute of Space Science;R. Bucharest;Muagurele;Romania.;Gran Sasso Science Institute;7. VialeFrancescoCrispi;00167 L'Aquila;University Mohammed V in Rabat;F. O. Sciences;4. A. I. Battouta;B. P. 1014;R. P. Rabat;I. Bologna;62 VialeBerti-Pichat;40129 Bologna;I. Bari;4. ViaE.Orabona;70125 Bari;Department of Computer Architecture;TechnologyCITIC;U. Granada;18012 Granada;G'eoazur;Uca;Cnrs;Ird;Observatoire de la Côte d'Azur;S. Antipolis;D. D. F. dell'Universita-D.;U. Paris-sud;91405 Orsay Cedex;I. UniversityMohammed;Laboratory of Physics of Matter-Laboratory-of-Physics-of-Matter-1422210837;Radiations;B.P.717;Oujda 6000;I. F. Astrophysik;U. Wurzburg;31 Emil-FischerStr.;97074 Wurzburg;D. D. F. dell'Universita-D.;62 vialeBertiPichat;Laboratoire de Physique Corpusculaire;Clermont Universit'e;Universit'e Blaise Pascal;BP 10448;F. Clermont-Ferrand;I. Catania;6. VialeAndreaDoria;95125 Catania;Lsis;A. Marseille;Universit'e de Toulon Cnrs Lsis Umr 7296;83957 La Garde;I. France;7. Paris;R. I. F. S. Research;4. Landsdiep;1797 SZ 't Horntje;D. Remeis-Sternwarte;Ecap;Universitat Erlangen-Nurnberg;7. Sternwartstr.;96049 Bamberg;M. University;S. I. O. N. Physics;L. Gory;117997 Moscow;Russia.;Mediterranean Institute of Oceanography;Aix-Marseille University;13288;9. Cedex;Universit'e du Sud Toulon-Var;CNRS-INSUIRD UM 110;83957;Lannion Cedex;D. D. F. dell'Universita-D.;Direction des Sciences de la Matiere - Institut de recherche Particules-Direction-des-Sciences-de-la-Matiere-Institut-de-1422213227;C. Saclay;9. Cedex;I. Pisa;3. LargoB.Pontecorvo;56126 Pisa;Infn Napoli;V. Napoli;D. Napoli;Via Cintia 80126;Napoli;Dpto. de F'isica Te'orica y del Cosmos C.A.F.P.E.;U. Strasbourg;Iphc Umr 7178;F. Strasbourg;Grappa;U. Amsterdam;Science Park 904;1098XH Amsterdam;Netherlands.
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文献类型：
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作者：
A. Albert;M. Andr'e;M. Anghinolfi;G. Anton;M. Ardid;J. Aubert;T. Avgitas;B. Baret;J. Barrios-Mart'i;S. Basa;B. Belhorma;V. Bertin;S. Biagi;R. Bormuth;S. Bourret;M. Bouwhuis;R. Bruijn;J. Brunner;J. Busto;A. Capone;L. Caramete;J. Carr;S. Celli;R. Moursli;T. Chiarusi;M. Circella;J. Coelho;A. Coleiro;R. Coniglione;H. Costantini;P. Coyle;A. Creusot;A. D'iaz;A. Deschamps;G. Bonis;C. Distefano;I. Palma;A. Domi;C. Donzaud;D. Dornic;D. Drouhin;T. Eberl;I. Bojaddaini;N. Khayati;D. Elsasser;A. Enzenhofer;A. Ettahiri;F. Fassi;I. Felis;L. Fusco;S. Galata;P. Gay;V. Giordano;H. Glotin;T. Gr'egoire;R. G. Ruiz;K. Graf;S. Hallmann;H. Haren;A. Heijboer;Y. Hello;J. Hern'andez-Rey;J. Hossl;J. Hofestadt;C. Hugon;G. Illuminati;C. James;M. Jong;M. Jongen;M. Kadler;O. Kalekin;U. Katz;D. Kiessling;A. Kouchner;M. Kreter;I. Kreykenbohm;V. Kulikovskiy;C. Lachaud;R. Lahmann;D. Lefèvre;E. Leonora;M. Lotze;S. Loucatos;M. Marcelin;A. Margiotta;A. Marinelli;J. A. Mart'inez-Mora;R. Mele;K. Melis;T. Michael;P. Migliozzi;A. Moussa;S. Navas;E. Nezri;Mukharbek Organokov;G. E. Puavualacs;C. Pellegrino;C. Perrina;P. Piattelli;V. Popa;T. Pradier;L. Quinn;C. Racca;G. Riccobene;A. S'anchez-Losa;M. Saldaña;I. Salvadori;D. Samtleben;M. Sanguineti;P. Sapienza;F. Schussler;C. Sieger;M. Spurio;T. Stolarczyk;M. Taiuti;Y. Tayalati;A. Trovato;D. Turpin;C. Tonnis;B. Vallage;V. Elewyck;F. Versari;D. Vivolo;A. Vizzoca;J. Wilms;J. Zornoza;J. Z'uniga;D. Gaggero;D. G. G. -. U. D. H. A. -. I. Colmar-D.-G.-G.-.-U.-D.-H.-A.-.-I.