Fermi LAT observations of cosmic-ray electrons from 7 GeV to 1 TeV

By M. Ackermann, M. Ajello, W. Atwood, L. Baldini, J. Ballet, G. Barbiellini, D. Bastieri, B. Baughman, K. Bechtol, F. Bellardi and 185 more. 2010

328 citations recorded by the source corpus.

We present the results of our analysis of cosmic-ray electrons using about 8 x 10(6) electron candidates detected in the first 12 months on-orbit by the Fermi Large Area Telescope. This work extend ...

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c766d62ab69fdbf7bf189b0b27369b8455290e6a

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Citations in the corpus

CONSTRAINTS ON COSMIC-RAY PROPAGATION MODELS FROM A GLOBAL BAYESIAN ANALYSIS (2010, methodology): “…is based on fitting to pre-Fermi electron data (conventional model, Strong et al. 2004; Ptuskin et al. 2006), and is parameterized as a broken power law with indices 1.6/2.5 below/above 4 GeV and a steepening (index 5) above 2 TeV, and normalized to the Fermi data at 25 GeV (Ackermann et al. 2010).”
A database of charged cosmic rays (2013, unknown): “…(2005/12-2006/01): Ahn et al. (2009, 2010) – CRISIS (1977/05): Freier et al. (1980); Young et al. (1981) – CRN-Spacelab2 (1985/07-1985/08): Swordy et al. (1990); Mueller et al. (1991) – CRRES (1990/07-1992/10): Duvernois et al. (1996a) – Fermi – Fermi-LAT (2008/06-2011/04): Ackermann et al.…”
Galactic synchrotron emission with cosmic ray propagation models (2013, methodology): “It helps in component separation and for multiwavelength studies including gamma-rays observed by Fermi-LAT and INTEGRAL.”
Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization (2014, unknown): “The PL model of synchrotron emission is related to the power-law energy distribution of the cosmic-ray electron spectrum (Abdo et al. 2009; Ackermann et al. 2010, 2012).”
Search for gamma-ray spectral lines with the Fermi Large Area Telescope and dark matter implications (2013, unknown): “More details regarding these topics can be found in references [29, 30, 31].”
Astrophysical models for the origin of the positron (2011, unknown): “3The so-called “ATIC peak” [6] has not been confirmed by later Fermi [8, 10] and HESS data [7, 9], although no consensus exis ts in the community for an explanation of the disagreement.”
Gamma Ray Signals from Dark Matter: Concepts, Status and Prospects (2012, methodology): “ of space-based instruments, we estimate the level of the diﬀuse background by the IGRB determined by Fermi [231]. For ground-based instruments, we add on top of that the e±-ﬂux measured by Fermi-LAT [319]. At the right end of Fig. 6, with dark blue and red markers, we show the limits that result fr”
The interstellar cosmic-ray electron spectrum from synchrotron radiation and direct measurements. (2011, methodology): “…CAPRICE94 (Boezio et al. 2000), HEAT (DuVernois et al. 2001), SANRIKU (Kobayashi 1999), BETS (Torii et al. 2001), PPT-BETS (Yoshida et al. 2008), ATIC-1-2 (Chang et al. 2008), H.E.S.S. (Aharonian et al. 2008, 2009), Fermi-LAT (Abdo et al. 2009b; Ackermann et al. 2010), PAMELA (Adriani et al. 2011).”
THE FERMI LARGE AREA TELESCOPE ON ORBIT: EVENT CLASSIFICATION, INSTRUMENT RESPONSE FUNCTIONS, AND CALIBRATION (2012, methodology): “Since launch, the particle model has been updated to include new measurements, (see, e.g., Ackermann et al. 2010a, for the electron population).”