Computer simulations of modern cosmic microwave background experiments, and an application to the Cosmology Large Angular Scale Surveyor

power read by the reader, what it is important is to observe that the assumed linear dependence (3) between analog and digital figures of power is checked, and with similar

– Spherical Mexican hat wavelet on the sphere software (developed by the Observational Cosmology and Instrumentation Group at

For the calculation of limits (see section 6), the number of observed events in data and expected signal remain the same, while the expected background is modified to correct for

The angular cuts (including the energy cut of 236 ± 30 MeV) and the resulting signal and background efficiencies, the expected number of signal and background events, the

In section 3, the effect of spurious transitions on datapath power and the efectiveness of pipelining and partitioning improvements is quantified by a set of case-studies;

This sample is then normalized to the simulation in the high-multiplicity (more than 6 extra tracks) region and used to estimate the W+jets background in the signal and inclusive W +

As a means to probe the possible fractal structure of the galaxy distribution we have studied the scaling of the num- ber density and angular correlation function of galaxies

A similar effect is found also for some of the cells with density exceeding the virial mean density (  ≈ 340 for the cosmological parameters assumed here), which are classified