-Colmar-1422209660;34 rue du Grillenbreit BP 50568 - 68008 Colmar;France.;Technical University of Catalonia;Laboratory of Applied Bioacoustics;Rambla Exposici'o;08800 Vilanova i la Geltr'u;Barcelona;Spain.;I. Genova;33 viaDodecaneso;16146 Genova;Italy.;Friedrich-Alexander-Universitat Erlangen-Nurnberg;Erlangen Centre for Astroparticle Physics;1. Erwin-Rommel-Str.;91058 Erlangen;H Germany;1. Institutd'Investigaci'operalaGesti'oIntegradadeles-1.-1422210245;46730 Gandia;A. Univ.;CNRSIN2p3;Cppm;Marseille;Apc;U. Diderot;CEAIrfu;O. Paris;Sorbonne Paris Cit'e;I. -. I. D. F. C. C. C. Beltr'an-I.-.-I.-D.-F.-C.-C.-C.-Beltr'an-1422210430;2. E. Paterna;Valencia;Lam Marseille;Pole de l''etoile Site de Chateau-Gombert-Pole-de-l''etoile-Site-de-Chateau-Gombert-1422209613;38 rueFr'ed'ericJoliot-Curie;13388 Marseille Cedex;13;National Center for Theoretical Sciences;Nuclear Techniques;B.P.1382;R. P. Rabat;Morocco.;I. N. D. Sud;64 viaS.Sofia;95125 Catania;Nikhef;Science Park;Amsterdam;The Netherlands.;Huygens Laboratorium;Universiteit Leiden;U. Amsterdam;Instituut voor Hoge-Energie Fysica;Science Park 105;1098 XG Amsterdam;Infn Roma;2. P.leAldoMoro;00133 Roma;Dipartimento di Fisica dell'Universita di RomaLa Sapienza-Dipartimento-di-Fisica-dell'Universita-di-RomaLa-1997533322;Institute of Space Science;R. Bucharest;Muagurele;Romania.;Gran Sasso Science Institute;7. VialeFrancescoCrispi;00167 L'Aquila;University Mohammed V in Rabat;F. O. Sciences;4. A. I. Battouta;B. P. 1014;R. P. Rabat;I. Bologna;62 VialeBerti-Pichat;40129 Bologna;I. Bari;4. ViaE.Orabona;70125 Bari;Department of Computer Architecture;TechnologyCITIC;U. Granada;18012 Granada;G'eoazur;Uca;Cnrs;Ird;Observatoire de la Côte d'Azur;S. Antipolis;D. D. F. dell'Universita-D.;U. Paris-sud;91405 Orsay Cedex;I. UniversityMohammed;Laboratory of Physics of Matter-Laboratory-of-Physics-of-Matter-1422210837;Radiations;B.P.717;Oujda 6000;I. F. Astrophysik;U. Wurzburg;31 Emil-FischerStr.;97074 Wurzburg;D. D. F. dell'Universita-D.;62 vialeBertiPichat;Laboratoire de Physique Corpusculaire;Clermont Universit'e;Universit'e Blaise Pascal;BP 10448;F. Clermont-Ferrand;I. Catania;6. VialeAndreaDoria;95125 Catania;Lsis;A. Marseille;Universit'e de Toulon Cnrs Lsis Umr 7296;83957 La Garde;I. France;7. Paris;R. I. F. S. Research;4. Landsdiep;1797 SZ 't Horntje;D. Remeis-Sternwarte;Ecap;Universitat Erlangen-Nurnberg;7. Sternwartstr.;96049 Bamberg;M. University;S. I. O. N. Physics;L. Gory;117997 Moscow;Russia.;Mediterranean Institute of Oceanography;Aix-Marseille University;13288;9. Cedex;Universit'e du Sud Toulon-Var;CNRS-INSUIRD UM 110;83957;Lannion Cedex;D. D. F. dell'Universita-D.;Direction des Sciences de la Matiere - Institut de recherche Particules-Direction-des-Sciences-de-la-Matiere-Institut-de-1422213227;C. Saclay;9. Cedex;I. Pisa;3. LargoB.Pontecorvo;56126 Pisa;Infn Napoli;V. Napoli;D. Napoli;Via Cintia 80126;Napoli;Dpto. de F'isica Te'orica y del Cosmos C.A.F.P.E.;U. Strasbourg;Iphc Umr 7178;F. Strasbourg;Grappa;U. Amsterdam;Science Park 904;1098XH Amsterdam;Netherlands.
在我们的银河系中，由加速宇宙射线与星际介质相互作用产生的非常高能量的中微子通量尚未确定。该通量的表征将揭示银河系加速器的功能，气体分布形态和银河宇宙线输运。银河系的中央平面可能是中微子产生增强的场所，因此导致冰立方合作组织测量到的地外中微子信号的各向异性。位于地中海的ANTARES中微子望远镜提供了这部分天空的有利视角，从而为确定这种通量做出了贡献。预期的弥漫银河系中微子发射可以得到，连接宇宙射线的产生和传播的模型与银河系中的气体分布的形态。本文以最近提出的解释银河系高能γ射线弥散辐射的“γ模型”为参考。由“伽马模型”预测的中微子通量依赖于假设的初级宇宙线光谱截止。考虑到一个径向依赖的扩散系数，这个建议的方案是能够占当地的宇宙射线测量，以及银河伽马射线观测。九年的ANTARES数据被用于这项工作，以寻找根据这种情况可能的银河贡献。所有味中微子相互作用被认为是。没有观察到过多的事件，中微子通量的上限设定为“伽马模型”预测的1.1（1.2）倍，假设初级宇宙线光谱截止值为5（50）PeV。这个限制排除了银河中微子的扩散发射，这是冰立方测量的两个半球之间的“光谱异常”的主要原因。
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.