We present a measurement of the atmospheric \nu _ { e } spectrum at energies between 0.1 TeV and 100 TeV using data from the first year of the complete IceCube detector .
Atmospheric \nu _ { e } originate mainly from the decays of kaons produced in cosmic-ray air showers .
This analysis selects 1078 fully contained events in 332 days of livetime , then identifies those consistent with particle showers .
A likelihood analysis with improved event selection extends our previous measurement of the conventional \nu _ { e } fluxes to higher energies .
The data constrain the conventional \nu _ { e } flux to be 1.3 ^ { +0.4 } _ { -0.3 } times a baseline prediction from a Honda ’ s calculation , including the knee of the cosmic-ray spectrum .
A fit to the kaon contribution ( \xi ) to the neutrino flux finds a kaon component that is \xi = 1.3 ^ { +0.5 } _ { -0.4 } times the baseline value .
The fitted/measured prompt neutrino flux from charmed hadron decays strongly depends on the assumed astrophysical flux and shape .
If the astrophysical component follows a power law , the result for the prompt flux is 0.0 ^ { +3.0 } _ { -0.0 } times a calculated flux based on the work by Enberg , Reno and Sarcevic .