Measurement of the Cosmic Ray e+ + e- spectrum from 20 GeV to 1 TeV with the Fermi Large Area Telescope.

A. A. Abdo; 1; M. Ackermann; M. Ajello; W. B. Atwood; M. Axelsson; 5; BALDINI, LUCA; J. Ballet; G. Barbiellini; D. Bastieri; M. Battelino; B. M. Baughman; K. Bechtol; R. Bellazzini; B. Berenji; R. D. Blandford; E. D. Bloom; G. Bogaert; E. Bonamente; A. W. Borgland; J. Bregeon; A. Brez; M. Brigida; P. Bruel; T. H. Burnett; G. A. Caliandro; R. A. Cameron; P. A. Caraveo; P. Carlson; J. M. Casandjian; C. Cecchi; E. Charles; A. Chekhtman; C. C. Cheung; J. Chiang; 3 S. Ciprini; R. Claus; J. Cohen Tanugi; L. R. Cominsky; J. Conrad; 3; S. Cutini; C. D. Dermer; A. deAngelis; F. dePalma; S. W. Digel; i. Bernardo; E. doCoutoeSilva; P. S. Drell; R. Dubois; D. Dumora; Y. Edmonds; C. Farnier; C. Favuzzi; W. B. Focke; M. Frailis; Y. Fukazawa; S. Funk; P. Fusco; 1.D. Gaggero; 7.F. Gargano; 1.9.D. Gasparrini; N. Gehrels; 3; 3.3.S. Germani; B. Giebels; N. Giglietto; F. Giordano; T. Glanzman; G. Godfrey; D. Grasso; A. Grenier; M. H. Grondin; J. E. Grove; L. Guillemot; S. Guiriec; 3. Hanabata; A. K. Harding; R. C. Hartman; M. Hayashida; 3 E. Hays; 2.3.R. E. Hughes; 14 G. J´ohannesson; 3.A. S. Johnson; 3.R. P. Johnson; 4.W. N. Johnson; 2.T. Kamae; 3 H. Katagiri; 3.2.J. Kataoka; 3.5.N. Kawai; 36; 3.7.M. Kerr; 2.0.J. Kn¨ odlseder; 3.8.D. Kocevski; 3.F. Kuehn; 1.4.M. Kuss; 7 J. Lande; 3 L. Latronico; 7 M. Lemoine Goumard; 30; 31 F. Longo; 9; 10 F. Loparco; 18; 19 B. Lott; 30; 31 M. N. Lovellette; 2.P. Lubrano; 16; 17 G. M. Madejski; 3 A. Makeev; 22; MASSAI, MARCO MARIA; 7.M. N. Mazziotta; 19 W. McConville; 23; 33 J. E. McEnery; 23 C. Meurer; 5; 26 P. F. Michelson; 3 W. Mitthumsiri; 3 T. Mizuno; 32 A. A. Moiseev; 39, 33; † C. Monte; 18; 1.9.M. E. Monzani; 3.E. Moretti; 9; 1.0.A. Morselli; 4.0.I. V. Moskalenko; 3.S. Murgia; 3 P. L. Nolan; 3.J. P. Norris; 4.1.E. Nuss; 2.4.T. Ohsugi; 3.2.N. Omodei; 7.E. Orlando; 4.2.J. F. Ormes; 4.1.M. Ozaki; 43 D. Paneque; 3.J. H. Panetta; 3 D. Parent; 30; 31 V. Pelassa; 2.4.M. Pepe; 16; 17 M. Pesce Rollins; 7.F. Piron; 24 M. Pohl; 4.4.T. A. Porter; 4.S. Profumo; 4.S. Rain` o; 18; 1.9.R. Rando; 11; RAZZANO, MASSIMILIANO; 7.A. Reimer; 3.O. Reimer; 3 T. Reposeur; 30; 3.1.S. Ritz; 23; 33 L. S. Rochester; 3.A. Y. Rodriguez; 4.5.R. W. Romani; 3.M. Roth; 2.0.F. Ryde; 5; 13 H. F. W. Sadrozinski; 4.D. Sanchez; 15 A. Sander; 14 P. M. SazParkinson; 4.J. D. Scargle; 4.6.T. L. Schalk; 4 A. Sellerholm; 5; 26 C. Sgr` o; 7.D. A. Smith; 30; 31 P. D. Smith; 14 G. Spandre; 7 P. Spinelli; 18; 19 J. L. Starck; 8 T. E. Stephens; 2.3.M. S. Strickman; 2.A. W. Strong; 4.2.D. J. Suson; 4.7.H. Tajima; 3.H. Takahashi; 3.2.T. Takahashi; 43 T. Tanaka; 3.J. B. Thayer; 3.J. G. Thayer; 3.D. J. Thompson; 2.3.L. Tibaldo; 11; 1.2.O. Tibolla; 4.8.D. F. Torres; 49; 45 G. Tosti; 16; 1.7.A. Tramacere; 50; 3 Y. Uchiyama; 3.T. L. Usher; 3.A. VanEtten; 3 V. Vasileiou; 23; 5.1.N. Vilchez; 38 V. Vitale; 40; 5.2.A. P. Waite; 3.E. Wallace; 2.0.P. Wang; 3.B. L. Winer; 1.4.K. S. Wood; 2.T. Ylinen; 53

doi:10.1103/PhysRevLett.102.181101

Designed as a high-sensitivity gamma-ray observatory, the Fermi Large Area Telescope is also an electron detector with a large acceptance exceeding 2 m2 sr at 300 GeV. Building on the gamma-ray analysis, we have developed an efficient electron detection strategy which provides sufficient background rejection for measurement of the steeply falling electron spectrum up to 1 TeV. Our high precision data show that the electron spectrum falls with energy as E-3.0 and does not exhibit prominent spectral features. Interpretations in terms of a conventional diffusive model as well as a potential local extra component are briefly discussed.