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Anisotropies and chemical composition of ultra-high energy cosmic rays using arrival directions measured by the Pierre Auger Observatory

Publicado en:Proceedings of the 32nd International Cosmic Ray Conference, ICRC 2011. 2 137-140 - 2011-01-01 2(), DOI: 10.7529/ICRC2011/V02/0868

Autores: Abreu P; Aglietta M; Ahn EJ; Albuquerque IFM; Allard D; Allekotte I; Allen J; Allison P; Alvarez Castillo J; Alvarez-Muñiz J; Ambrosio M; Aminaei A; Anchordoqui L; Andringa S; Anticic T; Anzalone A; Aramo C; Arganda E; Arqueros F; Asorey H; Assis P; Aublin J; Ave M; Avenier M; Avila G; Bäcker T; Balzer M; Barber KB; Barbosa AF; Bardenet R; Barroso SLC; Baughman B; Bäuml J; Beatty JJ; Becker BR; Becker KH; Bellétoile A; Bellido JA; BenZvi S; Berat C; Bertou X; Biermann PL; Billoir P; Blanco F; Blanco M; Bleve C; Blümer H; Bohácová M; Boncioli D; Bonifazi C; Bonino R; Borodai N; Brack J; Brogueira P; Brown WC; Bruijn R; Buchholz P; Bueno A; Burton RE; Caballero-Mora KS; Caramete L; Caruso R; Castellina A; Catalano O; Cataldi G; Cazon L; Cester R; Chauvin J; Cheng SH; Chiavassa A; Chinellato JA; Chou A; Chudoba J; Clay RW; Coluccia MR; Conceição R; Contreras F; Cook H; Cooper MJ; Coppens J; Cordier A; Cotti U; Coutu S; Covault CE; Creusot A; Criss A; Cronin J; Curutiu A; Dagoret-Campagne S; Dallier R; Dasso S; Daumiller K; Dawson BR; De Almeida RM; De Domenico M; De Donato C; De Jong SJ; De La Vega G; De Mello WJM; De Mello Neto JRT

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Resumen

The Pierre Auger Collaboration has reported evidence for anisotropy in the distribution of arrival directions of the cosmic rays with energies E > Eth = 5.5×1019 eV. These show a correlation with the distribution of nearby extragalactic objects, including an apparent excess around the direction of Centaurus A. If the particles responsible for these excesses at E > Eth are heavy nuclei with charge Z, the proton component of the sources should lead to excesses in the same regions at energies E/Z. We here report the lack of anisotropies in these directions at energies above Eth/Z (for illustrative values of Z = 6, 13, 26). If the anisotropies above Eth are due to nuclei with charge Z, and under reasonable assumptions about the acceleration process, these observations imply stringent constraints on the allowed proton fraction at the lower energies.

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